The 5th Zermatt ISM Symposium

Conditions and impact of star formation:

New results with Herschel and beyond

Abstract Book

Zermatt. Switzerland2010, September 19 – 24

Edited by Markus Rollig, roellig@ph1.uni-koeln.deand Robert Simon, simonr@ph1.uni-koeln.de

Scientific Organizing Committee

Michael Burton, UNSW, AustraliaJose Cernicharo, DEMIR, CSIS, SpainMartin Harwit, Cornell Univ., USADavid Hollenbach, SETI, USAMichael Meyer, ETH Zrich, SwitzerlandAlain Omont, CNRS IAP, FranceMonica Rubio, Univ. de Chile, ChileStephan Schlemmer, Cologne Univ., GermanyLinda Tacconi, MPE, GermanyXanderTielens, Leiden Sterrewacht, NetherlandsGlenn White, Open Univ., United KingdomSatoshi Yamamoto, Tokyo Univ., Japan

Local Organizing Committee

I. Physikalisches Institut, Koln:M. Akyilmaz, A. Eckart, Y. Okada, V. Os-senkopf, M. Rollig, P. Schilke, R. Simon,C. Straubmeier, J. StutzkiMPIfR, Bonn:S. Leurini, F. Wyrowski, S. BritzenAIfA, Bonn:F. Bertoldi, K. KnudsenETH Zurich:A. Benz, C. Dedes, S. Wampfler

The 5th Zermatt ISM Symposium is sponsored by the Deutsche Forschungsgemeinschaft (DFG), the Swiss Na-tional Science Foundation (SNSF), and the Hochalpine Forschungsstationen Jungfraujoch & Gornergrat (HFSJG).

Contents

Program 15

Talks 20I. Herschel Status and Perspectives including Instruments. . . . . . . . . . . . 20

Herschel Mission Status 21Goran Pilbratt

SPIRE 22Matt Griffin

PACS 23Albrecht Poglitsch

HIFI 24Frank Helmich

Herschel Science and Beyond 25Ewine van Dishoeck

II. Extreme star formation: high-z, starburst, gal. nuclei. . . . . . . . . . . . . 26

Dusty extreme starbursts in theearly universe 27Kotaro Kohno

Molecules at the Reionization Epoch 28Amiel Sternberg

The very large scale environment of star formation:Dust and gas inthe cosmic web 29Stephen Eales

Galaxy Formation (HerMES) 30Sebastian Oliver

Galaxy Formation from deep surveys with Herschel/PACS 31Dieter Lutz

Rapidly Star-Forming Galaxies in the Peak Epoch of Galaxy Formation 32Romeel Dave

Star formation in IR-bright galaxies (SHINING) 33Eckhard Sturm

Extreme star formation and AGNs in ultra luminous infrared galaxies: spectroscopic fingerprints 34Paul van der Werft

AzTEC/ASTE 1.1 mm Deep Surveys: Number Counts and Clustering of Millimeter-bright Galaxies 35Bunyo Hatsukade

Observations of CO J = 1-0 at z 2.5: constraints on the ISM of high-redshift galaxies. 36Andrew Harris

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Densitometry and Thermometry of Starburst Galaxies 37Jeff Mangum

The Peculiar Star Formation Environment of the Galactic Center 38Mark Morris

Large molecular loops in the Galactic Center: Evidence for Parker Instabiity 39Yasuo Fukui

High Redshift Star Formation: where are the baryons? 40Malcolm Bremer

III. SF in disk galaxies: morphology, structure, and dynamics. . . . . . . . . 41

Star formation in disk galaxies today 42Robert Kennicutt

The impact of star formation on low metallicity ISM 43Suzanne Madden

The Fine-scale Structure of th neutral ISM in nearby Galaxies 44Ioannis Bagetakos

HERACLES and the Spatially Resolved Star Formation Law 45Elias Brinks

Star formation in M33 (HERM33ES) 46Carsten Kramer

Galactic structure and Dynamics 47Clare Dobbs

Star formation in the Magellanic Clouds 48Margaret Meixner

Anomalous Dust in Late-Type Galaxies 49Frank Israel

NRO legacy project: M33 all disk survey of Giant Molecular Clouds (GMCs) with NRO-45m and ASTE-10m telescopes 50

Tomoka Tosaki

ATLASGAL, the APEX Telescope Large Area Survey of the Galaxy 51Friedrich Wyrowski

HOPS: The H2O southern Galactic Plane Survey 52Andrew Walsh

IV. Star formation: physical & chemical conditions/feedback. . . . . . . . . . 53

Radiative Feedback 54Norman Murray

Outflows and Jets from young stars and their feedback 55Sylvie Cabrit

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PDRs and XDRs 56Mark Wolfire

Understanding the physics of the X-factor 57Simon Glover

The CO-H2 conversion factor of diffuse ISM: Does the 12CO emission trace dense molecular gas? 58Jerome Pety

Deciphering the molecular fingerprints of evolved star’s envelopes 59Leen Decin

Formation and evolution of molecular clouds in a turbulentand multi-phase ISM 60Patrick Hennebelle

The relation between gas and dust in the Taurus Molecular Cloud 61Jorge Pineda

EPOS: A Herschel key programm on the earliest phasesof star formation 62Oliver Krause

The State of the Diffuse Interstellar Gasfrom Herschel’s GOT C+ Survey 63William Langer

V. Formation of stars: high M, low M, planetary systems. . . . . . . . . . . . . 64

High Mass star formation 65Hans Zinnecker

First results from Herschel Orion Protostar Survey 66Babar Ali

Probing the formation mechanism of prestellar cores and the origin of the IMF: First results from theHerschel Gould Belt Survey 67

Philippe Andre

Low Mass star formation 68Michael R. Meyer

From filaments to protostars: multi-scale star formationin the Hi-GAL survey 69Sergio Molinari

Water in massive star-forming regionswith Herschel Space Observatory 70Fabrice Herpin

WISHes coming true - Water in low-massstar-forming regions with Herschel 71Lars Kristensen

New insights to photon-dominated regionsfrom Herschel observations 72Volker Ossenkopf

Outflow and Inflow in high mass star forming regions 73Malcolm Walmsley

Physical and chemical conditions in star forming regions 74C Ceccarelli

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First results from the Herschel Gas in Protoplanetary disks Systemsproject 75Wing-Fai Thi

HIFI observations of high-mass star formation 76Floris van der Tak

VI. Laboratory astrophysics, astrochemistry. . . . . . . . . . . . . . . . . . . . . . 77

Chemical Processes in the ISM 78Edwin Bergin

The Evolution of Dust in the ISM 79Alain Abergel

Formation of complex carbon-containing molecules in space 80Wolf D. Geppert

Initial Results from the Herschel Oxygen Project (HOP) 81Paul Goldsmith

Collision Rate Coefficients 82Marie-Lise Dubernet

The Ortho/Para Ratio in Interstellar Water 83Darek Lis

Coreshine : the ubiquity of micron-size grains in star-forming regions 84Laurent Pagani

Gas phase Laboratory Astrophysics 85Stephan Schlemmer

Chemical Models of Hot Cores 86Hideko Nomura

Complex organic chemistry in the Galactic Center Region 87Jesus Martin-Pintado

Peculiar Carbon-Chain Chemistryin Low-Mass Star Forming Regions 88Nami Sakai

Radiation Diagnostics in YSOs Using Diatomic Hydrides 89Arnold Benz

Laboratory Astrophysics of dust 90Cornelia Jager

VII. Future opportunities. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 91

Tools for future progress: Laboratory, Instruments and Telescope 92Martin Harwit

Development status of ALMA 93Thijs de Graauw

APEX instrumentation: status and near-term developments 94Stefan Heyminck

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SOFIA - Update and the Beginning of Early Science Flights 95Erick Young

JWST and Star Formation 96Thomas Greene

Science with SPICA, the next generationmid- and far-IR space telescope 97Javier R. Goicoechea

Far-infrared Polarimetry of the ISM 98John Vaillancourt

The Echelon-cross-Echelle Spectrograph for SOFIA 99Matthew Richter

GISMO - A 2 millimeter Bolometer Camerafor the IRAM 30m Telescope 100Johannes Staguhn

NOEMA 101Karl-Friedrich Schuster

PosterSession 1, starting Tuesday, September 21 102

I. Herschel Status and Perspectives including Instruments. . . . . . . . . . . . 102

P-I-1: In-Flight Calibration of the Herschel/HIFI instrument 103Michael Olberg

II. Extreme star formation: high-z, starburst, gal. nuclei. . . . . . . . . . . . . 104

P-II-1: Molecules as Tracers of Galactic Evolution 105Francesco Costagliola

P-II-2: The Warm ISM in the Galactic Center: mid-J CO and Atomic Carb on Lines Observations withthe NANTEN 2 Telescope. 106

Pablo Garcia

P-II-3: The Zpectrometer: A wideband instrument for detecting and characterizing low-J CO emissionfrom high-redshift galaxies. 107

Andrew Harris

P-II-4: An AzTEC/ASTE detection of an ultra-bright submillimeter ga laxy in SXDF 108Soh Ikarashi

P-II-5: Disentangling star-formation and accretion at high redshift in a MAMBO deep field 109Robert Lindner

P-II-6: Characterizing the Molecular ISM in Extreme Star-Format ion Environments: a Starburst (M82)and a ULIRG (Arp 220) 110

Rangwala Naseem

P-II-7: Evolutionary Models of Infrared Galaxy Spectra 111Douglas O’Rourke

P-II-8: HerMES (the Herschel Multi-Tiered Extragalactic Survey): high redshift galaxies 112Ismael Perez-Fournon

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P-II-9: Submillimeter Array Identification of the Millimeter-selected Galaxy SSA22-AzTEC1: A Proto-quasar in a Proto-cluster? 113

Yoichi Tamura

P-II-10: The role of radiation pressure in the dynamics of HII regions at redshift z¿1 114Silvia Verdolini

III. SF in disk galaxies: morphology, structure, and dynamics. . . . . . . . . 115

P-III-1: WISE and the Dusty Universe 116Dominic Benford

P-III-2: On the spatial distribution of FIR sources in the Galactic plane 117Nicolas Billot

P-III-3: The effects of star formation on the low-metallicity ISM seen with the Herschel/PACS spectrom-eter 118

Diane Cormier

P-III-4: Herschel Observations of C+ in the Vicinity of Star Forming C omplexes in the Galactic Plane 119Jorge Pineda

P-III-5: Detecting spiral arm clouds by CH absorption lines 120Sheng-Li Qin

P-III-6: Tracers of star-formation in nearby Galaxies. NGC253 and NGC4945 1mm surveys with theAPEX telescope. 121

Miguel Angel Requena Torres

P-III-7: Dust and Stellar Emission of Nearby Galaxies 122Ramin Skibba

P-III-8: 3D decomposition of the dust emission in the Hi-GAL SDP fields 123Alessio Traficante

P-III-9: Molecular Gas and Star Formation in Barred Spiral Galaxy NGC 3 627 124Yoshimasa Watanabe

IV. Star formation: physical & chemical conditions/feedback. . . . . . . . . . 125

P-IV-1: FIR Fine-Structure Line Mapping the Interstellar Medium o f the Galactic Plane with Strato-spheric Terahertz Observatory (STO) 126

Meltem Akyilmaz Yabaci

P-IV-2: FIR Line Transfer Including Source Intrinsic Dust Opacities : Upgrading the Spherically Sym-metric SimLine Code 127

Meltem Akyilmaz Yabaci

P-IV-3: Assessing Radiation Pressure as a Feedback Mechanism in Star-forming Galaxies 128Brett Andrews

P-IV-4: Dust and gas in photodissociation regions observed with Herschel 129Heddy Arab

P-IV-5: An observational study of star formation feedback in Orion 130Olivier Berne

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P-IV-6: Multiple Molecular Line Mapping of the Central Molecular Zone at 3 and 7 mm 131Michael Burton

P-IV-7: Galactic genesis: star formation in the molecular cloud W43 132Philipp Carlhoff

P-IV-8: Molecules as Tracers of Galactic Evolution 133Francesco Costagliola

P-IV-9: Herschel observations of EXtra-Ordinary Sources: The Terahertz spectrum of Orion KL seenat high spectral resolution 134

Nathan Robert Crocket

P-IV-10: Clumpy PDR modelling of the Orion Bar region 135Markus Cubick

P-IV-11: The reliability of CII as a SF tracer 136Ilse De Looze

P-IV-12: Dynamical processes in the S140 region traced by HIFI [CII] emission 137Carolin Dedes

P-IV-13: Atmospheric calibration for submillimeter observation 138Xin Guan

P-IV-14: molecular emission in regions of star formation 139Antoine Gusdorf

P-IV-15: Equilibrium states of a recombining plasma heated by a ration field and dissipation of soundwaves 140

Miguel Ibanez

P-IV-16: Ionized Carbon in theMagellanic Clouds 141Frank Israel

P-IV-17: Analysis of CO, density, and temperature distributions in simulated molecular clouds 142Faviola Molina

P-IV-18: PDR properties and spatial structures probed by Herschel and Spitzer spectroscopy 143Yoko Okada

P-IV-19: Submillimeter Line Emission from LMC 30 Dor: The Impact of a Starburst on a Low Metal-licity Environment 144

Jorge Pineda

P-IV-20: Molecular Tracers of Turbulent Shocks in Giant Molecular Clouds 145Andy Pon

P-IV-21: KOSMA-tau: Recent Developments in Modeling Photodissociation Regions 146Markus Rollig

P-IV-22: Modeling Photo-Induced Chemistry in the Warm and DenseISM ( WADI) 147Markus Rollig

P-IV-23: Dust/gas correlations in the Large Magellanic Cloud 148Julia Roman-Duval

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P-IV-24: Star formation in the Rosette Molecular Cloud under the influence of NGC2244 149Nicola Schneider

P-IV-25: Submillimeter Astronomy with the SMART receiver at NANT EN2: New results 150Robert Simon

P-IV-26: Diffuse interstellar PAH emission in the LMC observed with the AKARI/IRC 151Hideki Umehata

P-IV-27: Herschel’s GOT C+ Survey of Cloud Transitions in the Inner Galaxy 152Thangasamy Velusamy

Session 2, starting Thursday, September 23 153

V. Formation of stars: high M, low M, planetary systems. . . . . . . . . . . . . 153

P-V-1: The mid-infrared extinction law in the Trifid nebula 154Laurent Cambresy

P-V-2: The CHESS Spectral Survey of the Solar Type Protostar IRAS16293-2422 155Emmanuel Caux

P-V-3: Water in massive star forming regions: HIFI observations of W3-IRS5 156Luis Chavarria

P-V-4: HIFI observations of deuterated water towards SgrB2-M 157Claudia Comito

P-V-5: Hot core millimeter and submillimeter spectra : Comparing simulations with IRAM and Herschel-HIFI spectra 158

Massimo De Luca

P-V-6: The morphology of the high mass star formation sites N44 and N63 in the LMC 159Sacha Hony

P-V-7: Water in Star-Forming Regions with Herschel - IntermediateMass Protostars 160Doug Johnstone

P-V-8: The Chemical Herschel Spectral Survey of Star Forming Regions: Peering into the protostellarshock L1157 B1. 161

Bertrand Lefloch

P-V-9: Herschel observations of the distribution of water in cluster-forming regions 162Silvia Leurini

P-V-10: Comprehensive View of Massive Quiescent Cores 163Di Li

P-V-11: Galactic Young Star Clusters and their Molecular Environment 164Esteban Morales

P-V-12: The Herschel view of the Perseus Star Forming region 165Stefano Pezzuto

P-V-13: HEXOS Observations of C18O & C17O in Orion KL 166Rene Plume

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P-V-14: Structure of Hot Cores 167Rainer Rolffs

P-V-15: Star formation in the Orion A Molecular Cloud 168Yoshito Shimajiri

P-V-16: Modelling Herschel observations of hot gas emission in low-mass protostars 169Ruud Visser

P-V-17: Cold Disks around Nearby Stars. A Search for Edgeworth-Kuiper Belt Analogues 170Glenn White

P-V-18: Energetic processes revealed by spectrally resolved high-J CO lines in the low-mass star-formingregions with Herschel 171

Umut A. Yildiz

VI. Laboratory astrophysics, astrochemistry. . . . . . . . . . . . . . . . . . . . . . 172

P-VI-1: DIMETHYL ETHER IN LABORATORY AND SPACE 173Christian Endres

P-VI-2: Laboratory Astrochemistry in the Infrared:High-Resolu tion-Spectroscopy and Molecular Struc-ture of Carbon-Silicon-Clusters 174

Jurgen Krieg

P-VI-3: Herschel and APEX Observations of Light Hydride Species: The Need for Further LaboratoryData and Developments in the CDMS 175

Holger Muller

P-VI-4: Deuterium chemistry : measuring the age of prestellar cores 176Laurent Pagani

P-VI-5: Deuterium astrochemistry 177Berengere Parise

P-VI-6: There is MAGIX in CATS 178Peter Schilke

P-VI-7: Laboratory Astrochemistry in the Infrared: High-Resolu tion-Spectroscopy and Molecular Struc-ture of Carbon-Silicon-Clusters 179

Sven Thorwirth

P-VI-8: Probing the Water Chemistry in Young Stellar Objects with Hyd roxyl Observations 180Susanne Wampfler

P-VI-9: Observations of the K-Doublet Lines of H2CO 181Alwyn Wootten

P-VI-10: Line survey of L1157 b1 shocked region 182Takahiro Yamaguchi

VII. Future opportunities. . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 183

P-VII-1: Submillimeter and THz Receiver Development at KOSMA 184Urs Graf

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P-VII-2: The German SOFIA first light instrument GREAT: status and f uture oppurtunities 185Stefan Heyminck

P-VII-3: KOSMA Submm and THz Detector Development 186Netty Honingh

List of Participants 187

Notes 192

14

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19

Talks

Session I:Herschel Status and Perspectives including Instruments

20

The ESA Herschel Space Observatory: first year inflight and early highlights

GORAN L. PILBRATT

ESA Research and Scientific Support Department, ESTEC/SRE-SA, Keplerlaan 1, NL-2201 AZ Noordwijk, TheNetherlands<gpilbratt@rssd.esa.int>

The Herschel Space Observatory was successfully launched on 14 May 2009, carried into space by an Ariane 5ECA launcher together with the second passenger Planck, both spacecraft being injected into transfer orbits to-wards L2 with exquisite precision. Herschel is the most recent observatory mission in the European Space Agency(ESA) science programme. It carries a 3.5 metre diameter Cassegrain passively cooled monolithic silicon carbidetelescope. The focal plane units of the science payload complement - two cameras/medium resolution imagingspectrometers, the Photodetector Array Camera and Spectrometer (PACS)and Spectral and Photometric ImagingREceiver (SPIRE), and the very high resolution Heterodyne Instrument for the Far-Infrared (HIFI) spectrometer -are housed in a superfluid helium cryostat.

Herschel is the first large aperture space infrared observatory, it builds on previous infrared space missions in-cluding the IRAS, ISO, AKARI, and Spitzer observatories, by offeringa much larger telescope and pushes towardslonger wavelengths. It will perform imaging photometry and spectroscopyin the far infrared and submillimetrepart of the spectrum, covering approximately the 55-671µm range. I will describe Herschel and its science capa-bilities putting it into perspective. Herschel is designed to observe the ’cool universe’; the key science objectivesinclude star and galaxy formation and evolution, and in particular the physics, dynamics, and chemistry of theinterstellar medium and its molecular clouds, the wombs of the stars and planets.

Herschel is currently opening a new window to study how the universe has evolved to become the universe wesee today, and how our star the sun, our planet the earth, and we ourselves fit in. I will outline the early inflightoperations of Herschel and the transition from launch and early operational phases into the routine science phase.I will present the demonstrated science capabilities and provide examples ofscientific highlights to date.

Herschel has been designed to offer a minimum of 3 years of routine science observations. Nominally∼20,000hours will be available for astronomy, 32% is guaranteed time (GT) and the remainder is open time (OT) offeredto the general astronomical community through a standard competitive proposal procedure. I will describe futureobserving opportunities.

21

Herschel SPIRE: in-flight performance and status of pipelines and calibration

MATT GRIFFIN1 ON BEHALF OF THESPIRE CONSORTIUM

1 Cardiff Uiversity,matt.griffin@astro.cf.ac.uk

SPIRE, the Spectral and Photometric Imaging Receiver, is Herschels submillimetre camera and spectrometer.SPIRE is fully functional in flight, with performance meeting or exceeding pre-flight estimates in all respects: thephotometer performance is comparable to or slightly better than the pre-launchpredictions, and the FTS achievesa sensitivity better than the pre-launch advertised performance by a factor of approximately two. The SPIREdata processing pipelines are also producing high quality photometric and spectroscopic data. The main designfeatures, operating modes, measured in flight performance, and scientific capabilities of the SPIRE photometerand spectrometer will be reviewed. The current status of the instrument flux calibration and the data processingpipleines will also be summarised, and plans for future data processing enhancements and user support will beoutlined.

22

PACS

A POGLITSCH1

1 Max-Planck-Institut fr extraterrestrische Physik, Garchin, Germany,alpog@mpe.mpg.de

23

Herschel-HIFI - introduction of instrument and its science

F.P. HELMICH1 ON BEHALF OF THEHIFI CONSORTIUM

1 SRON Netherlands Institute for Space Research,f.p.helmich@sron.nl

HIFI, the Heterodyne Instrument for the Far-Infrared, is the high resolution spectrometer on board of Herschel. Theinstrument is designed to be electronically tuneable over a wide and continuous frequency range in the Far Infrared,with velocity resolutions better than 0.1 km/s with a high sensitivity. This will enable detailed investigations ofa wide variety of astronomical sources, ranging from solar system objects, star formation regions to nuclei ofgalaxies. The instrument comprises 5 frequency bands covering 480-1150 GHz with SIS mixers and a sixth dualfrequency band, for the 1410-1910 GHz range, with Hot Electron Bolometer Mixers (HEB). The Local Oscillator(LO) subsystem consists of a dedicated Ka-band synthesizer followed by 7 times 2 chains of frequency multipliers,2 chains for each frequency band. A pair of Auto-Correlators and a pair of Acousto-Optic spectrometers processthe two IF signals from the dual-polarization front-ends to provide instantaneous frequency coverage of 4 GHz,with a set of resolutions (140kHz to 1 MHz), better than< 0.1 km/s. After a delay of half a year, caused by asingle event upset, HIFI has been successfully commissioned and verified in space at the time of writing.

The HIFI-consortium has defined several Guaranteed Time Key Programmes. In these large and coherentprogrammes different topics are studied in detail as well as in the larger context. Three programmes focus onstar-formation, two on general interstellar medium, one on late stages of stellarevolution, one on solar systemobjects and one on the interstellar medium in galaxies.

I will briefly introduce HIFI as an instrument and its observational modes and then continue with sciencehigh-lights taken from the first half year of observations in the HIFI Key Programmes.References:De Graauw, Th., et al. 2010, A&A in pressRoelfsema, P.R., et al. 2010, A&A in press

24

The interstellar medium and star formation: Herschel in the context of future facilities

E.F. VAN DISHOECK1,2

1 Leiden Observatory, Leiden University, P.O. Box 9513, 2300 RA Leiden, The Netherlandsewine@strw.leidenuniv.nl

2 Max Planck Institute for Extraterrestrial Physics, Garching, Germany

Over the past two decades, many conferences and workshops have been held discussing ’the promise of Her-schel’. It is a pleasure to present here an overview of actual data andresults from Herschel in the field of theinterstellar medium and star-formation. Herschel has more than lived up to thehigh expectations, as evidencedfrom the rich harvest of first papers. Some imaging and spectroscopic highlights from all three instruments ad-dressing major questions in the field will be presented. They will be placed in the context of future facilities beingbuilt or planned, including ALMA, JWST and E-ELT.

25

Session II:Extreme star formation: high-z, starburst, gal. nuclei

26

Dusty extreme starbursts in theearly universe

KOTARO KOHNO1

1 University of Tokyo,kkohno@ioa.s.u-tokyo.ac.jp

27

Molecules at the Reionization Epoch

A. STERNBERG1

1 Tel Aviv University, Israel,amiel@wise.tau.ac.il

Molecules containing elements heavier than hydrogen, helium, and lithium, firstformed at the epoch of reioniza-tion following the appearance of the ”Population III” stars, and the introduction of ”metals” into the interstellarand intergalactic medium. I will discuss the expected molecular compositions of cool clouds that may have formedat this epoch, with emphasis on interstellar ion-molecule chemistry at very low but non-zero metallicities.

28

The Herschel ATLAS

S. EALES1

1 School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3AA, UKsae@astro.cf.ac.uk

The Herschel ATLAS, the largest Herschel open-time survey, is a survey of 550 square degrees in five far-infrared and submillimetre bands. I will describe the early results from the first 50 square degrees of the survey.These results will include (i) the discovery that cosmic evolution starts at a very low redshift, (ii) the discoveryof star-forming clouds with very low masses at high galactic latitude, (iii) the confirmation that the Herschel 500-micron band is the ‘golden spot for finding gravitational lenses. I will discuss the contributions that large-areaHerschel surveys (with ALMA follow-up) are likely to make to our understanding of star formation in galaxies.

29

Galaxy Formation (HerMES)

SEBASTIAN OLIVER1

1 University of Sussex,S.Oliver@Sussex.ac.uk

30

Galaxy evolution from deep surveys with Herschel/PACS

D. LUTZ1

1Max-Planck-Institut fr extraterrestrische Physik,lutz@mpe.mpg.de

Beginning with science demonstration phase observations of the GOODS-N field and the lensing cluster Abell2218, deep cosmological surveys carried out with PACS as part of the PEP key programme have started to revealthe potential of deep far-infrared suveys with Herschel for the study of galaxy evolution. We have already observeda range of key multi-wavelength fields, from the full 2 square degrees ofthe COSMOS field observed at 100 and160micron to superdeep observations of the GOODS-S field at 70, 100, and 160micron. The PACS data resolve themajority of the cosmic infrared background near its peak wavelength into individually well detected sources, thatallow to determine the background’s constituents in terms of redshift and objects class, and to study the evolutionof star formation rate density and infrared luminosity function. The provide new insights into spectral energydistributions, luminosities, star formation rates, and dust masses of high redshift galaxies, suggesting subtle butimportant revisions of previous extrapolations from other wavelegnths. New light is being shed on the influence ofenvironment on star formation in z 1 galaxies, and on the star formation properties of AGN hosts.

31

Rapidly Star-Forming Galaxies in the Peak Epoch of Galaxy Formation

R. DAV E1

1 University of Arizona,rad@as.arizona.edu

I will discuss insights from cosmological hydrodynamic simulations on the nature and driving physics forrapidly star-forming galaxies during the peak epoch of galaxy formation(z ∼ 1 − 4). I will argue that most ofthese systems are being fueled from the IGM at very rapid rates, owing to efficient cold accretion during this epoch.Hence such galaxies are more analogous to local spirals rather than localULIRGs, i.e. they are not starbursts(asthey are commonly called) because they are not consuming their gas much faster than supplied. However, therapid accretion results in qualitative changes in morphologies as compared tolocal spirals. I will show that thisscenario neatly unites a wide range of observations, including all but the most extreme sub-millimeter galaxies. Iwill further discuss the role of feedback, which is ubiquitous and necessary in these galaxies, and how feedbackcritically governs the growth of mass and metallicity in early galaxies. Indeed, the recently-forwarded FundamentalMetallicity Relation yields tight constraints on the nature and form of feedback. I will conclude by identifying asmall but nagging (even in the era of Herschel) discrepancy between models and data that may require some ratherradical thinking to reconcile, either implying a substantial revision of our theoretical ideas or else a changing IMF.

References:Dave, R., Finlator, K., Oppenheimer, B.D., Fardal, M., Katz, N., Keres, D., Weinberg,D.H. 2010, MNRAS, 404, 1355Dave, R. 2008, MNRAS, 385, 147Mannucci, F., Cresci, G., Maiolino, R., Marconi, A., Gnerucci, A. 2010, MNRAS,submitted, arXiv:1005.0006

Far-IR diagnostics of the ISM in IR bright star-forming gala xies (SHINING)

E. STURM1

AND THE SHINING TEAM

1 Max-Planck-Institute for Extraterrestrial Physics (MPE),sturm@mpe.mpg.de

As part of the Herschel Key Project SHINING we are obtaining PACS far-infrared spectroscopy of local and distantstar-forming galaxies in order to study their ISM. I will present some surprising and promising first results fromthis programme. This includes spatially resolved PDR diagnostics, high-J CO lines, line deficit diagnostics and itsmodeling as two major modes of star formation, as well as OH as tracer of chemistry and kinematics (large scaleoutflows).

Extreme star formation and AGNs in ultraluminous infrared ga laxies - spectroscopic fingerprints

PAUL P. VAN DER WERF1

1 Leiden Observatory,pvdwerf@strw.leidenuniv.nl

Recent spectroscopic results from Herschel and from groundbased (sub)mm telescopes provide a new windowon the ISM of (ultra)luminous infrared galaxies ((U)LIRGs). Spectral lines reveal the fingerprints of the relevantprocesses: UV-radiation by hot stars, X-ray irradiation from an AGN,enhanced cosmic ray fluxes from multiplesupernova remnents, mechanical heating by shocks, etc. Local (U)LIRGs provide excellent laboratories for theseprocesses, and can be used as a local benchmark for high-z observations with ALMA. I will discuss recent ob-servational results on star forming galaxies and AGNs, discuss recent theoretical developments, and look forwardtowards the use of ALMA for probing high-z galaxies using these diagnostics.

AzTEC/ASTE 1.1 mm Deep Surveys: Number Counts and Clustering ofMillimeter-brightGalaxies

B. HATSUKADE1 ET AL .

1 Nobeyama Radio Observatory,hatsukade@ioa.s.u-tokyo.ac.jp

We present results of a 1.1 mm deep survey of the AKARI Deep Field South (ADF-S) with the AzTECmounted on the Atacama Submillimetre Telescope Experiment (ASTE). We obtaineda map of 0.25 deg2 areawith an rms noise level of 0.32–0.71 mJy. This is one of the deepest and widest maps thus far at millimetre andsubmillimetre wavelengths. We uncovered 198 sources with a significance of3.5–15.6σ, providing the largestcatalog of 1.1 mm sources in a contiguous region. Most of the sources arenot detected in the far-infrared bands oftheAKARI satellite, suggesting that they are mostly atz ≥ 1.5 given the detection limits. We construct differentialand cumulative number counts of the ADF-S, the Subaru/XMM Newton Deep Field (SXDF), and the SSA 22 fieldsurveyed by AzTEC/ASTE, which provide currently the tightest constraints on the faint end. The integration ofthe differential number counts of the ADF-S find that the contribution of 1.1 mmsources with≥1 mJy to thecosmic infrared background (CIB) at 1.1 mm is 12–16%, suggesting that the large fraction of the CIB originatesfrom faint sources of which number counts are not yet constrained. We estimate the cosmic star-formation ratedensity contributed by 1.1 mm sources with≥1 mJy using the differential number counts and find that it is lowerby about a factor of 5–10 compared to those derived from UV/optically-selected galaxies atz ∼ 2–3. If weconsider the fraction of 1.1 mm sources to the CIB, the star-formation rate density of 1.1 mm sources includingfainter sources (<1 mJy) would become comparable to or higher than those of UV/optically-selected galaxies.Clustering analyses of AzTEC sources in the ADF-S and the SXDF find thatbright (>3 mJy) AzTEC sources aremore strongly clustered than faint (<3 mJy) AzTEC sources and the average mass of dark halos hosting brightAzTEC sources was calculated to be 1013–1014 M⊙. Comparison of correlation lengths of AzTEC sources withother populations and with a bias evolution model suggests that dark halos hosting bright AzTEC sources evolveinto systems of clusters at present universe and the AzTEC sources residing the dark halos evolve into massiveelliptical galaxies located in the center of clusters.

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Signal map of the ADF-S. Whitecontours represent the 30% and50% coverage regions (corre-sponding to rms noise levelsof 0.55 and 0.72 mJy beam−1)from the inside to the out-side. Detected 198 sources with≥3.5σ in the 30% coverage re-gion are indicated by green cir-cles with a 30′′ diameter, andnumbered in order of signifi-cance.

Observations of COJ = 1–0 atz ∼ 2.5: constraints on the ISM of high-redshift galaxies.

A.I. HARRIS1, A.J. BAKER2, C.E. SHARON2, A.M. SWINBANK 3, A.J. DANIELSON3, I. SMAIL 3

1 Department of Astronomy, University of Maryland, College Park, MD 20742, USAharris@astro.umd.edu

2 Department of Physics and Astronomy, Rutgers, The State University of Mew Jersey, 136 Frelinghuysen Rd.,Piscataway, NJ 08854, USA,ajbaker@physics.rutgers.edu, csharon@physics.rutgers.edu

3 Department of Physics, Durham University, South Road, Durham, DH1 3LE, UK,a.m.swinbank@durham.ac.uk, a.l.r.danielson@durham.ac.uk,

ian.smail@durham.ac.uk

Observations of the ground-state rotational transition of the carbon monoxide (CO) molecule have been theworkhorse of galactic and local extragalactic millimeter-wave astronomy for many years. CO’s high abundance,small dipole moment, strong internal chemical bond, andJ = 1 energy 5 K above ground, all combine to allowthe molecule to trace molecular gas over a wide range of temperatures and densities. The COJ = 1–0 transitionhas proven to be an indispensable tool for estimating molecular gas masses and physical conditions in the localuniverse.

Most observations of CO at high redshift have been in midJ (Jupper of 3-7) lines, however; these redshift intothe observed-frame millimeter wave bands where high-sensitivity observations are possible. Observations of theJ = 1–0 line have been difficult because line flux drops from the mid-J lines as approximately frequency squared,requiring sensitivities about an order of magnitude larger than millimeter-waves for work on the 1–0 line: Stablecentimeter-wave receivers on large antennas are needed to observe the 1–0 line.

Here we reportJ = 1–0 observations of a number of submillimeter galaxies made with the Zpectrometercor-relation spectrometer on the National Radio Astronomy Observatory’s 100 meter diameter Green Bank Telescope.In addition to making accurate measurements of CO 1–0 line parameters, the Zpectrometer’s wide bandwidth,instantaneously coveringz = 2.2 to 3.5, has provided precise redshifts for strongly-lensed galaxies at unknownredshifts, enabling multi-line studies with narrower-band instruments.

Our observations directly test and verify the validity of assumed scaling relations used to relate mid-J fluxesto molecular gas masses. We show why understanding the 1–0 emission is key tousing flux from the 3–2 and4–3 lines to deduce the state of the interstellar medium in galactic nuclei. In the submillimeter galaxies we haveobserved, the 1–0/3–2 line flux ratios rule out emission dominated by subthermally excited gas, the basis for themass density conversion factor derived for ULIRGs in the local universe. Our results motivate a critical scrutinyof customary extrapolations of the conversion factor from local systems tothose at high redshift.

Densitometry and Thermometry of Starburst Galaxies

JEFFREYG. MANGUM1, JEREMY DARLING2, KARL M. M ENTEN3, AND CHRISTIAN HENKEL3

1 National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903-2475, USA,jmangum@nrao.edu

2 Center for Astrophysics and Space Astronomy, Department of Astrophysical and Planetary Sciences, Box 389,University of Colorado, Boulder, CO 80309-0389, USA,jdarling@origins.colorado.edu

3 Max Planck Institut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany,kmenten@mpifr-bonn.mpg.de; chenkel@mpifr-bonn.mpg.de

With a goal toward deriving the physical conditions in external galaxies, we present a survey of formaldehyde(H2CO) and ammonia (NH3) emission and absorption in a sample of starburst systems using the Green BankTelescope. By extending well-established techniques used to derive the spatial density in star formation regions inour own Galaxy, we show how the relative intensity of the110 − 111 and211 − 212 K-doublet transitions of H2COcan provide an accurate densitometer for the active star formation environments found in starburst galaxies (seeMangumet al. 2008). Similarly, we employ the well-established technique of using the relative intensities of the(1,1), (2,2), and (4,4) transitions of NH3 to derive the kinetic temperature in starburst galaxies.

For the H2CO measurements, we have applied our technique to a sample of twenty-four IR-bright galaxieswhich exhibit various forms of starburst activity. Figure 1 shows two examples of our measurement results. Emis-sion in either of the two H2CO transitions in this study are signs of high spatial density. Observed emission inthe H2CO 211 − 212 transition toward Arp 220 signals a relatively high density (log(n(H2)(cm

−3)) ≃ 5.7). Ab-sorption in both H2CO transitions toward NGC 253, on the other hand, signals an average density that is lower(log(n(H2)(cm

−3)) ≃ 5.0).Our NH3 measurements have uncovered both emission and absorption toward elevenstarburst galaxies. In

addition to providing kinetic temperature information necessary for our H2CO density measurements, we havefound two rather surprising results: NH3 absorptiontoward several galaxies and the discovery of absorption in thenon-metastable NH3 (2,1) transition toward NGC 660. Non-metastable transitions of NH3 are sensitive to infraredradiation fields, requiring high infrared intensities.

These measurements allow us to derive the kinetic temperature, spatial density, and dense gas mass in ourstarburst galaxy sample. The correlation between infrared luminosity (LIR) and dense gas properties is well-established, though the techniques generally employed to study this correlation use a simplistic approach to themolecular excitation. Our technique of using H2CO and NH3 to derive the physical conditions in starburst galaxiesaffords a more exact comparison between the infrared emission and dense gas properties in starburst environments.

Figure 1: Left-to-Right: H2CO 110 − 111 (top) and211 − 212 (bottom) spectra from Arp 220 and NGC 253, andNH3 (1,1), (2,2), (4,4), and (2,1) (top-to-bottom) spectra from IC 342 and NGC 660.

References:Mangum, J. G., Darling, J., Menten, K. M., & Henkel, C. 2008, ApJ, 673, 832

The Peculiar Star Formation Environment of the Galactic Center

MARK R. MORRIS

Department of Physics and Astronomy, University of California, Los Angeles, CA 90095-1547, USAmorris@astro.ucla.edu

Recent surveys have shown that young, massive stars are presentthroughout the central molecular zone (CMZ)of our Galaxy. The most prominent manifestation of this is the presence of several compact, massive star clusters(CMSCs), but the population of isolated massive stars appears to be comparable in number to that of massivestars in the CMSCs. An important fraction of the isolated massive stars is likely tobe escapees from the rapidlyevaporating CMSCs, so while there is evidence that some massive stars have formed in relative isolation, thedominant mode of star formation near the Galactic center appears to be the formation of CMSCs. This is likelyattributable to the peculiar physical properties of the clouds in the CMZ: compared to clouds in the Galactic disk,CMZ clouds have relatively high densities, high temperatures, large internal velocity dispersions, and probablystrong magnetic fields. The cloud dynamics and stability are also affected by the strong tidal field of the Galacticcenter. Implications of these conditions for the initial mass function will be discussed and compared with ob-servational results on the present-day mass function in two CMSCs. An extreme case of tidal influence occurswithin the gravitational sphere of influence of the Galactic black hole. Many of the young stars of the CMSC inthe central parsec are distributed in a well-defined disk, the most satisfactory explanation for which is anin situformation event in a long-since-dissipated massive accretion disk. While early assessments of this hypothesis werepessimistic, theoretical models of this dramatic event – still in early stages of elaboration – have shown promisingresults. The star formation environment of the center of our Galaxy, both inthe central parsec and beyond, hasmanifold commonalities with most disk galaxies, so its proximity provides an extremely convenient opportunityto assemble a detailed panorama of star formation processes in galactic nuclei,and their interaction with all otherforms of nuclear activity.

Large molecular loops in the Galactic center; Evidence for Parker instability

Y. FUKUI1

1 Department of Astrophysics, Nagoya University, Furocho, Chikusaku, Nagoya 464-8602, Japan,fukui@a.phys.nagoya-u.ac.jp

Fukui et al. (2006) discovered two huge molecular loops of several 100pc in length in the Galactic center andinterpreted that they were created by magnetic flotation by Parker instability. Ipresent new large scale moleculardistributions over kpc obtained at mm/sub-mm multi-J CO transitions (Torii et al. 2010, Kudo et al. 2010) andshow the loops have high temperatures up to more than 100K even at 1kpc from the center. The high temperaturesuggests that the gas is most likely heated up by shocks but not by radiationof high mass stars. I argue that theParker instability offers a natural explanation on the high temperature in termsof shock heating by violent motionsof around 30 km/s. I present details of the distribution of the foot points of the loops, the accumulated gas in theedges of the loops. These foot points are candidates for future massive cluster formation. The Parker instabilitymay be working in the CMZ as well that exhibits high-z loop-like features as recently unveiled in CO. In the endof the talk, I discuss some future prospects including search for similar loops in galaxies with ALMA.

Star formation at high redshift: Where are the Baryons?

M.BREMER1, E. STANWAY 1, M. LEHNERT2, L. DAVIES1, A. OMONT3, N. TANVIR4, A L EVAN5

1Department of Physics, University of Bristol, H.H. Wills Physics Laboratory, Tyndall Avenue, Bristol, BS8 1TL,UK

2Laboratoire d’Etudes des Galaxies, Etoiles, Physique et Instrumentation GEPI, Observatoire de Paris, Meudon,9219 5 France

3 IAP, Boulevard Arago, Paris, 92160.4 University of Leicester.5 University of Warwick.

We discuss the results of cm/mm/submm searches for redshifted CO emission anddust continuum emission fromobjects in the fields of high redshift (z > 5) Lyman break galaxies and gamma ray bursts, the sites of some of themost vigorous star formation events at the highest redshifts. These objects are identified through their rest-frameUV emission, so while it is clear that they mark out strong starbursts, we currently have little idea how much ofthe star formation in these objects is in a currently hidden or obscured UV-dark phase. By targetting these objectsat these wavelengths we aim to identify emission from otherwise obscured star forming regions. The LBG fieldswere chosen specifically because the LBGs showed a high degree of 3-dimensional clustering, indicating thatthey mark out peaks in the high redshift density field. This has two particularbenefits: (a) multiple LBGs can betargeted simultaneously and (b) the LBGs trace regions which will likely form the cores of clusters atz ∼ 0, and soshould contain many more galaxies and baryons at the same redshift as the LBGs distributed throughout the field.The targeted GRB is the most distant spectroscopically-confirmed source (z=8.2). Using standard assumptionsincluding the conversion between CO and H2 mass, we estimate the cold gas content of both the primary targetsand objects sharing the same large-scale structure. We discuss how the measurements constrain the timescale of thestarburst phase and the nature of the galaxies themselves. By comparing the results from our line and continuumobservations, we can determine the nature of the starbursts; whether theyare similar to those seen in ULIRGS orhave more in common with the events seen in galaxies like the Milky way.

Session III:SF in disk galaxies: morphology, structure, and dynamics

Star Formation in Disk Galaxies Today

R.C. KENNICUTT1

1 Institute of Astronomy, University of Cambridge,robk@ast.cam.ac.uk

Our understanding of star formation in galaxies is being transformed by a new wave of multi-wavelengthobservations in the UV, visible, infrared, and radio. These observations have helped to refine the measurementsof star formation rates in galaxies near and far, and they have revealed aset of fundamental scaling laws whichoffer tantalizing clues to the underlying physics of star formation on Galactic scales. At the same time they raisefundamental questions about some of the long-cherished assumptions about the nature and physics of the starformation, including the nature and universality of the Schmidt law and the stellar initial mass function. This talkwill summarize the most important accomplishments and insights gained over the past few years, with emphasison key questions being addressed by the Herschel Space Observatory.

Dwarf Galaxies as Keystones to Galaxy Evolution: effects of metallicity on ISM properties

SUZANNE C. MADDEN1, MAUD GALAMETZ 1, FREDERIC GALLIANO 1, DIANE CORMIER1, SACHA HONY1,V IANNEY LEBOUTEILLER1, ALESSANDROCONTURSI2, ALBRECHT POGLITSCH2 AND THE SAG 2 AND

SHINING CONSORTIA

1 Service d’Astrophysique, AIM, IRFU, CEA, Saclay,suzanne.madden@cea.fr,maud.galametz@cea.fr, frederic.galliano@cea.fr,diane.cormier@cea.fr, sacha.hony@cea.fr, vianney.lebouteiller@cea.fr

2 Max-Planck-Institut fuer Extraterrestrische Astrophisik,contursi@mpe.mpg.de, alpog@mpe.mpg.de

Local universe dwarf galaxies provide a rich variety of conditions to study star formation and is feedback onthe interstellar medium in conditions that may be representative of early universe environments. We approach thestudy of galaxy evolution by investigating the physical properties of dwarfgalaxies of widely varying metallicityvalues, over wide ranges of size scales and from the multi-wavelength point of view with the goal of understandinghow metallicity impacts the evolution of the gas and dust and thus the star formation properties in galaxies. Wehave been carrying out dwarf galaxy surveys with Spitzer as well as withground-based submillimetre telescopesand are currently targeting a large sample of dwarf galaxies with key programs using the Herschel PACS andSPIRE instruments. Their low mass, prominent star formation activity, and metal-poor ISM have a striking impacton the physical processes that take place to shape the structure of the ISM. The nature of the molecular clouds,photodissociation regions and ionised phases of dwarf galaxies is very different from those of their more metalrich counterparts. For example, while molecular gas is considered to be an essential ingredient for star formation,detecting CO, the standard tool to probe the molecular hydrogen reservoirin galaxies, has always been a challengein low metallicity dwarf galaxies. Surveys of CO in dwarf galaxies have shownthat CO is an unrelable tracer ofmolecular gas in dwarf galaxies. Initial FIR fine structure surveys of the 158 mu [CII] line dwarf galaxies show aremarkably high [CII]/CO ratio compared to the dustier starburst galaxies,suggesting a very clumpy environmentand the presence of a substantial reservoir of molecular gas which is nottraced by CO, but which is residingin the photodissociated envelopes. With Herschel we are expanding the surveys of the FIR fine structure lines.Additionally, the dust reservoirs of dwarf galaxies are certainly not negligible, as originally perceived, given theirrelatively low metal abundance. Modelling of the MIR to submm dust SpectralEnergy Distribution (SED) oflow metallicity galaxies also shows notable differences compared to their more metal-rich counterparts and apotentially large dust mass if the submm excess often seen in dwarf galaxies,is due to cold dust. In this talk wewill summarise the gas and dust properties of low metallicity dwarf galaxies as well as the dust-to-gas mass ratiosas a function of metallicity and the consequences on the chemical evolution of galaxies.

The Fine–Scale Structure of the neutral ISM in nearby Galaxies

I. BAGETAKOS1, E. BRINKS1, F. WALTER2, W.J.G.DE BLOK3, A. USERO4, A.K. L EROY5, J.W. RICH6 AND

R.C. KENNICUTT, JR.7

1 University of Hertfordshire,i.bagetakos@herts.ac.uk, e.brinks@herts.ac.uk2 Max–Planck–Institut fur Astronomie,walter@mpia-hd.mpg.de

3 University of Cape Town,edeblok@ast.uct.ac.za4 Observatorio Astronomico Nacional,a.usero@oan.es

5 National Radio Astronomy Observatory,aleroy@nrao.edu6 Mount Stromlo Observatory,joshua@mso.anu.edu.au

7 University of Cambridge,robk@ast.cam.ac.uk

We present an analysis of the properties of HI holes detected in 20 galaxies that are part of “The HI Nearby GalaxySurvey” (THINGS; Walter et al. 2008). We detected more than 1000 holesin total in the sampled galaxies. Wherethey can be measured, their sizes range from about 100 pc (our resolution limit) to about 2 kpc, their expansionvelocities range from 4 to 36km s−1, and their ages are estimated to range between 3 and 150 Myr. The holes arefound throughout the disks of the galaxies, out to the edge of the HI disk; 23% of the holes fall outsideR25. Wefind that shear limits the age of holes in spirals (shear is less important in dwarfgalaxies) which explains why HIholes in dwarfs are rounder, on average than in spirals. Shear, whichis particularly strong in the inner part of spiralgalaxies, also explains why we find that holes outsideR25 are larger and older. We derive the scale height of theH I disk as a function of galactocentric radius and find that the disk flares up inall galaxies. We proceed to derivethe surface and volume porosity (Q2D andQ3D) and find that this correlates with the type of the host galaxy: laterHubble types tend to be more porous. The size distribution of the holes in our sample follows a power law witha slope ofaν ∼ −2.9. Assuming that the holes are the result of massive star formation, we derive values for thesupernova rate (SNR) and star formation rate (SFR) which scales with the SFR derived based on other tracers. Ifwe extrapolate the observed number of holes to include those that fall belowour resolution limit, down to holescreated by a single supernova, we find that our results are compatible with the hypothesis that HI holes result fromstar formation. We present the first results from a comparison of the HI holes with Spitzer 8µm and 24µm, GalexNUV maps, and the CO(2–1) data provided by the SINGS (Kennicutt et al. 2003), NGS (Gil de Paz et al. 2007)and HERACLES (Leroy et al. 2009) surveys respectively.References:Bagetakos, I., Brinks, E., Walter, F., de Blok, W. J. G., Usero, A., Leroy, A., Rich, J. W.,& Kennicutt, R. C., Jr., 2010, AJ, submittedGil de Paz, A., et al. 2007, ApJS, 173, 185Kennicutt, R. C., Jr., et al. 2003, PASP, 115, 928Leroy, A., et al. 2009, AJ, 137, 4670Walter, F., Brinks, E., de Blok, E., Bigiel, F., Kennicutt, R. C., Jr., Thornley,M. D., &Leroy, A. 2008, AJ, 136, 2563

HERACLES and the Spatially Resolved Star Formation Law

ELIAS BRINKS1, ADAM LEROY2, FRANK BIGIEL3, FABIAN WALTER4, AND ANDREAS SCHRUBA4

1 Centre for Astrophysics Research, University of Hertfordshire, Hatfield AL10 9AB, UK,E.Brinks@herts.ac.uk

2 National Radio Astronomy Observatory, Charlottesville, VA 22903, USA,aleroy@nrao.edu3 Radio Astronomy Laboratory, University of California, Berkeley, CA 94720, USA,

bigiel@astro.berkeley.edu4 Max–Planck–Institut fur Astronomie, Konigstuhl 17, 69117 Heidelberg, Germany,walter@mpia.de,

schruba@mpia-hd.mpg.de

We present results on the phase change from an atomic to molecular ISM based on the HERACLES survey.HERACLES is a∼ 500 hr and IRAM Large Program that made wide (∼ r25), sensitive (∼ 2 M⊙ pc−2 of H2)maps of the12CO(2–1) transition in 47 galaxies, ranging from dwarf irregulars to massive spirals. The targetsheavily overlap the THINGS and SINGS surveys. Using these ancillary data, we produce spatially resolved mapsof the star formation rate density (SFRD), neutral atomic (HI), and molecular (H2) gas surface density. We find thatthe phase change from HI to H2 occurs in a systematic way and plays a key role in understanding star formationin galaxies. HI saturates at a surface density of∼ 10–20 M⊙ pc−2, above which gas is predominantly molecular.In this molecular regime, at gas surface densities of 20–200 M⊙ pc−2, star formation proceeds at a fixed depletiontime scale of∼ 2.5 Gyr, independent of radius, stellar or gas surface density, or hydrostatic pressure. Below∼ 20 M⊙ pc−2 (i.e., over most of the area in galaxies), the SFRD is largely set by the ISM’sability to convertHI to H2. This conversion, traced by the H2–to–HI ratio is a clear function of environment. We observe strongcorrelations between the H2–to–HI ratio and the local dust-to-gas ratio (the first such measurement) as well aswithhydrostatic pressure, radius, and stellar surface density.

Figure: Star formation and gas surface densities from inner to outer disks (left: spirals, right: dwarf galaxies).Filled contours show the pixel–by–pixel distribution ofΣSFR as a function of gas insider25 (filled contours) fora subset of our sample (Bigiel et al. 2008, AJ, 136, 2846). Empty contours show outer disk data (Bigiel et al.submitted) with black points indicating median and scatter.

The HerschelM33 extended survey (HERM33ES)

C. KRAMER1, J. BRAINE2, D. CALZETTI3, S. LORD4, G. STACEY5, AND THE HERM33ESTEAM

1 Instituto Radioastronomıa Milimetrica (IRAM), Av. Divina Pastora 7, E-18012 Granada, Spain,kramer@iram.es

2 Observatoire de Bordeaux, CNRS/INSU, B.P. 89, Floirac F-33270,Jonathan.Braine@obs.u-bordeaux1.fr

3 Department of Astronomy, University of Massachusetts, Amherst, MA 01003, USA ,calzetti@astro.umass.edu

4 IPAC, MS 100-22 California Institute of Technology, Pasadena, CA 91125, USA,lord@ipac.caltech.edu

5 Department of Astronomy, Cornell University, Ithaca, NY 14853, USA,stacey@astro.cornell.edu

Messier 33 is a small Local Group spiral galaxy with a subsolar metallicity, bluecolors, and is gas-rich – propertieswhich are common to early universe objects. In the framework of the open timekey projectHERM33ES, we useall three instruments onboardHerschelto study the dusty and gaseous ISM of M33. The goal is to understand thecycle of star formation from the atomic gas to the denser molecular phase and finally into stars in a low metallicityenvironment, exploiting the unique linear scales accessible in this nearby galaxy. One focus ofHERM33ES is onmaps of the FIR continuum observed with PACS and SPIRE, covering the entire galaxy. A second focus lies onobserving diagnostic FIR and submillimeter cooling lines [CII], [OI], [NII], [NIII], and H2O, toward a2′ × 40′

strip along the major axis with PACS and HIFI.Here, we present spectral energy distributions of the FIR emission obtained between 24 and 500µm wave-

lengths, together with dust emission models (Kramer et al. 2010, Xilouris et al.2010). A two component model,with β fixed at 1.5, best fits global and radially averaged SEDs. The cold dustcomponent clearly dominates themass. The temperature of the cold component drops from∼ 24 K in the inner 2 kpc radius to 13 K beyond 6 kpcradial distance. The gas-to-dust ratio, averaged over the galaxy, is higher than the solar value by a factor of 1.5 andis roughly in agreement with the subsolar metallicity of M33.

We select individual star forming regions and estimate their star formation rates (SFR) from the emission inHα and at24 µm, comparing those with the emission at PACS 100, 160µm (Boquien et al. 2010) and SPIRE250µm (Verley et al. 2010) wavelengths. We find the behaviour of individualstar forming regions surprisinglysimilar to that of entire galaxies. Taking advantage of the unprecedented Herschel resolution at these wavelengths,we also focus on a more precise study of some striking Hα shells in the northern part of the galaxy. The mor-phological study of the H shells shows a displacement between far-ultraviolet, Hα, and the SPIRE bands. Thecool dust emission from SPIRE clearly delineates the Hα shell structures. The different locations of the Hα andfar-ultraviolet emissions with respect to the SPIRE cool dust emission leadsto a dynamical age of a few Myr forthe Hα shells and the associated cool dust.

We combine the SPIRE data with new high-quality CO and HI data (Braine et al. 2010, Gratier et al 2010). Thesensitive FIR continuum observations allow us to independently measure thegas mass of M33, checking whetherCO can be used to trace H2 and whether the Star Formation Efficiency (defined here as the star formation rateper H2 mass) is indeed higher in subsolar metallicity galaxies. We measure the dust cross-section using the FIRcontinuum and the CO, HI data, and find a radial gradient from a near-solar neighborhood cross-section to abouthalf-solar. Calculating the total H column density from the measured dust temperature and cross-section, and thensubtracting the HI column, yields a morphology similar to that observed in CO. The H2/HI mass ratio decreasesfrom about unity to well below 10% and is about 15% over the optical disk. The planned observations of [CII] andother FIR lines, will allow to more precisely estimate the amount of molecular gas not seen in CO.

Spiral structure and star formation

C. L. DOBBS1,2

1 Max-Planck-Institut fur extraterrestrische Physik, Giessenbachstraße, D-85748 Garching, Germany,cdobbs@mpe.mpg.de

2 Universitats-Sternwarte Munchen, Scheinerstraße 1, D-81679, Germany

The dynamics of stars and gas appear markedly different in flocculent, tidally induced and quasi-stationary spiralgalaxies. I will present results from numerical simulations of spiral galaxies, and consider the relation between thegas dynamics and star formation. In flocculent galaxies, stars and gas appear coincident, their locations determinedby gravitational instabilities. Consequently there is little offset expected between star forming regions and the olderstellar population, and individual spiral arms are expected to contain star clusters of similar ages. With a steadyspiral potential, as predicted by Lin-Shu density wave theory, the gas accumulates into GMCs along the spiralarms. We estimate the distribution of stellar clusters from the location of dense gas, and find, as expected, a trendin the ages of stellar clusters with azimuthal distance from the arm. I will then illustrate an example of a tidallyinduced spiral using a simulation designed to model the grand design galaxy M51. In this case, the situation ismore complex due to the double interaction of M51 with NGC 5195. The spiral structure is very time dependent,and shows kinks and branches absent in the case of a steady state potential. We find that clusters of a given ageare distributed much more randomly than for a fixed potential. The lack of cleartrends in observations of spiralgalaxies may suggest that spiral structure is typically due to localised gravitational instabilities or tidal interactions.

HERschelInventory of The Agents of Galaxy Evolution (HERITAGE) in the Magellanic Clouds:ISM, Star formation and Stellar Feedback

M. M EIXNER1 AND THE HERITAGE TEAM

1 Space Telescope Science Institute,meixner@stsci.edu

The Large Magellanic Cloud (LMC) and the Small Magellanic Cloud (SMC) arethe best astrophysical laborato-ries to study the lifecycle of the interstellar medium (ISM), because their proximity (50 kpc, 61 kpc, respectively)permits detailed studies of resolved ISM clouds and their relation to stellar populations on global scales, in an un-ambiguous manner, and as a controlled function of environment. Their sub-solar metallicities (ZLMC ≃ 0.5×Z⊙,ZSMC ≃ 0.2×Z⊙) permit investigations on how processes governing galaxy evolution depend on metallicity. TheHerschelObservatory open-time key program, entitledHERschelInventory of The Agents of Galaxy Evolution(HERITAGE) in the Magellanic Clouds, is performing a uniform survey of the LMC (8◦ × 8◦), SMC (5◦ × 5◦),and the Magellanic Bridge (4◦×3◦) with the Spectral and Photometric Imaging Receiver (SPIRE) at 250, 350, and500µm and with the Photodetector Array Camera and Spectrometer (PACS) at 100and 160µm. The HERITAGEscience goals are to study the life cycle of matter in the Magellanic Clouds by probing the dust emission from theISM and stars, which are the agents of galaxy evolution.HerschelSPIRE and PACS images provide key insightsinto the life cycle of galaxies because the far-infrared and submillimeter emission from dust grains is an effectivetracer of the ISM dust, the most deeply embedded young stellar objects (YSOs), and the dust ejected by evolvedmassive stars and supernovae. In this talk, I will provide an overview ofthe initial results from HERITAGE on theISM in the LMC and SMC, in particular the dust composition, the discovery of Stage 0/I YSOs in the MCs, thedust mass-loss rates of massive evolved stars and the dust mass associated with supernova remnants (SNRs).

Anomalous Dust in Late-Type Galaxies

F.P. ISRAEL1

1 Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 Leiden, Netherlands,israel@strw.leidenuniv.nl

Almost all galaxies lack accurate flux density measurements in the millimeter and submillimeter range, which iscrucial for the determination of global free-free emission, a prime star formation indicator, and the amount of colddust, which may dominate the total dust mass of a galaxy and its gas-to-dust ratio. We have studied the few dozenlate-type galaxies with well-established submillimeter SEDs, and in particular the small susbset of galaxies with awell-determined millimeter continuum SED. We have discovered a significant millimeterand submillimeter excessin the Magellanic Clouds, which may also occur in other dwarf galaxies, but isabsent (ultra)luminous infratredgalaxies and more modest starburst galaxies. Emissivities areβ = 1.0-1.7, and do not reach the commonly assumedβ=2. The excess emission is not due to cold dust, but must represent an anomalous emission process. Dist emissionmechanisms at long wavelengths are briefly discussed. There is no good evidence for cold dust in the galaxiesstudied.

NRO legacy project: M33 all disk survey of Giant Molecular Clouds (GMCs) with NRO-45m andASTE-10m telescopes

T.TOSAKI1, N.KUNO2, S.ONODERA2, R. MIURA3, K. MURAOKA4, T. SAWADA 5, S.KOMUGI6, K.NAKANISHI 5., K.KOHNO3 , R.KAWABE2, N.ARIMOTO5

1 Joetsu University of Education,tosaki@juen.ac.jp2 Nobeyama Radio Observatory,3 University of Tokyo,4 Osaka Prefecture University,5 National Astronomical

Observatory of Japan,6 JAXA

We have conducted a large scale 12CO(J=1-0) imaging survey of the central 30′ × 30′ region of M33 usingNobeyama Radio Observatory (NRO) 45 m telescope, and partial mappingsof it in 13CO(J=1-0) using NRO 45mtelescope and 12CO(J=3-2) using ASTE telescope are also in progress. 12CO(J=1-0) observations were usedthe 25-Beam Array Receiver System (BEARS) and performed with On-the-Fly observation mode. The spatialresolution of the final map is19′′.3, corresponding to 80 pc at the distance of M33.

Our preliminary results are summarized as follows: (1) We found an overallcoincidence between CO (molec-ular gas) and HI (atomic gas). However we also found a different tendency between outer and inner regions ofM33; i.e., most of CO clouds are associated with local HI peaks in outer regions, while no such a clear corre-spondence can be found in the inner regions. (2) We found the variety of star forming activity among detectedmolecular clouds. We suggest that the observed variety of molecular clouds can be understood as a sequence alongan evolutionary path of massive star formation, from quiescent diffuse molecular clouds to stellar clusters wherenatal molecular clouds are already dispersed. (3) We compared surface densities of molecular gas (Σgas) and starformation rate (ΣSFR). We found no significant correlation between them in∼ 80 pc scale, although we foundΣSFR ∝ Σ1.1±0.1

gas when the map was smoothed to 1 kpc (240′′) resolution. We suggest that Kennicutt-Schimidtlaw breaks at a GMC scale. (4) We found a correlation between molecular gas mass and CO(3-2)/CO(1-0) ratio,i.e., more massive molecular clouds tend to exhibit higher CO(3-2)/CO(1-0) ratio.

We have also obtained a wide and deep 1.1 mm continuum map, observed by AzTEC camera on ASTE,showing a global gradient of the dust temperature from the center to the outer part of M33. Wide field multi-coloroptical images using SuprimeCam/SUBARU are also yielding spatially resolved age information of individualstars. These unique stellar data, combined with the tracers of massive star formation (i.e., Hα and Spitzer MIPSdata), will also be used as a clock of GMCs.

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Figure: Total integrated intensity map of CO(1-0) (contour) superposedon HI (left) and Spitzer 24µm (right).

References:Tosaki T. et al. . 2007, ApJ, 664, L27Onodera, S. 2009, PhD thesis, University of Tokyo

ATLASGAL, the APEX Telescope Large Area Survey of the Galaxy

F. WYROWSKI1 & AND THE ATLASGAL TEAM

1 Max-Planck-Institut fur Radioastronomie,wyrowski@mpifr-bonn.mpg.de

Submillimeter dust continuum emission traces high molecular column densities and, thus, dense cloud regionsin which new stars are forming. Surveys of the Galactic plane in such emissionhave the potential of delivering anunbiased view of high-mass star formation throughout the Milky Way. The location of the APEX telescope on theChajnantor plateau in Chile is ideally suited for mapping the inner Galaxy. ATLASGAL, The APEX TelescopeLarge Area Survey of the Galaxy at 870µm, is a survey of the Galactic plane using the Large APEX BolometerCamera (LABOCA), in the Galactic longitude and lattitude ranges of±60 and±1.5 ◦ , respectively. This surveyis providing an unbiased sample of cold dusty clumps in the Galaxy at submillimeter wavelength and a variety ofmolecular line follow-up observations have been started to characterize thephysical and chemical conditions inthe newly found clumps. Here, first results from this survey and its follow-up programs will be described.

HOPS - The H2O southern Galactic Plane Survey

A. WALSH1

1 James Cook University,andrew.walsh@jcu.edu.au

Over the past three years, we have used the Mopra radiotelescope, located in NSW, Australia, to survey 100square degrees of the Galactic Plane. The observations have focussed on emission lines in the frequency range19.5-27.5 GHz, with the most important lines being the water maser line, ammonia (1,1), (2,2), (3,3) inversiontransitions, HCCCN (3-2) and radio recombination lines. I will report on results from the Mopra observing cam-paign, where we have detected over 500 water masers, most of which arenew detections, widespread ammoniaemission, as well as a few unusual emission lines.

Session IV:Star formation: physical & chemical conditions/feedback

Radiative Feedback

NORMAN MURRAY1

1 University of Toronto,murray@cita.utoronto.ca

Outflows and Jets from young stars and their feedback

SYLVIE CABRIT1

1 Observatoire de paris,sylvie.cabrit@obspm.fr

PDRs and XDRs

M.G. WOLFIRE1

1 University of Maryland, Astronomy Department,mwolfire@astro.umd.edu

Photodissociation regions (PDRs) are gas phases in in which far-ultraviolet (6eV < hν < 13.6 eV; FUV)radiation plays a significant role in the heating and/or chemistry (Tielens & Hollenbach 1985). For example, PDRsare found in reflection nebulae and molecular cloud surfaces in which the radiation from nearby OB stars illuminatethe clouds. The incident starlight is absorbed by dust and polycyclic aromatic hydrocarbons (PAHs) and is mostlyused to excite the PAHs and heat the grains. However, a fraction (∼ 0.1 − 1%) of the absorbed FUV starlightmay be converted to energetic photoelectrons that are ejected from PAHs and grains, which subsequently heat thegas. The strong UV radiation acts as a beacon to illuminate the cloud structure,and to ionize and excite ions andmolecules which are rarely seen in emission. Thus, PDRs emit strong far-infrared grain continuum emission aswell as infrared, submillimeter, and millimeter wave line emission arising from the warm gas. The FUV radiationcan affect the chemistry in molecular clouds to a depth ofAV ∼ 5 by maintaining oxygen that is not tied up inCO in atomic form, a depth comparable to the mean column density in giant molecular clouds (Solomon et al.1987). The same PDR physics that is at work at the surfaces of molecularclouds also acts in the diffuse interstellarmedium (Wolfire et al. 2003) and thus much of the ISM is in PDRs.

X-ray dissociation regions (XDRs) are regions in which X-rays dominate the heating and/or chemistry (Moloneyet al. 1996). Hard X-rays (E > 1 keV) can penetrate large columns (N > 1022 cm−2) before being absorbed andproduce large columns of warm atomic and molecular gas. This is in contrast toPDRs where an optical depth ofone is reached atN ∼ 1021 cm−2 for FUV photons. Strong XDRs can be found for example, in AGN (Meijerinket al. 2007), protoplanetary disks (Meijerink et al. 2008) or planetary nebula with hot central sources (Natta &Hollenbach 1998). Weak XDRs can also be found in the diffuse ISM in warm (T ∼ 8000K) neutral gas (Wolfireet al. 1995), where soft-Xray (hν < 100 eV) emission is important in regulating the grain photoelectric heatingrate. Soft X-rays are also important in setting the two-phase thermal pressure in molecular cloud surfaces (Wolfireet al. 2010).

Much progress has been mode in modeling PDRs (e.g., Rollig et al. 2007) and XDRs (e.g., Meijerink etal. 2007) and the models predict several line intensities and line ratios of atomicand molecular species that aregood diagnostics for descriminating between the two. For example, the ([OI]63 µm + [CII] 158 µm)/IR ratio ispredicted to be∼ 0.1 for XDRs but< 0.03 for PDRs (Moloney et al. 1996). XDRs also produce strong [CI](Meijerink et al. 2006),OH+ andH2O

+ line emission (van der Wert at al. 2010), and high-J CO line intensities(Spaans & Meijerink 2008). Herschel observations have demonstratedthe ability to detect and separate PDR andXDR emission components in galaxies (van der Werf et al. 2010). I will discuss the theoretical models in light ofthe most recent observations.References:Meijerink, R., Glassgold, A. E., & Najita J. R. 2008, ApJ, 676, 518Meijerink, R., Spaans, M., & Israel, F. F. 2006, ApJ, 650, 103Meijerink, R., Spaans, M., & Israel, F. P., 2007 A&A, 461, 793Moloney, P. R., Hollenbach, D. J., & Tielens, A. G. G. M. 1996, ApJ, 466, 561Natta, N. & Hollenbach D. 1998, A&A, 337, 517Rollig et al. 2007, A&A, 467, 187Spaans, M., & Meijerink, R. 2008, 678, L5Solomon et al. 1987, ApJ, 319, 730Tielens, A. G. G. M., & Hollenbach D. J. 1995, ApJ, 291, 722van der Werf, P. P. et al. 2010, A&A, 518, 42Wolfire, M.G., McKee, C. F., Hollenbach, D. & Tielens A.G. G. M. 2003, ApJ, 587, 278Wolfire, M.G., Hollenbach D. J., & McKee, C. F. 2010, 716, 1191

Understanding the physics of the X-factor

S. C. O. GLOVER1 AND M. M AC LOW2

1 Zentrum fur Astronomie der Universitat Heidelberg, Institut fur Theoretische Astrophysik,Albert-Ueberle-Strasse 2, 69120 Heidelberg, Germany,sglover@ita.uni-heidelberg.de

2 Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, NewYork, NY 10024, USA,mordecai@amnh.org

CO is often used as a tracer of molecular gas. However, its reliability has longbeen questioned in environmentsdifferent from the Milky Way. We have studied the relationship between H2 and CO abundances in numericalmodels of giant molecular clouds (GMCs) using three-dimensional simulations of MHD turbulence coupled to asimplified chemical network, and examining models with a range of different metallicities and densities. In thiscontribution, I show that the abundance of H2 is primarily determined by the time available for its formation, and isinsensitive to photodissociation in all but the lowest column density clouds. Onthe other hand, CO forms quickly,but is highly sensitive to photodissociation, with only a weak dependence onH2 abundance. As a result, there isa sharp cutoff in CO abundance at mean visual extinctionsAV < 3. At lower AV, the X-factor – the ratio of H2column density to the CO emissivity – scales asXCO ∝ A−3.5

V . However, clouds in this regime are faint in CO andwill be difficult to detect in CO-based surveys. This therefore providesa simple explanation for the discrepancyobserved in low metallicity systems between cloud masses derived from CO observations, which primarily samplethe highAV end of the cloud distribution, and masses derived from other observational techniques that sample thewhole distribution.

Figure 1: Estimate of the CO-to-H2conversion factorXCO,est, plotted asa function of the mean visual extinc-tion of the gas,〈AV〉. At 〈AV〉 > 3,we find values forXCO,est, that areconsistent with the value ofXCO =2×1020cm−2 K−1 km−1 s determinedobservationally for the Milky Way byDame et al. (2001), indicated in theplot by the horizontal dashed line. At〈AV〉 < 3, we find evidence fora strong dependence ofXCO,est on〈AV〉. An empirical fit, withXCO,est

constant above〈AV〉 = 3 and scalingasXCO,est ∝ A−3.5

V below 〈AV〉 = 3is indicated by the dotted line.

References:Dame, T. M., Hartmann, D., & Thaddeus, P. 2001, ApJ, 547, 792Glover, S. C. O., Federrath, C., Mac Low, M. M., & Klessen, R. S. 2010,MNRAS, 404, 2Glover, S. C. O., Mac Low, M.-M. 2010, MNRAS, submitted; arXiv:1003.1340

The CO-H2 conversion factor of diffuse ISM:Does the12CO emission trace dense molecular gas?

J. PETY1, H. S. LISZT2, AND R. LUCAS3

1 IRAM, pety@iram.fr2 NRAO,hliszt@nrao.edu3 ALMA, rlucas@alma.cl

Summarizing 20 years of efforts, we will quantify the CO luminosity and CO-H2 conversion factor applicableto diffuse but partially-molecular ISM whenH2 and CO are present but C+ is the dominant form of gas-phasecarbon. To do this, we will discuss galactic lines of sight observed inHI, HCO+ and CO where CO emissionis present but the intervening clouds are diffuse (locally AV ∼<1 mag) with relatively small CO column densitiesNCO ∼<2× 1016 cm−2. We will separate the atomic and molecular fractions statistically using EB−V as a gauge ofthe total gas column density and compareNH2

to the observed CO brightness.Although there areH2-bearing regions where CO emission is too faint to be detected, we will show that the

mean ratio of integrated CO brightness toNH2for diffuse ISM does not differ from the usual value of 1K km s−1

of integrated CO brightness per2× 1020 H2 cm−2 . Moreover, the luminosity of diffuse CO viewed perpendicularto the galactic plane is 2/3 that seen at the Solar galactic radius in surveys of CO emission near the galactic plane.

Commonality of the CO-H2 conversion factors in diffuse and dark clouds can be understood from considera-tions of radiative transfer and CO chemistry. There is unavoidable confusion between CO emission from diffuseand dark gas and misattribution of CO emission from diffuse to dark or giant molecular clouds. The character ofthe ISM is different from what has been believed if CO andH2 that have been attributed to molecular clouds onthe verge of star formation are actually in more tenuous, gravitationally-unbound diffuse gas.References:Liszt, H. S., Pety, J. and Lucas, R., “The CO luminosity and CO-H2 conversion factor ofdiffuse ISM: does CO emission trace dense molecular gas?”, submitted toA&A.

Chemical enrichment of the interstellar medium through themass loss of evolved stars

L. DECIN1,2, ON BEHALF OF THEMESSAND HIFISTARS HERSCHEL CONSORTIUM

1 Instituut voor Sterrenkunde, Celestijnenlaan 200D, 3001 Leuven (Heverlee), Belgium,Leen.Decin@ster.kuleuven.be

2 Sterrenkundig Instituut Anton Pannekoek, University of Amsterdam, Science Park 904, NL-1098 Amsterdam,The Netherlands

Mass loss is the dominating factor in the post-main sequence evolution of most stars but many aspects of themass loss mechanism(s) are still not understood. The Herschel Space Observatory offers the astronomers someunique instruments (HIFI, PACS and SPIRE) to study circumstellar environments around evolved stars (see Fig. 1).We present the latest results obtained in the framework of the MESS (Mass Loss in Evolved StarS) HerschelGuaranteed Time Key Project (GTKP, 330 hrs, PACS and SPIRE) and HIFISTARSGTKP (205 hrs, HIFI). Themain focus of this talk will be on the chemistry occuring in the envelope of evolved oxygen-rich, carbon-richand S-type Asymptotic Giant Branch (AGB) stars. Various chemical processes, as shock-induced non-thermalequilibrium chemistry, ion-ion process, photodissociation, determine the chemical fractional abundances in thecircumstellar environments around these evolved stars and hence the total chemical enrichment of the interstellarmedium. The ejected material merges with the interstellar matter and is later incorporated into new generations ofstars and planet.

Figure 1: The continuum-subtracted PACS spectrum (black) of the red supergiant VY CMa between 173 and188.5µm (see Royer et al. 2010). The main contributing molecules and isotopes areidentified. Features not yetidentified are indicated with a ’U’. The first modeling results are shown in different colors, corresponding to thedifferent molecular species.

References:Royer, P., Decin, L., R. Wesson et al., 2010, A&A, in press

Formation and evolution of molecular clouds in a turbulent and multi-phase ISM P. Hennebelle1,E. Audit 2, R. Klessen3, R. Banerjee4 and E. Vazquez-Semadeni5

1 Observatoire de Paris ,patrick.hennebelle@ens.fr2 CEA Saclay,edouard.audit@cea.fr

3 ITA, Heidelberg Universityrklessen@ita.uni-heidelberg.de4 ITA, Heidelberg Universitybanerjee@ita.uni-heidelberg.de

5 Morelia Universitye.vazquez@crya.unam.mx

It is now well established that the interstellar medium is turbulent, magnetized andstructured in various phases.Understanding its dynamics is a crucial issue in the context of star formation as molecular clouds form out of thediffuse interstellar gas. For this reason, a lot of efforts have been carried out by theorists during the last decades,to model the complex multiphase ISM.

In the talk, I will briefly describe the classical phase description (Wolfire et al. 1995) and the supersonicisothermal simulations which have been performed by various groups (e.g.Kritsuk et al. 2007). I will then stressthe need for a description which includes both aspects self-consistently and describe the various works which havebeen carried out along this line (e.g. Koyama & Inutsuka 2002, Audit & Hennebelle 2005, 2009, Heitsch et al.2005, Vazquez-Semadeni et al. 2006). Then, I will present the numerical simulations which have been performedto study self-consistently the formation of molecular clouds from the diffuse atomic interstellar gas (Vazquez-Semadeni et al. 2007, Hennebelle et al. 2008, Banerjee et al. 2009). Statistical comparisons with observationswill also be presented as well as a physical interpretations of various properties as the index of the clump massspectrum (Hennebelle & Chabrier 2008).References:Audit, E., Hennebelle, P., 2005, A&A, 433, 1,Audit, E., Hennebelle, P., 2010, A&A, 511, 76,Banerjee, R., Vazquez-Enrique, E., Hennebelle, P., Klessen, R., 2009, MNRAS, 398, 1082Heitsch, F., Burkert, A., Hartmann, L. et al., 2005, ApJ, 633, 113Hennebelle, P., Banerjee, R., Vazquez-Enrique, E., Klessen, R., Audit,E., 2008, A&A,486, L43Hennebelle, P., Chabrier, G., 2008, ApJ, 684, 395Koyama, H., Inutsuka, S.-i., 2002, ApJ, 564, L97Kritsuk, A., Norman, M., Padoan, P., Wagner, R., 2007, ApJ, 665, 417Vazquez-Semadeni, E., Ryu, D., Passot, T. et al. 2006, ApJ, 643, 245Vazquez-Semadeni, E., Gomez, G., Jappsen, A., et al. 2006, ApJ, 657,870Wolfire, M., Hollenbach, D., McKee, C., 1995, ApJ, 443, 152

The relation between gas and dust in the Taurus Molecular Cloud

JORGEL. PINEDA1, PAUL GOLDSMITH1, NICHOLAS CHAPMAN1, RON ALD L. SNELL2, DI L I1, LAURENT

CAMBRESY3, AND CHRIS BRUNT4

1Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA91109-8099, USAJorge.Pineda@jpl.nasa.gov

2Department of Astronomy, LGRT 619, University of Massachusetts, 710North Pleasant Street, Amherst, MA01003, USA

3Observatoire Astronomique de Strasbourg, 67000 Strasbourg, France4Astrophysics Group, School of Physics, University of Exeter, Stocker Road, Exeter, EX4 4QL, U

We report a study of the relation between dust and gas over a 100 deg2 area in the Taurus molecular cloud. Wecompare the H2 column density derived from dust extinction with the CO column density derived from the12COand 13CO survey by Goldsmith et al. 2008. We derive the visual extinction from reddening determined from2MASS data. The comparison is done at an angular size of 200”, corresponding to 0.14 pc at a distance of 140 pc.We find that the relation between visual extinctionAV andN(CO) is linear betweenAV ≃ 3 and 10 mag in theregion associated with the B213–L1495. In other regions the linear relationis flattened forAV > 4 mag. We findthat the presence of temperature gradients in the molecular gas affects the determination ofN(CO) by ∼30–70%with the largest difference occurring at large column densities. Adding a correction for this effect and accountingfor the observed relation between the column density of CO and CO2 ices andAV from Whittet et al. 2007, we finda linear relationship between the column of carbon monoxide and dust for observed visual extinctions up to themaximum value in our data≃ 23 mag. We have used these data to study a sample of dense cores in Taurus. Fittingan analytical column density profile to these cores we derive an average volume density of about1.4 × 104 cm−3

and a CO depletion age of about4.2 × 105 years. At visual extinctions smaller than∼3 mag, we find that the COfractional abundance is reduced by up to two orders of magnitude. The data show a large scatter suggesting a rangeof physical conditions of the gas. We estimate the H2 mass of Taurus to be about1.5 × 104 M⊙, independentlyderived from theAV andN(CO) maps. We derive a CO integrated intensity to H2 conversion factor of about2.1×1020 cm−2(K km s−1)−1, which applies even in the region where the [CO]/[H2] ratio is reduced by up to twoorders of magnitude. The distribution of column densities in our Taurus maps resembles a log–normal functionbut shows tails at large and low column densities. The length scale at which thehigh–column density tail starts tobe noticeable is about 0.4 pc.This research was conducted at the Jet Propulsion Laboratory, California Institute ofTechnology under contract with the National Aeronautics and Space Administration.

References:Goldsmith, P. F., Heyer, M., Narayanan, G., Snell, R., Li, D., & Brunt, C. 2008, ApJ, 680,428Whittet , D. C. B., Shenoy , S. S., Bergin , E. A., Chiar , J. E., Gerakines , P. A., Gibb ,E. L., Melnick , G. J., & Neufeld , D. A. 2007, ApJ, 655, 332

EPOS: A Herschel key programm on the earliest phases of star formation

O. KRAUSE, TH. HENNING, AND H. BEUTHER

Max-Planck-Institute fur Astronomiekrause@mpia.de

We are currently conducting a 100h Herschel key program to characterise low- to high-mass prestellar cores andprotostars. Our target sample consists of 60 objects which have been carefully selected on the basis of multi-wavelength preparatory studies. The earliest phases of star formation occur in the densest and coldest regionsof molecular clouds, i.e. dense cloud cores. Far-infrared observations at the peak of thermal dust emission inthese objects provide important constraints of their temperature and density structure. The unprecedented spatialresolution of Herschel’s 3.5m mirror in the far-infrared provides now a breakthrough opportunity to extend thecapabilities of Spitzer to constraint the spectral energy distributions of embedded protostellar objects towardslonger wavelengths and hence earlier evolutionary phases. The talk focuses on first results published in the A&Aspecial issue and further recent progress.

Spitzer, Herschel and PdB observations of two high-mass (12 and 18 M⊙) protostars in the cloud complex ISOSSJ18364-0221. While both sources have roughly the same brightness in themm-continumm and the southern one

is readily detected in deep Spitzer 24µm imaging, the northern only becomes visible in the Herschel-PACSimage at 70µm, indicating the very recent onset of star formation in the latter object.

References:[1] H. Beuther, Th. Henning, H. Linz, O. Krause, M. Nielbock, J. Steinacker it From high-mass starless cores to high-mass protostellar objects, A&A in press (arXiv:1005.1960)[2] A. Stutz, R. Launhardt, H. Linz, O. Krause, T. Henning, J. Kainulainen, M. Nielbock,J. Steinacker, P. Andre,Dust-temperature of an isolated star-forming cloud: Herschelobservations of the Bok globule CB244, A&A in press (arXiv:1005.1943)[3] T. Henning, H. Linz, O. Krause, S. Ragan, H. Beuther, R. Launhardt, M. Nielbock,T. VasyuninaThe seeds of star formation in the filamentary infrared-dark cloud G011.11-0.12, A&A in press (arXiv:1005.1939)[4] H. Linz, O. Krause, H. Beuther, Th. Henning, R. Klein, M. Nielbock, B. Steck-lum, J. Steinacker, A. StutzThe structured environments of embedded star-forming cores.PACS and SPIRE mapping of the enigmatic outflow source UYSO 1, A&A in press(arXiv:1005.1937)

Detection of Warm Dark Gas (H2) in Galactic Diffuse Clouds from Herschel’s GOT C+ Survey ofCII

W. D. LANGER, T. VELUSAMY, J. L. PINEDA , P. F. GOLDSMITH, D. LI , H. W. YORKE

Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099,USA William.D.Langer@jpl.nasa.gov

To understand the lifecycle of the interstellar gas and star formation we needinformation about the propertiesof diffuse atomic and molecular gas clouds and PDR layers. Until now our knowledge of interstellar gas hasbeen limited primarily to the diffuse atomic phase traced by HI and to the dense molecular H2 phase traced by CO.However, we are missing an important phase of the ISM called “dark gas” which is mostly H2 and little HI and CO,and is best traced with CII. Galactic Observations of Terahertz C+ (GOTC+) is a Herschel Space ObservatoryOpen Time Key Program to study the atomic and molecular diffuse interstellar medium by sampling [CII] 1.9THz (158µm) line emission throughout the Galactic disk, using HIFI. To date we detected 147 interstellar cloudsalong sixteen lines-of-sight towards the inner Galaxy in [CII]. We also acquired HI and CO isotope data along eachline-of-sight to analyze their physical conditions. Here we review theGOTC+ first results. We find that [CII]emission is stronger than expected for diffuse and transitional clouds, and in some sources is much stronger thananticipated given their HI and12CO column densities. The excess [CII] emission is best explained by the presenceof a significant warm H2, “dark gas” component. This first [CII] 158µm detection of warm “dark gas” shows thevalue of this tracer for mapping it throughout the Milky Way and other galaxies. In a sample of 51 transition cloudson average∼ 25% of the total H2 is in the “dark gas” not traced by CO. We also discuss the PDR conditions in asample of 58 dense CII clouds with13CO emission. This research was conducted at the Jet Propulsion Laboratory,California Institute of Technology under contract with the National Aeronautics and Space Administration.

Session V:Formation of stars: high M, low M, planetary systems

Massive Star Formation - Key Issues

H. ZINNECKER1

1 DSI,hzinnecker@aip.de

Key issues of massive star formation include the following:

1. is massive star formation basically a scaled-up version of low-mass starsformation, including pre-stellarcores,collapse, same binary properties, same disk accretion?

2. What is the sequence of events? infrared dark filaments, cold cores,hot cores, hypercompact, ultra-compact,and compact HII regions (timescales of the various phases). Where do the outflows and OH / H20 / CH30Hmasers fit in? What is the role of radiation pressure and stellar winds? effects of anisotropic vs. isotropicfeedback?

3. How does the disk gas ultimately fall onto the star’s surface: at the equator or at higher latitudes? or viasome funnel flow channeled by a stellar magnetosphere? What is the strength and role of magnetic fields inregions of massives star formation? mass-to-flux ratio?

4. Do massive protostars exist? are massive stars born on the main sequence (i.e. accretion onto a hydrogen ordeuterium burning object)? their size and temperature? small and hot or large and cool (like red supergiants)?What are the accretion rates, how variable are they? what kind of accretion process in nature: competitive,cooperative, hierarchical, or collisional accretion?

5. How do the tight massive binaries (orbital period of a few days) originate? orbit shrinking during accretion?fragmentation/fission of a rapidly rotating protostar? How do such energeticbinaries affect the dynamicsof dense star clusters? Can massive binaries merge? Could such a mergerbe a progenitor for a gamma-rayburst?

6. Is there a physical upper stellar mass limit? if so, due to birth processes orstellar stability? or is statisticsat work (random sampling of the IMF, dependence of the max. stellar mass on cluster mass)? Is there auniversal upper IMF (Salpeter power law)?

7. Do all massive stars form in groups or star clusters? Can massive stars be born in isolation or are allthe isolated O-stars high-velocity ”runaway” stars, either dynamically ejected from young star clusters orslingshotted from supernova explosions in massive binary systems?

8. What is the difference between dense compact OB clusters and the spread-out OB association? two birthmodes or dynamical evolution (expansion) of a single OB mode?

9. How do starburst on small scales (R136) and on large scales (M82) come about? Is there a trigger, and if sowhich? collision of supershells, satellite accretion?

10. How was massive star formation different in the early universe? massive stars in proto-globular clusters?Massive starbursts in proto-elliptical galaxies? How?

We expect to illustrate these questions by way of examples and discuss critical observations to find some answers.

First results from the Herschel Orion Protostar Survey

BABAR ALI1, W. FISCHER2, T. MEGEATH2, J. TOBIN3, AND THE HOPSTEAM .2

1 NHSC/IPAC/Caltech, Pasadena, CA 91125 USAbabar@ipac.caltech.edu2 University of Toledo, Toledo, OH USA

wfische@UTNet.UToledo.Edu,tommegeath@gmail.com,tommegeath@gmail.com 3 Universityof Michigan, Ann Arbor, MI USAjjtobin@umich.edu

The Herschel Orion Protostar Survey (HOPS), is a 200-hour open-timeHerschel key program to study star for-mation in the Orion molecular cloud complex in a diverse range of environments.HOPS will obtain PACS 70and 160 micron imaging of 278 Orion protostars and PACS spectroscopy ofa subset of 37, sampling the expectedpeak of the spectral energy distributions (SEDs) of embedded protostars. The Herschel data are part of a de-tailed multi-wavelength imaging and spectroscopy survey of protostars. In addition to the Herschel data, we haveSpitzer IRAC photometry, Spitzer 5-40 micron spectra for nearly all of the protostars, and near-IR imaging andspectroscopy with Hubble and ground-based telescopes for subsets of the protostars. The combined 1-160 micronphotometry and spectroscopy data are fit with model SEDs generated by theradiative transfer code of Whitneyet al. (2003, ApJ, 591, 1049) to determine the fundamental properties (multiplicity, gas infall rate, bolometricluminosity, outflow cavity geometry) of a large sample of protostars in a single cloud complex. By extending ourstudy of a nearby, active, environmentally diverse star-forming regioninto the far infrared, Herschel will enablean improved understanding of star formation: the evolution of protostars from the deeply embedded stage to thedispersal of the envelope, and the dependence of this evolution on environment.

While our statistical sample is still incomplete, the first set of HOPS data are already yielding importantresults: (i) The inferred mass infall rates for a group of protostars associated with the Herbig-Haro complex HH1-2 in the Orion A cloud show variations of 3 orders of magnitude, hinting at avariety of accretion activity. Wewill present similar analysis for all Herschel fields observed to September2010. (ii) Spectroscopy of protostarsshows a wealth of ortho- and para- water lines from proto-stellar envelopes, as well as forbidden OI and CIIemission from surrounding gas. And, (iii) surprisingly, the PACS 70 and 160 micron revealed a far-IR dark featurecoincident with what was believed to be a dense, cold globule associated withthe NGC 1999 reflection nebula.Our subsequent analysis shows that Herschel has observed a hole inthe sky: that the dark feature is a cavity in thenebula presumably cleared by V380 Ori.

Probing the formation mechanism of prestellar cores and theorigin of the IMF:First results from the Herschel Gould Belt Survey

PH. ANDRE1 AND THE HERSCHELGOULD BELT CONSORTIUM2

1 CEA/SAp Saclay,pandre@cea.fr2 cf. http://gouldbelt-herschel.cea.fr/

The Herschel Space Observatory provides a unique opportunity to improve our global understanding of theearliest phases of star formation. I will present an overview of the firstresults from the Gould Belt survey (cf.http://gouldbelt-herschel.cea.fr/), one of the largest key projects withHerschel. The immediate objective of thisSPIRE/PACS imaging survey is to obtain complete samples of nearby prestellar cores and Class 0 protostars withwell characterized luminosities, temperatures, and density profiles, as wellas robust core mass functions andprotostar luminosity functions, in a variety of star-forming environments. Thanks to its high sensitivity and largespatial dynamic range, this survey can also probe, for the first time, the linkbetween diffuse cirrus-like structuresand compact self-gravitating cores. The main scientific goal is to elucidate thephysical mechanisms responsiblefor the formation of prestellar cores out of the diffuse interstellar medium, which is crucial for understanding theorigin of the stellar initial mass function. The first results, obtained toward theAquila Rift and Polaris Flare regionsduring the ’Science Demonstration Phase’ (SDP), are very promising (see, e.g., Andre et al. 2010, Konyves et al.2010, Bontemps et al. 2010, Men’shchikov et al. 2010, Ward-Thompson et al. 2010, Miville-Deschenes et al.2010 – A&A special issue onHerschel). Based on these SDP and other early results, I will discuss preliminaryimplications for our understanding of, e.g., the link between the prestellar core mass function and the stellar initialmass function, the timescale of the core formation process, and the luminosity evolution of protostars. Comparingand contrasting ourHerschel results in, e.g., Aquila and Polaris, we propose an observationally-driven scenariofor core formation according to which complex networks of long, thin filamentsform first within molecular clouds,as a result of a complex interplay between interstellar turbulence, gravity, and magnetic fields, and then the densestfilaments fragment into a number of prestellar cores via gravitational instability.

References:Andre, Ph., Men’shchikov, A., Bontemps, S. et al. 2010, A&A (Herschel special issue),in press (astro-ph/arXiv:1005.2618)Bontemps, S., Andre, Ph., Konyves, V. et al. 2010, A&A (special issue), in pressKonyves, V., Andre, Ph., Men’shchikov, A. et al. 2010, A&A (special issue), in pressMen’shchikov, A., Andre, Ph., Didelon, P. et al. 2010, A&A (special issue), in pressMiville-Deschenes, M.-A., Martin, P.G., Abergel, A. et al. 2010, A&A (Herschel specialissue), in pressWard-Thompson, D., Kirk, J.M., Andre, P. et al. 2010, A&A (Herschel special issue), inpress (astro-ph/arXiv:1005.2519)

The Formation of Low Mass Stars: A Dynamic Perspective

M ICHAEL R. MEYER1

1 Institute for Astronomy, ETH Zurichname1@email.address,name2@email.address

Does star formation occur instantly across the stellar mass spectrum when a giant molecular cloud is ”ready” toform stars or are their significant age spreads observed? How can observations be used to disentangle star formationefficiency and the lifetime of molecular clouds actively forming stars? Are smaller or larger star forming eventsmore likely to be gravitationally bound? I will review current ideas concerning low mass star formation with aparticular focus on new results from Herschel and other facilities which will become available in coming years.Topics covered will include: a) impacts of initial conditions on star formation; b) timescales for various stages ofevolution; c) commonality of various modes of star formation; and d) kinematic properties of young clusters as afunction of age, stellar mass, and location within a cluster. A central questionto be addressed in coming years iswhat sorts of star formation contribute most to the galactic field population and what impact those environmentsmight have on concomitant planet formation.

From filaments to protostars: multi-scale star formationin the Hi-GAL survey

SERGIO MOLINARI1

1 INAF-IFSI, molinari@ifsi-roma.inaf.it

Water in massive star-forming regions with Herschel Space Observatory

F. HERPIN1, L. CHAVARRIA 1, T. JACQ1, F. VAN DER TAK2, F. WYROWSKI3, E. F.VAN DISHOECK4

1 Laboratoire d’Astrophysique de Bordeaux/OASU, B.P. 89, 33271 Floirac Cedex, France,herpin@obs.u-bordeaux1.fr

2 SRON Netherlands Institute for Space Research, Landleven 12, 9747 AD Groningen, The Netherlands,vdtak@sron.nl

3 Leiden Observatory, PO Box 9513, 2300 RA Leiden, The Netherlands ,Ewine van Dishoeckewine@strw.leidenuniv.nl

4 Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germany,wyrowski@mpifr-bonn.mpg.de

The formation of high-mass stars is much less understood than the low-mass case: even the time order ofobservational phenomena is uncertain. Water, one of the most important molecules in the Universe, might elucidatekey episodes in the process of stellar birth, and especially could be a major role in the formation of high-mass stars.This talk presents the first results of the Heschel Space Observatory key-program WISH. A key-goal of that KPis to follow the process of star formation during the various stages and use the water as a physical diagnosticthroughout the evolution. The HIFI and PACS instruments are used to make maps and spectra of 20 lines in 20sources spanning a large range in physical parameters, from pre-stellar cores to UCHII regions.

I will review the status of the program and focus specifically on the spectroscopic results. I will show howpowerful are the HIFI high-resolution spectral observations to resolve different physical source components suchas the dense core, the outflows or the extended cold cloud aroung the high-mass object. The abundance variationssuggest that different chemical mechanisms are at work on these scales(e.g. evaporation of water-rich icy grainmantles). A comparison in tems of degree of evolution will be done.

In particular, for the brigh-IR massive dense core W3-IRS5, the spectra of the following water lines is ana-lyzed: o-H17

2 O (110-101), p-H2O (202-111), p-H182 O (111-000), p-H2O (111-000), o-H2O (221-212), o-H2O (212-101),

covering a frequency range from 987 GHz up to 1669 GHz. Radiative transfer models in 1-dimension are usedto estimate the water abundances and to study the kinematics of the region. We observed a clear contribution ofoutflow shocks with high velocity wings in the inner regions of the protostar. The water lines also show absorp-tion from the dense core, but also, for the low-energy lines, absorptionboth from maybe a cold molecular cloudwherein the source itself is embedded. Based on the line profile analysis andmodelling, we propose that there aretwo protostellar objects detected in the spectra, embedded in a cold cloud. We estimated water abundances of theorder of 10−9 in the region.

WISHes coming true - Water in low-mass star-forming regionswith Herschel

L.E. KRISTENSEN1, U.A. Y ILDIZ 1, R. VISSER1, E.F.VAN DISHOECK 1,2, G.J. HERCZEG2, S.D. DOTY3,T.A. VAN KEMPEN4, J.K. JØRGENSEN5, M.R. HOGERHEIJDE1, S.F. WAMPFLER6, S. BRUDERER6, A.O.

BENZ6 AND THE WISH TEAM

1 Leiden Observatory, the Netherlands,[kristensen; yildiz; ruvisser; ewine;michiel]@strw.leidenuniv.nl

2 Max Planck Institut fur Extraterrestrische Physik, Garching, Germany,gregoryh@mpe.mpg.de3 Harvard-Smithsonian Center for Astrophysics, Cambridge, USA,tvankemp@cfa.harvard.edu

4 Denison University, Granville, USA,doty@denison.edu5 Centre for Star and Planet Formation, Copenhagen, Denmark,jes@snm.ku.dk

6 ETH, Zurich, Switzerland,[wsusanne; simonbr; benz]@astro.phys.ethz,ch

Star formation is a violent process where the quiescent remains of the parental molecular cloud are exposed tointense UV fields and high-velocity shocks, both originating in the protostar itself. At the same time, in-fallinggas is heated to several 100 K through thermal heating by the protostellar luminosity. The Key Program ”Waterin Star-forming regions with Herschel” (WISH) uses high spectral and spatial resolution observations of water toprovide observational constraints on energetic input and trace its chemistry in all stages of star formation. Wateris a unique probe of energetic input. In cold, dark molecular clouds, wateris frozen out onto the surfaces of smalldust grains, and only through energetic input will it be released into the gas phase. As this happens, water acts as a‘switch’ with the abundance increasing by three orders of magnitude to 10−5–10−4 w.r.t. H2. By observing manytransitions simultaneously it is possible to quantify how much of the emission arisesfrom the passively heated,UV-heated and shock-heated gas.

An overview of the low-mass protostellar survey of WISH will be presentedhere. Observations made usingHIFI are complemented by PACS of a number of low-mass protostellar objects at various evolutionary stages.They comprise more than 10 H2O and H18

2 O lines per object with energies up to 500 K above the ground state.Part of the water emission is seen to move at surprisingly high velocities with respect to individual sources, upto >50 km/s, indicating that at least part of the emission arises in the post-shock wake of the outflows. This isconfirmed by the very broad profile of the H18

2 O 110–101 line (FWHM of 20 km/s). The observational results,along with detailed modeling, allow for a quantification of the energetics, and show that shocks dominate andaccount for∼60% of the far-IR line luminosity. UV-heated gas accounts for∼35% while the rest is produced inthe passively heated envelope.

Sample spectra of H2O and CO lines toward three low-mass protostellar

objects in the NGC1333 star-forming region (Kristensen et al. A&A, HIFI special issue).

New insights to photon-dominated regions from Herschel observations

V. OSSENKOPF1, M. ROLLIG1, AND C. KRAMER2 AND THE FULL WADI TEAM

1 I. Physikalisches Institut der Universitat zu Koln, Zulpicher Straße 77, 50937 Koln, Germany,ossk@ph1.uni-koeln.de,roellig@ph1.uni-koeln.de

2 Instituto de Radio Astronomıa Milimetrica (IRAM), Avenida Divina Pastora 7, Local 20, 18012 Granada,Spain,kramer@iram.es

Herschel systematically observed a number of prominent photon-dominatedregions (PDRs) to to measure theimpact of varying UV fields on the energy balance, the chemical and dynamical structure of heated molecularclouds.

The measured HIFI spectra trace a large variety of chemical species. Wereport the first detection of somereactive molecules that only occur in UV illuminated regions. The Herschel observations give the first insight intothe abundances of light hydrides in their ground state allowing to calibrate thechemical models.

Combining the PACS data on the FIR continuum and the 63m [OI] cooling line with the detailed HIFI spectraof [CII] and other important cooling lines allows to determine the relative contribution of the different heating andcooling processes, to distinguish the different phases on both sides of the interface regions, and to measure thedynamics of the gas.

Combining the information contained in the observed complex line profiles of species tracing different den-sities and temperatures allows to deduce the three-dimensional picture of the interface regions including theirvelocity fields.

Outflow and Inflow in high mass star forming regions

M. WALMSLEY1, A. LOPEZ-SEPULCRE1, R. CESARONI1 AND C. CODELLA1

1 INAF Osservatorio Astrofisico di Arcetri,walmsley@arcetri.astro.it,sepulcre@arcetri.astro.it

Discussion of the formation of high mass stars is complicated by the fact that high mass stars form in clustersof mostly low mass (solar mass) objects and it is difficult to differentiate betweenthe formation of individualstars and of the cluster as a whole. This is in particular true for estimates of theinflow rate onto young massiveprotostars where accretion onto individual objects is often confused byinflow onto the clump from which a youngprotocluster is forming. An extra complication is that caused by the difficulty in deriving the physical conditionsin the infalling material. These confusions combined with those inherent in estimating either infall or outflow frommolecular line observations have caused a wild variety of ”educated guesses” for accretion rates onto protostarstogether with a slightly less wild variety of guesses for outflow rates (in that case partly due to the limited spatialresolution available towards high mass star forming sites). The advent of HERSCHEL only serves to worsen thissituation. I will endeavour to illustrate some of these themes with results from a recent study by Lopez-Sepulcreand collaborators using data from the IRAM 30m. I will also discuss briefly whether ALMA data are likely toimprove the situation.

Physical and chemical conditions in star forming regions

CECILIA CECCARELLI1

1 Laboratoire d’Astrophysique de Grenoble,Cecilia.Ceccarelli@obs.ujf-grenoble.fr

First results from the Herschel Gas in Protoplanetary disksSystems project

W.-F. THI1, W. DENT2, AND GASPSTEAM3

1 Laboratoire d’Astrophysique de Grenoble,Wing-Fai.Thi@obs.ujf-grenoble.fr2 ESO-ALMA Chile,wdent@alma.cl

I will present the first results from the Herschel large open time programmeGas in Protoplanetary systems(GASPS). The main aim of the GAPS programme is to determine the gas and dust mass of∼200 known youngstar/disc systems. After a presentation of the programme, I will discuss the first observations and describe thephysico-chemical code ProDiMo, which is used to interpret the data. Two objects have been analyzed in detailsand published in the A&A special issue (TW Hya and HD169142). I will also show the on-going analysis of newobservations of T Tauri (η Cha) and Herbig Ae discs (HD141569A).

3Herschel-GASPS team: J. M. Alacid, S. Andrews, D.R. Ardila, G. Aresu,J.-C. Augereau, D. Barrado, S. Brittain,D. R. Ciardi, W. Danchi, W. R. F. Dent (P.I.), G. Duchene, B. C. Eiroa, D. Fedele, I., C. A. Grady, de Gregorio-Monsalvo, A. Heras, C. D. Howard, N. Huelamo, I. Kamp, A. Krivov, J. Lebreton, R. Liseau, C. Martin-Zaidi, G.Mathews, F. Menard, I. Mendigutıa, G. Meeus, B. Montesinos, A. Mora, M. Morales-Calderon, H. Nomura, E.Pantin, I. Pascucci, B. Riaz, A. Roberge, G. Sandell, N. Phillips, C. Pinte, L. Podio, D. R. Poelman, S. Ramsay,K. Rice, P. Riviere-Marichalar, E. Solano, W.-F. Thi, I. Tilling, B. Vandenbussche, H. Walker, G. J. White, J. P.Williams, P. Woitke, G. Wright

References:Mathews et al., 2010, A&A, 518, L127Meeus et al., 2010, A&A, 518, L126Thi et al., 2010, A&A, 518, L125Pinte et al., 2010, A&A,, 518, L124

HIFI observations of high-mass star formation

FLORIS VAN DER TAK1

1 SRON Netherlands Institute for Space Research, Groningen, The Netherlands,vdtak@sron.nl

High-mass stars are rare, but play a major role in the energy budget and the shaping of the Galactic environ-ment. Despite this importance, the formation of high-mass stars is much less understood than the low-mass case,due to large distances, short time scales, and heavy extinction. The HIFI spectrometer onboard the Herschel spaceobservatory allows a new approach to high-mass star formation. Most of itslarge frequency coverage is inacces-sible from the ground, but contains spectral lines of water, hydrides, and other astrochemically important specieswhich can now be studied for the first time. Its high resolution provides a fullview of the molecular compositionof star-forming regions, and a detailed picture of the motions in interstellar gasclouds.

This talk presents the first results of HIFI observations of high-mass star-forming regions, with an emphasison the H2O molecule. Line profiles of H2O toward high-mass star-forming regions show at least 3 physicalcomponents: a dense core, a bipolar outflow, and a warm tenuous foreground cloud. The H2O abundance variesby orders of magnitude between these components, and appears to be a complex interplay between freeze-out,warm gas-phase chemistry, and photodissociation processes. The H2O molecule is therefore a sensitive probe ofphysical conditions such as the density, the temperature, and the ultravioletradiation field. Studies of multiplesources show that the H2O abundance varies by a factor of 100 or more between regions, which may be related totheir evolutionary state.

Another early key result from HIFI is the discovery of exotic forms of H2O: ionized water (H2O+) and heavywater (D2O). While H2O+ appears to trace ultraviolet radiation fields in diffuse molecular clouds and X-rays inactive galactic nuclei, the main origin of H2O+ in high-mass star-forming regions seems to be low-density gasin molecular outflows. A large fraction of the hydrogen in these outflows mustbe in atomic form to prevent thereaction of H2O+ with H2; very likely, this gas has been dissociated by strong J-type shocks. Theheavy D2Oisotope is only seen toward low-mass star-forming regions, where it implies the(present or past) existence ofultracold phases (T ≈ 5 K) because of the small difference in zero point energy between D2O and H2O. Thisspecies has not been detected toward high-mass star-forming regions, suggesting that such a prolonged ultracoldphase does not occur during high-mass star formation.

Further clues to the origin of H2O come from its measured ortho/para ratio which HIFI has measured towardseveral sources. The results present a challenge to standard theories where H2O is formed as an ice mantle on dustgrains and is thermally evaporated into the gas phase as the dust is heated bynearby protostars.

A final specialty of HIFI turns out to be the study of diffuse foregroundclouds, some of which surrounddense star-forming regions while others are unrelated line-of-sight coincidences. Such foreground clouds are seenin several species including H2O, CH and HF; comparison between these species helps to pin down the physicalconditions in these clouds. The talk concludes with a comparison to low-mass star-forming regions, and an outlookto future HIFI observations.

References:Emprechtinger et al 2010, A&A, in press (arXiv: 1007.4226)Marseille et al 2010, A&A, in press (arXiv: 1007.4119)Van der Tak et al 2010, A&A 518, L107Van der Wiel et al 2010, A&A, in press (arXiv: 1007.1539)Vastel et al 2010, A&A, in press (arXiv: 1007.4410)Wyrowski et al 2010, A&A, in press (arXiv: 1007.4370)

Session VI:Laboratory astrophysics, astrochemistry

Chemistry in the Insterstellar Medium: New Views offered by Herschel

E. A. BERGIN1

1 University of Michigan, Ann Arbor (USA),ebergin@umich.edu

In this talk we will review our basic understanding of chemical processes ininterstellar medium extending fromquiescent chemistry in diffuse to dense gas, shocked regions, and regions exposed to energetic radiation. Ourunderstanding of chemistry in all of these physical environments is receiving a significant boost from the HerschelSpace Observatory. Where possible I will discuss the impact of these results with a particular emphasis on therich spectrum of gas emission seen in the far-infrared as illustrated in the figure below. I will end with a futureprospectus as we move into an era dominated by high spectral and spatial resolution studies.

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Figure 1: Herschel/HIFI band 1a and 4b spectrum of Orion KL (Bergin et al. 2010).

References:Bergin, E. et al. 2010, A&A, HIFI special issue

The Evolution of Dust in the ISM

ALAIN ABERGEL1

1 CNRS/Universit Paris-Sud 11,alain.abergel@ias.u-psud.fr

Formation of complex carbon-containing molecules in space

A. W. D. GEPPERT1, M. HAMBERG1, E. VIGREN1, V. ZHAUNERCHYK1, E. WIRSTROM2, H. ROBERTS3, C.M. PERSSON2, M. KAMINSKA 4, T. J. MILLAR 3, J. H. BLACK 2, A. HJALMARSON2,R. D. THOMAS1, J.

SEMANIAK 4, P. BERGMAN2 AND M. L ARSSON1

1 Physics Department, Stockholm University, Swedenwgeppert@hotmail.com2 Onsala Space Observatory, Chalmers University of Technology, Gothenburg, Sweden

3 Faculty of Engineering and Physical Sciences, Queen’s University Belfast, UK4 Jan Kochanowski University, Kielce, Poland

It has been a long-standing issue to what extent complex carbon-containing interstellar molecules like methanol,ethanol, dimethyl ether and formic acid are produced in the gas-phase or on grain surfaces. As gas-gas productionpathways very often ion-neutral reactions leading to the protonateed form of the species followed by dissociativerecombination to yield the final product has been invoked.

In the case of methanol, a feasible gas-phase production process is unlikely. The rate of radiative association ofCH3

+ and H2O leading to CH3OH2+ has been found to be far to low to explain the observed methanol abundances

(Gerlich & Smith 2006) and, on top of that, only a minor fraction of methanol (3%) is produced in the dissociativerecombination of the latter ion (Geppert et a. 2006). On the other hand, successive hydrogenation of CO on icygrain surface by H atoms has been found to produce this compound (Fuchs et al. 2009).

In order to gain some observational evidence for the origin of interstellar methanol, observations of the12C/13Cratio of methanol (using the 2-1 rotational line groups) in five massive young stellar objecrs were carried out at the20 m-telescope located at Onsala Space Observatory. These were then compared to the respective ratios in gaseousCO and solid CO2 for these environments. If the methanol was formed through hydrogenation of CO on icy grainsurfaces, these isotope ratios should resemble one another. If gas-phase processes were responsible, the12C/13Cratio observed in methanol should be considerably higher, since CO accumulates13C under cold conditions. This”isotope labelling a posteriori” can thus function as evidence for the origin of complex molecules in the interstellarmedium (Charnley, S. B. et al 2004).

It has been observed that with one exception (where the12CH3OH lines probably are optically thick ant theisotope ratio of methanol is actually smaller than the one of CO) the12C/13C ratios of methanol lie within theerror bars of those observed for CO (Langer and Penzias, 1990 and own observations). They are also found to besomewhat lower than the ones observed for solid CO2 (Gibb et al. 2004, Boogert et al. 2000). These findings arein agreement with a grain surface origin of interstellar methanol, which is also inline with the strong correlationof methanol and formaldehyde observed in massive hot cores (Bisschop 2007). In addition, the ratio between theE and A spin state reveal that the methanol molecules observed must have undergone their last chemical reactionat temperatures between 10 and 15 K.

References:Bisschop S. E., Ph. D. thesis, Leiden University, 2007Boogert, A. C. A et al. A&A, 353, 349Charnley, S. B. et al. 2004, MNRAS, 347, 157Fuchs, G. W. et al. 2009, A&A, 505, 629Geppert, W. D. et al. 2006, Faraday Discuss. 133, 177Gerlich, D. and Smith, M. 2006, Phys. Scripta, 73, C25Gibb, E. L. et al. 2004, ApJS, 151, 35Langer, W. D. and Penzias, A. A. 1990, ApJ, 357,477

Initial Results from the Herschel Oxygen Project (HOP)

PAUL F. GOLDSMITH1 ON BEHALF OF THEHOP TEAM

1 Jet Propulsion Laboratory, California Institute of Technology,Paul.F.Goldsmith@jpl.nasa.gov

Oxygen is the third most abundant element in the cosmos, but can be found inmany forms. In the gas phase,oxygen can be ionized, atomic, or in molecular form, and it is also incorporated into grains. The molecular formis expected to dominate in cold, well-shielded regions, and in such molecular clouds, oxygen can be found inkey species including carbon monoxide and water. Gas-phase chemistry models predict molecular oxygen (O2)to be almost as abundant as CO. A number of searches for rotational transitions of molecular oxygen have beencarried out. These include ground-based searches for the isotopologue16O18O and searches for16O2 in galaxieswith redshift sufficient to move the line away from terrestrial atmospheric absorption. Searches for Galactic16O2

carried out with the SWAS and Odin spacecraft have yielded upper limits on the abundance of molecular oxygentypically 1 to 2 orders of magnitude below those predicted by gas-phase models. There has been a statisticaldetection of O2 in one source, again indicating a low abundance. A variety of explanationshave been proposed toexplain this low abundance. Some of these are based on depletion of atomic oxygen onto dust grains, resulting inincorporation of this species into water that remains on the grain surface. Available gas-phase oxygen is largelyincorporated into CO leaving little for gas-phase O2. Other models involve circulation of material from less well-shielded to more highly-shielded regions.

To address this important problem in astrochemistry, which is likely connectedto fundamental questions aboutmolecular cloud structure, we have developed the Open Time Key Project HOP (Herschel Oxygen Project), whichexploits the high angular resolution and sensitivity of the HIFI instrument on Herschel to observe 3 rotationaltransitions of O2 in a broad sample of molecular clouds. These include Giant Molecular Cloudswith embed-ded massive stars that result in large column densities of warm dust, PhotonDominated Regions (PDRs), X-rayDominated Regions (XDRs), shocked regions, and Infrared Dark Clouds (IRDCs).

Collectively, these observations will probe a wide range of regions for which specific predictions for molecularoxygen abundance are available. The sensitivity of HIFI is a dramatic improvement over anything previously avail-able at these frequencies. The much higher angular resolution of Herschel compared to previous submillimeter-wavelength space missions is a great advantage for most of these types ofsources. The predictions of best currentmodels are that our HIFI observations should be give definitive detections of O2. These data should, whether yield-ing detections or significantly improved upper limits, provide critical information about interstellar chemistry andthe structure of these varied molecular regions. We will discuss the plannedHOP observations, and report on thestatus of HOP. The early results from Priority Science Phase observations are consistent with the low abundancesfound by SWAS and Odin, but these will be discussed in detail, along with the Regular Science Observation Phasedata that have been taken ad analyzed.

Collision Rate Coefficients

MARIE-L ISE DUBERNET1

1 Universite Pierre et Marie Curie (UPMC),marie-lise.dubernet-tuckey@upmc.fr

The Ortho/Para Ratio in Interstellar Water

D. C. LIS1, T. G. PHILLIPS1, P. F. GOLDSMITH2, AND THE HEXOS AND PRISMAS TEAMS

1 Caltech, MS 301-17, Pasadena, CA 91125, USAdcl@submm.caltech.edu,tgp@submm.caltech.edu

2 JPL, MS 180-703, Pasadena, CA 91109, USApaul.f.goldsmith@jpl.nasa.gov

Water molecules play an essential role in the physics and chemistry of the dense interstellar medium. Water is oneof the main reservoirs of oxygen, and as an important coolant of dense gas it strongly affects its star formationproperties. The ortho/para ratio for a molecule with a nuclear spin, such aswater, is a parameter, which is tem-perature dependent and from which, in principle, the temperature of the medium where the spins last equilibratedcan be deduced. The ortho/para ratio in water reaches an equilibrium value of 3 in the high temperature limit.Departures from the statistical equilibrium are seen for temperatures belowabout 60 K, with the ratio dropping tohalf of its statistical equilibrium value at about 20 K. The HIFI instrument aboard the Herschel Space Observatoryprovides exceptional capabilities to probe water vapor in cold, dense gasby means of absorption spectroscopytoward bright, distant submillimeter continuum sources. Compared to earlier studies, HIFI offers a tremendous ad-vantage in sensitivity and spectral coverage, giving access to the ground-state rotational transitions of both ortho-and para-water, as well as water isotopologues. Sgr B2, W31C, W49N,and W51 are some of the strongest submil-limeter continuum sources in the Galaxy. This makes them prime candidates for absorption studies, probing entiresightlines with clouds in multiple spiral arms easily identified at separate velocities.Sensitive observations of wa-ter toward these sources have been carried out as part of HEXOS andPRISMAS Guaranteed Time Key Programs.Results of these investigations will be discussed.

Coreshine : the ubiquity of micron-size grains in star-forming regions

L. PAGANI1, A. BACMANN2, J. STEINACKER1,3, A. STUTZ3, AND TH. HENNING3

1 LERMA & UMR 8112 du CNRS, Observatoire de Paris, Francelaurent.pagani@obspm.fr2 LAOG & UMR 5571 du CNRS, Observatoire de Grenoble, France

aurore.bacmann@obs.ujf-grenoble.fr3 Max-Planck-Institut fur Astronomie, Heidelberg, Germany

stein@mpia.de,stutz@mpia.de,henning@mpia.de

Dust grains are an important component of star forming regions and are therefore a powerful tracer of the locationand mass of prestellar cores. ŁHowever, the properties of dust grainsin such dense regions are poorly constrained,causing difficulties in the modeling of the physical properties of dense cores. ŁOne of the fundamental properties ofdust grains is their size distribution, which is relatively well-known in the diffuse ISM but not very well constrainedin dense regions. Indirect evidence is consistent with the presence of large grains; however, to date, interpretingsubmm emission measurements or absorption in the near-infrared (NIR) /mid-infrared (MIR) domains is difficultdue to the ambiguity between density variations and grain properties. Recently, we have discovered emission at3.6 and 4.5µm towards the densest parts of L183 (Steinacker et al. 2010). We havenamed this effect Coreshine,by analogy with the Cloudshine, seen at the surface of dark clouds in the near-infrared (Foster & Goodman). This3.6 and 4.5µm emission can only be explained by the strong scattering of background interstellar radiation dueto micron-size grains and show that the average grain size increase needs to be proportional to the cloud coredensity gradient to reproduce the observations. We show that the scattering effect is very sensitive to the grainsize distribution; therefore these observations will provide a new tool with which to study grain properties. In asubsequent search through about a hundred of dense core regions in the Spitzer Archive, we find that the effect ispresent in∼50% of the sources (the presence of diffuse MIR emission was already noticed by Stutz et al. 2009),including prestellar cores, Class 0 and I sources with or without outflow, showing that the Coreshine effect shouldrapidly become a general observational method to investigate dark cloud and grain properties. Implications forcloud and dense core mass estimates, 3D structure and chemistry will be discussed.

Figure 1: Spitzer-IRAC images of L183 at 3.6, 4.5, and 8.0µm. The superimposed contours mark the AV = 5 and10 mag. limits respectively (from Pagani et al. 2004)

References:Foster, J.B., & Goodman, A.A., 2006, ApJ, 636, L105Pagani, L., Bacmann, A., et al. 2004, A&A 417, 635Steinacker, J., Pagani, L., Bacmann, A., Guieu, S., 2010, A&A 511, A9Stutz, A., et al. 2009, ApJ 707, 137

New trends in laboratory spectroscopy of astrophysically relevant species

S. SCHLEMMER1 AND T. GIESEN1

1 I. Physikalisches Institut, Universitat zu Koln, 50937 Koln, Germanyschlemmer@ph1.uni-koeln.de,giesen@ph1.uni-koeln.de

With the operation of Herschel new windows for astronomical observations have been opened. Rotational transi-tions of light hydride molecules, radicals and ions are in the frequency range of HIFI and even at the higher THzfrequencies of PACS. Also more complex, well known species contribute tothe observed spectra. Transitions ofother well known species such as H2O, H2O+, OH+ etc. turn out as key species in understanding the physics andchemistry of the different environments they are found in. Some other species are speculated to exist but theirlaboratory spectra are not known.

Jet apparatuses, trap experiments and conventional absorption cells are used in Cologne to record spectra ofthese species. In low temperature ion traps ion-molecule reactions are promoted by the excitation of the parent ion.Using a home-built high-resolution OPO laser system in the 3 micron range very accurate ro-vibrational transitionsof CH2D+ have been recorded. The sensitivity of this method is unprecedented since only a few hundred ions arenecessary to record a spectrum. Based on the excessive amount of data the model description of the ro-vibrationaltransitions is so precise, that rotational transitions can be predicted to observational accuracy (MHz). Moreover,pure rotational transitions have been recorded for H2D+. The most recent development is a double resonancemethod, combining a THz radiation source, an IR laser with the trap to record pure rotational transitions of astored ion. This extension of the method of laser induced reactions (LIR) makes this a very versatile tool forspectroscopy and dynamics. The potential of the methods also for understanding deuterium fractionation in spacewill be discussed.

A dedicated IR OPO laser system around 5 micron has been developed in Cologne to record spectra of carbonchain molecules and heterosystems like Si2C3. These molecules are investigated in a new jet apparatus which isaimed at using cavity techniques to improve the sensitivity substantially w.r.t. conventional jet absorption tech-niques. Jet experiments are also used for spectroscopy of transient molecules in the THz region, namely at frequen-cies which are accessible with the Herschel/HIFI instrument and ground based telescopes. Target molecules arecarbonaceous species such as linear carbon chains (C3, C3H), small silicon-carbids (Si2C), and metal containingspecies (TiO, TiO2, AlO) as well. Spectra of these transient molecules reveal intermolecular coupling effects andtherefore serve as benchmark systems for state-of-the-artab initio calculations.

Chemical Models of Young Stellar Objects - Hot Core Chemistry-

H. NOMURA1, T.J. MILLAR 2

1 Department of Astronomy, Kyoto University,nomura@kusastro.kyoto-u.ac.jp2 ARC, School of Mathematics and Physics, Queen’s University Belfast,Tom.Millar@qub.ac.uk

It is observationally known that many high mass star-forming cores and somelow mass star-forming cores are char-acterized by anomalously large abundances of some molecular species, such as hydrogenated, saturated molecules(e.g., NH3, H2O) and complex molecules (e.g., CH3OH, HCOOCH3). These molecules are thought to originatefrom grain surface chemistry in a cold prestellar phase and the subsequent icy mantle evaporation and chemicalreactions in the gas in a hot (> 100K) protostellar phase.

The high and low mass young stellar objects basically consist of the central young stars, the circumstellardisks, and the associated bipolar outflows. Accretion flow towards the starin the disks and outflow from the disks,which transport molecules and destruct them at the shock front, togetherwith the irradiation from the central star,which heats the surrounding gas and dust as well as photodissociate molecules, control the chemical structure ofthe young stellar objects.

Recent Hershel observations have shown new detection of far-infrared molecular transition lines towards highmass star-forming regions. Meanwhile, the forth-coming ALMA observations are expected to reveal the chemicalstructure of high mass young stellar objects with high spatial resolution. In thispresentation I will talk about thechemical structure of young stellar objects based on our modelling which takes into account of the effects of thedynamical flow in the objects and the irradiation from the central star, and its implications for the Hershel andALMA observations.

References:Nomura, H. Millar, T.J. 2004, A&A, 414, 409Nomura, H. Millar, T.J. 2009, in Protostellar Jets in Context, ed. K. Tsinganos, T. Ray, M.Stute (Berlin: Springer), 593Nomura, H., Aikawa, Y., Nakagawa, Y., Millar, T.J. 2009, A&A, 495, 183

Complex organic chemistry in the Galactic Center Region

JESUSMARTIN-PINTADO1

1 CAB(CSIC-INTA),jmartin.pintado@iem.cfmac.csic.es

Peculiar Carbon-Chain Chemistry in Low-Mass Star Forming Regions

NAMI SAKAI 1, TAKESHI SAKAI 1, TOMOYA HIROTA2, SATOSHI YAMAMOTO1

1 The University of Tokyo,nami@taurus.phys.s.u-tokyo.ac.jp2 National Astronomical Observatory of Japan

We found low-mass star forming-regions which show extremely high abundances of carbon-chain molecules.Those are L1527 in Taurus and IRAS15398-3359 in Lupus (e.g. Sakai et al. 2008a; 2009a). This discovery wassurprising, because carbon-chain molecules are generally deficient instar-forming regions. Single-dish observa-tions toward L1527 reveal that C4H is distributed over the 40′′ scale around the protostar, and the C4H line showsapparent line broadening toward the protostar. In IRAS15398-3359,high excitation lines of CCH show centralcondensation around the protostar. In these sources, carbon-chainmolecules would be regenerated in a lukewarmregion near the protostar, triggered by the evaporation of the CH4 ice. This is new carbon-chain chemistry (WarmCarbon-Chain Chemistry: WCCC) in contrast to the conventional one whichhas long been applied to cold starlesscores.

Recently, we have observed carbon-chain molecules in L1527 with PdBI.The distributions show clear centralcondensation around the protostar, confirming that these molecules are associated with the protostar environment.The blue and red shifted components are concentrated near the protostar, indicating their existence in an infallingenvelope. The intensity distributions show a steep increase at the radius of500−1000 AU from the protostar. Bycomparing the distribution with H2 column density distribution from the DUSTY model, the abundances are foundto be enhanced by a factor of about 10 within the increasing point, where the temperature becomes higher than20-30 K. This result supports the picture of WCCC. On the other hand, thedistributions have a slight dip with aradius of 300-600 AU toward the protostar position, indicating that their abundances would decrease toward thecentral part. The present results provide a new picture of regeneration and destruction of carbon-chain moleculesin the closest vicinity of a low-mass protostar.

The discovery of the WCCC sources demonstrates that the chemical composition of low-mass star-formingregions is not uniform, but has a significant variety. In particular, a remarkable contrast can be seen between WCCCand hot corino chemistry. Carbon-chain molecules are deficient in hot corino sources like NGC1333IRAS4B,whereas complex organic molecules seem to be less abundant in the WCCC sources. A possible origin for thiswould be the time scale of the starless-core phase; a shorter contraction time would result in WCCC. Relativelylow deuterium fractionation ratios in L1527 also support this scenario. Thus, the chemical composition providesan important clue to explore the source-to-source variation of star-formation processes, which will be a good targetfor ALMA.References:Sakai, N. et al. 2009, ApJ, 697, 769Sakai, N. et al. 2009, ApJ, 702, 1025Sakai, N. et al. 2010, ApJ, submitted.

Radiation Diagnostics in Star-forming Regions using Hydrides

A. O. BENZ1, S. BRUDERER1, S. F. WAMPFLER1, C. DEDES1, E. F.VAN DISHOECK2,3, AND S. D. DOTY1

1 Institute of Astronomy, ETH Zurich, 8093 Zurich, Switzerlandbenz@astro.phys.ethz.ch

2 Leiden Observatory, PO Box 9513, Leiden, The Netherlands3 MPI fur Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany

4 Denison University, Granville, OH 43023, USA

Diatomic hydrides, such as OH, CH, NH, SH, and their ions are a class of molecules that have become observablein their major lines with the Herschel Space Observatory. They are key species in the chemical evolution. If high-energy photons - FUV or X-rays - interact with the molecular gas, hydrides and particularly their ions are greatlyenhanced in abundance (e.g. Hollenbach & Tielens, 1995), thus, tracing gas irradiated by UV or X-rays. As thecritical densities for line emission are of the order of> 107 cm−3, irradiated dense regions are expected to lightup or cold regions to absorb in the ground state of the molecule.

Depending on the type of irradiation (FUV or X-rays) and depending on temperature and density, differentlines of hydrides and ions are enhanced differently. The radiation may beemitted by the protostar surface oraccretion hot spot. Alternatively, high temperature regions such as shock heated interfaces to the outflow or ahot disk surface also can enhance hydride abundances and emission.In preparation for the Herschel observations,chemical-physical models in 2D have recently been developed . The modelingincludes radiative transfer includinggeometrical effects.

First observations by Herschel/HIFI have explored the abundances of major hydrides in high-mass objects.The target lines of CH, NH, H3O+, and the new molecules SH+, H2O+, and OH+ are detected (Benz et al. 2010;Bruderer et al. 2010a). The lines are observed in emission, absorptionor both (P-Cyg-like). For the first time,OH+ and tentatively H2O+ are observed in emission. Emissions need high density and thus originate likelynearthe protostar. This is corroborated by the absence of line shifts relative tothe young stellar object. In addition,H2O+ and OH+ also show strong absorption components shifted relative to the star forming region. Such linecomponents are attributed to foreground clouds.

The molecular column densities derived from observations correlate well with predictions of a model by Brud-erer et al. 2010b, assuming the main emission region in outflow walls, heated and irradiated by protostellar UVradiation.

References:Benz S. et al. 2010, A&A, submittedBruderer S. et al. 2010a, A&A, submitttedBruderer S., Benz A.O., Stauber P., & Doty S.D., 2010b, Ap.J., in pressHollenbach D.J. & Tielens A.G.G.M. 1999 Rev. Mod. Phys. 71, 173

Laboratory Astrophysics of Dust

C. JAGER1, H. MUTSCHKE2, AND TH. HENNING3

1 Max Planck Institute for Astronomy, Heidelberg and Institute of Solid State Physics, Friedrich SchillerUniversity, Helmholtzweg 3, D-07743 Jena, Germanycornelia.jaeger@uni-jena.de

2 Astrophysical Institute and University Observatory, Friedrich Schiller University, Schillergasschen 3, D-07745Jena, Germanymutschke@astro.uni-jena.de

3 Max Planck Institute for Astronomy, Konigstuhl 17, D-69117 Heidelberghenning@mpia.de

Dust is present in nearly all astrophysical environments proving its existence by interstellar extinction curves, IRspectra, and the elemental depletion patterns. Dust grains absorb and scatter stellar light and reemit the absorbedenergy at infrared and millimeter wavelengths.

Infrared spectroscopy is the best astronomical tool for studying the composition of cosmic dust. Thanks to theHerschel satellite, dust properties from the FIR to mm wavelength range willbe sampled in different astrophysicalenvironments. The observations will contribute to a better understanding and modeling of the FIR/mm interstellardust emission and will supply important information on most phases of the dust’s life cycle and will help to unravelphysical and chemical processes involved in star formation and early stellar evolution in our own Galaxy.

For the interpretation of these data, the spectral properties of cosmic dustat long wavelengths are required.These spectral data can be obtained by measurements on dust analogs prepared in the laboratory. In additionto spectral measurements, structural, compositional, and morphological modifications of the dust grains fromcircumstellar to planetary environments have to be studied in the laboratory to understand the diversity of majordust components such as silicates or carbonaceous materials.

The study of the temperature and structural dependence of FIR absorption including agglomeration is essentialto interpret observational spectra. For crystalline materials, FIR single phonon bands are temperature dependentdue to the anharmonicity of the vibrational potentials. This strong temperature dependence of the FIR bands’positions can be used as a thermometer of the dust temperature. In amorphous material, the FIR absorption isdominated by disorder-induced single phonon processes and in the submillimeter and millimeter range by highlytemperature-dependent low energy processes, e.g. tunneling transitions in two-level systems. The effect of theseprocesses on the FIR absorptivity in amorphous silicates will be demonstrated.

Session VII:Future opportunities

Future Directions: Instrumentation, Telescopes and Laboratory Investigations

MARTIN HARWIT1

1 Cornell University,harwit@verizon.net

Future investigations of star formation are likely to focus on the interplay of chemical and dynamic processesin highly localized regions — molecular, atomic, ionized, shocked, or radiationdominated. The emphasis willincreasingly require higher spatial and velocity (i.e., spectral) resolution.Because critical phases in star formationmay be short-lived we will need to sift through large volumes of data to locate and gain insight on them. Accessto this varied information will involve powerful instrumentation both on the ground and in space. While some ofthe requisite facilities are currently under construction others remain unspecified, and I plan to identify the mosturgently needed among them. Observational facilities alone will, however, not suffice. Many critically involvedchemical species and processes are likely to remain unidentified without further laboratory studies. Promotingthose investigations has traditionally been difficult, partly because they appear to have few engineering, or basictheoretical applications. This barrier will be overcome only if the astronomical community decides to provide therequisite political support. I plan to touch on this continuing quandary.

ALMA: Status Report on Construction and Preparations of Early Science

THIJS DEGRAAUW1, ON BEHALF OF THEALMA PARTNERSHIP

1 ALMA Observatory, Santiago, Chile ,thijsdg@alma.cl

The Atacama Large Millimeter/submillimeter Array (ALMA) is an international radio observatory under construc-tion in the Atacama region of northern Chile. It is a partnership among Europe, North America and East Asia incooperation with the Republic of Chile. ALMA is a combination of two arrays of high-precision submm antennas:one made of 50 12-meter antennas which can be arranged in configurations with diameters ranging from about 150meters to 15 km, the other consists of twelve 7-meter diameter antennas operatingin closely-packed configurationsof about 50m in diameter. In addition there will be four more 12-meter antennas to provide the ”zero-spacing”information, which is critical for making accurate images of extended objects.All together the collecting area willbe 6600 square meters. The antennas will be equipped with sensitive (sub)millimeter-wave receivers covering mostof the frequency range from 84 to 950 GHz. State-of-the-art microwave, digital, photonic and software systemswill be used to capture the signals, transfer them to the correlators as well as maintaining accurate synchronization.ALMA will enable the astronomical community with a (sub)mm facility to address keyquestions in all areas ofastronomy. It will provide (sub)mm images with Hubble type detail, a velocity resolution of 100m/s and with greatsensitivity and fidelity. This contribution provides an update on the status of construction and reports on progressof the development of the Observatory, the scientific commissioning and plansfor operations.

APEX instrumentation: status and near-term developments

S. HEYMINCK1, R. GUSTEN1, B. KLEIN1, T. KLEIN1, C. KASEMANN1, C. LEINZ1, F. SCHAFER1, A.BARYSHEV2, J. BASELMANS2, T.M. KLAPWIJK3, G. DE LANGE2, J. STUTZKI4, K. JACOBS4, N. HONINGH4,

D. MAIER5 AND K. SCHUSTER5

1 Max-Planck-Institut fur Radioastronomie,heyminck@mpifr-bonn.mpg.de2 SRON, Netherlands Institute for Space Research

3 Delft University of Technology4 KOSMA, I. Physikalisches Institut der Universitat zu Koln

5 IRAM, Institute de Radioastronomie Millimetrique

APEX, a 12 m sub-millimeter telescope located at the ALMA-site in northern Chile,5100m above sea-level,offers unique observing capabilities to the southern sky. The facility offers a wide variety of direct detection andheterodyne instruments in all routinely accessible atmospheric windows to the observers. The suite of APEXfacility instruments is described atwww.apex-telescope.org. In addition, the APEX Partners operate PrincipalInvestigator instruments, aiming at dedicated science topics. Here we present an overview of the MPIfR leaddevelopments of novel technology instruments.

LAsMA, a joint development with KOSMA, is a dual color multi-pixel heterodyne system now in the finaldesign phase, and will become operational in 2011. The receiver will have 7 pixels operating in the 345 GHz andup to 19 pixels – 7 in its first light configuration – in the 460 GHz atmospheric windows. Both sub-arrays canbe used simultaneously. LAsMA together with CHAMP+ (cooperation with SRON-G), our 2× 7-pixel 660 / 810GHz array, will offer outstanding heterodyne mapping capabilities in all atmospheric windows routinely accessibleform APEX.

Both heterodyne arrays are supplemented by special purpose single pixel PI-receivers. A 1.05 THz SIS receiver(with SRON-G), scheduled now for summer 2010, will allow – under very good weather conditions – observationsin the barely explored atmospheric window around the CO(9-8) rotational transition. The instrument will com-plement ongoing HIFI observations with higher angular resolution. Of great use for line-surveys in the 345 GHzwindow, our now re-worked FLASH receiver will offers up to 8 GHz ofinstantaneous bandwidth using 345 GHzsideband separating mixers provided by IRAM. In parallel, the receiveroperates a 460 GHz DSB SIS channel.

All front-ends are supported by state-of-art digital spectrometers. Currently each mixer can be connected to2x1.5 GHz back-ends (2.8 GHz in total, with overlap). Our next generationXFFT-spectrometer of 2.5 GHz ofinstantaneous bandwidth with 32k channels will be deployed end of 2010. The wide all-digital intrinsic bandwidth(no plat forming) of these new spectrometers will further improve the data quality, enlarge the usable bandwidth(e.g. using 2x2.5 GHz with overlap – most receiver channels offer 4 GHzbandwidth), or reduce the overall systemcomplexity.

Based on our reconfigurable FPGA spectrometer technology, we have developed a read-out system, operatingin the frequency domain, that will allow operation of large arrays of Microwave Kinetic Inductance Detectors(MKIDs). Encouraged by very promising performances reported forMKID detectors recently, we are – withSRON-U – in the final design study for a verylarge dual-color MKID camera for APEX.

SOFIA - Update and the Beginning of Early Science Flights

ERICK YOUNG1

1 SOFIA Science Center,eyoung@sofia.usra.edu

JWST and Star Formation

T. GREENE1

1 NASA’s Ames Research Center,tom.greene@nasa.gov

The 6.5-m aperture James Webb Space Telescope (JWST) will be a powerful tool for studying and advancingnumerous areas of astrophysics. Its Fine Guidance Sensor, Near-Infrared Camera, Near-Infrared Spectrograph,and Mid-Infrared Instrument will be capable of making very sensitive, high angular resolution imaging and spec-troscopic observations spanning 0.7 - 28µm wavelength. These capabilities are very well suited for probing theconditions of star formation in the distant and local Universe. Indeed, JWST has been designed to detect first lightobjects as well as to study the fine details of jets, disks, chemistry, envelopes, and the central cores of nearby pro-tostars (e.g., Gardner et al. 2006). We will be able to use its cameras, coronagraphs, and spectrographs (includingmulti-object and integral field capabilities) to study many aspects of star formingregions throughout the galaxy,the Local Group, and more distant regions. I will describe the basic JWSTscientific capabilities and illustrate afew ways how they can be applied to star formation issues and conditions with afocus on Galactic regions.References:Gardner, J. et al. 2006, Space Science Reviews, 123, 485

Science with SPICA, the next generation mid- and far-IR space telescope

JAVIER R. GOICOECHEA1, TAKAO NAKAGAWA 2, AND THE SPICA TEAMS

1 Centro de Astrobiologıa (CSIC-INTA), Madrid, Spainjr.goicoechea@cab.inta-csic.es

2 Institute of Space and Astronautical Science, Japan Aerospace Exploration Agencynakagawa@ir.isas.jaxa.jp

We present an overview of SPICA, a world-class space observatoryoptimized for mid- and far-IR astronomywith a cryogenically cooled 3-m class telescope (<6 K). Its high spatial resolution and unprecedented sensitivityin both photometry and spectroscopy modes will enable us to address a number of key problems in astronomy.SPICA’s large, cold aperture will provide a two order of magnitude sensitivity advantage over current far–IRfacilities (λ>30µm wavelength). In the present design, SPICA will carry mid-IR camera, spectrometers andcoronagraph (built by JAXA institutes) and a far-IR imager FTS-spectrometer, SAFARI (∼34-210µm, providedby an European/Canadian consortium). Complementary instruments such as afar-IR/sub-millimeter spectrometer(proposed by NASA) are also being discussed.

SPICA will be the only observatory of its era to bridge the far–IR wavelength gap between JWST and ALMA,and carry out unique science not achievable at visible or sub-mm wavelengths. In the mid-IR SPICA will be able tocarry out high-resolution spectroscopy (R∼30,000), one order of magnitude higher than in JWST, and will includespatial high multiplexing imaging and medium spectral resolution capabilities. In addition, the characteristics ofthe SPICA monolithic telescope will provide unique and optimal conditions for mid-IR coronagraphy in imag-ing and, uniquely, spectroscopic mode. According toHerschelfirst results, SPICA will go beyond and improvedrastically our understanding of planetary systems formation and evolution,exoplanet atmospheres and of galaxyevolution through cosmic history.

We will describe the scientific advances that will be made possible by this largeincrease in sensitivity, payingmore attention to Galatic Science. As an example, SPICA will study exoplanetarysystems in detail and make thefirst unbiased survey of the presence of zodiacal clouds in thousands of circumstellar disks around all stellar types.It will allow us to detect both the dust continuum emission and the brightest grain/ice bands as well as the brightestlines from any gas residual (e.g.,water vapor and oxygen). SPICA will have the unique capability to observewaterice in all environments. Besides, SPICA will greatly enhance our knowledge of the “primitive” Solar System bymaking the first detailed characterization of hundreds of Kuiper Belt Objects (studying our own debris disk “objectby object”). SPICA will provide the sensitivity in spectroscopy mode to quantify their composition, and determineunambiguously their size distribution: critical observational evidences forthe models of Solar System formation.SPICA coronagraph will providedirect imaging and low resolution mid–IR spectroscopy of outer young giantexoplanets (e.g.,at∼10 AU of a star at 10 pc), which will allow us to study the physics and composition of their at-mospheres in a wavelength range particularly rich in spectral signatures (e.g.,H2O, CH4, O3, silicate clouds, NH3,CO2). In addition, mid-IRtransit photometry and spectroscopy of “hot Jupiters” will be routine. SPICA willfinally provide an unprecedentedly sensitive window into key aspects of the dust life-cycle both in the Milky Wayand in nearby galaxies, from its formation in evolved stars, its evolution in the ISM, its processing in supernova-generated shock waves and massive stars, to its final incorporation into star forming cores and protoplanetary disks.

SPICA is an international mission and will be open to the worldwide astronomicalcommunity. Japan is incharge of the whole integration of the system. The assessment study on the European contribution to the SPICAproject has been carried out under the framework of the ESA Cosmic Vision 2015-2025 (SPICA Assessment StudyReport for ESA Cosmic Vision 2015-2025 Plan, 2010arXiv1001.0709S). US and Korean participation are also be-ing discussed. The target launch year of SPICA is 2018.

Far-infrared Polarimetry of the ISM

J. E. VAILLANCOURT1,2, R. M. CRUTCHER3, D. T. CHUSS4, J. L. DOTSON2, C. D. DOWELL5,R. H. HILDEBRAND6, M. HOUDE7, T. J. JONES8, M. M. K REJNY8, A. LAZARIAN 9, H.-B. L I10,

L. W. LOONEY3, G. NOVAK11, K. TASSIS5, AND M. W. WERNER5

1 SOFIA Science Center, Universities Space Research Associationjvaillancourt@sofia.usra.edu2 NASA Ames Research Center

3 University of Illinois, Urbana-Champaign4 NASA Goddard Space Flight Center

5 Jet Propulsion Laboratory6 University of Chicago

7 University of Western Ontario8 University of Minnesota9 University of Wisconsin

10 Max-Planck Institute for Astronomy11 Northwestern University

Polarimetry at far-infrared wavelengths is a key tool for studying physical processes on size scales ranging frominterstellar dust grains to entire galaxies (e.g., Vaillancourt et al. 2007). Amulti-wavelength continuum polarimeterat these wavelengths would allow studies of thermal dust polarization in an effort to constrain the grains’ physicalproperties and test grain alignment theory. High spatial resolution (5–30 arcsec) and sensitive observations willmeasure the influence of magnetic fields on infrared cirrus clouds, the envelopes and disks of YSOs (e.g., Krejnyet al. 2009), outflows from both low- and high-mass star forming regions,and the relative strength of magnetic,gravitational, and turbulent effects (e.g., Houde et al. 2010). Large-scale polarization maps will be made possibleby the advent of large-format detector arrays (e.g., Allen et al. 2006; Holland et al. 2006) matched to instrumentswith large focal planes (∼10 arcminutes). Such maps would finally make it feasible to perform statistical tests ofkey theories relating to grain alignment, gas dynamics, and star and galaxy formation (e.g., Falceta-Goncalves,Lazarian, & Kowal 2008).

There are currently no plans in active development for a space-basedobservatory to study polarized far-infraredemission.Herschelhas only limited capabilities for spectral line polarimetry with HIFI (e.g., Harwit etal. 2010),and all ofPlanck’s polarization channels are at wavelengths beyond800 µm. The next best opportunity lies withNASA’s Stratospheric Observatory for Infrared Astronomy (SOFIA1). Here we present a summary of key scienceobjectives that could be pursued with a far-infrared polarimeter on SOFIA operating at wavelengths of 5 – 300µm.References:Allen, C. A., et al. 2006, NIMPA, 559, 522Falceta-Goncalves, D., Lazarian, A., & Kowal, G. 2008, ApJ, 679, 537Harwit, M., et al. 2010, A&A, in preparationHolland, W., et al. 2006, in Proc. SPIE 6275, 62751EHoude, M., Vaillancourt, J. E., Hildebrand, R. H., Chitsazzadeh, S. & Kirby, L. 2009, ApJ,706, 1504Krejny, M., Matthews, T., Novak, G., Cho, J., Li, H., Shinnaga, H., & Vaillancourt, J. E.2009, ApJ. 705, 717Vaillancourt, J. E., et al. 2007, in Proc. SPIE 6678, 66780D

1http://sofia.usra.edu/, http://www.sofia.usra.edu/Science/sciencecases/index.html

The Echelon-cross-Echelle Spectrograph for SOFIA

M. RICHTER1, A. SEIFAHRT1, M. MCKELVEY2, K. ENNICO-SMITH2

1 UC Davis,mjrichter@ucdavis.edu,seifahrt@physics.ucdavis.edu2 NASA Ames Research Center,mark.e.mckelvey@nasa.gov,Kimberly.Ennico@nasa.gov

The Echelon-cross-Echelle Spectrograph (EXES), one of the first generation instruments for the StratosphericObservatory for Infrared Astronomy (SOFIA), will provide a unique tool for examining the ISM and star formation.The EXES high spectral resolution mode, R≤ 100,000, from 4.5 to 28.3µm is designed for molecular lineobservations throughout the various stages of astrophysical chemistry. The improved atmospheric transmissionguaranteed by SOFIA will make observations of gas phase molecules suchas H2O and CH4 routine. EXES willalso have medium and low resolution modes to enable a wide range of science projects. It will use a 10242 pixelSi:As detector array. We are currently testing the system in the laboratory atNASA Ames Research Center. Weplan on two ground-based observing runs to test thoroughly prior to ourfirst scheduled flights on SOFIA in 2013.EXES is a PI instrument open for collaborative proposals, both from the ground and from SOFIA, following themodel of the successful TEXES instrument (Lacy et al. 2002).

An observation of C2H2 gas cell emission usingEXES in the lab. The top panel shows the full 10242

detector at the best spectral focus (R=110,000 at13.7µm). At this setting, the high resolution ordersare smaller than the detector and some features arerecorded in two orders. The line near row 700 marksthe region fit with Gaussians and shown in the lowerpanel. We determine the resolving power from thesefits.

References:Lacy, J.H., Richter, M.J., Greathouse, T.K., Jaffe, D.T., and Zhu, Q. 2002, PASP, 114, 153

GISMO - A 2 millimeter Bolometer Camera for the IRAM 30m Telescope

J. STAGUHN1

1 Johans Hopkins University,johannes.staguhn@nasa.gov

In October 2010, we demonstrated our 2 mm bolometer camera GISMO (the Goddard IRAM Superconducting 2Millimeter Observer) for astronomical observations at the IRAM 30 m Telescope. The camera uses a monolithic8 by 16 Backshort Under Grid (BUG) array with superconducting Transition Edge Sensors (TES). GISMO isdesigned to allow efficient observations of dusty high-z galaxies. Illustrated by astronomical observations, I willdemonstrate the scientific potential of the camera, followed by a discussion ofthe achieved performance. GISMOis expected to become available to the community in 2011.

NOEMA

K.F. SCHUSTER1, R. NERI1, P. COX 1, J. PETY11, F. GUETH1, M. TORRES1, J.L. POLLET1, B. LEFRANC1,AND B. GAUTIER1

1 IRAM Institute for Radio Astronomy in the Millimeter Range, 300 Rue de la Piscine,38406 St Martin d’Heres,France,schuster@iram.fr

2 Institute of Thirdauthor,name3@email.address

NOEMA, theNorthernExtendedM illimeter Array will be a transformational extension of the IRAM Plateau deBure interferometer within the coming years. By doubling the number of antennas and by increasing bandwidthfourfold NOEMA will generate sensitivities in the millimeter wavelength range withinfactors of 3 of those ofALMA for the northern hemisphere. The increase in baseline length will makeNOEMAs angular resolutioncomparable to that of 8m class infrared telescopes. NOEMA will be optimized for millimeter wave surveys andallow for efficient upgrades in the future. The technical concepts and the status of related developments will bedescribed and the scientific drivers and synergy with other facilities will beoutlined.

PosterFirst Session, starting Tuesday, September 21

Session I:Herschel Status and Perspectives including Instruments

P-I-1

In-Flight Calibration of the Herschel/HIFI instrument

M. OLBERG1, C. RISACHER2, D.TEYSSIER3

1 Onsala Space Observatory, SE-439 92 Onsala, Sweden,<michael.olberg@chalmers.se>2 SRON-G, Landleven 12, NL-9700 AV Groningen, The Netherlands,<c.risacher@sron.nl>3 ESAC, ES-28691 Villanueva de la Canada, Madrid, Spain,<dteyssier@sciops.esa.int>

HIFI, the Heterodyne Instrument for the Far-Infrared is the Herschel Space Observatory’s submillimetre highresolution spectrometer. It contains seven separate mixer bands in dual polarization, covering the range from488–1271 GHz and 1430–1901 GHz.

We present results on HIFI in-flight performance based on calibration observations carried out during theperformance verification and routine phase of the Herschel satellite mission. We focus on beam properties, cali-bration accuracy and repeatability. Cross-calibration observations with the ground-based APEX telescope are alsopresented.

Session II:Extreme star formation: high-z, starburst, gal. nuclei

P-II-1

Molecules as Tracers of Galactic Evolution

F. COSTAGLIOLA1, S. AALTO1, M. I. RODRIGUEZ2, S. MULLER1, H. W. W. SPOON3, S. MARTIN4,M. A. PEREZ-TORRES2, A. ALBERDI2, J. E. LINDBERG1,5, F. BATEJAT1, E. JUTTE6, P. VAN DER WERF7,

F. LAHUIS7,8

1 Department of Radio and Space Science, Chalmers University of Technology, Onsala Space Observatory,SE-439 92 Onsala, Sweden,francesco.costagliola@chalmers.se

2 Instituto de Astrofısica de Andalucıa (IAA-CSIC), PO Box 3004, E-18080 Granada, Spain3 Cornell University, Astronomy Department, Ithaca, NY 14853, USA

4 European Southern Observarory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile5 Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster

Voldgade 5-7, 1350 København K, Denmark6 Astronomisches Institut Ruhr-Universitaet Bochum, Universitaetsstr. 150, 44780 Bochum, Germany

7 Leiden Observatory, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands8 SRON Netherlands Institute for Space Research, P.O. Box 800, NL-9700 AV Groningen, The Netherlands

The large luminosities of luminous infrared galaxies (LIRGs) imply that their power source must be either acompact starburst or an AGN, or a combination of both. Because of the large extinction, the inner regions ofLIRGs are precluded from direct investigation at IR and optical wavelengths and the evolution of the activity andthe connection between AGN and starburst are still not well understood.Millimeter observations of moleculartransitions can probe deeper into the gas column and provide valuable information about the chemistry inducedby the central radiation field. Mid–infrared studies suggest that dusty LIRGs may be early evolutionary stages ofAGN and starburst galaxies (Spoon et al., 2007). Here we investigate themolecular gas properties of a sampleof 23 galaxies in order to find, test and calibrate chemical signatures of galaxy evolution and to compare them toIR evolutionary tracers. Data were obtained in 2009 with the new EMIR receiver, mounted on the IRAM 30 mtelescope in Spain. The available bandwidth of nearly 8 GHz at 3 mm, offers the opportunity of achieving very highaccuracy of molecular line ratios. Line ratios of the main molecular species arecombined in diagnostic diagramsand compared with existing models of chemical evolution. We find that PDR (photon-dominated region) and XDR(X-rays dominated region) chemical models can not explain all the properties of the observed molecular emission.A crucial role seems to be played by dense gas distribution and different molecular excitation. The observed brightHC3N emission in HCO+-faint objects may imply that these are not dominated by X-ray chemistry, as suggestedin the literature. Thus we propose that the HCN/HCO+ line ratio is not, by itself, a reliable tracer of XDRs. As anexample of the crucial role played by radiative excitation in extragalactic molecular emission, we report the firstconfirmed extragalactic detection of vibrationally excited HC3N in the LIRG NGC 4418 (Costagliola&Aalto,2010). Vibrational transitions are excited by IR radiation and thus providean indirect probe of the physicalconditions in the obscured nuclear regions. The vibrationally excited transitions can be fit to a temperature of500 K, implying the potential presence of a compact source. The properties of the HC3N emitting gas are similarto those found in Galactic hot cores. The derived large HC3N abundance of 10−7 opens new questions about theability of this large molecule to survive in the presence of strong radiation fields.References:Costagliola, F, Aalto, S., 2010, A&A, 515, A71Spoon, H. W. W.et al., 2007, ApJ, 654, L49-L52

P-II-2

The Warm ISM in the Galactic Center: mid-J CO and Atomic Carbon Lines Observations withthe NANTEN 2 Telescope.

P. GARCIA1, R. SIMON1, J. STUTZKI1, Y. FUKUI2, H. YAMAMOTO2, H. OGAWA3, F. BERTOLDI4,B. KOO5,L. BRONFMAN6, M. BURTON7, AND A. BENZ8

1 I. Physikalisches Institut, Universitat zu Koln, 2 Nagoya University,3 Osaka Prefecture University,4 UniversitatBonn,5 Seoul National University,6 Universidad de Chile,7 University of New South Wales,8 ETH Zurich.

The interstellar medium (ISM) in the few central hundred parsecs of the Galaxy has physical properties that differstrongly from the rest of the ISM in the Galaxy: violent motions in dense high temperature gas, strong magnetic andradiation fields, and a rich chemistry make the Galactic Center (GC) of the Milky Way a unique testbed for studiesof the ISM and star formation under such extrem conditions and a powerful tool in comprehending the physicalprocesses in the nuclei of other galaxies. With the NANTEN 2 radiotelescope and its 16 pixel Sub-Mm Arrayfor Two Frequencies (SMART) we aim to perform systematic Nyquist-sampled (∼ 8.5′′ at 810 GHz) large scalemapping observations from -1◦ < l < 2◦ and from -0◦ .35< b < 0◦ .25 toward the Galactic Center in the carbonmonoxide rotational lines CO(4-3) and CO(7-6), and atomic carbon hyperfine lines CI(1-0) and CI(2-1), to coverall important cooling lines accesible from the ground. Interpretation of these data will be done within frameworkof detailed modeling (excitation and chemistry) including the clumpy structure of the clouds, photon dominatedregions PDRs (in particular the KOSMA-τ PDR model), shocks, and multi-line LVG models. The NANTEN 2Galactic Center survey plays also a complementary role in the HEXGAL projectrelated to the interpretation ofthe Galactic Center data as link to external galaxies nuclei and saving very expensive observation’s time for theHerschel Satellite.

P-II-3

The Zpectrometer: A wideband instrument for detecting and characterizing low-J CO emissionfrom high-redshift galaxies.

A.I. HARRIS1, A.J. BAKER2, C.E. SHARON2

1 Department of Astronomy, University of Maryland, College Park, MD 20742, USAharris@astro.umd.edu

2 Department of Physics and Astronomy, Rutgers, The State University of New Jersey, 136 Frelinghuysen Rd.,Piscataway, NJ 08854, USA,ajbaker@physics.rutgers.edu, csharon@physics.rutgers.edu

The Zpectrometer is a wideband spectrometer optimized for observations of CO J = 1–0 from galaxies atz = 2.2to 3.5 and CO 2–1 fromz = 5.4 to 7.9. These redshift ranges cover peak periods of vigorous star formation,mass assembly, and reionization in the history of the Universe. It operateson the National Radio AstronomyObservatory’s (NRAO’s) 100 meter Green Bank Telescope, with instantaneous bandwidth matched to the facilityKa-band receiver.

We describe the instrument and its operating principles, which pairs the Zpectrometer analog lag cross-correlator and the National Radio Astronomy Observatory’s Ka-band receiver for observations with spectral res-olution well-matched to extragalactic spectroscopy across a 34% instantaneous fractional bandwidth. Such largebandwidth, a factor of a few to ten times larger than typical millimeter-wave spectrometers, enables efficient linesearches that start directly from submillimeter continuum source positions. Identifying line detections in widebandspectra is complicated by system temperature changes across the band, and we discuss and show results from analgorithm that uses time-series as well as spectral information to assess detection probabilities.

P-II-4 An AzTEC/ASTE detection of an ultra-bright submillimeter gala xy in SXDF

S. IKARASHI1, K. KOHNO1, I. ARETXAGA3, H. FURUSAWA4, J. FURUSAWA4, B. HATSUKADE5,D. HUGHES3, D. IONO5, S. JONSON6, K. KAWABE5, H. MATSUHARA7, K. MOTOHARA1, K. NAKAJIMA 8,

K. NAKANISHI 5, K. SCOTT9, K. SHIMASAKU 8, T. TAKAGI 7, T. TAKATA 4,Y. TAMURA5, D. WILNER10, G. WILSON6, M. YUN6

1Institute of Astronomy, University of Tokyo,ikarashi@ioa.s.u-tokyo.ac.jp3Instituto Nacional de Astrofisica,Opitca y Electronica (INAOE)

4National Astronomical Observatory of Japan5Nobeyama Radio Observatory

6Department of Astronomy, University of Massachusetts7Institute of Space and Astronautical Science

8Department of Astronomy, University of Tokyo9Department of Physics and Astronomy, University of Pennsylvania

10Harvard-Smithsonian Center for Astrophysics

We report a detection of an extremely bright submillimeter galaxy (SMG), AzTEC-ASTE- SXDF1100.001(hereafter SXDF1100.001), discovered in 1100µm observations of Subaru/XMM-Newton Deep Field using the144 pixel bolometer camera AzTEC mounted on ASTE 10 m dish. SubsequentCARMA 1300µm and SMA 880µm observations successfully confirm the AzTEC/ASTE detection. This is one of the brightest SMGs known todate; its flux density is 33.9 0.78 mJy at 1100µm and 72.6 2.2 16.2 mJy at 880µm, which is already comparableto or brighter than known Submillimeter-bright high-z quasars such as Cloverleaf. CSO 10m telescope equippedwith Z-Spec, a single-beam grating spectrometer which disperses the 190 380 GHz (1570 970µm) band acrossa linear array of 160 bolometers, has also been used to make a blind searchfor redshifted molecular/atomic linesand continuum emission.

We find that SXDF1100.001 is spatially resolved and seems to have two components, i.e., an extended structure(FWHM of ∼ 4′′) and a compact unresolved one, based on the analysis of the visibility amplitude as a function ofthe projected baseline length in both SMA and CARMA data . About a half of thetotal millimeter/submillimeterflux is originated from the extended component. The discovery of the extended submm/mm bright component issurprising because such an extended bright structure has never seen in the previously studied SMGs, which showa median source size of0′′.4. Multi-wavelengths counterparts are identified at the CARMA/SMA position fromdeep optical (Subaru), near-infrared (UKIRT), mid-infrared (Spitzer), and radio (VLA 20 cm) images. The derivedspectral energy distribution (SED) at optical/NIR wavelengths of SXDF1100.001 clearly indicates a redshift of∼1.4, whereas the measured SED at submillimeter/millimeter to radio, obtained with SMA,CARMA, Z-Spec, andVLA, indicates a redshift ofz > 3. The derived upper limit of the line-to-continuum (L-to-C) flux ratio,∼ 0.10.3, for a wavelength range of 970µm 1400µm is also consistent with a redshift of∼ 3 5, because such a smallline-to-continuum ratio can be expected for very higher order CO rotational lines (9 < J < 16), which must be inthe Z-Spec coverage ifz ∼ 3−5, due to subthermal excitations of these very high-J CO lines in general conditionsof ISM. A possible explanation of this discrepancy can be understood if we are observing an optically dark SMGlying at z > 3 with a foreground galaxy aroundz ∼ 1.4. In fact, we find a positional offset of∼ 0′′.2 − 0′′.6between sub/mm/radio peaks and optical peak, implying a possible overlap of two objects along the line of sightby chance.

If the millimeter/submillimeter bright component of SXDF1100.001 is indeed lying atz ∼ 4, the deduced FIRluminosity (LFIR and star formation rate (SFR) will be∼ 4.5 × 1013L⊙ and 7800M⊙ yr−1, respectively, if thehugeLFIR is originated from massive starburst. The surface densities ofLFIR and SFR,ΣLFIR

andΣSFR, of theunresolved compact component are similar to those of local ULIRGs cores, i.e., close to the theoretically expectedmaxmum value imposed by Eddington limit. On the other hand,ΣLFIR

andΣSFR of the extended component arerather comparable to disk regions of local gas rich spirals, although the origin of the extended structure is stillunexplored.

P-II-5

Disentangling star-formation and accretion at high redshift in a MAMBO deep field

B. L INDNER1, A. BAKER2, A. OMONT3, A. BEELEN4, R. IVISON5, C. LONSDALE6, F. OWEN7, F.BERTOLDI8, H. DOLE9, N. FIOLET10, A. HARRIS11, D. LUTZ12, M. POLLETTA13

1 Rutgers - USA,lindner@physics.rutgers.edu 2 Rutgers - USA,ajbaker@physics.rutgers.edu 3 IAP - France,omont@iap.fr 4 IAS - France,

alexandre.beelen@ias.u-psud.fr 5 ROE - UK,rji@roe.ac.uk 6 NRAO - USA,clonsdal@nrao.edu 7 NRAO - USA,fowen@nrao.edu 8 Uni Bonn - Germany,

bertoldi@astro.uni-bonn.de 9 IAS - France,Herve.Dole@ias.u-psud.fr 10 IAP - France,fiolet@iap.fr 11 Maryland - USA,harris@astro.umd.edu 12 MPE - Germany,

lutz@mpe.mpg.de 13 Milan - Italy, polletta@lambrate.inaf.it

The large numbers of submillimeter galaxies discovered by blank field surveys (e.g., Smail et al. 1997, Hugheset al. 1998) revealed an important phase in galaxy evolution involving rapidstar-formation and rapid black holegrowth. Identifying the relative contributions of star-formation and accretion to the bolometeric luminosity is im-portant for identifying their low-redshift descendants and constructinga self-consistent model of galaxy formationand evolution.

To help disentangle these bolometeric contributions from star-formation and accretion, we have used the MaxPlanck Millimeter Bolometer (MAMBO) array at the IRAM 30 meter telescope to map the innermost 400 squarearcminutes of the 1046+59 field of theSpitzerWide-area InfraRed Extragalactic (SWIRE: Lonsdale et al. 2003)survey to a depth of 1 mJy rms at 1.2mm. Our supplementary data in the 1046+59 field include the deepest 20cmVLA map ever made (2.7µJy/beam rms: Owen & Morrison 2008) as well as deepChandra(Polletta et al. 2006)andSpitzer/MIPS (Fiolet et al. 2009) imaging. These diverse data allow us to performstacking analyses at 1.2mmon the radio, X-ray, and infrared sources in the field. With a depth of 1 mJyrms we are able to stack on subsets ofeach population as a function of size, redshift, flux density, or color andstill retain multiple statistically significantbins for each parameter. Stacking within a source population as well as making comparisons of the mean 1.2 mmflux densities between source populations allows us to identify the mechanism behind the bolometric power ofthese high-redshift ultraluminous infrared galaxy populations.References:Fiolet, N., et al. 2009, A&A, 508, 1, 117Hughes, D. H., et al. 1998, Nature, 394, 241Lonsdale, C.J., et al. 2003, PASP, 115, 897Owen, F. N. & Morrison, J. E. 2008, AJ, 136, 1889Polletta, M., et al. 2006, ApJ, 642, 2, 673Smail, I., Ivison, R. J., Blain, A. W., 1997, ApJ, 490, L5

P-II-6

Characterizing the Molecular ISM in Extreme Star-Formation Environments: a Starburst (M82)and a ULIRG (Arp 220)

N. RANGWALA 1, A. RYKALA 2, J. GLENN1, C. WILSON3, K. ISAAK4, P. PANUZZO5 AND SAG-2 TEAM

1 University of Colorado (USA),naseem.rangwala@colorado.edu2 Cardiff University (UK)

3 McMaster University (Canada)4 ESA Astrophysics Missions Division, ESTEC (Netherlands)

5 CEA (France)

We will present spectroscopic observations (195 – 670µm) of a nearby starburst galaxy M82 and a localULIRG Arp 220, measured using the Spectral and Photometric Imaging Receiver (SPIRE) on the Herschel SpaceObservatory. The spectrum of M82 is dominated by the CO rotational line ladder from J = 4-3 to J = 13-12. Incontrast, the Arp 220 spectrum shows a strong water emission line ladder in addition to a CO ladder of compa-rable total luminosity. We also detect molecular ion lines such as CH+ and OH+ lines, which were previouslyunobserved in an extragalactic source. We will present these observations, and results from the radiative transfermodeling of the CO lines. CO rotational lines are excellent probes of excitationconditions and physical propertiesof the molecular gas. The high-J CO lines have been observed for the first time, and put strong constraints on themodels indicating a very warm molecular gas component in the ISM of the two galaxies.

P-II-7

Evolutionary Models of Infrared Galaxy Spectra

D.J. O’ROURKE1, D.C. FORD1, S. SHABALA 2 AND P. ALEXANDER1

1 MRAO, Cavendish Laboratory, Univeristy of Cambridge,d.o’rourke@mrao.cam.ac.uk,d.ford@mrao.cam.ac.uk,p.alexander@mrao.cam.ac.uk

2 Department of Physics, Univeristy of Oxford,stanislav.shabala@new.ox.ac.uk

We use the galaxy model of Shabala et al. (2009) to predict the star formation histories for a range of halo masses.From this and the mass loss yields predicted by theSTARBURST99 package (Leitherer et al. 1999) we follow thechemical evolution of the ISM and hence determine the dust masses present.The dust is distributed between starforming regions and the diffuse ISM in a way consistent with the galaxy model,by considering the star formationefficiency of the molecular clouds. Input stellar spectra to be processedthrough a radiative transfer model areproduced by convolving the star formation histories withSTARBURST99 spectra.

We use the dust radiative transfer model presented in Ford et al. 2008.In the computational trade off betweenthe complex geometrical distribution of dust and stars and the detailed dust grain energetics, this model simplifiesthe geometry in order to utilise the latest dust models as described by Draine and Li (2007). The model has beenvalidated by fitting to IR photometric data fromSpitzerfor a sample of local galaxies and demonstrating that itsuccessfully reproduces star formation rates and dust masses as determined by other techniques.

This enables us to predict the synthetic spectra of a single galaxy to high redshift and determine how it evolves,as shown in the attached figure. When this is done for all halo masses we canpredict luminosity functions for agiven redshift and photometric passband, to compare with observationaldata. The wavelengths and sensitivitiesof the PACS and SPIRE photometric passbands ofHerschelare ideal for conducting this work at higher redshifts,complementing work already done bySpitzerat low redshift.

1e+19

1e+20

1e+21

1e+22

1e+23

1e+24

1e+25

1e+26

1e+27

1e+28

0.1 1 10 100 1000

Lum

inos

ity L

ν / W

Hz-1

Wavelength / µm

z=5.7819915z=4.308629

z=3.1258438z=2.1913595z=1.4519192z=0.859533

z=0.3725165z=0.0

Spectra of a galaxy with a1011M⊙ Halo at redshift zero betweenz = 5.78 & z = 0.0

References:Draine, B. T.; Li, A. 2007, ApJ, 657, 810Ford, D. C.; Nikolic, B.; Alexander, P. 2008, MNRAS, 391, 1176Leitherer, C.; Schaerer, D.; Goldader, J.D.; Delgado R.M.G.; Robert, C.; Kune, D.F.; deMello, D.F.; Devost, D.; Heckman, T.M. 1999, ApJS, 123, 3Shabala, S.; Alexander, P. 2009, ApJ, 699, 525

P-II-8

HerMES (the Herschel Multi-Tiered Extragalactic Survey): high redshift galaxies

I. PEREZ-FOURNON1,2, AND THE HERMES CONSORTIUM

1 Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain,ipf@iac.es1 Departamento de Astrofisica, Unviersidad de La Laguna, Tenerife, Spain,

Approximately 850 hours of SPIRE Guaranteed Time will be used in the high-redshift extragalactic Key ProjectHerMES being carried out with the Herschel Space Observatory. During the Science Demonstration Phase a smallfraction (about 7%) of this time has already been used in observations of the cosmological fieldsGOODS-N,Lockman Hole and Spitzer First Look Survey (FLS) and of the cluster of galaxies Abell 2218. The large numberof detected sources (> 27000, with fluxes at 250 micron larger than 20 mJy) constitute already a high-valuescientific legacy of Herschel allowing a large number of unique investigations of infrared galaxies up to very highredshifts. In this poster we will summarize the main results obtained by the HerMES survey in the followingareas: a) characterization of the Herschel high-redshift galaxy populations using multi-wavelength colours andSED fitting, b) the search for high-redshift candidates in the SDP fields, and c) the properties of HerMES sourceswithout optical counterparts in deep fields.

P-II-9

Submillimeter Array Identification of the Millimeter-selec ted Galaxy SSA22-AzTEC1: AProto-Quasar in a Proto-cluster?

Y. TAMURA1, D. IONO1, D. J. WILNER2, M. KAJISAWA3, D. M. ALEXANDER4, A. CHUNG2, H. EZAWA5, B.HATSUKADE1, T. HAYASHINO3, D. H. HUGHES6, T. ICHIKAWA 3, S. IKARASHI7, R. KAWABE1, K. KOHNO7,

B. D. LEHMER8, Y. MATSUDA4, K. NAKANISHI 5, T. TAKATA 5, Y. K. UCHIMOTO7, G. W. WILSON9, T.YAMADA 3, AND M. S. YUN9

1 Nobeyama Radio Observatory, Japan.yoichi.tamura@nao.ac.jp2 Harvard-Smithsonian Center for Astrophysics, US.

3 Tohoku University, Japan.4 Durham University, UK.

5 National Astronomical Observatory, Japan.6 Instituto Nacional de Astrofisica, Optica y Electronica, Mexico.

7 The University of Tokyo, Japan.8 The Johns Hopkins University, US.9 University of Massachusetts, US.

We present results from Submillimeter Array (SMA) 860-µm sub-arcsec astrometry and multi-wavelength obser-vations of the brightest millimeter (S1.1mm = 8.4 mJy) source, SSA22-AzTEC1, found near the core of the SSA22proto-cluster that is traced by Lyα emitting galaxies atz = 3.09. We identified a 860-µm counterpart with a fluxdensity ofS860µm = 12.2 ± 2.3 mJy and absolute positional accuracy that is better than0.3′′. At the SMA posi-tion, we found radio to mid-infrared counterparts, whilst no object was found in Subaru optical and near-infrareddeep images at wavelengths≤ 1 µm (J > 25.4 in AB, 2σ). The photometric redshift estimate, using flux den-sities at≥ 24 µm, indicateszphoto ≃ 3.23+0.23

−0.16, consistent with the proto-cluster redshift. We then model thenear-to-mid-infrared spectral energy distribution (SED) of SSA22-AzTEC1, and find that the SED requires largeextinction (AV ≈ 3 mag) of starlight from a young stellar component withMstar ∼ 1010.9M⊙, assumingz = 3.1.Additionally, we find a significant X-ray counterpart with a very hard spectrum (Γeff = −0.34+0.57

−0.61), stronglysuggesting that SSA22-AzTEC1 harbors a luminous AGN (LX ≈ 3 × 1044 erg s−1) behind a large hydrogen col-umn (NH ∼ 1024 cm−2). The AGN, however, is responsible for only∼ 10% of the bolometric luminosity of thehost galaxy, and therefore the star-formation activity likely dominates the submillimeter emission. It is possiblethat SSA22-AzTEC1 is the first example of a proto-quasar growing at thebottom of the gravitational potentialunderlying the SSA22 proto-cluster.

P-II-10

The role of radiation pressure in the dynamics of HII regions at redshift z > 1

S. VERDOLINI1, M. R. KRUMHOLZ2, AND A. G. G. M. TIELENS1

1 Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands,verdolini@strw.leidenuniv.nl,tielens@strw.leidenuniv.nl

2 Department of Astronomy & Astrophysics, University of California, SantaCruz, CA 95064, USAkrumholz@ucolick.org

Observations of starburst galaxy at high redshift hint that the ionizationparameter atz ∼ 2 is higher than in thelocal universe. Following Krumholz & Matzner (2009), a physical explanation of a higher ionization parametercan be a radiation pressure-dominated HII region. I will determine the validityof this hypothesis by using the linecharacteristics for HII regions in the radiation pressure regime.References:Liu, X., Shapley, A. E., Coil, A. L., Brinchmann, J., Ma, C. 2008, ApJ, 678, 758Krumholz, M. R., Matzner, C. D. 2009, ApJ, 703, 1352

Session III:SF in disk galaxies: morphology, structure, and dynamics

P-III-1

WISE and the Dusty Universe

D. J. BENFORD1 FOR THEWISE SCIENCE TEAM

1 NASA/GSFC,dominic.benford@nasa.gov

The Wide-field Infrared Survey Explorer (WISE) is a medium class Explorer mission that was launched on 14Dec 2009. WISE should detect hundreds of millions of stars and galaxies,including millions of ULIRGS andQSOs; hundreds of thousands of asteroids; and hundreds of cold brown dwarfs. The telescope cover was ejectedon 29 Dec 2009, and the all-sky survey started on 14 Jan 2010. WISE takes more the 7000 framesets per day,with each frameset covering 0.6 square degrees in four bands centered at 3.4, 4.6, 12 and 22 microns. WISE iswell-suited to the discovery of brown dwarfs, ultraluminous infrared galaxies, and near-Earth objects. With anangular resolution of 6 arcseconds at 12 microns, a 5σ point-source sensitivity of around 1 mJy at 12 microns and6 mJy at 22 microns, and coverage of over 99% of the sky, WISE also provides a powerful database for the studyof the dusty ISM in our own galaxy. A preliminary release of WISE data will bemade available to the community6 months after the end of the cryogenic survey, or about May 2011. Thefinal data release will be 11 months later,about April 2012.

P-III-2

On the Spatial Distribution of Far-Infrared Sources in the Galactic Plane

N. BILLOT1, AND THE HIGAL TEAM

1 NASA Herschel Science Center - IPAC/Caltech,nbillot@ipac.caltech.edu

The Hi-GAL Open Time Key Program is a survey of the inner Galactic Plane covering over 270 square degrees in5 wavelength bands (Molinari et al., 2010). Thousands of compact sources were extracted from the 2 SDP fieldscentered at l=59 and l=30. We characterize the spatial distribution of thesesources using the Minimum SpanningTree (MST) method. We investigate the correlation between source clustering properties with their intrinsic phys-ical properties - such as mass, luminosity, or evolutionary stage (Elai et al.,2010) - and also with their immediateenvironment (UC HII regions, IRDCs, diffuse ISM). Preliminary resultsfrom our MST analysis has revealed twodifferent populations of objects in the SDP fields: one population of FIR-bright sources (presumably protostars)appears to be grouped in compact clusters around HII regions while the other population of submm-bright objects(cold cores) seems to be distributed in wider and looser groups. Such a difference in spatial distribution could beattributed to events of triggered star formation.

Figure 1: Smooth evolution of the source density maps measured in the 5 bandsof Herschel for the l=30 field.

Figure 2: Minimum Spanning Trees in the 5 Herschel bands for the same field(but with a different conventionfor the direction of increasing Galactic longitude compared to figure 1). Short-wavelength sources are grouped incompact clusters while long-wavelength sources belong to looser groups.

References:Molinari, S., et al., 2010, A&A, in pressElia., D. et al., 2010, A&A, in press

P-III-3

The effects of star formation on the low-metallicity ISMseen with the Herschel/PACS spectrometer

D.CORMIER1, S.C.MADDEN1

1 Irfu/Service d’Astrophysique, CEA Saclay, 91191 Gif-sur-Yvette, France,diane.cormier@cea.fr,suzanne.madden@cea.fr

We observe key FIR fine-structure cooling lines such as OIII 88mu, CII158mu, and OI 63mu with the Her-schel/PACS spectrometer in several nearby low-metallicity galaxies. We find that the CII is the most extended lineand brighter than the OI 63um, dominating the cooling in the warm neutral medium. Line ratios of OIII/CII andOI/CII are indicators of the density and radiation field in these environments.Comparing our observations withmodels, we are able to derive values for the hydrogen density, the incident radiation field and source structure whenpossible in the different phases of the interstellar medium (notably, the HII region, the PDR/molecular clouds andthe diffuse ionized region). This allows us to study the detailed processes at work. We find that the structure ofthe ISM and the effects of star formation activity on the nearby molecular clouds in low-metallicity galaxies aredramatically different from that in the more metal-rich galaxies.

P-III-4

A Sample of [C II ] Clouds Tracing Dense Clouds in Weak FUV Fields observed by Herschel

JORGEL. PINEDA1, THANGASAMY VELUSAMY, WILLIAM D. LANGER, PAUL F. GOLDSMITH, DI L I ,HAROLD W. YORKE

Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099,USA Jorge.Pineda@jpl.nasa.gov

The [CII ] fine–structure line at 158µm is an excellent tracer of the warm diffuse gas in the ISM and the interfacesbetween molecular clouds and their surrounding atomic and ionized envelopes. Here we present the initial resultsfrom Galactic Observations of Terahertz C+ (GOT C+), a Herschel Key Project devoted to study the [CII ] finestructure emission in the galactic plane using the HIFI instrument. We use the [CII ] emission together withobservations of CO as a probe to understand the effects of newly–formed stars on their interstellar environmentand characterize the physical and chemical state of the star-forming gas.We collected data along 16 lines–of–sight passing near star forming regions in the inner Galaxy near longitudes330⊙ and 20⊙. We identify fifty-eight[C II ] components that are associated with high–column density molecular clouds astraced by13CO emission. Wecombine [CII ], 12CO, and13CO observations to derive the physical conditions of the [CII ]–emitting regions inour sample of high–column density clouds based on comparison with results from a grid of Photon DominatedRegion (PDR) models. From this unbiased sample, our results suggest thatmost of [CII ] emission originates fromclouds with H2 volume densities between103.5 and105.5 cm−3 and weak FUV strength (χ0 = 1 − 10). We findtwo regions where our analysis suggests high densities> 105 cm−3 and strong FUV fields (χ0 = 104 − 106),likely associated with massive star formation. We suggest that [CII ] emission in conjunction with CO isotopes is agood tool to differentiate between regions of massive star formation (high densities/strong FUV fields) and regionsthat are distant from massive stars (lower densities/weaker FUV fields) along the line–of–sight. This research wasconducted at the Jet Propulsion Laboratory, California Institute of Technology under contract with the NationalAeronautics and Space Administration.

P-III-5

Detecting spiral arm clouds by CH absorption lines

SHENG-L I QIN1

1 I. Physikalisches Institut, Universitat zu Koln,qin@ph1.uni-koeln.de

We have observed CH absorption lines against Sgr B2(M) using the Herschel/HIFI instrument. With the highspectral resolution and large velocity coverage provided by HIFI, 32 CH absorption features with different radialvelocities and line widths are detected and identified. The constant abundance in spiral arm clouds, suggestingthat CH is a good tracer of H2. The observations have shown that each ’spiral arm’ harbors multiple velocitycomponents, suggesting that clouds are not uniform, and have internal structure. This line-of-sight through almostthe entire Galaxy offers unique possibilities of studying the basic chemistry ofsimple molecules in diffuse andtranslucent clouds, as a variety of different cloud classes are sampledsimultaneously.

P-III-6

Tracers of star-formation in nearby Galaxies. NGC253 and NGC4945 1/,mm surveys with theAPEX telescope.

M. A. REQUENA TORRES1, R. GUESTEN1, J. MARTIN-PINTADO2 AND A. WEISS1

1 Max-Planck-Institute fuer Radioastronomie,mrequena@mpifr.de,rguesten@mpifr.de,aweiss@mpifr.de

2 CAB-INTA-CSIC,jmartin.pintado@iem.cfmac.csic.es

Spectral surveys provide the only way to determine the full molecular inventory of an object and hence build acomprehensive view of the state of the molecular gas and its role in star formation and the structure and evolutionof the ISM. Of course spectral surveys also provide the most efficientmethod of identifying new and unexpectedspecies. The most extensive and complete survey of an extragalactic system has been the continuous spectral sur-vey from 129 GHz to 175 GHz carried out by Martın et al. (2006) toward NGC253. This first spectral line surveysat 2 mm towards the prototypical starbursts galaxies NGC253 have shown an unexpected chemical richness.

However a spectral survey of a single atmospheric window suffers a number of limitations. 1) There are specieswhich may not any have transitions in a particular frequency range and sowould be overlooked. 2) Many specieshave only a single transition within the band, limiting the precision with which the columndensity and excitationof the molecule can be determined. 3) The different excitation requirements of the transitions of different specieswithin the band mean that different species are tracing different material, making it difficult to study the chemistryof particular components of the gas.

Our next step has been to extend the extragalactic spectral line survey ofNGC253 to higher frequencies andto carry out the first spectral line survey of an AGN nucleus like NGC4945. Those Surveys allow as to get betterestimates on the physical and chemical characteristics of the two Galaxies, aswell to search for better tracers tostudy the star-formation in those distant objects. The Hesrchel satellite will open as well the possibility to studythe higher excitation transitions of the same molecules that we observe with APEX. If the data arrive we will beable to present the excitation from different e species from the 100 GHz tothe 1.9 THz range.

We will also give an overview of the extragalactic spectral surveys that have been and are going to be observed.

References:Martın, S., Mauersberger, R., Martın-Pintado, J., Henkel, C., Garcıa-Burillo, S. 2006, ApJS., 164, 450

P-III-7 Dust and Stellar Emission of Nearby Galaxies

RAMIN A. SKIBBA 1, CHARLES W. ENGELBRACHT1, ET AL .

1 Steward Observatory, University of Arizona, 933 N. Cherry Avenue, Tucson, AZ 85721, USA,rskibba@as.arizona.edu

We exploit data from the UV to submillimeter wavelengths of a heterogeneous sample of 61 galaxies fromthe Herschel KINGFISH project (Key Insights on Nearby Galaxies: a Far-Infrared Survey with Herschel), toempirically study the emission from stars and dust in these galaxies. We use thespectral energy distributionscomputed by Dale et al. (2007, 2009), using data from GALEX, SDSS (and other optical measurements), 2MASS,Spitzer, SCUBA (when available), as well as new data from Herschel. The addition of Herschel observationsallows us to trace cold dust components invisible to Spitzer, and they reduce our systematic uncertainties relativeto ground-based submillimeter measurements.

We estimate the dust and stellar emission of these galaxies, in a way that is as empirical and model-independentas possible, and we use these to estimate the ratio of dust-to-stellar emission. Wealso estimate dust and stellarmasses, which are more physical quantities. The dust-to-stellar ratios can be compared to dust-to-gas ratios deter-mined from SED models, and yield important information about the properties ofthe ISM in these galaxies.

We examine how our dust-to-stellar ratios correlate with various galaxy properties: total infrared luminosity,dust mass, morphology, metallicity, and star formation rate. Finally, for a few well-resolved galaxies, such asM101, we plan to use Herschel observations to study the spatial variationsof the dust-to-stellar ratio within thegalaxies. The combination of information from such a wide range of wavelengths gives us a much more completepicture about the evolution of the interstellar medium within galaxies, and our results have important implicationsfor models of galaxy evolution.

Dust-to-stellar emission ratio (esti-mated from SEDs) versus dust mass(Draine & Li 2007 calibration). Red,green, and blue points indicate early-type, spiral, and later-type galaxies,respectively. Some of the early-typegalaxies that have large dust-to-stellarratios, but not correspondingly largedust masses, may have dust heated byrecent starbursts.

References:Dale, D. A., et al., 2007, ApJ, 655, 863Dale, D. A., et al., 2009, ApJ, 703, 517Draine, B. T., Li, A., 2007, ApJ, 657, 810Kennicutt, R. C., et al., 2003, PASP, 115, 928

P-III-8

3D decomposition of the dust emission in the Hi-GAL SDP fields

A. TRAFICANTE1, R. PALADINI 2, A. NORIEGA-CRESPO2, S. MOLINARI3 AND P. NATOLI1

1 Dipartimento di Fisica, Universita di Roma 2 ”Tor Vergata”, Rome, Italyalessio.traficante@roma2.infn.it

paolo.natoli@roma2.infn.it2 Spitzer Science Center, California Institute of Technology, Pasadena, CA paladini@ipac.caltech.edu

alberto@ipac.caltech.edu3 INAF-Istituto Fisica Spazio Interplanetario, I-00133 Rome. Italymolinari@ifsi-roma.inaf.it

Observing the inner Galactic Plane with both the PACS and SPIRE instruments, the Hi-GAL survey is providinga map of the infrared emission of the region between−60◦ < l < 60◦ and−1◦ < b < 1◦ with unprecedentedresolution and sensitivity, in an unique wavelengths domain, between70µm to 500µm. We study the dust prop-erties in the Hi-GAL fields observed during the Herschel Science Demonstration Phase and centered atl = 30◦

andl = 59◦. Using ancillary HI and CO data, we apply the inversion technique described in [Paladini et al. 2007]in order to spatially decompose the dust emission associated with different phases of the gas. In particular, weoptimize the decomposition to the angular resolution of the Hi-GAL survey and obtain temperature and spectralemissivity indeces on sub-kpc scales.References:Molinari, S. and the Hi-GAL consortium, 2010, PASP, 122, 314-325Paladini, R., Montier, L., Giard, M. et al., 2007, A&A, 465, 839-854

P-III-9

Molecular Gas and Star Formation in Barred Spiral Galaxy NGC 3627

Y. WATANABE1,2, K. SORAI1, N. KUNO3 AND T. TOSAKI 4

1 Hokkaido University,nabe@taurus.phys.s.u-tokyo.ac.jp2 The University of Tokyo3 Nobeyama Radio Observatory, National Astronomical Observatory of Japan4 Joetsu

University of Education

Barred spiral galaxies are one of ideal sources for studying the relation between star formation on small scales andkpc-scale galactic gas dynamics and gas kinematics. To better understand star formation under kpc-scale motionin a galaxy, it is crucial to investigate physical property of molecular gas that is raw material of stars. In this posterwe will present our results of13CO(J = 1−0) and12CO(J = 3−2) observation of the nearby barred spiral galaxyNGC 3627 with the Nobeyama 45 m telescope and the Atacama Submillimeter Telescope Experiment (ASTE).

We found that star formation efficiency (SFE) derived from Hα, mid-IR 24 µm and 13CO(1 − 0) data(SFE(12CO)) in the bar was comparable to that in the spiral arms. It have been thought that SFE in the barregion have been lower than that in the spiral arms due to strong shock wave and shear motion induced by non-circular motion of molecular gas (e.g. Athanassoula 1992, Sheth et al. 2000). In NGC 3627, SFE derived from12CO(1−0) data (SFE(12CO)) was also lower in the bar than in the spiral arms. This contradictory result was dueto the fact that averaged12CO(1− 0)/13CO(1− 0) ratios (R12/13) was 1.3 times higher in a bar (R12/13 ∼20) thanin spiral arms and bar ends (R12/13 ∼15). Therefore we supposed to overestimate column density of moleculargas due to higher optical depth of12CO(1 − 0) line than13CO(1 − 0) line.

The bar ends, however, remain to have twice higher SFE than the other regions, even though we use13CO(1−0) to estimate molecular gas mass. We also found that SFE correlated with12CO(J = 3 − 2) / 12CO(J = 1 − 0)ratio, which indicates dense gas fraction, and Toomre Q value was almost unity in the bar ends. With the aboveresults, we supposed that the high SFE in the bar ends is originated from frequent cloud-cloud collision that isinduced by gravitational instability of molecular cloud ensemble.References:Athanassoula 1992, MNRAS, 259, 345Kuno, N. et al. 2007, PASJ, 59, 117Sheth, K. et al. 2000, ApJ, 532, 221

Session IV:Star formation: physical & chemical conditions/feedback

P-IV-1

FIR Fine-Structure Line Mapping the Interstellar Medium of the Galactic Plane withStratospheric Terahertz Observatory (STO)

M. A KYILMAZ 1, C.K. WALKER2, D. HOLLENBACH3, P. BERNASCONI4, M. BORDEN2,M. BRASSE1,P.GOLDSMITH5, U. GRAF1, C. GROPPI2,6, C.E. HONINGH1, K. JACOBS1, M. JUSTEN1, J. KAWAMURA 5, C.

KULESA2, W. LANGER5, D. H. LESSER2,7, C. LISSE4, C. MARTIN7, D. NEUFELD4, P. PUETZ1, M.ROELLIG1, F. SCHOMACKER1, M. SCHULTZ1, G. STACEY8, A. STARK9, M. SHINE2, R. SIMON1, J.

STUTZKI1, H. YORKE5, S. WEINREB10, M. WOLFIRE11, S. WULFF1

1 I. Physikalisches Institut, Universitaet zu Koeln, Koeln, 50937, Germany2 Steward Observatory, University of Arizona, Tucson, AZ, 85721, USA

3 SETI Institute, Mountain View, CA, USA4 John Hopkins University, Applied Physics Lab, Laurel, MD 20707, USA

5 Jet Propulsion Laboratory, Pasadena, CA 91109, USA6 Arizona State University

7 Department of Physics and Astronomy, Oberlin College, Oberlin, OH 44074, USA8 Cornell University

9 Smithsonian Astrophysical Observatory10 California Institute of Technology

11 Department of Astronomy, University of Maryland, College Park, MD 20742, USA

The structure of the interstellar medium, the life cycle of interstellar clouds, andtheir relationship with star forma-tion are processes crucial to deciphering the internal evolution of galaxies. In order to improve our understandingof Galactic structure, formation and destruction of interstellar clouds and theinterplay between the phases of theISM, high resolution spectral line imaging of key gas tracers in the submm- andfar-IR spectral range are needed.The Stratospheric Terahertz Observatory (STO) is a balloon borne 0.8-meter telescope with an 8-beam far-infraredheterodyne spectrometer. The prime goal of the STO is the large scale mapping of the ISM in the important FIRfine structure lines of[CII]158µm and[NII]205µm. The Galactic plane will be surveyed from b= -1 to +1 degreein the latitude and from l= -20 to -55 degrees in longitude with a spatial resolutionof 1′ and a spectral resolutionof sub km/s. These will be complemented by ground based observations of the relevant key tracers. The firstlong-duration Antarctic flight is planned to be carried out in December 2011.

P-IV-2

FIR Line Transfer Including Source Intrinsic Dust Opacities: Upgrading the SphericallySymmetric SimLine Code

M. A KYILMAZ 1, A. GUSDORF2, T. MOELLER1, V. OSSENKOPF1, M. ROELLIG1, J. STUTZKI1, R.SZCZERBA3

1 I. Physikalisches Institut, Universitaet zu Koeln, Koeln, Germany2 MPIfR, Bonn, Germany

3 N. Copernicus Astronomical Center, Torun, Poland

SimLine is a radiative transfer code that computes the excitation and line profiles for a given, spherically symmetriccloud. The cloud structure is specified via the radial dependence of the parameters density, temperature, abundanceand velocity structure. The balance equations for all level populations and energy densities at all radial points aresolved self-consistently. The emergent line profiles observed by a telescope with finite beam width and chosenoffset are computed. Turbulence and clumping effects are treated in a local statistical approximation combinedwith a radial dependence of the correlation parameters. The user has full control over the input parameters and thenumerical control parameters both interactively and via file input.

In this work, we present the upgrades to the SimLine code in order to take intoaccount the IR pumping in thecomputation of the level excitation of the interstellar molecules. The dust properties are introduced to SimLinein a flexible manner which enables the code to treat different material compositions of dust such as multiple dusttypes and dust grain size distribution. Dust opacities and dust compostion are specified compatible to the syntaxdeveloped for R. Szczerba’s dust continuum radiative transfer model (Roellig et al., in prep). This setup allowsto use the upgraded SimLine also to calculate the detailed radiative transfer ofspecies, for which the chemicalabundances and the energy balance of the cloud has been calculated withthe KOSMA-tau spherically symmetricPDR code.

P-IV-3 Assessing Radiation Pressure as a Feedback Mechanism in Star-forming Galaxies

BRETT H. ANDREWS1, TODD A. THOMPSON1, NORMAN MURRAY2, AND ELIOT QUATAERT3

1 The Ohio State University,andrews@astronomy.ohio-state.edu,thompson@astronomy.ohio-state.edu

2 Canadian Institute for Theoretical Astrophysics,murray@cita.utoronto.ca3 The University of California, Berkeley,eliot@astro.berkeley.edu

Radiation pressure from the absorption and scattering of starlight by dust grains may be an important feedbackmechanism in regulating star-forming galaxies. We compile data from the literature on star clusters, star-formingsubregions, normal star-forming galaxies, and starbursts to assess theimportance of radiation pressure on dust asa feedback mechanism. We do so by comparing the luminosity and flux of these systems to their dust Eddingtonlimit: LEdd = 4πGMgc/κF, whereκF is the flux-mean opacity andMg is the total gas mass in the star-formingregion. This exercise motivates a novel interpretation of the Schmidt Law, as well as theLIR − L′

CO and theLIR − L′

HCN correlations. Overall, we find that the Eddington limit sets a hard upper bound to the luminosity ofany star-forming region. Importantly, however, many normal star-forminggalaxies have luminosities significantlybelowLEdd. We focus on the role of “intermittency” in normal spirals — the tendency for only a small numberof subregions within a galaxy to be actively forming stars at any moment because of the time-dependence of thefeedback process and the luminosity evolution of the stellar population (Murray et al. 2010). Finally, we highlightthe importance of observational uncertainties — namely, the dust-to-gas ratioand the CO-to-H2 and HCN-to-H2conversion factors — that must be understood before a definitive assessment of radiation pressure as a globalfeedback mechanism in star-forming galaxies.

Figure 1: Star formation rate surface density as a function of the molecular gas surface density (left) and IRluminosity as a function of HCN line luminosity (right) for star-forming subregions/galaxies (solid circles) and750 pc sub-regions of THINGS galaxies (small dots; Leroy et al. 2008). The line styles show the Eddingtonlimit in different limiting cases: optically thin to the FIR (solid line), optically thin to the FIR accounting forintermittency (dot-dashed line), optically thick to the FIR (shaded region), and optically thick to the FIR with anenhanced dust-to-gas ratio (dashed line). Overall, the Eddington limit suggests that radiation pressure sets an upperbound to theΣ⋆ or theLIR of a star-forming region or galaxy.

References:Leroy, A. K., et al. 2008, AJ, 136, 2782Murray, N., Quataert, E., & Thompson, T. A. 2010, ApJ, 709, 191

P-IV-4

Dust and gas in photodissociation regions observed with Herschel

H. ARAB1, M. COMPIEGNE2, E. HABART1, AND A. A BERGEL1

1 Institut d’Astrophysique Spatiale, UMR 8617, CNRS/Universite Paris-Sud 11, 91405 Orsay, France,heddy.arab@ias.u-psud.fr, emilie.habart@ias.u-psud.fr,

alain.abergel@ias.u-psud.fr2 Canadian Institute for Theoretical Astrophysics, Toronto, Ontario, M5S3H8, Canada,

compiegne@cita.utoronto.ca

In photodissociation regions (PDRs), the physical conditions and the excitation evolve on short spatial scalesas a function of depth within the cloud, providing a unique opportunity to studyhow the dust and gas populationsvary with the excitation and physical conditions.

The Herschel spatial telescope is currently observing several PDRs,enlightening for the first time the far-infrared/sub-millimeter emission of these objects. These new data allow us not only to probe the grains in thermal equilibriumwith the radiation field (photometric observations) but also to study this particlesin their gaseous environment(spectroscopic observations).

By combining the Herschel (SPIRE and PACS) and Spitzer maps, we derive at each position across the PDRsthe full emission spectrum of all dust components which we compare to dust and radiative transfer models so as tolearn about the spatial variations in both the excitation conditions and the dustproperties. We present a completemodeling of the dust emission in typical PDRs (e.g., NGC 7023 or the Orion bar)which brings strong constrainson their density profiles and also on their abundance of dust particles andtheir emitting properties. Finally, thespectroscopic data taken with SPIRE are analysed with the ”Meudon” PDR code (le Petit et al. 2006), bringing acoherent view on the heating and cooling of both the dust and gas components.

References:Abergel, A., Arab, H., Compiegne, M., Kirk, J. and the SPIRE ISM consortium 2010,A&A, Herschel special issue, acceptedHabart, E., Dartois, E., Abergel, A., Baluteau, J.-P., Naylor, D., Polehampton, E., Joblin,C. and the SPIRE ISM consortium, 2010, A&A, Herschel special issue, accepted

P-IV-5

An observational study of star formation feedback in Orion

O. BERNE1

1 Leiden Observatory,berne@strw.leidenuniv.nl

Massive stars have strong feedback on their parental molecular clouds. The energy they inject disturbs the previ-ously formed structures, and sets the initial conditions for the formation of a new generation of low mass stars.In this contribution, we will present the results of a IRAM 30m one square degree high spectral/spatial resolutionsurvey of the Orion molecular cloud in12CO (2-1) and13CO (2-1), combined to archival mid-infrared Spitzerobservations. The combination of molecular data, tracing the velocity structure of the cloud, to infrared data,tracing cloud boundaries and protostars provides a complete picture of thedynamics of the region. Our analysisprovides direct evidence of hydrodynamical instabilities driven by the expansion of the HII region. The statisticalanalysis, using 4 point velocity increment, evidences the highly turbulent nature of the cloud. The connectionbetween filamentary structures and star-formation is also investigated. We willdiscuss how these results improveour understanding of the evolution of the Orion nebula, and how this relatesto what is known on star formationfeedback, in particular to the light of the new Herschel results.

P-IV-6

Multiple Molecular Line Mapping of the Central Molecular Zone at 3 a nd 7mm

M ICHAEL BURTON1 AND PAUL JONES1,2

1 University of New South Walesm.burton@unsw.edu.au, pjones@phys.unsw.edu.au2 Universidad de Chile

The Central Molecular Zone (the CMZ) resides in the inner 3 degrees of the Galaxy, home to∼ 5% of its totalmolecular content. A rich variety of organic molecules are found there, widely spread over several hundred parsecs,a facet which remains unexplained. This organic repository in the galactic centre is a very different environment tothat of the GMCs in the molecular ring. Making use of the Mopra telescope’s ultra-wide bandpass spectrometer,the 8 GHz UNSW–MOPS, a multiple molecular line mapping survey is now possible ofthis unique region. Wehave mapped the CMZ in 18 molecular lines simultaneously in the 86–94 GHz band,and in a further 23 linessimultaneously in the 42–50 GHz band. We report on the early results of this survey, in particular of a pilot studyof the Sgr B2 region of the CMZ.

P-IV-7

Galactic genesis: star formation in the molecular cloud W43

P. CARLHOFF1, P. SCHILKE1, F. MOTTE2 AND Q. NGUYEN LUONG2

1 1. Physikalisches Institut, Universitt zu Kln,carlhoff@ph1.uni-koeln.de,schilke@ph1.uni-koeln.de

2 AIM, Service d’Astrophysique du CEA Saclay,motte@cea.fr, quang.nguyen-luong@cea.fr

We observe the Galactic complex W43 in the 2-1 transitions of13CO and C18O to study the process of giant cloudformation and star formation within. This cloud complex is located at the point where the spiral arm connects tothe Bar of the Milky Way, and therefore is ideally suited to test colliding flow modelsfor molecular cloud for-mation. Large scale maps (≈ 1◦2) are obtained with the HERA-array at the 30m-Telescope in Granada, Spain,which provides high spatial (11′′) and velocity resolution (0.1 km s−1). The maps show a very filamentary struc-ture, which is analyzed through comparison with the Herschel results fromHi-GAL. Our added value consists onvelocity information, so we can determine the velocity structure and velocity widthof the filaments which are alsoseen in the FIR continuum. We obtain opacities, excitation temperatures, column density, masses and energet-ics by comparison of the two CO isotopologues for each cloud and filament in the field, and obtain measures ofturbulence, which are compared between regions of active star formation, and more quiescent regions.

P-IV-8

Molecules as Tracers of Galactic Evolution

F. COSTAGLIOLA1, S. AALTO1, M. I. RODRIGUEZ2, S. MULLER1, H. W. W. SPOON3, S. MARTIN4,M. A. PEREZ-TORRES2, A. ALBERDI2, J. E. LINDBERG1,5, F. BATEJAT1, E. JUTTE6, P. VAN DER WERF7,

F. LAHUIS7,8

1 Department of Radio and Space Science, Chalmers University of Technology, Onsala Space Observatory,SE-439 92 Onsala, Sweden,francesco.costagliola@chalmers.se

2 Instituto de Astrofısica de Andalucıa (IAA-CSIC), PO Box 3004, E-18080 Granada, Spain3 Cornell University, Astronomy Department, Ithaca, NY 14853, USA

4 European Southern Observarory, Alonso de Cordova 3107, Vitacura, Casilla 19001, Santiago 19, Chile5 Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, Øster

Voldgade 5-7, 1350 København K, Denmark6 Astronomisches Institut Ruhr-Universitaet Bochum, Universitaetsstr. 150, 44780 Bochum, Germany

7 Leiden Observatory, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands8 SRON Netherlands Institute for Space Research, P.O. Box 800, NL-9700 AV Groningen, The Netherlands

The large luminosities of luminous infrared galaxies (LIRGs) imply that their power source must be either acompact starburst or an AGN, or a combination of both. Because of the large extinction, the inner regions ofLIRGs are precluded from direct investigation at IR and optical wavelengths and the evolution of the activity andthe connection between AGN and starburst are still not well understood.Millimeter observations of moleculartransitions can probe deeper into the gas column and provide valuable information about the chemistry inducedby the central radiation field. Mid–infrared studies suggest that dusty LIRGs may be early evolutionary stages ofAGN and starburst galaxies (Spoon et al., 2007). Here we investigate themolecular gas properties of a sampleof 23 galaxies in order to find, test and calibrate chemical signatures of galaxy evolution and to compare them toIR evolutionary tracers. Data were obtained in 2009 with the new EMIR receiver, mounted on the IRAM 30 mtelescope in Spain. The available bandwidth of nearly 8 GHz at 3 mm, offers the opportunity of achieving very highaccuracy of molecular line ratios. Line ratios of the main molecular species arecombined in diagnostic diagramsand compared with existing models of chemical evolution. We find that PDR (photon-dominated region) and XDR(X-rays dominated region) chemical models can not explain all the properties of the observed molecular emission.A crucial role seems to be played by dense gas distribution and different molecular excitation. The observed brightHC3N emission in HCO+-faint objects may imply that these are not dominated by X-ray chemistry, as suggestedin the literature. Thus we propose that the HCN/HCO+ line ratio is not, by itself, a reliable tracer of XDRs. As anexample of the crucial role played by radiative excitation in extragalactic molecular emission, we report the firstconfirmed extragalactic detection of vibrationally excited HC3N in the LIRG NGC 4418 (Costagliola&Aalto,2010). Vibrational transitions are excited by IR radiation and thus providean indirect probe of the physicalconditions in the obscured nuclear regions. The vibrationally excited transitions can be fit to a temperature of500 K, implying the potential presence of a compact source. The properties of the HC3N emitting gas are similarto those found in Galactic hot cores. The derived large HC3N abundance of 10−7 opens new questions about theability of this large molecule to survive in the presence of strong radiation fields.References:Costagliola, F, Aalto, S., 2010, A&A, 515, A71Spoon, H. W. W.et al., 2007, ApJ, 654, L49-L52

P-IV-9

Herschel observations of EXtra-Ordinary Sources: The Terahertz spectrum of Orion KL seen athigh spectral resolution

NATHAN ROBERT CROCKETT1

1 University of Michigan,ncrocket@umich.edu

We present Herschel/HIFI spectra of the Orion KL hot core region in thefrequency range 1425.9 - 1906.8 GHz(bands 6/7) at high spectral resolution. These observations, unavailable from ground based observatories becauseof atmospheric absorption, represent a dramatic improvement in sensitivity and spectral/spatial resolution overprevious space based spectra obtained at these frequencies by ISO (Lerate et al. 2006). In this work, we continueto characterize the THz spectrum of Orion KL first reported by Crockettet al. 2010. We find that the spectrumis dominated by strong lines of CO, H2O, OH, CH3OH, H2S, HCN, and NH3. These molecules trace severalcomponents associated with Orion KL (e.g. the hot core and compact ridge). We also observe a diminisheddensity in observed lines at THz frequencies when compared to lower frequency HIFI bands. We offer severalexplanations for this effect.

P-IV-10

Clumpy PDR modelling of the Orion Bar region

M. CUBICK1, J. STUTZKI1, M. ROLLIG1, AND V. OSSENKOPF1,2

1 I. Physikalisches Institut, Universitat zu Koln, Zulpicher Straße 77, 50937 Koln,cubick@ph1.uni-koeln.de

2 SRON, Postbus 800, 9700 AV Groningen, Netherlands

Observations of the interstellar medium (ISM) reveal structure on all scales. Quantification of the structure bydecomposition of the observed intensity distributions into clumps results in powerlaw distributions of the clumpnumber and size versus clump mass (e.g. Heithausen et al.1998). This has been shown to be consistent with afractal structure of the observed clump distributions (Stutzki et al. 1998). The conclusion of this result is a surfacedominated structure of the ISM. The stellar UV-radiation penetrating the Galactic ISM in consequence dominatesits physical and chemical conditions. Thus the bulge of the ISM can be identified as photon dominated regions(PDRs) (Hollenbach & Tielens 1999).

FIR observations of transition lines of CO,13CO, C, C+, O, HCO+, CS, and SO are extracted from theliterature along a stripe over the Orion Bar (see e.g. Hogerheijde et al. 1995).

They are compared with clump ensemble emissions from the KOSMA-τ PDR-model, which has already beenapplied on the COBE data of the Galactic disk by Cubick et al. (2008). The observational data, stemming froma large variety of different telescopes and receivers, are comparedwith the model results taking the observationalbeam size into account. The inconsistent velocity range of the integrated intensities given in the different referencesintroduce some additional uncertainty to be taken into account. For the model calculations the FUV flux, averagegas volume density, and average ensemble clump density distributions as well as the clump mass limits of theensemble has been varied to investigate the influence on the model results andto describe the observed intensitydistribution best.

The actual model results on the clumpy PDR contribution to the observed emission from the Orion Bar regionare presented and discussed.References:Cubick, M., Stutzki, J., Ossenkopf, V., Kramer, C., & Rollig, M., 2008, A&A, 488, 623Hogerheijde, M. R., Jansen, D. J., & van Dishoeck, E. F., 1995, A&A, 294, 792Hollenbach, D. J., & Tielens, A. G. G. M., 1999, Reviews of Modern Physics, 71, 173Stutzki, J., Bensch, F., Heithausen, A., Ossenkopf , V., & Zielinsky, M., 1998, A&A, 336,697

P-IV-11

The reliability of CII as a star formation tracer.

DE LOOZE I.1, BAES M. 1, FRITZ J. 1BENDO G. J.2 AND CORTESEL. 3

1 Sterrenkundig Observatorium, Universiteit Gent, Krijgslaan 281 S9, 9000 Ghent, BelgiumDe Looze I.@ilse.delooze@ugent.be, Baes M.@ maarten.baes@ugent.be, Fritz J. @

jacopo.fritz@ugent.be2 Astrophysics Group, Imperial College London, Blackett Laboratory, Prince Consort Road, London SW7 2AZ,

UK , Bendo G. J. @ g.bendo@imperial.ac.uk3 Department of Physics and Astronomy, Cardiff University, The Parade, Cardiff, CF24 3AA, UK,Cortese

L. @ Luca.Cortese@astro.cf.ac.uk

The [CII] line at 158µm is generally a very strong line in all star forming galaxies. The Herschel satellite iscurrently making [CII] observations; a readily available tool to study the ISM of nearby galaxies. The adventof ALMA will make this line observable at high redshifts. In order to examine the reliability of [CII] as a starformation indicator, we calibrate the [CII]-SFR relation in the nearby universe against GALEX FUV and MIPS 24µm luminosities, which are ideal tracers of the unobscured and dust-enshrouded star formation, respectively. Incase of infrared-luminous objects, the [CII] line flux correlates remarkably well with the star formation rate. Asthe contribution from PDR’s to the [CII] line flux declines for more infrared-luminous galaxies, [CII] will mainlytrace the star forming activity in those objects.

P-IV-12

Dynamical processes in the S140 region traced by HIFI [CII] emission

C. DEDES1, B. MOOKERJEA2, Y. OKADA 3, M. ROLLIG3, V. OSSENKOPF3,4, S. BRUDERER1 ,A.O. BENZ1 AND THE WADI KP TEAM

1 ETH Zurich,carolin.dedes@astro.phys.ethz.ch,simonbr@astro.phys.ethz.ch,benz@astro.phys.ethz.ch

2 TIFR,bhaswati@tifr.res.in3 Universitat zu Koln,

okada@ph1.uni-koeln.de,roellig@ph1.uni-koeln.de,ossk@ph1.uni-koeln.de4 SRON

We report the observation of [CII] emission in a cut through the S140 region together with single pointing ob-servations of several molecular tracers in key regions of the photon-dominated region (PDR) and molecular cloud.At a distance of 910 pc, the BOV star HD211880 ionizes the edge of the molecular cloud L1204, creating S140,a visible HII region and PDR (e.g. Crampton and Fisher, 1974). In addition, the dense molecular cloud hosts acluster of embedded massive young stellar objects (YSOs) only 75” from the HII region ( e.g. Beichman et al.,1979; Minchin et al. 1993). Multiple energetic outflows and stellar winds areobserved around the source S140IRS1 (e.g. Weigelt et al. 2002, Hoare 2006). We used HIFI on Herschel to observe [CII] in a strip following thedirection of the impinging radiation across the ionisation front and through thecluster of embedded YSOs. With[CII], which Emery et al. (1996) report to be fairly extended in the S140region, we can trace the ionising radiationand, together with the molecular tracers such as CO isotopologues and HCO+, study the dynamical processes inthe region. Combining HIFIs high spectral resolution data with ground based molecular data allows us to study thedynamics and excitation conditions both in the PDR and the dense molecular cloud, model their physical condi-tions (Rollig et al. 2006) and, together with upcoming PACS observations of major cooling lines, obtain a censusof the energy balance in the region. The study of the [CII] strip has revealed several emitting regions in the densecloud which are related to energetic outflow processes in S140.Observations of numerous other species, in particular light hydrides, provide new information on the chemistry ofthe PDR and the infrared source, revealing significant differences in the spatial distribution of the different species.

References:Crampton, D., Fisher, W. A. 1974, Publ. Dom. Astrophys. Obs, 14 , 283Beichman, C. A.; Becklin, E. E.; Wynn-Williams, C. G. 1979, ApJL, 232, 47Minchin, N. R., White, G. J., Padman, R. 1993, A&A, 277, 595Emery, R., Aannestad, P., Minchin, N., et al. 1996, 315, 285Weigelt, G., Balega, Y. Y., Preibisch, T., Schertl, D., Smith, M. D. 2002, A&A, 381, 905Hoare, M. G. 2006, ApJ, 649, 856Rollig, M., Ossenkopf, V., Jeyakumar, S., Stutzki, J., Sternberg, A. 2006,A&A, 451, 917

P-IV-13

Atmospheric calibration for submillimeter observation

X. GUAN1

1 1. Physikalisches Institut, Universtat zu Koln,guan@ph1.uni-koeln.de

Technological development has made sub-millimeter observations possible withlarge antennas. Almost all largeantennas reside in ground-based observatories. The atmosphere’s rich features at sub-mm wavelengths have greatinfluence over measurements from the ground. Calibration is therefore important for obtaining accurate data. Agood model and its proper application are necessary. We applied (Sun 2008) the ATM model (Pardo et al. 2001)to the KOSMA and NANTEN2 observations across 230 to 810 GHz. Results are obtained and analyzed. Furtherwork is proposed based on the analysis.References:Pardo, J. R., Cernicharo, J., & Serabyn, E., 2001, IEEE Trans. on Antennas and Propaga-tion, 49/12, 1683Sun, K., 2008, Ph.D Thesis, Universtat zu Koln

P-IV-14

Molecular emission in regions of star formation

A. GUSDORF1

1 Max Planck Institut fur Radioastronomie,agusdorf@mpifr-bonn.mpg.de

In this talk I will present results of observations and modelling of the bipolar outflow BHR71.

P-IV-15

Equilibrium states of a recombining plasma heated by a rationfield and dissipation of soundwaves

M. I BANEZ1 AND S. CONDE1

1 Centro de Fısica Fundamental, Universidad de los Andes, Venezuela,ibanez@ula.ve, sconde@ula.ve

The equilibrium resulting in a recombining plasma with arbitrary metallicityZ, and heated by a mean radiationfield E as well as by sound waves dissipation due to thermal conduction, dynamic and bulk viscosity is analyzed.Generally, the heating by acoustic waves dissipation introduces drastic changes in the range of temperature wherethe thermochemical equilibrium may exist. Additional equilibrium states appear which are characterized by a lowerionization and higher gas pressure than those resulting when the wave dissipation is neglected but equilibrium cannot exit for structures smaller than a threshold value. The above effectssensitively depend on the values of thegas parameters as well as the wave length and intensity of the acoustic waves. Observational implications in theinterstellar medium are outlined.

P-IV-16

Anomalous Dust in Late-Type Galaxies

F.P. ISRAEL1

1 Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 Leiden, Netherlands,israel@strw.leidenuniv.nl

Almost all galaxies lack accurate flux density measurements in the millimeter and submillimeter range, which iscrucial for the determination of global free-free emission, a prime star formation indicator, and the amount of colddust, which may dominate the total dust mass of a galaxy and its gas-to-dust ratio. We have studied the few dozenlate-type galaxies with well-established submillimeter SEDs, and in particular the small susbset of galaxies with awell-determined millimeter continuum SED. We have discovered a significant millimeterand submillimeter excessin the Magellanic Clouds, which may also occur in other dwarf galaxies, but isabsent (ultra)luminous infratredgalaxies and more modest starburst galaxies. Emissivities areβ = 1.0-1.7, and do not reach the commonly assumedβ=2. The excess emission is not due to cold dust, but must represent an anomalous emission process. Dist emissionmechanisms at long wavelengths are briefly discussed. There is no good evidence for cold dust in the galaxiesstudied.

P-IV-17 Analysis of CO, density, and temperature distributions in simulated molecular clouds

F. MOLINA1, S. GLOVER1, AND C. FEDERRATH1

1 Zentrum fur Astronomie der Universitat Heidelberg, Institut fur Theoretische Astrophysik, Albert-UeberleStr. 2, 69120 Heidelberg

fmolina@ita.uni-heidelberg.de,sglover@ita.uni-heidelberg.de,chfeder@ita.uni-heidelberg.de

We present the analysis of numerical simulations of molecular clouds in orderto prepare for the comparison oftheoretical predictions with molecular line data from real clouds. The simulations are performed using a fullydynamical 3D model of magnetized turbulence coupled to a chemical network simplified to follow the dominantpathways for CO formation and destruction. At the moment, we have compareddensity and temperature Prob-ability Density Functions (PDFs), as well as CO distributions, for simulations spanning a wide range in density,metallicity and UV field strength. We find only minor differences in the dimensionless density PDFs, but largerdifferences in the temperature PDFs, as can be seen in Figure 1. In gas with lower metallicity, or higher ambientUV radiation field, CO photodissociation is more efficient at destroying CO molecules, making the total abundanceof CO in the cloud smaller. We show that the CO primarly traces cloud material atn > 1000 cm−3 or higher,regardless of the mean cloud density, and therefore can give a misleadingview of the physical conditions in lowdensity and/or low metallicity clouds.

Figure 1: Mass-weighted PDF of gas temperature T at t≃ 5.7 Myrs grouped in panels according to the parametersused for the simulations. In general, the PDFs show a prominent peak at lowtemperatures, corresponding to fullymolecular gas, and a power-law tail extending to high temperatures which is composed of gas with a low effectivevisual extinction. The peak of the PDFs is shifted to higher temperatures forlow metallicities and/or low densities[see panels (a), (b) and (c)]. Comparing panels (b) and (c), we seethat the lower metallicity gas has a systematicallyhigher temperature than the solar metallicity gas. Panel (d) demonstrates that increasing the strength of the UVradiation field leads to a broader temperature distribution, due to more effective CO photodissociation and a higherphotoelectric heating rate.

References:Glover, S. C. O., Federrath, C., Mac Low, M.-M., Klessen, R. S. 2010, MNRAS, 404, 2Molina, F., Glover, S. C. O., Federrath, C., in prep.

P-IV-18

PDR properties and spatial structures probed by Herschel and Spitzer spectroscopy

YOKO OKADA 1, CAROLIN DEDES2, OLIVIER BERNE3, MANUEL GONZALEZ4, CHRISTINE JOBLIN5,6,CARSTEN KRAMER4, VOLKER OSSENKOPF1,7, BHASWATI MOOKERJEA8, MARKUS ROLLIG1

1 I. Physikalisches Institut der Universitat zu Koln,okada@ph1.uni-koeln.de2 Institute for Astronomy, ETH Zurich 3 Leiden Observatory, Universiteit Leiden4 Instituto de Radio Astronomıa

Milim etrica (IRAM) 5 Universite de Toulouse, UPS, CESR6 CNRS7 SRON Netherlands Institute for SpaceResearch8 TIFR

We investigate the photodissociation region (PDR) properties and spatial structures from the combination ofHerschel/HIFI and PACS and Spitzer/IRS observations. Herschel observations were carried out in the frameworkof the WADI (The warm and dense ISM) key program for several sources with a wide range of environments; e.g.S140 with the UV field strength of∼ 150 in Draine field (Spaans & van Dishoeck 1997) and Carina nebula withthat of103–104 (Kramer et al. 2008). They cover key molecular (13CO, C18O, HCO+ etc.), ionic ([CII ] 158µm),and atomic ([OI] 63µm and 145µm) line emissions and allow us the detailed modeling of the PDR properties(Ossenkopf et al. 2010, Dedes et al. 2010). On the other hand, PDRsshow significant features from PAHs andH2 pure rotational emissions in mid-infrared wavelengths, and they also trace physical properties of PDRs suchas the density and UV field (Berne et al. 2009). We compare the derived properties using these different tracersfrom different phases of the PDR stratification; [CII ] 158µm and PAH emissions from outer layers, warm H2 aswell as [OI] emissions fromAV ∼ 2, and molecular line emissions from denser inner layers (Tielens 2005). Wealso investigate possible chemical links between key species in chemical processes and PAHs. The similar spatialresolutions of Herschel and IRS are an advantage to obtain the spatial structures.

References:Berne et al. 2009, ApJ, 706, L160Dedes, C., et al. 2010, in preparationKramer, C., et al. 2008, A&A, 477, 547Ossenkopf, V., et al. 2010, A&A, acceptedSpaans, M., & van Dishoeck, E. F. 1997, A&A, 323, 953Tielens, A. G. G. M. 2005, The Physics and Chemistry of the Interstellar Medium(Cambridge: Cambridge Univ. Press)

P-IV-19

Submillimeter Line Emission from LMC 30 Dor:The Impact of a Starburst on a Low Metallicity Environment

JORGEL.PINEDA1 , NORIZAKU M IZUNO2 , JURGEN STUTZKI3, MARCUSCUBICK3 , CARSTEN. KRAMER4 ,ULRICH KLEIN5 , MONICA RUBIO6

1Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA91109-8099, USA

2 ALMA-J Project Office, National Astronomical Observatory of Japan,2-21-1 Osawa, Mitaka, Tokyo 181-8588,Japan

3 KOSMA, I. Physikalisches Institut, Universitat zu Koln, Zulpicher Straße 77, D-50937 Koln, Germany4 Instituto de Radioastronoma Milimetrica (IRAM), Av. Divina Pastora 7, Local 20, E-18012 Granada, Spain

5 Argelander-Institut fur Astronomie, Auf dem Hugel 71, D-53121 Bonn, Germany6 Departamento de Astronomıa, Universidad de Chile, Casilla 36-D, Santiag o, Chile

The 30 Dor region in the Large Magellanic Cloud (LMC) is the most vigorous star–forming region in the LocalGroup. There, star formation is taking place in low–metallicity molecular gas whichis exposed to an extremefar–ultraviolet (FUV) radiation field powered by the massive compact cluster R136. It is tqherefore ideally suitedto study the conditions at which stars formed at at earlier cosmological times. Carbon carrying species, CO, CIand CII , which originate in the surface layers of molecular clouds illuminated by the FUVradiation of youngstars, can be used to constrain the physical and chemical state of the star–forming ISM. We present high-angularresolution sub-millimeter observations in the 30Dor–10 region in the LMC obtained with the NANTEN2 telescopeof the 12CO J = 4 → 3, J = 7 → 6, and13CO J = 4 → 3 rotational and [CI] 3P1−

3P0 and3P2−3P1 fine-

structure transitions. We derive the physical and chemical properties ofthe low-metallicity molecular gas using anexcitation/radiative transfer code and a self-consistent solution of the chemistry and thermal balance of the gas inthe framework of a clumpy cloud PDR model. We compare the derived properties with those in the N159W regionwhich is exposed to a more moderate far-ultraviolet radiation field compared with 30Dor–10 but have similar gasmetallicity. We also combine our CO detections with previously observed low−J CO transitions to derive the COspectral line energy distribution in 30Dor–10 and N159W. CO lines and the carbon fine structure lines shows thatthe emitting gas in the 30 Dor–10 region has temperatures of about 160 K and densities of about 104cm−3. Wefind that the molecular gas in 30 Dor–10 is warmer and clumpier than in N159W, which might be a result of theeffect of a strong FUV radiation field heating and disrupting the low–metallicity molecular gas. We use a clumpyPDR model (including the [CII ] line intensity reported in the literature) to constrain the FUV intensity and averagedensity of the clump ensemble.This research was conducted at the Jet Propulsion Laboratory, California Instituteof Technology under contract with the National Aeronautics and Space Administration.

P-IV-20 Molecular Tracers of Turbulent Shocks in Giant Molecular Clouds

A. PON1, D. JOHNSTONE2, AND M. J. KAUFMAN3

1 University of Victoria,andypon1@shaw.ca2 NRC-HIA, doug.johnstone@nrc-cnrc.gc.ca

3 San Jose State University,michael.kaufman@sjsu.edu

We are investigating the manner in which energy flows through, into, and outof molecular clouds in order tobetter understand how energy is conserved throughout a cloud’s lifetime. For example, we examine the dissipationof turbulent energy through shocks. Current numerical simulations show that the turbulent energy of a GMCdissipates on the order of a crossing time, but do not explicitly follow how this energy is released. We have runmodels of shocks, appropriate for the conditions inside of a GMC, to determine which species and transitionsdominate the cooling and radiative energy release. Combining these models ofshock emission and estimates forthe rate of turbulent energy dissipation (Basu & Murali 2001), based upon the conditions in nearby molecularclouds, we predict those line emissions that will be observable with currentand upcoming observational facilitiessuch as Herschel, SOFIA and ALMA.

The relative strengths of various CO ro-tational transitions as calculated fromthe shock models of Kaufman andNeufeld (1996). The initial densitiesof the gas and the shock velocities forthe models are given along the top andleft sides of the grid respectively. Eachgrid box has been scaled to the flux ofthe most intense line in that grid boxand the flux of the strongest line andthe total flux of all of the lines com-bined are given, in ergs / s / cm2, inthe top left corner of each box. The ra-tios of the different CO lines can notonly be used to constrain density andvelocity, but they can also be used todifferentiate between shock emissionand emission from PDRs and the am-bient cool gas in molecular clouds. Weare currently planning to extend thesemodels to lower densities and shockvelocities, which are more appropriatefor molecular clouds. Other molecu-lar species, which are not major shockcoolants, can also be easily added intothese models to provide further diag-nostics for the shock conditions.

References:Basu, S. & Murali, C. 2001, ApJ, 551,743Kaufman, M. J. & Neufeld, D. A. 1996, ApJ, 456, 250

P-IV-21

KOSMA τ : Recent Developments in Modeling Photodissociation Regions

M. ROLLIG1, M. CUBICK1, R. SZCZERBA2, V. OSSENKOPF1, 3, M. AKYILMAZ 1, AND J. STUTZKI1

1 I. Physikalisches Institut der Universitat zu Koln, Zulpicher Straße 77, 50937 Koln, Germany,roellig@ph1.uni-koeln.de2 N. Copernicus Astronomical center

3 SRON Netherlands Institute for Space Research, P.O. Box 800, 9700 AVGroningen, Netherlands

With Herschel’s spectral access to so far obscured chemical tracers of initial astrochemical network nodes, as-trochemical models become more and more important. This is especially true for models of PhotodissociationRegions (PDR) since many of the chemical precursors of complex moleculesare formed under the influence ofintense FUV irradiation. Recent studies have shown that due to their complexity, different models might producevery different results (Rollig et al. 2007)

The KOSMA-τ PDR model is a spherical PDR model that has been developed in a collaborative effort in theUniversities of Cologne and Tel Aviv (Storzer at al, 1996, Rollig et. al 2006). The code features a finite, sphericalgeometry and solves the coupled chemistry and energy balance problem in the gas phase. Over the last years aseries of updates and extension have been added to the code and will be summarized. Particularly the followingtopics are covered:

• Updated to isotopologue chemistry (Rollig & Ossenkopf 2010)

• Clumpy PDR Model Approach (Cubick et. al. 2008)

• Update to the dust treatment in KOSM-τ (Rollig & Szczerba 2010, Szczerba et al. 1997)

• Improved radiative transfer computation using SimLine

• Online Acces to PDR Model results

References:Cubick et al. 2008, A&A, 488, 623-634Rollig et. al, 2006, A&A, 451, 917Rollig, M., Abel, N. P., Bell, T., et al. 2007, A&A, 467, 187Rollig, M. & Ossenkopf, 2010, in prep.Rollig, M. & Szczerba, R., 2010, in prep.Szczerba et al. 1997, A&A 317, 859Storzer H., Stutzki J. & Sternberg A. 1996, A&A, 310, 592

P-IV-22

Before and After Herschel – Modeling Photo-Induced Chemistryand PDR Line Emission in theWarm and Dense ISM (WADI)

M. ROLLIG1, CH. JOBLIN 2,3, V. OSSENKOPF1,4, AND THE WHOLE WADI CONSORTIUM

1 I. Physikalisches Institut der Universitat zu Koln, Zulpicher Straße 77, 50937 Koln, Germany,roellig@ph1.uni-koeln.de

2Universite de Toulouse, UPS, CESR, 9 avenue du colonel Roche, 31062 Toulouse cedex 4, France3CNRS, UMR 5187, 31028 Toulouse, France

4SRON Netherlands Institute for Space Research, P.O. Box 800, 9700 AVGroningen, Netherlands

In the interstellar framework, molecules are formed gradually from atoms andions. Chemical models describethese formation cycles and observations could already confirm many of thetheoretical ideas. The basic carbonchain C+ −→ C −→ CO is the most prominent of these cycles. However, the large spectral coverage of HIFIallows for the first time to observe species that are formed in the initial steps ofchemical networks and thus conveycrucial information on the local gas conditions which also govern the abundance of more evolved species. TheHerschel Guaranteed Time Key Project WADI was designed to study exactly these species in the the warm anddense ISM, particularly in Photodissociation Regions (PDRs). The Herschel data taken in the framework of WADIso far already offers a surprising view on key nodes of astrochemicalnetworks. Despite a steep energy barrier inthe main formation channel, OH+ appears to be much more abundant than expected. A possible explanation mightbe the reaction with excited hydrogen molecules, in order to provide the required formation energy (Agundezet al. 2010). Another example is the detection of ionized water molecules, H2O+ (Ossenkopf et al. 2010b),while the subsequent chemical precursor of water, H3O+ is much less abundant than expected. The new Herscheldata greatly increases the information that we have from sites of massive star formation. Consequently it alsoincreases the complexity of possible models meant to interpret the observations. We will present recent results onmodeling the photo-induced chemistry and PDR line emission of objects so far observed within WADI. We willalso compare the post-Herschel model results with the pre-Herschel status, i.e. discuss the question: ”What doesHerschel observations teach us?”.

Example realisation of a two-component clumpy PDR modelrepresenting the region DR21C. Theembedded star cluster is marked asred sphere, the surround HII regionas blue wireframe sphere. One en-semble is subject to very strong FUVillumination (yellow globes) while themore massive ensemble (beige globes)has less intense FUV illumination butprovides the bulk of the material.References:Agundez et al. 2010, ApJ, 713, 662Ossenkopf, V., et al., 2010, A&A,accepted

P-IV-23

Dust/gas correlations in the Large Magellanic Cloud: New insights from Herschel

J. ROMAN-DUVAL 1, F. ISRAEL2, A. BOLATTO3, A. HUGHES4,5, A. LEROY6, M. MEIXNER1, K. GORDON1,& THE HERITAGE AND MAGMA TEAMS

1 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA ,duval@stsci.edu2 Sterrewacht Leiden, Leiden University, P.O. 9513, NL-2300 RA Leiden, Netherlands,

israel@strw.leidenuniv.nl3University of Maryland, Department of Astronomy, Lab for Millimeter Wave Astronomy, College Park, MD

20742, USA4Centre for Supercomputing and Astrophysics, Swinburne University ofTechnology, Hawthorn VIC 3122,

Australia5CSIRO Australia Telescope National Facility, PO Box 76, Epping NSW 1710,Australia

6National Radio Astronomy Obsevatory, 20 Edgemont Road Charlottesville, VA 22903-2475, USA

Previous Spitzer and IRAS observations of the LMC suggest an excessof FIR emission with respect to the gassurface density traced by12CO rotational emission lines and HI 21 cm emission. This so-called “FIR excess”is especially noticeable near molecular clouds in the LMC, and has usually been interpreted as indicating thepresence of a self-shielded H2 component not traced by CO in the envelopes of molecular clouds. Based onHerschel HERITAGE observations taken as part of the Science Demonstration Phase, we examine the correlationbetween gas and dust surface densities at higher resolution than previously achieved.

We consider three additional possible causes for the FIR excess: X factor, FIR dust emissivity, and gas-to-dustratio variations between the diffuse and dense phases of the ISM. We examine the structure of NT80 and NT71,two molecular clouds detected in the NANTEN12CO survey of the LMC. Dust surface density maps were derivedfrom the HERITAGE data. The gas phase is traced by MAGMA12CO and ATCA+Parkes HI 21 cm observationsof the LMC. These data provide unprecedented resolution (1’) to examinethe structure of molecular clouds. Thedust emissivity, gas-to-dust ratio, and X factor required to match the dustand gas surface densities are derived, andtheir correlations with the dust surface density are examined.

We show that the dust surface density is spatially correlated with the atomic andmolecular gas phases. The dusttemperature is consistently lower in the dense phase of the ISM than in the diffuse phase. We confirm variations inthe ratio of FIR emission to gas surface density derived from HI and CO observations. There is an excess of FIRemission, spatially correlated with regions of intermediate HI and dust surface densities (AV = 1-2), and little orno CO. While there is no significant trend in the dust emissivity or gas-to-dust ratio with dust surface density, theX factor is enhanced at AV = 1-2. We conclude that H2 envelopes not traced by CO and X factor variations closeto the CO boundary may be more likely to cause these deviations between FIR emission and gas surface densitythan gas-to-dust ratio or emissivity variations.

P-IV-24

Star formation in the Rosette molecular cloud under the influence of NGC 2244

N. SCHNEIDER1, F. MOTTE1, S. BONTEMPS2, M. HENNEMANN1, P. TREMBLIN1, V. M INIER1, E. AUDIT1

1 IRFU/SAP Cea Saclay, France,nschneid@cea.fr2 OASU Bordeaux, France,sylvain.bontemps@obs.u-bordeaux1.fr

The Rosette molecular cloud (Williams et al. 1994, Schneider et al. 1998) is significantly influenced bythe O-stars which are illuminating the Rosette Nebulae (NGC2244). Figure 1 (left) shows a three-color imageof the recently obtained SPIRE/PACS data (70–500µm), obtained during the Science demonstration phase ofHerschel for the HOBYS (Herschel Imaging Survey of OB Young StellarObjects) key-program. The shortestwavelength (70µm, blue) is strongest in the warm interface between HII-region and molecular cloud while thelongest wavelength (500µm,red) dominates the cold gas emission in the remote part of the cloud. From thisdata, we observed a negative gradient of the dust temperature into the cloud and indications of an age-gradient(younger objects are found in the remote part of the cloud). These findings point towards a possbile large-scaletriggering of star formation by a first generation of stars (Elmegreen & Lada 1977). On smaller scales, we find starformation activity in dense ’pillars’ of gas that are directly exposed to UV radiation close to the HII region (Figure2, right). We present first results of turbulence models that combine the effect of ionization and gravity to modelthese pillars.

Figure 1: Left: Three-color image (70µm = blue, 160µm = green, 500µm = red) of Rosette, overlaid on anoptical image (Hα from the DSS). Right: Upper left: dust temperature, upper right: column density, lower left:Overlay 70µm and 350µm, lower right: three-color image.

References:Elmegreen, B., & Lada, C., 1977, ApJ 214, 725Schneider, N., Stutzki, J., Winnewisser, G., et al., 1998a, A&A, 335, 1049Schneider, N., et al., 2010, A&A Letter in press.Williams, J.P., de Geus, E.J., Blitz, L., 1994, ApJ 428, 693

P-IV-25

Submillimeter Astronomy with the SMARTreceiver at NANTEN2: New results

R. SIMON1, J. STUTZKI1, Y. FUKUI2, H. YAMAMOTO2, H. OGAWA3, F. BERTOLDI4,B. KOO5, L.BRONFMAN6, M. BURTON7, AND A. BENZ8

1 I. Physikalisches Institut, Universitat zu Koln, 2 Nagoya University,3 Osaka Prefecture University,4 UniversitatBonn,5 Seoul National University,6 Universidad de Chile,7 University of New South Wales,8 ETH Zurich.

NANTEN2 (Nanten=Japanese for Southern Sky) is a joint collaboration between Nagoya and Osaka University(Japan), KOSMA, AIfA (Cologne and Bonn University) and additionalpartners from Switzerland (ETH Zurich),South Korea (Seoul National University), Australia (UNSW Sydney), and Chile. The project combines the NAN-TEN2 4 m submm telescope and the Cologne SMART receiver, backends,and software at an excellent observingsite in the Chilean Atacama desert close to the ALMA site.

The high frequency windows between 440 495 GHz (45” angular resolution) and 800 880 GHz (25” angularresolution) are covered by the Cologne SMART (SubMillimeter Array Receiver for Two frequencies) instrument.This array receiver provides 8 mixers for each of the two simultaneously observable frequencies and thus has atotal of 2 x 8 = 16 pixels on the sky.

The science projects with NANTEN2 are focussed on observations and modelling of the large scale distribu-tion, structure, dynamics, and chemistry of the ISM in the Milky Way and nearby galaxies. The main task forSMART at NANTEN2 is large scale mapping of important cooling lines of the interstellar medium, namely both[CI] lines (492 and 809 GHz) and CO 4-3/7-6.

Observations of these lines towards the largely unexplored southern skywill be analyzed and inter-preted usingtools to characterize the cloud structure, radiative transfer models, and models of Photon Dominated Regions(PDRs). In addition, they serve as complementary and preparatory workfor studies with HIFI/Herschel, SOFIA,STO, APEX, and ALMA.

We have started observations of the key projects for the observatory asidentified by the NANTEN2 consortiummembers: Galactic Center, low- and high-mass star forming regions in the southern hemisphere, the Magellanicclouds, and nearby galaxies. This poster summarizes some of the recent results.

P-IV-26

Diffuse interstellar PAH emission in the LMC observed with theAKARI/IRC

H. UMEHATA1, I.SAKON2, AND T.ONAKA 2

1 Institute of Astronomy, University of Tokyo, 2-21-1 Osawa, Mitaka, Tokyo 181-0015, Japan,umehata@ioa.s.u-tokyo.ac.jp

2 Department of Astronomy, Graduate School of Science, The Universityof Tokyo, Bunkyo-ku, Tokyo 113-0033,Japan,isakon@astron.s.u-tokyo.ac.jp,onaka@astron.s.u-tokyo.ac.jp

We carried out mid-infrared slit spectroscopic observations of the diffuse ISM in the Large Magellanic Cloud(LMC) with the Infrared Camera (IRC) onboard AKARI. The target areas have been selected based on the criteriathat the J = 1-0 transition of12CO is detected in the NANTEN survey and that the IRAS 60µm/100µm colordistributes in a wide range.

Distinct unidentified Infrared (UIR) bands have been detected in most ofthe spectra except for one case atthe boundary of supergiant shells (SGSs). The band ratios of 6.2µm/11.2µm,7.7µm/11.2µm,8.6µm/11.2µm havebeen measured. We find that the band ratios peaks at positions with an intermediate IRAS 60µm/100µm color ofI(60/100)∼0.5 and decreases at positions with lower or higher IRAS 60µm/100µm colors of I(60/100)∼0.4 andI(60/100)∼0.6 –0.7, respectively.

These band ratios are thought to be sensitive to the ionization state of PAHs.Assuming that ionization ofPAHs is balanced by the photo-ionization and the recombination of electrons,it is a function of the ratio of theinterstellar radiation field strength to the electron density. The regions with the intermediate I(60/100) value mightbe dominated by photo dissociation regions (PDRs) rather than ionized (HII) regions and the result implies thatPDRs should offer the suitable environment for PAHs to be positively ionized.

In this presentation, we focus on the properties of PAHs at various positions in terms of interstellar radiationenvironments in the LMC.References:Allamandola, L. J., Tielens, A. G. G. M., Barker, J. R. 1985, ApJ, 290, L25Allamandola, L. J., Tielens, A. G. G. M., Barker, J. R. 1989, ApJS, 71, 733Bakes, E. L. O., Tielens, A. G. G. M., Bauschlicher, C. W., Jr. 2001, ApJ, 556, 501de Frees, D. J., Miller, M. D., Talbi, D., Pauzat, F., Ellinger, Y. 1993, ApJ,408, 530Draine, B. T., Li, A. 2007, ApJ, 657, 810Helou, G., Lu, N. Y., Werner, M. W., Malhotra, S.,Silbermann, N. 2000, ApJ, 532, L21Li, A., Draine, B. T. 2002, ApJ, 576, 762 Lutz, D., Variante, E., Sturm, E.,Genzel, R.,Tacconi, L. J., Lehnert, M. D., Sternberg, A.,Baker, A. J. 2005, ApJ,625, L83Meaburn, J. 1980, MNRAS, 192, 365Onaka, T., Yamamura, I., Tanabe , T., Roellig, T. L., Yuen, L. 1996, PASJ, 48, L59Peeters,E., Spoon, H.W.W.,Tielens,A.G.G.M. 2004, ApJ, 613, 986Sakon, I., et al. 2006, ApJ, 651, 174Sakon, I., Onaka, T., Wada, T., et al. 2007, PASJ, 49, S483Sakon, I., et al. 2008, IAUS, 251,S241Sakata, A., Wada, S., Tanabe , T.,Onaka, T. 1984, ApJ, 287, L51Sauvage, M., Vigroux, L.,Thuan, T. X. 1990, A&A, 237, 296Szczepanski, J.,Vala, M. 1993 ApJ, 414, 646Tokunaga, A.T. 1997, ASP Conf. Ser. 124, 149Yan, L., et al. 2005, ApJ, 628, 604

P-IV-27

Herschel’s GOT C+ Survey of Cloud Transitions in the Inner Galaxy

T. VELUSAMY, W. D. LANGER, J. L. PINEDA , P. F. GOLDSMITH, D. LI , H. W. YORKE

Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109-8099,USA velusamy@jpl.nasa.gov

To understand star formation and the lifecycle of the interstellar gas we needdetailed information about the tran-sition of diffuse atomic to molecular clouds. The C+ line at 1.9 THz traces a so-far poorly studied stage in cloudevolution - the cloud’s evolution from purely atomic HI to molecular H2 This transition phase, which is difficult toobserve in HI and CO alone, may be best characterized via CII emission orabsorption. Here we present the first re-sults on such cloud transitions along representative lines of sight in the inner Galaxy between longitudes 330◦ and30◦, observed under the GOT C+ program, a HIFI Herschel Key Project tostudy the diffuse ISM. The preliminaryHIFI results so far along a few lines of sight, show resolved velocity features in CII emission distributed all acrossthe Galactic disk along each line of sight. We have separated these different ISM components by comparisons ofthe high spectral resolution (∼ 1 km s−1) and high sensitivity (rms 0.1 K to 0.2 K) HIFI CII data with HI (fromexisting Galactic plane surveys: SGPS and VGPS),12CO, 13CO and C18O spectra obtained by us using Mopra.The CII features show a wide range of properties in their association with the CO and HI structures along eachline of sight. Out of the total 146 [CII] velocity components detected by profile fitting we identify 53 as diffusemolecular clouds with associated12CO emission but without13CO emission and characterized by AV < 5 mag.We estimate the fraction of the [CII] emission in the diffuse HI layer in each cloud and then determine the [CII]emitted from the molecular layers in the cloud. We show that the excess [CII] intensities detected in a few cloudsis indicative of a thick H2 layer around the12CO core. The wide range of clouds in our sample with thin to thickH2 layers suggests that these are at various evolutionary states characterized by the formation of H2 and CO layersfrom HI and C+, respectively. In about 30% of the clouds the H2 column densities (“dark gas”) traced by the [CII]is 50% or more than that traced by12CO emission. On the average∼ 25% of the total H2 in these clouds is in anH2 layer which is not traced by CO. We use the HI, [CII], and12CO intensities in each cloud along with simplechemical models to obtain constraints on the FUV fields and cosmic ray ionization rates. We discuss the observedcharacteristics of the cloud transitions as potential initial conditions for the formation of star forming clouds. Thisresearch was conducted at the Jet Propulsion Laboratory, CaliforniaInstitute of Technology under contract withthe National Aeronautics and Space Administration.

Second Session, starting Thursday, September 23

Session V:Formation of stars: high M, low M, planetary systems

P-V-1

The mid-infrared extinction law in the Trifid nebula.

L. CAMBRESY1, AND J. RHO2

1 Observatoire astronomique de Strasbourg, Universite de Strasbourg, CNRS, UMR 7550cambresy@astro.unistra.fr

2 IPAC/CALTECH,rho@ipac.caltech.edu

Our goal is to seek out variations of the dust properties in the molecular cloud associated with the Trifid nebula.Using color excess from 2MASS and Spitzer/GLIMPSE data we analyze theextinction law from 3.6 to 5.8 micronsand found variations in the densest part of the clouds. These variationssuggest a transition in the dust propertiesat high extinction.

P-V-2

The CHESS Spectral Survey of the Solar Type Protostar IRAS16293-2422

EMMANUEL CAUX1

1 CESR/CNRS - University of Toulouse,caux@cesr.fr

P-V-3

Water in massive star forming regions:HIFI observations of W3-IRS5

L. CHAVARRIA1, F. HERPIN1, T. JACQ1, J. BRAINE1, S. BONTEMPS1, A. BAUDRY1, ET AL .

1 Universite de Bordeaux, Laboratoire d’Astrophysique de Bordeaux, Floirac,France,Luis.Chavarria@obs.u-bordeaux1.fr

We present Herschel/HIFI observations of the water molecule in the massive star forming region W3-IRS5. High-mass proto-stellar inner cores reach temperatures well in excess of 100 Kso the water ices in the dust mantles arevaporized and water may become a powerful coolant in a specific part ofthe dense core. The o-H172 O 110-101,p-H18

2 O 111-000, p-H2O 202-111, p-H2O 111-000, o-H2O 221-212, and o-H2O 212-101 lines, covering a frequencyrange from 552 up to 1669 GHz, have been observed at high spectralresolution with HIFI. The well defined highvelocity wings seen in the H162 O lines show a clear contribution of outflow shocks that vaporize water from dustgrain mantles in the proto-stellar envelope. Moreover, the systematically blue-shifted absorption in the H162 O linesimplies expansion, presumably driven by the outflow. No infall signatures are detected. The p-H2O 111-000 ando-H2O 212-101 lines show absorption from the cool (T∼ 10 K) molecular envelope surrounding the inner core.Uni-dimensional radiative transfer models are used to estimate water abundances and study the kinematics of theregion. We show that the emission in the rare isotopologues comes directly from the hot inner regions where ajump in the water abundance (with a constant inner abundance of10−4) is necessary to reproduce the o-H17

2 O110-101 and p-H18

2 O 111-000 spectra. We estimate water abundances of 10−8 to 10−9 in the envelope (T < 100 K).The detection of two proto-stellar objects in the spectra is discussed.

P-V-4

HIFI observations of deuterated water towards SgrB2

C. COMITO1, R. ROLFFS1, P. SCHILKE2, E. A. BERGIN3, D. C. LIS4, ET AL .

1 Max-Planck-Institut fur Radioastronomie, Auf dem Hugel 69, 53121 Bonn, Germanyccomito@mpifr.de,rrolffs@mpifr.de

2 I. Physikalisches Institut, Universitat zu Koln, Zulpicher Str. 77, 50937 Koln, Germanyschilke@ph1.uni-koeln.de

3 Department of Astronomy, University of Michigan, 500 Church Street, Ann Arbor, MI 48109, USAebergin@umich.edu

4 California Institute of Technology, Cahill Center for Astronomy and Astrophysics 301-17, Pasadena, CA 91125USA dcl@caltech.edu

HDO has been found and modeled in SgrB2 before, using the fundamentaland some highly excited transitionsobserved with ground based telescopes. However, this study revealedthat the transitions observed were sensitiveonly to the very inner and the very outer parts of the SgrB2 cloud, i.e. to the outer envelope, where the ground-state lines were found in absorption, and the inner hot core, where the highly excited lines were found in emission.Nothing could be said of the distribution of HDO in the bulk of the envelope. Thisgap has been filled with linesobserved with HIFI, and modeling reveals the distribution of HDO throughout the cloud, which gives importantinformation on the formation pathways of both HDO and H2O - shocks or grain mantles?

P-V-5

Hot core millimeter and submillimeter spectra : Comparing simulations with IRAM andHerschel-HIFI spectra

MASSIMO DE LUCA1

1 LERMA, CNRS, Observatoire de Paris, ENS,massimo.de.luca@lra.ens.fr

P-V-6

The morphology of the high mass star formation sites N44 and N63 in the LMC

S. HONY1 , F. GALLIANO 1 , S. C. MADDEN1 , P. PANUZZO1 , M. MEIXNER2 , C. ENGELBRACHT3 ,K. M ISSELT3 , M. GALAMETZ 1 , M. SAUVAGE1 , J. ROMAN-DUVAL 2 , K. GORDON2 , B. LAWTON2 ,

J.-P. BERNARD4 , A. BOLATTO5 , K. OKUMURA1 , C.-H. R. CHEN6 , R. INDEBETOUW6 , F. P. ISRAEL7 ,E. KWON8 , A. L I9 , F. KEMPER10 , M. S. OEY11 , M. RUBIO12

1 Service d’Astrophysique, CEA, Saclay, 91191 Gif-Sur-Yvette Cedex, France,sacha.hony@cea.rf,frederic.galliano@cea.fr, smadden@cea.fr, pasquale.panuzzo@cea.fr,

maud.galametz@cea.fr, msauvage@cea.fr, koryo.okumura@cea.fr2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA,

meixner@stsci.edu, duval@stsci.edu, kgordon@stsci.edu, blawton@nmsu.edu3 Steward Observatory, University of Arizona, 933 North Cherry Ave.,Tucson, AZ 85721, USA,

cengelbracht@as.arizona.edu, kmisselt@as.arizona.edu4 Centre d’Etude Spatiale des Rayonnements, CNRS, 9 av. du Colonel Roche, BP 4346, 31028 Toulouse, France,

jean-philippe.bernard@cesr.fr5 Department of Astronomy, Lab for Millimeter-wave Astronomy, University ofMaryland. College Park, MD

20742-2421, USA,bolatto@astro.umd.edu6 Department of Astronomy, University of Virginia, PO Box 3818, Charlottesville, VA 22903, USA,

rchen@virginia.edu, remy@virginia.edu7 Sterrewacht Leiden, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands,

israel@strw.leidenuniv.nl8 Astronomy & Space Science, Sejong University, 143-747, Seoul, SouthKorea,ziazzz@naver.com

9 Department of Physics and Astronomy, University of Missouri, 314 Physics Building, Columbia, MO 65211,USA,lia@missouri.edu

10 Jodrell Bank Centre for Astrophysics, Alan Turing Building, School ofPhysics and Astronomy, The Universityof Manchester, Oxford Road, Manchester, M13 9PL, UK,ciska.kemper@manchester.ac.uk

11 Department of Astronomy, University of Michigan, 830 Dennison Building,Ann Arbor, MI 48109-1042,USA,msoey@umich.edu

12 Departamento de Astronomia, Universidad de Chile, Casilla 36-D, Santiago,Chile,monica@das.uchile.cl

We study the structure of the medium surrounding sites of high-mass star formation to determine the interrelationbetween the HII regions and the environment from which they were formed. The density distribution of thesurroundings is key in determining how the radiation of the newly formed starsinteracts with the surrounds ina way that allows it to be used as a star formation tracer. We present new Herschel/SPIRE 250, 350 and 500mum data of LHA 120-N44 and LHA 120-N63 in the LMC. We construct average spectral energy distributions(SEDs) for annuli centered on the IR bright part of the star formation sites. The annuli cover 10- 100 pc. Weuse a phenomenological dust model to fit these SEDs to derive the dust column densities, characterise the incidentradiation field and the abundance of polycyclic aromatic hydrocarbon molecules. We see a factor 5 decrease inthe radiation field energy density as a function of radial distance around N63. N44 does not show a systematictrend. We construct a simple geometrical model to derive the 3-D density profile of the surroundings of thesetwo regions. Herschel/SPIRE data have proven very efficient in deriving the dust mass distribution. We find thatthe radiation field in the two sources behaves very differently. N63 is more or less spherically symmetric and theaverage radiation field drops with distance. N44 shows no systematic decrease of the radiation intensity whichis probably due to the inhomogeneity of the surrounding molecular material andto the complex distribution ofseveral star forming clusters in the region.

P-V-7

Water in Star-Forming Regions with Herschel: IntermediateMass Protostars

D. JOHNSTONE1

1 NRC Canada/Herzberg Institute of Astrophysics,doug.johnstone@nrc-cnrc.gc.ca

The Herschel HIFI spectrograph is proving to be an excellent instrument for the detection of water in star-formingregions. As part of the WISH key program, we have undertaken a studyof water in the envelope around sixintermediate mass protostars. The first results, toward NGC 7129, have been completed during PSP and are to bepublished in the A&A HIFI Special Edition (Johnstone et al. 2010). The water spectra reveal broad lines (Firure1), connecting this emission with the energetic outflow being driven by the central protostar. By September amajority of the Intermediate mass protostars should have been observed by Herschel and a detailed investigationinto the components responsible for the emission - envelope, outflow, etc - willbe possible. As well, intermediatemass protostars serve as a link between the well-studied low-mass and high-mass extremes of star formation. Amajor goal of the WISH key program is to investigate this link.

Three water lines toward the source NGC 7129 overlaid on a Spitzer image ofthe region.

References:Johnstone, D. et al. A&A, in preparation.

P-V-8

The Chemical Herschel Spectral Survey of Star Forming Regions:Peering into the protostellar shock L1157-B1.

Lefloch B1., Codella C2., Cabrit S3 Ceccarelli C.1, Cernicharo J.4, Caux E.5

1 LAOG, Observatoire de Grenoble, BP 53, 38041 Grenoble Cedex, France2 INAF, Osservatorio Astrofisico di Arcetri, Firenze, Italy3 Observatoire de Paris-Meudon, LERMA UMR CNRS 8112. Meudon, France4 Centro de Astrobiologia, CSIC-INTA, Madrid, Spain5 CESR, Universite Toulouse 3 and CNRS, Toulouse, France

We present the first results of the spectral survey of bowshock B1 in the chemically active outflow drivenby the Class 0 protostar L1157. The observations are part of the CHESSKey Program, and were obtained withHIFI and PACS. The bright blue-shifted bow shock B1 is the ideal laboratory for studying the link between thehot (1000-2000 K) component traced by H2 IR-emission and the cold (10-20 K) swept-up material. The mainaim is to trace the warm gas chemically enriched by the passage of a shock and to infer the excitation conditionsin L1157-B1. We report on the identification of lines from NH3, H2CO, CH3OH, CS, HCN and HCO+. Thecomparison between the profiles due to molecules released from dust mantles(NH3, H2CO, CH3OH) with thatfor water is consistent with the scenario where water is also formed in the gasphase in high-temperature regions,where sputtering or grain-grain collisions are not efficient. The high excitation range of the observed tracers allowsus to infer, for the first time with these species, the existence of a warm (∼ 200 K) gas component coexisting inthe B1 bow structure with the cold and hot gas detected from ground. We discuss the detection of the high-J COlines (up to Jup= 16) and H2O lines. These lines exhibit broad high-velocitywings, allowing to probe the shockedregion. We found that the water abundance is enhanced by two orders of magnitude in the shock, up to 10-4 . Thehigh-optical depth of the line makes it a privileged tool to detect the highest excitation regions in the shock. Basedon comparison with MHD shock models and using complementary data in the millimeter and infrared (Spitzer,ISO), we discuss the shock parameters, in particular its age and the intensityof the magnetic field in the pre-shockgas.

P-V-9

Herschel observations of the distribution of water in cluster-forming regions

S. LEURINI1, F. WYROWSKI1 AND THE WISH TEAM

1 Max Planck Institut fur Radioastronomie,sleurini@mpifr.de,wyrowski@mpifr.de

Water is a key molecule for determining the physical and chemical structure ofstar-forming regions because of itslarge abundance variations between warm and cold regions. As part ofthe HIFI-led Key Program WISH, we aremapping six massive star-forming regions in different H2O lines with HIFI and PACS to investigate the effects ofclustered star formation and feedback by protostellar outflows on high-mass star formation. Such sources covera wide range of evolutionary phases, from mid-IR quiet HMPOs to sources alreay hosting UCHII regions. In mytalk, I will present preliminary results on the maps already obtained towards the sample of cluster-forming regions.

P-V-10

Comprehensive View of Massive Quiescent Cores

DI L I1

1 Jet Propulsion Lab,dili@jpl.nasa.gov

P-V-11 Galactic Young Star Clusters and their Molecular Environment

E. F. E. MORALES1, F. WYROWSKI1, K. M. M ENTEN1, F. SHULLER1

1 Max-Planck-Institut fur Radioastronomie,emorales@mpifr-bonn.mpg.de

In the last years, many new young embedded stars clusters have been discovered in the IR (mainly using2MASS; e.g., Dutra et al. 2003, Bica et al. 2003). Our aim is to study the molecular environment of them,searching for physical correlation with submm continuum emission (ATLASGAL survey at 870µm, Schuller etal. 2009), which traces the cold dust, and observing a subsample of objects in CO isotopes to probe the dynamicalevolution and kinematics of the cluster’s surrounding molecular gas.

After doing a literature compilation of all star clusters inside the ATLASGAL range (|l| ≤ 60◦ and |b| ≤1.5◦), we found that the 2MASS clusters are often (∼ 60% of them) associated with ATLASGAL emission, asopposed toSpitzer-GLIMPSE clusters (∼ 30%) and classical optical clusters (∼ 30%). A qualitative recognitionof different scenarios of cluster-environment interaction was done bycomparing the ATLASGAL morphologywith the near-infrared 2MASS images: 1) cluster deeply embedded (see figure,left), 2) cluster still embedded butalready undergoing feedback events, 3) cluster has cleared out the nearby material making visible a bubble (seefigure,right), and 4) cluster whose formation is probably triggered by another cluster/star in scenario 2) or 3). Forsome clusters in scenarios 2, 3, 4, strong emission at 8µm (Spitzer) has been found, correlated with ATLASGALand showing a ring structure (the so-calledIR bubbles), making them ideal targets to study triggered star formationat the periphery of the ring.

We carried out follow-up molecular line observations for a subsample ofconfirmed(as real clusters) 2MASSclusters, some of them associated with IR bubbles. 15 objects were mapped in13CO(2–1) and C18O(2–1) using theIRAM-30m and APEX telescopes. Two of them were also mapped in CO(6–5) and CO(7–6) (using CHAMP+) toprobe the high density UV-excited gas at the inner surface of the bubble.General kinematics is being studied forsome of the observed objects. For two of the bubble-like, the observationshave been compared and are consistentwith a simple geometrical model of an expanding bubble with a velocity of a few km/s.

Left: 2MASS K-band image of the cluster[DBS2003] 165. Right: GLIMPSE 3.6µm image of the cluster[DBS2003] 131 (at 8µm the bubble is even brigther). Contours are ATLASGAL (870µm).

References:Bica, E., Dutra, C. M., Soares, J., & Barbuy, B. 2003, A&A, 404, 223Dutra, C. M., Bica, E., Soares, J., & Barbuy, B. 2003, A&A, 400, 533Lada, C. J., & Lada, E. A. 2003, ARA&A, 41, 57Schuller, F., et al. 2009, A&A, 504, 415

P-V-12

The Herschel view of the Perseus Star Forming region

STEFANO PEZZUTO1, JAMES DI FRANCESCO2,3, P. ANDRE4, P. SARACENO1, M. BENEDETTINI1, A.M. D I

GIORGIO1, S. MOLINARI1, M. PESTALOZZI1, D. POLYCHRONI1, E. SCHISANO1, L. SPINOGLIO1, S.I.SADAVOY 2,3, L. TESTI5,6, S. BONTEMPS1, M. GRIFFIN7, K. JASON7, V. K ONYVES4, A. MEN’ SHCHIKOV4,

N. SCHNEIDER4, D. WARD-THOMPSON7

1 IFSI-INAF, pezzuto@ifsi-roma.inaf.it2 University of Victoria

3 National Research Council Canada4 CEA Saclay, France

5 INAF-Osservatorio Astrofisico di Arcetri, Italy6 ESO, Germany

7 Cardiff University, United Kingdom

Perseus is one of the nearby star forming cloud at an average distance of about 250 pc. It hosts low as wellintermediate mass stars and its properties are halfway between low mass stars forming regions like Taurus, andhigh mass stars as in Orion.

It has been observed photometrically at different wavelengths, mainly in the (sub)millimetre and NIR/FIR (egCurtis & Richer 2010, Sadavoy et al. 2010, Enoch et al. 2009) and spetroscopically (eg Johnstone et al. 2010,Foster et al. 2009) in a high numbers of tracers. It is one of the cloud observed with Spitzer for the c2d survey(Rebull et al. 2007, Jørgensen at al. 2007, Evans et al. 2003).

In this talk I present the results of the first observation of Perseus donewith Herschel as part of the Gould Beltprogram (Andre et al. 2010). The observation covers the region around NGC 1333 for a total of 5.6 deg2, seen inthe 70 and 160µm PACS bands, and 250, 350 and 500µm SPIRE bands. The physical properties of the detectedsources as derived from the observed SEDs are discussed.References:Andre, P., et al., 2010, A&A, special issueCurtis, E.I., Richer, J.S. 2010, MNRAS, 402, 603Enoch, M.L., Evans II, N.J., Sargent, A.I., Glenn, J., 2009, ApJ, 692, 973Evans, N.J., et al. 2003, PASP, 115, 965Foster, J.B., et al., 2009, ApJ, 696, 298Johnstone, D., Rosolowsky, E., Tafalla, M., Kirk, H., 2010, ApJ, 711, 655Jørgensen, J.K, Johnstone, D., Kirk, H., Myers, P.C., 2007, ApJ, 656, 293Rebull, L.M., et al., 2007, ApJS, 171, 447Sadavoy, S.I., et al., 2010, ApJ, 710, 1247

P-V-13 HEXOS Observations of C18O and C17O in Orion KL

RENE PLUME1, E. A. BERGIN2, T. G. PHILLIPS3, D. C. LIS3, D. A. NEUFELD4, G. J. MELNICK5, AND THE

HEXOS TEAM .

1 University of Calgary,plume@ras.ucalgary.ca2University of Michigan,ebergin@umich.edu

3California Institute of Technology,tgp@submm.caltech.edu, dcl@its.caltech.edu4 Johns Hopkins University,neufeld@pha.jhu.edu

5 Harvard-Smithsonian Center for Astrophysics,gmelnick@cfa.harvard.edu

The total H2 column density is a fundamental quantity used to determine a variety of properties such as chemicalabundances, the importance self-shielding from radiation fields, cloud mass, etc. Since H2 is a homonuclearmolecule without a dipole moment, CO is often used as a proxy for the H2 abundance. However, since CO isoften optically thick, especially towards the highest column density regions in molecular clouds, the total H2column density is often poorly constrained. The large number of high-J linesof C18O, available to us via theHerschel Space Observatory, provide an unprecedented ability to model the total molecular column density. Usingthe emission from all the observed lines (up to J = 17 - 16) we can simply sum upthe column densities in theindividual levels to obtain the total column. With additional knowledge of source size we can even include thesource filling factor, and so can get the true total column. We will present results of Herschel/HIFI observations ofC18O and C17O in Orion KL (from the HEXOS Key Project). LTE modeling of the known sizes, VLSR, and linewidths allow us to determine the total column densities in the extended ridge, outflow, hot core, and compact ridgecomponents.

Spectra (histograms) and results of LTE mod-eling of the C18O J = 5-4 (548.831 GHz), J =7-6 (768.251 GHz), J = 8-7 (877.922 GHz),J = 9-8 (987.560 GHz), J = 11-10 (1206.725GHz), and J = 15-14 (1644.495 GHz) transi-tions in Orion KL. Results are shown for theextended ridge (solid blue), outflow (dashedblue), compact ridge (solid red), hot core(dashed red) and for the sum of all four com-ponents (dashed black).

P-V-14

Structure of Hot Cores

R. ROLFFS1,2 AND P. SCHILKE2

1 Max-Planck-Institut fur Radioastronomie Bonn,rrolffs@mpifr.de2 I. Physikalisches Institut der Universitat zu Koln,schilke@ph1.uni-koeln.de

Hot molecular cores are a short-lived phase of massive star formation: The massive stars have heated up thedense molecular gas in which they are deeply embedded, but have not yetionized and disrupted it. Information ontheir structure (density, temperature, velocity, molecular abundances) is needed both for astrochemistry and for re-search on massive star formation. With this aim, we performed APEX observations of 12 hot cores, complementedin some sources by Herschel/HIFI HEXOS key project data, in various lines of HCN, HCO+, and CO, covering awide range of excitations. The line shapes of optically thick lines are good tracers of the structure, in particular atthe higher frequencies, where the dust continuum favors absorption features and the excitation is higher. This canbe nicely seen in the new Herschel/HIFI data of HCN in SgrB2(M) (see figure), from which we infer that the infallis reversed in the inner part, due to feedback from the massive stars.

We have modeled the sources as centrally heated spheres with density power law gradient. The temperaturegradient is steeper in the inner part, where dust is optically thick to its own radiation. The continuum is adaptedto the radial profile extracted from ATLASGAL (Schuller et al. 2009), and lines are computed by the radiativetransfer code RATRAN (Hogerheijde & van der Tak 2000). Most lines are well reproduced by such models,but some features require a more sophisticated geometry: There is an occasional lack of self-absorption in somesources, and the emission from high-J lines in the outer pixels of the CHAMP+receiver (15-20“ from the center)is often much higher than in the model. We find that the HCN abundance increases with temperature, as traced bythe emission from vibrationally excited HCN.

To constrain more complicated models and to further approach the real hot core structure, one needs very highangular resolution, however. We have therefore observed G10.47+0.03 with the SMA at 0.4” resolution, obtaininginformation on the velocity field, the dust continuum, and lots of molecular lines. With the VLA, we observedvibrationally excited HCN (direct l-type line) in G10.47, SgrB2-N and -M at aresolution of 0.1”, showing bothemission from very high column densities of hot molecular gas and absorptionagainst hypercompact HII regions.Our interferometer data demonstrate that these massive hot cores are notsingly peaked and heated, but are formingwhole star clusters.

Reversal of Infall in SgrB2(M): Thefigure shows Herschel/HIFI observa-tions of HCN lines in SgrB2-M(HEXOS key project). Note the chang-ing asymmetry from lower to higher Jand from HCN to H13CN 6–5. Themodel (dashed) reproduces this by in-fall in the colder, outer region and ex-pansion in the warmer, inner part. It is acentrally heated sphere with power lawdensity gradient (index 1.5), computedby RATRAN.

References:Hogerheijde, M. R. & van der Tak, F. F. S. 2000, A&A, 362, 697Schuller, F., Menten, K. M., Contreras, Y., et al. 2009, A&A, 504, 415

P-V-15

Star Formation in the Orion A Molecular Cloud

YOSHITO SHIMAJIRI1,2, RYOHEI KAWABE1,2, SHIGEHISA TAKAKUWA 3, MASAO SAITO2,4, TAKASHI

TSUKAGOSHI5, MUNETAKE MOMOSE6, NORIO IKEDA7, E. AKIYAMA 6, H. EZAWA2, K. FUKUE4,13, M.HIRAMATSU3,8, D. HUGHES9, Y. K ITAMURA 7, K. KOHNO5, Y. KURONO2,4, G. WILSON10, A. YOSHIDA11,

M.S. YUN10

2 Nobeyama Radio Observatory,yoshito.shimajiri@nao.ac.jp, 3 National Astronomical Observatory,4 Academia Sinica Institute of Astronomy and Astrophysics,5 ALMA Project Office, National Astronomical

Observatory of Japan,6 Institute of Astronomy, Faculty of Science, University of Tokyo,7 Institute ofAstrophysics and Planetary Sciences, Ibaraki University,8 Institute of Space and Astronoutical Science, Japan

Aero space Exploration Agency,9 Department of Physics and Institute of Astronomy, National Tsing HuaUniversity,10 Instituto Nacional de Astrofısica,Optica y Electronica (INAOE),11 Department of Astronomy,University of Massachusetts,12 Department of Earth and Planetary Sciences Tokyo Institute of Technology, 13

Department of Astronomy, School of Science, University of Tokyo,

We present new, wide and deep images in the 1.1 mm continuum and the12CO (J=1–0) emission towardthe northern part of the Orion A Giant Molecular Cloud (Orion-A GMC). The 1.1 mm data were taken with theAzTEC camera mounted on the Atacama Submillimeter Telescope Experiment (ASTE) 10 m telescope in Chile,and the12CO (J=1–0) data with the 25 beam receiver (BEARS) on the NRO 45 m telescope inthe On-The-Fly (OTF) mode. This is the widest 1.7 degree× 2.3 degree corresponding to 12 pc× 17 pc) and the highestsensitivity (∼9 mJy beam−1) 1.1 mm dust-continuum imaging with an effective spatial resolution of∼ 40 arcsec.The12CO (J=1–0) image was taken over the northern 1.2 degree× 1.2 degree (corresponding 9 pc× 9 pc) areawith a sensitivity of 0.93 K inTMB, a velocity resolution of 1.0 km s−1, and an effective spatial resolution of21arcsec. With these data, as well as the MSX 8µm, Spitzer 24µm and the 2MASS data, we have investigatedthe detailed structure and kinematics of molecular gas associated with the Orion AGMC and have found evidencefor interactions between molecular clouds and the external forces that maytrigger star formation. Four types ofpossible triggers were revealed; 1) Collision of the diffuse gas on the cloud surface, particularly at the easternside of the OMC-2/3 region, 2) UV compression from OB stars that forms shells and filamentary structures ofPhoto-Dominated Regions (PDR), 3) UV radiation implosion on the pre-existingdense molecular cloud cores inthe western region of Ori-KL, and 4) collision of dense gas with the powerful outflows in the OMC-2/3 and theOMC-4 regions. Our wide-field and high-sensitivity imaging has provided the first comprehensive views of thepotential sites of triggered star formation in the Orion A GMC.

P-V-16

Modelling Herschel observations of hot gas emission in low-mass protostars

R. VISSER1, L.E. KRISTENSEN1, S. BRUDERER2, C. BRINCH1, S.D. DOTY3, AND E.F. VAN DISHOECK1,4

1 Leiden Observatory,[ruvisser,kristensen,brinch]@strw.leidenuniv.nl2 ETH Zurich,simonbr@astro.phys.ethz.ch

3 Denison University,doty@denison.edu4 MPE Garching,ewine@strw.leidenuniv.nl

The Herschel Space Observatory is providing a wealth of new data on theenvironments of low-mass protostars. Itis a major challenge to interpret these data and use them to improve our understanding of how stars are formed.Radiative transfer models are an essential tool to do so. We present a set of models where the environment ofembedded protostars (Class 0 and I) is dissected into three components: a passively heated envelope, UV-heatedoutflow cavity walls, and small-scaleC-type shocks along the cavity walls (see Figure 1). Due to Herschel’s highspatial and spectral resolution, it is possible for the first time to quantitativelydisentangle the contribution fromeach of these components to the overall emission of molecules like CO, H2O and OH. From the observations andthe models, we conclude that shocks and turbulence play a much larger rolein the protostellar environment thanpreviously assumed. We derive the abundance of H2O in each of the components and we discuss the results in thecontext of evolutionary models of low-mass star formation (Visser et al. 2009, 2010).

Figure 1: Cartoon of the various physical components of a low-mass embedded protostar: the passively heatedenvelope (light grey, including a hot core shaded dark grey), the UV-heated cavity walls (black), and the small-scale shocks in the cavity walls (spirals).

References:Visser, R., van Dishoeck, E.F., Doty, S.D., and Dullemond, C.P. 2009, A&A, 495, 881Visser, R., van Dishoeck, E.F., and Doty, S.D. 2010, A&A, submitted

P-V-17

Cold Disks around Nearby Stars. A Search for Edgeworth-Kuiper Belt Analogues

GLENN J. WHITE1,2 AND THE HERSCHELDUNES TEAM3

1 Dept of Physics& Astronomy, The Open University, UKg.j.white@open.ac.uk2 The Rutherford Applton Laboratory, Didcot, UKglenn.white@stfc.ac.uk 3 Various

About two dozen exo-solar debris systems have been spatially resolved.These debris discs commonly displaya variety of structural features such as clumps, rings, belts, eccentric distributions and spiral patterns. In mostcases, these features are believed to be formed, shaped and maintained by the dynamical influence of planets orbit-ing the host stars. Only in a very few cases has the presence of the dynamically important planet(s) been inferredfrom direct observation to date.

DUNES (DUst disks around NEarby Stars) is a sensitivity-limited survey programme using the unique capa-bilities of Herschel to detect and characterize with cold disks as faint asLdust/Lstar ∼ 10−6 and temperatures ofthe order of∼ 30 - 40 K, i.e., faint exo-solar analogues to the Edgeworth-Kuiper Belt.

DUNES is observing a statistically significant, volume limited (d ≤ 20 pc) sample, only constrained by back-ground confusion, of 133 FGK nearby stars. Stars with already knownexo-planets and/or Spitzer-discovered faintdebris disks up to larger distances,d ≤ 25 pc, are also included in the sample. This contribution presents the cur-rent state of the survey, along with selected DUNES results achieved during the Herschel science demonstrationphase and first routine phase observations. Particular emphasis will be made on the results achieved for the solartype starsq1 Eri andζ2 Ret, which are among the exciting objects observed by DUNES up to now.

Figure 1. Left image: PACS photometric results ofζ2 Ret - Images and plots are from left to right 70µm (blue),100µm (green), and 160µm. The PACS data suggest the existence of a exo-Kuiper belt analogue witha fractionalluminosityLdust ∼ 10−6 L⊙ (from Eiroa et al 2010 A&A Special Issue). Right image: PACS photometric resultsof the F9V starq1 Eri - from left to right 70µm (blue), 100µm (green), and 160µm. The debris aroundq1 Erihas an oval-shaped brightness distribution, the size of which increases with the wavelength. The resolved data areconsistent with debris at temperatures below 30K at radii larger than 120 AU. From image deconvolution, and thisis similar to the Edgeworth-Kuiper Belt around the Sun. This may also hint at thepresence of another planet,q1

Eri c (from Liseau et al 2010 A&A Special Issue)

P-V-18

Energetic processes revealed by spectrally resolved high-J CO lines in the low-mass star-formingregions with Herschel

U. A. Y ILDIZ 1, E. F.VAN DISHOECK 1,2, L. E. KRISTENSEN1, R. VISSER1, G. HERGZEG2,T. A. VAN KEMPEN3, J .K. JØRGENSEN4, M. R. HOGERHEIJDE1, AND THE WISH TEAM

1 Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands,yildiz@strw.leidenuniv.nl

2 Max Planck Institut fur Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany3 Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 42, Cambridge, MA 02138, USA

4 Centre for Star and Planet Formation, Natural History Museum of Denmark, University of Copenhagen, ØsterVoldgade 5-7, DK-1350 Copenhagen K., Denmark

Several low-mass protostars have been observed with HIFI on Herschel, in lines of12CO 10–9 and isotopologues of13CO 10–9 and C18O 9–8, 5–4 in order to constrain the physical properties of these objects.The high temperaturesneeded to produce these lines can be explained by three physical processes: passive heating of the protostellarenvelope, UV-heating of the outflow cavity walls, andC-type shocks in the cavity walls. Results from HIFI showsurprisingly broad line-widths of∼25-30 km/s (FWHM) for the CO 10–9 lines whereas lower-J lines such asCO 2–1, 4–3 or 6–5 which were obtained from JCMT or APEX-CHAMP+, it is ∼10-15 km/s. Such broad emissionin high-J lines are indicative of shocked gas. The most likely explanation is that the UV-heated gas in the outflowcavity walls which is also probed by isotopic lines seen with PACS, is simultaneously being shocked by the smallscaleC-type shocks. For the low-J lines, a quiescent part with a gaussian of∼2km/s can be seen at the centerof the line profiles whereas it is not significant in the high-J lines. For the isotopologues:13CO 10-9 have broadwings contrary to the lower-J lines of the same isotopologue; C18O 5–4 is readily detected in all sources andprobes the bulk of the quiescent warm gas; tentative detections exist in theC18O 9-8 isotopologues. These high-JCO lines are important to quantify the dense and warm gas around the protostellar envelopes to determine chemicalabundances in the various regions.

Figure 1: The comparison of single12CO and C18O spectra obtained from the central positions of IRAS 2A, 4Aand 4B shown on aTMB scale.

References:Yıldız et. al. 2010 (A&A HIFI Special Issue)Kristensen et. al. 2010 (A&A HIFI Special Issue)

Session VI:Laboratory astrophysics, astrochemistry

P-VI-1

DIMETHYL ETHER IN THE LABORATORY AND IN SPACE

C. P. ENDRES1, S. BISSCHOP2, M. KOERBER1, B. J. DROUIN3, P. GRONER4, H. S. P. MULLER1,F. LEWEN1, T. F. GIESEN1, AND S. SCHLEMMER1

1 I. Physikalisches Institut, Universitat zu Koln, 50937 Koln, Germany,endres@ph1.uni-koeln.de,koerber@ph1.uni-koeln.de

2 Center for Star and Planet Formation, University of Copenhagen, DK-1350, Copenhagen, Denmark,suzanne@snm.ku.dk

3 Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA 91109-8099, USA4 Department of Chemistry, University of Missouri-Kansas City, Kansas City, MO 64110, USA

Dimethyl ether (CH3OCH3) is highly abundant in hot cores and numerous transitions within the vibrationalground state have been detected in various interstellar line surveys of sources such as Orion KL1,2 As a nearlyprolate asymmetric top with two internal rotors, it shows a complex spectrum with low lying torsional modes(ν11=200 cm−1 andν15=240 cm−1), which are thus sufficiently populated in these interstellar sources to exhibittransitions in line surveys due to high excitation temperatures in hot cores. Due to the13C/12C ratio in someof these sources, similar contributions of rotational transitions within the ground state of singly13C-substitutedCH3OCH3 can be expected. Astronomical studies have been hampered until recently, as precise predictions havebeen available only for the ground state of the main isotopomer and only up to about 600 GHz. Therefore, werecorded and analyzed laboratory spectra covering frequencies upto about 2.1 THz for the main isotopomer andup to 120 GHz for the13C-substituted species. Based on the analysis of these spectra, we were able not only toimprove the quality of frequency predictions for the vibrational ground state of the main isotopomer, but also tocalculate and provide for the first time reliable transition frequencies for astrophysical modeling of the torsionallyexcited statesv11 andv15 as well as for the13C-substituted species. These laboratory data has been used to studythe properties of CH3OCH3 in the high-mass star-forming region G327.3-0.6. A line survey has been obtainedusing the SHFI and CHAMP+ instruments of the single-dish Atacama Pathfinder EXperiment (APEX) telescope.Both excited states,v11 = 1 andv15 = 1, have been detected, which is the first interstellar detection of vibra-tionally excited dimethyl ether. The abundance of CH3OCH3 has been modeled throughout the envelope and it isclear that ”abundance” jumps are present likely associated with grain surface evaporation. Particular attention hasbeen paid to the exitation properties of ground and vibrationally excited states, which give important insights ofthe formation mechanisms of CH3OCH3.References:1 Schilke, P., Groesbeck, T.D. 1997, ApJ Suppl.Ser., 108, 3012 Schilke, P., Benford, D.J., Hunter, T.R. 2001, ApJ Suppl. Ser., 132, 281

P-VI-2

Laboratory Astrochemistry in the Infrared:High-Resolutio n-Spectroscopy and MolecularStructure of Carbon-Silicon-Clusters

JURGEN KRIEG1

1 Universitat zu Koln,email@missing

P-VI-3

Herschel and APEX Observations of Light Hydride Species:The Need for Further Laboratory Data and Developments in the CDMS

H. S. P. MULLER, C. P. ENDRES, AND J. STUTZKI

I. Physikalisches Institut, Universitat zu Koln, Germany,hspm@ph1.uni-koeln.de

Observations of CH+, J = 1 − 0 and2 − 1 near 0.835 and 1.67 THz with Herschel/HIFI and of13CH+, J =1 − 0 near 0.830 THz with APEX revealed their rest frequencies to be higher than the accepted values by 21and 30 km/s, respectively. Very recent laboratory measurements of theJ = 1 − 0 transition frequencies ofCH+, 13CH+ and CD+ by Amano (2010) and fits to these as well as electronic spectral data by Muller (2010)resolved the descrepancies. Similarly, Asvany et al. (2008) employed radiation induced reactions to show that theJKaKc

= 101 − 000 transition of H2D+ near 1.37 THz is lower by∼13.5 km/s than the previously accepted value.Finally, the Herschel/HIFI detection of theNKaKc

= 111 −000, J = 1.5−0.5 transition of H2O+ near 1.115 THzby Ossenkopf et al. (2010) along with subsequent observations raised the issue which of the apparently conflictingpredictions from two different laboratory spectroscopic studies provide the best rest frequencies, if any. The morerecent observations seem to indicate the laboratory data from Murtz et al. (1998) to be reliable which in turn wouldrequire more complex LSR velocity structures toward other sources, e.g. DR 21. Since the quality of predictionsof spectra provided, e.g., in the Cologne Database for Molecular Spectroscopy (CDMS; www.cdms.de; Muller etal., 2001, 2005) depend critically on the availability of rest-frequencies known with sufficient accuracy, a need forfurther laboratory spectroscopic studies, in particular for cationic light hydride species, is rather obvious. Theseand possibly additional examples will be presented in some detail. The mostly very different needs for ALMA,not only to identify all relevant lines of so-called weed species, but also todetect new flowers, may be outlinedto some extent. Finally, we will provide information on putting the CDMS into a VirtualObservatory compliantdatabase environment.

References:Amano, T., 2010, ApJ, 716, L1Asvany, O. et al., 2008, Phys. Rev. Lett., 100, 23304Muller, H. P. S. et al., 2001, A&A, 370, L49Muller, H. P. S. et al., 2005, J. Mol. Struct., 742, 215Muller, H. P. S., 2010, A&A, in press; DOI: 10.1051/0004-6361/201014398Murtz, P. et al., 1998, J. Chem. Phys., 109, 9744Ossenkopf, V., 2010, A&A, in press; http://de.arxiv.org/abs/1005.2521

P-VI-4

Deuterium chemistry : measuring the age of prestellar cores

L. PAGANI1, P. LESAFFRE2

1 LERMA & UMR 8112 du CNRS, Observatoire de Paris, Francelaurent.pagani@obspm.fr2 LERMA & UMR 8112 du CNRS, Ecole Normale Superieure & Observatoire de Paris, France

pierre.lesaffre@ens.fr

Prestellar cores are an important step in the long processus forming low-mass stars. They appear in clouds asvery cold condensations of dust and gas, mostly traced by dust emission,and somewhat by nitrogen species, NH3,N2H+ and their isotopologues. Their temperature can be below 10 K and density upto a few 106 cm−3. Severalscenarii exist to describe their formation, such as free-fall, inside-outcollapse, ambipolar diffusion, turbulence-driven,... which imply different time scales from less than 105 years to ten times more. Up to now, it has provenvery difficult to estimate the age of the cores (as a lower limit of their lifetime), because the usual clocks, basedon chemical models, are very sensitive to the initial conditions in the clouds which are not known. By looking atthe N2D+/N2H+ ratio together with the H2D+ abundance along the L183 core profile, we have shown that it ispossible to set a lower limit to the age of the core (Pagani et al. 2009) which islittle dependent upon the initialconditions. As long as depletion has not set in, N2D+ and N2H+ are being destroyed efficiently by CO and areabsent (at a detectable level) from the cloud. The CO freezing-out marks the beginning of their apparition andtherefore starts the Deuterium clock. We have combined this chemical network to a 1D dynamical model (Lesaffreet al. 2005) to reproduce the well-known properties of the L183 core (Pagani et al. 2004, 2005, 2007). Preliminaryresults will be presented.References:Pagani, L., et al. 2004, A&A 417, 635Pagani, L., et al. 2005, A&A 429, 181Lesaffre, P., Belloche, A., Chize, J.-P., Andr, P. 2005, A&A 443, 961Pagani, L., et al. 2007, A&A 467, 179Pagani, L., et al. 2009, A&A 494, 623

P-VI-5

Deuterium astrochemistry

BERENGEREPARISE1

1 MPIfR, bparise@mpifr-bonn.mpg.de

P-VI-6

There is MAGIX in CATS

P. SCHILKE1, T. MOLLER1, D. PANOGLOU1, I. BERNST1, V. OSSENKOPF1, M. ROLLIG1, J. STUTZKI1, AND

D. MUDERS2

1 I. Physikalisches Institut der Universitat zu Koln, Zulpicher Str. 77, 50937 Koln, Germany,schilke,moeller,panoglou,bernst,ossk,roellig,stutzki@ph1.uni-koeln.de

2 MPIfR, Auf dem Hugel 69, 53121 Bonn, Germanymuders@mpifr.de

CATS12 is an ASTRONET funded project German-French-Swedish Project thatwill provide common toolsand databases for astrophysical applications. One part of it is MAGIX34, which strives at providing a commonframework for modeling astronomical observations. (M)any theoretical models can plug into it, and its goal is toprovide the best-fit parameters, within the framework of the model, to a particular data set, including confidenceintervals for the parameters. It consists of a frontend to register new models, and to create model instances, i.e. setup a model with initial conditions, the fitting engine, and an output module. MAGIXis able to read a variety ofmodel data formats, including FITS, and has a number of algorithms avialable for finding the best fit: Levenberg-Marquardt, Simulated Annealing, as well as programs for exploring the parameter space, Bee’s algorithm andNested Sampling. The latter can also be used to determine the confidence intervals of parameters. The output willbe the best-fit model, the best-fit parameters, with an estimate of the goodnessof fit and the confidence intervalsand, optionally, an exploration of the parameter space, i.e. information about the existence of other minima.Parallelization of the Levenberg-Marquardt Algorithm has been achieved, and is under way for other algorithms.Pre-registered models include myXCLASS, myCloud, and RATRAN. In the final version, it is envisioned thatMAGIX will have a Heuristics module that will choose the best combination of algorithms based on user-definedpriorities. MAGIX has been used for fitting Herschel/HIFI data from line surveys, with great success.

1Coherent set of Astrophysical Tools for Spectroscopy2https://www.astro.uni-koeln.de/projects/schilke/CATS3Modeling and Analysis Generic Interface for eXternal numerical codes4https://www.astro.uni-koeln.de/projects/schilke/MAGIX

P-VI-7

Laboratory Astrochemistry in the Infrared:High-Resolution-Spectroscopy and Molecular Structure of Carbon-Silicon-Clusters

J. KRIEG, V.LUTTER, I. GOTTBEHUT, T. F. GIESEN, S. SCHLEMMER, AND S. THORWIRTH

I. Physikalisches Institut, Universitat zu Koln, Zulpicher Str. 77, 50937 Koln, Germanysthorwirth@ph1.uni-koeln.de

Many of the molecules found in space are carbonaceous, that is, they have a carbon backbone in their structure. Inaddition, many of these molecules carry heteroatoms such as nitrogen and oxygen and also second row elementssuch as silicon. To date, four silicon-carbon molecules SiCn (n = 1 − 4) have been detected in space and severalmore by high-resolution spectroscopic techniques in the laboratory. Owingto their symmetry, many clusters of theform SiCnSi are non-polar and hence have no pure rotational spectrum. In an effort to obtain the gas-phase spectraof these clusters in the infrared, we have started a dedicated laboratory program employing diode laser techniquesand more recently an optical parametric oscillator-based spectrometer operating at 5 microns, where many carbon-and carbon-silicon chains are expected to exhibit strong infrared-active vibrational modes. These studies shallsupport astronomical searches for these molecules with present and future astronomical infrared experiments.Owing to their importance for structural and theoretical chemistry, another major goal of this study is to determineaccurate molecular structures of selected clusters from a combination of experimental data and high-level quantumchemical calculations.

P-VI-8

Probing the Water Chemistry in Young Stellar Objects with Hydroxyl Observations

S.F. WAMPFLER1, G.J. HERCZEG2, S. BRUDERER1, A.O. BENZ1, E.F.VAN DISHOECK2,3,L.E. KRISTENSEN3, T.A. VAN KEMPEN4, S.D. DOTY5, R. VISSER3, U.A. Y ILDIZ 3 AND THE WISH TEAM

1 Institute for Astronomy, ETH Zurich, Switzerlandwampfler@astro.phys.ethz.ch,simonbr@astro.phys.ethz.ch, benz@astro.phys.ethz.ch

2 Max Planck Institut fur Extraterrestrische Physik, Garching, Germanygregoryh@mpe.mpg.de3 Leiden Observatory, Leiden University, The Netherlandsewine@strw.leidenuniv.nl,

kristensen@strw.leidenuniv.nl,ruvisser@strw.leidenuniv.nl, yildiz@strw.leidenuniv.nl

4 Harvard-Smithsonian Center for Astrophysics, Cambridge, USAtvankemp@cfa.harvard.edu5 Department of Physics and Astronomy, Denison University, Granville, USA doty@denison.edu

Water is the third most abundant molecule in star-forming regions and therefore plays a crucial role in both thechemistry and physics during the embedded evolutionary phases of youngstellar objects. Many of the speciesinvolved in the chemical reaction network of water can only be observed from space. One of the main waterphoto-dissociation products at temperatures typical for protostellar envelopes is the hydroxyl radical (OH). Chem-ical models predict the OH abundance to rise under irradiation and therefore to trace ionizing protostellar radiation(X-rays, FUV).Previous observations of OH with the ISO satellite have shown that it acts as an important molecular coolant (Gi-annini et al., 2001), but did not allow to disentangle the contribution of the various components like envelope,outflow, etc. contained in the large80′′ beam. The Herschel Space Observatory allows for the first time to observemany OH FIR transitions at a high spatial and spectral resolution. First results from PACS observations towardsthe low-mass, class I young stellar object HH 46 have shown that OH peaksstrongly on source, while other specieslike water are much more extended (van Kempen et al., 2010).We investigate the OH line ratios obtained from PACS observations for different sources and compare them tomodel predictions as well as water and oxygen observations. Spectrally resolved HIFI observations of the OH hy-perfine structure transitions at 163µm towards HH 46 yielded a non-detection, implying that the OH lines mightbe much broader than expected. Upcoming HIFI observations of more luminous sources will allow to derive theOH abundance more accurately and thus better constrain the chemistry of water during the protostellar evolution.

References:Giannini, T., Nisini, B. and Lorenzetti, D. 2001, ApJ, 555, 40van Kempen, T., Kristensen, L.E. et al., 2010, A&A, accepted

P-VI-9

Observations of the K-Doublet Lines of H2CO

A. WOOTTEN1, J. MANGUM1 AND P. MCCAULEY1,2

1 NRAO,awootten@nrao.edu,jmangum@nrao.edu2 James Madison University,jmccaunrao.edu

We have used the Green Bank Telescope to observe the J=2, 3 and 4 K-doublet transitions of formaldehyde. Themolecule is abundant and excellent sensitivity and resolution are achieved, resulting in detection of the lines innearly two dozen star formation sites. Although the lower transitions are well known to be refrigerated and seen inabsorption in a variety of regions, at high density the J=k and J=4 lines should be seen in emission, in accord withthe few published observations. Our observations show that these optically thin lines are useful as densitometersfor star-forming molecular clouds, probing regions with spatial densities around n(H2)∼ 1-2 x 106 cm−3.References:McCauley, P., Mangum, J., & Wootten, A. 2010, Bulletin of the American Astronomical Society, 41, 256

P-VI-10

Line Survey of L1157 B1 Shocked Region

T. YAMAGUCHI1, M. SUGIMURA1, T. SAKAI 1, T. UMEMOTO2, N. SAKAI 1,S. TAKANO2, Y. A IKAWA 3, N. HIRANO4, S. Y. LIU4, H. NOMURA5, Y. N. SU4, S. TAKAKUWA 4,

T. M ILLAR 6, S. YAMAMOTO1 AND L INE SURVEY GROUPMEMBERS

1 University of Tokyo,takahiro@taurus.phys.s.u-tokyo.ac.jp2 Nobeyama Radio Observatory, National Astronomical Observatory of Japan3 Kobe Univerity4 ASIAA 5 Kyoto University6 Queen’s University Belfast

L1157 B1 (d = 440 pc) is a famous schocked region formed by an interaction between thebipolar outflow fromthe low mass protostar IRAS 20386+6751 and the ambient gas, which was discovered by Umemoto et al. (1992)and Mikami et al. (1992). Strong SiO emission (Mikami et al. 1992) and infrared emission (Hodapp 1994)are detected, which are unambiguous evidences of the shock. So far, anumber of molecular species have beendetected by Bachiller et al. (1997) and Avery and Chiao. (1996). Arceet al. (2008) recently reported detections ofHCOOCH3, CH2H5OH and HCOOH.

We are conducting a spectral line survey of L1157 B1 with the Nobeyama 45m telescope in order to exploreshock chemistry in detail. Because of the simplicity of the shock structure as mentioned above, we can study“pure” shock chemistry without contaminations of other star-formation activities. So far, we have covered thefrequency range of 13.7 GHz (82-94.5, 96.3-97 GHz), and have detected 20 species including 9 isotopomers and67 lines. The new 2SB SIS receiver installed at the 45 m telescope is used toperform very sensitive observationswith a typical rms noise of 5 mK. We have detected various organic molecules such as HCOOCH3, CH3CHO,HCOOH, HNCO, HCNO and CH3CN. We have also detected the line of CH2DOH. This result demonstrates richorganic chemistry in a shocked region, which would mainly originate from evaporation of grain mantles by shockheating.References:Arce, H. G. et al. 2008, ApJ, 681, L21.Avery, L. W. and Chiao, M., 1996, ApJ, 463, 642.Bachiller and Perez Gutierrez, 1997, ApJ, 487, L93.Hodapp, K. W., 1994, ApJS, 94, 615.Mikami, H. et al. 1992, ApJ, 392, L87.Turner, B. E. et al. 1989, ApJ, 539, 622.Umemoto, T. et al. 1992, ApJ, 392, L83.

Session VII:Future opportunities

P-VII-1

Submillimeter and THz Receiver Development at KOSMA

U.U. GRAF, M. BRASSE, T. GRAMBUSCH, N. HURTADO, M. JUSTEN, O. RICKEN, AND J. STUTZKI

KOSMA, I. Physikalisches Institut, University of Cologne,<lastname>@ph1.uni-koeln.de

We present the recent and current development of heterodyne receiver frontends for submm and THz astronomyin the KOSMA group. Projects include receivers for ground based observatories (NANTEN2, APEX) as well asairborne (SOFIA) and balloon-borne (STO) platforms.

For all platforms we are developing multi-pixel receivers to maximize the science output under the difficultobserving conditions of this wavelength regime. A key ingredient is the increasing usage of integrated, monolithicoptics units, which facilitate the construction and improve the optical performance of the instruments.

A major obstacle for the development of large format array receivers atTHz frequencies is the lack of suf-ficiently powerful local oscillator sources. This problem is being attackedby an effort to improve the frequencycontrol of quantum cascade lasers (QCLs) to make them available as THz LO sources.

P-VII-2

The German SOFIA first light instrument GREAT: status and futur e opportunities

S. HEYMINCK1, R. GUSTEN1, B. KLEIN1, T. KLEIN1, I. CAMARA 1, J. STUTZKI2, U.U. GRAF2, K. JACOBS2,P. PUTZ2, H-W. HUBERS3, AND P. HARTOGH4

1 Max-Planck-Institut fur Radioastronomie,heyminck@mpifr-bonn.mpg.de2 KOSMA, I. Physikalisches Institut der Universitat zu Koln

3 DLR Institut fur Planetenforschung4 Max-Planck-Institut fur Sonnensystemforschung

GREAT on board of SOFIA will offer unique heterodyne observing capabilities in the frequency range abovethe highest Herschel/HIFI-bands. In the post-Herschel/HIFI phase itwill provide the only opportunity for FIRheterodyne observations at frequencies not accessible from ground. GREAT is planed to be shipped to the NASAPalmdale facilities, the present home of SOFIA, in October this year. First science flights with GREAT are expectedin the first half of 2011.

GREAT is a far-infrared heterodyne receiver based on a modular receiver concept, developed by a consortiumof four German science institutes. In its first incarnation the receiver will offer four independent receiver channelsout of which two can be operated simultaneously:

L#1 : 1.25 – 1.53 THz, including a.o.[NII], CO(12 − 11), 13CO(13 − 12), HCN(17 − 16), H2D+

L#2 : 1.82 – 1.92 THz, targeting at e.g.[CII], CO(16 − 15)

M : 2.5 – 2.7 THz, targeting atHD, OH(2π3/2), CO(22 − 21), 13CO(23 − 22)

H : 4.7 THz, targeting at the[OI]-line

We report on the current GREAT instrument status shortly before deployment and present our ongoing devel-opment activities. GREAT with its modular concept offers the possibility to implement small scale heterodynefocal plane arrays. We are currently working on a design for hexagonal 7 pixel[OI] and/or[CII] mappers. Withinthe GREAT instrument framework even a dual polarization 2× 7 pixel [CII] array would be possible. Thesefuture upgrades will become possible because of ongoing basic research activities for critical technologies withinthe GREAT consortium. We mention the continuing performance enhancements of the waveguide-based HEBmixers at KOSMA (providing increasingly wider IF bandwidth, and operating now for the M-channel) and the de-velopments for a quantum cascade laser (QCL) based local oscillator source for the H-band channel at the DLR inBerlin. At the MPIfR in Bonn our long term research project on photonicsLO systems now results in the design ofa 2.7 THz flight LO-system for the M-band channel. Our next generationFast Fourier transform spectrometer de-velopments now provide 2.5 GHz of instantaneous bandwidth, which will allow tocover large IF-bandwidths withhigh spectral resolution (32 k channels) also for array receivers in aspace, weight and power limited environmentsuch as the SOFIA aircraft.

P-VII-3

KOSMA Submm and THz Detector Development

C.E. HONINGH, K. JACOBS, P. PUTZ, M. JUSTEN, M.P. WESTIG, S. ANDREE, S. SELIG, S. WULFF, M.SCHULTZ, AND J. STUTZKI

KOSMA, I. Physikalisches Institut, Universitat zu Koln, Koln, Germanylastname@ph1.uni-koeln.de

KOSMA Submm and THz detector development for radioastronomical heterodyne receivers is dedicated to stateof the art superconducting detector development for the frequencies of approximately 0.2-10 THz. We presentlyfocus on extending the range of quantum limited detection with Superconductor-Isolator-Superconductor (SIS)mixers to 2 THz by the development of SIS devices with high current density barriers and electrodes with ahigh superconducting gap frequency. For frequencies higher than 2THz we are advancing the development ofHot Electron Bolometer (HEB) mixers. In addition advanced mixers schemes for large instantaneous bandwidth,balanced and sideband separation that are compatible with large focal plane arrays of mixers are being developed.The KOSMA superconducting detector group has contributed the SIS mixers for e.g. the band 2 of the HerschelSpace Observatory and the ground based observatories Nanten, KOSMA (Gornergrat) and AST/RO (South Pole).Our HEB mixers for 1.4 THz and 1.9 THz will be used in the SOFIA first light heterodyne receiver GREATand for the 1.9 THz channel of the Stratospheric Terahertz Observatory (STO). All mixers are based on in-housewaveguide micro-machining and superconducting device fabrication. We will report on our current developmentof SIS and HEB mixer designs using silicon and silicon nitride membranes and integrated beamlead technology.

References:[1] P. P. Munoz, S. Bedorf, M. Brandt, T. Tils, N. Honingh, and K. Jacobs, ”THzWaveg-uide Mixers With NbTiN HEBs on Silicon Nitride” Membranes, IEEE MWCL, vol. 16,no. 11, pp. 606-608, 2006[2] R. Teipen, M. Justen, S. Glenz, P. Putz, K. Jacobs, C.E. Honingh , ”Results and Anal-ysis or HIFI Band 2 Flight Mixer Performance”, Proc. of the 16th Intern. Symposium onSpace Terahertz Technology, Goteborg, Sweden, 2005

List of Participants

187

Abergel, Alain, CNRS/Universite Paris-Sud 11 alain.abergel@ias.u-psud.frAkyilmaz Yabaci, Meltem, Universitat zu Koln meltem@ph1.uni-koeln.deAli, Babar, NHSC/IPAC/Caltech babar@ipac.caltech.eduAlkhasawneh, Abeer, Balqaa applied university aseel00@yahoo.comAlmohammad, Abdalla, Balqaa applied university aseel00@yahoo.comAnderl, Sibylle, University of Bonn sanderl@astro.uni-bonn.deAndre, Philippe, CEA Saclay pandre@cea.frAndrews, Brett, The Ohio State University andrews@astronomy.ohio-state.eduArab, Heddy, Institut dAstrophysique Spatiale heddy.arab@ias.u-psud.frBagetakos, Ioannis, University of Hertfordshire i.bagetakos@herts.ac.ukBenford, Dominic, NASA / GSFC dominic.benford@nasa.govBenz, Arnold, ETH Zurich benz@astro.phys.ethz.chBergin, Edwin, University of Michigan ebergin@umich.eduBerne, Olivier, Leiden Observatory berne@strw.leidenuniv.nlBertoldi, Frank, Universitat Bonn bertoldi@astro.uni-bonn.deBillot, Nicolas, NASA Herschel Science Center - Caltech nbillot@ipac.caltech.eduBottinelli, Sandrine, CESR sandrine.bottinelli@cesr.frBremer, Malcolm, University of Bristol m.bremer@bristol.ac.ukBrinks, Elias, University if Hertfordshire e.brinks@herts.ac.ukBruderer, Simon, ETH Zurich simonbr@astro.phys.ethz.chBurton, Michael, University of New South Wales m.burton@unsw.edu.auCabrit, Sylvie, Observatoire de paris sylvie.cabrit@obspm.frCambresy, Laurent, Observatoire de Strasbourg cambresy@astro.unistra.frCarlhoff, Philipp, Universitat zu Koln carlhoff@ph1.uni-koeln.deCaux, Emmanuel, CESR/CNRS - University of Toulouse caux@cesr.frCeccarelli, Cecilia, Laboratoire d’Astrophysique de Grenoble Cecilia.Ceccarelli@obs.ujf-grenoble.frCernicharo, Jose, CAB. INTA-CSIC jcernicharo@cab.inta-csic.esChavarria, Luis, Laboratoire d’Astrophysique de Bordeaux luisagustinchavarria@gmail.comComito, Claudia, Max-Planck-Institut fur Radioastronomie ccomito@mpifr.deCormier, Diane, CEA Saclay diane.cormier@cea.frCostagliola, Francesco, Chalmers University of Technology francesco.costagliola@chalmers.seCoutens, Audrey, CESR audrey.coutens@cesr.frCrockett, Nathan, University of Michigan ncrocket@umich.eduCubick, Markus, Universitat zu Koln cubick@ph1.uni-koeln.deDave, Romeel, University of Arizona rad@as.arizona.edude Graauw, Thijs, ALMA Observatory tdegraau@alma.clDe Looze, Ilse, University of Ghent ilse.delooze@ugent.beDe Luca, Massimo, LERMA, CNRS, Observatoire de Paris, ENS massimo.de.luca@lra.ens.frDecin, Leen, Instituut voor Sterrenkunde Leen.Decin@ster.kuleuven.beDedes, Carolin, ETH Zurich carolin.dedes@astro.phys.ethz.chDobbs, Clare, MPE cdobbs@mpe.mpg.deDubernet, Marie-Lise, Universite Pierre et Marie Curie (UPMC) marie-lise.dubernet-tuckey@upmc.frEales, Stephen, Cardiff University sae@astro.cf.ac.ukEndres, Christian, University of Cologne endres@ph1.uni-koeln.deEsteras, Luis, Max Planck Institute for Radio Astronomy lesteras@mpifr.deFiedler, Simone, AIU Jena simone.fiedler@uni-jena.deFukui, Yasuo, Nagoya University fukui@a.phys.nagoya-u.ac.jpGarcia, Pablo, I. Physikalisches Institut pablo@ph1.uni-koeln.deGeppert, Wolf D., Stockholm University wgeppert@hotmail.comGlover, Simon, University of Heidelberg sglover@ita.uni-heidelberg.deGoicoechea, Javier R., Centro de Astrobiologia (CSIC-INTA) jr.goicoechea@cab.inta-csic.esGoldsmith, Paul, JPL/Caltech Paul.F.Goldsmith@jpl.nasa.govGreene, Thomas, NASA ARC tom.greene@nasa.govGriffin, Matt, Cardiff University matt.griffin@astro.cf.ac.uk

188

Guan, Xin, Universitat zu Koln guan@ph1.uni-koeln.deGusdorf, Antoine, Max Planck Institut fur Radioastronomie agusdorf@mpifr-bonn.mpg.deGusten, Rolf, MPI Radioastronomie rguesten@mpifr.deHarris, Andrew, University of Maryland harris@astro.umd.eduHarwit, Martin, Cornell University harwit@verizon.netHatsukade, Bunyo, Nobeyama Radio Observatory hatsukade@nro.nao.ac.jpHelmich, Frank, SRON Netherlands Inst. for Space Research f.p.helmich@sron.nlHennebelle, Patrick, Observatoire de Paris patrick.hennebelle@ens.frHerpin, Fabrice, LAB/OASU herpin@obs.u-bordeaux1.frHeyminck, Stefan, Max-Planck-Institut fur Radioastronomie heyminck@mpifr-bonn.mpg.deHony, Sacha, Service dAstrophysique, CEA Saclay sacha.hony@cea.frHussain, Sadiq, University of Peshawar sadiqedu@hotmail.comIbanez, Miguel, Universidad de los Andes ibanez@ula.veIkarashi, Soh, University of Tokyo ikarashi@ioa.s.u-tokyo.ac.jpIsrael, Frank, Sterrewacht Leiden israel@strw.leidenuniv.nlJager, Cornelia, Institute of Solid State Physics cornelia.jaeger@uni-jena.deJastrzebska, Magda, Astronomical Observatory kulczak@oa.uj.edu.plJohnstone, Doug, NRC Canada/HIA doug.johnstone@nrc-cnrc.gc.caKarpov, Alexandre, Calif karpov@phobos.caltech.eduKazmierczak, Maja, Nicolaus Copernicus University maja.kazmierczak@gmail.comKennicutt, Robert, University of Cambridge robk@ast.cam.ac.ukKhasawneh, Abeer, Balqaa Applied University aseel00@yahoo.comKohno, Kotaro, University of Tokyo kkohno@ioa.s.u-tokyo.ac.jpKrabbe, Alfred, Universitat Stuttgart krabbe@dsi.uni-stuttgart.deKramer, Carsten, IRAM kramer@iram.esKrause, Oliver, Max-Planck-Institut fur Astrononie krause@mpia.deKristensen, Lars, Leiden Observatory kristensen@strw.leidenuniv.nlLanger, William, JPL - Caltech William.Langer@jpl.nasa.govLefloch, Bertrand, LAOG lefloch@obs.ujf-grenoble.frLeurini, Silvia, MPIfR sleurini@mpifr.deLi, Di, Jet Propulsion Lab dili@jpl.nasa.govLindner, Robert, Rutgers University lindner@physics.rutgers.eduLis, Darek, Caltech dcl@caltech.eduLord, Steven, Caltech lord@ipac.caltech.eduLutz, Dieter, MPE lutz@mpe.mpg.deMadden, Suzanne, CEA, Saclay suzanne.madden@cea.frMangum, Jeff, NRAO jmangum@nrao.eduMartin-Pintado, Jesus, CAB(CSIC-INTA) jmartin.pintado@iem.cfmac.csic.esMeixner, Margaret, Space Telescope Science Institute hill@stsci.eduMeyer, Michael R., ETH Zurich mmeyer@phys.ethz.chMolina, Faviola, ZAH fmolina@ita.uni-heidelberg.deMolinari, Sergio, INAF-IFSI molinari@ifsi-roma.inaf.itMorales, Esteban, Max-Planck-Institut fuer Radioastronomie emorales@mpifr-bonn.mpg.deMorris, Mark, UCLA morris@astro.ucla.eduMuller, Holger, Universitat zu Koln hspm@ph1.uni-koeln.deMurray, Norman, University of Toronto murray@cita.utoronto.caNomura, Hideko, Kyoto University nomura@kusastro.kyoto-u.ac.jpOkada, Yoko, Universitat zu Koln okada@ph1.uni-koeln.deOlberg, Michael, SRON/Onsala Space Observatory michael.olberg@chalmers.seOliver, Sebastian, University of Sussex S.Oliver@Sussex.ac.ukO’Rourke, Douglas, Univeristy of Cambridge djo33@cam.ac.ukOssenkopf, Volker, Universitat zu Koln ossk@ph1.uni-koeln.dePagani, Laurent, Observatoire de Paris laurent.pagani@obspm.frParise, Berengere, MPIfR bparise@mpifr-bonn.mpg.de

189

Perez-Fournon, Ismael, Instituto de Astrofisica de Canarias ipf@iac.esPety, Jerome, IRAM pety@iram.frPezzuto, Stefano, IFSI - INAF pezzuto@ifsi-roma.inaf.itPilbratt, Goran, European Space Agency gpilbratt@rssd.esa.intPineda, Jorge, Jet Propulsion Laboratory Jorge.Pineda@jpl.nasa.govPlume, Rene, University of Calgary plume@ras.ucalgary.caPoglitsch, Albrecht, Max-Planck-Institut fur extraterrestrische Physik alpog@mpe.mpg.dePon, Andy, University of Victoria andypon1@shaw.caQin, Sheng-Li, I. Physikalisches Institut, Universitat qin@ph1.uni-koeln.deRangwala, Naseem, University of Colorado - Boulder naseem.rangwala@colorado.eduRequena Torres, Miguel Angel, Max-Planck-Institut fuer Radioastronomie mrequena@mpifr-bonn.mpg.deRichter, Matthew, UC Davis mjrichter@ucdavis.eduRolffs, Rainer, Max-Planck-Institut fur Radioastronomie rrolffs@mpifr.deRollig, Markus, Universitat zu Koln roellig@ph1.uni-koeln.deRoman-Duval, Julia, Space Telescope Science Institute duval@stsci.eduRubio, Monica, Universidad de Chile mrubiodas@uchile.clSakai, Nami, The University of Tokyo nami@taurus.phys.s.u-tokyo.ac.jpSan Jose Garcia, Irene, Leiden University sanjose@strw.leidenuniv.nlSaraceno, Paolo, IFSI INAF saraceno@ifsi-roma.inaf.itSchilke, Peter, Universitat zu Koln schilke@ph1.uni-koeln.deSchlemmer, Stephan, University of Cologne schlemmer@ph1.uni-koeln.deSchneider, Nicola, CEA Saclay nschneid@cea.frSchuster, Karl-Friedrich, IRAM schuster@iram.frShimajiri, Yoshito, NAOJ yoshito.shimajiri@nao.ac.jpSimon, Robert, Universitat zu Koln simonr@ph1.uni-koeln.deSkibba, Ramin, University of Arizona rskibba@as.arizona.eduStaguhn, Johannes, Johans Hopkins University johannes.staguhn@nasa.govSternberg, Amiel, Tel Aviv University amiel@astro.tau.ac.ilSturm, Eckhard, Max-Planck-inst. f. Extraterr. Physics sturm@mpe.mpg.deStutzki, Jurgen, Universitat zu Koln stutzki@ph1.uni-koeln.deTamura, Yoichi, National Astronomical Observatory yoichi.tamura@nao.ac.jpThi, Wing-Fai, University Joseph Fourier Wing-Fai.Thi@obs.ujf-grenoble.frThorwirth, Sven, Universitaet zu Koeln sthorwirth@ph1.uni-koeln.deTielens, Alexander, Leiden University tielens@strw.leidenuniv.nlTosaki, Tomoka, Joetsu University of Education tosaki@juen.ac.jpTraficante, Alessio, University of Tor Vergata, Astrophysics alessio.traficante@roma2.infn.itUmehata, Hideki, Institute of Astronomy umehata@ioa.s.u-tokyo.ac.jpVaillancourt, John, Universities Space Research Institution jvaillancourt@sofia.usra.eduvan der Tak, Floris, SRON vdtak@sron.nlvan der Werf, Paul, Leiden Observatory pvdwerf@strw.leidenuniv.nlvan Dishoeck, Ewine, Leiden Observatory ewine@strw.leidenuniv.nlVastel, Charlotte, CESR vastel@cesr.frVelusamy, Thangasamy, Jet Propulsion Laboratory velusamy@jpl.nasa.govVerdolini, Silvia, Leiden University verdolini@strw.leidenuniv.nlVisser, Ruud, Leiden University ruvisser@strw.leidenuniv.nlWalmsley, Malcolm, INAF Osservatorio Astrofisico di Arcetri walmsley@arcetri.astro.itWalsh, Andrew, James Cook University andrew.walsh@jcu.edu.auWampfler, Susanne, Institute for Astronomy, ETH Zurich wampfler@astro.phys.ethz.chWatanabe, Yoshimasa, The University of Tokyo nabe@taurus.phys.s.u-tokyo.ac.jpWhite, Glenn, The Open University / Rutherford Lab glenn.white@stfc.ac.ukWolfire, Mark, University of Maryland mwolfire@astro.umd.eduWootten, Alwyn, NRAO awootten@nrao.eduWyrowski, Friedrich, MPIfR Bonn wyrowski@mpifr-bonn.mpg.deYamaguchi, Takahiro, University of tokyo takahiro@taurus.phys.s.u-tokyo.ac.jp

190

Yamamoto, Satoshi, The University of Tokyo yamamoto@phys.s.u-tokyo.ac.jpYildiz, Umut A., Leiden Observatory yildiz@strw.leidenuniv.nlYoung, Erick, SOFIA Science Center eyoung@sofia.usra.eduZinnecker, Hans, Univ. Stuttgart hzinnecker@aip.de

191

Notes

192