Allen et al. (2005)

Allen et al. (2005)Allen et al. (2005)

Johnstone et al. (2000)Johnstone et al. (2000)

Oph B2Oph B2

850 m continuum (JCMT) NH3 (1,1) int. intensity (GBT)

NHNH33 emission shows excellent (but not perfect) emission shows excellent (but not perfect) correspondence with dust continuum emissioncorrespondence with dust continuum emission

Tracing Dense Core Structure with NHTracing Dense Core Structure with NH33

Oph B2Oph B2

850 m continuum (JCMT) NH3 (1,1) int. intensity (GBT+ATCA)

NHNH33 emission shows excellent (but not perfect) emission shows excellent (but not perfect) correspondence with dust continuum emissioncorrespondence with dust continuum emission


NHNH33 (1,1) in Oph B (1,1) in Oph B

Only 20/48 hr observed so far, rest scheduled for Only 20/48 hr observed so far, rest scheduled for October+October+

BB11

B2B2

BB33

Friesen et al. (2006, in preparation)


NHNH33 in Oph B, C & in Oph B, C & FFOver next semester, will get more GBT and new VLA Over next semester, will get more GBT and new VLA

data:data: with (1,1) and (2,2) lines, will derive kinetic with (1,1) and (2,2) lines, will derive kinetic temperature across several Oph corestemperature across several Oph cores

with opacity, column densities + NHwith opacity, column densities + NH33 abundances abundances

with line widths, probe velocities; with Twith line widths, probe velocities; with TKK, get , get thermal and non-thermal motions simultaneously, thermal and non-thermal motions simultaneously, dynamicsdynamics


5 Rationales for a K-band 5 Rationales for a K-band FPAFPA increase NH3 observing speed by >1 order of increase NH3 observing speed by >1 order of

magnitude, map dense cores faster and with better magnitude, map dense cores faster and with better samplingsampling

allow for more serendipitous discovery (early allow for more serendipitous discovery (early cores?) with wider areal coverage of mapscores?) with wider areal coverage of maps

maximize usage of “precious” K-band conditions maximize usage of “precious” K-band conditions at GBat GB

improve core statistics significantly with NHimprove core statistics significantly with NH33 follow-up of new Galactic surveysfollow-up of new Galactic surveys

will provide crucial single-dish data for K-band will provide crucial single-dish data for K-band EVLA projectsEVLA projects

Promise of a GBT K-band FPAPromise of a GBT K-band FPA

Gould Belt consists of SF molecular clouds within Gould Belt consists of SF molecular clouds within 500 pc including Orion, Taurus, Ophiuchus, 500 pc including Orion, Taurus, Ophiuchus, Perseus, Serpens, etc.Perseus, Serpens, etc.

Grenier (2004)

Gould Belt: 3D schematic


Orion

CepheusFlare

IC 5146

Pipe Nebula

Ophiuchus

Taurus

Lupus

Serpens

R CrA

~110 sq. deg. at~110 sq. deg. at AAvv ≥ 3 ≥ 3

~1000 sq. deg. at~1000 sq. deg. at AAvv ≥ 1 ≥ 1Nutter (2005), after Cambrésy (1999)Nutter (2005), after Cambrésy (1999)

New Local SF Surveys:New Local SF Surveys:

• JCMT Legacy SurveyJCMT Legacy Survey: using : using SCUBA-2/HARP to map SCUBA-2/HARP to map Gould’s Belt clouds to AGould’s Belt clouds to Av v = 1-2 = 1-2 in 450/850 in 450/850 m + lines, m + lines, polarization in sub-regions polarization in sub-regions (2006+)(2006+)

• Herschel GT Key ProjectHerschel GT Key Project: : using SPIRE/PACS to map using SPIRE/PACS to map entirety of Gould’s Belt clouds entirety of Gould’s Belt clouds to Ato Av v > 3 at 80/110, 170, 250, > 3 at 80/110, 170, 250, 360, 520 360, 520 m (2008+)m (2008+)

• Spitzer c2d2 LegacySpitzer c2d2 Legacy: using : using IRAC+MIPS over GB clouds IRAC+MIPS over GB clouds (2003-2007)(2003-2007)

Herschel Space Observatory

SCUBA-2 HARP


Spitzer Space Telescope

Infrared Dark Clouds:Infrared Dark Clouds:Extinction features in the mid-IRExtinction features in the mid-IR

~10,000 cold dust clouds seen in silhouette ~10,000 cold dust clouds seen in silhouette against warmer background dust. against warmer background dust.

MSX 8 m continuum

from Jackson (2005)from Jackson (2005)



ll = 326-335 deg, | = 326-335 deg, |bb| < | < 1 deg1 deg

New Galactic Plane Surveys:New Galactic Plane Surveys:

• JCMT Legacy SurveyJCMT Legacy Survey: (JPS) using : (JPS) using SCUBA-2 to map |SCUBA-2 to map |bb| < 1 (2006+)| < 1 (2006+)

• Herschel OT Key ProjectHerschel OT Key Project: (HiGal) : (HiGal) using SPIRE/PACS to map |using SPIRE/PACS to map |bb| < 1 | < 1 (2008+; not yet approved)(2008+; not yet approved)

• Spitzer LegacySpitzer Legacy: (GLIMPSE1, 2, & : (GLIMPSE1, 2, & 3, MIPSGAL) (2003-2007), using 3, MIPSGAL) (2003-2007), using IRAC and MIPS over various IRAC and MIPS over various ranges of ranges of ll

• HI SurveysHI Surveys: (IGPS, etc.), high-: (IGPS, etc.), high-resolution 21 cm mappingresolution 21 cm mapping

Herschel Space Observatory

SCUBA-2


Spitzer Space Telescope

Summary: K-band FPASummary: K-band FPA synergistic, unique data to other single-dish synergistic, unique data to other single-dish FPAsFPAs

allow large surveys of NHallow large surveys of NH33 emission, yielding emission, yielding kinetic temperatures, column densities, and kinetic temperatures, column densities, and insight into the dense core dynamics; improve insight into the dense core dynamics; improve core statisticscore statistics

maximize use of “precious” K-band conditions maximize use of “precious” K-band conditions in Green Bankin Green Bank

provide crucial single-dish data for K-band provide crucial single-dish data for K-band EVLA projects in NHEVLA projects in NH33, CCS, HC, CCS, HC33N, RRLs, HN, RRLs, H22O O masers, etc.masers, etc.

a 10 x 10 array could yield 5’ x 5’ full-beam a 10 x 10 array could yield 5’ x 5’ full-beam coveragecoverage

Mr. KLEANMr. KLEAN

K-band Line Emission Array of K-band Line Emission Array of NraoNrao

Documents

Allen et al. (2005)