Aug 8th, 2007MAGPOP Summer School Extragalactic infrared and submillimetre surveys Michael Rowan-Robinson Imperial College London Dole et al 2006 most

Aug 8th, 2007 MAGPOP Summer School

Extragalactic infrared and submillimetre surveys

Michael Rowan-RobinsonImperial College London

Dole et al 2006

most of the starlight ever generated in the universe is emitted at infrared wavelengths, ~ 50% is absorbed by dust and reemitted at far infrared and submillimetre wavelengths


1 micron - 1 mm

- a few terrestial windows

the infrared and submillimetre bands


Pre-IRAS, IRAS

Pre-IRAS: 1969: Caltech 2 Micron Survey (Neugebauer and Leighton) – circumstellar dust shells, BN object1976: The AFGL Survey at 4.2, 11, 19.8 and 27.4 m

(Price and Walker) – cds, HII regionsIRAS:1984: IRAS all sky survey at 12, 20, 60, 100 m

- 30,000 infrared galaxies (measured redshifts of 12000 with S(60)>0.6 Jy - PSCz)

- ir cirrus- ULIRGS, HLIRGS- AGN dust tori- ir dipole, large scale structure


IRAS

Horsehead Nebula


IRAS all-sky survey


Infrared galaxy populations

with IRAS we were able to identify the main infrared galaxy populations

- quiescent galaxies (ir cirrus)- starburst galaxies (prototype M82)- extreme starbursts (prototype A220)- AGN dust tori

but the IRAS survey was not deep enough (z ~ 0.3) to study the cosmological evolution of these populations, though 60 m source-counts showed that evolution is present, at a comparable rate to that seen in radio-galaxies and quasars

an important insight was that as infrared luminosity increased, the proportion of interactions and mergers increased


ISOISO, launched 1996, reached z~1, + spectroscopy


ISO surveysCAM Deep Surveys

Fadda et al, 2001, AA, astro-ph/011412 Franceschini et al, 2002, AA,

astro-ph/0108292Elbaz et al, 2002, AA 384, 848

ELAIS Survey at 6.7, 15, 90, 175 mOliver et al, 2000, MN 316, 749Serjeant et al, 2000, MN 316, 768Efstathiou et al, 2000, MN 319, 1169Serjeant et al, 2001, MN 322, 262Lari et al, 2001, MN 325, 1173Gruppioni et al, 2002, MN 341, L1Rowan-Robinson et al, 2004, MN 351,

1290ISO HDF-N and HDF-S surveys

Oliver et al, 2002, MN 332, 546Mann et al, 2002, MN 332, 549

FIRBACK 175 m surveyDole et al, 2001, AA 372, 264


ISO surveys * main result was very strong increase in star-formation rate in galaxies between z = 0 and 1 (factor ~10) (Rowan-Robinson et al 1997, Flores et al 1999), confirming the result from optical surveys (Lilley et al 1996, Madau et al 1996) and that the rate estimated from optical data without correction for extinction is severely underestimated.

• problems of screen model for extinction correction

• issue of consistency between estimates of star-formation rate from uv, H, radio, far infrared

sfr = 2.2 x 10-10 L60 = 2.5x10-8 LH = 4.5x10-10 L2800A


Dust extinction in local galaxies

<AV> ~ 0.3 in local galaxies(Rowan-Robinson, 2003, MN 344, 13)


comparison of star-formation rate estimates

Daddi et al 2007


HDFN at 850 mHughes et al 1998

impact of JCMT

SHADES

blank field surveys at 850 m showed that we were able to survey the whole universe to z = 5 with ultraluminous ir galaxies


Submillimetre surveysHubble Deep Field North

Hughes et al 1998

Hawaii surveysBarger et al 1998, 1999, Cowie et al 2002, Wang et al 2004

CUDSS surveyEales et al 1999, Webb et al 2003,Clements et al 2004, Ashby et al 2006

UK 8 mJy survey (200 sq arcmin)Scott et al 2001, Fox et al 2001,Ivison et al 2002, Almaini et al 2003

SHADES (0.5 sq deg)Mortier et al 2005, Coppin et al 2006, Ivison et al 2007, Aretxaga et al 2007


submillimetre associations and galaxy redshift distribution

Chapman et al, 2005, ApJ 622, 772 poor spatial resolution of JCMT means that reliable optical or infrared associations can only be made if have millimetreinterferometry or radio associations

why don’t we see submm galaxies at z > 4 ?

is this a selection effect ?


Near-ir Surveys2MASS all-sky survey at J, H, K (to 15.8, 15.1, 14.3 mag.)

– http://www.ipac.caltech.edu/2mass/UKIDDS survey of 7500 sq deg in JHK (K=18.3)

-http://www.ukidss.org/

FIR SurveysSPITZER surveys (GTO - various, FLS - 4 sq deg, SWIRE - 49 sq deg, GOODS - 0.1 sq deg, AEGIS - 1 sq deg, COSMOS - 1 sq deg) at 3.6, 4.5, 5.6, 8, 24, 70, 160 m

- http://ssc.spitzer.caltech.edu/

ASTRO-F all-sky survey in 6 bands at 9-180 m- http://www.akari.org.uk


2MASS• 2MASS provides a better picture of galaxy distribution at z<0.03


Layered SPITZER Surveys• Wide–shallow FLS GTO-shallow SWIRE

– greatest volume 4 8.5 49 sq deg

– rare luminous objects

– large-scale structure

• Confusion-limited GTO-deep GOODS-IRAC– maximum information 2.5 sq deg 300 sq arcmin

on faintest resolved sources

• Ultra-deep GTO-ultra GOODS-24 m– confusion distribution 150 300 sq arcmin


M51Sombrero

combined 3.6, 8 and 24 m images(SINGS consortium)


M82N2207/IC2163

Stefan’s Quintet


SIRTF SWIRE survey

49 sq deg in 6 areas, at 3.6, 4.5, 5.8, 8, 24, 70, 160 m


ELAIS N1: 9 sq. deg

SWIRE 3.6 m survey in ELAIS-N1


Photometric redshifts

method based on fixed galaxy and AGN templates, two passes through data to help identify QSOs and AGN dust tori, and selected priors Rowan-Robinson et al 2007


Photometric redshiftsSWIRE-VVDS sample (with VVDS team, PI LeFevre)

VIRMOS-VLT Deep Survey spectra>1000 sources~3% rms in (1+z)<1% outliers

~ IRAC 3.6 and 4.5 m big help in reducing outliers

z = 1 2 3 4

red: gals, blue QSOs


Photometric redshiftsAll SWIRE Catalogue

VVDS: 9 optical bandsN1,N2: 5 optical bandsLockman: 3-4 optical bndsCDFS: 3 optical bandsXMM-LSS: 5 optical bands

z = 1 2 3 4

SWIRE Photometric Redshift Catalogue contains over 1 million redshifts, 10% have z >2, 4% have z > 3, 20% detected at 24 m, 1% at 70 or 160 m

red: galaxies, blue QSOs


rms, % outliers, as function of number of bands


Redshift distributions

>=3 bands from U-8m

left: Suburu XDS, R<27.5

below: ELAIS-N1, r<23.5: for optically blank sources use 3.6-8 m for phot-z


Lir/Lopt• for galaxies with an ir excess, we fit ir templates (cirrus, M82, A220, AGN dust torus) and estimate Lir (reasonably accurate if have 70 m detection)• for cirrus galaxies, Lir/Lopt is a measure of optical depth of ism• for star-forming galaxies, Lir/Lopt is the specific star formation rate


Lir/Lopt for starbursts


star-forming ellipticals •* Lir/Lopt (specific star formation rate) versus Lopt (~ M•) for galaxies with elliptical galaxy template fits

* includes objects like Arp 220, whose star formation is heavily obscured

•Black: cirrus•Red: M82 starburst•Green: A220 starburst


ultraluminous cirrus gals(L), star-forming ellipticals(R)


AKARI• Japanese mission, 68 cm cooled telescope, first all-sky far infrared survey since IRAS, 90 and 140 m, sensitivity probably comparable to IRAS FSS, but much better spatial resolution, so in principle may be able to construct deeper all-sky sample than PSCz


HERSCHEL3.6 m passively cooled telecope operating at 50-500 m

layered survey will be carried out by SPIRE and PACS teams in guaranteed time, widest area 70 sq deg in 9 areas


PLANCKPLANCK will carry out a shallow all-sky extragalactic point-source survey, which will detect many high-z very luminous submm galaxies

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Aug 8th, 2007MAGPOP Summer School Extragalactic infrared and submillimetre surveys Michael Rowan-Robinson Imperial College London Dole et al 2006 most