Aug 8th, 2007MAGPOP Summer School Extragalactic infrared and submillimetre surveys Michael...
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Transcript of Aug 8th, 2007MAGPOP Summer School Extragalactic infrared and submillimetre surveys Michael...
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
Aug 8th, 2007 MAGPOP Summer School
1 micron - 1 mm
- a few terrestial windows
the infrared and submillimetre bands
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
IRAS
Horsehead Nebula
Aug 8th, 2007 MAGPOP Summer School
IRAS all-sky survey
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
ISOISO, launched 1996, reached z~1, + spectroscopy
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
Dust extinction in local galaxies
<AV> ~ 0.3 in local galaxies(Rowan-Robinson, 2003, MN 344, 13)
Aug 8th, 2007 MAGPOP Summer School
comparison of star-formation rate estimates
Daddi et al 2007
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
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 ?
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
2MASS• 2MASS provides a better picture of galaxy distribution at z<0.03
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
M51Sombrero
combined 3.6, 8 and 24 m images(SINGS consortium)
Aug 8th, 2007 MAGPOP Summer School
M82N2207/IC2163
Stefan’s Quintet
Aug 8th, 2007 MAGPOP Summer School
SIRTF SWIRE survey
49 sq deg in 6 areas, at 3.6, 4.5, 5.8, 8, 24, 70, 160 m
Aug 8th, 2007 MAGPOP Summer School
ELAIS N1: 9 sq. deg
SWIRE 3.6 m survey in ELAIS-N1
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
rms, % outliers, as function of number of bands
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
Lir/Lopt for starbursts
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
ultraluminous cirrus gals(L), star-forming ellipticals(R)
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
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
Aug 8th, 2007 MAGPOP Summer School
PLANCKPLANCK will carry out a shallow all-sky extragalactic point-source survey, which will detect many high-z very luminous submm galaxies