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Millimeter detection of Spitzer selected hyperluminous infrared starburst galaxies

Millimeter detection of Spitzer selected hyperluminous infrared starburst galaxies Alain Omont (IAP). The SWIRE Spitzer survey has detected by far the largest set of Sub-Millimeter Galaxies (SMG) But their identification is difficult and requires validation with (sub-)millimeter observations

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Millimeter detection of Spitzer selected hyperluminous infrared starburst galaxies

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  1. Millimeter detection of Spitzer selected hyperluminous infrared starburst galaxies Alain Omont (IAP) The SWIRE Spitzer survey has detected by far the largest set of Sub-Millimeter Galaxies (SMG) But their identification is difficult and requires validation with (sub-)millimeter observations With MAMBO/IRAMwe detected at 1.2mm 20 SWIRE z~2 starburst HLIRGs with LFIR~1013Lo They belong to a rather rare subclass of SMGs, with large PAH/FIR ratio and large stellar mass

  2. Millimeter detection of Spitzer selected hyperluminous infrared starburst galaxies • OUTLINE • General goals • Background: High z submillimeter galaxies (SMGs) • Summary of millimeter dust detection in SMG hosts of high z QSOs • Identification of hyperluminous SMGs in SWIRE Spitzer survey • The SWIRE survey • Detection of SMGs in SWIRE • 1.2mm Mambo observations of SWIRE HLIRGs • Properties of starburst SWIRE HLIGRs  a subclass of SMGs rich in PAH and stars • Search for AGN SWIRE HLIGRs • Prospects • Other projects in progress with CFHTLS & Spitzer data and IRAM observations

  3. z ~ 7 – 20 ? • Reionization • PopIII stars +1st galaxies • Formation of 1st galaxies • Pop. II stars • First AGN • z ~ 4 – 7 : • Current frontier • - Galaxy and Black-Holeearly assembly • - End of reionization • z ~ 1.5 -4: • - Peak of star formation • submm sources + LBGs • Peak of QSO activity • z ~ 0.5-1.5 : • Final phase of active SF • - Weak X-ray AGN • - Cluster formation Main z ranges in the Cosmic History of galaxies z Dphot (Gpc) 1000 -------------------- 20 230 12 130 -------------------- z= 6 60 -------------------- z=2 16 ------------------- 0.5 3 -------------------- 0 ~ 300million ~ 3.5 billion

  4. High-z Galaxies, Star Formation and AGN • Much progress in the last 5-10 years about the exploration of the high-z Universe • High-z galaxies: HDF, Lyman-Break Galaxies, Lyman-a Galaxies, etc. • z ~ 2 – 3  6 – 7 • High-z QSOs and radiogalaxies: peak at z ~2 – 3  6.4 • SCUBA/MAMBO submillimeter galaxies (SMGs): peak at z ~2 – 3 • Good view of history of star formation in the Universe: • - First starbursts at z > 7 • -Early star formation in early type (elliptical) galaxies  major mergers/starbursts • - Late type (spiral) galaxies formed most of their stars at z < 1 • Strong connection between AGN black-hole growth and galaxies (bulge/spheroid) • and their starbursts

  5. SMGs: strongest starbursts in the Universe Important players of star formation at z >~ 2 • Giant starbursts at the peak of elliptical formation z ~ 2-3  1-4 • Most of the energy in the far-infrared (FIR) dust at ~40K • At least Ultra-Luminous Infra-Red Galaxies (ULIRGs: Sanders & Mirabel 1996): • LFIR >~ 1012 Lo, star formation rate SFR > 100 Mo/yr • Relatively rare, but ~1 per arcmin2 • Generally not isolated; strongly biased along high-z Large Scale Structures • Probably progenitors of massive elliptical galaxies • A few of these objects are powerful QSOs or radiogalaxies  MBH >~ 108 Mo

  6. Spectral Energy Distribution (SED) of ULIRGs/SMGs FIR 1.2mm obs lobs=lrest(1+z) PAH Starbursts SiO AGN AGN+starburst

  7. SMGs: strongest starbursts in the Universe • Giant starbursts at the peak of elliptical formation z ~ 2-3  1-4 • At least Ultra-Luminous Infra-Red Galaxies (ULIRGs): • LFIR >~ 1012 Lo, SFR > 100 Mo/yr • Relatively rare, but ~1 per arcmin2 • Generally not isolated; strongly biased along high-z Large Scale Structures • Probably progenitors of massive elliptical galaxies • A few of these objects are powerful QSOs or radiogalaxies  MBH >~ 108 Mo • Most exceptional Hyper-Luminous IR Galaxies (HLIRGs): • LFIR >~ 1013 Lo, SFR ~ 1000 Mo/yr • Nothing equivalent in the local Universe • Very rare ~1 per 50-100 arcmin2 • CO already detectable • Probably in most massive DM halos progenitors of central cD galaxies of clusters • A fraction of them are very powerful QSOs or radiogalaxies  MBH >~ 108 Mo

  8. Dust detection: The Magic of the high-z submm window FIR emission of cold dust (Td ~ 35-50 K) : - steep submm spectrum - compensates for distance - Sn practically independent ofz from z ~ 0.5 to 10 Effect also known as « negative K correction » Redshift degeneracy from Bertoldi, Voss, Walter LFIR = 4x1012 S250(mJy) Lsun

  9. Dust detection: the magic of the submm window • SCUBA(-MAMBO) census of high-z ULIRGs • Take advantage of steep submm spectrum • Account for good part (most) of submm background • z at Keck for radio ones (~50%) (weak AGN ?)  History of star formation up to z~3-4 • Small but uncertain number at z > 4 SCUBA (+MAMBO) submm counts SCUBA(-radio) redshift distribution Chapman, Blain, Smail, Ivison 2005

  10. Submm counts from the SHADES survey Coppin et al. 2006

  11. High-z millimeter studies at IRAM 1. MAMBO detection of redshifted far-IR/submm dust emission from high-z QSOs A. Beelen F. Bertoldi C. Carilli P. Cox + J. Bergeron, K. Isaak, R. McMahon, R. Priddey, etc + X.H. Fan, M. Strauss, Ran Wang, etc. ( 2. CO detections with the Plateau de Bure Interferometer ) Omont et al. 1996 Carilli et al. 2001 Omont et al 2001 Omont et al 2003 Bertoldi etal. 2003 Beelen et al. 2007 Wang et al. 2007

  12. MAMBO/IRAM detection of redshifted far-IR/submm dust (and CO) emission from high-z QSOs • To establish correlations between major starbursts and black-holes at high z • It is the easiest way to find (biased) cases of HLIRGs at very high z, since the redshifts of SCUBA/MAMBOsources are practically unknown at z > 4 • IRAM 30m Telescope ( Spain) + MAMBO bolometer cameras (Bonn) • 200 bright QSOs Lbol ~ 1013 -1014 Lo with z~2-6: 55 detections • LFIR ~ 1013 Lo  HLIRGs • SFR ~ 1000 Mo/yr (if pure starburst) • Concommittant major starbursts • and AGN. But the far-IR luminosity is • weakly correlated with Lbol • CO has been detected in 18 high-zQSOs • with the IRAM interferometer

  13. High-z millimeter studies at IRAM. 3. • Millimeter detection of Spitzer selected • hyperluminous infrared starburst galaxies • The SWIRE survey • Detection of SMGs in SWIRE and identification strategy • 1.2mm Mambo observations of SWIRE HLIRGS • Properties of starburst SWIRE HLIGRS  a subclass of SMGs rich in • PAH and stars • Prospects Main collaborators: Carol Lonsdale, Mari Polletta (UCSD) + D. Farrah, D. Shupe, R. Zylka, S. Berta, B. Siana, N. Bavouzet, G.Lagache, H. E. Smith, F. Bertoldi., P. Cox, C. De Breuck, H. Dole, D. Lutz, L. Tacconi, I. Perez-Fournon, H. Aussel, H. McCracken, D. Clements, M. Rowan-Robinson A. Franceschini, D. Frayer

  14. Importance of extensive studies of larger samples of high-z SMGs • Major starbursts of massive (elliptical) galaxies: initial collapse or major mergers • Parallel growth of super-massive black holes • Trace density peaks, first massive dark matter halos and • early Large Scale Structures • Importance of larger samples of high-z SMGs • Various statistical studies • Trace their spatial distribution along early LSS • Identify the rare most extraordinary, mm-brightest ones •  strong lensed cases • or most luminous (far-IR) galaxies LFIR > 1013 Lo, HLIRGs

  15. Present SMG samples are very limited Only ~400 sources provided by SCUBA/MAMBO surveys( <~ 0.5 deg2) Waiting for very large samples/areas (~>2007) of SCUBA2 (850µm), ASTRO-F/AKARI (50-200 µm) and (~>2008) Herschel (100-500 µm) Much larger (x~20-50) samples already exist (buried) in Spitzer wide field surveys in particular SWIRE: 50 deg2, 10000 - 15 000 SMG

  16. Spitzer provides the first wide field (mid-)IR surveys • Spitzer is: • Very well matched to the detection of red galaxies (elliptical, LIRGs…) up to z~1 • As well as AGN (Type 1 and 2 QSOs, etc.) up to z~3 • Even pretty sensitive for high-z SMGs although most energy is in FIR outside • of Spitzer sensitive l range • Wide-field Spitzer surveys (FLS, GTO, SWIRE) cover in total about 70 deg2: • SWIRE Legacy Project: 50 deg2 (PI Carol Lonsdale) • µm 3.5 4.5 5.8 8.0 24 • µJy 3.7 4.5 48 38 106 nominal limits Lonsdale et al. 2004: • 10 10 45 50 250 present catalogs • ( ? ~100 mJy at 160 µm, ~20 mJy at 70 µm)

  17. Identification of SMGs in SWIRE • Direct Spitzer detections of ~90 known SCUBA/MAMBO SMGs at z~2 • with SWIRE sensitivities, HLIRGs with S(850µm) > 7 mJy or S(1.2mm) > 2.5 mJy: are detected at >90% at 3.8 and 4.5 µm and at ~45% in most IRAC (3-8µm) bands and MIPS 24µm • 150-300 per deg² (0.05-0.1 per arcmin2) • 0.7-1.5 104 in total SWIRE • ~20-40 times more than all existing MAMBO-SCUBA surveys HLIRGs

  18. Strategy for Identification of SMGs in SWIRE • Careful identification criteria of HLIRG candidates from SWIRE+ optical data + SMG SED templates • Difficult extrapolation from 24µm to 1.2mm (need to simultaneously determine the SED and redshift from five SWIRE bands (3.6-24µm)

  19. Spectral Energy Distribution (SED) of ULIRGs/SMGs Starbursts AGN AGN+starburst

  20. detected with SCUBA or MAMBO Spitzer infrared SED of SWIRE SCUBA-MAMBO

  21. Strategy for Identification of SMGs in SWIRE • Careful identification criteria of HLIRG candidates from SWIRE+ optical data + SMG SED templates • Difficult extrapolation from 24µm to 1.2mm (need to simultaneously determine the SED and redshift from five SWIRE bands (3.6-24µm) • Four successive MAMBO projects scheduled at IRAM-30m • (Fall 2005 – Winter 2007) for detecting SWIRE HLIRGs candidates at 1.2mm • (S1.2mm >~2-5 mJy): • 2005-2006: 24µm-bright starburst best candidates: 20 detections • November 2006: AGN best candidates • Winter 2007: 24µm-bright starbursts, unbiased sample

  22. 1.2mm observations of 24µm-bright starburst SWIRE HLIRGS Observation of a sample of ~60 best candidates with: - starburst-dominated SED - S(24µm) >~ 400 µJy - maximum in 5.8 µm IRAC band (redshifted 1.6 µm stellar bump  z ~ 2)

  23. 1.2mm observations of 24µm-bright starburst SWIRE HLIRGS Observation of a sample of ~60 best candidates with: - pure starburst SED - S(24µm) >~ 400 µJy - maximum in 5.8 µm IRAC band (redshifted 1.6µm stellar bump  z ~ 2) One third are detected with S(1.2mm) >~ 2 mJy Average value < S(1.2mm) > = 1.6 mJy Majority of the sources are ~HLIRGs with LFIR close to 1013 Lo Follow-up at 350µm at CSO in January 2007  Tdust , accurate LFIR

  24. Properties of 24µm-bright starburst SWIRE HLIRGS • Mid-IR spectra obtained with Spitzer IRS for 5 sources detected at 1.2mm • practically pure PAH spectra • confirmation of redshift ~ 2 (1.7 – 1.9) Observed spectrum

  25. Properties of 24µm-bright starburst SWIRE HLIRGS • Mid-IR spectra obtained with Spitzer IRS for 5 sources detected at 1.2mm • practically pure PAH spectra • confirmation of redshift ~ 2 (1.7 – 1.9) Average spectrum 9 starburst sources Weedman et al. 2006

  26. Properties of 24µm-bright starburst SWIRE HLIRGS Redshifts in the range 1.7 – 2.5 ( z-spectro 1.7 – 1.9 ) Ratio S(1.2mm)/S(24µm) much smaller than most SMGs whose typical SED is relatively cold, similar to Arp 220 Their SED is rather similar to M82 or NGC6090

  27. Properties of 24µm-bright starburst SWIRE HLIRGS 1. Large ratio PAH/FIR emission • Ratio S(1.2mm)/S(24µm) much smaller than most SMGs whose typical SED • is relatively cold, similar to Arp 220 • Their SED is rather similar to M 82 or NGC 6090 • Strong ratio of PAH/FIR emission •   • Maybe they are more extended starbursts • less opacity and less absorption of PAH emission • With perhaps strong superwind as in • M82 ? • But scaled by a factor > 10 • enrichment of intergalactic medium in heavy elements??

  28. Extended PAH emission in the super wind of M82 Engelbracht et al. 2006

  29. Properties of 24µm-bright starburst SWIRE HLIRGS 2. Large stellar masses Masses in red stars range from 8x1010 to 6x1011 Mo, if the mean stellar age is below 109 years, and significantly higher masses if the stars are older.  They are probably young massive ellipticals in the final stages of star formation, where much of their stellar mass is already in place, yet very high rates of star formation are still proceeding. The rare starburst episode is likely to be very short lived, to avoid that the total accumulated stellar mass by the end of the burst exceed that observed in the largest local ellipticals.  Probably one of the latest gas-rich major mergers of a massive elliptical

  30. MAMBO observations of SWIRE HLIRG AGN candidates • October-November 2006: bad weather; 1/3 of proposal observed • XMM-LSS and Lockman SWIRE fields • 14 Sources fitted with composite starburst-AGN SEDs • - average flux: 1.53 +/-0.40 mJy - the majority should be HLIRGs • 11 sources with « Torus » featureless SEDs - average flux: 0.46 +/-0.38 mJy - few HLIRGs

  31. Spectral Energy Distribution (SED) of ULIRGs/SMGs Starbursts AGN AGN+starburst

  32. MAMBO observations of SWIRE HLIRG AGN candidates • October-November 2006: bad weather; 1/3 of proposal observed • XMM-LSS and Lockman SWIRE fields • 14 Sources fitted with composite starburst-AGN SEDs • - average flux: 1.53 +/-0.40 mJy - the majority should be HLIRGs • 11 sources with « Torus » featureless SEDs - average flux: 0.46 +/-0.38 mJy - few HLIRGs • Confirmed detection of two exceptional sources - u-dropouts in D1 CFHTLS Deep Field:  z ~3 – 4 - probably red QSOs - S24µm ~ 2–3 mJy - S1.2mm ~ 5 mJy - Nature of IR emission still unknown

  33. Confirmed detection of two exceptional sources - u-dropouts in D1 CFHTLS Deep Field:  z ~3 – 4 (to be confirmed) - probably red QSOs - S24µm ~ 2–3 mJy - S1.2mm ~ 5 mJy - Nature of IR emission still unknown - Very large ratios 24/8.0µm and 8.0/5.8µm Band u g r i z 3.6 4.5 5.8 8.0 24um 1.2mm 20cm ------------------------------------------------------------------------------------------------------------------------ SW49208 z ~ 3 – 3.5 m_AB <26 24.6 23.4 23.0 22.5 20.9 20.7 Flux(µJy) 3.6 15.8 19.7 <50 185 2406 ~5000 350 ------------------------------------------------------------------------------------------------------------------------ SW55275 z ~ 3.5 - 4 m_AB 25.5 23.0 21.7 22.0 22.4 20.9 20.5 Flux(µJy) 4.0 15.5 23.0 <50 245 3271 ~5000 140 ------------------------------------------------------------------------------------

  34. PROSPECTS (2005-2006: 24µm-bright starbursts, best candidates: 20 detections November 2006: AGN best candidates) - Winter 2007: 24µm-bright starbursts, unbiased sample Goal to characterize this subclass ofstrong starbursts with 5.8µm bump and S(24µm) > 400µJy (50 per sq. deg.) and its average star formation rate. Previous samples were biased towards the identification of the most luminous objects, so that the average starburst properties of the bulk of this class remain undetermined. We have been awarded 39h of MAMBO observations to observe an unbiased complete random sample, which has excellent X-ray and optical coverage, to determine the average value of S(1.2mm) and inferred quantities

  35. PROSPECTS • (New 1.2mm Mambo observations: • - Winter 2007: 24µm-bright starbursts, unbiased sample) • Follow-up at 350µm at CSO in January 2007  Tdust , accurate LFIR •  • Observations in SWIRE southern fields with APEX/LABOCA • CO search with IRAM interferometer when accurate redshifts • Morphology studies: • - HST? • - Look for relatively nearby similar objects; at least ULIRGs •  • Full identification of SWIRE z~2 HLIRGs (+ ULIRGs)warranted with Scuba 2 • (2007) and Herschel (2008) • Detailed studies with ALMA (2012)

  36. Other projects in progress • with CFHTLS & Spitzer data and IRAM observations • Identification of Type 1 and 2 QSOs in CFHTLS/Spitzer fields • Pei Yu, J. Bergeron, X. Liu; N. Bavouzet • 1.2mm MAMBO maps of deep Spitzer + multi-l fields • A. Baker, C. Lonsdale, F. Owen; F. Bertoldi • 1.2mm observations of high z QSOs and IRS Spitzer sources • M. Jarvis; C. Willott; Ran Wang; D. Lutz, L. Yan • CO observations of high z sources • I. Smail, P. Cox; D. Lutz, L. Yan; Ran Wang; F. Bertoldi; R. Genzel

  37. CO detection in 18 high-z QSOs Plateau de Bure IRAM interferometer

  38. CO detection in 18 high-z QSOs CO detection in QSO SDSS J1148 at z=6.42 Dense gas density ~105 cm-3 T ~ 100 K size R ~400-1400 pc gaz mass 1-2 1010 Mo Multi-line excitation model Bertoldi et al. 03 PdBI Resolution of CO in 2 sources VLA Walter et al. 04 Walter et al. 03 VLA

  39. Dust detection: the magic of the submm window • SCUBA(-MAMBO) census of high-z ULIRGs • Take advantage of steep submm spectrum • Account for good part (most) of submm background • z at Keck for radio ones (~50%) (weak AGN ?)  History of star formation up to z~3-4 • Small but uncertain number at z > 4 SCUBA (+MAMBO) submm counts SCUBA(-radio) redshift distribution Chapman, Blain, Ivison, Smail 2003

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