Delphine Marcillac Moriond 2005 When UV meets IR... 1 IR properties of distant IR galaxies Delphine Marcillac (PhD student) Supervisor : D. Elbaz In collaboration with : Emeric Le Floc’h Herve Dole Herve Dole Ranga Chary Ranga Chary Mark Dickinson Mark Dickinson & GOODS consortium & GOODS consortium Emmanuel Moy Emmanuel Moy

Delphine MarcillacMoriond 2005 When UV meets IR SPITZER: Detection of LIRGs and ULIRGs beyond z ~1 => study of LIRG evolutions It confirms ISO Number counts Chary et al 04, Papovitch et al 04, Dole et al, 2004 ISOCAM redshift distribution … Detection of distant LIRGs LIRGs and ULIRGs = Rosetta stone for galaxy evolution IRAS local LIRGs and ULIRGs => rare 1983 IRAS : local LIRGs and ULIRGs => rare 1995 ISO : distant LIRGs and ULIRGs 1995 ISO : distant LIRGs and ULIRGs (ISO number counts => more numerous (ISO number counts => more numerous discovery of the CIRB 1996 :discovery of the CIRB

Delphine MarcillacMoriond 2005 When UV meets IR components of dust : BGs : size = nm VSGs : size = nm PAHs : size = nm Origin of the IR emission Desert, Boulanger & Puget 1990 M82 (disque) (Laurent et al. 2000)

Delphine MarcillacMoriond 2005 When UV meets IR...4 Origin of the IR emission < 20 % Fadda et al, 2001 HST-WFPC2 in B band (5252 A) and I band (8269 A) ISOCAM image (7 and 15  m) AGN ex NGC 1068 SB ex NGC 4038/39 Fadda et al, 2001 < 20 %

Delphine MarcillacMoriond 2005 When UV meets IR...5 How to derive SFR for distant LIRGs ? From the UV : strong attenuation +  slope (Meurer et al, 1999…..Goldader et al, 1999) (Meurer et al, 1999…..Goldader et al, 1999) From the optical range : high resolution spectra are needed. Faint Objects = long time exposure Faint Objects = long time exposure it needs a good correction for the attenuation. it needs a good correction for the attenuation. large uncertainties ( at z=0.7 ) large uncertainties ( Flores et al,2004 at z=0.7 ) From the radio : correlation radio LIR ( Condon 1992, Yun et al, 2001 ) not deep enough not deep enough F ~  F(FIR)/F(UV)= f(  ) does not work for LIRGs and ULIRGs Meurer et al (99) Goldader et al (2002) Anantharamaiah et al. (2000) Elbaz et al, 2002

Delphine MarcillacMoriond 2005 When UV meets IR...6 From the MIR ? Local universe : correlation MIR – LIR Local universe : correlation MIR – LIR (Elbaz et al, 2002) correlation radio-MIR correlation radio-MIR (Codon 1992, Yun et al, 2001) or radio is a tracer of LIR or radio is a tracer of LIR MIR + local templates or correlations => FIR=> LIR => SFR MIR + local templates or correlations => FIR=> LIR => SFR Chary & Elbaz 2001 Kennicutt 1998 Chary & Elbaz 2001 Kennicutt 1998 Dale & Helou, 2002 Lagache et et al, 2004 Lagache et et al, 2004 …….. …….. M82 (disque) (Laurent et al. 2000) 15  m vs IR IR vs IRAS 12  mIR vs ISOCAM 15  m

Delphine MarcillacMoriond 2005 When UV meets IR...7 Local templates I : Chary & Elbaz 2001 correlations between L 7,L 12,L 15,L 60,L 100, L 850 et L IR correlations between L 7,L 12,L 15,L 60,L 100, L 850 et L IR 4 typical templates 4 typical templates arp220 for ULIRGs, arp220 for ULIRGs, NGC 6090 for LIRGs NGC 6090 for LIRGs M81 for starbursts M81 for starbursts M51 for normal galaxies M51 for normal galaxies + FIR templates =>Local templates =>Local templates

Delphine MarcillacMoriond 2005 When UV meets IR...8 Local templates II : Dale & Helou, dust components … 3 dust components … DBP90 + update DBP90 + update BGs = grey body emission BGs = grey body emission VSGs = near grey body emission VSGs = near grey body emission PAH = 1 typical template PAH = 1 typical template + damping factor + damping factor

Delphine MarcillacMoriond 2005 When UV meets IR...9 Potential cause for variations of MIR SEDs : metallicity (Liang et al, 2004) metallicity (Liang et al, 2004) concentration concentration dust properties … dust properties … BUT : correlation radio – MIR OK correlation radio – MIR OK (Appleton et al, 2004) (Appleton et al, 2004) a PAH bump detected at z=0.7…. a PAH bump detected at z=0.7…. Elbaz et al, 2005 A&A Letters (in press) Elbaz et al, 2005 A&A Letters (in press) LIR radio in agrement with LIR MIR LIR radio in agrement with LIR MIR distant MIR is not very different …. distant MIR is not very different …. Can we derive SFR of distant LIRGs from MIR ? from MIR ?

Delphine MarcillacMoriond 2005 When UV meets IR...10 Marano field 30' (Elbaz et al. 99, 04) ISOCAM Emeric Le Floc’h/H.Dole MIPS The PAH bump exists at z= ° 4 0' 15  m Marano field MIPS 24  m (E. Le Floc'h/H.Dole) (Spitzer-MIPS Early Characterization Observation)

Delphine MarcillacMoriond 2005 When UV meets IR  m Spitzer-MIPS 15  m ISOCAM SED of a LIRG at z=0.69 (LIR~ L ,SFR~22 M  yr-1) The PAH bump exists at z=0.7

Delphine MarcillacMoriond 2005 When UV meets IR...12 Compatible with NGC 1068 Compatible with NGC 1068 No compatible with NGC 1068

Delphine MarcillacMoriond 2005 When UV meets IR...13 Great Observatories Origins Deep Surveys ISOCAM 15  m 5’ 2 Deep Survey Spitzer-MIPS 24  m 100’ 2 MIR SEDs of distant galaxies MIR SEDs of distant galaxies

Delphine MarcillacMoriond 2005 When UV meets IR...14 A more detailed study with GOODS 63 galaxies detected (secure association) 63 galaxies detected (secure association) at 15  m (ISOCAM) at 15  m (ISOCAM) at 24  m (MIPS) at 24  m (MIPS) with a secure redshift (ACS data) with a secure redshift (ACS data) + 20 galaxies detected at 1.4 GHz + 20 galaxies detected at 1.4 GHz + 13 galaxies detected at 8.5 GHz + 13 galaxies detected at 8.5 GHz 0.3<z< <z<1.3 3 AGNs +4 ? ( to be studied) 3 AGNs +4 ? ( to be studied)

Delphine MarcillacMoriond 2005 When UV meets IR...15 L IR (radio) versus L IR (MIR)

Delphine MarcillacMoriond 2005 When UV meets IR...16 observed RF observed RF Z~1 24  m (MIPS) ~ 12  m = IRAS 15  m (ISO-LW3) ~ 7  m = ISOLW2 15  m (ISO-LW3) ~ 7  m = ISOLW2 PAH at z~1 ?: L7 versus L12 PAH at z~1 ?: L7 versus L12

Delphine MarcillacMoriond 2005 When UV meets IR...17 The silicate absorption at z=0.6 L 10 versus L 7 z = 0.6 z =  m (MIPS) => 15  m(ISO) 24  m (MIPS) => 15  m(ISO) 15  m (ISO-LW3) 15  m (ISO-LW3) 12  m (IRAS 12 mm) => new filter for local galaxies 12  m (IRAS 12 mm) => new filter for local galaxies

Delphine MarcillacMoriond 2005 When UV meets IR...18 The SFR / mass relation Distant Starbursts IRAS Starbursts (Pasquali et al, in prep)

Delphine MarcillacMoriond 2005 When UV meets IR...19 Conclusion SFR and LIR can be derived from MIR up to z=1.2 SFR and LIR can be derived from MIR up to z=1.2 MIR properties of distant galaxies have weakly evolved up to z~1.2 but : IRS spectra of LIRGs are needed but : IRS spectra of LIRGs are needed

Delphine MarcillacMoriond 2005 When UV meets IR...20 LIR MIR can be used for distant galaxies MIR can be used for distant galaxies it corresponds to 7-15 mm in the rest frame it corresponds to 7-15 mm in the rest frame MIR properties of distant LIRGs do not change a lot MIR properties of distant LIRGs do not change a lot Comparison IR / radio OK Comparison IR / radio OK SFR : OK SFR : OK

Delphine MarcillacMoriond 2005 When UV meets IR...21 F  (L  ) (  m) SEDs Chanial et al. (in prep) CFRS SFR= 125 M  /yr M101 (spiral) SFR= 1.8 Mo/yr NGC 5018 Elliptical IR moyen FIR optical dust stars

Delphine MarcillacMoriond 2005 When UV meets IR...22 ISOCAM image (7 and 15  m) HST-WFPC2 in B band (5252 A) and I band (8269 A) The two galactic nuclei High star formation area : 60 % of the CO(1-0) emission Sanders and Mirabel,1985 A nearby merger system of 2 gaz rich galaxies Located at 20 Mpc L ir = Lsol A typical LIRG : NGC 4038/39 A typical LIRG : NGC 4038/39

Delphine MarcillacMoriond 2005 When UV meets IR...23 Discovery of infrared galaxies 1983 IRAS :detection of local LIRGs and ULIRGs detection of LIRGs (11< log (L IR/ Lo)<12 ) ULIRGs (12 <log L IR/ Lo) ULIRGs (12 <log L IR/ Lo) associated to mergers associated to mergers ( strong interactions ) (Sanders & Mirabel, 1996) rare ( not representative of the local universe) rare ( not representative of the local universe) 1995 ISO : detection of distant LIRGs and ULIRGs Far more numerous at higher redshifts ISO number counts ISO number counts Elbaz et al, 1999, Aussel et al, 99 … Isolated – or in little groups of galaxies ?

Delphine MarcillacMoriond 2005 When UV meets IR...24 COBE/DIRBE R=240  m B=60  m G=100  m 1996 :discovery of the CIRB (Puget et al, 1996) Discovery of infrared galaxies