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IR properties of distant IR galaxies Delphine Marcillac (PhD student) Supervisor : D. Elbaz

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

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IR properties of distant IR galaxies Delphine Marcillac (PhD student) Supervisor : D. Elbaz

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

  2. Detection of distant LIRGs 1983 IRAS : local LIRGs and ULIRGs => rare 1995 ISO : distant LIRGs and ULIRGs (ISO number counts => more numerous 1996 :discovery of the CIRB 2003 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 … LIRGs and ULIRGs = Rosetta stone for galaxy evolution. Moriond 2005 When UV meets IR ...

  3. M82 (disque) (Laurent et al. 2000) Origin of the IR emission 3 components of dust : BGs : size = 15-400 nm VSGs : size = 1.2-15 nm PAHs : size = 0.4-1.2 nm Desert, Boulanger & Puget 1990 Moriond 2005 When UV meets IR ...

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

  5. How to derive SFR for distant LIRGs ? From the UV : strong attenuation + b slope (Meurer et al , 1999…..Goldader et al, 1999) From the optical range : high resolution spectra are needed. Faint Objects = long time exposure it needs a good correction for the attenuation. 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 Fl~lb F(FIR)/F(UV)= f(b) does not work for LIRGs and ULIRGs Meurer et al (99) Goldader et al (2002) Elbaz et al, 2002 Anantharamaiah et al. (2000) Moriond 2005 When UV meets IR ...

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

  7. Local templates I : Chary & Elbaz 2001 • correlations between L7 ,L12,L15,L60,L100, L850 et LIR • 4 typical templates arp220 for ULIRGs, NGC 6090 for LIRGs M81 for starbursts M51 for normal galaxies + FIR templates =>Local templates Moriond 2005 When UV meets IR ...

  8. Local templates II : Dale & Helou, 2002 3 dust components … DBP90 + update BGs = grey body emission VSGs = near grey body emission PAH = 1 typical template + damping factor Moriond 2005 When UV meets IR ...

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

  10. 40' 1.4° 15 mm The PAH bump exists at z=0.7-1 Marano field (Elbaz et al. 99, 04) ISOCAM Emeric Le Floc’h/H.Dole MIPS 30' Marano field MIPS 24 mm (E. Le Floc'h/H.Dole) (Spitzer-MIPS Early Characterization Observation) Moriond 2005 When UV meets IR ...

  11. 15mm ISOCAM 24mm Spitzer-MIPS The PAH bump exists at z=0.7 SED of a LIRG at z=0.69 (LIR~1011.1 L,SFR~22 Myr-1) Moriond 2005 When UV meets IR ...

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

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

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

  15. LIR (radio) versus LIR (MIR) Moriond 2005 When UV meets IR ...

  16. PAH at z~1 ?: L7 versus L12 observedRF Z~1 24 mm (MIPS) ~ 12 mm = IRAS 15 mm (ISO-LW3) ~ 7 mm = ISOLW2 Moriond 2005 When UV meets IR ...

  17. The silicate absorption at z=0.6L10 versus L7 • z = 0.6 • 24 mm (MIPS) => 15 mm(ISO) • 15 mm (ISO-LW3) • 12 mm (IRAS 12 mm) => new filter for local galaxies Moriond 2005 When UV meets IR ...

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

  19. Conclusion 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 Moriond 2005 When UV meets IR ...

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

  21. optical FIR IR moyen nFn (L) CFRS 14.1139 SFR= 125 M/yr NGC 5018 Elliptical M101 (spiral) SFR= 1.8 Mo/yr l (mm) stars dust SEDs Chanial et al. (in prep) Moriond 2005 When UV meets IR ...

  22. A typical LIRG : NGC 4038/39 A nearby merger system of 2 gaz rich galaxies Located at 20 Mpc Lir = 1011 Lsol The two galactic nuclei HST-WFPC2 in B band (5252 A) and I band (8269 A) ISOCAM image (7 and 15 mm) High star formation area : 60 % of the CO(1-0) emission Sanders and Mirabel,1985 Moriond 2005 When UV meets IR ...

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

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

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