delphine marcillac moriond 2005 when uv meets ir... 1 ir properties of distant ir galaxies delphine...

Delphine MarcillacDelphine Marcillac Moriond 2005 When UV meets IR ..Moriond 2005 When UV meets IR ....

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IR properties of distant IR IR properties of distant IR galaxiesgalaxies

Delphine MarcillacDelphine Marcillac(PhD student) (PhD student)

Supervisor : D. ElbazSupervisor : D. Elbaz

In collaboration with : Emeric Le Floc’hIn collaboration with : Emeric Le Floc’h Herve DoleHerve Dole

Ranga CharyRanga Chary Mark Dickinson Mark Dickinson

& GOODS consortium& GOODS consortium Emmanuel MoyEmmanuel Moy


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2003 2003 SPITZER:SPITZER:

Detection of LIRGs and ULIRGs beyond z ~1 => study of LIRG evolutionsIt 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 LIRGs and ULIRGs = Rosetta stone for galaxy evolution.evolution.

1983 IRAS1983 IRAS : local LIRGs and ULIRGs => local LIRGs and ULIRGs => rarerare

1995 ISO :1995 ISO : distant LIRGs and ULIRGs distant LIRGs and ULIRGs (ISO number counts => (ISO number counts => more numerousmore numerous

1996 :discovery of the CIRB discovery of the CIRB


33

3 components of dust :3 components of dust :

BGs : BGs : size = 15-400 nmsize = 15-400 nm

VSGs : VSGs : size = 1.2-15 nmsize = 1.2-15 nm

PAHs : PAHs : size = 0.4-1.2 nmsize = 0.4-1.2 nm

Origin of the IR emissionOrigin of the IR emission

Desert, Boulanger & Puget 1990

M82(disque)

(Laurent et al. 2000)


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Origin of the IR emissionOrigin 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 4038/39AGN ex NGC 1068 SB ex NGC 4038/39

Fadda et al, 2001< 20 %


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How to derive SFR for distant LIRGs ?

From the UV :From the UV : strong attenuation + strong attenuation + slope slope (Meurer et al , 1999…..Goldader et al, 1999)(Meurer et al , 1999…..Goldader et al, 1999)

From the optical range :From the optical range : high resolution spectra are needed. high resolution spectra are needed. Faint Objects = long time exposure Faint Objects = long time exposure it needs a good correction for the it needs a good correction for the

attenuation. attenuation. large uncertainties (large uncertainties (Flores et al,2004 at at

z=0.7 )z=0.7 )

From the radio :From the radio : correlation radio LIR ( correlation radio LIR (Condon 1992, Yun et al, 2001Condon 1992, Yun et al, 2001)) not deep enough not deep enough

FF~~

F(FIR)/F(UV)= f(F(FIR)/F(UV)= f()) does not work for LIRGs and does not work for LIRGs and ULIRGsULIRGs

Meurer et al (99)Meurer et al (99) Goldader et al (2002) Goldader et al (2002)

Anantharamaiah et al. (2000)

Elbaz et al, 2002Elbaz et al, 2002


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From the MIR ? 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 LIRor radio is a tracer of LIR

MIR + local templates or correlations => FIR=> LIR => SFRMIR + local templates or correlations => FIR=> LIR => SFR Chary & Elbaz 2001 Kennicutt 1998Chary & Elbaz 2001 Kennicutt 1998

Dale & Helou, 2002 Dale & Helou, 2002 Lagache et et al, 2004Lagache et et al, 2004

…… ……....

M82(disque)

(Laurent et al. 2000)

15 m vs IRIR vs IRAS 12 mIR vs ISOCAM 15 m


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Local templates I : Chary & Local templates I : Chary & Elbaz 2001Elbaz 2001

correlations between Lcorrelations between L7 7 ,L,L1212,L,L1515,L,L6060,L,L100100, , LL850850 et L et LIRIR

4 typical templates 4 typical templates

arp220 for ULIRGs,arp220 for ULIRGs,

NGC 6090 for LIRGsNGC 6090 for LIRGs

M81 for starbursts M81 for starbursts

M51 for normal galaxies M51 for normal galaxies

+ FIR templates + FIR templates

=>Local templates =>Local templates


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Local templates II : Dale & Local templates II : Dale & Helou, 2002Helou, 2002

3 dust components … 3 dust components …

DBP90 + updateDBP90 + update

BGs = grey body emissionBGs = grey body emission

VSGs = near grey body emissionVSGs = near grey body emission

PAH = 1 typical template PAH = 1 typical template

+ damping factor+ damping factor


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Potential cause for variations of MIR SEDs : Potential cause for variations of MIR SEDs :

metallicity (Liang et al, 2004)metallicity (Liang et al, 2004)

concentrationconcentration

dust properties …dust properties …

BUT :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 MIRLIR radio in agrement with LIR MIR

distant MIR is not very different ….distant MIR is not very different ….

Can we derive SFR of distant Can we derive SFR of distant LIRGsLIRGs from MIR ?from MIR ?


1010

Marano fieldMarano field

30'

(Elbaz et al. 99, 04) ISOCAMEmeric Le Floc’h/H.Dole MIPS

The PAH bump exists at z=0.7-The PAH bump exists at z=0.7-11

1.4°

40'

15 m

Marano field MIPS 24 m (E. Le Floc'h/H.Dole)(Spitzer-MIPS Early Characterization Observation)


1111

24m Spitzer-MIPS

15m ISOCAM

SED of a LIRG at z=0.69 (LIR~10SED of a LIRG at z=0.69 (LIR~1011.111.1 L L,SFR~22 M,SFR~22 Myr-1)yr-1)

The PAH bump exists at z=0.7The PAH bump exists at z=0.7


1212

Compatible with NGC 1068

Compatible with NGC 1068

No compatible with NGC 1068


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Great Observatories Origins Deep SurveysGreat Observatories Origins Deep Surveys

ISOCAM 15 m 5’5’22

Deep SurveySpitzer-MIPS 24 m100’2

MIR SEDs of distant galaxiesMIR SEDs of distant galaxies


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A more detailed study with A more detailed study with GOODSGOODS

63 galaxies detected (secure association)63 galaxies detected (secure association) at 15 at 15 m (ISOCAM)m (ISOCAM) at 24 at 24 m (MIPS)m (MIPS) with a secure redshift (ACS with a secure redshift (ACS

data)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<1.30.3<z<1.3 3 AGNs +4 ? ( to be studied)3 AGNs +4 ? ( to be studied)


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LLIR IR (radio) versus L(radio) versus LIRIR (MIR)(MIR)


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observedobserved RFRF

Z~1 24 Z~1 24 m (MIPS) ~ 12 m (MIPS) ~ 12 m = IRASm = IRAS

15 15 m (ISO-LW3) ~ 7 m (ISO-LW3) ~ 7 m = ISOLW2m = ISOLW2

PAH at z~1 ?: L7 versus PAH at z~1 ?: L7 versus L12L12


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The silicate absorption at The silicate absorption at z=0.6z=0.6

LL1010 versus L versus L77

z = 0.6z = 0.6 24 24 m (MIPS) => 15 m (MIPS) => 15 m(ISO)m(ISO) 1515m (ISO-LW3) m (ISO-LW3) 12 12 m (IRAS 12 mm) => new filter for local galaxies m (IRAS 12 mm) => new filter for local galaxies


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The SFR / mass relationThe SFR / mass relation

Distant StarburstsDistant Starbursts

IRAS Starbursts IRAS Starbursts (Pasquali et al ,(Pasquali et al ,

in prep)in prep)


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Conclusion Conclusion

SFR and LIR can be derived from SFR and LIR can be derived from MIR up to z=1.2MIR up to z=1.2

MIR properties of distant galaxies MIR properties of distant galaxies have weakly evolved up to z~1.2have weakly evolved up to z~1.2

but : IRS spectra of LIRGs are but : IRS spectra of LIRGs are neededneeded


2020

LIRLIR

MIR can be used for MIR can be used for distant galaxiesdistant galaxies

it corresponds to 7-15 mm it corresponds to 7-15 mm in the rest framein the rest frame

MIR properties of distant MIR properties of distant LIRGs do not change a lotLIRGs do not change a lot

Comparison IR / radio Comparison IR / radio OKOK

SFR : OKSFR : OK


2121

F(L)

(m)

SEDs Chanial et al. (in prep)

CFRS 14.1139

SFR= 125 M/yr

M101 (spiral)SFR= 1.8 Mo/yr

NGC 5018Elliptical

IR moyen

FIR optical

duststars


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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 galaxiesLocated at 20 MpcLir = 1011 Lsol

A typical LIRG : NGC 4038/39A typical LIRG : NGC 4038/39


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Discovery of infrared galaxies

1983 IRAS :detection of local LIRGs and 1983 IRAS :detection of local LIRGs and ULIRGsULIRGs detection of LIRGs (11< log (Ldetection of LIRGs (11< log (LIR/IR/Lo)<12 )Lo)<12 ) ULIRGs (12 <log LULIRGs (12 <log LIR/IR/Lo) Lo) associated to mergersassociated to mergers ( strong interactions )

(Sanders & Mirabel, 1996)

rarerare ( not representative of the local universe) ( not representative of the local universe)

1995 ISO : detection of distant LIRGs and ULIRGs1995 ISO : detection of distant LIRGs and ULIRGs Far more numerousFar more numerous at higher redshifts at higher redshifts ISO number counts ISO number counts Elbaz et al, 1999, Aussel et al, 99 … IsolatedIsolated – or in little groups of galaxies ? – or in little groups of galaxies ?


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COBE/DIRBER=240 mB=60 mG=100 m

1996 :discovery of the CIRB (Puget et al, 1996)

Discovery of infrared galaxies

delphine marcillac moriond 2005 when uv meets ir... 1 ir properties of distant ir galaxies delphine...

Documents

lagache et et

chary et

dole et

yun et

goldader et

fadda et

papovitch et

ulirgsmeurer et