IR%20properties%20of%20distant%20IR%20galaxies

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• IR properties of distant IR galaxies
• Delphine Marcillac
• (PhD student)
• Supervisor D. Elbaz
• In collaboration with Emeric Le Floch
• Herve Dole
• Ranga Chary
• Mark Dickinson
• GOODS
  consortium
• Emmanuel Moy

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Detection of distant LIRGs
1983 IRAS local LIRGs and ULIRGs gt rare
1995 ISO distant LIRGs and ULIRGs
(ISO number counts
gt more numerous
1996 discovery of the CIRB
2003 SPITZER
Detection of LIRGs and ULIRGs beyond z 1
gt 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.
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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
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Origin of the IR emission

• AGN ex NGC 1068 SB ex NGC 4038/39

Fadda et al, 2001 lt 20
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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 z0.7 )
• From the radio correlation radio LIR (Condon
  1992, Yun et al, 2001)
• not deep enough

Fllb 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)
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• 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
  gt FIRgt LIR gt SFR
• Chary
  Elbaz 2001 Kennicutt 1998
• Dale Helou, 2002
• Lagache et et al, 2004
• ..

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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
• gtLocal templates

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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

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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 z0.7.
• Elbaz et al, 2005 AA Letters (in
  press)
• LIR radio in agrement with LIR MIR
• distant MIR is not very different .

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Marano field
The PAH bump exists at z0.7-1
(Elbaz et al. 99, 04) ISOCAM Emeric Le
Floch/H.Dole MIPS
30'
Marano field MIPS 24 mm (E. Le
Floc'h/H.Dole) (Spitzer-MIPS Early
Characterization Observation)
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SED of a LIRG at z0.69 (LIR1011.1 L?,SFR22
M?yr-1)
The PAH bump exists at z0.7
12
Compatible with NGC 1068
No compatible with NGC 1068
Compatible with NGC 1068
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MIR SEDs of distant galaxies
Great Observatories Origins Deep Surveys
Deep Survey Spitzer-MIPS 24 mm 1002
ISOCAM 15 mm 52
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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
• 0.3ltzlt1.3
• 3 AGNs 4 ? ( to be studied)

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LIR (radio) versus LIR (MIR)
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PAH at z1 ? L7 versus L12

• observed RF
  
• Z1 24 mm (MIPS) 12 mm
  IRAS
• 15 mm (ISO-LW3) 7 mm
  ISOLW2

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The silicate absorption at z0.6L10 versus L7

• z 0.6
• 24 mm (MIPS) gt 15
  mm(ISO)
• 15 mm (ISO-LW3)
• 12 mm (IRAS 12 mm) gt new filter for
  local galaxies

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The SFR / mass relation
IRAS Starbursts (Pasquali et al , in prep)
Distant Starbursts
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Conclusion

• SFR and LIR can be derived from MIR up to z1.2
• MIR properties of distant galaxies have weakly
  evolved up to z1.2
• but IRS spectra of LIRGs are needed

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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

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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
ISOCAM image (7 and 15 mm)
HST-WFPC2 in B band (5252 A) and I band (8269 A)
High star formation area 60 of the CO(1-0)
emission
Sanders and Mirabel,1985
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Discovery of infrared galaxies
1983 IRAS detection of local LIRGs and ULIRGs

• detection of LIRGs (11lt log (LIR/Lo)lt12 )
• ULIRGs (12 ltlog 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 ?
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Discovery of infrared galaxies
1996 discovery of the CIRB (Puget et al, 1996)
COBE/DIRBE R240 mm B60 mm G100 mm