Evolution of the comoving infrared energy density up to z~1 * Emeric Le Floch, Casey Papovich,...
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Transcript of Evolution of the comoving infrared energy density up to z~1 * Emeric Le Floch, Casey Papovich,...
Evolution of the comoving infraredenergy density up to z~1
* Emeric Le Floc’h, Casey Papovich, Eiichi Egami, George Rieke & the MIPS team (Steward Observatory, University of Arizona)
What can we learn from Spitzer ?
Rencontres de Moriond, March 6-12th 2005
* Hervé Dole & Guilaine Lagache (IAS-Orsay)
Chandra Deep Field South, MIPS 24μm
* Eric Bell (MPIA)
Redshift distribution @ 24μm
Rencontres de Moriond, March 6-12th 2005
- Chary et al. 2004- Gruppioni et al. 2005- Lagache et al. 2004- Pearson 2005
Predictions for flux limit : 80 μJy
(also Lewis et al. 2005)
Courtesy R.Chary/C.Gruppioni/C.Pearson
Chandra Deep Field South 24μm
Integ. time : 1380s / sky pixel 5 ~ 80 μJy ( ~5 sources / arcmin )2
~20’
Rencontres de Moriond, March 6-12th 2005
Chandra Deep Field South 24μm
Rencontres de Moriond, March 6-12th 2005
5589 MIPS sources
* 465 with spec z* 2170 with phot z (total 2635 with redshift)
MIPS 24μm
775 arcmin2
Le Fèvre et al. Vanzella et al.Szokoly et al. Wolf et al.
R-band mag versus Flux@24μm
Rencontres de Moriond, March 6-12th 2005
80% completeness limit at 24μm
VERY hard to be complete in the redshift identification at any 24μm flux, using VVDS/GOODS/COMBO-17
Rencontres de Moriond, March 6-12th 2005
Characterization of the completeness
Redshift identification (24μm-selected)
MIPS sourcehistograms
Complete identification up to z~0.8
Phot. z versus Spec. z
Rencontres de Moriond, March 6-12th 2005
Optically-selected sources MIPS sources
(COMBO-17 versus VVDS)
.
COMBO-17 photo. z
Rencontres de Moriond, March 6-12th 2005
Optically-selected sources
MIPS sources
Photometric redshift classification not dependent on the infrared luminosity
(IR emission very localized, does not affect the SED of the host galaxy)
Photo-z uncertainties:
<z> < 0.04 for R<22mag <z> < 0.09 for R<24mag
Rencontres de Moriond, March 6-12th 2005
Redshift distribution
~55% of 24μm sources at z<1 (flux 80μJy)
COMBO-17
VVDS
MIPSRedshift
CDFS
Total COMBO-17 (3 fields 30’x30’)
B-b
an
d l
um
in.
de
ns
ity
R<25.5
M <-16B
Rencontres de Moriond, March 6-12th 2005
Cumulative counts
~85% identified with R<25.5
optical counterparts
averaged over5 fields
(Papovich et al.)
observed in CDFS
CDFS underdensity
Cumulative counts
Rencontres de Moriond, March 6-12th 2005
Lagache et al.
Pearson
Gruppioni et al.
Chary et al.
15 10 5Wavelength
F
.
LIRGs
ULIRGsF = 0.3mJy
F = 0.08mJy24μm
24μm
Rencontres de Moriond, March 6-12th 2005
24 μm IR luminosity ?
IR luminosities in the CDFS
2635 sourceswith redshifts
* Modest IR emitters at 0<z<0.5
* ULIRGs : quite rare at 0<z<1
* LIRGS: significant contribution at z>0.5
* More « normal » starbursts are not negligible neither
80% completeness limit
Rencontres de Moriond, March 6-12th 2005
60 μm luminosity Functions
Local IRAS LF
Rencontres de Moriond, March 6-12th 2005
(Local LF 60mic : Saunders et al. 1990, Takeuchi et al. 2003)
60 μm luminosity Functions
Rencontres de Moriond, March 6-12th 2005
(L,z)=*(z) [L/L*(z), z=0]
L*
*
* Evolution in luminosity :
L*(z) = L* (1+z) oL
* Evolution in density :
*(z) = * (1+z) o D
A « too strong » evolution in density overproduce the counts at the faint end
Additional constraints from the counts at faint fluxes (Chary et al. 2004, Papovich et al. 2004)
Evolution of the LF
Rencontres de Moriond, March 6-12th 2005
L D =
Papovich et al.
Simulations (z<1)
* exclude a pure evolution in density (Blain et al. 99. Xu et al. 00, Chary & Elbaz 01, ....)
Star formation history at z<1
LIRGs/ULIRGs dominate beyond z~0.7
Chary & Elbaz 2001
Blain et al. 2002
Lagache et al. 2004
. . . . . .
_ _ _ _ _
ULIRGs
total
L >10 L .11
IR
L <10 L .11
IR
Rencontres de Moriond, March 6-12th 2005
Compilation by Hopkins 2004
Star formation history at z<1
LIRGs/ULIRGs dominate beyond z~0.7
AGN contribution ??* ISO/XMM : <20% (Fadda et al. 2002)* X-ray +IR bkg synthetic models : <5% (e.g., Silva et al. 2004)
First Spitzer results : <15% of sources flagged as AGNs by VVDS& COMBO-17 (see also SWIRE, Franceschini et al. 2005)
Rencontres de Moriond, March 6-12th 2005
Star formation history at z<1
LIRGs/ULIRGs dominate beyond z~0.7
Contribution fromunobscured star
formation ??
* 60% understimate at z~0* 20-30% at z~1
Rencontres de Moriond, March 6-12th 2005
Stellar masses
IR-luminous sources are more massive than field optically-selected galaxies
IMF: Salpeter 55
COMBO-17
MIPS sourcesLIRGs
L >10 L .11.5
IR
Rencontres de Moriond, March 6-12th 2005
(see C.Xu ‘s review this morning)
Star formation history at z<1
LIRGs/ULIRGs dominate beyond z~0.7
Chary & Elbaz 2001
Blain et al. 2002
Lagache et al. 2004
. . . . . .
_ _ _ _ _
ULIRGs
total
L >10 L .11
IR
L <10 L .11
IR
Rencontres de Moriond, March 6-12th 2005
Compilation by Hopkins 2004
MIPS in the redshift desert
(Le Floc’h et al. 2004)
Rencontres de Moriond, March 6-12th 2005
* Balmer-break selection :(Adelberger et al. 2004)
* « GALEX drop-outs » : z>1
* IRAC color-color plots :3.6-4.5 versus 5.8-8.0
(IRAC photo-z technique)
Bimodal redshift distribution of the MIPS sources ?? Still debated(i.e., SSC results [D.Fadda yesterday] versus Perez-Gonzalez et al..........)
(C.Martin’s review yesterday)
* 55~65 % of 24μm sources at z<1 for flux>80μJy
Summary
* At 0<z<1, L* evolves at least by (1+z) ( exclude a pure density evolution)
3.5
* IR luminous galaxies start to dominate the SFRH at z>0.6
* LIRGs+ULIRGs = 70% of SFR at z=1
* Need a better understanding of IR SEDs : IRS GTO, MIPS SED mode...
Cornell University - Ithaca, December 1st 2004