elodie giovannoli laboratoire d’astrophysique de marseille, france advisor : veronique buat...
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Elodie GIOVANNOLILaboratoire d’Astrophysique de Marseille, FRANCE
Advisor : Veronique BUATCollaborators : Denis Burgarella, Stefan Noll
Spectral energy distribution modeling from UV to 70µm for
LIRGs at z=0.7
15/12/2009ESF conference, Obergurgl
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OUTLINE
Motivation: accurate estimation of physical parameters , SED-fitting
1. Introduction : LIRGs’ characteristics
Description of the sample
2. SED fitting
Code CIGALE http://www.oamp.fr/cigale/
3. Application to the LIRGs sample
Mid-IR slope
SFR/Mass
4. Future task
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Population detected at 24 µm is dominated by LIRGs at 0.5≤z≤1.0
Plot :
At z≈1, IR-Luminous galaxies appears to be responsible for 70% of the comoving IR energy density.
REF: Le Floc’h et al. 05 Caputi et al. 07 Magnelli et al. 09 Roghiero et al. 09
Le Floc’h et al. 05
Study of LIRGs to understand the formation and evolution of galaxies from z=1.
LIRGs' characteristics (Luminous Infrared Galaxies)
ULIRGs
LIRGs
Low luminosity galaxies
Comoving IR energy density
1011 < LIR , L< 1012
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Description of the sampleSample of 181 LIRGs <z>=0.70 +/- 0.05 Detected at 24µm : f24µm ≥ 83 µJy
Sub-sample of 62 LIRGS (flux at 70 µm) Selection of the GTO SPITZER/MIPS CDFS (Chandra Deep Field South) (Le Floc’h et al. 2005), cross-correlated with MUSYC (Multiwavelength survey by Yale-Chile) and FIDEL (Far-Infrared Deep Extragalactic Legacy Survey)
UV (2310 A) GALEX images
U U38 B V R I z J H K MUSYC
3.6 4.5 5.8 8.0 µm CDFS, IRAC
24 and 70 µm CDFS + FIDEL, MIPS
17 filters
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CIGALE : Code Investigating GALaxy Emission *
SED-fitting
CIGALE code developped at LAM-Marseille (Burgarella et al. 05, Noll et al. 09)Task: To derive physical galaxy parameters from broad-band UV-to-IR SEDs at given redshifts.
INPUT : Photometric broad-bands
Star Formation History
Fraction of AGN
Dust Attenuation
IR library
AGN templates
Fit of the entire spectrum
Results : best model (χ2) + bayesian analysis (close to Kauffmann et al. 2003).
*http://www.oamp.fr/cigale/
*For now, only downloading the code is possible but a more sophisticated interface will be in place at the end of February 2010.
OUTPUT : input parameters + M, SFR, Ldust
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SFR0
SFR
SFR=SFR0.e-(t/tau)
age
Populations synthesis codes
Maraston et al. (2005) (including TP-AGB stars)
PEGASE
Stellar populations:
Combination of a young + an old stellar population with exponentially decreasing SFR at different rates.
Dust attenuation: Calzetti et al. (2000)
IR models:
Dale & Helou (2002) models , parametrised by the factor α, related to the ratio f60/f100
α : power law slope of the dust mass distribution over heating intensity
Wavelength, µm
t1 t2
AGN contribution : AGN templates, Siebenmorgen&Krugel 2004
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Application to the LIRGs sample : preliminary results of the bayesian analysis
Nu
mb
er o
f g
alax
ies
Log Mstar, M Log Ldust, L Log SFR, Myr-1
Age of ySP, Gyr Fraction of ySP Fraction of AGN
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Application to the LIRGs sample : preliminary results of the bayesian analysis
Nu
mb
er o
f g
alax
ies
Log Mstar, M Log Ldust, L Log SFR, Myr-1
Age of ySP, Gyr Fraction of ySP Fraction of AGN
Fraction of IR Luminosity reprocessed by dust heated by an AGN.
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AGN detection
Code CIGALE
49 objects identified
Stern et al. 2005
26 objects identified
Brand et al. 2006
9 objects identified
Total sample
After AGN identification:
Total sample: 121 objects70 µm sample : 42 objects
Before AGN identification:
Total sample: 181 objects70 µm sample : 62 objects
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Sample with a detection at 70μm, no AGNs
The mid-IR slope brings informations on the fit of IR libraries.
Dust temperature ?Association of a dust temperature following these models will give rather cold galaxies
L24/L70 higher than predicted by models.
In agreement with Zheng et al. 2007,stacking analysis
The mid-IR slope
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Sample with a detection at 70μm, no AGNs
The mid-IR slope brings informations on the fit of IR libraries.
Dust temperature ?Association of a dust temperature following these models will give rather cold galaxies
The mid-IR slope
The AGN contamination is too weak to induce such an increase of νLν24μm/νLν70μm observed.
The local SED templates are not well-suited to fit fluxes from distant galaxies.
See Symeonidis et al. 2009
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Magnelli et al. 2009
SFR density
Strong contribution to the star formation activity beyond z≈0.7
We expect actively star forming galaxies
LIRGs
Normal galaxies
ULIRGs
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Characteristics :
Millenium simulations underestimate the SFR
Mstar> 1011 M: in good agreement with semi analyticl models from Buat et al.08 and Noeske et al. 07
Mstar < 1011 M : in good agreement with Santini et al. 09 red area: unexepected high SFR , SFR/SFRmodels ~5
94% of the sample is actively star-bursting :M > 2.0.1010
The relation SFR/Mass
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Summary & perspectives
Our results show that CIGALE is able to fit SED from UV to FIR
Get ready forthcoming Herschel data
Improvment of the code to provide a valuable and friendly tool to interprete the future data of Herschel : HeRMES consortium
(The Herschel Multi-tiered Extragalactic Survey)
- Add IR libraries : Chary&Elbaz, Siebenmorgen&Krugel - Add AGN templates : accurate measure of the fraction of AGN
Fit of the IR counterpart thank to several black bodies Accurate estimation of the dust temperature
Evidence for a hot/cold population at high redshift?