The complex physics of dusty star-forming galaxies at high redshifts as revealed by Herschel and Spitzer
Date
2013Author
Lo Faro, Barbara
Franceschini, Alberto
Vaccari, M.
Silva, L.
Rodighiero, G.
Berta, S.
Bock, J.
Burgarella, D.
Buat, V.
Cava, A.
Clements, D.L.
Cooray, Asantha
Farrah, D.
Feltre, Anna
Gonzalez-Solares, Eduardo A.
Hurley, P.
Lutz, D.
Magdis, G.
Magnelli, B.
Marchetti, L.
Oliver, S.J.
Page, Matthew J.
Popesso, P.
Pozzi, F.
Rigopoulou, D.
Rowan-Robinson, M.
Roseboom, I.G.
Scott, Douglas
Smith, A.J.
Symeonidis, Myrto
Wang, L.
Wuyts, S.
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Show full item recordAbstract
We combine far-infrared photometry from Herschel (PEP/HerMES) with deep mid-infrared spectroscopy from
Spitzer to investigate the nature and the mass assembly history of a sample of 31 luminous and ultraluminous
infrared galaxies ((U)LIRGs) at z ∼ 1 and 2 selected in GOODS-S with 24μm fluxes between 0.2 and 0.5 mJy.We
model the data with a self-consistent physical model (GRASIL) which includes a state-of-the-art treatment of dust
extinction and reprocessing. We find that all of our galaxies appear to require massive populations of old (>1 Gyr)
stars and, at the same time, to host a moderate ongoing activity of star formation (SFR 100M yr−1). The bulk of
the stars appear to have been formed a few Gyr before the observation in essentially all cases. Only five galaxies of
the sample require a recent starburst superimposed on a quiescent star formation history.We also find discrepancies
between our results and those based on optical-only spectral energy distribution (SED) fitting for the same objects;
by fitting their observed SEDs with our physical model we find higher extinctions (by ΔAV ∼ 0.81 and 1.14)
and higher stellar masses (by Δlog(M ) ∼ 0.16 and 0.36 dex) for z ∼ 1 and z ∼ 2 (U)LIRGs, respectively. The
stellar mass difference is larger for the most dust-obscured objects. We also find lower SFRs than those computed
from LIR using the Kennicutt relation due to the significant contribution to the dust heating by intermediate-age
stellar populations through “cirrus” emission (∼73% and ∼66% of the total LIR for z ∼ 1 and z ∼ 2 (U)LIRGs,
respectively).
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