%0 Generic %1 Wuyts2011 %A Wuyts, Stijn %A Schreiber, Natascha M. Forster %A Lutz, Dieter %A Nordon, Raanan %A Berta, Stefano %A Altieri, Bruno %A Andreani, Paola %A Aussel, Herve %A Bongiovanni, Angel %A Cepa, Jordi %A Cimatti, Andrea %A Daddi, Emanuele %A Elbaz, David %A Genzel, Reinhard %A Koekemoer, Anton M. %A Magnelli, Benjamin %A Maiolino, Roberto %A McGrath, Elizabeth J. %A Garcia, Ana Perez %A Poglitsch, Albrecht %A Popesso, Paola %A Pozzi, Francesca %A Sanchez-Portal, Miguel %A Sturm, Eckhard %A Tacconi, Linda %A Valtchanov, Ivan %D 2011 %K calibration high-z sfh sfr %T On Star Formation Rates and Star Formation Histories of Galaxies out to z ~ 3 %U http://arxiv.org/abs/1106.5502 %X We compare multi-wavelength SFR indicators out to z~3 in GOODS-South. Our analysis uniquely combines U-to-8um photometry from FIREWORKS, MIPS 24um and PACS 70, 100, and 160um photometry from the PEP survey, and Ha spectroscopy from the SINS survey. We describe a set of conversions that lead to a continuity across SFR indicators. A luminosity-independent conversion from 24um to total infrared luminosity yields estimates of LIR that are in the median consistent with the LIR derived from PACS photometry, albeit with significant scatter. Dust correction methods perform well at low to intermediate levels of star formation. They fail to recover the total amount of star formation in systems with large SFR_IR/SFR_UV ratios, typically occuring at the highest SFRs (SFR_UV+IR 100 Msun/yr) and redshifts (z 2.5) probed. Finally, we confirm that Ha-based SFRs at 1.5<z<2.6 are consistent with SFR_SED and SFR_UV+IR provided extra attenuation towards HII regions is taken into account (Av,neb = Av,continuum / 0.44). With the cross-calibrated SFR indicators in hand, we perform a consistency check on the star formation histories inferred from SED modeling. We compare the observed SFR-M relations and mass functions at a range of redshifts to equivalents that are computed by evolving lower redshift galaxies backwards in time. We find evidence for underestimated stellar ages when no stringent constraints on formation epoch are applied. We demonstrate how resolved SED modeling, or alternatively deep UV data, may help to overcome this bias. The age bias is most severe for galaxies with young stellar populations, and reduces towards older systems. Finally, our analysis suggests that SFHs typically vary on timescales that are long (at least several 100 Myr) compared to the galaxies' dynamical time.

@misc{Wuyts2011, abstract = { We compare multi-wavelength SFR indicators out to z~3 in GOODS-South. Our analysis uniquely combines U-to-8um photometry from FIREWORKS, MIPS 24um and PACS 70, 100, and 160um photometry from the PEP survey, and Ha spectroscopy from the SINS survey. We describe a set of conversions that lead to a continuity across SFR indicators. A luminosity-independent conversion from 24um to total infrared luminosity yields estimates of LIR that are in the median consistent with the LIR derived from PACS photometry, albeit with significant scatter. Dust correction methods perform well at low to intermediate levels of star formation. They fail to recover the total amount of star formation in systems with large SFR_IR/SFR_UV ratios, typically occuring at the highest SFRs (SFR_UV+IR \gtrsim 100 Msun/yr) and redshifts (z \gtrsim 2.5) probed. Finally, we confirm that Ha-based SFRs at 1.5<z<2.6 are consistent with SFR_SED and SFR_UV+IR provided extra attenuation towards HII regions is taken into account (Av,neb = Av,continuum / 0.44). With the cross-calibrated SFR indicators in hand, we perform a consistency check on the star formation histories inferred from SED modeling. We compare the observed SFR-M relations and mass functions at a range of redshifts to equivalents that are computed by evolving lower redshift galaxies backwards in time. We find evidence for underestimated stellar ages when no stringent constraints on formation epoch are applied. We demonstrate how resolved SED modeling, or alternatively deep UV data, may help to overcome this bias. The age bias is most severe for galaxies with young stellar populations, and reduces towards older systems. Finally, our analysis suggests that SFHs typically vary on timescales that are long (at least several 100 Myr) compared to the galaxies' dynamical time. }, added-at = {2011-06-29T09:06:08.000+0200}, author = {Wuyts, Stijn and Schreiber, Natascha M. Forster and Lutz, Dieter and Nordon, Raanan and Berta, Stefano and Altieri, Bruno and Andreani, Paola and Aussel, Herve and Bongiovanni, Angel and Cepa, Jordi and Cimatti, Andrea and Daddi, Emanuele and Elbaz, David and Genzel, Reinhard and Koekemoer, Anton M. and Magnelli, Benjamin and Maiolino, Roberto and McGrath, Elizabeth J. and Garcia, Ana Perez and Poglitsch, Albrecht and Popesso, Paola and Pozzi, Francesca and Sanchez-Portal, Miguel and Sturm, Eckhard and Tacconi, Linda and Valtchanov, Ivan}, biburl = {https://www.bibsonomy.org/bibtex/24d61f64a7bac8246fa26863c70876c44/miki}, description = {[1106.5502] On Star Formation Rates and Star Formation Histories of Galaxies out to z ~ 3}, interhash = {6854952ec8fbaf0ca53143f114108ada}, intrahash = {4d61f64a7bac8246fa26863c70876c44}, keywords = {calibration high-z sfh sfr}, note = {cite arxiv:1106.5502Comment: Accepted for publication in The Astrophysical Journal, 19 pages, 15 figures}, timestamp = {2011-06-29T09:06:08.000+0200}, title = {On Star Formation Rates and Star Formation Histories of Galaxies out to z ~ 3}, url = {http://arxiv.org/abs/1106.5502}, year = 2011 }