Herschel PEP/HerMES: the redshift evolution (0 ≤ z ≤ 4) of dust attenuation and of the total (UV+IR) star formation rate density

By D. Burgarella, V. Buat, C. Gruppioni, O. Cucciati, Sébastien Heinis, S. Berta, M. B'ethermin, J. Bock, A. Cooray, J. Dunlop and 13 more. 2013

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Using new homogeneous luminosity functions (LFs) in the far-ultraviolet (FUV) from VVDS and in the far-infrared (FIR) from Herschel/PEP and Herschel/HerMES, we studied the evolution of the dust attenuation with redshift. With this information, we were able to estimate the redshift evolution of the total (FUV + FIR) star formation rate density (SFRDTOT). By integrating SFRDTOT, we followed the mass building and analyzed the redshift evolution of the stellar mass density (SMD). This article aims at providing a complete view of star formation from the local Universe to z ~ 4 and, using assumptions on earlier star formation history, compares this evolution with previously published data in an attempt to draw a homogeneous picture of the global evolution of star formation in galaxies. Our main conclusions are that: 1) the dust attenuation AFUV is found to increase from z = 0 to z ~ 1.2 and then starts to decrease until our last data point at z = 3.6; 2) the estimated SFRD confirms published results to z ~ 2. At z > 2, we observe either a plateau or a small increase up to z ~ 3 and then a likely decrease up to z = 3.6; 3) the peak of AFUV is delayed with respect to the plateau of SFRDTOT and a probable origin might be found in the evolution of the bright ends of the FUV and FIR LFs; 4) using assumptions (exponential rise and linear rise with time) for the evolution of the star formation density from z = 3.6 to zform = 10, we integrated SFRDTOT and obtained a good agreement with the published SMDs.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/092d64a340c25554118af249e2f64ad85f1e3efc

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Citations in the corpus

Evolution of galaxy stellar masses and star formation rates in the eagle simulations (2014, unknown): “For comparison, observations from Gilbank et al. (2010b) [H α], Rodighiero et al. (2010) [24μm], Karim et al. (2011) [Radio], Cucciati et al. (2012) [FUV], Bouwens et al. (2012) [UV], Robertson et al. (2013) [UV] and Burgarella et al. (2013) [FUV + FIR] are shown as well.”
The BAHAMAS project: Calibrated hydrodynamical simulations for large-scale structure cosmology (2016, background): “For comparison, we show a range of recent measurements which use different SFR tracers, including Rodighiero et al. (2010) (IR), Karim et al. (2011) (radio), Cucciati et al. (2012) (UV), Bouwens et al. (2012) (UV), and Burgarella et al. (2013) (IR+UV).”
Planck 2013 results. XXX. Cosmic infrared background measurements and implications for star formation (2013, result): “At higher redshift, our determination is marginally compatible (2σ) with Gruppioni et al. (2013), but in very good agreement with the recent work of Burgarella et al. (2013) at z = 3.”
CO excitation of normal star forming galaxies out to $z=1.5$ as regulated by the properties of their interstellar medium (2014, background): “On the other hand, the ISM dust attenuation properties are not changing much with only a modest rise of the attenuation at fixed stellar mass (e.g., Pannella et al 2014; Burgarella et al 2013) that is justified by the increase of the dust to stellar mass ratio (Tan et al 2014).”
Evolution of the dust emission of massive galaxies up to z=4 and constraints on their dominant mode of star formation (2014, background): “This trend is probably driven by the decrease in the infrared luminosity density at high redshift (Planck Collaboration XXX 2014; Burgarella et al. 2013) combined with the decrease in the number density of infrared emitters (Gruppioni et al. 2013).”
A unified multiwavelength model of galaxy formation (2015, background): “26 are based on a variety of SFR tracers: far-UV light (Cucciati et al. 2012; Oesch et al. 2012a), far-IR + far-UV luminosity (Burgarella et al. 2013),Hα emission (Sobral et al. 2013; Gunawardhana et al. 2013), and non-thermal radio emission (Karim et al. 2011).”
Introducing the Illustris Project: the evolution of galaxy populations across cosmic time (2014, unknown): “This prescription was calibrated for nearby galaxies, and hence probably it represents an overestimate for the dust extinction at high redshift, and in particular at low masses, where the metallicity is significantly lower7 (Bouwens et al. 2013; Burgarella et al. 2013).”
A deep ALMA image of the Hubble Ultra Deep Field (2016, background): “A complete understanding of cosmic star-formation history, and the physical mechanisms that drive galaxy formation and evolution, requires that we connect our UV/optical and infrared/mm views of the Universe (e.g. Hopkins & Beacom 2006; Dunlop 2011; Burgarella et al. 2013; Madau & Dickinson 2014).”
GRAVITATIONAL LENS MODELS BASED ON SUBMILLIMETER ARRAY IMAGING OF HERSCHEL-SELECTED STRONGLY LENSED SUB-MILLIMETER GALAXIES AT z > 1.5 (2013, background): “…Scale of Star-formation in Herschel-selected Lensed SMGs One of the central themes in understanding the evolution of the most luminous galaxies during the epoch of peak star-formation rate density in the Universe (i.e., 1 < z < 4; e.g., Burgarella et al. 2013) is the role played by major mergers.”
GOODS-HERSCHEL: STAR FORMATION, DUST ATTENUATION, AND THE FIR–RADIO CORRELATION ON THE MAIN SEQUENCE OF STAR-FORMING GALAXIES UP TO z ≃ 4 (2014, background): “…Pannella et al. 2009b; Bouwens et al. 2009; Ilbert et al. 2010; Hopkins & Beacom 2006; Karim et al. 2011; Muzzin et al. 2013; Ilbert et al. 2013; Burgarella et al. 2013; Madau & Dickinson 2014), we must now try to understand which are the main processes that drive the star formation histories…”
How sensitive are predicted galaxy luminosities to the choice of stellar population synthesis model (2013, methodology): “The diamonds show the total SFRD estimated by Burgarella et al. (2013) using both UV and IR observations.”
Constraining the properties of AGN host galaxies with spectral energy distribution modelling (2015, methodology): “The ones related to the galaxy host emission templates are selected based on the experience gained from galaxy SED modeling at intermediate and high redshift using CIGALE (e.g., Giovannoli et al. 2011; Buat et al. 2012; Burgarella et al. 2013; Buat et al. 2014).”