The Star Formation Rate Density and Dust Attenuation Evolution over 12 Gyr with the VVDS Surveys

By O. Cucciati, L. Tresse, O. Ilbert, O. Fèvre, B. Garilli, V. Brun, P. Cassata, P. Franzetti, D. Maccagni, M. Scodeggio and 8 more. 2011

228 citations recorded by the source corpus.

[Abridged] We investigate the global galaxy evolution over 12 Gyr (0.05 1.7, we set alpha steepening with (1+z). The absolute magnitude M*_FUV brightens in the entire range 0 2 it is on average brighter than in the literature, while phi* is smaller. Our total LD shows a peak at z=2, present also when considering all sources of uncertainty. The SFRD history peaks as well at z=2. It rises by a factor of 6 during 2 Gyr (from z=4.5 to z=2), and then decreases by a factor of 12 during 10 Gyr down to z=0.05. This peak is mainly produced by a similar peak within the population of galaxies with -21.5 2 of the SFRD is compelling for models of galaxy formation. The mean dust attenuation A_FUV of the global galaxy population rises by 1 mag during 2 Gyr from z=4.5 to z=2, reaches its maximum at z=1 (A_FUV=2.2 mag), and then decreases by 1.1 mag during 7 Gyr down to z=0. The dust attenuation maximum is reached 2 Gyr after the SFRD peak, implying a contribution from the intermediate-mass stars to the dust production at z<2.

Subfields: Astronomy and Astrophysics, Electrical and Electronic Engineering, Instrumentation

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Citations in the corpus

THE AVERAGE STAR FORMATION HISTORIES OF GALAXIES IN DARK MATTER HALOS FROM z = 0–8 (2012, unknown): “…0.2− 3 1.4 GHz 2 deg2 Ly et al. (2011b) 1− 3 UV 0.241 deg2 AI Kajisawa et al. (2010) 0.5− 3.5 UV/IR 0.029 deg2 AI Dunne et al. (2009) 0− 4 1.4 GHz 0.8 deg2 I Cucciati et al. (2012) 0− 5 UV 0.611 deg2 I Le Borgne et al. (2009) 0− 5 IR-mm varies I van der Burg et al. (2010) 3− 5 UV 4 deg2…”
Galactic star formation and accretion histories from matching galaxies to dark matter haloes (2012, background): “…estimates derived from the UV (Salim et al. 2007; van der Burg et al. 2010; Bouwens et al. 2009; Robotham & Driver 2011; Bouwens et al. 2011; Cucciati et al. 2012), Hα (Ly et al. 2011), both UV and IR (Zheng et al. 2007), the FIR (Rujopakarn et al. 2010) and from radio observations…”
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).”
The deepest Herschel-PACS far-infrared survey: number counts and infrared luminosity functions from combined PEP/GOODS-H observations (2013, methodology): “Combined with the unobscured SFR density of the Universe derived by Cucciati et al. (2012) using rest-frame UV observations, we can then infer the total SFR density and its evolution up to z∼ 2 (dashed red line on a white background in the bottom right panel of Fig.”
UniverseMachine: The correlation between galaxy growth and dark matter halo assembly from z = 0−10 (2018, unknown): “…al. (2010) 0.5-3.5 UV/IR 0.03 I Schreiber et al. (2015) 0-4 FIR 1.75 IN Planck Collab. et al. (2014) 0-4 FIR 2240 IN Dunne et al. (2009) 0-4 Radio 0.8 I Cucciati et al. (2012) 0-5 UV 0.6 I Le Borgne et al. (2009) 0-5 IR-mm varies I van der Burg et al. (2010) 3-5 UV 4 I Yoshida et al. (2006) 4-5 UV…”
Galaxy Protoclusters as Drivers of Cosmic Star Formation History in the First 2 Gyr (2017, result): “The global CSFRD predicted in the models are in general agreement with that derived observationally (Schiminovich et al. 2005; Cucciati et al. 2012; Oesch et al. 2013; Finkelstein et al. 2015), with a broad peak at z = 1–3 and decays on both sides.”
The rate, luminosity function and time delay of non-Collapsar short GRBs (2014, methodology): “The lower redshift part of this SFR is measured using the VIMOS-VLT Deep Survey, a single deep galaxy redshift survey (Cucciati et al. 2012) up to redshift z ∼ 4.5.”
Extragalactic science, cosmology, and Galactic archaeology with the Subaru Prime Focus Spectrograph (2012, unknown): “We will observe sources brighter thanL∗, with massesM∗ > 1010 M⊙, typicallyM∗ ≈ 1011 M⊙ (see, e.g., Cucciati et al. 2012).”
The VIMOS VLT Deep Survey final data release: a spectroscopic sample of 35 016 galaxies and AGN out to z ~ 6.7 selected with 17.5 ≤ iAB ≤ 24.75 (2013, methodology): “The luminosity function and star-formation rate evolution presented in Cucciati et al. (2012) have used the latest VVDS weights, as presented here.”
GRB hosts through cosmic time - VLT/X-Shooter emission-line spectroscopy of 96 γ-ray-burst-selected galaxies at 0.1 (2015, background): “Interestingly, however, a very similar trend - highest visual extinctions at z ∼ 1.5 − 2 - exists in the complete sample of AV values derived from afterglow data (Covino et al. 2013) and in the evolution of the far UV attenuation in field galaxies (Cucciati et al. 2012).”
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).”
The ESO UVES advanced data products quasar sample: II. Cosmological evolution of the neutral gas mass density (2013, background): “Top panel: Total dust-corrected UV-derived SFR density as a function of lookback time from the visible multi object-spectrograph (VIMOS)-VLT deep survey (VVDS) Deep + Ultra-Deep sample from Cucciati et al. (2012) is illustrated as black open circles.”
How sensitive are predicted galaxy luminosities to the choice of stellar population synthesis model (2013, background): “The crosses show the SFRD estimated by Cucciati et al. (2012) from the the intrinsic non-ionising UV stellar continuum of galaxies.”
THE EVOLUTION OF THE GALAXY REST-FRAME ULTRAVIOLET LUMINOSITY FUNCTION OVER THE FIRST TWO BILLION YEARS (2014, methodology): “Thanks to the combination of observations from GALEX and HST, estimates of the UV luminosity function now exist from z < 1 (Arnouts et al. 2005; Cucciati et al. 2012) out to z 8 (e.g., Bouwens et al. 2007, 2011b; McLure et al. 2009; Oesch et al. 2012, 2013; Lorenzoni et al. 2013).”
The EAGLE simulations of galaxy formation: the importance of the hydrodynamics scheme (2015, methodology): “Observational data from Rodighiero et al. (2010), Karim et al. (2011), Cucciati et al. (2012) and Bouwens et al. (2012) is also shown.”
ALMA SPECTROSCOPIC SURVEY IN THE HUBBLE ULTRA DEEP FIELD: THE INFRARED EXCESS OF UV-SELECTED z = 2–10 GALAXIES AS A FUNCTION OF UV-CONTINUUM SLOPE AND STELLAR MASS (2016, background): “…energy output from UV - selected galaxies at far-infrared wavelengths is most developed over the redshift range z ∼ 0 to z ∼ 3, with increasing maturity (Reddy et al. 2008; Daddi et al. 2009; Magnelli et al. 2009, 2011, 2013; Karim et al. 2011; Cucciati et al. 2012; Álvarez-Márquez et al. 2016).”