The Dust-Unbiased Cosmic Star-Formation History From the 20 Cm Vla-Cosmos Survey

Smolčić, Vernesa; Schinnerer, E.; Zamorani, G.; Bell, Eric F.; Bondì, M.; Carilli, C. L.; Ciliegi, P.; Mobasher, Bahram; Paglione, Timothy A. D.; Scodeggio, M.; Scoville, N. Z.

doi:10.1088/0004-637x/690/1/610

Cited by 130 publications

(213 citation statements)

References 53 publications

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“…Dark blue triangles represent the SFR density estimated by Seymour et al (2008) using deep radio observations. Green circles represent the SFR density estimated by Smolčić et al (2009) using deep 20 cm observations and dark blue squares represent the relative contribution of ULIRGs to this SFR density.…”

Section: Discussionmentioning

confidence: 99%

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

Magnelli

Elbaz

Chary

et al. 2011

A&A

352

422

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Aims. We derive the evolution of the infrared luminosity function (LF) over the last 4/5ths of cosmic time using deep 24 and 70 μm imaging of the GOODS North and South fields. Methods. We use an extraction technique based on prior source positions at shorter wavelengths to build the 24 and 70 μm source catalogs. The majority (93%) of the sources have a spectroscopic (39%) or a photometric redshift (54%) and, in our redshift range of interest (i.e., 1.3 < z < 2.3) ∼20% of the sources have a spectroscopic redshift. To extend our study to lower 70 μm luminosities we perform a stacking analysis and we characterize the observed L 24/(1+z) vs. L 70/(1+z) correlation. Using spectral energy distribution (SED) templates which best fit this correlation, we derive the infrared luminosity of individual sources from their 24 and 70 μm luminosities. We then compute the infrared LF at z ∼ 1.55 ± 0.25 and z ∼ 2.05 ± 0.25. Results. We observe the break in the infrared LF up to z ∼ 2.3. The redshift evolution of the infrared LF from z = 1.3 to z = 2.3 is consistent with a luminosity evolution proportional to (1 + z) 1.0±0.9 combined with a density evolution proportional to (1 + z) −1.1±1.5 . At z ∼ 2, luminous infrared galaxies (LIRGs: 10 11 L < L IR < 10 12 L ) are still the main contributors to the total comoving infrared luminosity density of the Universe. At z ∼ 2, LIRGs and ultra-luminous infrared galaxies (ULIRGs: 10 12 L < L IR ) account for ∼49% and ∼17% respectively of the total comoving infrared luminosity density of the Universe. Combined with previous results using the same strategy for galaxies at z < 1.3 and assuming a constant conversion between the infrared luminosity and star-formation rate (SFR) of a galaxy, we study the evolution of the SFR density of the Universe from z = 0 to z = 2.3. We find that the SFR density of the Universe strongly increased with redshift from z = 0 to z = 1.3, but is nearly constant at higher redshift out to z = 2.3. As part of the online material accompanying this article, we present source catalogs at 24 μm and 70 μm for both the GOODS-North and -South fields.

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Section: Discussionmentioning

confidence: 99%

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

Magnelli

Elbaz

Chary

et al. 2011

A&A

352

422

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“…10). Measured SFR densities were taken from the compilation by Behroozi et al (2013), which includes Hα (Sobral et al 2012;Tadaki et al 2011;Shim et al 2009) radio (1.4 GHz; Karim et al 2011;Dunne et al 2009;Smolčić et al 2009), combined ultraviolet/infrared (Gruppioni et al 2015;Cucciati et al 2012;Kajisawa et al 2010;Salim et al 2007;Zheng et al 2007), ultraviolet data only (Bouwens et al 2012;Robotham & Driver 2011;van der Burg et al 2010;Yoshida et al 2006), and far infrared data only (Rujopakarn et al 2010;Le Borgne et al 2009). The default model is in good agreement with observation at z > 2 (especially with UV data) because it has strong feedback that suppresses star formation but forms too many stars at low z (Figs.…”

Section: Star Formation Ratesmentioning

confidence: 99%

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

Cattaneo

Blaizot

Devriendt

et al. 2017

Monthly Notices of the Royal Astronomical Society

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GalICS 2.0 is a new semianalytic code to model the formation and evolution of galaxies in a cosmological context. N-body simulations based on a Planck cosmology are used to construct halo merger trees, track subhaloes, compute spins and measure concentrations. The accretion of gas onto galaxies and the morphological evolution of galaxies are modelled with prescriptions derived from hydrodynamic simulations. Star formation and stellar feedback are described with phenomenological models (as in other semianalytic codes). GalICS 2.0 computes rotation speeds from the gravitational potential of the dark matter, the disc and the central bulge. As the rotation speed depends not only on the virial velocity but also on the ratio of baryons to dark matter within a galaxy, our calculation predicts a different Tully-Fisher relation from models in which v rot ∝ v vir . This is why GalICS 2.0 is able to reproduce the galaxy stellar mass function and the Tully-Fisher relation simultaneously. Our results are also in agreement with halo masses from weak lensing and satellite kinematics, gas fractions, the relation between star formation rate (SFR) and stellar mass, the evolution of the cosmic SFR density, bulge-to-disc ratios, disc sizes and the Faber-Jackson relation.

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“…In the past decade it has been demonstrated that a panchromatic, X-ray to radio, observational approach is key to develop a consensus on galaxy formation and evolution (e.g., Dickinson et al 2003;Scoville et al 2007;Driver et al 2009Driver et al , 2011Koekemoer et al 2011;Grogin et al 2011). In this context, the radio regime offers an indispensable window toward star formation and supermassive black hole properties of galaxies as radio A&A 602, A1 (2017) continuum emission i) provides a dust-unbiased star formation tracer at high angular resolution (e.g., Condon 1992;Haarsma et al 2000;Seymour et al 2008;Smolčić et al 2009b;Karim et al 2011); and ii) directly probes those active galactic nuclei (AGN) that are hosted by the most massive quiescent galaxies and deemed crucial for massive galaxy formation (e.g., Croton et al 2006;Bower et al 2006;Best et al 2006;Evans et al 2006;Hardcastle et al 2007;Smolčić et al 2009aSmolčić et al , 2015Smolčić 2009;Smolčić & Riechers 2011).…”

Section: Introductionmentioning

confidence: 99%

“…These past surveys have shown that deep observations at high angular resolution ( 1 ) with exquisite panchromatic coverage are critical to comprehensively study the radio properties of the main galaxy populations, avoiding cosmic variance with large area coverage (e.g., Padovani et al 2009;Padovani 2011;Smolčić et al 2008Smolčić et al , 2009bSmolčić 2009;Smolčić & Riechers 2011;Seymour et al 2008;Bonzini et al 2012Bonzini et al , 2013. In this context, large area surveys down to unprecedented depths are planned with new and upgraded facilities (e.g., VLA, Westerbork, Australian Square Kilometre Array Pathfinder, MeerKAT, and Square Kilometre Array; e.g., Jarvis 2012; Norris et al 2011Norris et al , 2013Norris et al , 2015Prandoni & Seymour 2015).…”

Section: Introductionmentioning

confidence: 99%

The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release

Smolčić

Novak

Bondì

et al. 2017

A&A

Self Cite

309

365

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We present the VLA-COSMOS 3 GHz Large Project based on 384 h of observations with the Karl G. Jansky Very Large Array (VLA) at 3 GHz (10 cm) toward the two square degree Cosmic Evolution Survey (COSMOS) field. The final mosaic reaches a median rms of 2.3 µJy beam −1 over the two square degrees at an angular resolution of 0.75 . To fully account for the spectral shape and resolution variations across the broad (2 GHz) band, we image all data with a multiscale, multifrequency synthesis algorithm. We present a catalog of 10 830 radio sources down to 5σ, out of which 67 are combined from multiple components. Comparing the positions of our 3 GHz sources with those from the Very Long Baseline Array (VLBA)-COSMOS survey, we estimate that the astrometry is accurate to 0.01 at the bright end (signal-to-noise ratio, S /N 3 GHz > 20). Survival analysis on our data combined with the VLA-COSMOS 1.4 GHz Joint Project catalog yields an expected median radio spectral index of α = −0.7. We compute completeness corrections via Monte Carlo simulations to derive the corrected 3 GHz source counts. Our counts are in agreement with previously derived 3 GHz counts based on single-pointing (0.087 square degrees) VLA data. In summary, the VLA-COSMOS 3 GHz Large Project simultaneously provides the largest and deepest radio continuum survey at high (0.75 ) angular resolution to date, bridging the gap between last-generation and next-generation surveys.

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The Dust-Unbiased Cosmic Star-Formation History From the 20 Cm Vla-Cosmos Survey

Cited by 130 publications

References 53 publications

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

Evolution of the dusty infrared luminosity function fromz = 0toz = 2.3using observations fromSpitzer

The new semi-analytic code GalICS 2.0 – reproducing the galaxy stellar mass function and the Tully–Fisher relation simultaneously

The VLA-COSMOS 3 GHz Large Project: Continuum data and source catalog release

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