Encoding of the infrared excess in the<i>NUVrK</i>color diagram for star-forming galaxies

Arnouts, S.; Floc’h, E. Le; Chevallard, Jacopo; Johnson, Benjamin D.; Ilbert, O.; Treyer, Marie; Aussel, H.; Capak, P.; Sanders, D. B.; Scoville, N. Z.; McCracken, H. J.; Milliard, B.; Pozzetti, L.; Salvato, M.

doi:10.1051/0004-6361/201321768

Cited by 186 publications

(275 citation statements)

References 92 publications

(151 reference statements)

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“…The importance of the assumed extinction laws for the physical parameter estimation has been stressed in several recent studies, for example, by Ilbert et al (2010) and Mitchell et al (2013) for the stellar masses, or by Arnouts et al (2013) for the star formation rate (SFR). We considered three laws and a maximum dust reddening of E(B − V) ≤ 0.5: the Prevot et al (1984), the Calzetti et al (2000), and an intermediate-extinction curve (see Arnouts et al 2013, for more details).…”

Section: Methodsmentioning

confidence: 99%

The VIPERS Multi-Lambda Survey

Moutard

Arnouts

Ilbert

et al. 2016

A&A

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171

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We investigate the evolution of the galaxy stellar mass function and stellar mass density from redshift z = 0.2 to z = 1.5 of a K s < 22-selected sample with highly reliable photometric redshifts and over an unprecedentedly large area. Our study is based on near-infrared observations carried out with the WIRCam instrument at CFHT over the footprint of the VIPERS spectroscopic survey and benefits from the high-quality optical photometry from the CFHTLS and ultraviolet observations with the GALEX satellite. The accuracy of our photometric redshifts is σ ∆z/(1+z) < 0.03 and 0.05 for the bright (i AB < 22.5) and faint (i AB > 22.5) samples, respectively. The galaxy stellar mass function is measured with ∼760 000 galaxies down to K s ∼ 22 and over an effective area of ∼22.4 deg 2 , the latter of which drastically reduces the statistical uncertainties (i.e. Poissonian error and cosmic variance). We point out the importance of carefully controlling the photometric calibration, whose effect becomes quickly dominant when statistical uncertainties are reduced, which will be a major issue for future cosmological surveys with EUCLID or LSST, for instance. By exploring the rest-frame (NUV−r) vs. (r − K s ) colour-colour diagram with which we separated star-forming and quiescent galaxies, (1) we find that the density of very massive log(M * /M ) > 11.5 galaxies is largely dominated by quiescent galaxies and increases by a factor 2 from z ∼ 1 to z ∼ 0.2, which allows for additional mass assembly through dry mergers. (2) We also confirm the scenario in which star formation activity is impeded above a stellar mass log(M sf /M ) = 10.64 ± 0.01. This value is found to be very stable at 0.2 < z < 1.5. (3) We discuss the existence of a main quenching channel that is followed by massive star-forming galaxies, and we finally (4) characterise another quenching mechanism that is required to explain the clear excess of low-mass quiescent galaxies that is observed at low redshift.

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Section: Methodsmentioning

confidence: 99%

The VIPERS Multi-Lambda Survey

Moutard

Arnouts

Ilbert

et al. 2016

A&A

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171

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“…Stellar masses are computed with the initial mass function (IMF) of Chabrier (2003) truncated at 0.1 and 100 M , and the stellar population synthesis templates from Bruzual & Charlot (2003). For the details of the procedure we refer the reader to Arnouts et al (2013).…”

Section: Stellar Fractionmentioning

confidence: 99%

The XXL Survey

Eckert

Ettori

Coupon

et al. 2016

A&A

116

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Traditionally, galaxy clusters have been expected to retain all the material accreted since their formation epoch. For this reason, their matter content should be representative of the Universe as a whole, and thus their baryon fraction should be close to the Universal baryon fraction Ω b /Ω m . We make use of the sample of the 100 brightest galaxy clusters discovered in the XXL Survey to investigate the fraction of baryons in the form of hot gas and stars in the cluster population. Since it spans a wide range of mass (10 13 −10 15 M ) and redshift (0.05−1.1) and benefits from a large set of multiwavelength data, the XXL-100-GC sample is ideal for measuring the global baryon budget of massive halos. We measure the gas masses of the detected halos and use a mass-temperature relation directly calibrated using weak-lensing measurements for a subset of XXL clusters to estimate the halo mass. We find that the weak-lensing calibrated gas fraction of XXL-100-GC clusters is substantially lower than was found in previous studies using hydrostatic masses. Our best-fit relation between gas fraction and mass reads f gas,500 = 0.055 +0.007 −0.006 M 500 /10 14 M 0.21 +0.11 −0.10 . The baryon budget of galaxy clusters therefore falls short of the Universal baryon fraction by about a factor of two at r 500,MT . Our measurements require a hydrostatic bias 1 − b = M X /M WL = 0.72 +0.08 −0.07 to match the gas fraction obtained using lensing and hydrostatic equilibrium, which holds independently of the instrument considered. Comparing our gas fraction measurements with the expectations from numerical simulations, we find that our results favour an extreme feedback scheme in which a significant fraction of the baryons are expelled from the cores of halos. This model is, however, in contrast with the thermodynamical properties of observed halos, which might suggest that weak-lensing masses are overestimated. In light of these results, we note that a mass bias 1 − b = 0.58 as required to reconcile Planck cosmic microwave background and cluster counts should translate into an even lower baryon fraction, which poses a major challenge to our current understanding of galaxy clusters.

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“…Multiple rest-frame color selection techniques have been devised to separate QGs from SFGs, such as U−V versus V−J ("UVJ-selection"; Williams et al 2009), NUV−r versus r−J ("NUVrJ-selection"; Ilbert et al 2013), and NUV−r versus r−K (Arnouts et al 2013). Here, we have adopted the NUVrJ selection technique for the reasons explained in Ilbert et al (2013, Section 3.3), although we note that the stacking results from our selection are comparable to those using the UVJ-selection (see Section 4.7).…”

Section: Data and Sample Selectionmentioning

confidence: 99%

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

Man

Greve

Toft

et al. 2016

ApJ

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We performed a comprehensive stacking analysis on ∼14,200 quiescent galaxy (QG) candidates at z=0-3 across mid-, far-infrared (MIR and FIR), and radio wavelengths. Identified via their rest-frame NUV−r and r−J colors, the QG candidates (M M 10 9.8 12.2 - =  ) have drastically different IR and radio properties depending on their 24 μm emission strength. The fraction of QG candidates with strong 24 μm emission (equivalent to inferred star formation rates SFR M yr 100, hereafter "IR-bright") increases with redshift and peaks at 15%, and their stacked MIPS 24 μm, Herschel (PACS and SPIRE) and VLA emissions are consistent with being starforming galaxies (SFGs). In contrast, the majority of QG candidates are faint or undetected at 24 μm individually (i.e., SFR 24 <100 M e yr −1 , hereafter "IR-faint"). Their low dust-obscured SFRs derived from Herschel stacking (SFR H  3, 15, 50 M e yr −1 out to z∼1, 2, 3) are >2.5-12.5×lower than compared to SFGs. This is consistent with the quiescence, as expected from their low unobscured SFRs, as inferred from modeling their ultraviolet-to-NIR photometry. The discrepancy between the L IR derived from stacking Herschel and 24 μm indicates that IRfaint QGs have dust SEDs that are different from those of SFGs. For the most massive (M M 10 11    ) IR-faint QGs at z<1.5, the stacked 1.4 GHz emission is in excess of that expected from other SFR indicators, suggesting a widespread presence of low-luminosity active galactic nuclei. Our results reaffirm the existence of a significant population of QGs out to z=3, thus corroborating the need to quench star formation in galaxies at early epochs.

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Encoding of the infrared excess in theNUVrKcolor diagram for star-forming galaxies

Cited by 186 publications

References 92 publications

The VIPERS Multi-Lambda Survey

The VIPERS Multi-Lambda Survey

The XXL Survey

CONFIRMING THE EXISTENCE OF A QUIESCENT GALAXY POPULATION OUT TO z = 3: A STACKING ANALYSIS OF MID-, FAR-INFRARED, AND RADIO DATA

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