The Munich Near‐Infrared Cluster Survey (MUNICS). VI. The Stellar Masses of<i>K</i>‐Band–selected Field Galaxies to<i>z</i> ∼ 1.2

Drory, Niv; Bender, Ralf; Feulner, Georg; Hopp, U.; Maraston, Claudia; Snigula, J.; Hill, Gary J.

doi:10.1086/420781

Cited by 201 publications

(304 citation statements)

References 54 publications

Supporting

Mentioning

275

Contrasting

Order By: Relevance

“…2) are typical for massive galaxies. Specifically, the median (0.68 M L −1 ) is similar to the values for M * > 10 11 M galaxies (Drory et al 2004, their Table 1) and to simulated massive galaxies at z ∼ 1 (Courty et al 2007, their Fig. 4).…”

Section: Stellar Massessupporting

confidence: 79%

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Michalowski

Hjorth

Watson

2010

A&A

234

278

View full text Add to dashboard Cite

The nature of galaxies selected at submillimeter wavelengths (SMGs, S 850 3 mJy), some of the bolometrically most luminous objects at high redshifts, is still elusive. In particular their star formation histories and source of emission are not accurately constrained. In this paper we introduce a new approach to analyse the SMG data. Namely, we present the first self-consistent UV-to-radio spectral energy distribution fits of 76 SMGs with spectroscopic redshifts using all photometric datapoints from ultraviolet to radio simultaneously. We find that they are highly star-forming (median star formation rate 713 M yr −1 for SMGs at z > 0.5), moderately dust-obscured (median A V ∼ 2 mag), hosting significant stellar populations (median stellar mass 3.7 × 10 11 M ) of which only a minor part has been formed in the ongoing starburst episode. This implies that in the past, SMGs experienced either another starburst episode or merger with several galaxies. The properties of SMGs suggest that they are progenitors of present-day elliptical galaxies. We find that these bright SMGs contribute significantly to the cosmic star formation rate density (∼20%) and stellar mass density (∼30-50%) at redshifts 2-4. Using number counts at low fluxes we find that as much as 80% of the cosmic star formation at these redshifts took place in SMGs brighter than 0.1 mJy. We find evidence that a linear infrared-radio correlation holds for SMGs in an unchanged form up to redshift of 3.6, though its normalization is offset from the local relation by a factor of ∼2.1 towards higher radio luminosities. We present a compilation of photometry data of SMGs and determinations of cosmic SFR and stellar mass densities.

show abstract

Section: Stellar Massessupporting

confidence: 79%

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Michalowski

Hjorth

Watson

2010

A&A

234

278

View full text Add to dashboard Cite

show abstract

“…As several other authors (Fontana et al 2004;Drory et al 2004;Labbé et al 2005) have noted, IR-selected samples are not equivalent to mass-selected samples. At any redshift, galaxies detected above the sample magnitude limit can have a fairly wide range of M /L ratios, depending on their spectral properties, ages, dust extinction, and metallicities.…”

Section: Incompleteness Effects and Mass Selection Criteriamentioning

confidence: 88%

“…Second, the 4.5 μm band selection allows us to construct a more complete sample in terms of stellar mass than an optical or near-IR selection. This is an important difference from previous work: we attempted to construct a sample that was as complete as possible, including objects undetected in optical and near-IR bands, and hence missed by the optical or K-band selection criteria used so far in the literature (Drory et al 2004;Fontana et al 2006;Dunlop et al 2007;Wiklind et al 2008;Brammer & van Dokkum 2007). As already mentioned, Rodighiero et al (2007) also used an IRAC band (3.6 μm) selection, but their additional conditions about the lack of optical emission and the faint near-IR detection (K > 23, AB system) ensured that their sample was incomplete by construction.…”

Section: Introductionmentioning

confidence: 99%

Searching for massive galaxies at z ≥ 3.5 in GOODS-North

Mancini

Matute

Cimatti

et al. 2009

A&A

View full text Add to dashboard Cite

Aims. We constrain the space density and properties of massive galaxy candidates at redshifts of z ≥ 3.5 in the Great Observatories Origin Deep Survey North (GOODS-N) field. By selecting sources in the Spitzer + IRAC bands, a sample highly complete in stellarmass is assembled, including massive galaxies that are very faint in the optical/near-IR bands and would be missed by samples selected at shorter wavelengths. Methods. The z ≥ 3.5 sample was selected to m AB = 23 mag at 4.5 μm using photometric redshifts obtained by fitting the galaxies spectral energy distribution at optical, near-IR bands, and IRAC bands. We also require that the brightest band (in AB scale) in which candidates are detected is the IRAC 8.0 μm band to ensure that the near-IR 1.6 μm (rest-frame) peak is falling in or beyond this band. Results. We found 53 z ≥ 3.5 candidates, of masses in the range M ∼ 10 10 −10 11 M . At least ∼81% of these galaxies are missed by traditional Lyman Break selection methods based on ultraviolet light. Spitzer + MIPS emission is detected for 60% of the sample of z ≥ 3.5 galaxy candidates. Although in some cases this might suggest a residual contamination from lower redshift starforming galaxies or Active Galactic Nuclei, 37% of these objects are also detected in the sub-mm/mm bands in SCUBA, AzTEC, and MAMBO surveys, and have properties fully consistent with vigorous starburst galaxies at z ≥ 3.5. The comoving number density of galaxies with stellar masses of above 5 × 10 10 M (a reasonable stellar-mass completeness limit for our sample) is 2.6 × 10 −5 Mpc −3 (using the volume within 3.5 < z < 5), and the corresponding stellar mass density is ∼(2.9 ± 1.5) × 10 6 M Mpc −3 , or about 3% of the local density above the same stellar mass limit. For the subsample of MIPS-undetected galaxies, we measure a number density of ∼0.97 × 10 −5 Mpc −3 and a stellar mass density of ∼(1.15 ± 0.7) × 10 6 M Mpc −3 . Even in the unlikely case that these are all truly quiescent galaxies, this would imply an increase in the space density of passive galaxies by a factor of ∼15 between z ∼ 4 and z = 2, and by ∼100 to z = 0.

show abstract

“…Dickinson et al 2003;Drory et al 2004;Ilbert et al 2013;Muzzin et al 2013;Tomczak et al 2014). More precisely, to derive the stellar mass of each galaxy, we have fitted the observed SED after fixing the redshift to the high-quality spectroscopic value, or to the photometric one when the former is not available or is not robust.…”

Section: Stellar Massesmentioning

confidence: 99%

The galaxy stellar mass function at 3.5 ≤z≤ 7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields

Grazian

Fontana

Santini

et al. 2015

A&A

264

212

View full text Add to dashboard Cite

Context. The form and evolution of the galaxy stellar mass function (GSMF) at high redshifts provide crucial information on star formation history and mass assembly in the young Universe, close or even prior to the epoch of reionization. Aims. We used the unique combination of deep optical/near-infrared/mid-infrared imaging provided by HST, Spitzer, and the VLT in the CANDELS-UDS, GOODS-South, and HUDF fields to determine the GSMF over the redshift range 3.5 ≤ z ≤ 7.5. Methods. We used the HST WFC3/IR near-infrared imaging from CANDELS and HUDF09, reaching H 27−28.5 over a total area of 369 arcmin 2 , in combination with associated deep HST ACS optical data, deep Spitzer IRAC imaging from the SEDS programme, and deep Y and K-band VLT Hawk-I images from the HUGS programme, to select a galaxy sample with high-quality photometric redshifts. These have been calibrated with more than 150 spectroscopic redshifts in the range 3.5 ≤ z ≤ 7.5, resulting in an overall precision of σ z /(1 + z) ∼ 0.037. With this database we have determined the low-mass end of the high-redshift GSMF with unprecedented precision, reaching down to masses as low as M * ∼ 10 9 M at z = 4 and ∼6 × 10 9 M at z = 7. Results. We find that the GSMF at 3.5 ≤ z ≤ 7.5 depends only slightly on the recipes adopted to measure the stellar masses, namely the photometric redshifts, the star formation histories, the nebular contribution, or the presence of AGN in the parent sample. The low-mass end of the GSMF is steeper than has been found at lower redshifts, but appears to be unchanged over the redshift range probed here. Meanwhile the high-mass end of the GSMF appears to evolve primarily in density, although there is also some evidence of evolution in characteristic mass. Our results are very different from previous mass function estimates based on converting UV galaxy luminosity functions into mass functions via tight mass-to-light relations. Integrating our evolving GSMF over mass, we find that the growth of stellar mass density is barely consistent with the time-integral of the star formation rate density over cosmic time at z > 4. Conclusions. These results confirm the unique synergy of the CANDELS+HUDF, HUGS, and SEDS surveys for the discovery and study of moderate/low-mass galaxies at high redshifts, and reaffirm the importance of space-based infrared selection for the unbiased measurement of the evolving GSMF in the young Universe.

show abstract

The Munich Near‐Infrared Cluster Survey (MUNICS). VI. The Stellar Masses ofK‐Band–selected Field Galaxies toz ∼ 1.2

Cited by 201 publications

References 54 publications

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Cosmic evolution of submillimeter galaxies and their contribution to stellar mass assembly

Searching for massive galaxies at z ≥ 3.5 in GOODS-North

The galaxy stellar mass function at 3.5 ≤z≤ 7.5 in the CANDELS/UDS, GOODS-South, and HUDF fields

Contact Info

Product

Resources

About