The evolution of Ks-selected galaxies in the GOODS/CDFS deep ISAAC field

Caputi, K.; Dunlop, James; McLure, R. J.; Roche, N.

doi:10.1111/j.1365-2966.2005.09222.x

Cited by 35 publications

(84 citation statements)

References 44 publications

(85 reference statements)

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“…Table 5 reports the stellar mass densities thus obtained. Figure 20 compares the ρ based on IR-peakers to a collection of data from the literature (Rudnick et al 2006Fontana et al 2006Fontana et al , 2004Fontana et al , 2003Drory et al 2005Drory et al , 2004Franceschini et al 2006;Bundy et al 2005;Gwyn & Hartwick 2005;Caputi et al 2006Caputi et al , 2005Dickinson et al 2003b; While the literature data were obtained by integrating the mass function down to 10 8 M , the IR-peaker data points belong to sources above ∼10 11 M only. The solid thick line simply connects the ρ estimate for galaxies more massive than 10 11 M by Fontana et al (2006).…”

Section: The Integrated Stellar Mass Densitymentioning

confidence: 99%

The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function

Berta

Lonsdale

Polletta

et al. 2007

A&A

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Context. In the last couple of years a population of very massive (M > 10 11 M ), high-redshift (z ≥ 2) galaxies has been identified, but its role in galaxy evolution has not yet been fully understood. Aims. It is necessary to perform a systematic study of high-redshift massive galaxies, in order to determine the shape of the very massive tail of the stellar mass function and determine the epoch of their assembly. Methods. We selected high-z massive galaxies at 5.8 µm, in the SWIRE ELAIS-S1 field (1 deg 2 ). Galaxies with the 1.6 µm stellar peak redshifted into the IRAC bands (z 1−3, called "IR-peakers") were identified. Stellar masses were derived by means of spectrophotometric fitting and used to compute the stellar mass function (MF) at z = 1−2 and 2−3. A parametric fit to the MF was performed, based on a Bayesian formalism, and the stellar mass density of massive galaxies above z = 2 determined. Results. We present the first systematic study of the very-massive tail of the galaxy stellar mass function at high redshift. A total of 326 sources were selected. The majority of these galaxies have stellar masses in excess of 10 11 M and lie at z > 1.5. The availability of mid-IR data turned out to be a valuable tool to constrain the contribution of young stars to galaxy SEDs, and thus their M /L ratio. The influence of near-IR data and of the chosen stellar library on the SED fitting are also discussed. The z = 2−3 stellar mass function between 10 11 and ∼10 12 M is probed with unprecedented detail. A significant evolution is found not only for galaxies with M ∼ 10 11 M , but also in the highest mass bins considered. The comoving number density of these galaxies was lower by more than a factor of 10 at z = 2−3, with respect to the local estimate. SWIRE 5.8 µm peakers more massive than 1.6 × 10 11 M provide 30−50% of the total stellar mass density in galaxies at z = 2−3.

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Section: The Integrated Stellar Mass Densitymentioning

confidence: 99%

The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function

Berta

Lonsdale

Polletta

et al. 2007

A&A

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“…In this framework, massive galaxies (M > 10 10.5 M ) play a special role because they host A&A 549, A63 (2013) place at z ∼ 0.7−1, whereas lower mass galaxies display a much faster increase in their number density from z ∼ 1 to z ∼ 0 (see e.g., Fontana et al 2004;Glazebrook et al 2004;Drory et al 2005;Caputi et al 2005Caputi et al , 2006Bundy et al 2006).…”

Section: Introductionmentioning

confidence: 99%

GMASS ultradeep spectroscopy of galaxies atz ~ 2

Kurk

Cimatti

Daddi

et al. 2012

A&A

111

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Context. Ultra-deep imaging of small parts of the sky has revealed many populations of distant galaxies, providing insight into the early stages of galaxy evolution. Spectroscopic follow-up has mostly targeted galaxies with strong emission lines at z > 2 or concentrated on galaxies at z < 1. Aims. The populations of both quiescent and actively star-forming galaxies at 1 < z < 2 are still under-represented in our general census of galaxies throughout the history of the Universe. In the light of galaxy formation models, however, the evolution of galaxies at these redshifts is of pivotal importance and merits further investigation. In addition, photometry provides only limited clues about the nature and evolutionary status of these galaxies.We therefore designed a spectroscopic observing campaign of a sample of both massive, quiescent and star-forming galaxies at z > 1.4. Methods. To determine redshifts and physical properties, such as metallicity, dust content, dynamical masses, and star formation history, we performed ultra-deep spectroscopy with the red-sensitive optical spectrograph FORS2 at the Very Large Telescope. We first constructed a sample of objects, within the CDFS/GOODS area, detected at 4.5 μm, to be sensitive to stellar mass rather than star formation intensity. The spectroscopic targets were selected with a photometric redshift constraint (z > 1.4) and magnitude constraints (B AB < 26, I AB < 26.5), which should ensure that these are faint, distant, and fairly massive galaxies. Results. We present the sample selection, survey design, observations, data reduction, and spectroscopic redshifts. Up to 30 h of spectroscopy of 174 spectroscopic targets and 70 additional objects enabled us to determine 210 redshifts, of which 145 are at z > 1.4. The redshift distribution is clearly inhomogeneous with several pronounced redshift peaks. From the redshifts and photometry, we deduce that the BzK selection criteria are efficient (82%) and suffer low contamination (11%). Several papers based on the GMASS survey show its value for studies of galaxy formation and evolution. We publicly release the redshifts and reduced spectra. In combination with existing and on-going additional observations in CDFS/GOODS, this data set provides a legacy for future studies of distant galaxies.

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“…In the case of m < 0, the number density is decreasing to higher redshift (hereafter ''negative density evolution''). In the past decade, there have been a number of determinations of the NIR local LF of galaxies based on both photometric (Balogh et al 2001;Kashikawa et al 2003;Caputi et al 2005;Saracco et al 2006) and spectroscopic redshifts (Glazebrook et al 1995;Huang et al 2003;Pozzetti et al 2003). From optical surveys, it has also been shown that each galaxy type has a characteristic LF shape (Folkes et al 1999;Madgwick et al 2002;Nakamura et al 2003;Dahlen et al 2005).…”

Section: Comparison With Early-type Galaxy Count Modelsmentioning

confidence: 99%

Number Density Evolution ofK_s‐Band–Selected High‐Redshift Galaxy Populations in theAKARINorth Ecliptic Pole Field

Imai¹,

Pearson

Matsuhara

et al. 2008

Astrophysical Journal

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We present the number counts of K s -bandYselected high-redshift galaxy populations such as extremely red objects (EROs), B-, z-, and K-bandYselected galaxies ( BzKs) and distant red galaxies ( DRGs) in the AKARI NEP field. These high-redshift galaxy samples are extracted from a multicolor catalog combining optical data from SuprimeCam on the 8.2 m Subaru Telescope with near-infrared data from the Florida Multiobject Imaging Near-IR Grism Observational Spectrometer on the Kitt Peak National Observatory 2.1 m telescope over 540 arcmin 2 in the NEP region field. The final catalog contains 308 EROs (K s < 19:0; 54% are dusty star-forming EROs, and the rest are passive old EROs), 137 star-forming BzKs, and 38 passive old BzKs (K s < 19:0) and 64 DRGs (K s < 18:6). We also produce individual component source counts for both the dusty star-forming and passive populations. We compare the observed number counts of the high redshift passively evolving galaxy population with a backward pure luminosity evolution ( PLE) model allowing different degrees of number density evolution. We find that the PLE model without density evolution fails to explain the observed counts at faint magnitudes, while the model incorporating negative density evolution is consistent with the observed counts of the passively evolving population. We also compare our observed counts of dusty star-forming EROs with a phenomenological evolutionary model postulating that the nearinfrared EROs can be explained by the source densities of the far-infraredYsubmillimeter populations. Our model predicts that the dusty ERO source counts can be explained assuming a 25% contribution of submillimeter starforming galaxies with the majority of brighter K s -bandYdetected dusty EROs having luminous (rather than HR 10 type ultraluminous) submillimeter counterparts. We propose that the fainter K s > 19:5 population is dominated by the submillijansky submillimeter population. We also predict a turnover in dusty ERO counts around 19 < K s < 20.

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The evolution of Ks-selected galaxies in the GOODS/CDFS deep ISAAC field

Cited by 35 publications

References 44 publications

The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function

The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function

GMASS ultradeep spectroscopy of galaxies atz ~ 2

Number Density Evolution ofK_s‐Band–Selected High‐Redshift Galaxy Populations in theAKARINorth Ecliptic Pole Field

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The evolution of Ks-selected galaxies in the GOODS/CDFS deep ISAAC field

Cited by 35 publications

References 44 publications

The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function

The contribution of very massive high-redshift SWIRE galaxies to the stellar mass function

GMASS ultradeep spectroscopy of galaxies atz ~ 2

Number Density Evolution ofKs‐Band–Selected High‐Redshift Galaxy Populations in theAKARINorth Ecliptic Pole Field

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Product

Resources

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Number Density Evolution ofK_s‐Band–Selected High‐Redshift Galaxy Populations in theAKARINorth Ecliptic Pole Field