The Hubble Space Telescope GOODS NICMOS Survey: overview and the evolution of massive galaxies at 1.5&lt; z&lt; 3

Conselice, Christopher J.; Bluck, Asa F. L.; Buitrago, F.; Bauer, A.; Grützbauch, Ruth; Bouwens, Rychard; Bevan, S.; Mortlock, Alice; Dickinson, Mark; Daddi, E.; Yan, Haojing; Scott, D.; Chapman, Scott; Chary, R.-R.; Ferguson, Henry C.; Giavalisco, Mauro; Grogin, Norman A.; Illingworth, G. D.; Jogee, Shardha; Koekemoer, Anton M.; Lucas, Ray A.; Mobasher, Bahram; Moustakas, Leonidas A.; Papovich, Casey; Ravindranath, Swara; Siana, Brian; Teplitz, Harry I.; Trujillo, Ignacio; Urry, C. Megan; Weinzirl, Tim

doi:10.1111/j.1365-2966.2010.18113.x

Cited by 86 publications

(80 citation statements)

References 80 publications

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“…These massive galaxies are in the redshift range z = 1.7-2.9 and at a depth of three orbits. The galaxies are redshift selected based on their optical to infrared colour described in Conselice et al (2011). Details on the data reduction pipeline are described in Magee, Bouwens & Illingworth (2007).…”

Section: The Goods Nicmos Surveymentioning

confidence: 99%

A deep probe of the galaxy stellar mass functions at z∼ 1-3 with the GOODS NICMOS Survey

Mortlock

Conselice

Bluck

et al. 2011

Monthly Notices of the Royal Astronomical Society

106

149

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We use a sample of 8298 galaxies observed as part of the Hubble Space Telescope (HST) H160‐band GOODS NICMOS Survey (GNS) to construct the galaxy stellar mass function both as a function of redshift and as stellar mass up to z= 3.5. Our mass functions are constructed within the redshift range z= 1–3.5 and consist of galaxies with stellar masses of M*= 1012 M⊙ down to nearly dwarf galaxy masses of M*= 108.5 M⊙ in the lowest redshift bin. We discover that a significant fraction of all massive M* > 1011 M⊙ galaxies are in place up to the highest redshifts we probe, with a decreasing fraction of lower mass galaxies present at all redshifts. This is an example of ‘galaxy mass downsizing’, and is the result of massive galaxies forming before lower mass ones, and not just simply ending their star formation earlier as in traditional downsizing scenarios, whose effect is seen at z < 1.5. By fitting Schechter functions to our mass functions we find that the faint‐end slope ranges from α=−1.36 to −1.73, which is significantly steeper than what is found in previous investigations of the mass function at high redshift. We demonstrate that this steeper mass function better matches the stellar mass added due to star formation, thereby alleviating some of the mismatch between these two measures of the evolution of galaxy mass. We furthermore examine the stellar mass function divided into blue/red systems, as well as for star‐forming and non‐star‐forming galaxies. We find a similar mass downsizing present for both blue/red and star‐forming/non‐star forming galaxies, and further find that red galaxies dominate at the high‐mass end of the mass function, but that the low‐mass galaxies are mostly all blue, and therefore blue galaxies are creating the steep mass functions observed at z > 2. We furthermore show that, although there is a downsizing such that high‐mass galaxies are nearer their z= 0 values at high redshift, this turns over at masses M*∼ 1010 M⊙, such that the lowest mass galaxies are more common than galaxies at slight higher masses, creating a ‘dip’ in the observed galaxy mass function. We argue that the galaxy assembly process may be driven by different mechanisms at low and high masses, and that the efficiency of the galaxy formation process is lowest at masses M*∼ 1010 M⊙ at 1 < z < 3. Finally, we calculate the integrated stellar mass density for the total, blue and red populations. We find the integrated stellar mass density of the total and blue galaxy population is consistent with being constant over z= 1–2, while the red population shows an increase in integrated stellar mass density over the same redshift range.

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Section: The Goods Nicmos Surveymentioning

confidence: 99%

A deep probe of the galaxy stellar mass functions at z∼ 1-3 with the GOODS NICMOS Survey

Mortlock

Conselice

Bluck

et al. 2011

Monthly Notices of the Royal Astronomical Society

106

149

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“…The epoch between z ∼ 3 and z ∼ 1 appears to be crucial for the assembly of massive galaxies, as many authors find that the number density of galaxies with masses around 10 11 M and larger evolves very rapidly over this period of time (Fontana et al 2006;Marchesini et al 2009;Ilbert et al 2010;Conselice et al 2011). By redshift z ∼ 1, however, the number density of early-types is comparable to the local one, with an increase of a factor of 1.5 allowed at most (Cimatti et al 2006;Franceschini et al 2006;Borch et al 2006).…”

Section: Introductionmentioning

confidence: 97%

THE RELATIVE ABUNDANCE OF COMPACT AND NORMAL MASSIVE EARLY-TYPE GALAXIES AND ITS EVOLUTION FROM REDSHIFTz∼ 2 TO THE PRESENT

Cassata

Giavalisco

Guo

et al. 2011

ApJ

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137

210

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We report on the evolution of the number density and size of early-type galaxies (ETGs) from z ∼ 2 to z ∼ 0. We select a sample of 563 massive (M > 10 10 M ), passively evolving (specific star formation rate <10 −2 Gyr −1 ), and morphologically spheroidal galaxies at 0 < z < 2.5, using the panchromatic photometry and spectroscopic redshifts available in the Great Observatories Origins Deep Surveys fields. We combine Advanced Camera for Surveys and Wide Field Camera 3 Hubble Space Telescope images to study the morphology of our galaxies in their optical rest frame in the entire 0 < z < 2.5 range. We find that throughout the explored redshift range the passive galaxies selected with our criteria have weak morphological K-correction, with size being slightly smaller in the optical than in the UV rest frame (by ∼20% and ∼10% at z > 1.2 and z < 1.2, respectively). We measure a significant evolution of the mass-size relation of ETGs, with a fractional increment that is almost independent of the stellar mass. ETGs formed at z > 1 appear to be preferentially small, and the evolution of the mass-size relation at z < 1 is driven by both the continuous size growth of the compact galaxies and the appearance of new ETGs with large sizes. We also find that the number density of all passive ETGs increases rapidly, by a factor of five, from z ∼ 2 to z ∼ 1, and then more mildly by another factor of 1.5 from z ∼ 1 to z ∼ 0. We interpret these results as evidence that the bulk of the ETGs are formed at 1 < z < 3 through a mechanism that leaves very compact remnants. At z < 1 the compact ETGs grow gradually in size, becoming normal-size galaxies, and at the same time new ETGs with normal-large sizes are formed.

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“…Observational data have shown that galaxies in the local universe generally fall into two categories: quiescent ellipticals, which dominate the massive galaxy population (M * 10 10.5 M ), and blue star-forming disk galaxies, which occupy the lower mass regime Balogh et al 2004;Kauffmann et al 2003). This color bimodality, which groups galaxies into the "blue cloud" and "red sequence," exists not only in the local universe, but also out to redshift z ∼ 1 (Bell et al 2004;Willmer et al 2006), and possibly up to z = 2 and beyond (Pozzetti et al 2010;Conselice et al 2011). The origin and the evolution of this color bimodality are largely unknown.…”

Section: Introductionmentioning

confidence: 99%

A Close-Pair Analysis of Damp Mergers at Intermediate Redshifts

Chou

Bridge

Abraham

2012

ApJ

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We have studied the kinematics of ∼2800 candidate close-pair galaxies at 0.1 < z < 1.2 identified from the Canada-France-Hawaii Telescope Legacy Survey fields. Spectra of these systems were obtained using spectrometers on the 6.5 m Magellan and 5 m Hale telescopes. These data allow us to constrain the rate of dry mergers at intermediate redshifts and to test the "hot halo" model for quenching of star formation. Using virial radii estimated from the correlation between dynamical and stellar masses published by Leauthaud et al., we find that around 1/5 of our candidate pairs are likely to share a common dark matter halo (our metric for close physical association). These pairs are divided into red-red, blue-red, and blue-blue systems using the rest-frame colors classification method introduced in Chou et al.. Galaxies classified as red in our sample have very low star formation rates, but they need not be totally quiescent, and hence we refer to them as "damp," rather than "dry," systems. After correcting for known selection effects, the fraction of blue-blue pairs is significantly greater than that of red-red and blue-red pairs. Red-red pairs are almost entirely absent from our sample, suggesting that damp mergers are rare at z ∼ 0.5. Our data support models with a short merging timescale (<0.5 Gyr) in which star formation is enhanced in the early phase of mergers, but quenched in the late phase. Hot halo models may explain this behavior, but only if virial shocks that heat gas are inefficient until major mergers are nearly complete.

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The Hubble Space Telescope GOODS NICMOS Survey: overview and the evolution of massive galaxies at 1.5< z< 3

Cited by 86 publications

References 80 publications

A deep probe of the galaxy stellar mass functions at z∼ 1-3 with the GOODS NICMOS Survey

A deep probe of the galaxy stellar mass functions at z∼ 1-3 with the GOODS NICMOS Survey

THE RELATIVE ABUNDANCE OF COMPACT AND NORMAL MASSIVE EARLY-TYPE GALAXIES AND ITS EVOLUTION FROM REDSHIFTz∼ 2 TO THE PRESENT

A Close-Pair Analysis of Damp Mergers at Intermediate Redshifts

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