Confirmation of the Remarkable Compactness of Massive Quiescent Galaxies at
                    <i>z</i>
                    ~ 2.3: Early-Type Galaxies Did not Form in a Simple Monolithic Collapse

Dokkum, Pieter van; Franx, Marijn; Kriek, Mariska; Holden, B.; Illingworth, G. D.; Magee, D.; Bouwens, Rychard; Marchesini, Danilo; Quadri, Ryan; Rudnick, G.; Taylor, Edward N.; Toft, Sune

doi:10.1086/587874

Cited by 667 publications

(435 citation statements)

References 29 publications

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“…This large scatter is consistent with the large range of sersic index observed by van Dokkum et al (2011) in a sample of massive galaxies at z = 1 − 1.5. Szomoru et al 2012).…”

Section: Classical Spheroids and Exponential Discssupporting

confidence: 88%

“…High-redshift spheroids are much more compact than galaxies of similar mass at z=0 (Daddi et al 2005;Trujillo et al 2006;Toft et al 2007;van Dokkum et al 2008;Cimatti et al 2008). These galaxies with stellar masses of ∼10 11 M ⊙ at z = 1.5 − 2 have typical effective radii of ∼2 kpc, a factor ∼3 smaller than present-day spheroids and a factor ∼2 lower than extended discs with similar mass at the same redshift (Patel et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers

Ceverino

Dekel

Tweed

et al. 2015

Monthly Notices of the Royal Astronomical Society

101

100

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We address the formation of massive stellar spheroids between redshifts z = 4 and 1 using a suite of AMR hydro-cosmological simulations. The spheroids form as bulges, and the spheroid mass growth is partly driven by violent disc instability (VDI) and partly by mergers. A kinematic decomposition to disc and spheroid yields that the mass fraction in the spheroid is between 50% and 90% and is roughly constant in time, consistent with a cosmological steady state of VDI discs that are continuously fed from the cosmic web. The density profile of the spheroid is typically "classical", with a Sersic index n = 4.5 ± 1, independent of whether it grew by mergers or VDI and independent of the feedback strength. The disc is characterized by n = 1.5±0.5, and the whole galaxy by n = 3±1. The high-redshift spheroids are compact due to the dissipative inflow of gas and the high universal density. The stellar surface density within the effective radius of each galaxy as it evolves remains roughly constant in time after its first growth. For galaxies of a fixed stellar mass, the surface density is higher at higher redshifts.

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“…This large scatter is consistent with the large range of sersic index observed by van Dokkum et al (2011) in a sample of massive galaxies at z = 1 − 1.5. Szomoru et al 2012).…”

Section: Classical Spheroids and Exponential Discssupporting

confidence: 88%

Section: Introductionmentioning

confidence: 99%

Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers

Ceverino

Dekel

Tweed

et al. 2015

Monthly Notices of the Royal Astronomical Society

101

100

View full text Add to dashboard Cite

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“…Although this conclusion is drawn from limited numbers, the low fraction of sources with Hα emission lines in our sample suggests that most of the sources probably don't have much ongoing star formation (SFR < 0.5 M yr −1 ) and so their formation epoch might be quite high. This would be contrary to the idea of the giant elliptical assembly epoch being z ∼ 2−3 (e.g., van Dokkum et al 2008;Kriek et al 2008), but is consistent with results from SED age fitting of stellar populations, which point to z form > 3 (e.g., Eisenhardt et al 2008). The discrepancy may be resolved if subclumps form early and merge without inducing much star formation (i.e.…”

Section: Discussionsupporting

confidence: 71%

Optical and near-IR spectroscopy of candidate red galaxies in two z ~ 2.5 proto-clusters

Doherty¹,

Tanaka

Breuck

et al. 2010

A&A

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We present a spectroscopic campaign to follow-up red colour-selected candidate massive galaxies in two high redshift proto-clusters surrounding radio galaxies. We observed a total of 57 galaxies in the field of MRC 0943−242 (z = 2.93) and 33 in the field of MRC 1138−262 (z = 2.16) with a mix of optical and near-infrared multi-object spectroscopy. We confirm two red galaxies in the field of MRC 1138−262 at the redshift of the radio galaxy. Based on an analysis of their spectral energy distributions, and their derived star formation rates from the Hα and observed frame 24 μm flux, one object belongs to the class of dust-obscured star-forming red galaxies, while the other is evolved with little ongoing star formation. This result represents the first red and mainly passively evolving galaxy to be confirmed as companion galaxies in a z > 2 proto-cluster. Both red galaxies in MRC 1138−262 are massive, of the order of 4−6 × 10 11 M . They lie along a colour−magnitude relation which implies that they formed the bulk of their stellar population around z = 4. In the MRC 0943−242 field we find no red galaxies at the redshift of the radio galaxy but we do confirm the effectiveness of our JHK s selection of galaxies at 2.3 < z < 3.1, finding that 10 out of 18 (56%) of JHK s -selected galaxies whose redshifts could be measured fall within this redshift range. We also serendipitously identify an interesting foreground structure of 6 galaxies at z = 2.6 in the field of MRC 0943−242. This may be a proto-cluster itself, but complicates any interpretation of the red sequence build-up in MRC 0943−242 until more redshifts can be measured.

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“…Such evolution has been observed for some time (Bell et al 2004;Brown et al 2007) in surveys of massive field galaxies. Additional significant growth of the massive red galaxy population occurs at z > 1 van Dokkum et al 2008;Taylor et al 2009;Whitaker et al 2010), and this may likely be true in all environments. We therefore consider the possibility that our cluster sample selects, at least in part, a continuous evolutionary sequence that experiences star formation over an extended period leading to an increase in stellar mass on the red sequence.…”

Section: Red Sequence Growthmentioning

confidence: 97%

Assembly of the Red Sequence in Infrared-Selected Galaxy Clusters From the Irac Shallow Cluster Survey

Snyder

Brodwin

Mancone

et al. 2012

ApJ

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We present results for the assembly and star formation histories (SFHs) of massive (∼L * ) red sequence galaxies (RSGs) in 11 spectroscopically confirmed, infrared-selected galaxy clusters at 1.0 < z < 1.5, the precursors to present-day massive clusters with M ∼ 10 15 M . Using rest-frame optical photometry, we investigate evolution in the color and scatter of the RSG population, comparing with models of possible SFHs. In contrast to studies of central cluster galaxies at lower redshift (z < 1), these data are clearly inconsistent with the continued evolution of stars formed and assembled primarily at a single, much earlier time. Specifically, we find that the colors of massive cluster galaxies at z ≈ 1.5 imply that the bulk of star formation occurred at z ∼ 3, whereas by z ≈ 1 their colors imply formation at z ∼ 2; therefore these galaxies exhibit approximately the same luminosity-weighted stellar age at 1 < z < 1.5. This likely reflects star formation that occurs over an extended period, the effects of significant progenitor bias, or both. Our results generally indicate that massive cluster galaxy populations began forming a significant mass of stars at z 4, contained some red spheroids by z ≈ 1.5, and were actively assembling much of their final mass during 1 < z < 2 in the form of younger stars. Qualitatively, the slopes of the cluster color-magnitude relations are consistent with no significant evolution relative to local clusters.

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Confirmation of the Remarkable Compactness of Massive Quiescent Galaxies at z ~ 2.3: Early-Type Galaxies Did not Form in a Simple Monolithic Collapse

Cited by 667 publications

References 29 publications

Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers

Early formation of massive, compact, spheroidal galaxies with classical profiles by violent disc instability or mergers

Optical and near-IR spectroscopy of candidate red galaxies in two z ~ 2.5 proto-clusters

Assembly of the Red Sequence in Infrared-Selected Galaxy Clusters From the Irac Shallow Cluster Survey

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