Hubble Space TelescopeandSpitzerImaging of Red and Blue Galaxies atz∼ 2.5: A Correlation between Size and Star Formation Activity from Compact Quiescent Galaxies to Extended Star‐forming Galaxies

Toft, Sune; Dokkum, Pieter van; Franx, Marijn; Labbé, Ivo; Schreiber, N. M. Förster; Wuyts, Stijn; Webb, Tracy; Rudnick, G.; Zirm, A.; Kriek, Mariska; Werf, P. van der; Blakeslee, John P.; Illingworth, G. D.; Rix, H. W.; Papovich, Casey; Moorwood, A. F. M.

doi:10.1086/521810

Cited by 229 publications

(223 citation statements)

References 83 publications

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“…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%

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

103

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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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

103

100

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“…Daddi et al 2005;Trujillo et al 2006Trujillo et al , 2007Longhetti et al 2007;Zirm et al 2007;Toft et al 2007;Franx et al 2008;Cimatti et al 2008;Buitrago et al 2008;van der Wel et al 2008van der Wel et al , 2014Bernardi 2009;Damjanov et al 2009;Bezanson et al 2009;Mancini et al 2009Mancini et al , 2010Cassata et al 2011;Damjanov et al 2011;Bruce et al 2012;Szomoru et al 2012;Newman et al 2012;Cassata et al 2013;Belli et al 2014). For example, van der Wel et al (2014) find that the mean effective radius R e of passive galaxies selected with a colour−colour criterion increases as R e ∝ (1 + z) −1.48 over the redshift range 0 < z < 3.…”

Section: Introductionmentioning

confidence: 99%

Ultramassive dense early-type galaxies: Velocity dispersions and number density evolution sincez= 1.6

Gargiulo

Saracco

Tamburri

et al. 2016

A&A

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Aims. We investigate the stellar mass assembly history of ultramassive (M 10 11 M ) dense (Σ = M /2πR 2 e > 2500 M pc −2 ) early-type galaxies (ETGs, elliptical and spheroidal galaxies) selected on basis of visual classification over the last 9 Gyr. Methods. We traced the evolution of the comoving number density ρ of ultramassive dense ETGs and compared their structural (effective radius R e and stellar mass M ) and dynamical (velocity dispersion σ e ) parameters over the redshift range 0 < z < 1.6. We derived the number density ρ at 1.6 < z < 1 from the MUNICS and GOODS-South surveys, while we took advantage of the COSMOS spectroscopic survey to probe the intermediate redshift range [0.2−1.0]. We derived the number density of ultramassive dense local ETGs from the SDSS sample taking all of the selection bias affecting the spectroscopic sample into account. To compare the dynamical and structural parameters, we collected a sample of 11 ultramassive dense ETGs at 1.2 < z < 1.6 for which velocity dispersion measurements are available. For four of these ETGs (plus one at z = 1.91), we present previously unpublished estimates of velocity dispersion, based on optical VLT-FORS2 spectra. We probe the intermediate redshift range (0.2 < ∼ z < ∼ 0.9) and the local Universe with different ETGs samples. Results. We find that the comoving number density of ultramassive dense ETGs evolves with z as ρ(z) ∝ (1 + z) 0.3 ± 0.8 implying a decrease of ∼25% of the population of ultramassive dense ETGs since z = 1.6. By comparing the structural and dynamical properties of high-z ultramassive dense ETGs over the range 0 < ∼ z < 1.6 in the [R e , M , σ e ] plane, we find that all of the ETGs of the high-z sample have counterparts with similar properties in the local Universe. This implies either that the majority (∼70%) of ultramassive dense ETGs already completed the assembly and shaping at z = 1.4, or that, if a significant portion of dense ETGs evolves in size, new ultramassive dense ETGs must form at z < 1.5 to maintain their number density at almost constant. The difficulty in identify good progenitors for these new dense ETGs at z < ∼ 1.5 and the stellar populations properties of local ultramassive dense ETGs point towards the first hypothesis. In this case, the ultramassive dense galaxies missing in the local Universe could have joined, in the last 9 Gyr, the so colled non-dense ETGs population through minor mergers, thus contributing to mean size growth. In any case, the comparison between their number density and the number density of the whole population of ultramassive ETGs relegates their contribution to the mean size evolution to a secondary process.

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“…The size evolution appears to be quite dramatic; Toft et al (2007) find that, on average, the quiescent galaxies in their sample z ∼ 2.5 have a factor of 30-40 higher surface density than do red galaxies of the same mass in the Sloan Digital Sky Survey (SDSS).…”

mentioning

confidence: 97%

“…Several recent studies have found evidence that massive galaxies at high redshift are indeed quite compact, particularly those with the lowest estimated star formation rates (Daddi et al 2005;Trujillo et al 2006Trujillo et al , 2007Zirm et al 2007;Toft et al 2007;Longhetti et al 2007;Cimatti et al 2008). The size evolution appears to be quite dramatic; Toft et al (2007) find that, on average, the quiescent galaxies in their sample z ∼ 2.5 have a factor of 30-40 higher surface density than do red galaxies of the same mass in the Sloan Digital Sky Survey (SDSS).…”

mentioning

confidence: 99%

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

Dokkum¹,

Franx²,

Kriek³

et al. 2008

ApJ

674

397

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Using deep near-infrared spectroscopy, Kriek et al. found that ∼45% of massive galaxies at have evolved z ∼ 2.3 stellar populations and little or no ongoing star formation. Here we determine the sizes of these quiescent galaxies using deep, high-resolution images obtained with HST/NIC2 and laser guide star (LGS)-assisted Keck/adaptive optics (AO). Considering that their median stellar mass is , the galaxies are remarkably small, with 11 1.7 # 10 M , a median effective radius kpc. Galaxies of similar mass in the nearby universe have sizes of ≈5 kpc and r p 0.9 e average stellar densities that are 2 orders of magnitude lower than the galaxies. These results extend earlier z ∼ 2.3 work at and confirm previous studies at that lacked spectroscopic redshifts and imaging of sufficient z ∼ 1.5 z 1 2 resolution to resolve the galaxies. Our findings demonstrate that fully assembled early-type galaxies make up at most ∼10% of the population of K-selected quiescent galaxies at , effectively ruling out simple monolithic z ∼ 2.3 models for their formation. The galaxies must evolve significantly after , through dry mergers or other z ∼ 2.3 processes, consistent with predictions from hierarchical models.

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Hubble Space TelescopeandSpitzerImaging of Red and Blue Galaxies atz∼ 2.5: A Correlation between Size and Star Formation Activity from Compact Quiescent Galaxies to Extended Star‐forming Galaxies

Cited by 229 publications

References 83 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

Ultramassive dense early-type galaxies: Velocity dispersions and number density evolution sincez= 1.6

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

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