The Evolution of the Number Density of Compact Galaxies

Poggianti, Bianca M.; Moretti, Alessia; Calvi, Rosa; D’Onofrio, M.; Valentinuzzi, T.; Fritz, J.; Renzini, A.

doi:10.1088/0004-637x/777/2/125

Cited by 92 publications

(117 citation statements)

References 47 publications

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“…We avoid comparing our results with other analyses (e.g. Poggianti et al 2013b) which, although treating the evolution of the number density of compact galaxies, adopt a much lower cut in stellar mass with respect to our cut (e.g. ∼1−5 × 10 10 M ).…”

Section: Local Universementioning

confidence: 95%

“…Valentinuzzi et al 2010;Carollo et al 2013)? A promising approach to shed light on the origin of the size evolution is to investigate how the number density of dense galaxies evolves over the cosmic time (Saracco et al 2010;Bezanson et al 2012;Cassata et al 2013;Poggianti et al 2013b;Carollo et al 2013;Damjanov et al 2014Damjanov et al , 2015. The analyses by various authors differ slightly in the selection of the sample, for example via passivity, visual classification, colour, and Sersic index; in the definition of so-called dense galaxies, selected for example on the basis of their mean stellar mass density Σ = M /2πR 2 e or sigma deviation from the local size-mass relation (SMR); and in the treatment of the progenitor bias.…”

Section: Introductionmentioning

confidence: 99%

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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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Section: Local Universementioning

confidence: 95%

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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“…The third scenario to explain the fast decline in the zero point of e Q S is that newly quenched galaxies at lower redshifts may arrive on the quiescent relation with significantly larger r e , and hence smaller e S , at a given mass than did earlier galaxies (e.g., Carollo et al 2013;Poggianti et al 2013). This is an example of the "progenitor bias" effect pointed out by van Dokkum & Franx (2001) S -than earlyevolving SFGs, giving some weight to this possibility.…”

Section: Is a Mass Loss) Thus The Ratio Between The Two Ismentioning

confidence: 98%

“…(2) Part of the increase in the overall radius can also be caused by additional processes, such as stellar mass loss associated with passive evolution (i.e., death of old stars), which causes adiabatic expansion (Damjanov et al 2011;Poggianti et al 2013;Porter et al 2014;. (3) Lastly, the strong decline in e Q S could also be caused by the arrival of new quiescent galaxies with progressively larger effective radii at lower redshifts (e.g., Carollo et al 2013;Poggianti et al 2013;Porter et al 2014). Each of these scenarios leads to a different evolution in the zero points of e Q S and 1 Q S , and thus we can test whether any of them matches the observed evolution in the ratio of zero points.…”

Section: Redshift Evolution Of the Zero Points Of The Quiescent Strucmentioning

confidence: 99%

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

Barro

Faber

Koo

et al. 2017

ApJ

270

384

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We study the evolution of the scaling relations that compare the effective density ( r r , e e S < ) and core density ( r , 1 1 S < kpc) to the stellar masses of star-forming galaxies (SFGs) and quiescent galaxies. These relations have been fully in place since z 3 and have exhibited almost constant slope and scatter since that time. For SFGs, the zero points in e S and 1 S decline by only 2 . This fact plus the narrowness of the relations suggests that galaxies could evolve roughly along the scaling relations. Quiescent galaxies follow different scaling relations that are offset to higher densities at the same mass and redshift. Furthermore, the zero point of their core density has declined by only 2 since z 3 , while the zero point of the effective density declines by 10 . When galaxies quench, they move from the star-forming relations to the quiescent relations. This involves an increase in the core and effective densities, which suggests that SFGs could experience a phase of significant core growth relative to the average evolution along the structural relations. The distribution of massive galaxies relative to the SFR-M and the quiescent M  Srelations exhibits an L-shape that is independent of redshift. The knee of this relation consists of a subset of "compact" SFGs that are the most likely precursors of quiescent galaxies forming at later times. The compactness selection threshold in 1 S exhibits a small variation from z=3 to 0.5, M 0.65 log 10.5 9.6 9.3 1 * S --> -( ) M e kpc −2 , allowing the most efficient identification of compact SFGs and quiescent galaxies at every redshift.

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“…Several studies have found a relation between the size and the age of passive galaxies at intermediate and high redshift (e.g., Valentinuzzi et al 2010;Poggianti et al 2013;Belli et al 2015;Shetty & Cappellari 2015, but see also Fagioli et al 2016 for different opinions), suggesting that the selection of old galaxies could minimize the descendant/progenitor mismatch. Following this idea, we select Coma galaxies whose ages are older than the difference between the look-back times of Coma and our highest redshift KCS overdensity (e.g., 9…”

Section: Distribution Of Galaxy Properties and Selection Effectsmentioning

confidence: 99%

The KMOS Cluster Survey (KCS). I. The Fundamental Plane and the Formation Ages of Cluster Galaxies at Redshift 1.4 < Z < 1.6*

Beifiori

Mendel

Chan

et al. 2017

ApJ

106

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We present the analysis of the fundamental plane (FP) for a sample of 19 massive red-sequence galaxies (M > 4 × 10 10 M ) in 3 known overdensities at 1.39 < z < 1.61 from the KMOS Cluster Survey, a guaranteed time program with spectroscopy from the K-band Multi-Object Spectrograph (KMOS) at the VLT and imaging from the Hubble Space Telescope. As expected, we find that the FP zero-point in B band evolves with redshift, from the value 0.443 of Coma to −0.10 ± 0.09, −0.19 ± 0.05, −0.29 ± 0.12 for our clusters at z = 1.39, z = 1.46, and z = 1.61, respectively. For the most massive galaxies (log M /M > 11) in our sample, we translate the FP zero-point evolution into a mass-to-light-ratio M/L evolution finding ∆ log M/L B = (−0.46 ± 0.10)z, ∆ log M/L B = (−0.52 ± 0.07)z, to ∆ log M/L B = (−0.55 ± 0.10)z, respectively. We assess the potential contribution of the galaxies structural and stellar velocity dispersion evolution to the evolution of the FP zeropoint and find it to be ∼6-35% of the FP zero-point evolution. The rate of M/L evolution is consistent with galaxies evolving passively. By using single stellar population models, we find an average age of 2.33 +0.86 −0.51 Gyr for the log M /M > 11 galaxies in our massive and virialized cluster at z = 1.39, 1.59 +1.40 −0.62 Gyr in a massive but not virialized cluster at z = 1.46, and 1.20 +1.03 −0.47 Gyr in a protocluster at z = 1.61. After accounting for the difference in the age of the Universe between redshifts, the ages of the galaxies in the three overdensities are consistent within the errors, with possibly a weak suggestion that galaxies in the most evolved structure are older.

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The Evolution of the Number Density of Compact Galaxies

Cited by 92 publications

References 47 publications

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

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

Structural and Star-forming Relations since z ∼ 3: Connecting Compact Star-forming and Quiescent Galaxies

The KMOS Cluster Survey (KCS). I. The Fundamental Plane and the Formation Ages of Cluster Galaxies at Redshift 1.4 < Z < 1.6*

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