SIMBAD references

2017ApJ...835..254M - Astrophys. J., 835, 254-254 (2017/February-1)

The Grism Lens-Amplified Survey from Space (GLASS). IX. The dual origin of low-mass cluster galaxies as revealed by new structural analyses.

MORISHITA T., ABRAMSON L.E., TREU T., VULCANI B., SCHMIDT K.B., DRESSLER A., POGGIANTI B.M., MALKAN M.A., WANG X., HUANG K.-H., TRENTI M., BRADAC M. and HOAG A.

Abstract (from CDS):

Using deep Hubble Frontier Fields imaging and slitless spectroscopy from the Grism Survey from Space, we study 2200 cluster and 1748 field galaxies at 0.2 z 0.7 to determine the impact of environment on galaxy size and structure at stellar masses logM*/M 7.8, an unprecedented limit at these redshifts. Based on simple assumptions-re=f(M*)-we find no significant differences in half-light radii (re) between equal-mass cluster or field systems. More complex analyses-re=f(M*,U-V,n,z,Σ)-reveal local density (Σ) to induce only a 7% ± 3% (95% confidence) reduction in re beyond what can be accounted for by U - V color, Sersic index (n), and redshift (z) effects. Almost any size difference between galaxies in high- and low-density regions is thus attributable to their different distributions in properties other than environment. Indeed, we find a clear color-re correlation in low-mass passive cluster galaxies (logM*/M 9.8) such that bluer systems have larger radii, with the bluest having sizes consistent with equal-mass star-forming galaxies. We take this as evidence that large-re low-mass passive cluster galaxies are recently acquired systems that have been environmentally quenched without significant structural transformation (e.g., by ram pressure stripping or starvation). Conversely, ∼20% of small-re low-mass passive cluster galaxies appear to have been in place since z 3. Given the consistency of the small-re galaxies' stellar surface densities (and even colors) with those of systems more than ten times as massive, our findings suggest that clusters mark places where galaxy evolution is accelerated for an ancient base population spanning most masses, with late-time additions quenched by environment-specific mechanisms mainly restricted to the lowest masses.

Abstract Copyright: © 2017. The American Astronomical Society. All rights reserved.

Journal keyword(s): galaxies: clusters: general - galaxies: elliptical and lenticular, cD - galaxies: evolution - galaxies: structure - galaxies: structure

VizieR on-line data: <Available at CDS (J/ApJ/835/254): table1.dat>

Nomenclature: Table 1: [MAT2017] Abell2744CLS NNNN N=661 among (Nos Abell2744CLS 1225-Abell2744CLS 5450), [MAT2017] Abell2744PR1 NNNN N=148 among (Nos Abell2744PR1 843-Abell2744PR1 2749), [MAT2017] MACS0416CLS NNNN N=594 among (Nos MACS0416CLS 2857-MACS0416CLS 3980), [MAT2017] MACS0416PR1 NNNN N=215 among (Nos MACS0416PR1 1215-MACS0416PR1 3693), [MAT2017] MACS0717CLS NNNN N=1237 among (Nos MACS0717CLS 486-MACS0717CLS 4959), [MAT2017] MACS0717PR1 NNNN N=251 among (Nos MACS0717PR1 896-MACS0717PR1 3356), [MAT2017] MACS1149CLS NNNN N=982 among (Nos MACS1149CLS 275-MACS1149CLS 4935), [MAT2017] MACS1149PR1 NNNN N=164 (Nos MACS1149PR1 735-MACS1149PR1 3682), [MAT2017] XDF NNNN N=57 among (Nos XDF 21-XDF 1509), N=4309.

Simbad objects: 4301

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2019.12.13-09:00:28

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