HOMOGENEOUS
                    <i>UGRIZ</i>
                    PHOTOMETRY FOR ACS VIRGO CLUSTER SURVEY GALAXIES: A NON-PARAMETRIC ANALYSIS FROM SDSS IMAGING

Chen, Chin-Wei; Côté, Patrick; West, Andrew A.; Peng, Eric W.; Ferrarese, Laura

doi:10.1088/0067-0049/191/1/1

Cited by 70 publications

(92 citation statements)

References 136 publications

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“…On average, the center of the galaxy has a redder color, with a maximum value up to (g − i) ∼ (1.3 ± 0.18) mag. Our (g − i) color profile is fully consistent with that published by Chen et al (2010), which only extends up to a 1/4 ∼ 2.8 or a/a e ∼ 1, however. The color stays bluer in the range 5 ≤ a ≤ 150 (1.5 ≤ a 1/4 ≤ 3.5), then it turns redder again, and the gradient is almost flat, although the errors here are too large to robustly assess whether there are color gradients outside this radial range.…”

Section: Ngc 4472supporting

confidence: 90%

VEGAS: A VST Early-type GAlaxy Survey

Capaccioli

Spavone

Grado

et al. 2015

A&A

141

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Context. We present the VST Early-type GAlaxy Survey (VEGAS), which is designed to obtain deep multiband photometry in g, r, i, of about one hundred nearby galaxies down to 27.3, 26.8, and 26 mag/arcsec 2 respectively, using the ESO facility VST/OmegaCAM. Aims. The goals of the survey are 1) to map the light distribution up to ten effective radii, r e ; 2) to trace color gradients and surface brightness fluctuation gradients out to a few r e for stellar population characterization; and 3) to obtain a full census of the satellite systems (globular clusters and dwarf galaxies) out to 20% of the galaxy virial radius. The external regions of galaxies retain signatures of the formation and evolution mechanisms that shaped them, and the study of nearby objects enables a detailed analysis of their morphology and interaction features. To clarify the complex variety of formation mechanisms of early-type galaxies (ETGs), wide and deep photometry is the primary observational step, which at the moment has been pursued with only a few dedicated programs. The VEGAS survey has been designated to provide these data for a volume-limited sample with exceptional image quality. Methods. In this commissioning photometric paper we illustrate the capabilities of the survey using g-and i-band VST/OmegaCAM images of the nearby galaxy NGC 4472 and of smaller ETGs in the surrounding field. Results. Our surface brightness profiles reach rather faint levels and agree excellently well with previous literature. Genuine new results concern the detection of an intracluster light tail in NGC 4472 and of various substructures at increasing scales. We have also produced extended (g − i) color profiles. Conclusions. The VST/OmegaCAM data that we acquire in the context of the VEGAS survey provide a detailed view of substructures in the optical emission from extended galaxies, which can be as faint as a hundred times below the sky level.

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Section: Ngc 4472supporting

confidence: 90%

VEGAS: A VST Early-type GAlaxy Survey

Capaccioli

Spavone

Grado

et al. 2015

A&A

141

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“…However, the origin of this large population of dEs is still a topic of ongoing debate, partly because they were found to follow a number of continuous relations in structure and colour with bright elliptical and/or lenticular galaxies (e.g. Côté et al 2007;Chen et al 2010;Kormendy & Bender 2012), but also since their identification Appendices are available in electronic form at http://www.aanda.org and detailed analysis are not yet possible at higher shifts (see Barazza et al 2009 for dEs in a z = 0.165 cluster). Clues to the origin of dEs may be given by the presence of weak disk features in a significant fraction of them (Jerjen et al 2000;De Rijcke et al 2003;Lisker et al 2006b), the presence of residual star formation activity in dEs outside of the densest environments (Lisker et al 2006a;Tully & Trentham 2008;Pak et al 2014) and the finding that these have significantly flatter shapes than dEs with low relative velocities in the Virgo cluster core ).…”

Section: Introductionmentioning

confidence: 99%

On the occurrence of galaxy harassment

Bialas

Lisker

Olczak

et al. 2015

A&A

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Context. Tidal interactions of galaxies in galaxy clusters have been proposed as one potential explanation of the morphology-density relation at low masses. Earlier studies have shown that galaxy harassment is a suitable mechanism for inducing a morphological transformation from low-mass late-type disk galaxies to the abundant early-type galaxies. Aims. The efficiency of tidal transformation is expected to depend strongly on the orbit of a galaxy within the cluster halo. The orbit determines both the strength of the cluster's global tidal field and the probability of encounters with other cluster members. Here we aim to explore these dependencies. Methods. We use a combination of N-body simulation and Monte-Carlo method to study the efficiency of the transformation of late-type galaxies by tidal interactions on different orbits in a galaxy cluster. Additionally, we investigate the effect of an inclination between the disk of the infalling galaxy and its orbital plane. We compare our results to observational data to assess the possible relevance of such transformations for the existing cluster galaxy population. Results. We find that galaxies that entered a cluster from the outskirts are unlikely to be significantly transformed (stellar mass loss ≤6%). Closer to the cluster centre, tidal interactions are a more efficient mechanism (stellar mass loss up to 50%) for producing harassed galaxies. The inclination of the disk can reduce the mass loss significantly, yet it amplifies the thickening of the galaxy disk. Galaxies with smaller sizes on intermediate orbits are nearly unaffected by tidal interactions. The tidal influence on an infalling galaxy and the likelihood that it leads to galaxy harassment make a very stochastical process that depends on the galaxy's specific history. Conclusions. We conclude that harassment is a suitable mechanism that could explain the transformation of at least a fraction of galaxies inside galaxy clusters. However, the transformation would have to start at an early epoch in protocluster environments and continue until today, in order to result in a complete morphological transformation.

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“…This is illustrated in the left panel of Fig. 1 (from Chen et al 2010), which provides a comparison between independent determinations of R e for well-studied galaxies in the Virgo cluster.…”

Section: Uncertainties Of Galaxy Sizesmentioning

confidence: 99%

“…Differences in the measurement approach combine with (i) differences in the restframe wavelength of the observations, Chen et al (2010) with independent determinations of the same quantity from the literature. Bottom Panel: Gray dots show the fractional error in the effective radius measurements, plotted as a function of the SDSS effective radii; the mean and standard deviation for individual galaxies are plotted as the black dots with error bars.…”

Section: Uncertainties Of Galaxy Sizesmentioning

confidence: 99%

“…Bottom Panel: Gray dots show the fractional error in the effective radius measurements, plotted as a function of the SDSS effective radii; the mean and standard deviation for individual galaxies are plotted as the black dots with error bars. Differences in Re of a factor 2× are common, especially for the largest galaxies (taken from Chen et al 2010). Right: Comparing images of nearby and distant ETGs.…”

Section: Uncertainties Of Galaxy Sizesmentioning

confidence: 99%

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Dynamical masses of early-type galaxies at z ~ 2

Cappellari¹

2012

Proc. IAU

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Abstract. The evolution of masses and sizes of passive (early-type) galaxies with redshift provides ideal constraints to galaxy formation models. These parameters can in principle be obtained for large galaxy samples from multi-band photometry alone. However the accuracy of photometric masses is limited by the non-universality of the IMF. Galaxy sizes can be biased at high redshift due to the inferior quality of the imaging data. Both problems can be avoided using galaxy dynamics, and in particular by measuring the galaxies stellar velocity dispersion. Here we provide an overview of the efforts in this direction.

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HOMOGENEOUS UGRIZ PHOTOMETRY FOR ACS VIRGO CLUSTER SURVEY GALAXIES: A NON-PARAMETRIC ANALYSIS FROM SDSS IMAGING

Cited by 70 publications

References 136 publications

VEGAS: A VST Early-type GAlaxy Survey

VEGAS: A VST Early-type GAlaxy Survey

On the occurrence of galaxy harassment

Dynamical masses of early-type galaxies at z ~ 2

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