The Extended Virgo Cluster Catalog

Kim, S.; Rey, Soo-Chang; Jerjen, Helmut; Lisker, Thorsten; Sung, Eon‐Chang; Lee, Youngdae; Chung, Jiwon; Pak, Mina; Yi, Wonhyeong; Lee, Woong

doi:10.1088/0067-0049/215/2/22

Cited by 140 publications

(199 citation statements)

References 67 publications

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“…The Extended Virgo Cluster Catalogue (EVCC, Kim et al 2014) provides the redshifts and positions on the sky of 1589 galaxies in a footprint of 725 deg 2 centred on M87, extending to 3.5 times the cluster virial radius. The redshifts are compiled from the SDSS DR7 release and the NASA Extragalactic Database (NED), and each object is classified as either a certain cluster member, a possible member or a background source based on morphological and spectroscopic criteria.…”

Section: Satellite Galaxiesmentioning

confidence: 99%

Galaxy structure from multiple tracers – II. M87 from parsec to megaparsec scales

Oldham

Auger

2016

Mon. Not. R. Astron. Soc.

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Following a number of conflicting studies of M87's mass profile, we undertake a dynamical analysis of multiple tracer populations to constrain its mass over a large radius range. We combine stellar kinematics in the central regions with the dynamics of 612 globular clusters out to 200 kpc and satellite galaxies extending to scales comparable with the virial radius. Using a spherical Jeans analysis, we are able to disentangle the mass contributions from the dark and baryonic components and set constraints on the structure of each. Assuming isotropy, we explore four different models for the dark matter halo and find that a centrally-cored dark matter distribution is preferred. We infer a stellar mass-to-light ratio Υ ,v = 6.9 ± 0.1 -consistent with a Salpeter-like IMF -and a core radius r c = 67±20 kpc. We then introduce anisotropy and find that, while the halo remains clearly cored, the radial stellar anisotropy has a strong impact on both Υ ,v and the core's radius; here we find Υ ,v = 3.50 +0.32 −0.36 -consistent with a Chabrier-like IMF -and r c = 19.00 +8.38 −8.34 kpc. Thus the presence of a core at the centre of the dark halo is robust against anisotropy assumptions, while the stellar mass and core size are not. We are able to reconcile previously discrepant studies by showing that modelling the globular cluster data alone leads to the very different inference of a super-NFW cusp, thus highlighting the value of multiple-population modelling, and we point to the possible role of M87's AGN and the cluster environment in forming the central dark matter core.

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Section: Satellite Galaxiesmentioning

confidence: 99%

Galaxy structure from multiple tracers – II. M87 from parsec to megaparsec scales

Oldham

Auger

2016

Mon. Not. R. Astron. Soc.

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“…Despite their relative low scatter, these relations are unfortunately not sufficiently accurate for an unambiguous identification of cluster members and thus need to be combined with statistical tests. These scaling relations are determined using either the Extended Virgo Cluster Catalogue (EVCC, Kim et al 2014) or the GUViCS catalogue of galaxies analysed in Boselli et al (2014a). The EVCC catalogue was chosen because it includes galaxies at the same distance as Virgo (vel ≤ 3000 km s −1 ), it has both star forming and quiescent galaxies, and provides structural parameters comparable to those listed in the GUViCS point-like catalogue of Voyer et al (2014).…”

Section: Statistical Correction Based On Galex-sdss Scaling Relationsmentioning

confidence: 99%

“…This can be done either by using the accurate morphological classification given in the VCC or in the EVCC (Kim et al 2014), or by using the colour of galaxies as in Boselli et al (2014a). As in our previous work, we select galaxies belonging to the red sequence, the green valley, and the blue cloud Notes.…”

Section: Luminosity Function As a Function Of Morphological Typementioning

confidence: 99%

The GALEX Ultraviolet Virgo Cluster Survey (GUViCS)

Boselli

Boissier

Voyer

et al. 2015

A&A

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We use the GALEX data of the GUViCS survey to construct the near-ultraviolet (NUV) luminosity function of the Virgo cluster over ∼300 deg 2 , an area covering the cluster and its surrounding regions up to ∼1.8 virial radii. The NUV luminosity function is also determined for galaxies of different morphological types and NUV − i colours, and for the different substructures within the cluster. These luminosity functions are robust vs. statistical corrections since based on a sample of 833 galaxies mainly identified as cluster members with spectroscopic redshift (808) or high-quality optical scaling relations (10). We fit these luminosity functions with a Schechter function, and compare the fitted parameters with those determined for other nearby clusters and for the field. The faint end slope of the Virgo NUV luminosity function (α = −1.19), here sampled down to ∼NUV = −11.5 mag, is significantly flatter than the value measured in other nearby clusters and similar to the field value. Similarly, M * = −17.56 is one to two magnitudes fainter than measured in Coma, A1367, the Shapley supercluster, and the field. These differences seem to be due to the quite uncertain statistical corrections and the small range in absolute magnitude sampled in these clusters. We do not observe strong systematic differences in the overall NUV luminosity function of the core of the cluster with respect to that of its periphery. We note, however, that the relative contribution of red and blue galaxies at the faint end is inverted, with red quiescent objects dominating the core of the cluster and star forming galaxies dominating beyond one virial radius. This observational evidence is discussed in the framework of galaxy evolution in dense environments.

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“…The Virgo Cluster, instead, is still growing. Subclusters around the ellipticals M86 and M49 (whose systemic velocities are, respectively, −181 and 950 km s −1 , Kim et al 2014) are merging with the main cluster around the central elliptical M87. Several H I imaging surveys of the cluster revealed that the H I discs of its central late-type galaxies are truncated to well within the optical discs, suggesting that ICM-ISM interactions play an important role in driving the evolution of galaxies in the inner region of the cluster (Warmels 1988;Cayatte et al 1990;Chung et al 2009;Boselli et al 2014).…”

Section: Introductionmentioning

confidence: 99%