The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

Sohn, Jubee; Geller, Margaret J.; Zahid, H. Jabran; Fabricant, Daniel G.; Diaferio, Antonaldo; Rines, Kenneth J.

doi:10.3847/1538-4365/aa653e

Cited by 58 publications

(119 citation statements)

References 106 publications

(256 reference statements)

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“…The centre region of the Coma cluster (green points) is a clearly distinguishable component in the Coma cluster. The centre of this component is located at redshift 0.0235, which is slightly higher than the value (0.0231) given A100, page 6 of 12 in the NASA/IPAC Extragalactic Database 6 (Struble & Rood 1999), but is consistent with the value given in Sohn et al (2017). The difference comes from the identification of the Coma cluster members.…”

Section: Selected Known Clusterssupporting

confidence: 43%

Merging groups and clusters of galaxies from the SDSS data

Tempel

Tuvikene

Kipper

et al. 2017

A&A

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Context. Galaxy groups and clusters are the main tools used to test cosmological models and to study the environmental effect of galaxy formation. Aims. This work provides a catalogue of galaxy groups and clusters, as well as potentially merging systems based on the SDSS main galaxy survey. Methods. We identified galaxy groups and clusters using the modified friends-of-friends (FoF) group finder designed specifically for flux-limited galaxy surveys. The FoF group membership is refined by multimodality analysis to find subgroups and by using the group virial radius and escape velocity to expose unbound galaxies. We look for merging systems by comparing distances between group centres with group radii. Results. The analysis results in a catalogue of 88 662 galaxy groups with at least two members. Among them are 6873 systems with at least six members which we consider to be more reliable groups. We find 498 group mergers with up to six groups. We performed a brief comparison with some known clusters in the nearby Universe, including the Coma cluster and Abell 1750. The Coma cluster in our catalogue is a merging system with six distinguishable subcomponents. In the case of Abell 1750 we find a clear sign of filamentary infall toward this cluster. Our analysis of mass-to-light ratio (M/L) of galaxy groups reveals that M/L slightly increases with group richness.

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Section: Selected Known Clusterssupporting

confidence: 43%

Merging groups and clusters of galaxies from the SDSS data

Tempel

Tuvikene

Kipper

et al. 2017

A&A

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“…MACH is a remarkable spectroscopic campaign for nearby clusters that provides more than 2500 spectra per cluster. For example, Abell 2029, used for a pilot study of MACH, is one of the best sampled clusters with ∼ 1200 spectroscopically identified members (Sohn et al 2017. A more detailed discussion of the entire MACH sample will be included in Sohn et al (in preparation).…”

Section: Spectroscopymentioning

confidence: 99%

“…We derive stellar masses based on the SDSS photometry using the Le Phare fitting code (Arnouts et al 1999;Ilbert et al 2006). We follow the stellar mass estimation process described in Sohn et al (2017) who measured the stellar mass function of spectroscopic members of the nearby massive cluster A2029. We briefly review the stellar mass estimation here (see Sohn et al 2017.…”

Section: Stellar Massmentioning

confidence: 99%

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Velocity Dispersions of Brightest Cluster Galaxies and Their Host Clusters

Sohn

Geller

Diaferio

et al. 2020

ApJ

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We explore connections between brightest cluster galaxies (BCGs) and their host clusters. We first construct a HeCS-omnibus cluster sample including 227 galaxy clusters within 0.02 < z < 0.30; the total number of spectroscopic members from MMT/Hectospec and SDSS observations is 52325. Taking advantage of the large spectroscopic sample, we compute physical properties of the clusters including the dynamical mass and cluster velocity dispersion (σ cl ). We also measure the central stellar velocity dispersion of the BCGs (σ * ,BCG s) to examine the relation between BCG velocity dispersion and cluster velocity dispersion for the first time. The observed relation between BCG velocity dispersion and the cluster velocity dispersion is remarkably tight. Interestingly, the σ * ,BCG /σ cl ratio decreases as a function of σ cl unlike the prediction from the numerical simulation of Dolag et al. (2010). The trend in σ * ,BCG /σ cl suggests that the BCG formation is more efficient in lower mass halos.

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“…The Coma cluster has a median redshift of cz = 7090 km s −1 (Geller et al 1999) and a velocity dispersion ∼1000 km s −1 (e.g., Colless & Dunn 1996;Mobasher et al 2001;Rines et al 2013;Sohn et al 2016 Dokkum et al 2015a), indicating that they are typical examples in the UDG population. We provide the first measurement of a recession velocity of DF17 and confirmation measurements of the recession velocities of DF7 and DF44.…”

mentioning

confidence: 99%

Low Metallicities and Old Ages for Three Ultra-diffuse Galaxies in the Coma Cluster

Conroy

Law

et al. 2018

ApJ

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A large population of ultra-diffuse galaxies (UDGs) was recently discovered in the Coma cluster. Here we present optical spectra of three such UDGs, DF7, DF44, and DF17, which have central surface brightnesses of μ g ≈24.4-25.1 mag arcsec −2 . The spectra were acquired as part of an ancillary program within the SDSS-IV MaNGA Survey. We stacked 19 fibers in the central regions from larger integral field units (IFUs) per source. With over 13.5 hr of on-source integration, we achieved a mean signal-to-noise ratio in the optical of 9.5 Å −1 , 7.9 Å −1 , and 5.0 Å −1 , respectively, for DF7, DF44, and DF17. Stellar population models applied to these spectra enable measurements of recession velocities, ages, and metallicities. respectively. Their stellar masses are (3-6)×10 8 M e . The UDGs in our sample are as old or older than galaxies at similar stellar mass or velocity dispersion (only DF 44 has an independently measured dispersion). They all follow the well-established stellar mass-stellar metallicity relation, while DF44 lies below the velocity dispersionmetallicity relation. These results, combined with the fact that UDGs are unusually large for their stellar masses, suggest that stellar mass plays a more important role in setting stellar population properties for these galaxies than either size or surface brightness.

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The Velocity Dispersion Function of Very Massive Galaxy Clusters: Abell 2029 and Coma

Cited by 58 publications

References 106 publications

Merging groups and clusters of galaxies from the SDSS data

Merging groups and clusters of galaxies from the SDSS data

Velocity Dispersions of Brightest Cluster Galaxies and Their Host Clusters

Low Metallicities and Old Ages for Three Ultra-diffuse Galaxies in the Coma Cluster

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