CIRS: Cluster Infall Regions in the Sloan Digital Sky Survey. I. Infall Patterns and Mass Profiles

Rines, Kenneth J.; Diaferio, Antonaldo

doi:10.1086/506017

Cited by 229 publications

(402 citation statements)

References 88 publications

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“…They studied the cluster masses in an X-ray-selected sample of clusters with data from SDSS DR4. The masses were computed in two ways, one using the virial theorem (black squares) and the other (red squares) using the caustic technique (Rines & Diaferio 2006). Both mass functions are similar to our mass functions for massive clusters.…”

Section: Volume-limited Groups and Mass Functionmentioning

confidence: 89%

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Tempel

Tamm

Gramann

et al. 2014

A&A

222

488

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We provide flux-and volume-limited galaxy group and cluster catalogues based on the spectroscopic sample of the galaxies of SDSS data release 10. We used a modified friends-of-friends method with a variable linking length in the transverse and radial directions to identify as many realistic groups as possible. The flux-limited catalogue incorporates galaxies down to m r = 17.77 mag. It includes 588 193 galaxies and 82 458 groups. The volume-limited catalogues are complete for absolute magnitudes down to M r,lim = −18.0, −18.5, −19.0, −19.5, −20.0, −20.5, and −21.0; the completeness is achieved within different spatial volumes. Our analysis shows that flux-and volume-limited group samples are well compatible, especially for the larger groups/clusters. Dynamical mass estimates based on radial velocity dispersions and group extent in the sky were added to the extracted groups.

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Section: Volume-limited Groups and Mass Functionmentioning

confidence: 89%

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Tempel

Tamm

Gramann

et al. 2014

A&A

222

488

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“…Over time, the measured escape edge in the outskirts of galaxy clusters grows in amplitude to represent the predicted escape velocity defined by the potential. This dynamical evolution of the escape edge in the cluster infall regions is important for studies which use the escape velocity technique to measure mass profiles to well beyond the virial radius (Rines & Diaferio 2006;Rines et al 2013). …”

Section: Mass and Redshift Dependencementioning

confidence: 99%

Inferring Gravitational Potentials From Mass Densities in Cluster-Sized Halos

Miller

Stark

Gifford

et al. 2016

ApJ

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We use N-body simulations to quantify how the escape velocity in cluster-sized halos maps to the gravitational potential in a ΛCDM universe. Using spherical density-potential pairs and the Poisson equation, we find that the matter density inferred gravitational potential profile predicts the escape velocity profile to within a few percent accuracy for group and cluster-sized halos (10 < < M 1013 200 15 M  , with respect to the critical density). The accuracy holds from just outside the core to beyond the virial radius. We show the importance of explicitly incorporating a cosmological constant when inferring the potential from the Poisson equation. We consider three density models and find that the Einasto and Gamma profiles provide a better joint estimate of the density and potential profiles than the Navarro, Frenk, and White profile, which fails to accurately represent the escape velocity. For individual halos, the 1σ scatter between the measured escape velocity and the density-inferred potential profile is small (<5%). Finally, while the sub-halos show 15% biases in their representation of the particle velocity dispersion profile, the sub-halo escape velocity profile matches the dark matter escape velocity profile to high accuracy with no evidence of velocity bias outside 0.4r 200 .

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“…However, this is not the case for some nearby galaxy clusters with deep spectroscopic LFs (e.g. Rines & Diaferio 2006). Agulli et al (2014) showed that the LF of A 85 measured in three decades in luminosities has an upturn at Mr ∼ −18 and a steep faint end.…”

Section: Introductionmentioning

confidence: 99%

“…We have undertaken a campaign of deep spectroscopic observations of nearby clusters down to the dwarf regime (Mr M * r + 4) in order to infer accurate cluster membership and study the properties of low-mass galaxies, such as star formation histories and orbital parameters. The richness class 1 cluster Abell 85 (A 85 hereafter) is a nearby (z = 0.055) and massive cluster (R200 = 1.02 h −1 Mpc and M200 = 2.5 × 10 14 M ⊙ Rines & Diaferio 2006). It is one of the brightest clusters in the X-ray sky (Edge et al 1990) with a smoothed gas distribution.…”

Section: Introductionmentioning

confidence: 99%

“…It is one of the brightest clusters in the X-ray sky (Edge et al 1990) with a smoothed gas distribution. It has been extensively studied in the whole electromagnetic spectrum: in the radio (Slee et al 2001), in the optical (Rines & Diaferio 2006;Ramella et al 2007;Bravo-Alfaro et al 2009) and in the X-ray (e.g. Schenck et al 2014;Ichinohe et al 2015).…”

Section: Introductionmentioning

confidence: 99%

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Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

Agulli¹,

Aguerri²,

Sánchéz-Janssen³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a new deep spectroscopic catalogue for Abell 85, within 3.0 × 2.6 Mpc 2 and down to M r ∼ M * r +6. Using the Visible Multi-Object Spectrograph at the Very Large Telescope and the AutoFiber 2 at the William Herschel Telescope, we obtained almost 1430 new redshifts for galaxies with m r ≤ 21 mag and µ e,r ≤ 24 mag arcsec −2 . These redshifts, together with SDSS-DR6 and NED spectroscopic information, result in 460 confirmed cluster members. This data set allows the study of the luminosity function (LF) of the cluster galaxies covering three orders of magnitudes in luminosities. The total and radial LFs are best modelled by a double Schechter function. The normalized LFs show that their bright (M r ≤ −21.5) and faint (M r ≥ −18.0) ends are independent of clustercentric distance and similar to the field LFs unlike the intermediate luminosity range (−21.5 ≤ M r ≤ −18.0). Similar results are found for the LFs of the dominant types of galaxies: red, passive, virialized and early-infall members. On the contrary, the LFs of blue, star-forming, non-virialized and recent-infall galaxies are well described by a single Schechter function. These populations contribute to a small fraction of the galaxy density in the innermost cluster region. However, in the outskirts of the cluster, they have similar densities to red, passive, virialized and early-infall members at the LF faint end. These results confirm a clear dependence of the colour and star formation of Abell 85 members in the cluster centric distance.

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CIRS: Cluster Infall Regions in the Sloan Digital Sky Survey. I. Infall Patterns and Mass Profiles

Cited by 229 publications

References 88 publications

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Flux- and volume-limited groups/clusters for the SDSS galaxies: catalogues and mass estimation

Inferring Gravitational Potentials From Mass Densities in Cluster-Sized Halos

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

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