A new method to measure the mass of galaxy clusters

Falco, Martina; Hansen, Steen H.; Wojtak, Radosław; Brinckmann, Thejs; Lindholmer, Mikkel; Pandolfi, Stefania

doi:10.1093/mnras/stu971

Cited by 43 publications

(178 citation statements)

References 64 publications

(65 reference statements)

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“…7) they show narrow velocity (z) dispersions at all r, which supports the idea that they are indeed cosmic filaments. In fact their phase-space distribution is similar to the large-scale filaments found around Virgo (see Figure 3 in Lee, Kim & Rey 2015) and Coma (see Figure 4 in Falco et al 2014). It is possible that the groups (plotted as grey open circles in Fig.…”

Section: Accretion History Of the Clustersupporting

confidence: 66%

BUDHIES – III: the fate of H i and the quenching of galaxies in evolving environments

Jaffé

Verheijen

Haines

et al. 2016

Mon. Not. R. Astron. Soc.

114

111

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In a hierarchical Universe clusters grow via the accretion of galaxies from the field, groups and even other clusters. As this happens, galaxies can lose their gas reservoirs via different mechanisms, eventually quenching their star formation. We explore the diverse environmental histories of galaxies through a multiwavelength study of the combined effect of ram-pressure stripping and group 'processing' in Abell 963, a massive growing cluster at z = 0.2 from the Blind Ultra Deep Hi Environmental Survey (BUDHIES). We incorporate hundreds of new optical redshifts (giving a total of 566 cluster members), as well as Subaru and XMM-Newton data from LoCuSS, to identify substructures and evaluate galaxy morphology, star formation activity, and Hi content (via Hi deficiencies and stacking) out to 3×R 200 . We find that Abell 963 is being fed by at least seven groups, that contribute to the large number of passive galaxies outside the cluster core. More massive groups have a higher fraction of passive and Hi -poor galaxies, while low-mass groups host younger (often interacting) galaxies. For cluster galaxies not associated with groups we corroborate our previous finding that Hi gas (if any) is significantly stripped via ram-pressure during their first passage through the intracluster medium, and find mild evidence for a starburst associated with this event. In addition, we find an overabundance of morphologically peculiar and/or star-forming galaxies near the cluster core. We speculate that these arise as groups pass through the cluster (post-processing). Our study highlights the importance of environmental quenching and the complexity added by evolving environments.

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Section: Accretion History Of the Clustersupporting

confidence: 66%

BUDHIES – III: the fate of H i and the quenching of galaxies in evolving environments

Jaffé

Verheijen

Haines

et al. 2016

Mon. Not. R. Astron. Soc.

114

111

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“…The peculiar velocity profiles for the nDGP models are still well fitted by Equation (2), which was empirically derived by Falco et al (2014) from N-body simulations for the GR+ΛCDM cosmology. Having no analytic framework within which the bound-zone velocity profile can be derived from the first principles for nDGP models, we have assumed that no matter what background cosmology is used, the peculiar velocity of a bound-zone galaxy may be proportional to some power of the separation distance and thus that the same functional form of Equation (2) can still describe the average peculiar velocity profile even for the nDGP models.…”

Section: Bound-zone Velocity Profiles In Ndgp Modelsmentioning

confidence: 62%

“…Recently, Lee & Yepes (2016) showed that the odds of the bound violations become larger if the odds are calculated from the bound-zone velocity profiles constructed along the filaments. In fact, in order to apply the routine of Lee et al (2015) to real observational data for the estimate of the turn-around radius of a galaxy group, finding a filamentary structure in the bound zone and to construct the bound-zone velocity profile along the filament (Falco et al 2014;Lee et al 2015) is a prerequisite since the anisotropic distribution of the bound-zone galaxies along the filaments allows us to construct the bound-zone velocity profile without measuring accurately the peculiar velocities (see Falco et al 2014 for details).…”

mentioning

confidence: 99%

The Effect of Modified Gravity on the Odds of the Bound Violations of the Turn-around Radii

Lee

2017

ApJ

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(2017) 'The eect of modied gravity on the odds of the bound violations of the turn-around radii.', Astrophysical journal., 842 (1). p. 2.Further information on publisher's website:https://doi.org/10.3847/1538-4357/aa706fPublisher's copyright statement: c 2017. The American Astronomical Society. All rights reserved. Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. AbstractThe turn-around radii of the galaxy groups show the imprint of a long battle between their self-gravitational forces and the accelerating space. The standard ΛCDM cosmology based on the general relativity (GR) predicts the existence of an upper bound on the expectation value of the turn-around radius that is rarely violated by individual galaxy groups. We speculate that a deviation of the gravitational law from GR on the cosmological scale could cause an appreciable shift of the mean turn-around radius to higher values and make the occurrence of the bound violation more probable. Analyzing the data from high-resolution N-body simulations for two specific models with modified gravity (MG) and the standard GR+ΛCDM cosmology, we determine the turn-around radii of the massive Rockstar groups from the peculiar motions of the galactic halos located in the bound zone where the fifth force generated by MG is expected to be, at most, partially shielded. We detect a s 4 signal of difference in the odds of the bound violations between a fiducial MG and the GR models, which proves that the odds of the bound violations increase with the strength of the fifth force produced by the presence of MG. The advantage of using the odds of the bound violations as a complementary diagnostics to probe the nature of gravity is discussed.

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“…A structural feature held in common by all four of the Galaxy clusters discussed here (Coma, A2052, A2147, and A2199 from Paper II) is a prominent X-ray halo gas component. Of 60 nearby clusters listed by Edwards et al (2007) that were selected from the NOAO Fundamental Plane Survey, these four rank among the highest in X-ray luminosity, but not all of them have strong cooling flows or central optical (e.g., Blanton et al 2003;Łokas et al 2006;Kubo et al 2007;Wen et al 2010;Wojtak & Lokas 2010;Falco et al 2014).…”

Section: Metallicity and Color Distributionsmentioning

confidence: 99%

Globular Cluster Systems in Brightest Cluster Galaxies. Iii. Beyond Bimodality

Harris

Ciccone

Eadie

et al. 2017

ApJ

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We present new deep photometry of the rich globular cluster (GC) systems around the Brightest Cluster Galaxies UGC 9799 (Abell 2052) and UGC 10143 (Abell 2147), obtained with the Hubble Space Telescope (HST) ACS and WFC3 cameras. For comparison, we also present new reductions of similar HST/ACS data for the Coma supergiants NGC 4874 and 4889. All four of these galaxies have huge cluster populations (to the radial limits of our data, comprising from 12,000 to 23,000 clusters per galaxy). The metallicity distribution functions (MDFs) of the GCs can still be matched by a bimodal-Gaussian form where the metal-rich and metalpoor modes are separated by 0.8 dex, but the internal dispersions of each mode are so large that the total MDF becomes very broad and nearly continuous from [Fe/H];−2.4 to solar. There are, however, significant differences between galaxies in the relative numbers of metal-rich clusters, suggesting that they underwent significantly different histories of mergers with massive gas-rich halos. Last, the proportion of metal-poor GCs rises especially rapidly outside projected radii  R R 4 eff , suggesting the importance of accreted dwarf satellites in the outer halo. Comprehensive models for the formation of GCs as part of the hierarchical formation of their parent galaxies will be needed to trace the systematic change in structure of the MDF with galaxy mass, from the distinctly bimodal form in smaller galaxies up to the broad continuum that we see in the very largest systems.

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A new method to measure the mass of galaxy clusters

Cited by 43 publications

References 64 publications

BUDHIES – III: the fate of H i and the quenching of galaxies in evolving environments

BUDHIES – III: the fate of H i and the quenching of galaxies in evolving environments

The Effect of Modified Gravity on the Odds of the Bound Violations of the Turn-around Radii

Globular Cluster Systems in Brightest Cluster Galaxies. Iii. Beyond Bimodality

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