Mass–Velocity Dispersion Relation in HIFLUGCS Galaxy Clusters

  title={Mass–Velocity Dispersion Relation in HIFLUGCS Galaxy Clusters},
  author={Yong Tian and Po-Chieh Yu and Pengfei Li and Stacy S. McGaugh and Chung-Ming Ko},
  journal={The Astrophysical Journal},
We investigate the mass–velocity dispersion relation (MVDR) in 29 galaxy clusters in the HIghest X-ray FLUx Galaxy Cluster Sample (HIFLUGCS). We measure the spatially resolved, line-of-sight velocity dispersion profiles of these clusters, which we find to be mostly flat at large radii, reminiscent of the rotation curves of galaxies. We discover a tight empirical relation between the baryonic mass M bar and the flat velocity dispersion σ of the member galaxies, i.e., MVDR, log(Mbar/M⊙)=4.1−0.4+0… 
4 Citations
Analytic radial acceleration relation for galaxy clusters
Recently, a tight correlation between the dynamical radial acceleration and the baryonic radial acceleration in galaxies - the radial acceleration relation - has been discovered. This has been
On a Generalized Mass-Velocity Relation for Disk Galaxies and Galaxy Clusters
We consolidate the BFJ and BTF (MVD) relations into a generalized Scaling Mass Velocity Relation applicable to both pressure-supported galaxy clusters and rotation-supported galaxies. Unlike MOND
Mass–Velocity Dispersion Relation in MaNGA Brightest Cluster Galaxies
We investigate a kinematic scaling relation between the baryonic mass and the flat velocity dispersion, i.e., mass–velocity dispersion relation (MVDR), from the brightest cluster galaxies (BCGs) to


Cluster–galaxy weak lensing
Weak gravitational lensing of background galaxies provides a direct probe of the projected matter distribution in and around galaxy clusters. Here, we present a self-contained pedagogical review of
MOND vs. dark matter in light of historical parallels
  • M. Milgrom
  • Physics
    Studies in History and Philosophy of Science Part B: Studies in History and Philosophy of Modern Physics
  • 2020
The Radial Acceleration Relation in CLASH Galaxy Clusters
The radial acceleration relation (RAR) in galaxies describes a tight empirical scaling law between the total acceleration $g_\mathrm{tot}(r)=GM_\mathrm{tot}(<r)/r^2$ observed in galaxies and that
Stellar and Total Baryon Mass Fractions in Groups and Clusters Since Redshift 1
We investigate if the discrepancy between estimates of the total baryon mass fraction obtained from observations of the cosmic microwave background (CMB) and of galaxy groups/clusters persists when a
Living Reviews in Relativity
  • AJ, 98,
  • 2012
ADAP grant 80NSSC19k0570 and NSF PHY1911909
  • 2016
Fitting the radial acceleration relation to individual SPARC galaxies
Galaxies follow a tight radial acceleration relation (RAR): the acceleration observed at every radius correlates with that expected from the distribution of baryons. We use the Markov chain Monte
Modified Newtonian Dynamics (MOND): Observational Phenomenology and Relativistic Extensions
It is shown that many of these puzzling observations are predicted by one single relation — Milgrom’s law — involving an acceleration constant a0 on the order of the square-root of the cosmological constant in natural units.
The baryonic Tully-Fisher relation (BTFR) is an empirical relation between baryonic mass and rotation velocity in disk galaxies. It provides tests of galaxy formation models in ΛCDM and of
Isothermal spheres in the modified dynamics
On considere des spheres isothermes soumises a leur propre gravitation (isotrope et anisotrope) en utilisant une dynamique qui differe de la newtonienne dans la limite des petites accelerations. On