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Paper   IPM / Astronomy / 16111
School of Astronomy
  Title:   Kinematic unrest of low mass galaxy groups
1.  G. Gozaliasl
2.  A. Finoguenov
3.  H. Khosroshahi
4.  C. Laigle
5.  C. C. Kirkpatrick
6.  K. Kiiveri
7.  J. Devriendt
8.  Y. Dubois
9.  J. Ahoranta
  Status:   Published
  Journal: Astronomy & Astrophysics
  Vol.:  635
  Year:  2020
  Supported by:            ipm IPM
In an effort to better understand the formation of galaxy groups, we examine the kinematics of a large sample of spectroscopically confirmed X-ray galaxy groups in the Cosmic Evolution Survey with a high sampling of galaxy group members up to z = 1. We compare our results with predictions from the cosmological hydrodynamical simulation of HORIZON-AGN. Using a phase-space analysis of dynamics of groups with halo masses of M200c ∼ 1012.6 - 1014.50 M☉, we show that the brightest group galaxies (BGG) in low mass galaxy groups (M200c < 2 × 1013 M☉) have larger proper motions relative to the group velocity dispersion than high mass groups. The dispersion in the ratio of the BGG proper velocity to the velocity dispersion of the group, σBGG/σgroup, is on average 1.48 ± 0.13 for low mass groups and 1.01 ± 0.09 for high mass groups. A comparative analysis of the HORIZON-AGN simulation reveals a similar increase in the spread of peculiar velocities of BGGs with decreasing group mass, though consistency in the amplitude, shape, and mode of the BGG peculiar velocity distribution is only achieved for high mass groups. The groups hosting a BGG with a large peculiar velocity are more likely to be offset from the Lx - σv relation; this is probably because the peculiar motion of the BGG is influenced by the accretion of new members.

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