Are brightest halo galaxies central galaxies?
Article first published online: 29 SEP 2010
© 2010 The Authors. Journal compilation © 2010 RAS
Monthly Notices of the Royal Astronomical Society
Volume 410, Issue 1, pages 417–431, January 2011
How to Cite
Skibba, R. A., van den Bosch, F. C., Yang, X., More, S., Mo, H. and Fontanot, F. (2011), Are brightest halo galaxies central galaxies?. Monthly Notices of the Royal Astronomical Society, 410: 417–431. doi: 10.1111/j.1365-2966.2010.17452.x
- Issue published online: 14 DEC 2010
- Article first published online: 29 SEP 2010
- Accepted 2010 July 29. Received 2010 July 28; in original form 2009 December 17
- methods: statistical;
- galaxies: clusters: general;
- galaxies: haloes;
- galaxies: kinematics and dynamics;
- dark matter
It is generally assumed that the central galaxy in a dark matter halo, that is the galaxy with the lowest specific potential energy, is also the brightest halo galaxy (BHG), and that it resides at rest at the centre of the dark matter potential well. This central galaxy paradigm (CGP) is an essential assumption made in various fields of astronomical research. In this paper, we test the validity of the CGP using a large galaxy group catalogue constructed from the Sloan Digital Sky Survey. For each group, we compute two statistics, and , which quantify the offsets of the line-of-sight velocities and projected positions of brightest group galaxies relative to the other group members. By comparing the cumulative distributions of and to those obtained from detailed mock group catalogues, we rule out the null hypothesis that the CGP is correct. Rather, the data indicate that in a non-zero fraction fBNC(M) of all haloes of mass M the BHG is not the central galaxy, but instead a satellite galaxy. In particular, we find that fBNC increases from ∼0.25 in low-mass haloes (1012 h−1≤M≲ 2 × 1013 h−1 M⊙) to ∼0.4 in massive haloes (M≳ 5 × 1013 h−1 M⊙). We show that these values of fBNC are uncomfortably high compared to predictions from halo occupation statistics and from semi-analytical models of galaxy formation. We end by discussing various implications of a non-zero fBNC(M), with an emphasis on the halo masses inferred from satellite kinematics.