Hostname: page-component-7479d7b7d-fwgfc Total loading time: 0 Render date: 2024-07-14T01:54:31.889Z Has data issue: false hasContentIssue false

The quasar clustering and its evolution in a semi-analytic model based on ultra high-resolution N-body simulations

Published online by Cambridge University Press:  17 August 2016

Taira Oogi
Affiliation:
Faculty of Education, Bunkyo University, 3337 Minami-Ogishima, Koshigaya-shi, Saitama 343-8511, Japan email: oogi@koshigaya.bunkyo.ac.jp
Motohiro Enoki
Affiliation:
Faculty of Business Administration, Tokyo Keizai University, Japan
Tomoaki Ishiyama
Affiliation:
Institute of Management and Infomation Technologies, Chiba University, Japan
Masakazu A. R. Kobayashi
Affiliation:
Research Center for Space and Cosmic Evolution, Ehime University, Japan
Ryu Makiya
Affiliation:
Institute of Astronomy, the University of Tokyo, Japan
Masahiro Nagashima
Affiliation:
Faculty of Education, Bunkyo University, 3337 Minami-Ogishima, Koshigaya-shi, Saitama 343-8511, Japan email: oogi@koshigaya.bunkyo.ac.jp
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

We investigate clustering properties of quasars using a new version of our semi-analytic model of galaxy and quasar formation with state-of-the-art cosmological N-body simulations (Ishiyama et al. 2015; Oogi et al. 2015). We assume that a major merger of galaxies triggers quasar activity. We find that the quasar bias does not depend significantly on the quasar luminosity, similar to observed trends. This result reflects the fact that quasars with a fixed luminosity have various Eddington ratios and thus have various host halo masses that primarily determine the quasar bias. The quasar bias increases with redshift, which is in qualitative agreement with observations. Our bias value is lower than the observed values at high redshifts, implying that we need some mechanisms that make quasars inactive in low-mass haloes and/or that make them more active in high-mass haloes.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2016 

References

Ishiyama, T., Enoki, M., Kobayashi, M. A. R., Makiya, R., Nagashima, M., & Oogi, T. 2015, PASJ, 67, 61 CrossRefGoogle Scholar
Oogi, T., Enoki, M., Ishiyama, T., Kobayashi, M. A. R., Makiya, R., & Nagashima, M. 2015, MNRAS (Letters), acceptedGoogle Scholar
Sheth, R. K., Mo, H. J., & Tormen, G. 2001, MNRAS, 323, 1 Google Scholar