Assembly Bias: clues from a ΛCDM cosmology

Details Assembly Bias: clues from a ΛCDM cosmology Assembly Bias: clues from a ΛCDM cosmology

Oct 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011rmxac..40...17l&link_type=abstract

XIII Latin American Regional IAU Meeting (Eds. W. J. Henney & S. Torres-Peimbert) Revista Mexicana de Astronomía y Astrofísica (

Statistics

Cosmology: Theory, Dark Matter, Galaxies: Formation, Galaxies: Statistics, Large-Scale Structure Of Universe

Scientific paper

We present a new proxy for the overdensity peak height for which the large-scale clustering of haloes of a given mass does not vary significantly with the assembly history. The peak height, usually taken to be well represented by the virial mass, can instead be approximated by the mass inside spheres of different radii, which in some cases can be larger than the virial radius and therefore include mass outside the individual host halo. At large scales, i.e. in the two-halo regime, this model properly recovers the simple prescription where the bias responds to the height of the mass peak alone, in contrast to the usual definition (virial mass) that shows a strong dependence on additional halo properties such as formation time. The population of galaxies whose ``peak height'' changes with this new definition consists mainly of old stellar populations and are preferentially hosted by low-mass haloes located near more massive objects. The latter is in agreement with recent results which indicate that old, low-mass haloes would suffer truncation of mass accretion by nearby larger haloes or simply due to the high density of their surroundings, thus showing an assembly bias effect. The change in mass is small enough that the Sheth et al. (2001) mass function is still a good fit to the resulting distribution of new masses.

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