Astronomy and Astrophysics – Astrophysics
Scientific paper
2005-04-06
Mon.Not.Roy.Astron.Soc. 362 (2005) 337-348
Astronomy and Astrophysics
Astrophysics
13 pages, 9 figures, submitted to MNRAS. Minor changes, suggested by referee
Scientific paper
10.1111/j.1365-2966.2005.09309.x
We present a new, galaxy-halo model of large-scale structure, in which the galaxies entering a given sample are the fundamental objects. Haloes attach to galaxies, in contrast to the standard halo model, in which galaxies attach to haloes. The galaxy-halo model pertains mainly to the relationships between the power spectra of galaxies and mass, and their cross-power spectrum. With surprisingly little input, an intuition-aiding approximation to the galaxy-matter cross-correlation coefficient R(k) emerges, in terms of the halo mass dispersion. This approximation seems valid to mildly non-linear scales (k < ~3 h/Mpc), allowing measurement of the bias and the matter power spectrum from measurements of the galaxy and galaxy-matter power spectra (or correlation functions). This is especially relevant given the recent advances in precision in measurements of the galaxy-matter correlation function from weak gravitational lensing. The galaxy-halo model also addresses the issue of interpreting the galaxy-matter correlation function as an average halo density profile, and provides a simple description of galaxy bias as a function of scale.
Gnedin Nickolay Y.
Hamilton Andrew J. S.
Neyrinck Mark C.
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