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A Possible Effect of the Period of Galaxy Formation on the Angular Correlation Function | | Tomoya Ogawa
; Boudewijn F. Roukema
; Kazuyuki Yamashita
; | | Date: |
25 Mar 1997 | | Journal: | Astrophys.J. 484 (1997) 53 | | Subject: | astro-ph | | Affiliation: | Chiba Univ.), Boudewijn F. Roukema (Nat. Ast. Obs. Japan) and Kazuyuki Yamashita (Chiba Univ. | | Abstract: | During the epoch of galaxy formation, the formation of the first galaxies in regions of high overdensity may lead to an initial amplitude of the spatial correlation function of galaxies, $xi_0,$ much higher than that expected in linear perturbation theory. This initially high ``bias’’ would consequently decrease to the near-unityvalues expected from local observations. Such a ``Decreasing Correlation Period’’ (DCP), detected in N-body simulations under certain conditions by several authors, is parametrised in a simple way, ending at a ``transition’’ redshift $z_t.$ Consequences on $w_0,$ the amplitude of the angular correlation function of faint galaxies (for a fixed apparent magnitude range), have been estimated. The sensitivity of $w_0$ to $z_t,$ and how this is affected by the redshift distribution of the galaxies in the sample, by low redshift spatial correlation function behaviour, by cosmology, and by the rate at which $xi_0$ decreases during the DCP, are shown and discussed. This simple model is intended as a first exploration of the effects of the DCP for a likely range of parameter space. Comparison with the Hubble Deep Field (HDF) estimate of $w_0$ (Villumsen et al. 1996) indicates that the DCP is compatible with observation for values of $z_t$ in the theoretically expected range $z_t gtapprox 1.$ However, tighter observational constraints on the HDF redshift distribution and on low redshift correlation function growth will be needed either to detect the DCP unambiguously or to constrain $z_t$ to redshifts greater than those of galaxies in existing surveys. | | Source: | arXiv, astro-ph/9703158 | | Services: | Forum | Review | PDF | Favorites | |
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