Astronomy and Astrophysics – Astronomy
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aas...182.6705l&link_type=abstract
American Astronomical Society, 182nd AAS Meeting, #67.05; Bulletin of the American Astronomical Society, Vol. 25, p.914
Astronomy and Astrophysics
Astronomy
Scientific paper
Monte-Carlo simulations of three dimensional galaxy distributions are performed to study the photometric properties of evolving galaxy populations in the optical and near infrared bands to high redshifts. Galaxies are spatially distributed in a range of cluster to field environments. Details of individual galaxy properties, including luminosities, morphologies, disk-to-bulge ratios, and size distributions are simulated to match local observed galaxy properties. Galaxies have evolving spectral energy distributions that include both stellar emission and internal dust absorption and re-emission. The simulations result in two dimensional galaxy distributions on the sky that can be compared to the observed deep images in the blue and near-infrared bands. In this paper, the first of a series, we present our baseline model in which galaxy numbers are conserved, and in which no explicit ``starburst'' population is included. We find that our baseline models, with a formation redshift, z_f, of 1000, and H_o=50, are able to reproduce the observed blue counts to b_j=22, independent of the value of Omega_o , and also to provide a satisfactory fit to the observed blue band redshift distributions, but for neither value of Omega_o do we achieve an acceptable fit to the fainter blue counts. In the K-band, we fit the number counts to the limit of the present day surveys only for an Omega_o =0 cosmology. We investigate the effect on the model fits of varying H_o, z_f, and the local luminosity function. Reducing z_f to =~ 5 in a low Omega_o universe improves the fit to the faintest photometric blue data without any need to invoke a new population of galaxies, substantial merging, or a significant starburst galaxy population. For an Omega_o =1 universe, however, reducing z_f is less successful at fitting the blue band counts, and has little effect at all at K. Varying the parameters of the local luminosity function can also have a significant effect. In particular the steep low end slope of the local luminosity function of Franceschini et al. allows an acceptable fit to the b_j<= 25 counts for Omega_o =1, but is incompatible with Omega_o =0.
Chokshi Arati
de Zotti Gainfranco
Lonsdale Carol
Mazzei Paola
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