Near Infrared Faint Galaxies in the Subaru Deep Field: Comparing the Theory with Observations for Galaxy Counts, Colors, and Size Distributions to K=24.5

Details Near Infrared Faint Galaxies in the Subaru Deep Field: Comparing the Theory with Observations for Galaxy Counts, Colors, and Size Distributions to K=24.5 Near Infrared Faint Galaxies in the Subaru Deep Field: Comparing the Theory with Observations for Galaxy Counts, Colors, and Size Distributions to K=24.5

2001-06-19

arxiv.org/abs/astro-ph/0106323v2

Astronomy and Astrophysics

Astrophysics

References updated. Accepted by ApJ

Scientific paper

10.1086/322338

Galaxy counts in the K band, (J-K)-colors, and apparent size distributions of faint galaxies in the Subaru Deep Field (SDF) down to K~24.5 were studied in detail. Special attention has been paid to take into account various selection effects including the cosmological dimming of surface brightness, to avoid any systematic bias which may be the origin of controversy in previously published results. We also tried to be very careful about systematic model uncertainties; we present a comprehensive surveys of these systematic uncertainties and dependence on various parameters. We found that the pure luminosity evolution (PLE) model is well consistent with all the SDF data down to K~22.5, without any evidence for number or size evolution in a low-density, Lambda-dominated flat universe which is now favored by various cosmological observations. If the popular Lambda-dominated universe is taken for granted, our result then gives a strong constraint on the number evolution of giant elliptical or early-type galaxies to z~1-2 which must be met by any models in the hierarchically clustering universe, since such galaxies are the dominant population in this magnitude range (K<~22.5). In the fainter magnitude range of K>~22.5, we found a slight excess of observed counts over the prediction of the PLE model when elliptical galaxies are treated as a single population. We suggest that this discrepancy reflects some number evolution of dwarf galaxies and/or the distinct populations of giant and dwarf elliptical galaxies which have been known for local elliptical galaxies.

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