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Deep optical galaxy counts with the Keck Telescope | | Ian Smail
; David W. Hogg
; Lin Yan
; Judy Cohen
; | | Date: |
17 Jun 1995 | | Subject: | astro-ph | | Affiliation: | OCIW), David W. Hogg (Caltech), Lin Yan (Caltech), and Judy Cohen (Caltech | | Abstract: | We present faint galaxy counts from deep $VRI$ images obtained with the Keck Telescope. These images reach $Rsim27$ in median seeing FWHM $sim 0.5$--0.6 arcsec and we detect a integrated galaxy number density of $7 imes 10^{5}$ degree$^{-2}$, equivalent to $3 imes 10^{10}$ galaxies in the observable Universe. In addition we present median galaxy colors as a function of magnitude; bluing trends are visible in all colors to $Rsim 24.5$. Fainter than $Rsim24.5$, however, the typical VR color becomes redder again, VI remains constant, and RI becomes yet bluer. These trends are consistent with the $VRI$ count slopes, implying a decrease in the $V$ slope at the faintest levels, which our data supports. Taking advantage of our good seeing we also present median half-light radii for faint galaxies, these show a steady decline at fainter magnitudes, leading to an intrinsic half-light radius of $sim 0.2$ arcsec for a typical $Rsim25.5$--26 galaxy. Irrespective of the redshift distribution, the extremely high galaxy surface densities and their small intrinsic sizes are consistent with a scenario in which the majority of the very faint field population are dwarf galaxies or sub-galactic units. | | Source: | arXiv, astro-ph/9506095 | | Services: | Forum | Review | PDF | Favorites | |
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