Deep imaging of high redshift QSO fields below the Lyman limit. II - Number counts and colors of field galaxies

Details Deep imaging of high redshift QSO fields below the Lyman limit. II - Number counts and colors of field galaxies Deep imaging of high redshift QSO fields below the Lyman limit. II - Number counts and colors of field galaxies

Jun 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993aj....105.2017s&link_type=abstract

Astronomical Journal (ISSN 0004-6256), vol. 105, no. 6, p. 2017-2030, 2362.

Astronomy and Astrophysics

Astronomy

223

Astronomical Photography, Color, Faint Objects, Galaxies, Red Shift, Astronomical Photometry, Magnitude

Scientific paper

We present an analysis of the number counts and colors of faint galaxies to about 26.5 mag in the fields of two high Galactic latitude, very-high-redshift QSOs. We concentrate on the general properties of the field galaxies at faint magnitudes. In particular, we readdress the faint galaxy number counts and colors as a function of apparent magnitude and we reexamine the possible contribution of very-high-redshift galaxies to the faint samples. We find that the number counts to R = 26 are well fitted by the relation log N(m) = 0.31R + C. The G-band counts for the same galaxies are consistent with the same slope fainter than G about 23.5, but exhibit a much steeper slope at brighter magnitudes. At R = 25.5, the differential number counts have reached about 1.2 x 10 exp 5/sq deg; the same surface density of galaxies is reached at G = 26.5. We confirm the existence of a gradual 'blueing' trend of the field galaxies toward fainter apparent magnitude; however, the blueing trend appears to extend only as faint as G about 24, fainter than which both the (G-R) and (Un-G) colors appear to level off. The mean colors of faint galaxies are considerably redder than flat spectrum. There are essentially no objects to R = 26 which have spectral energy distributions which are bluer than flat spectrum. The potential contribution of very-high-redshift galaxies may have been underestimated in previous analyses; the current data are consistent with the same population of relatively luminous galaxies at z about 3 as exist at z about 0.7.

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