Dust obscuration and QSO luminosity functions

Details Dust obscuration and QSO luminosity functions Dust obscuration and QSO luminosity functions

Oct 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994pasj...46..461t&link_type=abstract

PASJ: Publications of the Astronomical Society of Japan (ISSN 0004-6264), vol. 46, no. 5, p. 461-471

Astronomy and Astrophysics

Astronomy

1

Astronomical Models, Chemical Evolution, Cosmic Dust, Galactic Evolution, Luminosity, Occultation, Optical Thickness, Quasars, Spiral Galaxies, Stellar Color, Black Holes (Astronomy), Red Shift

Scientific paper

We consider two models of quasi-stellar object (QSO) luminosity functions (the number-density evolution model and the dust-obscuration model) in connection with the observational QSO number counts. For the latter model, we first consider the obscuration by dust in intervening spiral galaxies and discuss our calculations of the total optical depths and color excesses. Calculations were performed taking into account the chemical evolution of galaxies in three cosmological models: (omega0, lambda0) = (1.0, 0), (0.1, 0), and (0.1, 0.9). Next, for the two models we derive the number counts of QSOs as functions of the apparent magnitudes at the B band and make parameter fittings by comparing them with the observational counterparts. As a result, we find that: (1) the above two model of luminosity functions can be fitted by adjusting the model parameters, (2) in the dust-obscuration model the size of dusty regions in the (0.1, 0.9) model is by about 30% smaller than that in the (1.0, 0) model, and (3) the sizes decrease by 10 - 20% due to chemical evolution. In order to discriminate observationally between the two models, moreover, we derive theoretical number counts at the other bands, such as the I and K bands, and compare them with those at the B band.

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