Galaxy correlations and the luminosity function

Details Galaxy correlations and the luminosity function Galaxy correlations and the luminosity function

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987mnras.227..115p&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 227, July 1, 1987, p. 115-121.

Statistics

Computation

23

Computational Astrophysics, Correlation, Functions (Mathematics), Galactic Structure, Luminosity, Galactic Nuclei, Red Shift

Scientific paper

By using the simple assumption that any excess of correlated galaxies seen close on the sky to a galaxy of known distance are also at the same distance, a galaxy luminosity function can be determined from the variation in excess number with magnitude. By averaging over the many 'center' galaxies, this luminosity function can be used to obtain good statistical accuracy at the faint end compared to the usual direct estimation from magnitude-limited surveys. Assuming a Schechter form for the luminosity function, a flat, alpha = -1 faint end slope is found. The characteristic magnitude is also determined reasonably accurately, a good fit being obtained only for -19.8 + or - 0.2. For typical values of the correlation amplitude, a normalization of 0.015 h-cubed/cu Mpc is found.

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