The Luminosity Function Normalization and the Faint Galaxy Counts

Details The Luminosity Function Normalization and the Faint Galaxy Counts The Luminosity Function Normalization and the Faint Galaxy Counts

Dec 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003aas...20314612c&link_type=abstract

American Astronomical Society Meeting 203, #146.12; Bulletin of the American Astronomical Society, Vol. 36, p.591

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We present a study of the B-band galaxy counts as a function of morphological type measured from publicly available images from three recent wide field ground-based surveys. These new data with B≲18 mag are then combined with the fainter HST surveys (19≲B≲27 mag) in an effort to more fully understand the faint blue galaxy excess and the distribution of Hubble types for the faintest classifiable galaxies. This new combination of data, along with new models which incorporate the currently favored set of cosmological parameters, are used to study the possible need to re-normalize the models at B=18 mag for the E/S0, Sabc, and Sd/Irr populations both separately and as a whole.
The combined data do not suggest that the counts of any of the individual morphological types or the combination of all types need to be renormalized, because the models fit the bright (B≲18 mag) data reasonably well. This important result strengthens the interpretations that can be made with regards to galaxy evolution. With the models now anchored at the bright end, we show that the faintest counts suggest a similar amount of luminosity evolution for all types (parametrized by β =2), with the Sd/Irr class perhaps requiring slightly stronger luminosity evolution than the earlier types. Alternative interpretations of the data are also discussed.
Funding for various HST related aspects of this project was provided by NASA grants GO.6609.01.95A, AR.6385.01.95A, & AR.7534.02.96A from STScI, which is operated by AURA, Inc., under NASA contract NAS5-26555. The ground-based work was supported by NASA/JWST grant NAG5-12460.

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