Mathematics – Logic
Scientific paper
Jan 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995phdt.........1d&link_type=abstract
Thesis (PH.D.)--PRINCETON UNIVERSITY, 1995.Source: Dissertation Abstracts International, Volume: 56-02, Section: B, page: 0869.
Mathematics
Logic
10
Luminosity, Galaxy Evolution
Scientific paper
I present results of a CCD survey for ULSBs that reaches central surface brightnesses of 27 mag/arcsec ^2 in V. I have analyzed 17 degree ^2 of drift-scan data, and found 35 candidate ULSB's with central surface brightnesses fainter than 23 mag/arcsec^2 and with angular scale lengths larger than 3". The data is consistent with these galaxies being local and uniformly distributed, and with there being constant number density of galaxies in every surface brightness interval between 23 and 27 mag/arcsec ^2. The implied number densities are over a hundred times larger than the number density in L > 0.1L_{*} galaxies, and the luminosity density is anywhere between 15% and 110% of the luminosity density in cataloged galaxies. The associated mass density is likely to be even larger, due to the likely decrease in star formation efficiency with decreasing surface density. Therefore, ULSBs are likely to be the most numerous type of galaxy, and probably make a significant contribution to the mass of the universe. ULSBs are much less correlated than bright galaxies on small angular scales (theta = 0.1 ^circ). The population of ULSBs is in many ways consistent with the predicted properties of the low mass end of the galaxy mass distribution. I also show that the observed surface brightnesses and angular sizes of distant clusters are comparable to the properties of local low-surface brightness galaxies. Thus, surveys for ULSBs are also capable of finding candidate high-redshift clusters. I calculate the number of clusters per square degree that are expected, and show that, for almost any cosmological model, the expected detection rates are high enough for this to present an efficient means to detect clusters. The ULSB survey bears this out, and has uncovered many strong cluster candidates. Finally, the thesis contains a discussion of the luminosity density at z = 0.4 as it compares to the luminosity density at z = 0. I show that the luminosity density at z = 0.4 is 3-5 times larger than the luminosity density locally, and use this to argue that merging of the large numbers of galaxies visible at z = 0.4 cannot explain the dramatic reduction in the number of galaxies seen today. The apparent difference in luminosity density may in some part reflect that LSBs are represented in much greater numbers in deep surveys of high redshift galaxies than they are in shallow large-area surveys of local galaxies.
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