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2002MNRAS.335..712T - Mon. Not. R. Astron. Soc., 335, 712-732 (2002/September-3)
The faint end of the galaxy luminosity function.
TRENTHAM N. and TULLY R.B.
Abstract (from CDS):
In all cases, there are far fewer dwarfs than the numbers of low-mass haloes anticipated by cold dark matter theory. The mean logarithmic slope of the luminosity function between MR=-1018 and MR=-1010 is α≃-1.2, far shallower than the cold dark matter mass function slope of α≃-1.8. We would therefore need to be missing about 90 per cent of the dwarfs at the faint end of our sample in all the environments we study to achieve consistency with CDM theory. It is unlikely that such large numbers of dwarfs are missed because (i) the data are deep enough that we are sensitive to very low surface brightness galaxies, and (ii) the seeing is good enough that we can have some confidence in our ability to distinguish high surface brightness dwarfs from background galaxies brighter than R = 22.5. One caveat is that we miss compact members taken to be background galaxies, but such objects (like M32) are thought to be rare.
Abstract Copyright: RAS
Journal keyword(s): galaxies: clusters: individual: Virgo - galaxies: clusters: individual: NGC 1407 Group - galaxies: clusters: individual: Leo Group - galaxies: clusters: individual: Coma I Group - galaxies: clusters: individual: NGC 1023 Group - galaxies: luminosity function, mass function.
VizieR on-line data: <Available at CDS (J/MNRAS/335/712): tables.dat>
Nomenclature: Table 2: [TT2002] Virgo NN (Nos 1-99). Table 3: [TT2002] NGC 1407 NN (Nos 1-58). Table 4: [TT2002] Coma I NN (Nos 1-38). Table 5: [TT2002] Leo NN (Nos 1-26). Table 6: [TT2002] NGC 1023 NN (Nos 1-28).
Simbad objects: 279