1997/10/01 by Julianne J. Dalcanton · 4 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Fundamental plane (elliptical galaxies) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Luminosity #Luminosity function #Normalization (sociology) #Point spread function #Redshift #Scientific Research and Discoveries #Source counts #astro-ph
paper · pdf · doi:10.1086/305256
31 pages, including 12 pages of figures. LaTex with aaspp4.sty. Accepted to the Astrophysical Journal
arxiv created 1997/10/01 · openalex publication_date 1998/03/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Both the detection of galaxies and the derivation of the luminosity function depend upon isophotal magnitudes, implicitly in the first case and explicitly in the latter. However, unlike perfect point sources, the fraction of a galaxy's light contained within the limiting isophote is a function of redshift, owing to the combined effects of the point-spread function and cosmological dimming. This redshift variation in the measured isophotal luminosity can strongly affect the derived luminosity function. Using simulations that include the effects of seeing upon both disk and elliptical galaxies, we explore the size of the systematic biases that can result from ignoring the redshift variation in the fraction of detected light. We show that the biases lead to underestimates in the normalization of the luminosity function, as well as changes in shape. The size of the bias depends upon redshift, and thus can mimic galaxy evolution. Surprisingly, these biases can be extremely large without affecting ⟨ V / V max ⟩. However, these biases can be detected in the full distribution of V / V max and in fact may have already been detected in recent surveys. Because the systematic biases result from the redshift variation in the fraction of lost light, the biases are not significant when the fraction of lost light is always small over the entire survey volume, for all galaxy types. However, as modern galaxy surveys now reach higher redshifts, lower surface brightnesses, and smaller angular sizes, the effects of seeing and galaxy visibility are becoming increasingly important and need to be taken into account. We show that the expected biases are not necessarily eliminated when using aperture magnitudes, Faint Object Classification and Analysis System "total" magnitudes, or Kron magnitudes, but may be reduced significantly if Petrosian magnitudes are used. These considerations may also apply to samples of clusters selected in X-rays.