The bivariate brightness function of galaxies and a demonstration of the impact of surface brightness selection effects on luminosity function estimations

Nicholas Cross, Simon P. Driver

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59 Citations (Scopus)

Abstract

In this paper we fit an analytic function to the bivariate brightness distribution (BBD) of galaxies. It is a combination of the classical Schechter Function convolved with a Gaussian distribution in surface brightness: thus incorporating the luminosity-surface brightness correlation as seen in many recent data sets. We fit this function to a recent measurement of the BBD based on 45 000 galaxies from the Two-Degree Field Galaxy Redshift Survey. The parameters for the best-fitting model are φ* = (0.0206 ± 0.0009)h3 Mpc-3, M*bj - 5 log h = (-19.72 ± 0.04) mag, α = -1.05 ± 0.02, βμ = 0.281 ± 0.007, μ*e, bj = (22.45 ± 0.01) mag arcsec-2 and σμ = 0.517 ± 0.006. φ*, M*bj and α equate to the conventional Schechter parameters. βμ is the slope of the luminosity-surface brightness correlation, μ*e, bj is the characteristic effective surface brightness at M*bj and σμ is the width of the Gaussian. Using a BBF we explore the impact of the limiting detection isophote on classical measures of the galaxy luminosity distribution. We demonstrate that if isophotal magnitudes are used then errors of ΔM*bj ∼ 0.62 mag, Δφ* ∼ 26 per cent and Δα ∼ 0.04 are likely for μlim, bj = 24.0 mag arcsec-2. If Gaussian corrected magnitudes are used these change to ΔM*bj ∼ 0.38mag, Δφ* ∼ 11 per cent and Δα < 0.01 for μlim, bj = 24.0 mag arcsec-2. Hence while the faint-end slope, α, appears fairly robust to surface brightness issues, both the M* and φ* values are highly dependent. The range over which these parameters were seen to vary is fully consistent with the scatter in the published values, reproducing the range of observed luminosity densities (1.1 < jbj < 2.2 × 108hL⊙ Mpc-3). If total magnitudes are recovered then there is no change in the luminosity function within the errors for μlim, bj = 24.0 mag arcsec-2. We conclude that surface brightness selection effects are primarily responsible for this variation. After due consideration of these effects, we derive a value of jbj = 2.16 × 108hL⊙ Mpc-3.

Original languageEnglish
Pages (from-to)579-587
Number of pages9
JournalMonthly Notices of the Royal Astronomical Society
Volume329
Issue number3
DOIs
Publication statusPublished - 21 Jan 2002
Externally publishedYes

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