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Department of Physics

Staff profile

Publication details for Prof Carlton Baugh

Norberg, P. , Cole, S. , Baugh, C. M. , Frenk, C. S. , Baldry, I., Bland-Hawthorn, J. Bridges, T. Cannon, R., Colless, M., Collins, C. Couch, W. Cross, N. J. G. Dalton, G. De Propris, R. Driver, S. P. Efstathiou, G. Ellis, R. S. Glazebrook, K. Jackson, C. Lahav, O. Lewis, I., Lumsden, S. Maddox, S. Madgwick, D. Peacock, J. A. Peterson, B. A. Sutherland, W. & Taylor, K. (2002). The 2dF Galaxy Redshift Survey: the bJ-band galaxy luminosity function and survey selection function. Monthly Notices of the Royal Astronomical Society 336(3): 907-931.

Author(s) from Durham


We use more than 110 500 galaxies from the 2dF Galaxy Redshift Survey (2dFGRS) to estimate the bJ-band galaxy luminosity function at redshift z= 0, taking account of evolution, the distribution of magnitude measurement errors and small corrections for incompleteness in the galaxy catalogue. Throughout the interval −16.5 >MbJ− 5 log10h > −22, the luminosity function is accurately described by a Schechter function with MbJ− 5 log10h=−19.66 ± 0.07, α=−1.21 ± 0.03 and Φ= (1.61 ± 0.08) × 102h3 Mpc3, giving an integrated luminosity density of ρL= (1.82 ± 0.17) × 108h L Mpc3 (assuming an Ω0= 0.3, Λ0= 0.7 cosmology). The quoted errors have contributions from the accuracy of the photometric zero-point, from large-scale structure in the galaxy distribution and, importantly, from the uncertainty in the appropriate evolutionary corrections. Our luminosity function is in excellent agreement with, but has much smaller statistical errors than, an estimate from the Sloan Digital Sky Survey (SDSS) data when the SDSS data are accurately translated to the bJ band and the luminosity functions are normalized in the same way. We use the luminosity function, along with maps describing the redshift completeness of the current 2dFGRS catalogue, and its weak dependence on apparent magnitude, to define a complete description of the 2dFGRS selection function. Details and tests of the calibration of the 2dFGRS photometric parent catalogue are also presented.


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Figure A1. Map showing the variation of the parameter μwith position on the sky. The dependence of the redshift completeness on apparent magnitude is
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