Volume 589, May 2016
|Number of page(s)||3|
|Section||Cosmology (including clusters of galaxies)|
|Published online||11 April 2016|
The extended Baryon Oscillation Spectroscopic Survey: Variability selection and quasar luminosity function (Corrigendum)
CEA, Centre de Saclay,
2 INAF−Osservatorio Astronomico di Trieste, via G. B. Tiepolo 11, 34131 Trieste, Italy
3 UPMC-CNRS, UMR7095, Institut d’Astrophysique de Paris, 75014 Paris, France
4 Department of Physics and Astronomy, University of Utah, Salt Lake City, UT 84112, USA
5 Steward Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85 721, USA
6 Department of Physics and Astronomy, University of Wyoming, Laramie, WY 82 071, USA
7 Department of Astronomy and Space Science, Sejong University, 143-747 Seoul, Korea
8 Lawrence Berkeley National Laboratory, 1 Cyclotron Road, Berkeley, CA 94 720, USA
9 Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16 802, USA
10 Institute for Gravitation and the Cosmos, The Pennsylvania State University, University Park, PA 16802, USA
11 Instituto de Astrofisica de Canarias (IAC), 38200, La Laguna, Tenerife, Spain
12 Universidad de La Laguna (ULL), Dept. Astrofisica, 38206, La Laguna, Tenerife, Spain
13 Center for Cosmology and Particle Physics, New York University, New York, NY 10 003, USA
Key words: quasars: general / large-scale structure of Universe / surveys / errata, addenda
The correct tables are published below.
Predicted differential quasar counts over 15.5 <g< 25 and 0 <z< 6 for a survey covering 10 000 deg2, based on our best-fit PLE or PLE+LEDE luminosity function model.
Predicted differential quasar counts over 15.5 <r< 24 and 0 <z< 6 for a survey covering 10 000 deg2, based on our best-fit PLE or PLE+LEDE luminosity function model.
© ESO, 2016
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