Modelling the number density of H<i>α</i>emitters for future spectroscopic near-IR space missions
L. PozzettiINAF – Osservatorio Astronomico di Bologna, via Ranzani 1, 40127 Bologna, ItalyC. M. HirataCenter for Cosmology and Astroparticle Physics, The Ohio State University, 191 West Woodruff Lane, Columbus, Ohio 43210, USAJ. E. GeachCentre for Astrophysics Research, Science and Technology Research Institute, University of Hertfordshire, Hatfield, AL10 9AB, UKA. CimattiDipartimento di Fisica e Astronomia, Università di Bologna, viale Berti Pichat 6/2, 40127 Bologna, ItalyC. BaughInstitute for Computational Cosmology (ICC), Department of Physics, Durham University, South Road, Durham, DH1 3LE, UKO. CucciatiDipartimento di Fisica e Astronomia, Università di Bologna, viale Berti Pichat 6/2, 40127 Bologna, ItalyA. MersonDepartment of Physics and Astronomy, University College London, Gower Street, London, WC1E 6BT, UKP. NorbergInstitute for Computational Cosmology (ICC), Department of Physics, Durham University, South Road, Durham, DH1 3LE, UKD. ShiInstitute for Computational Cosmology (ICC), Department of Physics, Durham University, South Road, Durham, DH1 3LE, UK
2016en
ABI
Annotatsiya
Context. The future space missions Euclid and WFIRST-AFTA will use the Hα emission line to measure the redshifts of tens of millions of galaxies. The Hα luminosity function at z> 0.7 is one of the major sources of uncertainty in forecasting cosmological constraints from these missions.
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