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Title:
A spectroscopic measure of the star formation rate density in dwarf galaxies at z ~ 1
Authors:
Davies, G. T.; Gilbank, David G.; Glazebrook, Karl; Bower, Richard G.; Baldry, I. K.; Balogh, Michael L.; Hau, G. K. T.; Li, I. H.; McCarthy, P.; Savaglio, S.
Affiliation:
AA(Institute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE), AB(Department of Physics and Astronomy, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada), AC(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia), AD(Institute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE), AE(Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD), AF(Department of Physics and Astronomy, University of Waterloo, Waterloo, Ontario N2L 3G1, Canada), AG(Institute for Computational Cosmology, Department of Physics, University of Durham, South Road, Durham DH1 3LE; Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia), AH(Centre for Astrophysics and Supercomputing, Swinburne University of Technology, PO Box 218, Hawthorn, VIC 3122, Australia), AI(Carnegie Observatories, 813 Santa Barbara Street, Pasadena, CA 91101, USA), AJ(Max-Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, 85748 Garching bei Munchen, Germany)
Publication:
Monthly Notices of the Royal Astronomical Society: Letters, Volume 395, Issue 1, pp. L76-L80. (MNRAS Homepage)
Publication Date:
05/2009
Origin:
MNRAS
MNRAS Keywords:
galaxies: dwarf, galaxies: evolution, galaxies: general
DOI:
10.1111/j.1745-3933.2009.00646.x
Bibliographic Code:
2009MNRAS.395L..76D

Abstract

We use a K-selected (22.5 < KAB < 24.0) sample of dwarf galaxies (8.4 < log(M*/Msolar) < 10) at 0.89 < z < 1.15 in the Chandra Deep Field-South to measure their contribution to the global star formation rate density (SFRD), as inferred from their [OII] flux. By comparing with [OII]-based studies of higher stellar mass galaxies, we robustly measure a turnover in the [OII] luminosity density at a stellar mass of M ~ 1010Msolar. By comparison with the [OII]-based SFRD measured from the Sloan Digital Sky Survey we confirm that, while the SFRD of the lowest mass galaxies changes very little with time, the SFRD of more massive galaxies evolves strongly, such that they dominate the SFRD at z = 1.
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