2009/02/23 by G. T. Davies, David Gilbank, Karl Glazebrook +10
Physics and Astronomy · #Astronomy and Astrophysical Research #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph.CO
paper · pdf · doi:10.1111/j.1745-3933.2009.00646.x
Accepted for publication in MNRAS Letters. 6 pages, 2 figures
arxiv created 2009/02/23 · openalex publication_date 2009/03/17 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/29
Abstract We use a K-selected (22.5 < KAB < 24.0) sample of dwarf galaxies (8.4 < log(M*/M⊙) < 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 [O ii] flux. By comparing with [O ii]-based studies of higher stellar mass galaxies, we robustly measure a turnover in the [O ii] luminosity density at a stellar mass of M∼ 1010 M⊙. By comparison with the [O ii]-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.