2017/10/31 by Ivana Damjanov, H. Jabran Zahid, Margaret J. Geller +2 · 54 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Field galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Population #Redshift #Redshift survey #Sky #Spectrograph #Stellar mass #Stellar population #Stellar, planetary, and galactic studies #Velocity dispersion #astro-ph.GA
paper · pdf · doi:10.3847/1538-4365/aaa01c
published in The Astrophysical Journal Supplement Series 234(2), 21 (Institute of Physics) · ApJS accepted. Complete Table 2 in a machine-readable format is available at https://www.cfa.harvard.edu/~hzahid/Data_files/Table2_MR.dat
openalex created_date 2017/10/20 · arxiv created 2017/11/30 · openalex publication_date 2018/01/25 · arxiv updated 2018/02/07 · openalex updated_date 2026/08/06
Abstract We describe the hCOSMOS redshift survey of the COSMOS field conducted with the Hectospec spectrograph on the MMT. In the central 1 deg 2 , the hCOS20.6 subset of the survey is complete to a limiting magnitude r = 20.6. The hCOSMOS survey includes 1701 new redshifts in the COSMOS field. We also use the total of 4362 new and remeasured objects to derive the age-sensitive index over the entire redshift interval . For 85% of the quiescent galaxies in hCOS20.6, we measure the central line-of-sight velocity dispersion. To explore potential uses of this survey, we combine previously measured galaxy sizes, profiles, and stellar masses with the spectroscopy. The comparison reveals the known relations among structural, kinematic, and stellar population properties. We also compare redshift and distributions of hCOS20.6 galaxies with SHELS; a complete spectroscopic survey of 4 deg 2 observed to the same depth. The redshift distributions in the two fields are very different, but the distribution is remarkably similar. The relation between velocity dispersion and stellar mass for massive hCOS20.6 galaxies is consistent with the local relation from the Sloan Digital Sky Survey. Using measured velocity dispersions, we test a photometric proxy calibrated to galaxies in the local universe. The systematic differences between the measured and photometric proxy velocity dispersions are correlated with galaxy dynamical and stellar population properties highlighting the importance of direct spectroscopic measurements.