The Nature and Distribution of O VI Absorbers in the Vicinity of Galaxies

Details The Nature and Distribution of O VI Absorbers in the Vicinity of Galaxies The Nature and Distribution of O VI Absorbers in the Vicinity of Galaxies

Jul 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000hst..prop.8695t&link_type=abstract

HST Proposal ID #8695

Mathematics

Logic

Hst Proposal Id #8695 Quasar Absorption Lines And Igm

Scientific paper

Hydrodynamic cosmological simulations predict that at z 0, up to 50 of the baryons are in a shock-heated gaseous phase at 10^5 - 10^7 ^degreesK. Such gas may be easiest to detect via O VI absorption lines in the spectrum of a background QSO. We have recently discovered several low redshift O VI absorption line systems in the vicinity of groups of galaxies. In some cases these absorbers are highly ionized, and the O VI lines can be quite weak. In one case, low and intermediate ionization stages are detected, as well as O VI, with complex velocity structure. Here we propose to study PG1259+593 {z_ Q = 0.472} with the STIS E140M echelle mode to substantially improve the statistical base of observed O VI absorbers {including weak lines} for comparison with the cosmological models and to constrain the physical conditions and abundances in these systems and their relationships with galaxies. We will also obtain follow-up observations of PG0953+415. With these observations we will {1} measure the number of O VI absorbers per unit redshift {dN/dz} with a limiting equivalent width of W_Lambda 25 mAngstrom , {2} examine whether the O VI absorption arises in photoionized, collisionally ionized, or multiphase gas, {3} estimate the absorber metallicities, and {4} study the dependence of the absorber properties on the proximity of luminous galaxies. These observations will be useful for testing predictions from the cosmological models.

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