Computer Science
Scientific paper
Jul 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008hst..prop11585c&link_type=abstract
HST Proposal ID #11585. Cycle 17
Computer Science
Scientific paper
The distribution of the gaseous intergalactic medium {IGM} around galaxies is fundamentally important to our understanding of galaxy evolution. Simulations suggest that 'feedback' - the return of gas and radiation to the IGM via active galactic nuclei or star-formation-driven winds - is an important part of galaxy formation and a possible way to enrich the IGM with metals. We propose to use COS to observe the IGM towards the brightest known group of three QSOs {z=0.96, 0.96 and 0.73} separated by a few arcminutes on the sky. Using far-UV spectra of the Lyman-alpha forest region at resolutions > 20000, we will detect both the cooler photo-ionized IGM at 10,000K using narrow HI absorbers, and the warm-hot intergalactic medium {WHIM} at 100,000 K using OVI and broad HI absorbers over a redshift range of 0 < z < 0.48 {HI} and 0.17 < z < 0.73 {OVI}. The immediate objective is to compare the distribution of the WHIM and cooler IGM to the distribution of galaxies in the same field over redshifts from 0 to 0.6, and scales from 100 kpc to 1 Mpc. In particular we will look for signs of feedback, such as metal-enriched WHIM gas close to galaxies. The three sight-lines with separations of 400 kpc to 1 Mpc will allow us to constrain the size and geometry of gas overdensities in the IGM, which is not possible with only one or two QSO sight-lines. The QSO separations are ideally suited for this purpose, as they are comparable to the expected size of IGM gas clouds. Using state-of-the-art hydrodynamical simulations, which include gas cooling inflows, outflows, feedback, and the introduction of gas and metals in the IGM, we will construct mock spectra and galaxy distributions to compare with the observations. Taken together, our new HST observations, ground-based galaxy redshift survey, and simulations will enable us to investigate the nature and extent of the connection between the IGM and galaxies.;
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