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Date and Time of the Query: 2018-09-18 T08:03:52 PDT
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For refcode 2014MNRAS.437.2017T:
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Copyright by Royal Astronomical Society. 2014MNRAS.437.2017T On the connection between the intergalactic medium and galaxies: the H I-galaxy cross-correlation at z <~ 1 Tejos, Nicolas; Morris, Simon L.; Finn, Charles W.; Crighton, Neil H. M.; Bechtold, Jill; Jannuzi, Buell T.; Schaye, Joop; Theuns, Tom; Altay, Gabriel; Le Fevre, Olivier; Ryan-Weber, Emma; Dave, Romeel Abstract. We present a new optical spectroscopic survey of 1777 'star-forming' ('SF') and 366 'non-star-forming' ('non-SF') galaxies at redshifts z ~ 0-1 (2143 in total), 22 AGN and 423 stars, observed by instruments such as the Deep Imaging Multi-Object Spectrograph, the Visible Multi-Object Spectrograph and the Gemini Multi-Object Spectrograph, in three fields containing five quasi-stellar objects (QSOs) with Hubble Space Telescope (HST) ultraviolet spectroscopy. We also present a new spectroscopic survey of 173 'strong' (10^14^ <= N_HI_<~ 10^17^ cm^-2^) and 496 'weak' (10^13^ <~ N_HI_ < 10^14^ cm^-2^) intervening H I (Ly-{alpha}) absorption-line systems at z <~ 1 (669 in total), observed in the spectra of eight QSOs at z ~ 1 by the Cosmic Origins Spectrograph and the Faint Object Spectrograph on the HST. Combining these new data with previously published galaxy catalogues such as the Very Large Telescope Visible Multi-Object Spectrograph Deep Survey and the Gemini Deep Deep Survey, we have gathered a sample of 654 H I absorption systems and 17 509 galaxies at transverse scales <~50 Mpc, suitable for a two-point correlation function analysis. We present observational results on the H I-galaxy (xi_ag_) and galaxy-galaxy (xi_gg_) correlations at transverse scales r_ is perpendicular to_ <~ 10 Mpc, and the H I-H I autocorrelation (xi_aa_) at transverse scales r_ is perpendicular to_ <~ 2 Mpc. The two-point correlation functions are measured both along and transverse to the line of sight, xi(r_ is perpendicular to_, r_||_). We also infer the shape of their corresponding 'real-space' correlation functions, xi(r), from the projected along the line-of-sight correlations, assuming power laws of the form xi(r) = (r/r_0_)^-gamma^. Comparing the results from xi_ag_, xi_gg_ and xi_aa_, we constrain the H I-galaxy statistical connection, as a function of both H I column density and galaxy star formation activity. Our results are consistent with the following conclusions: (i) the bulk of H I systems on ~ Mpc scales have little velocity dispersion (<~120 km s^-1^) with respect to the bulk of galaxies (i.e. no strong galaxy outflow/inflow signal is detected); (II) the vast majority (~100 per cent) of 'strong' H I systems and 'SF' galaxies are distributed in the same locations, together with 75 +/- 15 per cent of 'non-SF' galaxies, all of which typically reside in dark matter haloes of similar masses; (III) 25 +/- 15 per cent of 'non-SF' galaxies reside in galaxy clusters and are not correlated with 'strong' H I systems at scales <~2 Mpc; and (IV) >50 per cent of 'weak' H I systems reside within galaxy voids (hence not correlated with galaxies), and are confined in dark matter haloes of masses smaller than those hosting 'strong' systems and/or galaxies. We speculate that H I systems within galaxy voids might still be evolving in the linear regime even at scales <~2 Mpc. Key words: galaxies: formation, intergalactic medium, quasars: absorption lines, large-scale structure of Universe
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