On the connection between the intergalactic medium and galaxies : the H i-galaxy cross-correlation at
We present a new optical spectroscopic survey of 1777 'star-forming' ('SF') and 366 'non-star-forming' ('non-SF') galaxies at redshifts z similar to 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 less than or similar to 10(17) cm(-2)) and 496 'weak' (10(13) less than or similar to N-HI 10(14) cm(-2)) intervening H i (Ly alpha) absorption-line systems at z less than or similar to 1 (669 in total), observed in the spectra of eight QSOs at z similar to 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 less than or similar to 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(perpendicular to) less than or similar to 10 Mpc, and the H i-H i autocorrelation (xi(aa)) at transverse scales r(perpendicular to) less than or similar to 2 Mpc. The two-point correlation functions are measured both along and transverse to the line of sight, xi(r(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 similar to Mpc scales have little velocity dispersion (less than or similar to 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 (similar to 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 less than or similar to 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 less than or similar to 2 Mpc.
Source (journal)
Monthly notices of the Royal Astronomical Society. - Oxford
Oxford : 2014
437:3(2014), p. 2017-2075
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Publication type
Publications with a UAntwerp address
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Web of Science
Creation 06.02.2014
Last edited 09.01.2018
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