期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 460, 期 1, 页码 590-616出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stw918
关键词
galaxies: formation; intergalactic medium; quasars: absorption lines; large-scale structure of Universe
资金
- STFC [ST/J201013/1]
- Australian Research Council [DP130100568]
- Interuniversity Attraction Poles Programme
- Belgian Science Policy Office [AP P7/08 CHARM]
- European Research Council under the European Union [278594-GasAroundGalaxies]
- NASA [NAS 5-26555]
- European Southern Observatory, Chile [070.A-9007, 086.A-0970, 087.A-0857]
- STFC (UK)
- ARC (Australia)
- AAO
- BIS National E- infrastructure capital grant [ST/K00042X/1]
- STFC capital grant [ST/H008519/1]
- STFC DiRAC Operations grant [ST/K003267/1]
- Durham University
- Science and Technology Facilities Council [ST/I001573/1, 1089495, ST/H008519/1, ST/I00162X/1, ST/M007006/1, ST/K00042X/1, ST/L00075X/1] Funding Source: researchfish
- STFC [ST/I001573/1, ST/I00162X/1, ST/L00075X/1, ST/K00042X/1, ST/M007006/1, ST/H008519/1] Funding Source: UKRI
We present new results on the auto- and cross-correlation functions of galaxies and O vi absorbers in a similar to 18 Gpc(3) comoving volume at z < 1. We use a sample of 51 296 galaxies and 140 O vi absorbers in the column density range 13 a parts per thousand(2) log N a parts per thousand(2) 15 to measure two-point correlation functions in the two dimensions transverse and orthogonal to the line of sight xi(r(aSyen), r(ayen)). We furthermore infer the corresponding 'real-space' correlation functions, xi(r), by projecting xi(r(aSyen), r(ayen)) along r(ayen), and assuming a power-law form, xi(r) = (r/r(0))(-gamma). Comparing the results from the absorber-galaxy cross-correlation function, xi(ag), the galaxy autocorrelation function, xi(gg), and the absorber autocorrelation function, xi(aa), we constrain the statistical connection between galaxies and the metal-enriched intergalactic medium as a function of star formation activity. We also compare these results to predictions from the eagle cosmological hydrodynamical simulation and find a reasonable agreement. We find that: (i) O vi absorbers show very little velocity dispersion with respect to galaxies on similar to Mpc scales, likely a parts per thousand(2)100 km s(-1); (ii) O vi absorbers are less clustered, and potentially more extended around galaxies than galaxies are around themselves; (iii) on a parts per thousand(3)100 kpc scales, the likelihood of finding O vi absorbers around star-forming galaxies is similar to the likelihood of finding O vi absorbers around non-star-forming galaxies; and (iv) O vi absorbers are either not ubiquitous to galaxies in our sample, or their distribution around them is patchy on scales a parts per thousand(3)100 kpc (or both), at least for the column densities at which most are currently detected.
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