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• W2157671444 startingPage "301" @default.
• W2157671444 abstract "We estimate the two-point correlation function in redshift space of the recently compiled HI Parkes All-Sky Survey neutral hydrogen (HI) sources catalogue, which if modelled as a power law, xi(r) = (r(0)/r)(gamma), the best-fitting parameters for the HI selected galaxies are found to be r(0) = 3.3 +/- 0.3 h(-1) Mpc with gamma = 1.38 +/- 0.24. Fixing the slope to its universal value gamma = 1.8, we obtain r(0) = 3.2 +/- 0.2 h(-1) Mpc. Comparing the measured two-point correlation function with the predictions of the concordance cosmological model (Omega(Lambda) = 0.74), we find that at the present epoch the HI selected galaxies are antibiased with respect to the underlying matter fluctuation field with their bias value being b(0) similar or equal to 0.68. Furthermore, dividing the HI galaxies into two richness subsamples we find that the low-mass HI galaxies have a very low present bias factor (b(0) similar or equal to 0.48), while the high-mass HI galaxies trace the underlying matter distribution as the optical galaxies (b(0) similar or equal to 1). Using our derived present-day HI galaxy bias we estimate their redshift-space distortion parameter, and correct accordingly the correlation function for peculiar motions. The resulting real-space correlation length is r(0)(re) = 1.8 +/- 0.2 h(-1) Mpc r(0)(re) = 3.9 +/- 0.6 h(-1) Mpc for the low- and high-mass HI galaxies, respectively. The low-mass HI galaxies appear to have the lowest correlation length among all extragalactic populations studied to date. In order to corroborate these results we have correlated the IRAS-Point Source Catalogue for Redshift (PSCz) reconstructed density field, smoothed over scales of 5 h(-1) Mpc, with the positions of the HI galaxies, to find that indeed the HI galaxies are typically found in negative overdensity regions (delta rho/rho(PSCz) less than or similar to 0), even more so the low-mass HI galaxies. Finally, we also study the redshift evolution of the HI galaxy linear bias factor and find that the HI-galaxy population is antibiased up to z similar to 1.3. While at large redshifts similar to 3, we predict that the HI galaxies are strongly biased. Our bias evolution predictions are consistent with the observational bias results of Ly alpha galaxies." @default.
• W2157671444 created "2016-06-24" @default.
• W2157671444 creator A5006349174 @default.
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• W2157671444 creator A5085403901 @default.
• W2157671444 creator A5089583649 @default.
• W2157671444 date "2007-06-11" @default.
• W2157671444 modified "2023-09-27" @default.
• W2157671444 title "Large-scale structure in the H I Parkes All-Sky Survey: filling the voids with H I galaxies?" @default.
• W2157671444 cites W1745134529 @default.
• W2157671444 cites W1967936658 @default.
• W2157671444 cites W1972155987 @default.
• W2157671444 cites W1972197045 @default.
• W2157671444 cites W1973524841 @default.
• W2157671444 cites W1973728684 @default.
• W2157671444 cites W1974249877 @default.
• W2157671444 cites W1976620664 @default.
• W2157671444 cites W1982364216 @default.
• W2157671444 cites W1984743356 @default.
• W2157671444 cites W1995333740 @default.
• W2157671444 cites W2000444334 @default.
• W2157671444 cites W2002142654 @default.
• W2157671444 cites W2003055164 @default.
• W2157671444 cites W2004491479 @default.
• W2157671444 cites W2006189395 @default.
• W2157671444 cites W2012199985 @default.
• W2157671444 cites W2019814800 @default.
• W2157671444 cites W2021719201 @default.
• W2157671444 cites W2027591012 @default.
• W2157671444 cites W2027953984 @default.
• W2157671444 cites W2029168586 @default.
• W2157671444 cites W2031497590 @default.
• W2157671444 cites W2046107284 @default.
• W2157671444 cites W2046344907 @default.
• W2157671444 cites W2049971403 @default.
• W2157671444 cites W2051694884 @default.
• W2157671444 cites W2054225619 @default.
• W2157671444 cites W2059805965 @default.
• W2157671444 cites W2065201732 @default.
• W2157671444 cites W2073603601 @default.
• W2157671444 cites W2074242573 @default.
• W2157671444 cites W2078921403 @default.
• W2157671444 cites W2098000362 @default.
• W2157671444 cites W2103091483 @default.
• W2157671444 cites W2109338946 @default.
• W2157671444 cites W2110238788 @default.
• W2157671444 cites W2117105462 @default.
• W2157671444 cites W2118265220 @default.
• W2157671444 cites W2118311540 @default.
• W2157671444 cites W2129489826 @default.
• W2157671444 cites W2133843193 @default.
• W2157671444 cites W2135202711 @default.
• W2157671444 cites W2139440433 @default.
• W2157671444 cites W2139847770 @default.
• W2157671444 cites W2144716116 @default.
• W2157671444 cites W2151761100 @default.
• W2157671444 cites W2154219156 @default.
• W2157671444 cites W2155711232 @default.
• W2157671444 cites W2156856858 @default.
• W2157671444 cites W2157917411 @default.
• W2157671444 cites W2165003596 @default.
• W2157671444 cites W2166756424 @default.
• W2157671444 cites W2170689655 @default.
• W2157671444 cites W2286633221 @default.
• W2157671444 cites W2951915383 @default.
• W2157671444 cites W2951971039 @default.
• W2157671444 cites W3006532701 @default.
• W2157671444 cites W3098017603 @default.
• W2157671444 cites W3098082341 @default.
• W2157671444 cites W3100566562 @default.
• W2157671444 cites W3101099925 @default.
• W2157671444 cites W3101168514 @default.
• W2157671444 cites W3101469085 @default.
• W2157671444 cites W3102200478 @default.
• W2157671444 cites W3104214663 @default.
• W2157671444 cites W3104345759 @default.
• W2157671444 cites W3106003577 @default.
• W2157671444 cites W3106212922 @default.
• W2157671444 cites W3122244790 @default.
• W2157671444 cites W3122345961 @default.
• W2157671444 cites W3125927684 @default.
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• W2157671444 doi "https://doi.org/10.1111/j.1365-2966.2007.11781.x" @default.
• W2157671444 hasPublicationYear "2007" @default.
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