We measure the two-point redshift-space correlation function of loose groups of galaxies, {xi {GG}(s)} , for the combined CfA2 and SSRS2 surveys. Our combined group catalog constitutes the largest homogeneous sample available (885 groups). We compare {xi {GG}(s)} with the correlation function of galaxies, {xi {gg}(s)} , in the same volume. We find that groups are significantly more clustered than galaxies: {xi {GG}/xi {gg}} m=1.64+/-0.16. A similar result holds when we analyze a volume-limited sample (distance limit 78 {{h}-1 Mpc} h) of 139 groups. For these groups, with median velocity dispersion sigma {v} ~ 200 {km s-1} and mean group separation d ~ 16 {{h}-1 Mpc} h, we find that the correlation length is s{0}=8+/-1 {{h}-1 Mpc} h, which is significantly smaller than that found for rich clusters. We conclude that clustering properties of loose groups of galaxies are intermediate between galaxies and rich clusters. Moreover, we find evidence that group clustering depends on physical properties of groups: correlation strengthens for increasing sigma {v}.

The redshift-space two-point correlation functionof galaxy groups in the CfA2 and SSRS2 surveys

GIRARDI, MARISA;
2000

Abstract

We measure the two-point redshift-space correlation function of loose groups of galaxies, {xi {GG}(s)} , for the combined CfA2 and SSRS2 surveys. Our combined group catalog constitutes the largest homogeneous sample available (885 groups). We compare {xi {GG}(s)} with the correlation function of galaxies, {xi {gg}(s)} , in the same volume. We find that groups are significantly more clustered than galaxies: {xi {GG}/xi {gg}} m=1.64+/-0.16. A similar result holds when we analyze a volume-limited sample (distance limit 78 {{h}-1 Mpc} h) of 139 groups. For these groups, with median velocity dispersion sigma {v} ~ 200 {km s-1} and mean group separation d ~ 16 {{h}-1 Mpc} h, we find that the correlation length is s{0}=8+/-1 {{h}-1 Mpc} h, which is significantly smaller than that found for rich clusters. We conclude that clustering properties of loose groups of galaxies are intermediate between galaxies and rich clusters. Moreover, we find evidence that group clustering depends on physical properties of groups: correlation strengthens for increasing sigma {v}.
http://adsabs.harvard.edu/abs/2000A%26A...353...57G
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11368/1695159
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