Show simple item record

Files in this item

Thumbnail

Item metadata

dc.contributor.authorLoveday, J.
dc.contributor.authorChristodoulou, L.
dc.contributor.authorNorberg, P.
dc.contributor.authorPeacock, J. A.
dc.contributor.authorBaldry, I. K.
dc.contributor.authorBland-Hawthorn, J.
dc.contributor.authorBrown, M. J. I.
dc.contributor.authorColless, M.
dc.contributor.authorDriver, S. P.
dc.contributor.authorHolwerda, B. W.
dc.contributor.authorHopkins, A. M.
dc.contributor.authorKafle, P. R.
dc.contributor.authorLiske, J.
dc.contributor.authorLopez-Sanchez, A. R.
dc.contributor.authorTaylor, E. N.
dc.date.accessioned2018-01-19T11:30:07Z
dc.date.available2018-01-19T11:30:07Z
dc.date.issued2017-11-17
dc.identifier.citationLoveday , J , Christodoulou , L , Norberg , P , Peacock , J A , Baldry , I K , Bland-Hawthorn , J , Brown , M J I , Colless , M , Driver , S P , Holwerda , B W , Hopkins , A M , Kafle , P R , Liske , J , Lopez-Sanchez , A R & Taylor , E N 2017 , ' Galaxy and Mass Assembly (GAMA) : small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies ' , Monthly Notices of the Royal Astronomical Society , vol. 474 , no. 3 , pp. 3435-3450 . https://doi.org/10.1093/mnras/stx2971en
dc.identifier.issn0035-8711
dc.identifier.otherPURE: 252091104
dc.identifier.otherPURE UUID: 10172772-1b6e-4a6d-ac78-1a6edb04120a
dc.identifier.otherArXiv: http://arxiv.org/abs/1711.05636v1
dc.identifier.otherScopus: 85040222691
dc.identifier.otherWOS: 000424347900043
dc.identifier.urihttp://hdl.handle.net/10023/12518
dc.description.abstractThe galaxy pairwise velocity dispersion (PVD) can provide important tests of non-standard gravity and galaxy formation models. We describe measurements of the PVD of galaxies in the Galaxy and Mass Assembly (GAMA) survey as a function of projected separation and galaxy luminosity. Due to the faint magnitude limit (r < 19.8) and highly complete spectroscopic sampling of the GAMA survey, we are able to reliably measure the PVD to smaller scales (r⊥ = 0.01 h−1 Mpc) than previous work. The measured PVD at projected separations r⊥ ≲ 1 h−1 Mpc increases near monotonically with increasing luminosity from σ12 ≈ 200 km s−1 at Mr = −17 mag to σ12 ≈ 600 km s − 1 at Mr ≈ −22 mag. Analysis of the Gonzalez-Perez et al. (2014) galform semi-analytic model yields no such trend of PVD with luminosity: the model overpredicts the PVD for faint galaxies. This is most likely a result of the model placing too many low-luminosity galaxies in massive haloes.
dc.language.isoeng
dc.relation.ispartofMonthly Notices of the Royal Astronomical Societyen
dc.rights© 2017, the Author(s). This work has been made available online in accordance with the publisher’s policies. This is the final published version of the work, which was originally published at https://doi.org/10.1093/mnras/stx2971en
dc.subjectGalaxies: kinematics and dynamicsen
dc.subjectGalaxies: statisticsen
dc.subjectQB Astronomyen
dc.subjectQC Physicsen
dc.subject3rd-DASen
dc.subject.lccQBen
dc.subject.lccQCen
dc.titleGalaxy and Mass Assembly (GAMA) : small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxiesen
dc.typeJournal articleen
dc.description.versionPublisher PDFen
dc.contributor.institutionUniversity of St Andrews.School of Physics and Astronomyen
dc.identifier.doihttps://doi.org/10.1093/mnras/stx2971
dc.description.statusPeer revieweden


This item appears in the following Collection(s)

Show simple item record