The clustering of the SDSS main galaxy sample - II. Mock galaxy catalogues and a measurement of the growth of structure from redshift space distortions at z=0.15

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dc.contributor.author Howlett, C.
dc.contributor.author Ross, A. J.
dc.contributor.author Samushia, Lado
dc.contributor.author Percival, W. J.
dc.contributor.author Manera, M.
dc.date.accessioned 2016-04-06T15:11:42Z
dc.date.available 2016-04-06T15:11:42Z
dc.identifier.uri http://hdl.handle.net/2097/32455
dc.description Citation: Howlett, C., Ross, A. J., Samushia, L., Percival, W. J., & Manera, M. (2015). The clustering of the SDSS main galaxy sample - II. Mock galaxy catalogues and a measurement of the growth of structure from redshift space distortions at z=0.15. Monthly Notices of the Royal Astronomical Society, 449(1), 848-866. doi:10.1093/mnras/stu2693
dc.description We measure redshift space distortions in the two-point correlation function of a sample of 63 163 spectroscopically identified galaxies with z < 0.2, an epoch where there are currently only limited measurements, from the Sloan Digital Sky Survey Data Release 7 main galaxy sample (MGS). Our sample, which we denote MGS, covers 6813 deg(2) with an effective redshift z(eff) = 0.15 and is described in our companion paper (Paper I), which concentrates on baryon acoustic oscillation (BAO) measurements. In order to validate the fitting methods used in both papers, and derive errors, we create and analyse 1000 mock catalogues using a new algorithm called PICOLA to generate accurate dark matter fields. Haloes are then selected using a friends-of-friends algorithm, and populated with galaxies using a halo-occupation distribution fitted to the data. Using errors derived from these mocks, we fit a model to the monopole and quadrupole moments of the MGS correlation function. If we assume no Alcock-Paczynski (AP) effect (valid at z = 0.15 for any smooth model of the expansion history), we measure the amplitude of the velocity field, f sigma(8), at z = 0.15 to be 0.49(-0.14)(+0.15) . We also measure f sigma(8) including the AP effect. This latter measurement can be freely combined with recent cosmic microwave background results to constrain the growth index of fluctuations, gamma Assuming a background Lambda cold dark matter cosmology and combining with current BAO data, we find gamma = 0.64 +/- 0.09, which is consistent with the prediction of general relativity (gamma approximate to 0.55), though with a slight preference for higher gamma and hence models with weaker gravitational interactions.
dc.relation.uri https://doi.org/10.1093/mnras/stu2693
dc.rights This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2015 Howlett, C.;Ross, A. J.;Samushia, L.;Percival, W. J.;Manera, M. Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
dc.rights.uri http://www.sherpa.ac.uk/romeo/issn/0035-8711/
dc.subject Surveys
dc.subject Galaxies: Statistics
dc.subject Cosmological Parameters
dc.subject Cosmology:
dc.subject Observations
dc.subject Large-Scale Structure Of Universe
dc.title The clustering of the SDSS main galaxy sample - II. Mock galaxy catalogues and a measurement of the growth of structure from redshift space distortions at z=0.15
dc.type Article
dc.date.published 2015
dc.citation.doi 10.1093/mnras/stu2693
dc.citation.epage 866
dc.citation.issn 0035-8711
dc.citation.issue 1
dc.citation.jtitle Monthly Notices of the Royal Astronomical Society
dc.citation.spage 848
dc.citation.volume 449
dc.contributor.authoreid lado


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