Howlett, C.Ross, A. J.Samushia, LadoPercival, W. J.Manera, M.2016-04-062016-04-062015-05-01http://hdl.handle.net/2097/32455Citation: 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/stu2693We 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.This Item is protected by copyright and/or related rights. You are free to use this Item in any way that is permitted by the copyright and related rights legislation that applies to your use. For other uses you need to obtain permission from the rights-holder(s).SurveysGalaxies: StatisticsCosmological ParametersCosmology:ObservationsLarge-Scale Structure Of UniverseArticle