Galaxy and Mass Assembly (GAMA) : small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies
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The 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.
Loveday , 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 . DOI: 10.1093/mnras/stx2971
Monthly Notices of the Royal Astronomical Society
© 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/stx2971
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