Galaxy and Mass Assembly (GAMA): small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies

J. Loveday; L. Christodoulou; P. Norberg; J. A. Peacock; I. K. Baldry; J. Bland-Hawthorn; M. J.I. Brown; M. Colless; S. P. Driver; B. W. Holwerda; A. M. Hopkins; P. R. Kafle; J. Liske; A. R. Lopez-Sanchez; E. N. Taylor

doi:10.1093/mnras/stx2971

Galaxy and Mass Assembly (GAMA): small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies

J. Loveday^*, L. Christodoulou, P. Norberg, J. A. Peacock, I. K. Baldry, J. Bland-Hawthorn, M. J.I. Brown, M. Colless, S. P. Driver, B. W. Holwerda, A. M. Hopkins, P. R. Kafle, J. Liske, A. R. Lopez-Sanchez, E. N. Taylor

^*Corresponding author for this work

Research output: Contribution to journal › Article › peer-review

14 Citations (Scopus)

Abstract

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 M_r = -17 mag to σ₁₂ ≈ 600 km s^-1 at M_r ≈ -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.

Original language	English
Pages (from-to)	3435-3450
Number of pages	16
Journal	Monthly Notices of the Royal Astronomical Society
Volume	474
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stx2971
Publication status	Published - 1 Mar 2018

Keywords

Galaxies: kinematics and dynamics
Galaxies: statistics

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10.1093/mnras/stx2971

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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. (2018). Galaxy and Mass Assembly (GAMA): small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies. Monthly Notices of the Royal Astronomical Society, 474(3), 3435-3450. https://doi.org/10.1093/mnras/stx2971

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title = "Galaxy and Mass Assembly (GAMA): small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies",

abstract = "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.",

keywords = "Galaxies: kinematics and dynamics, Galaxies: statistics",

author = "J. Loveday and L. Christodoulou and P. Norberg and Peacock, {J. A.} and Baldry, {I. K.} and J. Bland-Hawthorn and Brown, {M. J.I.} and M. Colless and Driver, {S. P.} and Holwerda, {B. W.} and Hopkins, {A. M.} and Kafle, {P. R.} and J. Liske and Lopez-Sanchez, {A. R.} and Taylor, {E. N.}",

year = "2018",

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doi = "10.1093/mnras/stx2971",

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Loveday, J, Christodoulou, L, Norberg, P, Peacock, JA, Baldry, IK, Bland-Hawthorn, J, Brown, MJI, Colless, M, Driver, SP, Holwerda, BW, Hopkins, AM, Kafle, PR, Liske, J, Lopez-Sanchez, AR & Taylor, EN 2018, '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/stx2971

TY - JOUR

T1 - Galaxy and Mass Assembly (GAMA)

T2 - small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies

AU - Loveday, J.

AU - Christodoulou, L.

AU - Norberg, P.

AU - Peacock, J. A.

AU - Baldry, I. K.

AU - Bland-Hawthorn, J.

AU - Brown, M. J.I.

AU - Colless, M.

AU - Driver, S. P.

AU - Holwerda, B. W.

AU - Hopkins, A. M.

AU - Kafle, P. R.

AU - Liske, J.

AU - Lopez-Sanchez, A. R.

AU - Taylor, E. N.

PY - 2018/3/1

Y1 - 2018/3/1

N2 - 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.

AB - 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.

KW - Galaxies: kinematics and dynamics

KW - Galaxies: statistics

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U2 - 10.1093/mnras/stx2971

DO - 10.1093/mnras/stx2971

M3 - Article

AN - SCOPUS:85040222691

SN - 0035-8711

VL - 474

SP - 3435

EP - 3450

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Galaxy and Mass Assembly (GAMA): small-scale anisotropic galaxy clustering and the pairwise velocity dispersion of galaxies

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