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

School of Physics and Astronomy

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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 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
Journal	Monthly Notices of the Royal Astronomical Society
Volume	474
Issue number	3
Early online date	17 Nov 2017
DOIs	https://doi.org/10.1093/mnras/stx2971
Publication status	E-pub ahead of print - 17 Nov 2017

Keywords

Galaxies: kinematics and dynamics
Galaxies: statistics

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Loveday-2017-GAMA-MNRAS-3435
© 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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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, 474(3), 3435-3450. Advance online publication. 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.}",

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month = nov,

day = "17",

doi = "10.1093/mnras/stx2971",

language = "English",

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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 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/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 - 2017/11/17

Y1 - 2017/11/17

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

U2 - 10.1093/mnras/stx2971

DO - 10.1093/mnras/stx2971

M3 - Article

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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Keywords

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