The UV-optical colour dependence of galaxy clustering in the local universe

Yeong Shang Loh, R. Michael Rich, Sébastien Heinis, Ryan Scranton, Ryan P. Mallery, Samir Salim, D. Christopher Martin, Ted Wyder, Stéphane Arnouts, Tom A. Barlow, Karl Forster, Peter G. Friedman, Patrick Morrissey, Susan G. Neff, David Schiminovich, Mark Seibert, Luciana Bianchi, Jose Donas, Timothy M. Heckman, Young Wook LeeBarry F. Madore, Bruno Milliard, Alex S. Szalay, Barry Y. Welsh

Research output: Contribution to journalArticle

20 Citations (Scopus)

Abstract

We measure the UV-optical colour dependence of galaxy clustering in the local Universe. Using the clean separation of the red and blue sequences made possible by the NUV-r colour-magnitude diagram, we segregate the galaxies into red, blue and intermediate 'green' classes. We explore the clustering as a function of this segregation by removing the dependence on luminosity and by excluding edge-on galaxies as a means of a non-model dependent veto of highly extincted galaxies. We find that ξ(rp, π) for both red and green galaxies shows strong redshift-space distortion on small scales - the 'finger-of-God' effect, with green galaxies having a lower amplitude than is seen for the red sequence, and the blue sequence showing almost no distortion. On large scales, ξ(rp, π) for all three samples show the effect of large-scale streaming from coherent infall. On scales of 1 h-1 Mpc < rp < 10 h-1 Mpc, the projected auto-correlation function wp(rp) for red and green galaxies fits a power law with slope γ∼ 1.93 and amplitude r0∼ 7.5 and 5.3, compared with γ∼ 1.75 and r0∼ 3.9 h-1 Mpc for blue sequence galaxies. Compared to the clustering of a fiducial L* galaxy, the red, green and blue have a relative bias of 1.5, 1.1 and 0.9, respectively. The wp(rp) for blue galaxies display an increase in convexity at ∼ 1 h-1 Mpc, with an excess of large-scale clustering. Our results suggest that the majority of blue galaxies are likely central galaxies in less massive haloes, while red and green galaxies have larger satellite fractions, and preferentially reside in virialized structures. If blue sequence galaxies migrate to the red sequence via processes like mergers or quenching that take them through the green valley, such a transformation may be accompanied by a change in environment in addition to any change in luminosity and colour.

Original languageEnglish
Pages (from-to)55-70
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume407
Issue number1
DOIs
Publication statusPublished - 2010 Sep 1

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universe
galaxies
color
autocorrelation
merger
power law
diagram
valley
luminosity
effect
convexity
color-magnitude diagram
valleys
halos
quenching
slopes

All Science Journal Classification (ASJC) codes

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Loh, Y. S., Rich, R. M., Heinis, S., Scranton, R., Mallery, R. P., Salim, S., ... Welsh, B. Y. (2010). The UV-optical colour dependence of galaxy clustering in the local universe. Monthly Notices of the Royal Astronomical Society, 407(1), 55-70. https://doi.org/10.1111/j.1365-2966.2010.16908.x
Loh, Yeong Shang ; Rich, R. Michael ; Heinis, Sébastien ; Scranton, Ryan ; Mallery, Ryan P. ; Salim, Samir ; Martin, D. Christopher ; Wyder, Ted ; Arnouts, Stéphane ; Barlow, Tom A. ; Forster, Karl ; Friedman, Peter G. ; Morrissey, Patrick ; Neff, Susan G. ; Schiminovich, David ; Seibert, Mark ; Bianchi, Luciana ; Donas, Jose ; Heckman, Timothy M. ; Lee, Young Wook ; Madore, Barry F. ; Milliard, Bruno ; Szalay, Alex S. ; Welsh, Barry Y. / The UV-optical colour dependence of galaxy clustering in the local universe. In: Monthly Notices of the Royal Astronomical Society. 2010 ; Vol. 407, No. 1. pp. 55-70.
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Loh, YS, Rich, RM, Heinis, S, Scranton, R, Mallery, RP, Salim, S, Martin, DC, Wyder, T, Arnouts, S, Barlow, TA, Forster, K, Friedman, PG, Morrissey, P, Neff, SG, Schiminovich, D, Seibert, M, Bianchi, L, Donas, J, Heckman, TM, Lee, YW, Madore, BF, Milliard, B, Szalay, AS & Welsh, BY 2010, 'The UV-optical colour dependence of galaxy clustering in the local universe', Monthly Notices of the Royal Astronomical Society, vol. 407, no. 1, pp. 55-70. https://doi.org/10.1111/j.1365-2966.2010.16908.x

The UV-optical colour dependence of galaxy clustering in the local universe. / Loh, Yeong Shang; Rich, R. Michael; Heinis, Sébastien; Scranton, Ryan; Mallery, Ryan P.; Salim, Samir; Martin, D. Christopher; Wyder, Ted; Arnouts, Stéphane; Barlow, Tom A.; Forster, Karl; Friedman, Peter G.; Morrissey, Patrick; Neff, Susan G.; Schiminovich, David; Seibert, Mark; Bianchi, Luciana; Donas, Jose; Heckman, Timothy M.; Lee, Young Wook; Madore, Barry F.; Milliard, Bruno; Szalay, Alex S.; Welsh, Barry Y.

In: Monthly Notices of the Royal Astronomical Society, Vol. 407, No. 1, 01.09.2010, p. 55-70.

Research output: Contribution to journalArticle

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T1 - The UV-optical colour dependence of galaxy clustering in the local universe

AU - Loh, Yeong Shang

AU - Rich, R. Michael

AU - Heinis, Sébastien

AU - Scranton, Ryan

AU - Mallery, Ryan P.

AU - Salim, Samir

AU - Martin, D. Christopher

AU - Wyder, Ted

AU - Arnouts, Stéphane

AU - Barlow, Tom A.

AU - Forster, Karl

AU - Friedman, Peter G.

AU - Morrissey, Patrick

AU - Neff, Susan G.

AU - Schiminovich, David

AU - Seibert, Mark

AU - Bianchi, Luciana

AU - Donas, Jose

AU - Heckman, Timothy M.

AU - Lee, Young Wook

AU - Madore, Barry F.

AU - Milliard, Bruno

AU - Szalay, Alex S.

AU - Welsh, Barry Y.

PY - 2010/9/1

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N2 - We measure the UV-optical colour dependence of galaxy clustering in the local Universe. Using the clean separation of the red and blue sequences made possible by the NUV-r colour-magnitude diagram, we segregate the galaxies into red, blue and intermediate 'green' classes. We explore the clustering as a function of this segregation by removing the dependence on luminosity and by excluding edge-on galaxies as a means of a non-model dependent veto of highly extincted galaxies. We find that ξ(rp, π) for both red and green galaxies shows strong redshift-space distortion on small scales - the 'finger-of-God' effect, with green galaxies having a lower amplitude than is seen for the red sequence, and the blue sequence showing almost no distortion. On large scales, ξ(rp, π) for all three samples show the effect of large-scale streaming from coherent infall. On scales of 1 h-1 Mpc < rp < 10 h-1 Mpc, the projected auto-correlation function wp(rp) for red and green galaxies fits a power law with slope γ∼ 1.93 and amplitude r0∼ 7.5 and 5.3, compared with γ∼ 1.75 and r0∼ 3.9 h-1 Mpc for blue sequence galaxies. Compared to the clustering of a fiducial L* galaxy, the red, green and blue have a relative bias of 1.5, 1.1 and 0.9, respectively. The wp(rp) for blue galaxies display an increase in convexity at ∼ 1 h-1 Mpc, with an excess of large-scale clustering. Our results suggest that the majority of blue galaxies are likely central galaxies in less massive haloes, while red and green galaxies have larger satellite fractions, and preferentially reside in virialized structures. If blue sequence galaxies migrate to the red sequence via processes like mergers or quenching that take them through the green valley, such a transformation may be accompanied by a change in environment in addition to any change in luminosity and colour.

AB - We measure the UV-optical colour dependence of galaxy clustering in the local Universe. Using the clean separation of the red and blue sequences made possible by the NUV-r colour-magnitude diagram, we segregate the galaxies into red, blue and intermediate 'green' classes. We explore the clustering as a function of this segregation by removing the dependence on luminosity and by excluding edge-on galaxies as a means of a non-model dependent veto of highly extincted galaxies. We find that ξ(rp, π) for both red and green galaxies shows strong redshift-space distortion on small scales - the 'finger-of-God' effect, with green galaxies having a lower amplitude than is seen for the red sequence, and the blue sequence showing almost no distortion. On large scales, ξ(rp, π) for all three samples show the effect of large-scale streaming from coherent infall. On scales of 1 h-1 Mpc < rp < 10 h-1 Mpc, the projected auto-correlation function wp(rp) for red and green galaxies fits a power law with slope γ∼ 1.93 and amplitude r0∼ 7.5 and 5.3, compared with γ∼ 1.75 and r0∼ 3.9 h-1 Mpc for blue sequence galaxies. Compared to the clustering of a fiducial L* galaxy, the red, green and blue have a relative bias of 1.5, 1.1 and 0.9, respectively. The wp(rp) for blue galaxies display an increase in convexity at ∼ 1 h-1 Mpc, with an excess of large-scale clustering. Our results suggest that the majority of blue galaxies are likely central galaxies in less massive haloes, while red and green galaxies have larger satellite fractions, and preferentially reside in virialized structures. If blue sequence galaxies migrate to the red sequence via processes like mergers or quenching that take them through the green valley, such a transformation may be accompanied by a change in environment in addition to any change in luminosity and colour.

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