Color gradients of the galaxies at 0.5 < z < 1 Ⅱ. Clustering properties
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摘要
We investigate the dependence of clustering on luminosity, stellar mass and color gradient for galaxies at 0.5 < z < 1, using a sample of ~6300 galaxies from the final data release of the VIMOS Public Extragalactic Redshift Survey(VIPERS-PDR2). We estimate both the auto-correlation function for galaxy samples selected by B-band absolute magnitude and stellar mass, and the cross-correlation function of galaxy samples selected by color gradient with respect to the full galaxy sample. The autocorrelation function amplitudes at fixed scale are found to positively correlate with both galaxy luminosity and stellar mass, and the effect holds for all the scales probed(0.2 h~(-1) Mpc < rp< 20 h~(-1) Mpc),in good agreement with previous measurements based on an earlier data release of VIPERS. When the stellar mass is limited to a narrow range, we find the clustering power to be essentially independent of galaxy color gradient, and this conclusion is true for all the masses and all the scales considered here. In a parallel paper, we find that the half-light radius is the only galaxy property other than stellar mass that is related to color gradient. Considering the previous finding that clustering depends weakly on galaxy structure at given mass, the non-dependence of clustering on color gradient found here reinforces our conclusion that the color gradient and structural parameters of a galaxy are intrinsically related to each other.
We investigate the dependence of clustering on luminosity, stellar mass and color gradient for galaxies at 0.5 < z < 1, using a sample of ~6300 galaxies from the final data release of the VIMOS Public Extragalactic Redshift Survey(VIPERS-PDR2). We estimate both the auto-correlation function for galaxy samples selected by B-band absolute magnitude and stellar mass, and the cross-correlation function of galaxy samples selected by color gradient with respect to the full galaxy sample. The autocorrelation function amplitudes at fixed scale are found to positively correlate with both galaxy luminosity and stellar mass, and the effect holds for all the scales probed(0.2 h~(-1) Mpc < rp< 20 h~(-1) Mpc),in good agreement with previous measurements based on an earlier data release of VIPERS. When the stellar mass is limited to a narrow range, we find the clustering power to be essentially independent of galaxy color gradient, and this conclusion is true for all the masses and all the scales considered here. In a parallel paper, we find that the half-light radius is the only galaxy property other than stellar mass that is related to color gradient. Considering the previous finding that clustering depends weakly on galaxy structure at given mass, the non-dependence of clustering on color gradient found here reinforces our conclusion that the color gradient and structural parameters of a galaxy are intrinsically related to each other.
We investigate the dependence of clustering on luminosity, stellar mass and color gradient for galaxies at 0.5 < z < 1, using a sample of ~6300 galaxies from the final data release of the VIMOS Public Extragalactic Redshift Survey(VIPERS-PDR2). We estimate both the auto-correlation function for galaxy samples selected by B-band absolute magnitude and stellar mass, and the cross-correlation function of galaxy samples selected by color gradient with respect to the full galaxy sample. The autocorrelation function amplitudes at fixed scale are found to positively correlate with both galaxy luminosity and stellar mass, and the effect holds for all the scales probed(0.2 h~(-1) Mpc < rp< 20 h~(-1) Mpc),in good agreement with previous measurements based on an earlier data release of VIPERS. When the stellar mass is limited to a narrow range, we find the clustering power to be essentially independent of galaxy color gradient, and this conclusion is true for all the masses and all the scales considered here. In a parallel paper, we find that the half-light radius is the only galaxy property other than stellar mass that is related to color gradient. Considering the previous finding that clustering depends weakly on galaxy structure at given mass, the non-dependence of clustering on color gradient found here reinforces our conclusion that the color gradient and structural parameters of a galaxy are intrinsically related to each other.
引文
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Marulli,F.,Bolzonella,M.,Branchini,E.,et al.2013,A&A,557,A17
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Tortora,C.,&Napolitano,N.R.2012,MNRAS,421,2478
Wang,L.,Li,C.,Kauffmann,G.,&De Lucia,G.2007,MNRAS,377,1419
Wang,Y.,Yang,X.,Mo,H.J.,et al.2008,ApJ,687,919
White,S.D.M.,Tully,R.B.,&Davis,M.1988,ApJ,333,L45
Willmer,C.N.A.,da Costa,L.N.,&Pellegrini,P.S.1998,AJ,115,869
York,D.G.,Adelman,J.,Anderson,Jr.,J.E.,et al.2000,AJ,120,1579
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Zheng,Z.,Wang,H.,Ge,J.,et al.2017,MNRAS,465,4572
1http://vipers.inaf.it
2 http://cesam.lam.fr/vipers-mls
3http://cesam.lam.fr/vipers-mls
4http://vipers.inaf.it/rel-pdr2.html
Blanton,M.R.,&Moustakas,J.2009,ARA&A,47,159
Bundy,K.,Bershady,M.A.,Law,D.R.,et al.2015,ApJ,798,7
Colless,M.,Dalton,G.,Maddox,S.,et al.2001,MNRAS,328,1039
Cuillandre,J.-C.J.,Withington,K.,Hudelot,P.,et al.2012,in Proc.SPIE,8448,Observatory Operations:Strategies,Processes,and Systems IV,84480M
de la Torre,S.,Guzzo,L.,Peacock,J.A.,et al.2013,A&A,557,A54
Ferreras,I.,Lisker,T.,Pasquali,A.,Khochfar,S.,&Kaviraj,S.2009,MNRAS,396,1573
Goddard,D.,Thomas,D.,Maraston,C.,et al.2017,MNRAS,465,688
Goto,T.,Yamauchi,C.,Fujita,Y.,et al.2003,MNRAS,346,601
Guo,H.,Zehavi,I.,Zheng,Z.,et al.2013,ApJ,767,122
Guzzo,L.,Scodeggio,M.,Garilli,B.,et al.2014,A&A,566,A108
Ilbert,O.,Tresse,L.,Zucca,E.,et al.2005,A&A,439,863
Kauffmann,G.,White,S.D.M.,Heckman,T.M.,et al.2004,MNRAS,353,713
Ko,J.,&Im,M.2005,Journal of Korean Astronomical Society,38,149
Kovaˇc,K.,Lilly,S.J.,Knobel,C.,et al.2010,ApJ,718,86
La Barbera,F.,de Carvalho,R.R.,Gal,R.R.,et al.2005,ApJ,626,L19
La Barbera,F.,Ferreras,I.,de Carvalho,R.R.,et al.2011,ApJ,740,L41
Landy,S.D.,&Szalay,A.S.1993,ApJ,412,64
Li,C.,Kauffmann,G.,Heckman,T.M.,Jing,Y.P.,&White,S.D.M.2008a,MNRAS,385,1903
Li,C.,Kauffmann,G.,Heckman,T.M.,White,S.D.M.,&Jing,Y.P.2008b,MNRAS,385,1915
Li,C.,Kauffmann,G.,Jing,Y.P.,et al.2006a,MNRAS,368,21
Li,C.,Kauffmann,G.,Wang,L.,et al.2006b,MNRAS,373,457
Liang,Z.-X.&Li,C.,2018,RAA(Research in Astronomy and Astrophysics),18,143(Paper I)
Liu,F.S.,Jiang,D.,Guo,Y.,et al.2016,ApJ,822,L25
Liu,F.S.,Jiang,D.,Faber,S.M.,et al.2017,ApJ,844,L2
Madgwick,D.S.,Hawkins,E.,Lahav,O.,et al.2003,MNRAS,344,847
Martin,D.C.,Fanson,J.,Schiminovich,D.,et al.2005,ApJ,619,L1
Marulli,F.,Bolzonella,M.,Branchini,E.,et al.2013,A&A,557,A17
Meneux,B.,Guzzo,L.,Garilli,B.,et al.2008,A&A,478,299
Meneux,B.,Guzzo,L.,de la Torre,S.,et al.2009,A&A,505,463
Moutard,T.,Arnouts,S.,Ilbert,O.,et al.2016a,A&A,590,A102
Moutard,T.,Arnouts,S.,Ilbert,O.,et al.2016b,A&A,590,A103
Noll,S.,Burgarella,D.,Giovannoli,E.,et al.2009,A&A,507,1793
Norberg,P.,Baugh,C.M.,Hawkins,E.,et al.2002,MNRAS,332,827
Oke,J.B.,&Gunn,J.E.1983,ApJ,266,713
Peebles,P.J.E.1980,The Large-scale Structure of the Universe(Princeton University Press)
Saglia,R.P.,Maraston,C.,Greggio,L.,Bender,R.,&Ziegler,B.2000,A&A,360,911
Schlegel,D.J.,Finkbeiner,D.P.,&Davis,M.1998,ApJ,500,525
Scodeggio,M.,Guzzo,L.,Garilli,B.,et al.2018,A&A,609,A84
Spolaor,M.,Kobayashi,C.,Forbes,D.A.,Couch,W.J.,&Hau,G.K.T.2010,MNRAS,408,272
Tamura,N.,&Ohta,K.2000,AJ,120,533
Thibault,S.,Cui,Q.,Poirier,M.,et al.2003,in Proc.SPIE,4841,Instrument Design and Performance for Optical/Infrared Ground-based Telescopes,eds.M.Iye&A.F.M.Moorwood,932
Tortora,C.,&Napolitano,N.R.2012,MNRAS,421,2478
Wang,L.,Li,C.,Kauffmann,G.,&De Lucia,G.2007,MNRAS,377,1419
Wang,Y.,Yang,X.,Mo,H.J.,et al.2008,ApJ,687,919
White,S.D.M.,Tully,R.B.,&Davis,M.1988,ApJ,333,L45
Willmer,C.N.A.,da Costa,L.N.,&Pellegrini,P.S.1998,AJ,115,869
York,D.G.,Adelman,J.,Anderson,Jr.,J.E.,et al.2000,AJ,120,1579
Zehavi,I.,Zheng,Z.,Weinberg,D.H.,et al.2005,ApJ,630,1
Zehavi,I.,Zheng,Z.,Weinberg,D.H.,et al.2011,ApJ,736,59
Zheng,Z.,Wang,H.,Ge,J.,et al.2017,MNRAS,465,4572
1http://vipers.inaf.it
2 http://cesam.lam.fr/vipers-mls
3http://cesam.lam.fr/vipers-mls
4http://vipers.inaf.it/rel-pdr2.html