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THE ALHAMBRA SURVEY: EVOLUTION of GALAXY SPECTRAL SEGREGATION Ll Draft version August 11, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 THE ALHAMBRA SURVEY: EVOLUTION OF GALAXY SPECTRAL SEGREGATION Ll. Hurtado-Gil1,2, P. Arnalte-Mur1, V. J. Mart´ınez1,3,4, A. Fernandez-Soto´ 2,4, M. Stefanon5, B. Ascaso6,21, C. Lopez-Sanju´ an´ 8, I. Marquez´ 7, M. Povic´7, K. Viironen8, J. A. L. Aguerri9,10, E. Alfaro7, T. Aparicio-Villegas11,7 N. Ben´ıtez7, T. Broadhurst12,13, J. Cabrera-Cano~ 14, F. J. Castander15, J. Cepa9,10, M. Cervino~ 7,9,10, D. Cristobal-Hornillos´ 8, R. M. Gonzalez´ Delgado7, C. Husillos7, L. Infante16, J. Masegosa7, M. Moles8,7, A. Molino17,7, A. del Olmo7, S. Paredes18, J. Perea7, F. Prada7,19,20, J. M. Quintana7 Draft version August 11, 2018 Abstract We study the clustering of galaxies as a function of spectral type and redshift in the range 0:35 < z < 1:1 using data from the Advanced Large Homogeneous Area Medium Band Redshift Astronomical (ALHAMBRA) survey. The data cover 2.381 2 deg in 7 fields, after applying a detailed angular selection mask, with accurate photometric redshifts [σz < 0:014(1 + z)] down to IAB < 24. From this catalog we draw five fixed number density, redshift-limited bins. We estimate the clustering evolution for two different spectral populations selected using the ALHAMBRA-based photometric templates: quiescent and star-forming galaxies. For each sample, we measure the real-space clustering using the projected correlation function. Our calculations are −1 −1 performed over the range [0:03; 10:0]h Mpc, allowing us to find a steeper trend for rp . 0:2h Mpc, which is especially clear for star-forming galaxies. Our analysis also shows a clear early differentiation in the clustering properties of both populations: star-forming galaxies show weaker clustering with evolution in the correlation length over the analysed redshift range, while quiescent galaxies show stronger clustering already at high redshifts, and no appreciable evolution. We also perform the bias calculation where similar segregation is found, but now it is among the quiescent galaxies where a growing evolution with redshift is clearer.These findings clearly corroborate the well known colour-density relation, confirming that quiescent galaxies are mainly located in dark matter halos that are more massive than those typically populated by star-forming galaxies. 1. INTRODUCTION VVDS galaxies covering half a square degree, have unam- It has been well established that different types biguously established that early-type galaxies are more of galaxies cluster in different ways (Hamilton 1988; strongly clustered than late-type galaxies at least since redshift z ∼ 1:2. The correlation length obtained by Davis et al. 1988; Dom´ınguez-Tenreiro & Mart´ınez1989; −1 Einasto 1991; Loveday et al. 1995; Guzzo et al. 1997; Li these authors for late-type galaxies is r0 ∼ 2:5h Mpc at et al. 2006; Mart´ınezet al. 2010; Phleps et al. 2006). El- z ∼ 0:8 and roughly twice this value for early-type galax- liptical galaxies are preferentially located at the cores of ies. They have also calculated the relative bias between rich galaxy clusters, i.e, in high density environments, the two types of galaxies obtaining an approximately con- while spiral galaxies are the dominant population in the stant value brel ∼ 1:3 − 1:6 for 0:2 ≤ z ≤ 1:2 depending field (Davis & Geller 1976; Dressler 1980; Giovanelli et al. on the sample. This value is slightly larger than the one 1986; Cucciati et al. 2006). This phenomenon, called obtained by Madgwick et al. (2003) brel ∼ 1:45 ± 0:14 galaxy segregation, has been confirmed in the largest for the 2dF Galaxy Redshift Survey with median red- galaxy redshift surveys available up to date, the 2dF shift z = 0:1. The results obtained by Coil et al. (2008) Galaxy redshift survey (2dFGRS, Madgwick et al. 2003), for DEEP2 reinforced those outlined above, although the the Sloan Digital Sky Survey (SDSS, Abbas & Sheth measured correlation lengths for DEEP2 galaxies are sys- 2006; Zehavi et al. 2011) and the Baryonic Oscillation tematically slightly larger than the values reported for Spectroscopic Survey (BOSS, Guo et al. 2013). The de- the VVDS sample by Meneux et al. (2006). In addition, Coil et al. (2008) have detected a significant rise of the pendence of clustering on different galaxy properties such −1 as stellar mass, concentration index, or the strength of correlation function at small scales rp ≤ 0:2h Mpc for the 4000 A-break˚ has been studied by Li et al. (2006). their brighter samples. For the zCOSMOS-Bright red- Since segregation is a consequence of the process of shift survey, de la Torre et al. (2011) found also that early-type galaxies exhibit stronger clustering than late- arXiv:1601.03668v1 [astro-ph.GA] 14 Jan 2016 structure formation in the universe, it is therefore very −1 important to understand its evolution with redshift or type galaxies on scales from 0:1 to 10h Mpc already at cosmic time. Several works have extended the analysis z ' 0:8, and the relative difference increases with cosmic of segregation by colour or spectral type to redshifts in time on small scales, but does not significantly evolve the range z ∼ 0:3−1:2 using recent spectroscopic surveys from z = 0:8 to z = 0 on large scales. A similar re- such as the VIMOS-VLT Deep Survey (VVDS, Meneux sult is reported by Skibba et al. (2014). These authors et al. 2006), the Deep Extragalactic Evolutionary Probe show that the clustering amplitude for the PRIMUS sam- ple increases with color, with redder galaxies displaying 2 survey (DEEP2, Coil et al. 2008), or the PRIsm Multi- −1 object Survey (PRIMUS, Skibba et al. 2014). De la stronger clustering at scales rp ≤ 1h Mpc. They have Torre et al. (2011), instead, used the zCOSMOS survey also detected a color dependence within the red sequence, to study segregation by morphological type at z ∼ 0:8. with the reddest galaxies being more strongly correlated All these studies show that segregation by colour or than their less red counterparts. This effect is absent in spectral type was already present at z ∼ 1. In par- the blue cloud. ticular, Meneux et al. (2006), using a sample of 6,500 Several broad-band photometric surveys have extended these studies to even larger redshift (e.g. Hartley et al. 2 2010; McCracken et al. 2015). Hartley et al., using data ent behaviour for galaxies with spectral energy distribu- from the UKIDSS Ultra Deep Survey, find segregation tions corresponding to quiescent or star-forming types. between passive and star-forming galaxies at z . 1:5, Contamination by AGNs is minor (approximately 0.1% but find consistent clustering properties for both galaxy of the sources could correspond to this class, which has types at z ∼ 2. not been purged from the ALHAMBRA catalogues) and In the present paper we use the high-quality data of the should be dominated by low-luminosity AGN, which are Advanced Large Homogeneous Area Medium-Band Red- in many cases fit by strong emission-line galaxies with an shift Astronomical survey (ALHAMBRA) (Moles et al. approximately correct redshift. 2008; Molino et al. 2014)1 to study the clustering seg- Object detection is performed over a synthetic im- regation of quiescent and star-forming galaxies. AL- age, created via a combination of ALHAMBRA filters, HAMBRA is very well suited for the analysis of galaxy that mimics the Hubble Space Telescope F814W filter clustering and segregation studies at very small scales. (hereafter denoted by I) so that the reference magnitude With a reliable calculation of the projected correlation is directly comparable to other surveys. Photometric function we find a clear steepening of the correlation at redshifts were obtained using the template-fitting code scales between 0:03 to 0:2h−1 Mpc (Phleps et al. 2006; BPZ (Ben´ıtez2000), with an updated set of 11 Spectral Coil et al. 2008), specially for the star-forming galax- Energy Distribution (SED) templates, as described in ies. Moreover, its continuous selection function over a Molino et al. (2014). Although a full posterior probabil- large redshift range makes ALHAMBRA an ideal sur- ity distribution function in redshift z and spectral type vey for evolution studies. In Arnalte-Mur et al. (2014) T is produced for each object, in this work we take a sim- (hereafter AM14) the authors presented the results of pler approach and assign to each galaxy the redshift zb −1 the evolution of galaxy clustering on scales rp < 10h and type Tb corresponding to the best fit to its observed Mpc for samples selected in luminosity and redshift over photometry. We have checked that the errors induced by ∼ 5 Gyr by means of the projected correlation function the redshift uncertainties, which are partly absorbed by wp(rp). In this paper we use the same statistic to study the deprojection technique, are under control as long as the evolution of galaxy segregation by spectral type at we use relatively bright galaxies with good quality pho- 0:35 < z < 1:1. tometric redshift determinations. This makes ALHAM- Details on the samples used in this analysis are de- BRA a very well suited catalogue: together with the high scribed in Section 2. In Section 3, we introduce the resolution photometric redshifts, the abundant imaging statistic used in our analysis, the projected correlation allows us both a reliable color segregation, used in this function, and the methods to obtain reliable estimates work, and a high completeness in the galaxy population of this quantity and to model the results. Finally, in at small scale separations, which will be the specific ob- Section 4, we present our results, and in Section 5 the ject of a future work.
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