The evolution of passive galaxies

The evolution of passive galaxies in z ~ 1.5 galaxy clusters with KMOS in a z = 0.65 LSS with VIMOS Audrey Galametz - MPE, Garching On behalf of the KCS GTO Program: A. Beifiori, R. Bender, M. Cappellari, J. Chan, R. Davies, A. Galametz, R. Houghton, T. Mendel, L. Prichard, R. Saglia, R. Sharples, R. Smith, J. Stott, D. Wilman

Formation history of passive galaxies In the local Universe: Red sequence Early formation / old ages Fundamental plane zp varies M/L varies At z > 1: Smaller sizes (factor 3-5) More compact (e.g., van de Sande 2013) More disky (van der Wel et al 2011) Younger at fixed M * (Bezanson et al. 2013) Bezanson et al. 2013 Van der Wel et al. 2014 Pushing kinematics and stellar population analysis to higher z Absorption- line diagnostics are hard Optical rest- frame at 1 < z < 2 is challenging What were the properties of passive galaxies near their epoch of formation?

Environmental effects z f = 2 z f = 1.2 z ~ 0.7 EDisCs clusters; Saglia et al. 2010 Different evolution of the M/L in cluster and field galaxies Most massive galaxies in clusters have formed the bulk of their stars at z > 1.5 Shortage of derived kinematics in dense environments at z > 1.3 How do passive galaxy properties depend on the environment?

The evolution of passive galaxies in z ~ 1.5 clusters with KMOS Stellar kinematics of passive galaxies at z~1.5 in dense environments

The K- band Multi- Object Spectrograph Integral- Field Unit (IFU) spectrograph in the near- infrared 24 Arms 7.2 patrol field 2.8 x 2.8 FoV - 0.2 /spaxel Optimal for cluster studies Five gratings (IZ, YJ, H, K, HK) - R ~ 3500 (R ~ 2000 for HK)

Study of high- z galaxies with KMOS (GTO @MPE) KMOS 3D Survey (P.I. N. Forster- Schreiber, D. Willman): ~600 galaxies at 0.7 < z < 2.7 in the CANDELS fields Goals: Gas kinematics (H α maps); gas metallicity etc. Well- calibrated environmental metrics: Science goals. With these observations we will address: The evolution of galaxy structure Mergers are expected to transform the disky, compact quies galaxies observed at high redshift into the early-type galaxy population we observe locally (e.g., van der et al. 2011). Such violent interactions should have a corresponding impact on galaxies stellar dynam Establishing the connection between galaxy structure available from high-resolution CANDELS imagin and stellar dynamics accessible by KMOS is therefore crucial to understanding the role of mergers vs. sec processes in the formation of early-type galaxies. The relationship between galaxies and their haloes VIRIAL will provide a flux-limited sampl galaxy stellar kinematics, and allow us to directly probe the connection between galaxies and their halo high redshift for the first time. In phenomenological models of quenching the suppression of star forma depends on both galaxy stellar mass and environment (e.g., Peng et al. 2010). The parent 3D-HST sam will allow us to study quiescent galaxies in the context of the full density field and explore connections betw galaxy properties and their host environment (e.g., Wilman et al. 2010). Quenching As part of VIRIAL we will obtain rest-frame optical spectra that probe Balmer absorption l and the 4000Å break, both of which are sensitive diagnostics of recent star-formation activity and can be u to di erentiate between various physical models of the quenching process. The observed correlation of gal structure and star-formation activity (e.g., Wuyts et al. 2011) suggests that central stellar mass den plays an important role in regulating star-formation. However, establishing a causal relationship betw bulge growth and quenching requires more precise assessment of star-formation histories than is possible u photometric data alone. Attachments (Figures) Fossati et al. submitted Wisnioski et al.~2015 van de Sande et al. 2013 (3) Bezanson et al. 2013 (6) 12.0 Onodera et al. 2012 (1) 12.0 Cappellari et al. 2009 (2) VIRIAL: VLT IR IFU Absorption Newman et al. 2010 (12) Line Survey (a) van de Sande et al. 2013 (3) Bezanson et al. VIRIAL 2013 (6) IZ Onodera et al. 2012 (1) 2.0 1.2 apple z apple 1.45 Cappellari et al. 2009 (2) Newman et al. 2010 (12) 11.5 11.5 1.5 (P.I. T. Mendel, R. Saglia; Mendel et al. 2015 & in prep.) Stellar Mass [log M ] Absorption line kinematics 11.0 of ~130 passive galaxies 11.0 1.0 at z > 1.5 UVJ- selected passive galaxies in the CANDELS VIRIAL YJ (124) fields 10.5 10.5 0.5 VIRIAL IZ (92) Goal: Stellar kinematics for passive galaxies in the field (a) Stellar Mass [log M ] 10.5 11.0 11.5 12.0 Dynamical Mass [log M ] U-V (b) Passive Star forming VIRIAL YJ (124) VIRIAL IZ (92) VIRIAL YJ IZ 1.45 1.2 appleapple zzapple apple1.45 2.0 10.5 0.0 11.00.5 11.51.0 12.01.5 2.0 0.0 0.5 1.0 1.5 2.0 Dynamical Mass [log V-J M ] V-J Figure 1. (a) VIRIAL will provide Figure velocity 1. (a) dispersion VIRIAL will measurements, provide velocity and hence dispersion dynamical measurements, masses, for and >200 hence dynamical masses, for > galaxies at z>1.2. Symbols indicate galaxiesstellar at z>1.2. vs. dynamical Symbolsmass indicate for galaxies stellar vs. with dynamical 1.2 <z<2.0 mass for drawn galaxies fromwith 1.2 <z<2.0 drawn f the literature, while the underlying the literature, greyscale while showsthe underlying distributiongreyscale of SDSSshows galaxies theindistribution same parameter of SDSS galaxies in the same param space. Black lines and shadingspace. show the Black expected lines and coverage shading of show VIRIAL thetargets expected (see coverage Boxes 7ofand VIRIAL 8). (b) targets We (see Boxes 7 and 8). (b) identify passive galaxies based on identify their passive U V and galaxies V Jbased colours on in their twou di erent V andredshift V J colours slices corresponding two di erent redshift slices correspond to the KMOS IZ and YJ filters. to the Black KMOS pointsizshow andthe YJ distribution filters. Black ofpoints selected show VIRIAL the distribution targets. Underlying of selected VIRIAL targets. Underly shading shows the distribution of shading U V and shows V the J colour distribution for galaxies of U in V the andparent V J colour 3D-HST forsample galaxiescolour-coded in the parent 3D-HST sample colour-co by mean specific-sfr. by mean specific-sfr. References: Belletal.2012,ApJ,753,167 References: Bezanson Belletal.2012,ApJ,753,167 et 2009, 697, 1290; Bezanson 2013, ApJ, et764, al. 2009, 8 Brammer ApJ, 697, et 1290; al. 2012, 2013, ApJS, ApJ, 764, 8 Brammer et al. 2012, A 200, 13 Bundy et al. 2010, ApJ, 719, 200, 1969 13 Bundy Cappellari et al. et 2010, al. 2004, ApJ, PASP, 719, 1969 116, 138; Cappellari 2009, ApJ, et al. 704, 2004, 34 PASP, Ceverino 116, et138; al. 2009, 2010, ApJ, 704, 34 Ceverino et al. 2 MNRAS, 404, 2151 Dekel et al. 2009, MNRAS, ApJ, 703, 404, 785 2151 van Dekel Dokkum et al. et2009, al. 2009, ApJ, Nature, 703, 785460, van717; Dokkum 2010, et ApJ, al. 709, 2009, 1018 Nature, Elbaz 460, 717; 2010, ApJ, 709, 1018 E et al. 2007, A&A, 468, 33 Genzel et etal. al. 2008, 2007, ApJ, A&A, 687, 468, 5933 Graves Genzel et et al. al. 2010, 2008, ApJ, ApJ, 717, 687, 803 59 Hilz Graves et al. et 2012, al. 2010, MNRAS, ApJ, 717, 425, 803 Hilz et al. 2012, MNRAS, 3119 Karim et al. 2011, ApJ, 730, 3119 61 Knobel Karimetetal. al. 2013, 2011, ApJ, 769, 730, 2461 Kriek Knobel et al. et al. 2009, 2013, ApJ, ApJ, 700, 769, 22124 Lilly Kriek et et al. al. 2013, 2009, ApJ, 700, 221 Lilly et al. 2 ApJ, 772, 119 Mendel et al. 2013, MNRAS, ApJ, 772, 429, 1192212 Mendel Moster et al. et 2013, al. 2013, MNRAS, MNRAS, 429, 428, 22123121 Moster Newman et al. 2013, et al. MNRAS, 2010, ApJ, 428, 717, 3121 Newman et al. 2010, ApJ, Audrey Galametz The evolution of passive 103; 2012, galaxies ApJ, 746, Workshop 162 Noeske High et Redshift 103; al. 2007, 2012, (proto)clusters: ApJL, ApJ, 746, 660, 162 43 anecdotal Noeske Onoderaetetal. or al. important 2007, 2012, ApJL, ApJ, phases?, 660, 755, 43 26 Paris, Onodera Peng et October al. et al. 2010, 2016 2012, ApJ, ApJ, 721, 755, 26 Peng et al. 2010, ApJ, 193 Saglia et al. 2010, A&A, 524, 6 193 van Saglia de Sande et al. et2010, al. 2013, A&A, ApJ, 524, 771, 6 85 van Toft de Sande et al. et 2012, al. 2013, ApJ, ApJ, 754, 3771, Trujillo 85 Toft et al. et al. 2007, 2012, ApJ, 754, 3 Trujillo et al. 2 MNRAS, 382, 109 van der Wel et al. MNRAS, 2011, ApJ, 382, 730, 109 38 van Whitaker der Wel et al. 2011, 2013, ApJ, ApJL, 730, 770, 3839 Whitaker Williamset etal. al. 2013, ApJL, ApJ, 691, 770, 39 Williams et al. 2013, ApJ, U-V (b) 2.0 1.5 1.0 0.5 Passive Star forming KCS: KMOS- Cluster Survey (P.I. R. Bender, R. Davies) Beifiori et al. in prep MPE/USM Munich + Oxford/Durham Collaboration Absorption line kinematics of ~100 quiescent galaxies at z > 1.4 in clusters Aim: Stellar kinematics for passive galaxies in dense environments Av = 1mag 2.0 1.5 1.0 0.5 0.0 0.5 log SSFR [Gyr 1 ] VIRIAL YJ 1.45 apple z apple 2.0 Courtesy: T. Mendel Av = 1mag 0.0 0.5 1.0 1.5 2.0 V-J

The KMOS- Cluster Survey - Sample RCS234526-3632.6 z = 1.04 Jee et al. 2011 XMMUJ2235-2557 z = 1.39 Mullis et al. 2005 XMMXCSJ2215. 9-1738 z = 1.46 Jee et al. 2011 Cl0332-2742 z = 1.62 Kurk et al. 2009 JKCS 041 z = 1.8 Newman et al. 2013 Redshift Cluster selection / Requirements: Multi- band HST photometry (for light/mass- weighted structural parameters) Deep complementary imaging (for red- sequence studies and SED fitting) Large number of spectroscopically confirmed members (for selection efficiency) Adequate redshift to avoid absorption lines falling into telluric contaminated regions

The KMOS- Cluster Survey Since P92: 90 sources - in YJ - 15-20hr/source 70 red sequence targets ~30 confirmed or new redshifts 20 stellar velocity dispersions First measurements in dense regions at z > 1.3 Literature z > 1.35: 27 sources KCS: 20 new measurements

The KMOS- Cluster Survey

The fundamental plane of cluster galaxies at z~1.5 Beifiori et al. in prep Image Model Residuals KMOS stellar velocity dispersions σ e : - ppxf (Cappellari & Emsellem 2004) - Maraston &Strömbäck (2011) SSP models based on the ELODIE v3.1 stellar library HST (archival + new Cycle 22 WFC3): - - Chan et al. 2016 Structural parameters (rest- B): - Size / Effective radius R e - Source surface brightness I e KMOS source extraction spaxels

The fundamental plane of cluster galaxies at z~1.5 Beifiori et al. in prep Low- z reference: z = 0 Coma cluster (Jørgensen et al. 2006) - z~0.7: EDisCS (Saglia et al. 2010) Assume homology - Adopt local slope coefficients Evolution of mass- to- light ratio with z (galaxies are getting younger) Different evolution/formation age for different clusters

The fundamental plane of cluster galaxies at z~1.5 Beifiori et al. in prep z = 1.39: 3.18 ± 0.63 Gyr z = 1.46: 1.78 ± 0.34 Gyr z = 1.61: 1.37 ± 0.33 Gyr FP ages consistent with luminosity- weighted ages derived from stack- and- fit of galaxies using Mendel et al. 2015 Passive galaxies in XMMUJ2235-2557 have much older median ages than in the two other structures. Stopped their SF earlier Accelerated evolution for galaxies in more massive and virialized clusters

Passive galaxies evolution in different environments Cl0332 XMMXCSJ2215 XMMUJ2235 Mendel et al. 2015 Mendel et al. 2015

Conclusions / Perspectives 20 (for now) new measurements of stellar σ e in clusters at z~1.5 Older ages in massive and virialized clusters than in the field XMMXCSJ2215.9 and Cl0332-2742 ages are consistent with the field. XMMUJ2235-2557 passive population has older ages. On- going projects / perspectives: z = 1.8 cluster SF fillers / gas kinematics

The evolution of passive galaxies in a large- scale structure at z=0.65 in UDS

LSS at z ~ [0.6-0.7] in UKIDSS UDS VIMOS follow- up - 6 masks; ~750 sources

LSS at z ~ [0.6-0.7] in UKIDSS UDS ~ 10 confirmed clusters/groups - 3 LSS at z ~ 0.6-0.7 Confirmed super- cluster at z = 0.645: 8 confirmed clumps including at least 2 clumps with M 200 10 14 M Galametz et al. in prep

The LSS passive population Class E: Strong Absorption only Class E/SF: Strong Abs + Emission (EW[OII] < - 5A) Class SF: Strong Emission - Stellar velocity dispersions for ~115 sources (Ppxf / miuscat Vazdekis 2012 SSP models) - Structural parameters from CANDELS & UKIDSS