The evolution of passive galaxies

Transcription

1 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

2 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 Van der Wel et al 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?

3 Environmental effects z f = 2 z f = 1.2 z ~ 0.7 EDisCs clusters; Saglia et al 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?

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

5 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 /spaxel Optimal for cluster studies Five gratings (IZ, YJ, H, K, HK) - R ~ 3500 (R ~ 2000 for HK)

6 Study of high- z galaxies with KMOS 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 (3) Bezanson et al (6) 12.0 Onodera et al (1) 12.0 Cappellari et al (2) VIRIAL: VLT IR IFU Absorption Newman et al (12) Line Survey (a) van de Sande et al (3) Bezanson et al. VIRIAL 2013 (6) IZ Onodera et al (1) apple z apple 1.45 Cappellari et al (2) Newman et al (12) (P.I. T. Mendel, R. Saglia; Mendel et al & in prep.) Stellar Mass [log M ] Absorption line kinematics 11.0 of ~130 passive galaxies at z > 1.5 UVJ- selected passive galaxies in the CANDELS VIRIAL YJ (124) fields VIRIAL IZ (92) Goal: Stellar kinematics for passive galaxies in the field (a) Stellar Mass [log M ] Dynamical Mass [log M ] U-V (b) Passive Star forming VIRIAL YJ (124) VIRIAL IZ (92) VIRIAL YJ IZ appleapple zzapple apple 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. 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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, anecdotal Noeske Onoderaetetal. or al. important 2007, 2012, ApJL, ApJ, phases?, 660, 755, Paris, Onodera Peng et October al. et al. 2010, , ApJ, ApJ, 721, 755, 26 Peng et al. 2010, ApJ, 193 Saglia et al. 2010, A&A, 524, 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, 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) 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 log SSFR [Gyr 1 ] VIRIAL YJ 1.45 apple z apple 2.0 Courtesy: T. Mendel Av = 1mag V-J

7 The KMOS- Cluster Survey - Sample RCS z = 1.04 Jee et al XMMUJ z = 1.39 Mullis et al XMMXCSJ z = 1.46 Jee et al Cl z = 1.62 Kurk et al JKCS 041 z = 1.8 Newman et al 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

8 The KMOS- Cluster Survey Since P92: 90 sources - in YJ hr/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

9 The KMOS- Cluster Survey

10 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 Structural parameters (rest- B): - Size / Effective radius R e - Source surface brightness I e KMOS source extraction spaxels

11 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

12 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 Passive galaxies in XMMUJ 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

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

14 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 XMMXCSJ and Cl ages are consistent with the field. XMMUJ passive population has older ages. On- going projects / perspectives: z = 1.8 cluster SF fillers / gas kinematics

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

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

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

18 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