Observing Galaxy Evolution in the Stormy Environment of Shapley Supercluster

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1 Observing Galaxy Evolution in the Stormy Environment of Shapley Supercluster Paola Merluzzi INAF - Osservatorio Astronomico di Capodimonte Napoli - Italy & G. Busarello, C.P. Haines, A. Mercurio, M.A. Dopita, K. A. Pimbblet, D. Steinhauser, N. Okabe, A. Grado, L. Limatola, H. Bourdin

2 Shapley Supercluster Survey: ShaSS to investigate the role of cluster-scale mass assembly on galaxy evolution to map the effects of the environment out to the cluster outskirts along the galaxy filaments

3 Shapley Supercluster Survey: ShaSS 23 sq. deg. (260 Mpc 2 ) around the core of the Shapley supercluster UV - Galex OPTICAL - ugri VST NIR - K VISTA (+ WISE W1, W2) MIR - Spitzer MIPS (+ WISE W3) fibre S - AAOmega + lit. IFS - ANU 2.3m X-ray - XMM Radio - lit. depth r*+8.5

4 VST : sub-kpc resolution Data: optical imaging 60 arcsec

5 Ram-pressure stripping: how and where multi-wavelengths detailed studies e.g. Owen et al Cortese et al Donahue & Vogt Sun et al Abramson et al Vollmer et al Jáchym et al Merluzzi et al Yagi et al Fumagalli et al Abramson & Kenney Kenney et al simulations e.g. Roediger & Hensler Kronberger et al Roediger & Brügger 2008 Kapferer et al Jáchym et al Tonnesen & Bryan Bekki 2009, Bekki & Couch Book & Benson 2010 Steinhauser et al Bischko et al

6 Ram-pressure stripping: how and where beyond Gunn & Gott (1972) low-mass galaxies in poor environments truncates, but also bends the gas disc of massive spirals efficiently contributes to transform galaxies outside the cluster core compresses and shocks the ISM temporarily enhancing star formation both in the disc and in the tail acts in different phases open issues how many cluster galaxies and how differently are affected by RPS? does the cluster mass or the cluster dynamics matter? where do the cluster galaxies feel the ram-pressure: infalling from the filaments, crossing cold fronts? observational bias geometry timing disentangle between RPS and tidal interaction (TI) sensitivity

7 ANU 2.3m telescope Dual beam image-slicing integral field spectrograph Spectral range: Å fov: 25 x 38 arcsec 950 spectra L*+2 galaxy WiFeS observations: WiFeS field of view 40 kpc gas and stellar kinematics nature of the gas emission star formation across the galaxy abundances dust attenuation

Extraplanar emission: RPS or TI? ShaSS-403015754 composite gri ShaSS-408053848 K=K*+2.1 M star 1.

8 Extraplanar emission: RPS or TI? ShaSS composite gri ShaSS K=K*+2.1 M star M ʘ SFR UV+FIR 2.5 M ʘ yr -1 K=K*+2.7 M star M ʘ SFR UV+FIR 1.4 M ʘ yr -1 (Merluzzi et al. submitted)

ShaSS-403015754: ionized gas velocity field Ionized gas: gas extending up to 30 kpc in

9 ShaSS : ionized gas velocity field Ionized gas: gas extending up to 30 kpc in projection from the galaxy centre truncated disc and large-scale regular motion up to kpc

10 ShaSS : RPS vs. TI companion ~17 kpc in projection and ΔV~300 km s -1 extraplanar emission toward the companion, but with extraplanar ionized gas extending further in projection truncated gas disc rotational component is preserved into the extraplanar ionized gas asymmetric velocity profile of the gas fairly symmetric stellar velocity profile gas e stellar velocity components are decoupled peak of star formation in the centre dominated by a young (< 1 Gyr) stellar component star formation in the West leading edge ρ ICM V 2 = 2π G Σ ISM Σ * V > 450 km s -1

ShaSS-403015754: simulations AREPO: sator arepo tenet opera rotas (Springel 2010) 2 10 5 particles/cells for the stellar and gas disc 5 10 4 particles for the stellar bulge wind-tunnel contains on

11 ShaSS : simulations AREPO: sator arepo tenet opera rotas (Springel 2010) particles/cells for the stellar and gas disc particles for the stellar bulge wind-tunnel contains on average gas cells. V w = 500, 750, 1000, 1500 km s -1 β = ρ ICM = gcm -3 model: V w = 750 km s -1 β= 30 ρ ICM = gcm Myr star formation history 2 SFR ~200 Myr ago

12 ShaSS : ionized gas velocity field Ionized gas: gas tail up to kpc truncated gas disc

13 SOS-90630: RPS vs. TI 4-5 more massive companion ~68 kpc in projection and ΔV~320 km s -1 in redshift extraplanar emission toward the companion truncated gas disc the gas tail follows the galaxy rotation fairly symmetric stellar velocity profile double nuclei ρ ICM V 2 = 2π G Σ ISM Σ * V > 300 km s -1

ShaSS-408053848: simulations V w = 500, 1000 km s -1 β =

14 ShaSS : simulations V w = 500, 1000 km s -1 β = ρ ICM = , gcm -3 merging + RPS (Bischko et al 2015) TI + RPS (Kapferer et al. 2008) model: V w = 500 km s -1 β = 80 ρ ICM = gcm -3 t = 370 Myr

15 ShaSS : simulations current SF model: V w = 500 km s -1 β = 80 ρ ICM = gcm -3 t = 370 Myr

16 ShaSS (Merluzzi et al. 2013) K=K* M star M ʘ SFR UV+FIR 8.5 M ʘ yr -1 BRK composite

ShaSS-408053060: gas and stellar kinematics Complex gas velocity field extending 13 kpc from the disc High gas velocity

17 ShaSS : gas and stellar kinematics Complex gas velocity field extending 13 kpc from the disc High gas velocity dispersion with maxima in the regions of the detached gas and in the opposite disc side ρ ICM V 2 = 2π G Σ ISM Σ * V > 550 km s -1

ShaSS-408053060: simulations V w = 830-2600 km s -1 β = 15-85 ρ ICM = 1.

18 ShaSS : simulations V w = km s -1 β = ρ ICM = gcm -3 model data β = 45 V wind = 1400 km s -1 t ~ 60 Myr a starburst with 5x increase in SFR over the last 100 Myr (SW disc)

19 i = i* - 1 M star M ʘ SFR 6 M ʘ yr -1 ShaSS

22 X-ray surface brightness XMM-Newton KeV

23 Conclusions RPS (+ TI + merging +...): multi-band data + IFS + simulations (e.g. Vollmer et al. 2005, Cortese et al , Cortés et al. 2015) RPS often temporarily enhances SF also in the disc (e.g Kromberger et al. 2008, Merluzzi et al. 2013) RPS can take place everywhere and affect any cluster/group galaxy at least in the Shapley supercluster

Dissecting jellyfish galaxies with MUSE

Dissecting jellyfish galaxies with MUSE Yara L. Jaffé (ESO Chile) & the GASP collaboration reviewby byboselli Boselli &&Gavazzi (2006) SeeSee review Gavazzi (2006) Gas stripping of cluster galaxies cold