News from. the Atlas 3D project. Eric Emsellem

Transcription

1 News from the Atlas 3D project Eric Emsellem and the team

2 U - B 10 Mpc Hierarchical Galaxy Formation Dark Matter Gas Density Gas T Stars The Mare Nostrum Simulation = Teyssier et al. Adapted from Faber et al. Red sequence mixture of remnants from mergers of gas-rich galaxies (blue cloud) gas-poor galaxies (red sequence) [e.g. Robertson et al. 2006; Cox et al. 2006; Cattaneo et al. 2006]

3 P(l) From DM halos to galaxies Mergers Interactions, harassment Secular evolution, bars, Bullock et al. (2001) Disk instabilities and clumps Cold accretion (at high z) Star formation, feedback Cooling and shocks 2D/3D Turbulence Small scales physics l = Specific Angular momentum Mare Nostrum = Teyssier et al.

4 Galaxy Classification (z=0) Edwin Hubble The turning fork Bulge / Disk Gas / Dust content Mean stellar Age / Metallicity

5 Galaxy Classification (z=0) Edwin Hubble Kormendy & Bender 1996

6 Complications Beware the Jabberwock my son! Martig & Bournaud 2009 Spheroidal-like galaxies (z=2) can regrow disks Multiple mergers, cold accretion, massive clumps

7 Downsizing Assembly time Formation time De Lucia et al > M sun Ellipticals M > M sun < M sun All galaxies M > 10 9 M sun Stars assembled Stars formed

8 The paradigm Early-type galaxies ~50% of E s spheroid-shaped galaxies ~50% of S0s bulge dominated disk galaxies Edwin Hubble E + S0s ~ 40% of (SDSS) mass Bernardi et al E/S0s are overall red, S0s can have young stars Mergers important to build E s Two flavours of E s? Davies/Nieto/Kormendy/Bender/Lauer... Boxy with flat cores or light deficit, anisotropic, oblate Disky with cusps or light excess, isotropic, triaxial

9 Structure of ellipticals: V/σ diagram «Low» luminosity ellipticals Disky, Rotate faster, isotropic O = big ellipticals = small ellipticals Fast rotation (Davies et al. 1983) Giant ellipticals Boxy, Rotate slowly, likely anisotropic Slow rotation

10 Classification of ellipticals Disky ellipticals are intermediate between big ellipticals and lenticulars (Kormendy & Bender 1996) Big and small ellipticals also distinct in their luminosity profile (Faber et al. 1997; Trujillo et al. 2004) Light Excess/Deficit also defines a (more robust) E-E dichotomy (Kormendy et al. 2009) Small Big Lauer et al. 1995

11 E and S0s Elliptical galaxies are spheroidal look similar from all directions S0 galaxies ( disk + bulge ) look like E if near face-on Some E galaxies show kinematics similar to S0 Need a physical classification

12 The Team PIs: Michele Cappellari, Eric Emsellem, Davor Krajnović, Richard McDermid CoIs : Katey Alatalo, Leo Blitz, Maxime Bois, Frederic Bournaud, Martin Bureau, Alison Crocker, Roger Davies, Tim Davis, Tim de Zeeuw, Pierre-Alain Duc, Sadegh Khochfar, Harald Kuntschner, Pierre-Yves Lablanche, Raffaella Morganti, Thorsten Naab,Tom Oosterloo, Marc Sarzi, Nicholas Scott, Paolo Serra, Lisa Young, Anne-Marie Weijmans Associates: Estelle Bayet, Jean-Charles Cuillandre, Jesus Falcon-Barroso, Gijs Verdoes-Kleijn, Marie Martig, Leo Michel- Dansac, Kristina Nyland, Krysten Shapiro, Remco van der Bosch, Glenn van de Ven

13 Atlas 3D : the sample Observe a complete volume-limited sample of ETGs M K < -21.5, D < 42 Mpc δ 29 < 35º, b > 15º - Bell et al Atlas 3D spirals Parent sample: 871 nearby galaxies No spiral structure (SDSS/DSS2/INT) 260 galaxies Cappellari, EE, DK, et al., 2011 (P1)

14 2D-spectroscopy (SAURON-WHT) Single-dish + interferometric CO (IRAM 30m, CARMA PdB) HI survey (WRST, excl. Virgo) Multi-band and deep Photometry (INT, 2MASS, SDSS, MegaCam) Stellar populations & Dynamical modelling (JAM) Suite of high-res numerical simulations of mergers Simulations in a cosmological context Semi Analytic Modeling (SAM)

15 Press Releases

16 Atlas 3D Project : First results I. Cappellari, Emsellem, Krajnović, McDermid et al (Sample) II. Krajnović, Emsellem, Cappellari et al (Kinematic properties) III. Emsellem, Cappellari, Krajnović et al (Angular momentum) IV. Young, Bureau, Davis et al (CO Singe dish) V. Davis, Bureau, Young et al (CO Tully Fisher relation) VI. Bois, Emsellem, Bournaud et al (Binary disk mergers) VII. Cappellari, Emsellem, Krajnović, McDermid et al (Environment) VIII. Khochfar, Emsellem, Serra, et al (SAM) IX. Duc, Cuillandre, Serra, et al (Deep Imaging) X. Davis, Alatalo, Sarzi, et al (Origin of ionised/molecular gas) XI. Crocker, Kripps, Bureau et al (Dense molecular gas) XII. Lablanche, Cappellari, Emsellem et al (M/L recovery) XIII. Serra, Oosterloo, Morganti et al., 2011 (HI content) + Bois, Bournaud, Emsellem et al (Numerical resolution) + Alatalo, Blitz, Young et al (Large-scale AGN outflow in NGC1266)

17 Slow rotators λ R =0.1 l R R R V V 2 2 Fast rotators Emsellem et al., 2007

18 l R : radial profiles FR have high and rising l R SR have quite flat or decreasing l R Emsellem et al., 2007

19 IFU Stellar angular momentum Emsellem, MC, DK et al., 2011 (P3) λ R R/Re

20 l R : Stellar angular momentum Emsellem, MC, DK et al., 2011 (P3) Early-Type Galaxies mostly fast rotators! (with a mass dependence)

21 l R (Re) l R : the kinematic Zoo Krajnović, EE, MC et al., 2011 (P2) Emsellem, MC, DK et al., 2011 (P3) Non-Rotators e

22 l R (Re) l R : Inclination effects Emsellem, MC, DK et al., 2011 (P3) EDGE-ON FACE-ON e

23 l R (Re) l R : Fast versus Slow rotators Emsellem, MC, DK et al., 2011 (P3) 86% of all nearby ETGs are fast rotators λ R = 0.31 ε e

24 l R (Re) e Fast Rotators Family of oblate rotators Emsellem, MC, DK et al., 2011 (P3) EDGE-ON FACE-ON

25 l R (Re) Trend with Mass Emsellem, MC, DK et al., 2011 (P3) e

26 l R (Re) What about E s and S0 s? Emsellem, MC, DK et al., 2011 (P3) e 20% of FR are E 66% of E are FR

27 Intermediate mass ETGs Misgeld & Hilker 2011 Zoology Star clusters vs galaxies Small vs Big Stellar component: Formation vs Assembly

28 Intermediate mass ETGs Misgeld & Hilker 2011 Zoology Star clusters vs galaxies Small vs Big Stellar component: Formation vs Assembly

29 Morphology-Density relation Cappellari, EE, DK et al., 2011 (P7) FR SR Only 1/3 of systems classified as E s are SR ~4% of the parent sample are Slow Rotators Slow rotators : efficient formation only at high densities Monotonic trends from low to high densities Excludes cluster processes for the onset of fast rotators Processes at the small-groups scale in low density environments

30 Duc, JCC, PS, et al (P9) Duc et al. In prep.

31 NGC 5557 Signatures for a merger Duc, JCC, PS, et al (P9)

32 Molecular Gas CO (1-0) / (2-1) detection + CARMA maps Detection rate 23 % Same in clusters or outside, or from < M_K < -26 No CO in slowly rotating galaxies VIRGO FIELD MISALIGNMENT Angle Young, Bureau, Davis et al., 2011 (P4) Davis, Bureau, Young et al.,2011 (P10) Alatalo et al., 2011, in prep.

33 Molecular+Ionised Gas Misalignment angles Davis, Bureau, Young et al.,2011 (P10)

34 Molecular/Ionised Gas Misalignment Angles: Fast rotators Davis, Bureau, Young et al.,2011 (P10)

35 Molecular/Ionised Gas Misalignment Angles : Slow rotators Davis, Bureau, Young et al.,2011 (P10)

36 NGC 1266 hosts a massive molecular Alatalo et al outflow Regular rotation in center M out(h I + H2) ~ M dm out /dt ~ 13 M yr -1 R out ~ 450 pc t dyn ~ 2.6 Myr t dep ~ 85 Myr

37 Generic Simulations: Binary mergers Bois, EE, FB et al (P6) Fastest ETGs are as spirals (l R ) Most binary mergers Fast Rotators Slow rotators have KDCs, but are TOO flat

38 Probing Growth processes via SAM Khochfar, EE, PS, et al (P8) Growing in size and mass: SF versus Assembly Slow rotators Accrete more material (50-90%), more major mergers (~3), KDCs Very few at z> 2: progenitors should have been fast Complete shut-down of gas cooling Fast rotators: 2/3 have large B/T, 1/3 have low B/T (e.g., stripped in clusters)

39 Morphological Quenching (Martig et al. 2009) Gas in ETGs at very high resolution (~ 5pc) Bournaud et al. 2011, in prep NGC 524

40 Cappellari, Emsellem, Krajnović et al., 2011 (P7)

41 ATLAS 3D comb van den Bergh 1976 Kormendy & Bender 1996 Cappellari, Emsellem, Krajnović et al., 2011 (P7)

42 Our view of ETGs E/S0 separation should be abandoned: results based on this separation consider with scepticism Continuity from spirals: fastest rotators stripped spirals? > 86% of ETGs are disk-like S0, anaemic spiral & regular, each can be barred. Fewer major mergers, lower stellar mass accretion <14% of ETGs have low angular momentum : mostly massive, quiescent, mildly triaxial & rounder than E4 more (gas-rich) major mergers (mostly high z) + minor mergers Only 4% (9% in mass) of local galaxies are ellipticals Environment & local (groups) effects are important Slow rotators in cores of clusters/groups Mass dependent growth process: SF vs Assembly

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