Mariya Lyubenova, Glenn van de Ven

Transcription

1 Mariya Lyubenova, Glenn van de Ven and the CALIFA collaboration Galaxies Inside & Out Tehran January 2015

2 TH UNIVRS IN MOTION AGL simulation movie

3 TH IMPORTANC OF AM Angular momentum is set early on in the life of galaxies Importance for discriminating formation and evolution scenarios Angular momentum in DM halos shows a narrow distribution with hardly any evolution in redshift or mass volution in baryons much more complex Star formation Feedback Dynamical instabilities.. Kimm et al. (arxiv: )

4 AM OF LLIPTICAL GALAXIS Originally ellipticals thought to be axisymmetric flattened by rotation Giant ellipticals rotate slowly and are likely triaxial (Bertola & Capaccioli 1975; Binney 1978) Faint ellipticals rotate more rapidly Consistent with isotropic rotators (Davies et al. 1983) Tend to have disky isophotes (Bender et al. 1989) Do they actually contain disks? (Rix & White 1990) Kormendy & Illingworth (1982)

5 OBSRVATIONAL CONSTRAINTS Krajnović et al. (2011) arly studies on this issue (e.g. Bertola & Capaccioli 1978; Binney 1978; Davies et al. 1983; Franx et al. 1989) Difficult to gather large samples to homogeneously study this aspect SAURON and ATLAS3D Slow/Fast rotators Defined AM parameter (λ R )

6 LOOKS CAN B DCIVING TH CAS OF ARLY-TYP GALAXIS lliptical galaxies are spheroidal look similar from all directions galaxies (disk+bulge) look like if near face-on Some galaxies show kinematics similar to

7 Large-scale rotation Fast Rotators 40% classified by RC3 as ellipticals

8 Slowly rotating SAURON galaxies General agreement with RC3

9 New Kinematic Quantifier: λ R SAURON galaxies show either ordered rotation, or no rotation except for decoupled component How to quantify the spatial difference in velocity maps? Weighted with Radius NGC3379 NGC5813 Sky-averaged - Need IFU Normalized by Mass (msellem et al. 2007)

10 Angular Momentum in TGs (msellem et al. 2007) AM profiles (with radius) were different Marked difference in integrated (1Re) values

11 A NW STP FORWARD ATLAS3D The ATLAS3D project provides the best current mapping of stellar kinematics for early-type galaxies in the nearby Universe (Cappellari et al. 2011) Large variety of kinematic features (Krajnović et al. 2011) Angular momentum in early-type galaxies expand over a large range (msellem et al. 2011) Still restricted to early-type galaxies msellem et al. (2011)

12 Color TH CALIFA SURVY Where and when do the stars in galaxies form? How is angular momentum lost and found? Where and when are the heavy elements made? How is the gas in galaxies processed? Absolute Magnitude

13 TH CALIFA SURVY IFU survey using the CAHA 600 galaxies in the local universe (0.005 < z < 0.03) Large wavelength coverage Large FoV (2 Reff) with 1 kpc spatial resolution Large, homogeneous sample across the Hubble sequence V1200 (R 1650) V500 (R 850)

14 TH CALIFA SURVY Granted 210 dark nights at CAHA over 3 years 80 scientists from 20 institutions in 7 countries PI: S. Sanchez (IAA), PS: C.J. Walcher (AIP) 400 objects observed in both setups ( 500 V500) 20 refereed articles already published Automatic data reduction pipeline working, v.1.4 Data Release 2: October 2014! 200 objects with good quality

15 COLOR MAGNITUD DIAGRAM Observed V1200 sample (300 galaxies) covers from the Red Sequence and the Blue Cloud

16 SAMPL PROPRTIS (300 galaxies) Rmax/Reff,major Selection allows for volume corrections Good coverage across Hubble sequence Most galaxies reaching up to 2 Reff

17 Vel. dispersion Velocity GALAXIS AR COMPLX Slow Rotator (low V, high σ) Bulge + Disk (high V, high σ) Pure disk (high V, low σ) Interacting (e.g. ARP220)

18 ANGULAR MOMNTUM ACROSS HUBBL SQUNC Alternative to the classical (V/σ) vs ellipticity diagram developed by SAURON & A3D Distribution of CALIFA TGs galaxies similar to A3D Target selection favours edge-on over face-on galaxies This samples two areas: Very Fast rotators Low-λ Re spiral galaxies

19 Color TH CALIFA SURVY Are lenticulars faded spiral galaxies? Are low-mass (spiral) galaxies DM dominated? Absolute Magnitude

20 Are lenticulars faded spirals?

21 AR LNTICULARS FADD SPIRALS? What processes dominate this Morphological (kinematic) transition? Minor/Major mergers nvironmental processes (e.g. harrasment) Secular evolution van den Berg (1976) The idea has been around for some time (e.g. van den Berg 1976) Cappellari et al. (2011) Revived again recently (e.g. Laurikainen et al. 2010, A3D team, Kormendy & Bender 2012) Kormendy & Bender (2012)

22 AR LNTICULARS FADD SPIRALS? Fading explains offset of galaxies in Tully-Fisher relation Also explains observed specific frequency of globular clusters in s Bedregal et al. (2006) Aragón-Salamanca et al. (2006)

23 AR LNTICULARS FADD SPIRALS? (ANGULAR MOMMTUM CONSISTNCY) YS? NO YS? YS Sa galaxies in general compatible with FRs Many Sb galaxies cannot turn into FRs by fading Sc galaxies mostly compatible as well Sd galaxies compatible But this is not the whole story.

24 AR LNTICULARS FADD SPIRALS? (GAS SUPPLY) Sc/Sd galaxies cannot make it to the Red sequence by fading alone

25 NOT FADING (ALON) Mergers: major/minor? wet/dry? nvironment: tidal harassment? ram pressure stripping? Fastest rotators (λ R > 0.8) contain very small bulges Internal: feedback? fading?

26 AR LNTICULARS FADD SPIRALS? KMOS will reveal whether we are looking at the right progenitors Hα velocity Hα velocity dispersion Wisnioski et al. (2014) [arxiv: ]

27 Are low-mass spirals DM dominated?

28 TOTAL MASS FROM DYNAMICAL MODLLING NGC4210 Jeans dynamical models & Schwarzschild

29 STLLAR MASSS FROM SPCTRAL FITTING STARLIGHT code applied to CALIFA (Cid Fernandes et al. 2013) observed spectrum masked emission composite SSP models residuals González-Delgado et al. (2014)

30 AR LOW-MASS SPIRALS DM DOMINATD? CALIFA SR/FR If bottom-heavy IMF, DM content of most massive galaxies will decrease

31 AR LOW-MASS SPIRALS DM DOMINATD? Most galaxies have similar DM content except low-mass spirals

32 AR LOW-MASS SPIRALS DM DOMINATD? Gas mass estimates from Papastergis et al. (2012) Situation remains even if gas content considered

33 NGC5682 TH OUTLIRS

34 AR LOW-MASS SPIRALS DM DOMINATD? dsphs (Collins et al. 2014) DiskMass survey (Martinsson et al. 2013) 10 6

35 CONCLUSIONS AM is a powerful parameter to unravel the evolution of galaxies CALIFA offers high quality stellar kinematics across the Hubble sequence DR2 data available. Go get them! Are lenticulars faded spiral galaxies? NO Are low-mass (spiral) galaxies DM dominated? YS

36 LOOKING INTO TH (NAR) FUTUR MUS Atlas of Disks (MAD), large survey of nearby spirals KMOS3D 600 galaxies 0.7<z<2.7 UK teams at higher-z 3000 nearby nearby

37 The nd