Crete, 1/24 Mapping the kinematics and stellar populations of E/S0s with SAURON Harald Kuntschner Crete, 12 th August 2004

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Crete, 1/24 Mapping the kinematics and stellar populations of E/S0s with SAURON Harald Kuntschner Crete, 12 th August 2004 Slide 2 Crete, 2/24 Outline Introduction The SAURON survey Results from Kinematics Stellar populations with focus on environmental effects Conclusions Slide 3 Crete, 3/24 The SAURON team PIs: Bacon, Davies, de Zeeuw COIs: Bureau, Cappellari, Emsellem, Falcn- Barroso, Krajnovi , Kuntschner, McDermid, Peletier plus associated members Slide 4 Crete, 4/24 Galaxy formation When and how do E/S0/Sa galaxies form? What is the orbital make-up of E/S0s? What is the average age and metal content? Origin of substructures; e.g. faint disks in Es, decoupled cores, etc. E S0 Sa transformations? What is the relationship between global properties and super-massive black holes ? SAURON Slide 5 Crete, 5/24 The SAURON project Systematic study of a representative sample of 48 nearby E/S0s and 24 Sa-type spirals Wide field integral-field spectroscopy from the ground (SAURON) Central high spatial sampling integral-field spectroscopy with OASIS/GMOS HST imaging (and some STIS spectroscopy) Large scale ground based imaging de Zeeuw et al, 2002, MNRAS, 329, 513 Slide 6 Crete, 6/24 The sample selection Uniformly covering the ellipticity vs MB plane MB -18 mag (factor of 50 in luminosity) 24 E, 24 S0, 24 Sa (each 12 cluster, 12 field) cz < 3000 km/s DEC: -6 < d < +64 and |b| 15 Slide 7 Crete, 7/24 Why integral-field spectroscopy? Galaxy Image Velocity field Velocity curve Integral field Long slit Slide 8 Crete, 8/24 Status of the SAURON survey Observations completed in April 2002 8 runs on William Herschel Telescope (4m) 35.5/56 clear nights ~200.000 independent galaxy spectra All data homogeneously reduced Analysis and interpretation ongoing 5 refereed papers in 2004 so far Slide 9 Crete, 9/24 48 E/S0 DSS images Emsellem et al., 2004, MNRAS, 352, 721 Slide 10 Crete, 10/24 SAURON-classified rotators S0 E E E E E E E E E E E EE 40% classified by RC3 as ellipticals Slide 11 Crete, 11/24 SAURON-classified ellipticals E E E E S0 E E E E E E E General agreement with RC3 Slide 12 Crete, 12/24 Results from the kinematic maps Two classes of early-type galaxies Flattened rotating lenticulars (some with bars) Triaxial ellipticals (many kinematically decoupled components) Discontinuous transition NGC 4660NGC 4458 Slide 13 Crete, 13/24 Line-strength: Age, Z, [Mg/Fe] Wavelength covers H , Fe5015, [OIII], Mgb & Fe5270 Lick/IDS index definitions (+ SAURON adjustments) Indices + Models can be used to estimate luminosity weighted age, Z and abundance ratios. Slide 14 Crete, 14/24 Kinematics and line-Strengths I V Mgb Fe NGC 4546 NGC 4570 NGC 4406 NGC 4365 NGC 4660 NGC 4382 NGC 4374 N E Slide 15 Crete, 15/24 Stellar population models Vazdekis (1999) models at Lick resolution (~8.4 FWHM) based on Jones (1999) library [MgFe52]=(Mgb x Fe5270)^0.5 Goal: Estimate the luminosity weighted age, metallicity and abundance ratios. Slide 16 Crete, 16/24 Central Re/8 measurements Traditional RC3 morphologies Mostly old Es Weak evidence for young stellar populations in some field Es S0s in all environs spread to younger ages Slide 17 Crete, 17/24 Central Re/8 measurements New morphologies based on 2-dim kinematics 7 triaxial Es in field only 4 triaxial Es in cluster Slide 18 Crete, 18/24 NGC 5198 (E; field) V HH [MgFe50] Age mapZ map Slide 19 Crete, 19/24 NGC 4150 (S0; cluster) V HH [MgFe50] Age mapZ map Slide 20 Crete, 20/24 NGC 4570 (S0; cluster) V HH [MgFe50] Age mapZ map Slide 21 Crete, 21/24 A bar in NGC 4570 van den Bosch & Emsellem (1998) Metal lines Age map Slide 22 Crete, 22/24 NGC 4382 (S0; cluster) V HH [MgFe50] Age mapZ map Slide 23 Crete, 23/24 Statistics young populations 19/48 (40%) of our sample show some evidence of young (