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Constraints on secular evolution in unbarred spiral galaxies: understanding bulge and disk formation April 23rd 2012 July 10th 2012 Marja Kristin Seidel Jesús Falcón - Barroso Instituto de Astrofísica de Canarias www.iac.es/project/traces Constraints on secular evolution in unbarred spiral galaxies: understanding bulge and disk formation disentangling disk heating agents April 23rd 2012 July 10th 2012 Marja Kristin Seidel Jesús Falcón - Barroso Instituto de Astrofísica de Canarias www.iac.es/project/traces [email protected] Introduction: Disk heating More than half of the stellar mass in the local Universe is found in disk galaxies (e.g. Driver et al. 2007) but we are far from understanding them. Especially: What is driving the heating of the disk? Investigate 3D-distribution of stellar velocity dispersions ellipsoid with axes ratios: σz/σR (and σϕ/σR) σz σR Possible disk heating agents: • encounters with giant molecular clouds (GMCs) • scattering by dark halo objects or globular clusters • perturbation by spiral structure • perturbation by stellar bars talk on: www.iac.es/project/traces • dissolution of young stellar clusters • disturbances by satellite galaxies or minor mergers (e.g. from Spitzer & Schwarzschild, 1951 to Saha et al. 2010) [email protected] Introduction: Disk heating Model predictions • encounters with GMCs (Sellwood, 2008): 3D agent • perturbation by spiral structure (Jenkins & Binney, 1990): σR Age • radial migration (e.g. Roskar et al. 2008): σR increases with age Metallicity • for an existing metallicity gradient (e.g. Sánchez-Blázquez, 2009)* : σz/σR increase with metallicity talk on: www.iac.es/project/traces But: in the solar neighborhood little evidence for the age-metallicity-relation (e.g. Feltzing et al., 2001) *still present even with satellites! [email protected] Introduction: Our study Our study focuses on: • 6 disk galaxies across the Hubble sequence • obtaining the ages and metallicities in different regions of the galaxies via full-spectrum fitting techniques • relating these stellar population parameters with earlier kinematic results, i.e. σz/σR and the individual values (Shapiro & Gerssen 2003 and 2012) talk on: www.iac.es/project/traces [email protected] Sample Disk-heating (Shapiro & Gerssen 2003 and 2012) credit: HST/WFPC2 image spectra with resolutions of ~ 30 km s-1 and ~ 23 km s-1 NGC 2280 (Scd) NTT NGC 3810 (Sc) NGC 4030 (Sbc) NGC 1068 (Sb) KPNO NGC 2775 (Sa/Sab) NGC 2460 (Sa) different regions from radial surface brightness profiles and disk scale lengths: center bulge [trans] disk talk on: www.iac.es/project/traces Note: all our galaxies show central sigma drops! [email protected] Methods pPXF (Cappellari & Emsellem, 2004) ; Gandalf (Sarzi et al. 2006) STARLIGHT (Cid Fernandes, 2007) gal_3810mj_cor.fits [Bin 1 ; x = -15.0 ; SN= 15.5] 12 Starlight + Miles models NGC 3810 (Sc) DISKV= 1062.6, != 2.0 km/s (Sánchez-Blazquez et al.2006) gal_3810mj_cor.fits [Bin 1 ; x = -15.0 ; SN= 15.5] 10 12 V= 1062.6, != 2.0 km/s 1.2 8 10 pPXF 6 8 40 1 4 6 2 4 0 500 1000 1500 20 0.8 2 0 500 1000 1500 30 Gandalf 0 0.6 30 +ELODIE 20 (Prugniel et Intensity [arb.units] counts al. 2007) 20 10 0.4 40 counts 10 0 0 500 1000 1500 0 λpixels [Å] 20 0.2 0 500 1000 1500 pixels 0 For all three 4861.33 4958.91 regions 5006.84 in major 5175.36 and 5270.00 minor 5335.00 5406.00 axes: " H [OIII] [OIII] Mgb Fe5270 Fe5335 Fe5406 0 -0.2 10 talk on: www.iac.es/project/traces 4861.33 4958.91 5006.84 5175.36 5270.00 5335.00 ages 5406.00 " mass &H luminosity[OIII] [OIII] weightedMgb Fe5270 Fe5335 Fe5406 4800 5000 5200 5400 0 5 10 15 8 metallicities 10 6 8 Counts Analyze4 the stellar populations! 6 2 Counts 4 0 4800 5000 5200 5400 2 Restwavelength [Angstroms] 0 4800 5000 5200 5400 Restwavelength [Angstroms] How can stellar populations help us to understand • secular evolution in spirals? • disk heating processes? [email protected] Preliminary results: Ages and [Fe/H] Luminosity weighted Mass weighted age [Gyr] [Fe / H] repr. error 250 center bulge disk center bulge disk Sa Sab Young populations dominate the luminosity weighted age (e.g. Serra & Trager, 2006) talk on: www.iac.es/project/traces Sb Sbc We mostly confirm inside-out growth scenario (e.g. Muños-Mateos, 2007) 200 Sc In our sample: late types show stronger [Fe/H] gradients than the early types Scd (adding to MacArthur et al., 2009) R ! 150 100 50 0 5 10 15 20 age [Gyr] [email protected] Preliminary results: Ages and [Fe/H] Luminosity weighted Mass weighted age [Gyr] [Fe / H] repr. error 250 center bulge disk center bulge disk Sa Sab Young populations dominate the luminosity weighted age (e.g. Serra & Trager, 2006) talk on: www.iac.es/project/traces Sb Sbc We mostly confirm inside-out growth scenario (e.g. Muños-Mateos, 2007) 200 Sc In our sample: late types show stronger [Fe/H] gradients than the early types Scd (adding to MacArthur et al., 2009) R ! 150 100 50 0 5 10 15 20 age [Gyr] [email protected] Preliminary results: Disk heating With our stellar population results: 6 J.Gerssen & K. Shapiro Griffin is it possible to relate these two findings?Evolutionary stellar population synthesis 1659 Z B-V talk on: www.iac.es/project/traces Figure 4. Velocity ellipsoid ratio σz/σR as a function of galactic Figure 5. Velocity ellipsoid ratio σz/σR as a function of type (Hubble stage T). The solid points show the results that inclination- and extinction-corrected galaxy colour (available in age [Gyr] Figure 19. We plot the broad-band B V colour derived from the SSP we obtained previously (Shapiro et al. 2003). The results that we HyperLeda for 7 of our 8 spirals and the fast-rotating E/S0s). The − derive in this paper for two late type spirals are shown as the black points indicate our spiral galaxy data, and the red squaresSEDs for different ages and metallicities (as indicated within the panel) and Gerssen & Shapiro, 2012 the KroupaVazdekis universal IMF with et the al., zero-point 2010 set with two different Vega Figure 17. Variation of Balmer line-strength indices with metallicity pre- open circles. Horizontal errors represent the uncertainty inherent are the data of Cappellari et al. (2007) for fast-rotating E andspectra in black (very thin) and red (thicker) (see the text for details). The dicted by our single stellar population models of 10 Gyr and Kroupa uni- thickest green line represents the photometric colour computed by Vazdekis in galaxy classification (Naim et al. 1995). The filled square is the S0 galaxies.versal The IMF. linear Different fit line (dashed styles show line) predictions is to for theindices spiral measured gala at xies et al. (1996), as updated in this work, which is based on extensive empirical value in the Solar Neighbourhood derived from Hipparcos data only. The probabilitydifferent spectral of resolutions, no correlation, as in Fig. 14. null hypothesis H , is one 0 photometric stellar libraries. (Dehnen & Binney 1998). percent. of 4300 Å are significantly larger than for the redder part of the units (IFUs) to observe velocity dispersions in disk galaxies. “fast rotators,” are bulge-dominated galaxies that neverthe-spectra∼ for all the clusters. We do not discard possible effects due to This is observationally more efficient than obtaining long-slit less contain a significant disk component (Kuntschner et al.the fact that the Milky Way GCs show oxygen-enhanced abundance spectra, one at a time, along two (or more) position angles. ratios for low metallicities. In fact, Cassisi et al. (2004) have shown 2006; Krajnovi´cet al. 2008). It is therefore interesting tothat such effects become relevant for the spectral ranges covered by Additionally, since IFUs uniformly sample velocity disper- investigate how the disks of these early-type galaxies arethe B, and mostly U, broad-band filters. Therefore, an appropriate sions along both azimuth and radius across the disk, the related to those in spiral galaxies. modelling for these clusters requires working with such α-enhanced assumption of the epicycle approximation, employed here stellar evolutionary isochrones as well as the use of stellar spectra Cappellari et al. (2007) have used axisymmetricwith a similar abundance pattern. In addition, we also require to for long-slit data, can be relaxed. Noordermeer et al. (2008) Schwarzschild dynamical models to extract the three-use specific stellar spectra with CN-strong absorption features and use the PPAK IFU to explore velocity dispersions in disk dimensional orbital structure of a subsample of theCN-enhanced isochrones. galaxies and to constrain the shape of the velocity ellipsoid In Fig. 21, we show our SED fit to the integrated spectrum of SAURON galaxies and measure the shape of their velocitythe standard open cluster M67 (Schiavon, Caldwell & Rose 2004). in one system, NGC 2985. Their measurement of σz/σR ellipsoids. These anisotropy measurements are luminosity-Unlike for the GCs of Fig. 20, these authors obtained the integrated ≈ 0.7 is consistent with our previous result for this sys- weighted, giving more weight to the high-density equatorialspectrum for M67 by co-adding individual spectra of cluster mem- tem (0.75 ± 0.09; Gerssen et al. 2000) and confirms that the bers, weighted according to their luminosities and relative numbers. plane, and volume-averaged, giving more weight to largerThe age and metallicity obtained are in good agreement with these epicycle theory we assume is indeed applicable in this galaxy. radii; as aFigure result, 18. Comparison the global of the Hβ anisotropiesindex computed on (see the basis table of the 2 ofauthors (see also Schiavon 2007) and with our isochrone fitting re- In a series of conference proceedings Westfall et al.
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  • Kinematic Signatures of Bulges Correlate with Bulge Morphologies and Sersic´ Index∗

    The Astrophysical Journal, 754:67 (27pp), 2012 July 20 doi:10.1088/0004-637X/754/1/67 C 2012. The American Astronomical Society. All rights reserved. Printed in the U.S.A. KINEMATIC SIGNATURES OF BULGES CORRELATE WITH BULGE MORPHOLOGIES AND SERSIC´ INDEX∗ Maximilian H. Fabricius1,2, Roberto P. Saglia1,DavidB.Fisher3, Niv Drory4, Ralf Bender1,2, and Ulrich Hopp1,2 1 Max Planck Institute for Extraterrestrial Physics, Giessenbachstrasse, D-85748 Garching, Germany 2 University Observatory Munich, Schienerstrasse 1, D-81679 Munich, Germany 3 Laboratory of Millimeter Astronomy, University of Maryland, College Park, MD 29742, USA 4 Instituto de Astronomia, Universidad Nacional Autonoma de Mexico (UNAM), A.P. 70-264, 04510 Mexico, D.F., Mexico Received 2011 August 30; accepted 2012 April 20; published 2012 July 6 ABSTRACT We use the Marcario Low Resolution Spectrograph at the Hobby–Eberly Telescope to study the kinematics of pseudobulges and classical bulges in the nearby universe. We present major axis rotational velocities, velocity −1 dispersions, and h3 and h4 moments derived from high-resolution (σinst ≈ 39 km s ) spectra for 45 S0 to Sc galaxies; for 27 of the galaxies we also present minor axis data. We combine our kinematics with bulge-to-disk decompositions. We demonstrate for the first time that purely kinematic diagnostics of the bulge dichotomy agree systematically with those based on Sersic´ index. Low Sersic´ index bulges have both increased rotational support (higher v/σ values) and on average lower central velocity dispersions. Furthermore, we confirm that the same correlation also holds when visual morphologies are used to diagnose bulge type.
  • Seen Galaxies Count Ref1 Ref2 Con Visual Scale Mag SBR SIZE M Distance Rv Dist COMMENTS

    Seen Galaxies Count Ref1 Ref2 Con Visual Scale Mag SBR SIZE M Distance Rv Dist COMMENTS

    Seen galaxies Count ref1 ref2 con visual_scale mag SBR SIZE_M Distance Rv dist COMMENTS 1. NGC 224 M 31 AND 5 3.4 13.5 189 2.6 -14 Very large and bright 2. NGC 3031 M 81 UMA 4 6.9 13.2 24.9 12 -3 Fine large galaxy 3. NGC 598 M 33 TRI 3 5.7 14.2 68.7 2.8 -10 Large faint glow in square of stars 4. NGC 4594 M 104 VIR 3 8.0 11.6 8.6 30 48 Moon therefore little detail 5. NGC 221 M 32 AND 3 8.1 12.4 8.5 2.6 -10 Small but easy to see 6. NGC 4472 M 49 VIR 3 8.4 13.2 9.8 53 43 Lovely fuzzy galaxy 7. NGC 3034 M 82 UMA 3 8.4 12.5 10.5 12 13 Could make out bright and dark patches 8. NGC 4258 M 106 CVN 3 8.4 13.6 17.4 24 21 Fine large oval galaxy. So much brighter than most I have been looking at recently. 9. NGC 4826 M 64 COM 3 8.5 12.7 10.3 24 21 Easy galaxy to see 10. NGC 4486 M 87 VIR 3 8.6 13 8.7 51 57 Bright ball 11. NGC 4649 M 60 VIR 3 8.8 12.9 7.6 54 49 Lovely view with three galaxies visible. M60 is the brightest of the three. A nice bright ball of stars 12. NGC 3115 MCG - 1-26- 18 SEX 3 8.9 11.9 7.3 33 29 Bright spindle 13.