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Title:
The SAURON project - X. The orbital anisotropy of elliptical and lenticular galaxies: revisiting the (V/σ, ɛ) diagram with integral-field stellar kinematics
Authors:
Cappellari, Michele; Emsellem, Eric; Bacon, R.; Bureau, M.; Davies, Roger L.; de Zeeuw, P. T.; Falcón-Barroso, Jesús; Krajnović, Davor; Kuntschner, Harald; McDermid, Richard M.; Peletier, Reynier F.; Sarzi, Marc; van den Bosch, Remco C. E.; van de Ven, Glenn
Affiliation:
AA(Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, the Netherlands; Sub-Department of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH), AB(Centre de Recherche Astrophysique de Lyon, 9 Avenue Charles André, 69230 Saint Genis Laval, France), AC(Centre de Recherche Astrophysique de Lyon, 9 Avenue Charles André, 69230 Saint Genis Laval, France), AD(Sub-Department of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH), AE(Sub-Department of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH), AF(Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, the Netherlands), AG(Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, the Netherlands; European Space and Technology Centre, Postbus 299, 2200 AG Noordwijk, the Netherlands), AH(Sub-Department of Astrophysics, University of Oxford, Denys Wilkinson Building, Keble Road, Oxford OX1 3RH), AI(Space Telescope European Coordinating Facility, European Southern Observatory, Karl-Schwarzschild-Str 2, 85748 Garching, Germany), AJ(Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, the Netherlands), AK(Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen, the Netherlands), AL(Centre for Astrophysics Research, University of Hertfordshire, Hatfield, Herts AL 10 9AB), AM(Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, the Netherlands), AN(Leiden Observatory, Leiden University, Postbus 9513, 2300 RA Leiden, the Netherlands; Department of Astrophysical Sciences, Peyton Hall, Princeton, NJ 08544, USA; Institute for Advanced Study, Einstein Drive, Princeton, NJ 08540, USA)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 379, Issue 2, pp. 418-444. (MNRAS Homepage)
Publication Date:
08/2007
Origin:
MNRAS
MNRAS Keywords:
galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: formation, galaxies: kinematics and dynamics, galaxies: structure
DOI:
10.1111/j.1365-2966.2007.11963.x
Bibliographic Code:
2007MNRAS.379..418C

Abstract

We analyse the orbital distribution of elliptical (E) and lenticular (S0) galaxies using SAURON integral-field stellar kinematics within about one effective (half-light) radius. We construct the anisotropy diagram, which relates the ratio of the ordered and random motion in a galaxy (V/σ) to its observed ellipticity (ɛ), for the 48 E/S0 galaxies from the SAURON survey. For a subsample of 24 galaxies consistent with axisymmetry, we use three-integral axisymmetric Schwarzschild dynamical models to recover the detailed orbital distribution, and we find good agreement with the anisotropy derived from the (V/σ, ɛ) diagram. In a companion paper (Paper IX), we show that the early-type galaxies can be subdivided into two classes of systems with or without a significant amount of specific stellar angular momentum. Here, we show that the two classes have different distributions on the (V/σ, ɛ) diagram. The slow rotators are more common among the most massive systems and are generally classified as E from photometry alone. Those in our sample tend to be fairly round (ɛ <~ 0.3), but can have significant kinematical misalignments, indicating that as a class they are moderately triaxial, and span a range of anisotropies (δ <~ 0.3). The fast rotators are generally fainter and are classified as either E or S0. They can appear quite flattened (ɛ <~ 0.7), do not show significant kinematical misalignments (unless barred or interacting), indicating they are nearly axisymmetric and span an even larger range of anisotropies (δ <~ 0.5). These results are confirmed when we extend our analysis to 18 additional E/S0 galaxies observed with SAURON. The dynamical models indicate that the anisotropy inferred from the (V/σ, ɛ) diagram is due to a flattening of the velocity ellipsoid in the meridional plane (σR > σz), which we quantify with the β anisotropy parameter. We find a trend of increasing β for intrinsically flatter galaxies. A number of the fast rotators show evidence for containing a flattened, kinematically distinct component, which in some cases counter-rotates relative to the main galaxy body. These components are generally more metal rich than the galaxy body. All these results support the idea that fast rotators are nearly oblate and contain disc-like components. The role of gas must have been important for their formation. The slow rotators are weakly triaxial. Current collisionless merger models seem unable to explain their detailed observed properties.

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Part 1     Part  2     Part  3     Part  4     Part  5     Part  6     Part  7     Part  8     Part  9     Part 10     Part 11    

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