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Title:
The SAURON project - V. Integral-field emission-line kinematics of 48 elliptical and lenticular galaxies
Authors:
Sarzi, Marc; Falcón-Barroso, Jesús; Davies, Roger L.; Bacon, Roland; Bureau, Martin; Cappellari, Michele; de Zeeuw, P. Tim; Emsellem, Eric; Fathi, Kambiz; Krajnović, Davor; Kuntschner, Harald; McDermid, Richard M.; Peletier, Reynier F.
Affiliation:
AA(Denys Wilkinson Building, University of Oxford, Keble Road, Oxford), AB(Leiden Observatory, Postbus 9513, 2300 RA Leiden, the Netherlands), AC(Denys Wilkinson Building, University of Oxford, Keble Road, Oxford), AD(Centre de Recherche Astronomique de Lyon, 9 Avenue Charles André, 69230 Saint Genis Laval, France), AE(Denys Wilkinson Building, University of Oxford, Keble Road, Oxford), AF(Leiden Observatory, Postbus 9513, 2300 RA Leiden, the Netherlands), AG(Leiden Observatory, Postbus 9513, 2300 RA Leiden, the Netherlands), AH(Centre de Recherche Astronomique de Lyon, 9 Avenue Charles André, 69230 Saint Genis Laval, France), AI(Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen, the Netherlands; Rochester Institute of Technology, Rochester, New York 14623, USA), AJ(Denys Wilkinson Building, University of Oxford, Keble Road, Oxford), AK(Space Telescope European Coordinating Facility, European Southern Observatory, Karl-Schwarzschild-Str 2, 85748 Garching, Germany), AL(Leiden Observatory, Postbus 9513, 2300 RA Leiden, the Netherlands), AM(Kapteyn Astronomical Institute, Postbus 800, 9700 AV Groningen, the Netherlands)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 366, Issue 4, pp. 1151-1200. (MNRAS Homepage)
Publication Date:
03/2006
Origin:
MNRAS
MNRAS Keywords:
galaxies: elliptical and lenticular, cD, galaxies: evolution, galaxies: formation, galaxies: ISM, galaxies: kinematics and dynamics, galaxies: structure
DOI:
10.1111/j.1365-2966.2005.09839.x
Bibliographic Code:
2006MNRAS.366.1151S

Abstract

We present the emission-line fluxes and kinematics of 48 representative elliptical and lenticular galaxies obtained with our custom-built integral-field spectrograph, SAURON, operating on the William Herschel Telescope. Hβ, [OIII]λλ4959,5007 and [NI]λλ5198,5200 emission lines were measured using a new procedure that simultaneously fits both the stellar spectrum and the emission lines. Using this technique we can detect emission lines down to an equivalent width of 0.1 Å set by the current limitations in describing galaxy spectra with synthetic and real stellar templates, rather than by the quality of our spectra. Gas velocities and velocity dispersions are typically accurate to within 14 and 20 km s-1, respectively, and at worse to within 25 and 40 km s-1. The errors on the flux of the [OIII] and Hβ lines are on average 10 and 20 per cent, respectively, and never exceed 30 per cent. Emission is clearly detected in 75 per cent of our sample galaxies, and comes in a variety of resolved spatial distributions and kinematic behaviours. A mild dependence on the Hubble type and galactic environment is observed, with higher detection rates in lenticular galaxies and field objects. More significant is the fact that only 55 per cent of the galaxies in the Virgo cluster exhibit clearly detected emission. The ionized-gas kinematics is rarely consistent with simple coplanar circular motions. However, the gas almost never displays completely irregular kinematics, generally showing coherent motions with smooth variations in angular momentum. In the majority of the cases, the gas kinematics is decoupled from the stellar kinematics, and in half of the objects this decoupling implies a recent acquisition of gaseous material. Over the entire sample however, the distribution of the mean misalignment values between stellar and gaseous angular momenta is inconsistent with a purely external origin. The distribution of kinematic misalignment values is found to be strongly dependent on the apparent flattening and the level of rotational support of galaxies, with flatter, fast rotating objects hosting preferentially corotating gaseous and stellar systems. In a third of the cases, the distribution and kinematics of the gas underscore the presence of non-axisymmetric perturbations of the gravitational potential. Consistent with previous studies, the presence of dust features is always accompanied by gas emission while the converse is not always true. A considerable range of values for the [OIII]/Hβ ratio is found both across the sample and within single galaxies. Despite the limitations of this ratio as an emission-line diagnostic, this finding suggests either that a variety of mechanisms is responsible for the gas excitation in E and S0 galaxies or that the metallicity of the interstellar material is quite heterogeneous.

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