The SAURON project - V. Integral-field emission-line kinematics of 48 elliptical and lenticular galaxies

By M. Sarzi, J. Falc'on-Barroso, Roger Davies, R. Bacon, M. Bureau, M. Cappellari, P. de Zeeuw, Eric Emsellem, K. Fathi, D. Krajnovi'c and 3 more. 2005

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We present the emission-line fluxes and kinematics of 48 representative elliptical and lenticular galaxies obtained with our custom-built integral-field spectrograph SAURON. Hb, [OIII], and [NI] 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 0.1A set by the current limitations in describing galaxy spectra with synthetic and real stellar templates, rather than by the quality of our spectra. Emission is detected in 75% of our sample galaxies, and comes in a variety of resolved spatial distributions and kinematic behaviours. The ionised-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. 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]/Hb 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.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/36d5fa9404fe59e61fe3058d2f790f26bb17036e

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Citations in the corpus

A REVISED PARALLEL-SEQUENCE MORPHOLOGICAL CLASSIFICATION OF GALAXIES: STRUCTURE AND FORMATION OF S0 AND SPHEROIDAL GALAXIES (2011, result): “…to note the generally good agreement between the above dichotomy and the results of the SAURON and ATLAS3D surveys (e. g., de Zeeuw et al. 2002; Emsellem et al. 2004, 2007, 2011; Cappellari et al. 2007, 2011a, b; Krajnović et al. 2008, 2011; McDermid et al. 2006): 3 PARALLEL-SEQUENCE GALAXY…”
The ATLAS3D project – IV. The molecular gas content of early-type galaxies (2011, background): “…the SAURON observations of kinematics in early-type galaxies have shown that there is often little if any structural difference between lenticulars and ellipticals (Emsellem et al. 2004), so a purely isophotal classification contributes little to our understanding of their formation histories.”
Improving the full spectrum fitting method: accurate convolution with Gauss-Hermite functions (2016, methodology): “…et al. 2013, 2015; McDermid et al. 2015; Shetty & Cappellari 2015), but it can also be used when extracting the stellar kinematics with ppxf (e.g. Emsellem et al. 2004; Oh et al. 2011; Thomas et al. 2013), while the remaining choices are useful when extracting the stellar or gas kinematics…”
THE BLACK HOLE MASS IN M87 FROM GEMINI/NIFS ADAPTIVE OPTICS OBSERVATIONS (2011, methodology): “Emsellem et al.(2004) present the SAURON data in terms of Gauss-Hermite polynomials.”
The ATLAS3D project - II. Morphologies, kinemetric features and alignment between photometric and kinematic axes of early-type galaxies (2011, methodology): “The data reduction follows procedures described in Bacon et al. (2001) and Emsellem et al. (2004).”
STRUCTURE AND FORMATION OF ELLIPTICAL AND SPHEROIDAL GALAXIES (2008, background): “Similarly, in NGC 4387, Halliday et al. (2001) suggest that a central decrease inσ implies a rotationally supported subsystem that is confirmed by Emsellem et al. (2004) and Krajnovíc et al. (2008).”
The SAURON project – XII. Kinematic substructures in early-type galaxies: evidence for discs in fast rotators (2008, background): “…early-type galaxies (E, S0), these observations clearly show the previously hintedrich variety of kinematic substructures such as: kinematically decoupled c© 2007 RAS, MNRAS000, 1–20 cores, kinematic twists, counter-rotating structures andcentral disks (Emsellem et al. 2004, hereafter Paper III).”
Formation of Early-Type Galaxies from Cosmological Initial Conditions (2005, background): “A similar behavior is seen in some field ellipticals, such as NGC 2768 (Emsellem et al. 2004), and could have the same origin.”
The ATLAS3D project XV: benchmark for early-type galaxies scaling relations from 260 dynamical models: mass-to-light ratio, dark matter, fundamental plane and mass plane (2012, methodology): “Various comparisons of the accuracy of kinematic quantities have been performed in the literature (e.g. Emsellem et al. 2004).”
Spatially resolved spectroscopy of early-type galaxies over a range in mass (2007, background): “It is a boxy galaxy and it shows a central velocity dispersion drop (Halliday et al. 2001; Emsellem et al. 2004).”
The ATLAS3D project – I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria (2010, methodology): “By the application of integral-field spectroscopy to a representative sample of nearby ETGs, theSAURON survey (de Zeeuw et al. 2002) has revealed the full richness of the kinematics of these objects (Emsellem et al. 2004; McDermid et al. 2006; Krajnovi´c et al. 2008).”
Bar Diagnostics in Edge-On Spiral Galaxies. III. N-Body Simulations of Disks (2004, methodology): “…the next level of tests, along with a full two-dimensional analysis of N-body simulations (including higher order LOSVD terms), but preliminary results support both the above long-slit work and our current simulations (e.g., de Zeeuw et al. 2002; Bureau et al. 2002a, 2002b; Emsellem et al. 2004).”
The ATLAS3D project - XIV. The extent and kinematics of the molecular gas in early-type galaxies (2012, methodology): “In brief, for each target, individual datacubes were merged and analysed as described in Emsellem et al. (2004), ensuring a minimum signal-to-noise ratio of 40 per spatial and spectral pixel using the binning scheme developed by Cappellari & Copin (2003).”
The ATLAS3D project – III. A census of the stellar angular momentum within the effective radius of early‐type galaxies: unveiling the distribution of fast and slow rotators (2011, methodology): “…misalignment between the kinematic and photometric axes (excluding the few systems consistent with having no apparent rotation at all), or complex/irregular stellar velocity maps with twists and strong misalignment with respect to the photometry (Emsellem et al. 2004; Krajnović et al. 2008).”