The SAURON project – VIII. OASIS/CFHT integral-field spectroscopy of elliptical and lenticular galaxy centres

By R. McDermid, Eric Emsellem, K. Shapiro, R. Bacon, M. Bureau, M. Cappellari, Roger Davies, P. de Zeeuw, J. Falc'on-Barroso, D. Krajnovi'c and 3 more. 2006

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We present high spatial resolution integral-field spectros copy of 28 elliptical (E) and lenticular (S0) galaxies from the SAURON representative survey obtained with the OASIS spectrograph during its operation at the CFHT. These seeing-limited observations explore the central 8 ′′ ×10 ′′ (typically one kiloparsec diameter) regions of these galax ies using a spatial sampling four times higher than SAURON (0. 27 vs. 0. 94 spatial elements), resulting in almost a factor of two improvement in the median PSF. These data allow accurate study of the central regions to complement the large-scale view provided by SAURON. Here we present the stellar and gas kinematics, stellar absorption-line strengths and neb ular emission-line strengths for this sample. We also characterise the stellar velocity maps using the ‘kinemetry’ technique, and derive maps of the luminosity-weighted stellar age, metallicity and abundance ratio via stellar population models. We give a brief review of the structures found in our maps, linking also to larger-scale structures measured with SAURON. We present two previously unreported kinematically-decoupled components (KDCs) in the centres of NGC 3032 and NGC 4382. We compare the intrinsic size and luminosity-weighted stellar age of all the visible KDCs in the full SAURON sample, and find two types of components: kiloparsec-scale K DCs, which are older than 8 Gyr, and are found in galaxies with little net rot ation; and compact KDCs, which have intrinsic diameters of less than a few hundred parsec, show a range of stellar ages from 0.5 - 15 Gyr (with 5/6 younger than 5 Gyr), are found exclusively in fast-rotating galaxies, and are close to counter-rotating around the same axis as their host. Of the 7 galaxies in the SAURON sample with integrated luminosity-weighted ages less than 5 Gyr, 5 show such compact KDCs, suggesting a link between counter-rotation and recent star-formation. We show that this may be due to a combination of small sample size at young ages, and an observational bias, since young KDCs are easier to detect than their older and/or co-rotating counterparts.

Subfields: Astronomy and Astrophysics, Global and Planetary Change, Instrumentation

View Paper: https://www.semanticscholar.org/paper/61eeb6908287d75652fb2cb4fd18678a70b36700

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Citations in the corpus

Discriminating Between the Physical Processes that Drive Spheroid Size Evolution (2009, background): “Massive, old ellipticals at z = 0 have weak colour gradients (McDermid et al. 2006; Sánchez-Blázquez et al. 2007, and references therein).”
The SLUGGS Survey: kinematics for over 2500 globular clusters in 12 early-type galaxies (2012, background): “Spectroscopic studies of the very central regions (McDermid et al. 2006) have also suggested a young (2.5 Gyr) stellar population associated with the disc, as supported by the recent supernova SN2000ds (Filippenko & Chornock 2000).”
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The ATLAS3D project - X. On the origin of the molecular and ionized gas in early-type galaxies (2011, background): “As discussed above, NGC 3032 and NGC 4150 have KDCs that may be affecting the gas properties (McDermid et al. 2006; Sarziet al. c© 2009 RAS, MNRAS000, 1–17 2006).”
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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).”
The ATLAS3D project - XIII. Mass and morphology of H I in early-type galaxies as a function of environment (2011, background): “In the former the gas disc is aligned with a kinematically decoupled stellar component (McDermid et al. 2006, O10).”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, background): “This is also true for slow rotators with KDCs, which have a population indistinguishable from the rest of the galaxy, in agreement with the SAURON observations of NGC 4365 by Davies et al. (2001) and the OASIS high-resolution observations by McDermid et al. (2006).”
The ATLAS3D Project – XXX. Star formation histories and stellar population scaling relations of early-type galaxies (2015, methodology): “…strength due to velocity broadening by measuring the equivalent indices on the broadened and unbroadened optimal template fit, thus accounting for line strength and line-ofsight velocity distribution dependences of the velocity dispersion corrections (Kuntschner et al. 2006; McDermid et al. 2006).”
A Theoretical Interpretation of the Black Hole Fundamental Plane (2007, methodology): “Where possible, we update measurements ofRe, σ andns with more recent values from Lauer et al. (2005, 2006a); McDermid et al. (2006) and from Kormendy et al. (2007), which extends the baseline of surface brightness measurements allowing more robust estimates of ns andRe.”