The SAURON project - VI. Line strength maps of 48 elliptical and lenticular galaxies

By H. Kuntschner, Eric Emsellem, R. Bacon, M. Bureau, M. Cappellari, Roger Davies, P. de Zeeuw, J. Falc'on-Barroso, D. Krajnovi'c, R. McDermid and 2 more. 2006

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We present absorption line strength maps of 48 representative elliptical and lenticular galaxies obtained as part of a survey of nearby galaxies using our custom-built integral-field spectrograph, SAURON, operating on the William Herschel Telescope. Using high-quality spectra, spatially binned to a constant signal-to-noise, we measure four key age, metallicity and abundance ratio sensitive indices from the Lick/IDS system over a two-dimensional field extending up to approximately one effective radius. A discussion of calibrations and offsets is given, as well as a description of error estimation and nebular emission correction. We modify the classical Fe5270 index to define a new index, Fe5270 S, which maximizes the usable spatial coverage ofSAURON. Maps of H�, Fe5015, Mgb and Fe5270S are presented for each galaxy. We use the maps to compute average line strengths integrated over circular apertures of oneeighth effective radius, and compare the resulting relatio ns of index versus velocity dispersion with previous long-slit work. The metal line strength maps show generally negative gradients with increasing radius roughly consistent with the morphology of the light profiles. Remarkable deviations from this general trend exist, particularl y the Mgb isoindex contours appear to be flatter than the isophotes of the surface brightness for ab out 40% of our galaxies without significant dust features. Generally these galaxies exhibi t significant rotation. We infer from this that the fast-rotating component features a higher met allicity and/or an increased Mg/Fe

Subfields: Astronomy and Astrophysics, Instrumentation

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Citations in the corpus

Discriminating Between the Physical Processes that Drive Spheroid Size Evolution (2009, background): “…material at the centre) yielding a slightly red core (typical in z = 0 massive ellipticals; see Caon, Capaccioli & Rampazzo 1990; Peletier et al. 1990; Kuntschner et al. 2006; Sánchez-Blázquez et al. 2007), the B-band Re here is about ∼10 per cent larger than the stellar mass Re at late times.”
The ATLAS3D project – I. A volume-limited sample of 260 nearby early-type galaxies: science goals and selection criteria (2010, methodology): “Disks in fast rotators have enhanced metallicity, while kinematically distinct cores in slow rotators show no stellar population signatures (Kuntschner et al. 2006, 2010).”
The SAURON project - XVI. On the sources of ionization for the gas in elliptical and lenticular galaxies (2009, background): “…of the gravitational potential of our sample galaxies (Cappellari et al. 2006, Paper IV) and of the basic properties of their stellar populations (Kuntschner et al. 2006, Paper VI), but we can also draw from a variety of ancillary data that have been collected and analysed over the course of…”
The ATLAS3D project – XX. Mass–size and mass–σ distributions of early-type galaxies: bulge fraction drives kinematics, mass-to-light ratio, molecular gas fraction and stellar initial mass function (2012, methodology): “The parameters for the SAURON survey (de Zeeuw et al. 2002) subset of 48 galaxies was already given in Kuntschner et al. (2006).”
The SAURON project – VIII. OASIS/CFHT integral-field spectroscopy of elliptical and lenticular galaxy centres (2006, background): “TheSAURON spectra have been truncated to a wavelength range of 4825-5280 Å, to ensure a common wavelength coverage within the aperture for all galaxies, without encountering gaps in the field coverage due to the filter cut-off (see Kuntschner et al. 2006). c© RAS, MNRAS000, 1–56 Figure D1.”
Evolutionary stellar population synthesis with MILES – I. The base models and a new line index system (2010, methodology): “By far the most popular method is to build key diagnostic model grids by plotting an age-sensitive indicator (e.g. Hβ) versus a metallicitysensitive indicator (e.g., Mgb, 〈Fe〉), to estimate the age and metallicity (e.g. Trager et al. 2000; Kuntschner et al. 2006).”
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): “The RC3 normalization agree within 5 per cent with the SAURON determinations in Cappellari et al. (2006), Kuntschner et al. (2006) and Falcón-Barroso et al. (2011).”
The SAURON project – XII. Kinematic substructures in early-type galaxies: evidence for discs in fast rotators (2008, background): “Kuntschner et al. (2006) find that all morphologically flat fast rotators have Mgb line-strength distribution flatter than theisophotes, and associate it with the rotationally supported substructu e, which features a higher metallicity and/or an increased Mg/Fe ratio s compared to the galaxy as a…”
The ATLAS3D Project – XXX. Star formation histories and stellar population scaling relations of early-type galaxies (2015, methodology): “Fe5270 is measured indirectly via the Fe5270S by applying the relation Fe5270 = 1.28 × Fe5270S + 0.03 (Kuntschner et al. 2006).”
Spatially resolved spectroscopy of early-type galaxies over a range in mass (2007, methodology): “In particular, we have 5 galaxies in common with Kuntschner et al. (2006) and 2 galaxies in common with Fisher, Sadler & Peletier (1996).”
The SAURON project – IX. A kinematic classification for early‐type galaxies (2007, background): “…accreted some gas (e.g. via interaction with a companion, see Falcón-Barroso et al. 2004), and sometimes show the presence of a younger stellar popu- c© 0000 RAS, MNRAS000, 000–000 lation (such as NGC 3032, NGC 3489, NGC 4150, see Kuntschner et al. 2006, Paper VI, and see also Paper VIII).”
The ATLAS3D project - X. On the origin of the molecular and ionized gas in early-type galaxies (2011, background): “The gas we detect in these galaxies could be a remnant, left over from the progenitors that formed the ETG. Stellar population analyses (e.g. Kuntschner et al. 2006, Kuntschner et al. 2010, McDermid et al., in prep), however, show that the underlyingstellar populations in these galaxies are old (≫…”
The ATLAS3D project - II. Morphologies, kinemetric features and alignment between photometric and kinematic axes of early-type galaxies (2011, background): “In addition, the stellar population content of RR galaxies often shows distinct and flattened regions of increased metallicity, suggesting a link with regions of ordered rotation (Kuntschner et al. 2006, 2010).”
IMPROVED AND QUALITY-ASSESSED EMISSION AND ABSORPTION LINE MEASUREMENTS IN SLOAN DIGITAL SKY SURVEY GALAXIES (2011, methodology): “…models have been effectively used to study galaxy properties, such as : luminosity-weighted ages, metallicities and abundance ratios of early-type galaxies (Davies, Sadler & Peletier 1993; Fisher, Franx & Illingworth 1995, 1996; Jorgensen, I. 1999; Kuntschner 2000; Kuntschner et al. 2006).”
STRUCTURE AND FORMATION OF ELLIPTICAL AND SPHEROIDAL GALAXIES (2008, background): “In all three galaxies, SAURON two-dimensional maps of Hβ line strength reveal no difference in age between the decoupled center and the rest of the galaxy (Kuntschner et al. 2006).”
Molecular gas and star formation in the SAURON early-type galaxies (2007, unknown): “…et al. 2004), SAURON simultaneously maps the ionised-gas distribution and kinematics (Hβ, [O III] and [N I] lines; Sarzi et al. 2006), as well as the age, metallicity and overabundance of the stellar populations (through the Hβ, Mgb, Fe5015 and Fe5270 line-strength indices; Kuntschner et al. 2006).”
The SAURON project – XVII. Stellar population analysis of the absorption line strength maps of 48 early-type galaxies (2010, methodology): “…6 how the oneRe aperture index values of our sample of 48 5 We convert our Fe5270S measurements to Fe5270 by usingFe5270 = 1.26× Fe5270S + 0.06 (for details see Kuntschner et al. 2006). early-type galaxies project onto the model grids in planes of [α/Fe] vs [Z/H], [Z/H] vs Age and Age vs [α/Fe].”
The star formation history of CALIFA galaxies: Radial structures (2013, background): “Sánchez-Blázquez et al. 2007; Mehlert et al. 2003), or IFU data (eg., Rawler et al. 2010; Kuntschner et al. 2006).”