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

By Eric Emsellem, M. Cappellari, D. Krajnovi'c, K. Alatalo, L. Blitz, M. Bois, Frédéric Bournaud, M. Bureau, Roger Davies, T. Davis and 14 more. 2011

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Citations in the corpus

THE MBH–LSPHEROID RELATION AT HIGH AND LOW MASSES, THE QUADRATIC GROWTH OF BLACK HOLES, AND INTERMEDIATE-MASS BLACK HOLE CANDIDATES (2012, background): “…galaxies with boxy isophotes, while the less luminous early-type galaxies tend to have disky isophotes and often contain a rotating disk of stars (e.g. Carter 1978, 1987; Davies et al. 1983; Bender et al. 1988; Peletier et al. 1990; Jaffe et al. 1994; Faber et al. 1997; Emsellem et al. 2011).”
Radial variations in the stellar initial mass function of early-type galaxies (2014, background): “NGC4552 and NGC5557 are massive ETGs, with a velocity dispersion σ ∼ 300 km s−1 in their centre (Emsellem et al. 2011), whereas NGC4387 is a lower-mass system with a central value of σ ∼ 100 km s−1.”
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 – XXVIII. Dynamically driven star formation suppression in early-type galaxies (2014, background): “…for stellar luminosity, the offsets aboveand below the line defined in Equation 1 for the CO non-detected sample do not correlate with stellar kinematic quantities (Krajnović et al. 2011; Emsellem et al. 2011), ionised-gas quantities,or measures of galaxy environment (Cappellari et al. 2011b).”
The ATLAS3D project - XXIX. The new look of early-type galaxies and surrounding fields disclosed by extremely deep optical images (2014, methodology): “All galaxies in the ATLAS3D sample benefit from a wealth of ancillary multi-wavelength data, including the internal stellar kinematics derived from SAURON observations, based on which they have been classified as slow or fast rotators (Emsellem et al. 2011).”
The SAMI Galaxy Survey: Instrument specification and target selection (2014, unknown): “By contrast, ATLAS 3D images galaxies to a median of 0.9Re (Emsellem et al. 2011).”
The ATLAS3D Project – XXX. Star formation histories and stellar population scaling relations of early-type galaxies (2015, methodology): “In Emsellem et al. (2011), we expand on this work with the complete ATLAS3D sample, using the quantity λR as a way of separating these two classes of ETG.”
WHAT TURNS GALAXIES OFF? THE DIFFERENT MORPHOLOGIES OF STAR-FORMING AND QUIESCENT GALAXIES SINCE z ∼ 2 FROM CANDELS (2011, background): “Furthermore, kinematic studies of local quiescent galaxies have demonstrated thatthe vast majority of quiescent galaxies have significant rotatin (Emsellem et al. 2011), and the incidence of strong rotation signatures in quiescent galaxies does not change fromz∼ 1 to the present day (at∼ 60%, van…”
The Sydney-AAO Multi-object Integral field spectrograph (2011, methodology): “Integral field spectroscopy also enables studies of stellar kinematics that describe the observed projected stellar angular momentum per unit mass of galaxies, not possible with other techniques (Emsellem et al. 2007, 2011; Brough et al. 2011).”
One Law to Rule Them All: The Radial Acceleration Relation of Galaxies (2016, methodology): “Here we consider two different data sets of ETGs: (i) 16 ETGs from Atlas3D (Cappellari et al. 2011) that have inner rotating stellar components (Emsellem et al. 2011) and outer low-density H I disks/rings (den Heijer et al. 2015); and (ii) 9 ETGs with relaxed X−ray haloes.”
TRACING OUTFLOWS AND ACCRETION: A BIMODAL AZIMUTHAL DEPENDENCE OF Mg ii ABSORPTION (2012, unknown): “We modeled all galaxy morphological types since 86% of early-types have regular stellar rotation (14% exhibit slow r - tation), spanning the full range of apparent ellipticities, with 90% being kinematically and photometrically aligned (see Emsellem et al. 2011; Krajnović et al. 2011).”
Wet Disc Contraction to Galactic Blue Nuggets and Quenching to Red Nuggets (2013, background): “The predicted systems resemble most of the present day elliptical galaxies, which show rapid rotation within their effective radii (Emsellem et al. 2011), dropping to slow rotation velocities at a few effective radii (Romanowsky et al. in preparation).”
Idealized models for galactic disc formation and evolution in ‘realistic’ ΛCDM haloes (2012, methodology): “The system might be classified as a barred, fast rotating early-type galaxy applying a classification scheme as used for the ATLAS3D survey (Emsellem et al. 2011).”
The ATLAS3D project - XIII. Mass and morphology of H I in early-type galaxies as a function of environment (2011, background): “We find that as many as 80 per cent of all ETGs in the nearby Universe consist of nearly axisymmetric, fast rotating stellar systems (Krajnović et al. 2011, hereafter Paper II; Emsellem et al. 2011, hereafter Paper III), most of which resemble spiral galaxies with the arms removed (Cappellari et al”
The SLUGGS Survey: kinematics for over 2500 globular clusters in 12 early-type galaxies (2012, methodology): “For our sample, we use λReff from Emsellem et al. (2011) if the galaxy is in ATLAS3D, whereas we use the conversion formulae provided by the same authors to convert Vmax/σ 0 into λReff , where Vmax and σ 0 are the maximum rotation amplitude and the central velocity dispersion of the host galaxy,…”
Structure and Kinematics of Early-Type Galaxies from Integral Field Spectroscopy (2016, methodology): “The results were presented by Emsellem et al. (2011) and are reproduced, on top of the theoretical relations, in Figure 13.”
The ATLAS3D project - X. On the origin of the molecular and ionized gas in early-type galaxies (2011, background): “When combined with the fact that most ETGs show relaxed stellar kinematics (Emsellem et al. 2011, hearafter Paper III) and evidencefrom deep imaging (Duc et al., submitted; Paper IX) this suggeststhat the last major merger that could have formed such systems wasat least several gigayears ago.”
Galaxy Masses: A Review (2013, unknown): “This includes fast-rotators (Emsellem et al. 2007; Cappellari et al. 2007; Emsellem et al. 2011) and spirals.”