Third Reference Catalogue of Bright Galaxies

By G. de Vaucouleurs, A. de Vaucouleurs, H. Corwin, R. Buta, G. Paturel, P. Fouqué. 2012

2,091 citations recorded by the source corpus.

Subfields: Computational Mechanics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/cbab65a3dd01e12fb3fc41653dd68f5558eeb044

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In Computational Mechanics

In Instrumentation

In Statistical and Nonlinear Physics

Citations in the corpus

X-ray emission from star-forming galaxies - II. Hot interstellar medium (2012, background): “The surface brightness profiles were constructed in concentric elliptical annuli, around the centre of the galaxy, with shape parameters – the axis ratio and the position angle, set equal to the corresponding parameters of the optical emission (de Vaucouleurs et al. 1991).”
An expanded Mbh–σ diagram, and a new calibration of active galactic nuclei masses (2010, methodology): “When such corrections are made, rather than using data from de Vaucouleurs et al. (1991), as done by Gültekin et al. (2009b), the uncertainty on the slope and intercept of the Mbh–”
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 analytic growth curve of the R1/4 (de Vaucouleurs 1948) profile (e.g. the Seven Samurai: Burstein et al. 1987; Faber et al. 1989; the RC3: de Vaucouleurs et al. 1991; Jorgensen, Franx & Kjaergaard 1995a); (ii) fitting an R1/n (Sérsic 1968) profile (e.g. Graham & Colless 1997), possibly…”
Galaxy Zoo 2: detailed morphological classifications for 304,122 galaxies from the Sloan Digital Sky Survey (2013, methodology): “The data include RC3 T-types (a numerical index of a galaxy’s stage along the Hubble sequence; de Vaucouleurs et al. 1991) as well as measurements of bars, rings, lenses, pairs, interactions, and tails.”
HyperLEDA. III. The catalogue of extragalactic distances (2014, methodology): “BBSLF, BRSLF, BS, BS3B, BS3R: All these methods use the luminosity of the brightest stars in galaxies as standard ca ndles. BBSLF and BRSLF consider the luminosity function of the brightest blue and red stars. BS3B and BS3R take the mean absolute magnitude of the three brightest blue or red stars. T”
CLUSTERING OF LOCAL GROUP DISTANCES: PUBLICATION BIAS OR CORRELATED MEASUREMENTS? III. THE SMALL MAGELLANIC CLOUD (2014, background): “For instance, let us take i = 70◦ as an extreme example, combined with the SMC’s size given by de Vaucouleurs et al. (1991), a× b = 9487× 5588 arcsec2 and a ‘best’ distance modulus to the galaxy of (m − M)0 = 18.96 mag (this paper).”
Masses and scaling relations for nuclear star clusters, and their co-existence with central black holes (2016, methodology): “To define our NSC sample, We use the t−type galaxy morphological parameter defined by de Vaucouleurs et al. (1991).”
AINUR: Atlas of Images of NUclear Rings (2009, background): “2000) or as the length of the region with a constant m = 2 phase in NIR images (Laurikainen & Salo 2002). Other authors, such as Erwin (2005), assign as a lower limit to the bar length the location of the maximum in ellipticity and as an upper limit the minimum of two ellipse fit measures: the first”