1973
DOI: 10.1086/152030
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Stellar Motions Near the Nucleus of M31

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Cited by 16 publications
(9 citation statements)
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“…One was from the group later called the Seven Samurai, who collected redshifts and distance estimates for elliptical galaxies and searched for deviations from Hubble flow. Their result was consistent, to within the rather large error bars, with that of Rubin et al, (1976)…”
Section: Large Scale Structure In Velocity Spacesupporting
confidence: 81%
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“…One was from the group later called the Seven Samurai, who collected redshifts and distance estimates for elliptical galaxies and searched for deviations from Hubble flow. Their result was consistent, to within the rather large error bars, with that of Rubin et al, (1976)…”
Section: Large Scale Structure In Velocity Spacesupporting
confidence: 81%
“…She and they embarked on what they described as an unconventional investigation, designed not to measure H or even q but to look for deviations from isotropy of the Hubble law. The first hint of a "yes" answer appears in Rubin et al (1973). The fullblown result was presented at the 1975 Bloomington AAS meeting and promptly dubbed "the Rubin-Ford effect."…”
Section: Large Scale Structure In Velocity Spacementioning
confidence: 99%
See 1 more Smart Citation
“…M33, the Triangulum Galaxy, is the third most massive galaxy in the Local Group, with a mass close to one tenth that of M31 (Corbelli & Salucci 2000 measure M33's rotation curve out to 16 kpc, and find an implied dark halo mass of M M 33 5 x 10 10 M ⊙ ). M33 has a total host luminosity of L M 33,host,V ∼ 10 9 L ⊙ (de Vaucouleurs et al 1991) and is more face-on (i = 56 • ± 1 • , Zaritsky et al 1989) than M31 (i = 77 • ; e.g., Rubin et al 1973;Athanassoula & Beaton 2006). It is classified as a SA(s)cd II-III galaxy (de Vaucouleurs et al 1991), has little or no bulge component, a UV-and X-ray bright nuclear cluster (e.g., Long et al 1981, Dubus et al 1999and Foschini et al 2004, and perhaps a bar (Javadi et al 2011), so most of the central light is distributed over an exponential disk component (e.g., de Vaucouleurs 1959;Bothun 1992;Minniti et al 1993;McLean & Liu 1996;Corbelli et al 2008;Kormendy et al 2010;Javadi et al 2011).…”
Section: The Triangulum Galaxymentioning
confidence: 99%
“…The identification of rotating bulges goes back a long time (e.g., Pease 1918;Babcock 1938Babcock , 1939Rubin et al 1973;Pellet 1976;Bertola and Capaccioli 1977;Peterson 1978;Mebold et al 1979). Early-type galaxies can also display significant rotation, albeit likely due to the presence of a disk (e.g., Davies et al 1983;Graham et al 1998;Emsellem et al 2007Emsellem et al , 2011Krajnović et al 2008).…”
Section: Rotationmentioning
confidence: 99%