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Publications of the Astronomical Society of the Pacific, 1981
The projected mass method of Bahcall and Tremaine has been used to derive the mass of the core of M31. From the observed radial velocities of 43 globular clusters, the mass interior to 30' is found to be MI = (9 ± 2) × 1010 Msun. For six clusters with 100' MI = (2.4 ± 1.2) × 1011 Msun. From the observed radial velocities of M32, M33, NGC 147, NGC 185,
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The projected mass method of Bahcall and Tremaine has been used to derive the mass of the core of M31. From the observed radial velocities of 43 globular clusters, the mass interior to 30' is found to be MI = (9 ± 2) × 1010 Msun. For six clusters with 100' MI = (2.4 ± 1.2) × 1011 Msun. From the observed radial velocities of M32, M33, NGC 147, NGC 185,
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Catalogue of model star clusters in the Milky Way and M31 galaxies
Monthly Notices of the Royal Astronomical Society, 2023Oleg Y Gnedin +2 more
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The Tucana dwarf spheroidal: a distant backsplash galaxy of M31?
Monthly Notices of the Royal Astronomical Society, 2023Julio Navarro +2 more
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First detection and characterization of symbiotic stars in M31
Monthly Notices of the Royal Astronomical Society, 2014Michael Shara +2 more
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M31 satellite masses compared to ΛCDM subhaloes
Monthly Notices of the Royal Astronomical Society, 2014Erik Tollerud +2 more
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Reddening, colour and metallicity of the M31 globular cluster system
Monthly Notices of the Royal Astronomical Society, 2008Richard De Grijs, De Grijs R
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Globular clusters in the outer halo of M31: the survey
Monthly Notices of the Royal Astronomical Society, 2008Rodrigo Ibata +2 more
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The ‘remarkable’ M31 globular cluster 037–B327 revisited
Monthly Notices of the Royal Astronomical Society, 2002Pauline Barmby, Terry Bridges
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PHOTOGRAPHIC ISOPHOTOMETRY OF M31
Publications of the Astronomical Society of the Pacific, 1970O. K. Krienke, P. W. Hodge
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