The observed infall of galaxies towards the Virgo cluster

We examine the velocity field of galaxies around the Virgo cluster induced by its overdensity. We have studied the velocity–distance relation in Virgocentric coordinates using a sample of 1792 galaxies with distances from the tip of the Red Giant Branch, the Cepheid luminosity, the luminosity of typ...

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Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2010-06, Vol.405 (2), p.1075-1083
Main Authors: Karachentsev, I. D., Nasonova, O. G.
Format: Article
Language:English
Subjects:
dark matter
galaxies: clusters: individual: Virgo
Stars & galaxies
Velocity
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Summary:We examine the velocity field of galaxies around the Virgo cluster induced by its overdensity. We have studied the velocity–distance relation in Virgocentric coordinates using a sample of 1792 galaxies with distances from the tip of the Red Giant Branch, the Cepheid luminosity, the luminosity of type Ia supernovae, the surface brightness fluctuation method and the Tully–Fisher relation. Attention was paid to some observational biases affecting the Hubble flow around Virgo. We estimate the radius of the zero-velocity surface for the Virgo cluster to be within 5.0–7.5 Mpc, corresponding to 17–26° at the mean cluster distance of 17.0 Mpc. In the case of spherical symmetry with the cosmological parameter Ωm= 0.24 and the age of the Universe T0= 13.7 Gyr, it yields the total mass of the Virgo cluster to be within MT= (2.7–8.9) × 1014 M⊙ in reasonable agreement with the existing virial mass estimates for the cluster.
ISSN:0035-8711
1365-2966
DOI:10.1111/j.1365-2966.2010.16501.x