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Structure of the Canes Venatici I cloud of galaxies

Published online by Cambridge University Press:  12 October 2016

Dmitry I. Makarov ,
Lidia N. Makarova  and
Roman I. Uklein
Dmitry I. Makarov
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, 369167Russia email: [email protected], [email protected], [email protected]
Lidia N. Makarova
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, 369167Russia email: [email protected], [email protected], [email protected]
Roman I. Uklein
Affiliation:
Special Astrophysical Observatory, Russian Academy of Sciences, Nizhnii Arkhyz, 369167Russia email: [email protected], [email protected], [email protected]
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Abstract

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We study the spatial distribution of the sparse cloud of galaxies in the Canes Venatici constellation. We determined distances of 30 galaxies using the tip of the red giant branch (TRGB) method. This homogeneous sample allows us to distinguish the zone of chaotic motions around the center of the system. A group of galaxies around M94 is characterized by the mass-luminosity ratio of M/LB=159 (M/L)⊙. It is significantly higher than the typical ratio M/LB=159 (M/L)⊙ for the nearby groups of galaxies. The CVn I cloud of galaxies contains 4–5 times less luminous matter compared with the well-known nearby groups, such as the Local Group, M 81 and Centaurus A. The central galaxy M 94 is at least 1 mag fainter than any other central galaxy of these groups. However, the concentration of galaxies in the Canes Venatici may have a comparable total mass.

Keywords

galaxies: distances and redshifts
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , Symposium S308: The Zeldovich Universe: Genesis and Growth of the Cosmic Web , June 2014 , pp. 209 - 210
Copyright
Copyright © International Astronomical Union 2016 

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