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The tip-of-the-red-giant-branch distance indicator and the structure of the nearest galaxy groups

Published online by Cambridge University Press:  26 February 2013

Lidia Makarova  and
Dmitry Makarov
Lidia Makarova
Affiliation:
Special Astrophysical Observatory, Nizhnij Arkhyz, Karachai–Cherkessian Republic, Russia, 369167 email: [email protected]
Dmitry Makarov
Affiliation:
Special Astrophysical Observatory, Nizhnij Arkhyz, Karachai–Cherkessian Republic, Russia, 369167 email: [email protected]
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Abstract

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The tip of the red giant branch (TRGB) is one of the most accurate distance indicators to galaxies in the Local Universe (for distances up to 8–10 Mpc). A distance accuracy as high as 5% can be achieved with the recently developed maximum-likelihood implementation of the TRGB method and modern calibrations. In this paper, we consider in detail TRGB distance determinations to nearby groups of galaxies (within 8 Mpc). We discuss the photometric accuracy and describe colour–magnitude-diagram features of nearby dwarf galaxies and their influence on the accuracy of distance determination. We have determined accurate structures of the two nearest galaxy groups, M81 and Cen A, using observations of galaxies in these groups with the Hubble Space Telescope's WFPC2 and ACS instruments. The new technique allows us to see new details in the distribution of galaxies in the Canes Venatici i Cloud.

Keywords

galaxies: distances and redshiftsgalaxies: dwarfgalaxies: stellar content
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 8 , Symposium S289: Advancing the Physics of Cosmic Distances , August 2012 , pp. 240 - 243
Copyright
Copyright © International Astronomical Union 2013

References

Karachentsev, I. D., Dolphin, A., Tully, R. B., et al. 2006, AJ, 131, 1361CrossRefGoogle Scholar
Karachentsev, I. D., Tully, R. B., Dolphin, A., et al. 2007, AJ, 133, 504Google Scholar
Lee, M. G., Freedman, W. L., & Madore, B. F. 1993, ApJ, 417, 553Google Scholar
Makarov, D., Makarova, L., Rizzi, L., Tully, R. B., Dolphin, A. E., Sakai, S., & Shaya, E. J. 2006, AJ, 132, 2729Google Scholar
Makarov, D., Makarova, L., Sharina, M., Uklein, R., Tikhonov, A., Guhathakurta, P., Kirby, E., & Terekhova, N. 2012, MNRAS, 425, 709Google Scholar
Makarova, L. N., Grebel, E. K., Karachentsev, I. D., et al. 2002, A&A, 396, 473Google Scholar
Makarova, L., Makarov, D., Dolphin, A., et al. 2007, Proc. IAU Symp., 235, 320Google Scholar
Méndez, B., Davis, M., Moustakas, J., Newman, J., Madore, B. F., & Freedman, W. L. 2002, AJ, 124, 213CrossRefGoogle Scholar
Rizzi, L., Tully, R. B., Makarov, D., Makarova, L., Dolphin, A. E., Sakai, S., & Shaya, E. J. 2007, ApJ, 661, 815Google Scholar
Sakai, S., Madore, B. F., & Freedman, W. L. 1996, ApJ, 461, 713Google Scholar