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Title:
Discovery of New Dwarf Galaxies in the M81 Group
Authors:
Chiboucas, Kristin; Karachentsev, Igor D.; Tully, R. Brent
Affiliation:
AA(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., Honolulu, HI 96821, USA ), AB(Special Astrophysical Observatory (SAO) of the Russian Academy of Sciences, Nizhnij Arkhyz 369167, Karachaero-Cherkessia, Russia ), AC(Institute for Astronomy, University of Hawaii, 2680 Woodlawn Dr., Honolulu, HI 96821, USA )
Publication:
The Astronomical Journal, Volume 137, Issue 2, pp. 3009-3037 (2009). (AJ Homepage)
Publication Date:
02/2009
Origin:
IOP
AJ Keywords:
galaxies: clusters individual: M81, galaxies: dwarf, galaxies: fundamental parameters, galaxies: luminosity function, mass function, galaxies: photometry
DOI:
10.1088/0004-6256/137/2/3009
Bibliographic Code:
2009AJ....137.3009C

Abstract

An order of magnitude more dwarf galaxies are expected to inhabit the Local Group, based on currently accepted galaxy formation models, than have been observed. This discrepancy has been noted in environments ranging from the field to rich clusters. However, no complete census of dwarf galaxies exists in any environment. The discovery of the smallest and faintest dwarfs is hampered by the limitations in detecting such faint and low surface brightness galaxies. An even greater difficulty is establishing distances to, or group/cluster membership for, such faint galaxies. The M81 Group provides an almost unique opportunity for establishing membership for galaxies in a low-density region complete to magnitudes as faint as M_{r^{\prime }} = -10. With a distance modulus of 27.8, the tip of the red giant branch just resolves in ground-based surveys. We have surveyed a 65 deg2 region around M81 with Canada-France-Hawaii Telescope/MegaCam. From these images, we have detected 22 new dwarf galaxy candidates. Photometric, morphological, and structural properties are presented for the candidates. The group luminosity function has a faint-end slope characterized by the parameter α = -1.27 ± 0.06. We discuss implications of this dwarf galaxy population for cosmological models.
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