2011/04/28 by И. Д. Караченцев, Igor Karachentsev, Elena Kaisina +5
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Dwarf galaxy #Dwarf spheroidal galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Interacting galaxy #Irregular galaxy #Knot (papermaking) #Local Group #Physics #Star formation #Stars #Stellar, planetary, and galactic studies #astro-ph.CO
paper · pdf · doi:10.1111/j.1745-3933.2011.01069.x
published as MNRAS Letters, 2011 · 6 pages, 4 figures, accepted
arxiv created 2011/04/28 · openalex publication_date 2011/06/07 · arxiv updated 2015/05/28 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
Abstract We use Hα images of three clumps of young stars situated between M 81 and NGC 3077 to estimate their star formation rate. Radial velocities of the clumps measured by us, as well as the velocity of the H ii region in the dwarf spheroidal (dSph) galaxy KDG 61, are compatible with their location at the outskirts of a large rotating gaseous disc around M 81. In contrast to KDG 61, the radial velocity of the emission knot in the dSph galaxy DDO 44, +213 ± 25 km s-1, tells us that this Hα spark belongs to the dSph galaxy itself. F475W and F814W images of DDO 44 extracted from the Hubble Space Telescope archive reveal eight bluish (B − I < 0.8) stars apparently associated with the Hα knot.