Документ взят из кэша поисковой машины. Адрес оригинального документа : http://www.sao.ru/precise/Laboratory/Publications/1999/0335W_mmt/0335w6/0335w6.html
Дата изменения: Tue Nov 24 21:32:27 1998
Дата индексирования: Sat Sep 11 22:14:21 2010
Кодировка:

Special Astrophysical Observatory, Russian Academy of Sciences, Nizhny Arkhyz, Karachai-Circessia 357147, Russia
Electronic mail: val@sao.ru - W. M. Keck Observatory, 65-1120 Mamalahoa Hwy., Kamuela, HI 96743
Electronic mail: fchaffee@keck.hawaii.edu - Main Astronomical Observatory, Ukrainian National Academy of Sciences, Goloseevo, Kiev 252650, Ukraine
Electronic mail: izotov@mao.kiev.ua - Multiple Mirror Telescope Observatory, University of Arizona, Tucson, AZ 85721
Electronic mail: cfoltz@as.arizona.edu - Special Astrophysical Observatory, Russian Academy of Sciences, Nizhny Arkhyz, Karachai-Circessia 357147, Russia
Electronic mail: akn@sao.ru - Universitäts-Sternwarte, Scheiner Str. 1, D-81679, Munich, Germany
Electronic mail: hopp@usm.uni-muenchen.de

Abstract:

We present Multiple Mirror Telescope (MMT) and Keck II telescope spectrophotometry and 3.5m Calar Alto telescope R, I photometry of the western component of the extremely low-metallicity blue compact galaxy SBS 0335-052. Both components, separated by 22 kpc, resemble a unique, physically connected system. It is shown that the new component, SBS 0335-052W, consists of at least of three stellar clusters and has the same redshift as SBS 0335-052. The oxygen abundance in its two brightest knots is extremely low, 12 + log (O/H) = 7.22$\pm$0.03 and 7.13$\pm$0.07, respectively. These values are lower than in SBS 0335-052 and are nearly the same as those in I Zw 18. The (R-I) color profiles are very blue in both galaxies due to the combined effects of ionized gas and a young stellar population emission. We argue that SBS 0335-052W is a good candidate for a nearby, young dwarf galaxy.

galaxies: abundances -- galaxies: irregular -- galaxies: photometry -- galaxies: evolution -- galaxies: formation -- galaxies: ISM -- HII regions -- ISM: abundances