NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-06-19 T10:59:42 PDT
Help | Comment | NED Home

For refcode 2002A&A...389..855E:
Retrieve 1 NED object in this reference.
Please click here for ADS abstract

NED Abstract

Copyright by European Southern Observatory (ESO). Reproduced by permission
2002A&A...389..855E 6-m telescope spectroscopic observations of the bubble complex in NGC 6946 Yu. N. Efremov, S. A. Pustilnik, A. Y. Kniazev, B. G. Elmegreen, S. S. Larsen, E. J. Alfaro, P. W. Hodge, A. G. Pramsky and T. Richtler Sternberg Astronomical Institute of Moscow State University, Universitetsky Prospect, 13, Moscow, 119899, Russia Special Astrophysical Observatory of RAS, Nizhnij Arkhyz, Karachai-Circassia, 369167, Russia Isaac Newton Institute of Chile, SAO Branch, Russia Max Planck Institut fur Astronomie, Konigstuhl 17, 69117, Heidelberg, Germany IBM Research Division, T.J. Watson Research Center, PO Box 218, Yorktown Heights, NY 10598, USA UC Observatories / Lick Observatory, University of California, Santa Cruz, CA 95064, USA Instituto de Astrofisica de Andalucia, 18008 Granada, Spain University of Washington, Seattle, USA Grupo de Astronomia, Departamento de Fisica, Casilla 160-C, Universidad de Concepcion, Concepcion, Chile Received 9 September 2001/Accepted 16 May 2002 Abstract. We describe the results of a long-slit spectroscopic study of an unusual star complex in the nearby spiral galaxy NGC 6946 using the SAO 6 m telescope and the Keck 10 m telescope. The complex resembles a circular bubble 600 pc in diameter with a young super star cluster (SSC) near the center. The kinematics of ionized gas is studied through H{alpha} emission with several slit positions. Position-velocity diagrams show two distinct features with high speed motions. One is an irregularly shaped region to the east of the SSC, 270 pc in size, in which most of the H{alpha} emission is blue shifted by 120 km s^-1^, and another is a 350 pc shell centered on the SSC with positive and negative velocity shifts of 60 km s^-1^. Balmer and He I absorption lines in the SSC give an age of 12-13 Myr, which is consistent with the photometric age but significantly older than the kinematic ages of the high speed regions. The energetics of the SSC and its interaction with the environment are considered. The expansion energies exceed 10^52^ ergs, but the power outputs from winds and supernova in the SSC are large enough to account for this. The intensities of Balmer, N II, and S II emission lines within and around the complex indicate that shock excitation makes a significant contribution to the emission from the most energetic region. Key words: galaxies: ISM - galaxies: globular clusters: general - galaxies: formation - galaxies: individual: NGC 6946 - ISM: bubbles
Retrieve 1 NED object in this reference.
Please click here for ADS abstract

Back to NED Home