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Revista mexicana de astronomía y astrofísica
versão impressa ISSN 0185-1101
Rev. mex. astron. astrofis vol.44 no.2 Ciudad de México Out. 2008
Kinematics of the Nebular Complex MH9/10/11 Associated with HoIX X1
P. Abolmasov and A. V. Moiseev
Special Astrophysical Observatory, Nizhnij Arkhyz, Zelenchukskij region, KarachaiCirkassian Republic, Russia 369167. (pasha@sao.ru, moisav@sao.ru).
Received 2008 April 18
Accepted 2008 June 26
RESUMEN
Reportamos los resultados de nuestras observaciones del complejo nebular MH9/10/11 asociado a la ULX HoIX X1 usando un interferómetro FabryPérot de barrido. Se distinguen dos regiones con distinta cinemática y distintos cocientes de intensidades de líneas, que corresponden aproximadamente a la nebulosa de burbuja MH9/10 y a una región HII más débil, MH11. Para MH9/10 encontramos una tasa de expansión de 20 a 70 km s1, distinta para la región que se acerca y para la que se aleja. MH11 se caracteriza por una dispersión de velocidades muy pequeña (15 km s1), y por velocidades a lo largo de la visual casi constantes. Las propiedades de MH11 pueden explicarse mediante la fotoionización de un gas con densidad de hidrógeno de ~ 0.2 cm3. La luminosidad requerida para ello debe ser del orden de 1039 erg s1. Una fuente igualmente luminosa se requiere también para explicar la expansión de MH9/10. Los resultados del modelo indican también que la abundancia de oxígeno en MH11 es solar.
ABSTRACT
We report the results of our observations of the nebular complex MH9/10/11, associated with the ULX HoIX X1, with a scanning FabryPérot Interferometer. Two regions differing by their kinematics and line ratios may be distinguished, roughly corresponding to the bubble nebula MH9/10 and the fainter HIIregion MH11. For MH9/10 we find an expansion rate of 20 to 70 km s1 that is different for the approaching and receding parts. MH11 is characterised by a very low velocity dispersion (15 km s1) and nearly constant lineofsight velocities. The properties of MH11 may be explained by photoionization of a gas with hydrogen density of ~ 0.2 cm3. The luminosity required for that should be of the order of 1039 erg s1. A source of similar power is required to explain the expansion rate of MH9/10. Modelling results also indicate that the oxygen abundance in MH11 is about solar.
Key Words: ISM: bubbles ISM: individual (MH9/10/11) ISM: kinematics and dynamics Xrays: individual (HoIX X1).
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