Ma. T. García–Díaz,1 W. J. Henney,2 J. A. López,1 and T. Doi3
1 Instituto de Astronomía, Universidad Nacional Autónoma de México, Ensenada, B. C. Mexico. Instituto de Astronomía, Universidad Nacional Autónoma de México, Apdo. Postal 22860, Ensenada, B. C., Mexico (tere@astrosen.unam.mx, jal@astrosen.unam.mx)
2 Centro de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia, Apdo. Postal 3–72, 58090 Morelia, Michoacán, Mexico (w.henney@astrosmo.unam.mx)
3 Japan Aerospace Exploration Agency, 7–44–1 Jindaiji–Higashi–machi, Chofu–shi, Tokyo 182–8522, Japan (takao.doi1@jsc.nasa.gov)
4 Publicly available from http://www.astrosmo.unam.mx/~w.henney/orionatlas.
Received 2007 October 10 ]]> Accepted 2008 February 5
RESUMEN
Presentamos un atlas4 de espectros tridimensionales (posición–posición–velocidad) de la Nebulosa de Orion en líneas de emisión ópticas de una variedad de diferentes etapas de ionización: [OI] 6300Å, [SII] 6716,6731 Å, [Nil] 6584Å, [SIII] 6312 Å, Hα 6563 Å, y [O III] 5007 Å. Estas transiciones nos dan información punto a punto sobre la estructura física y cinemática de la nebulosa a una resolución efectiva de 3" x 2" x 10 km s–1, mostrando claramente el comportamiento a gran escala del gas ionizado y la presencia de fenómenos localizados tales como flujos colimados relacionados a objetos Herbig–Haro. Como un ejemplo de la aplicación del atlas presentamos un análisis estadístico de los anchos de las líneas de Hα, [O III] y [NII], que permiten una determinación de la temperatura electrónica media en la nebulosa de (9200 ± 400) K. También, en contraste con trabajos anteriores, encontramos que no hay diferencia entre el ensanchamiento no térmico de las líneas de recombinación y el de las líneas colisionales.
ABSTRACT
We present an atlas4 of three–dimensional (position–position–velocity) spectra of the Orion Nebula in optical emission lines from a variety of different ionization stages: [O I] 6300Å, [SII] 6716,6731 Å, [Nil] 6584Å, [SIII] 6312Å, Hα 6563Å, and [O III] 5007 Å. These transitions provide point to point information about the physical structure and kinematics of the nebula at an effective resolution of 3" x 2" x 10 km s–1 , clearly showing the large scale behavior of the ionized gas and the presence of localized phenomena such as Herbig–Haro outflows. As an example application of the atlas, we present a statistical analysis of the widths of the Hα, [OIII], and [NII] lines that permits a determination of the mean electron temperature in the nebula of (9200 ± 400) K. We also find, in contradiction to previous claims, that the non–thermal line broadening is not significantly different between recombination lines and collisional lines.
Key Words: H II regions — ISM: Herbig–Haro objects — ISM: individual: Orion nebula — techniques: spectroscopy — turbulence
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