A. Riera,2,3 A. C. Raga,4 B. Reipurth,5 Ph. Amram,6 J. Boulesteix,6 and O. Toledano7
2 Departament de Física i Enginyeria Nuclear, Universitat Politecnica de Catalunya, Av. Víctor Balaguer s/n, E-08800 Vilanova i la Geltrú, Spain (angels.riera@upc.edu).
3 Departament d'Astronomia i Meteorologia. Universitat de Barcelona, Spain.
4 Instituto de Ciencias Nucleares, UNAM, Apdo. Postal 70-543, 04510 México, D. F., México (raga@nucleares.unam.mx).
5 Institute for Astronomy, University of Hawaii, 640 N. Aohoku Place, Hilo, HI 96720, USA (reipurth@ifa.hawaii.edu).
6 Laboratoire d'Astrophysique de Marseille, 2 Place Le Verrier, 13248 Marseille, France (Philippe.Amram@oamp.fr, jacques.boulesteix@oamp.fr).
]]> 7 Instituto de Astronomía, UNAM, Apdo. Postal 70-264, 04510 México, D. F., México.
Received, 2004 December 15
Accepted 2005 April 1
RESUMEN
Presentamos nuevas observaciones Fabry-Perot del sistema HH1/2 en la línea de Hα. Se han obtenidos los perfiles de las líneas, y los mapas de velocidad radial y de dispersión de velocidades a partir de los canales de velocidad de los objetos HH 1 y HH 2. La distribución espacial de la velocidad radial de ambos objetos (HH 1, HH 2) presenta material desplazado al rojo hacia la fuente, y material desplazado al azul alejándose de la fuente. Un modelo que contempla la presencia de emisión directa+dispersada con tres condensaciones emisoras reproduce cualitativamente la distribución espacial de la velocidad radial y de la dispersión de velocidades de HH 2.
ABSTRACT
We present new Hα Fabry-Perot observations of the HH 1/2 system. Line profiles, barycenter radial velocity maps and dispersion maps are derived from the channel maps of HH 1 and HH 2. The radial velocity barycenter maps of both HH 1 and HH 2 show a general trend of "red-shifted upstream/blue-shifted downstream" pattern. A "direct+scattered" component model for three emitting condensations is qualitatively successful at reproducing the general features of the barycenter and the velocity dispersion of HH 2.
]]> Key Words: ISM: Herbig-Haro objects — ISM: Individual (HH 1, HH 2) — ISM: Jets and outflows — ISM: Kinematics and dynamics.
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ACKNOWLEDGMENTS
We acknowledge an anonymous referee for her/his helpful comments. The work of ACR was supported by the CONACyT grants 36572-E and 41320 and the DGAPA (UNAM) grant IN 112602. The work of AR was supported by a grant from the Spanish Ministry of Science and Technology (AYA 2002-00205).
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1 Based on observations collected at the European Southern Observatory, La Silla, Chile.
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