Luis F. Rodríguez,1,2 Bo Reipurth,3,4 and Hsin-Fang Chiang3,4
1 Centro de Radioastronomía y Astrofísica, UNAM, Apdo. Postal, 3-72, (Xangari), 58089 Morelia, Michoacán, México (l.rodriguez@crya.unam.mx).
2 Astronomy Department, Faculty of Science, King Abdulaziz University, Saudi Arabia.
3 Institute for Astronomy, University of Hawaii at Manoa, 640 North Aohoku Place, Hilo, HI 96720, USA (hchiang, reipurth@ifa.hawaii.edu).
4 NASA Astrobiology Institute, University of Hawaii at Manoa, Hilo, HI, USA.
]]> Received 2014 April 14.
RESUMEN
Presentamos observaciones de alta resolución angular y alta sensitividad en el radiocontinuo a 8.46 GHz (3.6 cm) hacia el núcleo del flujo HH 92 hechas con el Very Large Array en 2002-2003 y con el Expanded Very Large Array en 2011. Detectamos un grupo de tres fuentes compactas distribuidas en una región con 2" de extensión y discutimos su naturaleza. Concluimos que una de las fuentes (VLA 1) es la excitadora del flujo gigante asociado con HH 92. En el caso de HH 34 presentamos nuevas observaciones a 43.3 GHz (7 mm) que revelan la presencia de una estructura asociada con la fuente excitadora y alargada perpendicularmente al chorro óptico altamente colimado en la región. Proponemos que la fuente de 7 mm es un disco circunestelar con radio de ≈80 AU y masa de ≈0.21 Mʘ.
ABSTRACT
We present high angular resolution, high sensitivity 8.46 GHz (3.6 cm) radio continuum observations made toward the core of the HH 92 outflow with the Very Large Array in 2002-2003 and with the Expanded Very Large Array in 2011. We detect a group of three compact sources distributed in a region 2" in extension and discuss their nature. We conclude that one of the objects (VLA 1) is the exciting source of the giant outflow associated with HH 92. In the case of HH 34 we present new 43.3 GHz (7 mm) observations that reveal the presence of a structure associated with the exciting source and elongated perpendicularly to the highly collimated optical jet in the region. We propose that this 7 mm source is a circumstellar disk with radius of ≈80 AU and mass of ≈0.21 Mʘ.
Key Words: ISM: jets and outflows — radio continuum: stars — stars: formation — stars: mass-loss.
]]> DESCARGAR ARTÍCULO EN FORMATO PDF
ACKNOWLEDGMENTS
LFR acknowledges the support of DGAPA, UNAM, and of CONACyT (Mexico). BR and HFC acknowledge support by the National Aeronautics and Space Administration through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A issued through the Office of Space Science. This research has made use of the SIMBAD database, operated at CDS, Strasbourg, France.
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