The molecular environment of the HH 34 system

Details The molecular environment of the HH 34 system The molecular environment of the HH 34 system

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995apj...443..682a&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 443, no. 2, p. 682-697

Astronomy and Astrophysics

Astronomy

21

Ammonia, Herbig-Haro Objects, Interstellar Gas, Jet Flow, Molecules, Radio Astronomy, Radio Spectra, Stellar Evolution, Stellar Winds, Astronomical Maps, Cavities, Data Reduction, Optical Polarization, Radio Antennas, Very Large Array (Vla)

Scientific paper

We present single-dish (angular resolution approximately 40 sec) and Very Large Array (VLA; angular resolution approximately 4 sec) ammonia observations toward the HH 34 region. Two main condensations are distinguished in both our single-dish and out VLA maps. The northern ammonia condensation is resolved by the VLA as an arclike structure that surrounds the east side of the star HH 34 IRS (the exciting source of the jet) and coincides in projection with Re 24, the reflection nebula associated with the infrared source IRS 5. We suggest that this ammonia structure is tracing the wall of a cavity around HH 34 IRS. Our results are in good agreement with the hypothesis that this cavity was created by the stellar wind from HH 34 IRS, indicating that along the life of the star two kinds of stellar wind might have been present: a low-collimation wind that created the cavity, and a highly collimated wind that is at the origin of the jet. A second VLA ammonia condensation coincides with Re 23, the brightest part of the arc of optical nebulosity previously proposed to be tracing the western wall of a cavity that contains the jet. The inner edges of these two ammonia condensations coincide with zones of a high level of polarization of the optical emission. With the angular resolution of our VLA observations, no ammonia (1, 1) emission is detected directly associated with the star HH 34 IRS, setting an upper limit of 0.1/(X(NH3)/10-8) solar masses for the mass of a possible circumstellar disk. From our single-dish observations, we find that there is extended emission (approximately 3 min) of high-density gas, not seen with the VLA. For this gas, we estimate a total mass of approximately 15 solar masses and a kinetic temperature of 15 K.

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