The Molecular Core Associated with HH 25-26: Contraction or Expansion?

Details The Molecular Core Associated with HH 25-26: Contraction or Expansion? The Molecular Core Associated with HH 25-26: Contraction or Expansion?

Dec 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...473..929v&link_type=abstract

Astrophysical Journal v.473, p.929

Astronomy and Astrophysics

Astronomy

5

Ism: Clouds, Ism: Individual Alphanumeric: Hh 25-26, Ism: Jets And Outflows, Ism: Molecules, Stars: Pre-Main-Sequence

Scientific paper

We mapped the star formation region HH 25-26 IR in the NH3(1, 1) and (2, 2) transitions using the VLA in its D configuration. The study has been made with 5" angular resolution and 0.3 km 1 velocity resolution.
As has been seen before, there is an elongated NH3 core that lies perpendicular to the molecular outflow as traced in high-velocity CO emission. In this experiment, the NH3 core is resolved, showing a central cavity and a number of distinct velocity features. Heating is seen at the position where the velocity features overlap spatially, and on the edges of the cavity, which is also seen as a reflection nebula with evidence for shock excitation. We have also detected what appears to be a new 1.3 cm continuum source on the wall of the cavity, associated with a 2.2 μm point source and jetlike structure. It is not clear at this time whether this is a truly continuum emission or high-velocity ammonia emission. The overall kinematics is complicated. A velocity gradient can be seen, together with the signatures for expanding or contracting motions.
We consider here two possible models: (a) a disk or ring structure, slowly rotating and contracting, and (b) an expanding cavity.

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