The kinematic structure of the HH 24 complex derived from high-resolution spectroscopy

Details The kinematic structure of the HH 24 complex derived from high-resolution spectroscopy The kinematic structure of the HH 24 complex derived from high-resolution spectroscopy

Oct 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...184..322s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 184, no. 1-2, Oct. 1987, p. 322-328.

Astronomy and Astrophysics

Astrophysics

54

Herbig-Haro Objects, Interstellar Gas, Jet Flow, Mass Flow, Stellar Mass Ejection, Stellar Spectrophotometry, Charge Coupled Devices, H Alpha Line, High Resolution

Scientific paper

High-resolution long-slit spectra obtained from various positions within the HH 24 complex are presented. The radial velocity field deduced from the spatially resolved emission line features indicates the presence of a bipolar system of highly collimated mass flow (jets) with velocities exceeding 200 km s-1. The bipolar structure presents a remarkable degree of symmetry and consists of the elongated nebular component HH 24C and a new weak component, designated HH 24F, which has been identified by its high positive radial velocity. HH 24F is elongated (2arcsec×15arcsec) resembling its counterpart HH 24C in both shape and orientation. The infrared source SSV 63 is located near the midpoint on the line joining HH 24C and HH 24F, suggesting that the bipolar jets are emanating from that source. Hence SSV 63 is probably a young stellar object and the main source of excitation of the HH 24 complex. Some evidence is presented that HH 24A traces the region where the head of the jet (HH 24F) interacts with a condensation in the ambient material.

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