Scanning interferometer observations of the shell N186E in the Large Magellanic Cloud

Details Scanning interferometer observations of the shell N186E in the Large Magellanic Cloud Scanning interferometer observations of the shell N186E in the Large Magellanic Cloud

Nov 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...238..315r&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 238, no. 1-2, Nov. 1990, p. 315-324.

Astronomy and Astrophysics

Astrophysics

14

Interferometers, Interstellar Matter, Magellanic Clouds, Nebulae, Stellar Envelopes, Emission Spectra, H Alpha Line, Scanning, Supernova Remnants, Velocity Distribution

Scientific paper

The velocity field ad the H-alpha flux of the large shell N186E of the LMC are measured over a 7 x 7 arcsec field, covering most of the filamentary structure. The radial velocity field appears to be contaminated by faint blue-shifted and red-shifted emission which confirms the presence of H-I slabs along the line of sight. The remaining gas in N186E does not show high velocity expansion motions (25 km/s), much less than found inside the similar but smaller bubble N185. The recently detected exciting stars are sufficient to explain the ionization of N186E, although none of them is located close to the center. The density inside the filaments is produced by weak shocks, whereas the circular shape and the size of the shell indicate homogeneity of the preshock material. An intense interaction is found at the dense border between N186E and the young neighboring SNR, N186D. N186E is probably an old SNR, now being ionized by internal stars.

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