The origin of broad emission lines in the extragalactic giant H II region NGC 2363

Details The origin of broad emission lines in the extragalactic giant H II region NGC 2363 The origin of broad emission lines in the extragalactic giant H II region NGC 2363

Feb 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992apj...386..498r&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 386, Feb. 20, 1992, p. 498-505. Research supported by NSERC.

Astronomy and Astrophysics

Astrophysics

50

Emission Spectra, H Ii Regions, Interstellar Gas, Interstellar Matter, Line Spectra, Dwarf Galaxies, Electron Scattering, Spectral Line Width, Spectrum Analysis, Stellar Winds, Ultraviolet Spectroscopy, Visible Spectrum

Scientific paper

High signal-to-noise long-slit spectra have been obtained of the giant H II region NGC 2363 located in the dwarf SBm galaxy NGC 2366. A discovery of low-intensity broad spectral components (FWHM is approximately equal to 40 A or 2400 km/s) in the bright nebular lines H-alpha, H-beta, and forbidden O III is reported. The broad spectral components are detected over a large spatial extent (not less than 500 pc) centered on the nebula. Several mechanisms for broadening nebular lines are explored: stellar winds, Thomson scattering by hot gas, supernova remnants, and superbubble blowout. All mechanisms have problems. Superbubble blowout, which is the only known mechanism capable of accelerating interstellar gas over such a volume of space, does not appear consistent with the physical properties of the H II region NGC 2363 or with the nature of the host galaxy. It is concluded that the broad nebular lines are probably due to very high velocity gas whose origin is, at present, unknown.

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