Recombination spectrum and reddening in NGC 1068

Details Recombination spectrum and reddening in NGC 1068 Recombination spectrum and reddening in NGC 1068

Jun 1980

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1980apj...238..502n&link_type=abstract

Astrophysical Journal, Part 1, vol. 238, June 1, 1980, p. 502-509.

Other

88

Galactic Nuclei, Interstellar Extinction, Optical Emission Spectroscopy, Radiative Recombination, Seyfert Galaxies, Continuous Spectra, Data Reduction, H Ii Regions, Infrared Spectra, Iue, Radiant Flux Density, Spectral Energy Distribution, Ultraviolet Spectra

Scientific paper

Measurements of the emission-line intensities of NGC 1068 have been made over the wavelength range extending from rest wavelengths equal to 1216 A to 1.875 micron. The data, plus other available emission-line data, can be explained in terms of a simple model where the emission lines are formed in an H II region, and the line ratios are consistent with those predicted by standard radiative recombination theory and reddening corresponding to 0.4 mag. The continuum flux is seen to consist of a galaxy component plus a nonstellar component which dominates the observed flux in the ultraviolet. The observed ultraviolet continuum does not show an absorption dip caused by the intertellar 2200 A feature nor does it contain enough energy to power the observed infrared flux.

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