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Recombination spectrum and reddening in NGC 1068
Neugebauer, G.; Morton, D.; Oke, J. B.; Becklin, E.; Daltabuit, E.; Matthews, K.; Persson, S. E.; Smith, A. M.; Soifer, B. T.; Torres-Peimbert, S.; Wynn-Williams, C. G.
AA(California Institute of Technology, Pasadena, Calif.), AB(California Institute of Technology, Pasadena, Calif.), AC(California Institute of Technology, Pasadena, Calif.), AD(Anglo-Australian Observatory, Epping, New South Wales, Australia), AE(California Institute of Technology; Palomar Observatory, Palomar Mountain, Calif.), AF(Hawaii, University, Honolulu, Hawaii), AG(Universidad Nacional Autonoma de Mexico, Mexico City, Mexico), AH(Universidad Nacional Autonoma de Mexico, Mexico City, Mexico), AI(Mount Wilson and Las Campanas Observatoires, Pasadena, Calif.), AJ(NASA, Goddard Space Flight Center, Greenbelt, Md.)
Astrophysical Journal, Part 1, vol. 238, June 1, 1980, p. 502-509. (ApJ Homepage)
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NASA/STI Keywords:
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
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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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