Recombination spectrum and reddening in NGC 1068
Abstract
Measurements of the emission-line intensities of NGC 1068 have been made over the wavelength range extending from λ_(rest) = 1216 Å to 1.875 μm. 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 E_(B-v) = 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 interstellar 2200 A feature nor does it contain enough energy to power the observed infrared flux.
Additional Information
© 1980 American Astronomical Society. Received 1979 November 7; accepted 1979 December 11. We thank D. Peterson for providing us with stellar models, D. Cruikshank for giving us the spectrum of the atmosphere above Mauna Kea, W. Sargent and D. Helfand for providing observations prior to publication, and W. Stein for commenting on the text. The work has been supported by NASA grants NGL 05-002-207, NSG 5243, NGL 05-002-134, and NSF grant AST77-20516.Attached Files
Published - 1980ApJ___238__502N.pdf
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Additional details
- Eprint ID
- 74735
- Resolver ID
- CaltechAUTHORS:20170303-153446408
- NASA
- NGL 05-002-207
- NASA
- NSG 5243
- NASA
- NGL 05-002-134
- NSF
- AST77-20516
- Created
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2017-03-06Created from EPrint's datestamp field
- Updated
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2021-11-11Created from EPrint's last_modified field