Astronomy and Astrophysics – Astrophysics
Scientific paper
Feb 1986
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...301..105m&link_type=abstract
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 301, Feb. 1, 1986, p. 105-115. NSF-supported research.
Astronomy and Astrophysics
Astrophysics
14
Galactic Radiation, H Lines, Infrared Spectra, Interstellar Matter, Seyfert Galaxies, Balmer Series, Emission Spectra, Interstellar Extinction, Line Spectra
Scientific paper
We have observed the Paα (1.875 μm) and Bry (2.166 μm) lines of hydrogen in a number of Seyfert 1 galaxies. In agreement with the findings published by Lacy et al. in 1982, we find that the Paα line can usually be used as a reddening diagnostic. However, particularly for objects with steep Balmer decrements, the available hydrogen recombination line strengths occasionally deviate sharply from those expected from case B radiative recombination. For steep decrement objects, we conclude that at least two upper level lines should be measured before a strong statement can be made regarding the effects of dust upon the observed spectrum of a Seyfert 1 galaxy. Further observations of the Paβ line (1.28 μm) may be very useful in studying the effects of extreme physical conditions versus those of dust.
Lebofsky Marcia J.
McAlary Christopher Walter
Rieke George H.
Stocke John T.
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