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2001•Publications of the Astronomical Society of the PacificOpen access

Markarian 478: A Second Seyfert Galaxy with 1 Micron Fe ii Emission Lines

R. J. Rudy, D. K. Lynch, S. Mazuk, C. C. Venturini, R. C. Puetter, Fred Hamann

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Abstract

We present infrared spectroscopy of the narrow‐line Seyfert 1 galaxy Mrk 478 that shows the 1 μm Fe ii lines λ9997, λ10501, λ10863, and λ11126. This is the second active galaxy, after I Zw 1, in which these features have been observed. Like I Zw 1, the 1 μm Fe ii lines of Mrk 478 appear to arise from collisional excitation of their common, intermediate‐energy, upper term. Under this formation process, these features should be common in active galaxies exhibiting strong ultraviolet and optical Fe ii emission but may be obscured in the spectra of the objects with broader lines because of blending with nearby features of hydrogen and helium.

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We present infrared spectroscopy of the narrow‐line Seyfert 1 galaxy Mrk 478 that shows the 1 μm Fe ii lines λ9997, λ10501, λ10863, and λ11126. This is the second active galaxy, after I Zw 1, in which these features have been observed. Like I Zw 1, the 1 μm Fe ii lines of Mrk 478 appear to arise from collisional excitation of their common, intermediate‐energy, upper term. Under this formation process, these features should be common in active galaxies exhibiting strong ultraviolet and optical Fe ii emission but may be obscured in the spectra of the objects with broader lines because of blending with nearby features of hydrogen and helium.

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Available abstract

We present infrared spectroscopy of the narrow‐line Seyfert 1 galaxy Mrk 478 that shows the 1 μm Fe ii lines λ9997, λ10501, λ10863, and λ11126. This is the second active galaxy, after I Zw 1, in which these features have been observed. Like I Zw 1, the 1 μm Fe ii lines of Mrk 478 appear to arise from collisional excitation of their common, intermediate‐energy, upper term. Under this formation process, these features should be common in active galaxies exhibiting strong ultraviolet and optical Fe ii emission but may be obscured in the spectra of the objects with broader lines because of blending with nearby features of hydrogen and helium.

Key concepts: Physics, Galaxy, Astrophysics, Emission spectrum, Line (geometry), Active galactic nucleus, Spectral line, Spectroscopy

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