1997/08/11 by James E. Larkin, J. E. Larkin, L. Armus +3 · 7 citations
Physics and Astronomy · #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #Stellar, planetary, and galactic studies #astro-ph
paper · pdf · doi:10.1086/313063
36 pages, Plain LaTex(epsf) with 8 postscript figures, ApJ Supplements, accepted
arxiv created 1997/08/11 · openalex publication_date 1998/01/01 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
This paper reports the results of a near-infrared spectroscopic survey of LINER galaxies undertaken with a new infrared spectrograph at the 5 m Hale telescope. The galaxy sample includes 11 LINERs with spectra covering the [Fe II] (1.2567 μm), Paβ (1.2818 μm), H 2 [1-0 S (1), 2.1218 μm], and Brγ (2.1655 μm) near-infrared emission lines and one additional galaxy with only [Fe II] and Paβ line coverage. All of the LINERs with infrared line detections have strong [Fe II] and/or H 2 emission, with about half (four of nine) having extremely high ratios (>2) of [Fe II] to Paβ. The strength of the H 2 and [Fe II] lines is well correlated with the optical [O I] line, with many LINERs having higher ratios of [Fe II]/Paβ, H 2 /Brγ, and [O I]/Hα than other galaxy types. The LINERs with the highest [Fe II]/Paβ ratios (termed "strong" [Fe II] LINERs) show evidence for recent star formation. Shocks from compact supernova remnants may enhance the [Fe II] emission in these "strong" [Fe II] LINERs. The LINERs with lower [Fe II]/Paβ ratios (termed "weak" [Fe II] LINERs) are more consistent with Seyfert-like activity, including higher ionization states, some strong X-ray sources, and some broad Hα detections. The [Fe II] luminosity and the [Fe II]/Paβ ratio in these objects are more easily explained by hard X-ray excitation than in the "strong" [Fe II] LINERs. These "weak" [Fe II] LINERs are considered prime candidates for being low-luminosity Seyfert nuclei.