A Near‐Infrared Spectroscopic Survey of LINER Galaxies

Abstract

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), H2 [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 H2 emission, with about half (four of nine) having extremely high ratios (>2) of [Fe II] to Paβ. The strength of the H2 and [Fe II] lines is well correlated with the optical [O I] line, with many LINERs having higher ratios of [Fe II]/Paβ, H2/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.