2009/02/06 by J. Wang, J. Y. Wei, P. F. Xiao
Physics and Astronomy · #Astronomical spectroscopy #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Emission spectrum #Gamma-ray bursts and supernovae #Line (geometry) #Population #Spectral line #Stellar evolution #Supernova #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1088/0004-637x/693/2/l66
12 pages, 2 figures, accepted by ApJ Letter
arxiv created 2009/02/06 · openalex publication_date 2009/02/17 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
The nature of low-ionization nuclear emission-line regions (LINERs) has been an open question for a long time. We study the properties of LINERs from several different aspects. The LINERs are found to consist of two different categories that can be clearly separated in the traditional Baldwin–Phillips–Terlevich diagrams, especially in the [O i ]/Hα versus [O iii ]/Hβ diagram. LINERs with high [O i ]/Hα ratios (Population I) differ from ones with low ratios (Population II) in several properties. Broad emission lines are only identified in the spectra of Population I LINERs. While only the Population II LINERs show luminous infrared emission and occurrence of core-collapse supernovae in the host. Combining these results with the known distribution of stellar populations not only suggests that the two populations have different line-excitation mechanisms, but also implies that they are at different evolutionary stages.