2015/02/28 by Bon-Chul Koo, Bon‐Chul Koo, Yong‐Hyun Lee +1
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #Ejecta #Emission spectrum #Galaxy #Gamma-ray bursts and supernovae #Infrared #Interstellar medium #Line (geometry) #Near-infrared spectroscopy #Optics #Physics #Spectral line #Spectroscopy #Stars #Supernova #astro-ph.GA
paper · pdf · doi:10.5303/pkas.2015.30.2.145
published as Publications of the Korean Astronomical Society 30 (2015) 145-148 · 4 pages, 4 figures, Invited talk at the 12th Asia-Pacific Regional IAU Meeting, Error in Figure 3 is fixed
openalex publication_date 2015/09/30 · arxiv created 2016/12/29 · arxiv updated 2016/12/30 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Young Galactic supernova remnants (SNRs) are where we can observe closely supernova (SN) ejecta and their interaction with the circumstellar/interstellar medium. They also provide an opportunity to explore the explosion and the final stage of the evolution of massive stars. Near-infrared (NIR) emission lines in SNRs mostly originate from shocked dense material. In shocked SN ejecta, forbidden lines from heavy ions are prominent, while in shocked circumstellar/interstellar medium, [Fe II] and <TEX>H2</TEX> lines are prominent. [Fe II] lines are strong in both media, and therefore [Fe II] line images provide a good starting point for the NIR study of SNRs. There are about twenty SNRs detected in [Fe II] lines, some of which have been studied in NIR spectroscopy. We will review the NIR [Fe II] observations of SNRs and introduce our recent NIR spectroscopic study of the young core-collapse SNR Cas A where we detected strong [P II] lines.