The Honeycomb supernova remnant

You Hua Chu, John R. Dickel, Lister Staveley-Smith, Jürgen Osterberg, R. Chris Smith

Research output: Contribution to journalArticle

Abstract

At 2′.5 southeast of SN 1987 A, the Honeycomb Nebula is named after its interesting morphology, which consists of over ten loops with sizes of 2-3 pc. High-dispersion spectra of these loops show hemispheres expanding toward the observer at 100-300 km s-1. Using archival X-ray data and a combination of new and archival radio data, we find bright X-ray and nonthermal radio emission associated with the Honeycomb Nebula. New CCD images further show enhanced [S II]/Hα ratios. These results confirm a model in which the Honeycomb Nebula is due to a supernova shock front, traveling toward the observer, encountering an intervening sheet of dense, but porous, interstellar gas. The bulk of the supernova remnant resides in a low-density cavity, and is not otherwise visible. The situation is similar to the hidden supernova remnants postulated for the X-ray bright superbubbles. The Honeycomb Nebula has an unusually steep radio spectral index (Sv ∝ v-1.2), normally associated with young SNRs.

Original languageEnglish (US)
Pages (from-to)1729-1734
Number of pages6
JournalAstronomical Journal
Volume109
Issue number4
DOIs
StatePublished - Apr 1995

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

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    Chu, Y. H., Dickel, J. R., Staveley-Smith, L., Osterberg, J., & Smith, R. C. (1995). The Honeycomb supernova remnant. Astronomical Journal, 109(4), 1729-1734. https://doi.org/10.1086/117401