2002/02/13 by Cindy Tam, Cindy R. Tam, M. S. Roberts +3 · 29 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Cosmic Phenomena #Physics #Pulsar #Pulsar wind nebula #Pulsars and Gravitational Waves Research #Radio Astronomy Observations and Technology #Spectral index #Spectral line #Supernova #Supernova remnant #astro-ph
paper · pdf · doi:10.1086/340229
published in The Astrophysical Journal 572(1), 202-208 (IOP Publishing) · 9 pages, 5 figures, Accepted to the Astrophysical Journal
arxiv created 2002/02/13 · openalex publication_date 2002/06/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We present a high-resolution radio study of the supernova remnant (SNR) G11.2-0.3 using archival Very Large Array data. Spectral tomography is performed to determine the properties of this composite-type SNR's individual components, which have only recently been distinguished through X-ray observations. Our results indicate that the spectral index of the pulsar wind nebula (PWN), or plerion, is α P = 0.25 . We observe a spectral index of α S = 0.56 ± 0.02 throughout most of the SNR shell region but also detect a gradient in α in the southeastern component. We compare the spectral index and flux density with recent single-dish radio data of the source. Also, the radio efficiency and morphological properties of this PWN are found to be consistent with results for other known PWN systems.