Journal Article

The deepest radio study of the pulsar wind nebula G21.5−0.9: still no evidence for the supernova shell

M. F. Bietenholz, H. Matheson, S. Safi-Harb, C. Brogan and N. Bartel

in Monthly Notices of the Royal Astronomical Society

Published on behalf of The Royal Astronomical Society

Volume 412, issue 2, pages 1221-1228
Published in print April 2011 | ISSN: 0035-8711
Published online March 2011 | e-ISSN: 1365-2966 | DOI:
The deepest radio study of the pulsar wind nebula G21.5−0.9: still no evidence for the supernova shell

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We report on sensitive new 1.4-GHz Very Large Array radio observations of the pulsar wind nebula G21.5−0.9, powered by PSR J1833−1034, and its environs. Our observations were targeted at searching for the radio counterpart of the shell-like structure seen surrounding the pulsar wind nebula in X-rays. Some such radio emission might be expected as the ejecta from the ≲1000 yr old supernova expand and interact with the surrounding medium. We find, however, no radio emission from the shell, and can place a conservative 3σ upper limit on its 1-GHz surface brightness of 7 × 10−22 W m−2 Hz−1 sr−1, comparable to the lowest limits obtained for radio emission from shells around other pulsar wind nebulae. In addition, our wide-field radio image also shows the presence of two extended objects of low surface brightness. We re-examine previous 327-MHz images, on which both the new objects are visible. We identify the first, G21.64−0.84, as a new shell-type supernova remnant, with a diameter of ∼13 arcmin and an unusual double-shell structure. The second, G21.45−0.59, ∼1 arcmin in diameter, is likely an H ii region.

Keywords: ISM: supernova remnants

Journal Article.  5823 words.  Illustrated.

Subjects: Astronomy and Astrophysics

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