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Title:
Measurement of Spectral Breaks in Pulsar Wind Nebulae with Millimeter-Wave Interferometry
Authors:
Bock, D. C.-J.; Gaensler, B. M.
Affiliation:
AA(Radio Astronomy Laboratory, University of California, Berkeley, CA 94720; ), AB(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-6, Cambridge, MA 02138; )
Publication:
The Astrophysical Journal, Volume 626, Issue 1, pp. 343-349. (ApJ Homepage)
Publication Date:
06/2005
Origin:
UCP
ApJ Keywords:
Stars: Pulsars: Individual: Alphanumeric: PSR J1846-0258, Radio Continuum: ISM, Stars: Supernovae: Individual: Alphanumeric: G11.2-0.3, Stars: Supernovae: Individual: Alphanumeric: G16.7+0.1, Stars: Supernovae: Individual: Alphanumeric: G29.7-0.3, ISM: Supernova Remnants
DOI:
10.1086/429789
Bibliographic Code:
2005ApJ...626..343B

Abstract

We have observed pulsar wind nebulae (PWNe) in the three supernova remnants G11.2-0.3, G16.7+0.1, and G29.7-0.3 at 89 GHz with the Berkeley-Illinois-Maryland Association array, measuring total flux densities of two of them for comparison with archival data at other frequencies. In G16.7+0.1, we find a break in the spectrum of the PWN at ~26 GHz. In G29.7-0.3, our data suggest a break in the integrated spectrum of the central nebula at ~55 GHz, lower than previously estimated. However, we have found spatial structure in the spectrum of this nebula. The emission to the north of pulsar J1846-0258 has a broken spectrum with break frequency <~100 GHz, consistent with a conventional pulsar-powered nebula. The emission to the south of the pulsar has a nearly power-law spectrum from radio to X-rays: this component may be unrelated to the PWN, or it may be evidence of asymmetries and/or time evolution in the pulsar's energy output. We present 89 GHz images of each remnant.
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