TY - JOUR
T1 - A broadband study of the emission from the composite supernova remnant MSH 11-62
AU - Slane, Patrick
AU - Hughes, John P.
AU - Temim, Tea
AU - Rousseau, Romain
AU - Castro, Daniel
AU - Foight, Dillon
AU - Gaensler, B. M.
AU - Funk, Stefan
AU - Lemoine-Goumard, Marianne
AU - Gelfand, Joseph D.
AU - Moffett, David A.
AU - Dodson, Richard G.
AU - Bernstein, Joseph P.
PY - 2012/4/20
Y1 - 2012/4/20
N2 - MSH 11-62 (G291.0-0.1) is a composite supernova remnant for which radio and X-ray observations have identified the remnant shell as well as its central pulsar wind nebula. The observations suggest a relatively young system expanding into a low-density region. Here, we present a study of MSH 11-62 using observations with the Chandra, XMM -Newton, and Fermi observatories, along with radio observations from the Australia Telescope Compact Array. We identify a compact X-ray source that appears to be the putative pulsar that powers the nebula, and show that the X-ray spectrum of the nebula bears the signature of synchrotron losses as particles diffuse into the outer nebula. Using data from the Fermi Large Area Telescope, we identify γ-ray emission originating from MSH 11-62. With density constraints from the new X-ray measurements of the remnant, we model the evolution of the composite system in order to constrain the properties of the underlying pulsar and the origin of the γ-ray emission.
AB - MSH 11-62 (G291.0-0.1) is a composite supernova remnant for which radio and X-ray observations have identified the remnant shell as well as its central pulsar wind nebula. The observations suggest a relatively young system expanding into a low-density region. Here, we present a study of MSH 11-62 using observations with the Chandra, XMM -Newton, and Fermi observatories, along with radio observations from the Australia Telescope Compact Array. We identify a compact X-ray source that appears to be the putative pulsar that powers the nebula, and show that the X-ray spectrum of the nebula bears the signature of synchrotron losses as particles diffuse into the outer nebula. Using data from the Fermi Large Area Telescope, we identify γ-ray emission originating from MSH 11-62. With density constraints from the new X-ray measurements of the remnant, we model the evolution of the composite system in order to constrain the properties of the underlying pulsar and the origin of the γ-ray emission.
KW - ISM: individual objects (MSH-11-62)
KW - ISM: supernova remnants
KW - radiation mechanisms: non-thermal
KW - stars: neutron
UR - http://www.scopus.com/inward/record.url?scp=84859369702&partnerID=8YFLogxK
UR - http://www.scopus.com/inward/citedby.url?scp=84859369702&partnerID=8YFLogxK
U2 - 10.1088/0004-637X/749/2/131
DO - 10.1088/0004-637X/749/2/131
M3 - Article
AN - SCOPUS:84859369702
SN - 0004-637X
VL - 749
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 2
M1 - 131
ER -