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Title:
INTEGRAL observations of PSR J1811-1925 and its associated pulsar wind nebula
Authors:
Dean, A. J.; de Rosa, A.; McBride, V. A.; Landi, R.; Hill, A. B.; Bassani, L.; Bazzano, A.; Bird, A. J.; Ubertini, P.
Affiliation:
AA(School of Physics and Astronomy, University of Southampton, Highfield, SO17 1BJ), AB(INAF/IASF, via del Fosso del Cavaliere 100, Roma, 00113, Italy), AC(School of Physics and Astronomy, University of Southampton, Highfield, SO17 1BJ), AD(INAF/IASF, via P. Gobetti 101, Bologna, 40129, Italy), AE(School of Physics and Astronomy, University of Southampton, Highfield, SO17 1BJ), AF(INAF/IASF, via P. Gobetti 101, Bologna, 40129, Italy), AG(INAF/IASF, via del Fosso del Cavaliere 100, Roma, 00113, Italy), AH(School of Physics and Astronomy, University of Southampton, Highfield, SO17 1BJ), AI(INAF/IASF, via del Fosso del Cavaliere 100, Roma, 00113, Italy)
Publication:
Monthly Notices of the Royal Astronomical Society: Letters, Volume 384, Issue 1, pp. L29-L33. (MNRAS Homepage)
Publication Date:
02/2008
Origin:
MNRAS
MNRAS Keywords:
pulsars: individual: PSR J1811-1925, supernovae: individual: G11.2-0.3, γ-rays: observations
DOI:
10.1111/j.1745-3933.2007.00415.x
Bibliographic Code:
2008MNRAS.384L..29D

Abstract

We present spectral measurements made in the soft (20-100keV) γ-ray band of the region containing the composite supernova remnant G11.2-0.3 and its associated pulsar PSR J1811-1925. Analysis of INTEGRAL/IBIS data allows characterization of the system above 10keV. The IBIS spectrum is best fitted by a power law having photon index Γ = 1.8+0.4-0.3 and a 20-100keV flux of 1.5 × 10-11 erg cm-2 s-1. Analysis of archival Chandra data over different energy bands rules out the supernova shell as the site of the soft γ-ray emission while broadband (1-200keV) spectral analysis strongly indicates that the INTEGRAL/IBIS photons originate in the central zone of the system which contains both the pulsar and its nebula. The composite X-ray and soft γ-ray spectrum indicates that the pulsar provides around half of the emission seen in the soft γ-ray domain; its spectrum is hard with no sign of a cut off up to at least 80keV. The other half of the emission above 10keV comes from the pulsar wind nebula; with a Γ = 1.7 its spectrum is softer than that of the pulsar. From the IBIS/ISGRI mosaics we are able to derive 2σ upper limits for the 20-100keV flux from the location of the nearby TeV source HESS J1809-193 to be 4.8 ×10-12 erg cm-2 s-1. We have also examined the likelihood of an association between PSR J1811-1925 and HESS J1809-193. Although PSR J1811-1925 is the most energetic pulsar in the region, the only one detected above 10 keV and thus a possible source of energy to fuel the TeV fluxes, there is no morphological evidence to support this pairing, making it an unlikely counterpart.
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