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INTEGRAL observations of PSR J1811?1925 and its associated pulsar wind nebula

INTEGRAL observations of PSR J1811?1925 and its associated pulsar wind nebula
INTEGRAL observations of PSR J1811?1925 and its associated pulsar wind nebula
We present spectral measurements made in the soft (20–100 keV) ?-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 10 keV. The IBIS spectrum is best fitted by a power law having photon index ?= 1.8+0.4?0.3 and a 20–100 keV 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 ?-ray emission while broadband (1–200 keV) 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 ?-ray spectrum indicates that the pulsar provides around half of the emission seen in the soft ?-ray domain; its spectrum is hard with no sign of a cut off up to at least 80 keV. The other half of the emission above 10 keV comes from the pulsar wind nebula; with a ?= 1.7 its spectrum is softer than that of the pulsar. From the IBIS/ISGRI mosaics we are able to derive 2? upper limits for the 20–100 keV 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.
pulsars: individual: PSR J1811?1925, supernovae: individual: G11.2-0.3, ?-rays: observations
1745-3933
L29-L33
Dean, A.J.
2f9093f2-855c-4769-b1aa-6dd621b5dcf1
De Rosa, A.
b2a68e71-5c23-4649-94f0-1d8ffd40bb77
McBride, V.A.
a4608811-5a3f-4218-ada0-28f57ec2a0fd
Landi, R.
b8243478-d7a1-4774-8a66-4158a65a33d3
Hill, A.B.
b1007941-b5b1-47cd-8476-7c6b9c57f347
Bassani, L.
07e5602c-f97e-4334-a0fa-c2212431a61a
Bazzano, A.
8eef0c6e-1a5f-4bcd-a034-9a5c3b29104d
Bird, A.J.
045ee141-4720-46fd-a412-5aa848a91b32
Ubertini, P.
7035748e-152c-473e-8766-a2fa3ac49fcb
Dean, A.J.
2f9093f2-855c-4769-b1aa-6dd621b5dcf1
De Rosa, A.
b2a68e71-5c23-4649-94f0-1d8ffd40bb77
McBride, V.A.
a4608811-5a3f-4218-ada0-28f57ec2a0fd
Landi, R.
b8243478-d7a1-4774-8a66-4158a65a33d3
Hill, A.B.
b1007941-b5b1-47cd-8476-7c6b9c57f347
Bassani, L.
07e5602c-f97e-4334-a0fa-c2212431a61a
Bazzano, A.
8eef0c6e-1a5f-4bcd-a034-9a5c3b29104d
Bird, A.J.
045ee141-4720-46fd-a412-5aa848a91b32
Ubertini, P.
7035748e-152c-473e-8766-a2fa3ac49fcb

Dean, A.J., De Rosa, A., McBride, V.A., Landi, R., Hill, A.B., Bassani, L., Bazzano, A., Bird, A.J. and Ubertini, P. (2008) INTEGRAL observations of PSR J1811?1925 and its associated pulsar wind nebula. Monthly Notices of the Royal Astronomical Society: Letters, 384 (1), L29-L33. (doi:10.1111/j.1745-3933.2007.00415.x).

Record type: Article

Abstract

We present spectral measurements made in the soft (20–100 keV) ?-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 10 keV. The IBIS spectrum is best fitted by a power law having photon index ?= 1.8+0.4?0.3 and a 20–100 keV 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 ?-ray emission while broadband (1–200 keV) 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 ?-ray spectrum indicates that the pulsar provides around half of the emission seen in the soft ?-ray domain; its spectrum is hard with no sign of a cut off up to at least 80 keV. The other half of the emission above 10 keV comes from the pulsar wind nebula; with a ?= 1.7 its spectrum is softer than that of the pulsar. From the IBIS/ISGRI mosaics we are able to derive 2? upper limits for the 20–100 keV 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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More information

Published date: February 2008
Keywords: pulsars: individual: PSR J1811?1925, supernovae: individual: G11.2-0.3, ?-rays: observations

Identifiers

Local EPrints ID: 144823
URI: http://eprints.soton.ac.uk/id/eprint/144823
ISSN: 1745-3933
PURE UUID: ca94ff37-a3e0-4ac2-9462-4fefe264d649
ORCID for A.B. Hill: ORCID iD orcid.org/0000-0003-3470-4834
ORCID for A.J. Bird: ORCID iD orcid.org/0000-0002-6888-8937

Catalogue record

Date deposited: 24 May 2010 11:14
Last modified: 09 Nov 2021 03:08

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Contributors

Author: A.J. Dean
Author: A. De Rosa
Author: V.A. McBride
Author: R. Landi
Author: A.B. Hill ORCID iD
Author: L. Bassani
Author: A. Bazzano
Author: A.J. Bird ORCID iD
Author: P. Ubertini

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