English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We present spectral measurements made in the soft (20–100 keV) 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 10 keV. The IBIS spectrum is best fitted by a power law having photon index  Γ= 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 γ‐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 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 80 keV. The other half of the emission above 10 keV 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 20–100 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.

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