A Chandra Observation of the Vela-like Pulsar PSR B1823-13 and Its TeV Pulsar Wind Nebula

Details A Chandra Observation of the Vela-like Pulsar PSR B1823-13 and Its TeV Pulsar Wind Nebula A Chandra Observation of the Vela-like Pulsar PSR B1823-13 and Its TeV Pulsar Wind Nebula

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006head....9.0120g&link_type=abstract

American Astronomical Society, HEAD meeting #9, #1.20; Bulletin of the American Astronomical Society, Vol. 38, p.332

Astronomy and Astrophysics

Astronomy

1

Scientific paper

We present results obtained from a Chandra observation of the Vela-like pulsar PSR B1823-13 and its pulsar wind nebula (PWN). Recent HESS observations of the pulsar suggest an association between its PWN and the bright TeV source HESS J1825-137. The association is proposed based on matching the g-ray size and spectrum to those of the X-ray PWN derived using an XMM-Newton observation. However, our analysis of the Chandra data suggests the XMM-Newton results were contaminated by nearby point sources, over-estimating the size and giving a steeper spectrum for the PWN. Using Chandra, the nebula is seen to contain a bright core 8"x4" in size embedded within a compact region 32"x16". Extended emission can be seen out to 4' from the pulsar and appears to be concentrated to the south-west rather than symmetrically south of the pulsar position. Based on the size of the core region we find a revised estimate for the wind termination shock radius of Rs < 4". Spectral steepening within the nebula is seen with power-law photon indices increasing from 1.3-2.1. The revised PWN characteristics presented here have important implications for our understanding of the TeV emission mechanism.

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