Chandra and XMM-Newton Observations of the Vela-like Pulsar B1046-58

Details Chandra and XMM-Newton Observations of the Vela-like Pulsar B1046-58 Chandra and XMM-Newton Observations of the Vela-like Pulsar B1046-58

2006-10-17

arxiv.org/abs/astro-ph/0610523v2

Astrophys.J.652:569-575,2006

Astronomy and Astrophysics

Astrophysics

8 pages, 4 figures. Accepted to ApJ

Scientific paper

10.1086/507125

We present results from Chandra and XMM-Newton observations of the radio pulsar B1046-58. A high-resolution spatial analysis reveals an asymmetric pulsar wind nebula (PWN) ~6"x11" in size. The combined emission from the pulsar and its PWN is faint, with a best-fit power-law photon index of $\Gamma$=1.7 and unabsorbed luminosity of ~10^32 ergs/s in the 0.5-10.0 keV range (assuming a distance of 2.7 kpc). A spatially resolved imaging analysis suggests the presence of softer emission from the pulsar. No pulsations are detected from PSR B1046-58; assuming a worst-case sinusoidal pulse profile, we derive a 3$\sigma$ upper limit for the pulsed fraction in the 0.5-10.0 keV range of 53%. Extended PWN emission is seen within 2" of the pulsar; the additional structures are highly asymmetric and extend predominantly to the south-east. We discuss the emission from the PWN as resulting from material downstream of the wind termination shock, as outflow from the pulsar or as structures confined by a high space velocity. The first two interpretations imply equipartition fields in the observed structures of ~40-100 uG, while the latter case implies a velocity for the pulsar of ~ 190 n^-1/2 km/s (where n is the ambient number density in units of cm^-3). No emission from an associated supernova remnant is detected.

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