We detected X-ray emission from PSR B1800-21 (J1803-2137) and its synchrotron nebula with the Chandra X-Ray Observatory. The observed pulsar flux is(1.4 ± 0.2)× 10-14 ergs cm-2 s-1 in the 1-6 keV band. The spectrum can be described by a two-component power law + blackbody (PL + BB) model, suggesting a mixture of thermal and magneto-spheric emission. For a plausible nH = 1.4 × 10 22 cm-2 , the PL component has a slope T = 1.4 ± 0.6 and a luminosity LPSRnonth = 4 × 10 31(d/4 kpc)2 ergs s-1. The properties of the thermal component (kT = 0.1-0.3 keV, LPSRbol = 10 31-1033 ergs s-1) are very poorly constrained because of the strong interstellar absorption. The compact, 7″ × 4″, inner pulsar wind nebula (PWN), elongated perpendicular to the pulsar's proper motion, is immersed in a fainter asymmetric emission. The observed flux of the PWN is (5.5 ± 0.6) × 10-14 ergs cm-2 s-1 in the 1-8 keV band. The PWN spectrum fits a PL model with T = 1.6 ± 0.3, LPWN = 1.6 × 10 32(d/4 kpc)2 ergs s-1. The shape of the inner PWN suggests that the pulsar moves subsonically and X-ray emission emerges from a torus associated with the termination shock in the equatorial pulsar wind. The inferred PWN-pulsar properties (e.g., the PWN X-ray efficiency, L PWN/Ė ∼ 10-4; the luminosity ratio, L PWN/LPSRnonth = 4; the pulsar wind pressure at the termination shock, Ps = 10-9 ergs cm-3) are very similar to those of other subsonically moving Vela-like objects detected with Chandra (LPWN/Ė ∼ 10-4.5 to 103.5 LPWN//LPSRnonth ∼ 5, ps = 10-10 to 10-8 ergs cm-1).
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science