Candidate supernova remnants (SNRs) G23.5+0.1 and G25.5+0.0 were observed by XMM-Newton in the course of a snapshot survey of plerionic and composite SNRs in the Galactic plane. In the field of G23.5+0.1, we detected an extended source, 3′ in diameter, which we tentatively interpret as a pulsar wind nebula (PWN) of the middle-aged radio pulsar B1830-08 (J1833-0827; P = 85.3ms, τ = 147kyr, = 5.8 × 1035ergs-1, d = 5.7kpc), with the PWN luminosity L 0.2-10 keV 5 × 10 33ergs-1 8 × 10-3 . The pulsar is not resolved in the EPIC images. Our analysis suggests an association between PSR B1830-08 and the surrounding diffuse radio emission. If the radio emission is due to the SNR, then the pulsar must be significantly younger than its characteristic age. Alternatively, the radio emission may come from a relic PWN. The field also contains SGR 1833-0832 and another middle-aged pulsar B1829-08 (J1832-0827; P = 647ms, τ = 161kyr, = 9.3 × 1033ergs -1, d = 4.7kpc), none of which are detected in our observation. In the field of G25.5+0.0, which contains the extended TeV source HESS J1837-069, we detected the recently discovered young high-energy pulsar J1838-0655 (P = 70.5ms, τ = 23kyr, 5.5× 1036ergs-1) embedded in a PWN with extent of 13. The unabsorbed pulsar+PWN luminosity is L 2-11 keV 2 × 1034ergs-1 4 × 10 -3 at an assumed distance of 7kpc. We also detected another PWN candidate (AX J1837.3-0652) with an extent of 2′ and unabsorbed luminosity L 2-10 keV 4 × 1033ergs-1 at d = 7kpc. The third X-ray source, located within the extent of the HESS J1837-069, has a peculiar extended radio counterpart, possibly a radio galaxy with a double nucleus or a microquasar. We did not find any evidence of the SNR emission in the G25.5+0.0 field. We provide detailed multiwavelength analysis and identifications of other field sources and discuss robustness of the G25.5+0.0 and G23.5+0.1 classifications as SNRs.
All Science Journal Classification (ASJC) codes
- Astronomy and Astrophysics
- Space and Planetary Science