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We present X-ray observations of pulsar wind nebula (PWN) G16.73+0.08/supernova remnant (SNR) G16.7+0.1 using archival data of Chandra ACIS. The X-ray emission peak location of this PWN is found to be offset by 24 arcsec from the centre of the 1.4-GHz emission of this nebula. The X-ray nebula is elongated in the direction from the X-ray peak to the 1.4-GHz emission centre. This offset suggests that G16.73+0.08 is an evolved PWNinteractingwith the SNR reverse shock.We identify a point source, CXO J182058.16 - 142001.5, near the location of the X-ray peak. The spectrum of the X-ray nebula can be described by an absorbed power law of photon index 0.98+0.79-0.71 and hydrogen column density NH = 4.99+2.75-2.28 x 1022 cm-2. CXO J182058.16 - 142001.5 is likely a pulsar. We estimate its spin-down power to be about 2.6 x 1036 erg s-1. Assuming its age at 3000 and 10 000 yr, its dipole magnetic field strength at the polar surface is estimated to be about 4.2 x 1013 and 1.3 x 1013 G, respectively. [ABSTRACT FROM AUTHOR]

We analyse the Suzaku X-ray Imaging Spectrometer data of the central region of supernova remnant G332.5-5.6. The X-ray data are well described by a single non-equilibrium ionization thermal model, vnei, with an absorbing hydrogen column density of 1.4+0.4-0.1 × 1021 cm-2. The plasma is characterized by an electron temperature of 0.49+0.08-0.06 keV with subsolar abundances for O (0.58+0.06-0.05 solar value) and Fe (0.72+0.06-0.05 solar value) and slightly overabundance for Mg (1.23+0.14-0.14 solar value). It seems that the central X-ray emission originates from a projection effect or evaporation of residual clouds inside G332.5-5.6. We estimate a distance of 3.0 ± 0.8 kpc for G332.5-5.6 based on the extinction-distance relation. G332.5-5.6 has an age of 7-9 kyr. [ABSTRACT FROM AUTHOR]