  Aims: IKT 16 is an X-ray and radio-faint supernova remnant (SNR) in the Small
Magellanic Cloud (SMC). A detailed X-ray study of this SNR with XMM-Newton
confirmed the presence of a hard X-ray source near its centre, indicating the
detection of the first composite SNR in the SMC. With a dedicated Chandra
observation we aim to resolve the point source and confirm its nature. We also
acquire new ATCA observations of the source at 2.1 GHz with improved flux
density estimates and resolution.
  Methods: We perform detailed spatial and spectral analysis of the source.
With the highest resolution X-ray and radio image of the centre of the SNR
available today, we resolve the source and confirm its pulsar wind nebula (PWN)
nature. Further, we constrain the geometrical parameters of the PWN and perform
spectral analysis for the point source and the PWN separately. We also test for
the radial variations of the PWN spectrum and its possible east west asymmetry.
  Results: The X-ray source at the centre of IKT 16 can be resolved into a
symmetrical elongated feature centering a point source, the putative pulsar.
Spatial modeling indicates an extent of 5.2 arcsec of the feature with its axis
inclined at 82 degree east from north, aligned with a larger radio feature
consisting of two lobes almost symmetrical about the X-ray source. The picture
is consistent with a PWN which has not yet collided with the reverse shock. The
point source is about three times brighter than the PWN and has a hard spectrum
of spectral index 1.1 compared to a value 2.2 for the PWN. This points to the
presence of a pulsar dominated by non-thermal emission. The expected E_{dot} is
~ 10^37 erg s^-1 and spin period < 100 ms. However, the presence of a compact
nebula unresolved by Chandra at the distance of the SMC cannot completely be
ruled out.
