  G15.9+0.2 is a Galactic shell-type supernova remnant (SNR), which was
detected in radio and has been confirmed in X-rays based on Chandra
observations. An X-ray point source CXOUJ181852.0-150213 has been detected and
suggested to be an associated neutron star. In a recent study, we have
confirmed the source to be a central compact object (CCO). We have studied the
SNR using high-resolution X-ray data taken with Chandra in combination with
infrared (IR) data in order to understand its emission and to derive its
physical parameters. This will also help to constrain, e.g., the age of the CCO
and the environment in which it was born. The spectral analysis of the X-ray
emission using the new Chandra data and the comparison to the IR data have
shown that the SNR is relatively young with an age of a few thousand years and
that its emission is dominated by that of shocked interstellar medium (ISM).
However, the analysis of the spectrum of the bright eastern shell shows that
there is an additional emission component with enhanced abundances of {\alpha}
elements and Fe, suggesting ejecta emission. The multi-wavelength emission is
consistent with SNR G15.9+0.2 expanding in an ISM with a density gradient,
while there is also colder material located in front of the SNR, which absorbs
its thermal X-ray emission in the softer bands.
