  Aims: We present a detailed X-ray study of the recently discovered supernova
remnant (SNR) G53.41+0.03 that follows up and further expands on the previous,
limited analysis of archival data covering a small portion of the SNR. Methods:
With the new dedicated 70ks XMM-Newton observation we investigate the
morphological structure of the SNR in X-rays, search for a presence of a young
neutron star and characterise the plasma conditions in the selected regions by
means of spectral fitting. Results: The first full view of SNR G53.41+0.03
shows an X-ray emission region well aligned with the reported half-shell radio
morphology. We find three distinct regions of the remnant that vary in
brightness and hardness of the spectra, and are all best characterised by a hot
plasma model in a non-equilibrium ionisation state. Of the three regions, the
brightest one contains the most mature plasma, with ionisation age $\tau
\approx 4\times10^{10}$s cm$^{-3}$ (where $\tau = n_e t$), a lower electron
temperature of kT$_\mathrm{e} \approx 1$ keV and the highest estimated gas
density of n$_\mathrm{H}\approx 0.87$ cm$^{-3}$. The second, fainter but
spectrally harder, region reveals a younger plasma ($\tau \approx
1.7\times10^{10}$s cm$^{-3}$) with higher temperature (kT$_\mathrm{e} \approx
2$ keV) and two to three times lower density (n$_\mathrm{H}\approx 0.34$
cm$^{-3}$). The third region is very faint, but we identify spectroscopically
the presence of a hot plasma.Employing several methods for age estimation, we
find the remnant to be $t \approx 1000-5000$ yrs old, confirming the earlier
reports of a relatively young age. The environment of the remnant also contains
a number of point sources, of which most are expected to be positioned in the
foreground. Of the two point sources in the geometrical centre of the remnant
one is consistent with the characteristics of a young neutron star.
