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We report on an {\it XMM-Newton} observation of the supernova remnant (SNR)\object{DEM L241} in the Large Magellanic Cloud. In the soft band image, theemission shows an elongated structure, like a killifish, with a central compactsource. The compact source is point-like, and named as XMMU J053559.3$-$673509.The source spectrum is well reproduced with a power-law model with a photonindex of $\Gamma = 1.57$ (1.51--1.62) and the intrinsic luminosity is$2.2\times 10^{35} \mathrm{ergs s^{-1}}$ in the 0.5--10.0 keV band, with theassumed distance of 50 kpc. The source has neither significant coherentpulsations in $2.0\times 10^{-3}$ Hz--8.0 Hz, nor time variabilities. Itsluminosity and spectrum suggest that the source might be a pulsar wind nebula(PWN) in DEM L241. The spectral feature classifies this source into ratherbright and hard PWN, which is similar to those in Kes 75 and B0540$-$693. Theelongated diffuse structure can be divided into a ``Head'' and ``Tail'', andboth have soft and line-rich spectra. Their spectra are well reproduced by aplane-parallel shock plasma ({\it vpshock}) model with a temperature of0.3--0.4 keV and over-abundance in O and Ne and a relative under-abundance inFe. Such an abundance pattern and the morphology imply that the emission isfrom the ejecta of the SNR, and that the progenitor of DEM L241 is a verymassive star, more than 20 M\sun. This result is also supported by theexistence of the central point source and an OB star association, LH 88. Thetotal thermal energy and plasma mass are $\sim 4\times 10^{50}$ ergs and $\sim200$ M\sun, respectively.

A detailed observation of a LMC supernova remnant DEM L241 withXMM-Newton