We report on an XMM-Newton observation of the supernova remnant ( SNR ) DEM~L241 in the Large Magellanic Cloud .
In the soft band image , the emission shows an elongated structure , like a killifish , with a central compact source .
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 photon index 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 the assumed distance of 50 kpc .
The source has neither significant coherent pulsations in 2.0 \times 10 ^ { -3 } Hz–8.0 Hz , nor time variabilities .
Its luminosity and spectrum suggest that the source might be a pulsar wind nebula ( PWN ) in DEM L241 .
The spectral feature classifies this source into rather bright and hard PWN , which is similar to those in Kes 75 and B0540 - 693 .
The elongated diffuse structure can be divided into a “ Head ” and “ Tail ” , and both have soft and line-rich spectra .
Their spectra are well reproduced by a plane-parallel shock plasma ( vpshock ) model with a temperature of 0.3–0.4 keV and over-abundance in O and Ne and a relative under-abundance in Fe .
Such an abundance pattern and the morphology imply that the emission is from the ejecta of the SNR , and that the progenitor of DEM L241 is a very massive star , more than 20 M☉ .
This result is also supported by the existence of the central point source and an OB star association , LH 88 .
The total thermal energy and plasma mass are \sim 4 \times 10 ^ { 50 } ergs and \sim 200 M☉ , respectively .