SIMBAD references

2006A&A...450..585B - Astronomy and Astrophysics, volume 450, 585-591 (2006/5-1)

A detailed observation of a LMC supernova remnant DEM L241 with XMM-Newton.

BAMBA A., UENO M., NAKAJIMA H., MORI K. and KOYAMA K.

Abstract (from CDS):

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 XMMU J053559.3-673509. The source spectrum is reproduced well by a power-law model with a photon index of Γ=1.57 (1.51-1.62); and the intrinsic luminosity is 2.2x1035erg/s in the 0.5-10.0 keV band, with an assumed distance of 50kpc. The source has neither significant coherent pulsations in 2.0x10–3-8.0Hz 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 as 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 reproduced well by a plane-parallel shock plasma (vpshock) model with a temperature of 0.3-0.4 keV, over-abundance in O and Ne, and a relative under-abundance in Fe. Such an abundance pattern and the morphology imply both that the emission is from the ejecta of the SNR and that the progenitor of DEM L241 is a very massive star, more than 20M. 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 ∼4x1050erg and ∼200M, respectively.

Abstract Copyright:

Journal keyword(s): ISM: supernova remnants - X-rays: individual: DEM L241 - X-rays: individual: XMMU J053559.3-673509

Simbad objects: 15

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2021.03.08-01:32:42

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