Three XMM-Newton observations of the Anomalous X-ray Pulsar 1E 1048.1-5937: long term variations in spectrum and pulsed fraction

Details Three XMM-Newton observations of the Anomalous X-ray Pulsar 1E 1048.1-5937: long term variations in spectrum and pulsed fraction Three XMM-Newton observations of the Anomalous X-ray Pulsar 1E 1048.1-5937: long term variations in spectrum and pulsed fraction

2005-03-17

arxiv.org/abs/astro-ph/0503390v1

Astronomy and Astrophysics

Astrophysics

10 pages, 6 figures; accepted for publication in A&A

Scientific paper

10.1051/0004-6361:20052633

We report the results of a recent (July 2004) XMM-Newton Target of Opportunity observation of the Anomalous X-ray pulsar 1E 1048.1-5937, together with a detailed re-analysis of previous observations carried out in 2000 and 2003. In July 2004 the source had a 2-10 keV flux of 6.2$\times10^{-12}$ erg cm$^{-2}$ s$^{-1}$ and a pulsed fraction P$_F$=0.68. The comparison of the three data sets shows the presence of an anti-correlation between flux and pulsed fraction, implying that previous estimates of the source energetics based on the assumption of a large and constant pulsed fraction might be significantly underestimated. The source spectrum is well described by a power law plus blackbody model (kT~0.63 keV, photon index $\Gamma$~2.7-3.5) or, alternatively, by the sum of two blackbodies of which the hotter is Comptonized by relativistic electrons. In this case the temperatures are kT${_1}$~0.2-0.3 keV and kT${_2}$~0.4-0.5 keV and the emitting area of the cooler component is consistent with the whole neutron star surface. The long term luminosity variation of a factor >~2 is accompanied by relatively small variations in the spectral shape. Phase resolved spectroscopy indicates a harder spectrum in correspondence of the pulse maximum. No spectral features have been detected with 4$\sigma$ limits on the equivalent width in the range ~10-220 eV, depending on line energy and width.

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