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Title:
Influence of the Neutron Star 1E 161348-5055 in RCW 103 on the Surrounding Medium
Authors:
Reynoso, E. M.; Green, A. J.; Johnston, S.; Goss, W. M.; Dubner, G. M.; Giacani, E. B.
Affiliation:
AA(School of Physics, University of Sydney, Sydney NSW 2006, Australia. Instituto de Astronomía y Física del Espacio, CC 67, Suc 28, 1428 Buenos Aires, Argentina. Author to whom correspondence should be addressed (e-mail: ereynoso@iafe.uba.ar); ), AB(School of Physics, University of Sydney, Sydney NSW 2006, Australia.), AC(School of Physics, University of Sydney, Sydney NSW 2006, Australia.), AD(National Radio Astronomy Observatory, P. O. Box 0, Socorro, NM 87801, USA.), AE(Instituto de Astronomía y Física del Espacio, CC 67, Suc 28, 1428 Buenos Aires, Argentina. Member of the Carrera del Investigador Cientí fico, CONICET, Argentina.), AF(Instituto de Astronomía y Física del Espacio, CC 67, Suc 28, 1428 Buenos Aires, Argentina. Member of the Carrera del Investigador Cientí fico, CONICET, Argentina.)
Publication:
Publications of the Astronomical Society of Australia, Volume 21, Issue 1, pp. 82-88. (PASA Homepage)
Publication Date:
00/2004
Origin:
PASA
Keywords:
stars: neutron, supernova remnants, ISM: individual: RCW 103, X-rays: individual: 1E 161348-5055, spectral lines: neutral hydrogen.
DOI:
10.1071/AS03053
Bibliographic Code:
2004PASA...21...82R

Abstract

We have carried out a study of the neutral hydrogen in the direction of the X-ray source 1E 161348-5055, a compact central object (CCO) located in the interior of the supernova remnant (SNR) RCW 103. The HI 21cm line observations were carried out using the Australia Telescope Compact Array, complemented with single dish data from the Parkes radio telescope to recover information at all spatial scales. We derive a distance to RCW 103 of 3.1kpc, in agreement with previous distance measurements. We have also detected a small hole in the HI emission which is positionally and kinematically coincident with the location of the CCO which confirms the association between the SNR and the CCO. This is the third case of a depression in HI emission seemingly associated with CCOs in SNRs. The characteristic parameters of the holes such as their size, eccentricity and evacuated mass are similar in all three cases. We estimate the absorbing HI column density towards 1E 161348-5055 to be ~6×1021cm-2, a value compatible with a blackbody solution for the CCO X-ray emission. However, the implied temperature and luminosity are very high compared to most neutron stars. Moreover, the strong long-term variability in X-rays favours the hypothesis that 1E 161348-5055 is an accreting binary source rather than an isolated, cooling neutron star. An analysis of the continuum image obtained at 1.4GHz from these observations shows no trace of a pulsar wind nebula around 1E 161348-5055, in spite of it being a young object.
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