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Title:
The nature of the compact X-ray source in the supernova remnant G27.4+0.0
Authors:
Helfand, David J.; Becker, R. H.; Hawkins, G.; White, R. L.
Affiliation:
AA(Columbia University, New York, NY, US), AB(Columbia University, New York, NY, US), AC(Lawrence Livermore National Laboratory, Livermore, CA, US), AD(Lawrence Livermore National Laboratory, Livermore, CA, US)
Publication:
Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 434, no. 2, p. 627-634 (ApJ Homepage)
Publication Date:
10/1994
Category:
Astronomy
Origin:
STI
NASA/STI Keywords:
ASTRONOMICAL MODELS, NEUTRON STARS, RADIO SOURCES (ASTRONOMY), SUPERNOVA REMNANTS, X RAY ASTRONOMY, X RAY BINARIES, X RAY SPECTRA, HEAO 2, ROSAT MISSION, STELLAR WINDS, VERY LARGE ARRAY (VLA), X RAY IMAGERY
DOI:
10.1086/174764
Bibliographic Code:
1994ApJ...434..627H

Abstract

High-resolution X-ray imaging data obtained with ROSAT is used to constrain the nature of the central compact source in the supernova remnant G27.4+0.0. Diffuse emission is seen from throughout the approximately 4 min diameter radio shell, while the central source remains unresolved at approximately 3 sec. We combine archival data from the Einstein HRI, IPC, and MPC with the ROSAT HRI data to define the X-ray spectra of the diffuse and point-like emission. The bulk of the shell radiation is consistent with that of a approximately 107 K plasma, although a higher temperature component is also suggested by the data; coupled with the remnant's size and distance, we derive an age of between 500 and 2500 yr. The point source has a substantially harder spectrum, with a power-law photon index less than or approximately equal to 1. A search for periodic modulation from the point source yields upper limits ranging from 10%-35% for periods between 0.025 and 1000 s, depending on the assumed pulse shape. No aperiodic variability on timescales of from 103 to 108 s is required, although a factor of approximately 2 change between the Einstein and ROSAT eras is possible. We show that the point source cannot represent thermal emission from the surface of a young neutron star and is unlikely to be explained as nonthermal, Crab-like X-ray pulses or a small synchrotron nebula. The most likely models involve accretion-powered systems -- either a wind-fed neutron star with a massive companion or a low-mass X-ray binary. In all probability, this is the youngest X-ray binary in the Galaxy.

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