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X-ray Images of PKS1209-52 and its Central Compact X-ray Source

Published online by Cambridge University Press:  12 April 2016

Yutaka Matsui ,
Knox S. Long  and
Ian R. Tuohy
Yutaka Matsui
Affiliation:
Dept. of Physics & Astronomy, Northwestern Univ., Evanston, IL 60201, USA., Evanston, IL 60201
Knox S. Long
Affiliation:
Center for Astrophysical Sciences, Johns Hopkins Univ., Baltimore, MD 21218, USA
Ian R. Tuohy
Affiliation:
Mount Stromlo and Siding Spring Observatories, Australian National Univ., ACT 2606, Canberra, Australia

Abstract

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A complete X-ray image of the SNR PKS1209-52 (= G296.5+10.0) was obtained with the IPC and HRI on the Einstein Observatory. The remnant has a shell-like X-ray morphology much like its appearance at radio wavelengths, while a compact X-ray source is clearly detected near the center of the remnant. The flux observed from the X-ray nebula F(0.1−4.5 keV) is 8 × 10−11 ergs cm−2 s−1, which corresponds to a luminosity L(0.1−4.5 keV) = 8 × 1035 ergs s−1 for a distance of 2 kpc. Applying a simple shell model to the X-ray emission distribution, we derived an ambient interstellar medium nO = 0.08 H atoms cm−3, total X-ray emitting plasma mass 150 M⊙, and thermal energy 1.2 × 1050 ergs. The flux from the compact X-ray source F(0.15−4.5 keV) is ~2 × 10−12 ergs cm−2 s−1. There are no obvious optical counterparts brighter than mv ~ 22 within the 3.3″ radius HRI error circle. If the object is a hot neutron star, the HRI/IPC count rate ratio implies a surface temperature of 1.6 × 106 K for NH = 3.2 × 1021 cm−2.

Type
Research Article
Information
International Astronomical Union Colloquium , Volume 101: Supernova Remnants and the Interstellar Medium , 1988 , pp. 157 - 160
Copyright
Copyright © Cambridge University Press 1988

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