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Searching for Compact Objects in Supernova Remnants: Initial Results

Published online by Cambridge University Press:  19 July 2016

D. L. Kaplan ,
S. R. Kulkarni ,
D. A. Frail ,
B. M. Gaensler ,
P. O. Slane  and
E. V. Gotthelf
D. L. Kaplan
Affiliation:
Department of Astronomy, 105-24 California Institute of Technology, Pasadena, CA 91125, USA
S. R. Kulkarni
Affiliation:
Department of Astronomy, 105-24 California Institute of Technology, Pasadena, CA 91125, USA
D. A. Frail
Affiliation:
National Radio Astronomy Observatory, P.O. Box O, Socorro, NM 87801, USA
B. M. Gaensler
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-6, Cambridge, MA 02138, USA
P. O. Slane
Affiliation:
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS-6, Cambridge, MA 02138, USA
E. V. Gotthelf
Affiliation:
Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USA

Abstract

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Most astronomers now accept that stars more massive than about 9 M⊙ explode as supernovae and leave stellar remnants, either neutron stars or black holes. However, less than half of the SNRs within 5 kpc have identified central sources. Here, we discuss a systematic effort to search for compact central sources in the remaining 23 SNRs of this distance-limited sample. As the first part of this survey, we are able to state with some confidence that there are no associated central sources down to a level of one tenth of that of the Cas A central source, LX ≲ 1031 ergs s−1, in four SNRs (G093.3+6.9, G315.4−2.3, G084.2+0.8, and G127.1+0.5). We compare our limits with cooling curves for neutron stars and find that any putative neutron stars in these SNRs must be cooling faster than expected for traditional 1.35 M⊙ neutron stars.

Type
Part 3: Pulsars: Surveys and Galactic Distribution
Information
Symposium - International Astronomical Union , Volume 218: Young Neutrons Stars and their Environments , 2004 , pp. 123 - 126
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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