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Title:
Observations of 20 Millisecond Pulsars in 47 Tucanae at 20 Centimeters
Authors:
Camilo, F.; Lorimer, D. R.; Freire, P.; Lyne, A. G.; Manchester, R. N.
Affiliation:
AA(University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire, SK11 9DL, UK.; Marie Curie Fellow. E-mail: . Present address: Columbia Astrophysics Laboratory, 550 West 120th Street, New York, NY 10027), AB(Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121, Bonn, Germany.; Present address: NAIC, Arecibo Observatory, HC3 Box 53995, Arecibo, PR 00613), AC(University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire, SK11 9DL, UK), AD(University of Manchester, Jodrell Bank Observatory, Macclesfield, Cheshire, SK11 9DL, UK), AE(Australia Telescope National Facility, CSIRO, P.O. Box 76, Epping, NSW 1710, Australia)
Publication:
The Astrophysical Journal, Volume 535, Issue 2, pp. 975-990. (ApJ Homepage)
Publication Date:
06/2000
Origin:
UCP
ApJ Keywords:
Stars: Binaries: Eclipsing, Stars: Binaries: General, Galaxy: Globular Clusters: Individual: Name: 47 Tucanae, Stars: Pulsars: General, Radio Continuum: Stars
DOI:
10.1086/308859
Bibliographic Code:
2000ApJ...535..975C

Abstract

We have used a new observing system on the Parkes radio telescope to carry out a series of pulsar observations of the globular cluster 47 Tucanae at 20 cm wavelength. We detected all 11 previously known pulsars and have discovered nine others, all of which are millisecond pulsars in binary systems. We have searched the data for relatively short orbital period systems, and found one pulsar with an orbital period of 96 minutes, the shortest of any known radio pulsar. The increased rate of detections with the new system resulted in improved estimates of the flux density of the previously known pulsars, determination of the orbital parameters of one of them, and a coherent timing solution for another one. Five of the pulsars now known in 47 Tucanae have orbital periods of a few hours and implied companion masses of only ~0.03 Msolar. Two of these are eclipsed at some orbital phases, while three are seen at all phases at 20 cm but not always at lower frequencies. Four and possibly six of the other binary systems have longer orbital periods and companion masses ~0.2 Msolar, with at least two of them having relatively large orbital eccentricities. All 20 pulsars have rotation periods in the range 2-8 ms.
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