An improved technique for the search for optical emission from radio pulsars, and its application to PSR 0301 + 19, 1919 + 21 and 2303 + 30

Details An improved technique for the search for optical emission from radio pulsars, and its application to PSR 0301 + 19, 1919 + 21 and 2303 + 30 An improved technique for the search for optical emission from radio pulsars, and its application to PSR 0301 + 19, 1919 + 21 and 2303 + 30

May 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989a%26a...215..195p&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 215, no. 1, May 1989, p. 195-210.

Astronomy and Astrophysics

Astronomy

4

Faint Objects, Light Emission, Pulsars, Radio Sources (Astronomy), Astrometry, Data Flow Analysis, Quantum Counters, Signal To Noise Ratios, Statistical Analysis

Scientific paper

The theoretical basis and implementation of a technique to identify radio-pulsar optical counterparts are described. The method is based on time-resolved imaging and rigorous statistical analysis; two-dimensional epoch-folding and chi-squared mapping are used to select promising candidates, which are then evaluated with one-dimensional time-series methods. Preliminary results for three long-period pulsars are presented in extensive tables, graphs, and maps, based on observations obtained with the ESA photon-counting detector on the Canada-France-Hawaii Telescope on October 20 and 22, 1984. Optical peaks are detected near the pulsar locations, but also at significant distances, and the optical pulsations persist for only part of the observation period. The need for further observations is indicated.

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