The Crab nebula pulsar was observed in 2009 January and December with a novel very fast optical photon counter, Iqueye, mounted at the ESO 3.5 m New Technology Telescope. Thanks to the exquisite quality of the Iqueye data, we computed accurate phase coherent timing solutions for the two observing runs and over the entire year 2009. Our statistical uncertainty on the determination of the phase of the main pulse and the rotational period of the pulsar for short (a few days) time intervals are ≈ 1 μs and ˜0.5 ps, respectively. Comparison with the Jodrell Bank radio ephemerides shows that the optical pulse leads the radio one by ˜ 240 μs in January and ˜ 160 μs in December, in agreement with a number of other measurements performed after 1996. A third-order polynomial fit adequately describes the spin-down for the 2009 January plus December optical observations. The phase noise is consistent with being Gaussian distributed with a dispersion σ of ≈ 15 μs in most observations, in agreement with theoretical expectations for photon noise-induced phase variability.

Optical phase coherent timing of the Crab nebula pulsar with Iqueye at the ESO New Technology Telescope

BARBIERI, CESARE;NALETTO, GIAMPIERO;VERROI, ENRICO;
2014

Abstract

The Crab nebula pulsar was observed in 2009 January and December with a novel very fast optical photon counter, Iqueye, mounted at the ESO 3.5 m New Technology Telescope. Thanks to the exquisite quality of the Iqueye data, we computed accurate phase coherent timing solutions for the two observing runs and over the entire year 2009. Our statistical uncertainty on the determination of the phase of the main pulse and the rotational period of the pulsar for short (a few days) time intervals are ≈ 1 μs and ˜0.5 ps, respectively. Comparison with the Jodrell Bank radio ephemerides shows that the optical pulse leads the radio one by ˜ 240 μs in January and ˜ 160 μs in December, in agreement with a number of other measurements performed after 1996. A third-order polynomial fit adequately describes the spin-down for the 2009 January plus December optical observations. The phase noise is consistent with being Gaussian distributed with a dispersion σ of ≈ 15 μs in most observations, in agreement with theoretical expectations for photon noise-induced phase variability.
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Utilizza questo identificativo per citare o creare un link a questo documento: http://hdl.handle.net/11577/2808283
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