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    Broadband pulsations from PSR B1821-24: Implications for emission models and the pulsar population of M28

    Access Status
    Open access via publisher
    Authors
    Johnson, T.
    Guillemot, L.
    Kerr, M.
    Cognard, I.
    Ray, P.
    Wolff, M.
    Bégin, S.
    Janssen, G.
    Romani, R.
    Venter, C.
    Grove, J.
    Freire, P.
    Wood, M.
    Cheung, C.
    Casandjian, J.
    Stairs, I.
    Camilo, F.
    Espinoza, C.
    Ferrara, E.
    Harding, A.
    Johnston, S.
    Kramer, M.
    Lyne, A.
    Michelson, P.
    Ransom, S.
    Shannon, Ryan
    Smith, D.
    Stappers, B.
    Theureau, G.
    Thorsett, S.
    Date
    2013
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Johnson, T. and Guillemot, L. and Kerr, M. and Cognard, I. and Ray, P. and Wolff, M. and Bégin, S. et al. 2013. Broadband pulsations from PSR B1821-24: Implications for emission models and the pulsar population of M28. Astrophysical Journal. 778 (2).
    Source Title
    Astrophysical Journal
    DOI
    10.1088/0004-637X/778/2/106
    ISSN
    0004-637X
    School
    Curtin Institute of Radio Astronomy (Physics)
    URI
    http://hdl.handle.net/20.500.11937/26206
    Collection
    • Curtin Research Publications
    Abstract

    We report a 5.4δ detection of pulsed gamma rays from PSR B1821-24 in the globular cluster M28 using ~44 months of Fermi Large Area Telescope (LAT) data that have been reprocessed with improved instrument calibration constants. We constructed a phase-coherent ephemeris, with post-fit residual rms of 3 µs, using radio data spanning ~23.2 yr, enabling measurements of the multi-wavelength light-curve properties of PSR B1821-24 at the milliperiod level. We fold RXTE observations of PSR B1821-24 from 1996 to 2007 and discuss implications on the emission zones. The gamma-ray light curve consists of two peaks separated by 0.41 ± 0.02 in phase, with the first gamma-ray peak lagging behind the first radio peak by 0.05 ± 0.02 in phase, consistent with the phase of giant radio pulses. We observe significant emission in the off-peak interval of PSR B1821-24 with a best-fit LAT position inconsistent with the core of M28. We do not detect significant gamma-ray pulsations at the spin or orbital periods from any other known pulsar in M28, and we place limits on the number of energetic pulsars in the cluster. The derived gamma-ray efficiency, ~2%, is typical of other gamma-ray pulsars with comparable spin-down power, suggesting that the measured spin-down rate (2.2 × 1036 erg s-1) is not appreciably distorted by acceleration in the cluster potential. This confirms PSR B1821-24 as the second very energetic millisecond pulsar in a globular cluster and raises the question of whether these represent a separate class of objects that only form in regions of very high stellar density.

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