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    On detecting millisecond pulsars at the galactic center

    231376_231376.pdf (626.9Kb)
    Access Status
    Open access
    Authors
    Macquart, Jean-Pierre
    Kanekar, N.
    Date
    2015
    Type
    Journal Article
    
    Metadata
    Show full item record
    Citation
    Macquart, J. and Kanekar, N. 2015. On detecting millisecond pulsars at the galactic center. Astrophysical Journal. 805 (2): Article ID 172.
    Source Title
    Astrophysical Journal
    DOI
    10.1088/0004-637X/805/2/172
    ISSN
    0004-637X
    School
    Curtin Institute of Radio Astronomy (Physics)
    Remarks

    This is an author-created, un-copy edited version of an article accepted for publication in Astrophysical Journal. The publisher is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at http://doi.org/10.1088/0004-637X/805/2/172

    URI
    http://hdl.handle.net/20.500.11937/4944
    Collection
    • Curtin Research Publications
    Abstract

    The lack of detected pulsars at the Galactic Center (GC) region is a long-standing mystery. We argue that the high stellar density in the central parsec around the GC is likely to result in a pulsar population dominated by millisecond pulsars (MSPs), similar to the situation in globular cluster environments. Earlier GC pulsar searches have been largely insensitive to such an MSP population, accounting for the lack of pulsar detections. We estimate the best search frequency for such an MSP population with present and upcoming broad-band radio telescopes for two possible scattering scenarios, the “weak-scattering” case suggested by the recent detection of a magnetar close to the GC, and the “strong-scattering” case, with the scattering screen located close to the GC. The optimal search frequencies are ≈ 8 GHz ( weak-scattering ) and ≈ 25 GHz ( strong-scattering ) , for pulsars with periods 1 – 20 ms, assuming that GC pulsars have a luminosity distribution similar to that those in the rest of the Milky Way. We find that 10 – 30 hr integrations with the Very Large Array and the Green Bank Telescope would be sufficient to detect MSPs at the GC distance in the weak-scattering case. However, if the strong-scattering case is indeed applicable to the GC, observations with the full Square Kilometre Array would be needed to detect the putative MSP population.

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