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Can we see pulsars around Sgr A*? - The latest searches with the Effelsberg telescope

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arxiv 1210.3770 v1 pith:2XZS76I5 submitted 2012-10-14 astro-ph.GA astro-ph.HE

R. P. Eatough , M. Kramer , B. Klein , R. Karuppusamy , D. J. Champion , P. C. C. Freire , N. Wex , K. Liu This is my paper · ORCID
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keywords radioaroundcentreeffelsbergpulsarpulsarsscatteringsearches
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Radio pulsars in relativistic binary systems are unique tools to study the curved space-time around massive compact objects. The discovery of a pulsar closely orbiting the super-massive black hole at the centre of our Galaxy, Sgr A*, would provide a superb test-bed for gravitational physics. To date, the absence of any radio pulsar discoveries within a few arc minutes of Sgr A* has been explained by one principal factor: extreme scattering of radio waves caused by inhomogeneities in the ionized component of the interstellar medium in the central 100 pc around Sgr A*. Scattering, which causes temporal broadening of pulses, can only be mitigated by observing at higher frequencies. Here we describe recent searches of the Galactic centre region performed at a frequency of 18.95 GHz with the Effelsberg radio telescope.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Pulsar timing in the Galactic Center

    gr-qc 2025-01 conditional novelty 6.0 of 10

    A fully relativistic (geodesic) pulsar timing model for the Galactic Center shows that 1PN-based timing formulas produce errors of up to seconds for tight orbits around Sgr A*.

  2. Thermal emission from dark matter-heated neutron stars in the Galactic Center

    astro-ph.HE 2026-06 unverdicted novelty 3.0 of 10

    DM-heated neutron stars in the Galactic Center reach equilibrium temperatures of 10^4-10^6 K but their emission is below detection thresholds due to extinction.

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