Testing space-time geometries and theories of gravity at the Galactic Center with pulsar's time delay

Abstract

We developed a numerical methodology to compute the fully-relativistic propagation time of photons emitted by a pulsar in orbit around a massive compact object, like the supermassive black hole Sagittarius A* in the Galactic Center, whose gravitational field is described by a generic spherically symmetric space-time. Pulsars at the Galactic Center are usually regarded as the next major precision probe for theories of gravity, filling the current experimental gap between horizon-scale gravity tests and those at larger scales. We retain a completely general approach, which allows us to apply our code to the Schwarzschild space-time (by which we successfully validate our methodology) and to three different well-motivated alternatives to the standard black hole paradigm. The results of our calculations highlight departures spanning several orders of magnitudes in timing residuals, that are supposed to be detectable with future observing facilities like the Square Kilometer Array.

15 pages, 8 figures, 1 table. Accepted for publication in MNRAS

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Cited by in corpus (9)

• Probing the vector charge of Sagittarius A* with pulsar timing
• Future prospects for measuring 1PPN parameters using observations of S2 and S62 at the Galactic Center
• Relativistic time delay analysis of pulsar signals near ultra-compact objects
• Kerr-scalaron metric and astronomical consequences near the Galactic Center black hole
• PyGRO: a Python Integrator for General Relativistic Orbits
• Higher-derivative Heterotic Kerr-Sen Black Holes
• Consistent Four-derivative Heterotic Truncations and the Kerr-Sen Solution
• On the Deepest Search for Galactic Center Pulsars and an Examination of an Intriguing Millisecond Pulsar Candidate
• Timing Gravity with Pulsars in the Strong Field