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Constraints on ultralight scalar dark matter from pulsar timing
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Constraints on ultralight scalar dark matter from pulsar timing
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We performed a Bayesian analysis of pulsar timing residuals from the NANOGrav pulsar timing array to search for a specific form of stochastic narrow-band signal produced by oscillating gravitational potential in the Galactic halo. Such oscillations arise in models of warm dark matter composed of an ultralight massive scalar field (m\sim 10^{-23} eV), recently considered by Khmelnitsky and Rubakov (2014). In the monochromatic approximation, the stringent upper limit (95% c.l.) on the variable gravitational potential amplitude is found to be Psi_c<1.14 10^{-15}, corresponding to the characteristic strain h_c=2\sqrt{3}\Psi_c < 4 10^{-15} at frequency f=1.75 10^{-8} Hz. In the narrow-band approximation, the upper limit of this background energy density is \Omega_{GPB}<1.27 10^{-9} at frequency f=6.2 10^{-9} Hz. These limits are an order of magnitude higher than the expected signal amplitude if the galactic dark matter consists of the ultralight scalar field. The applied analysis of pulsar timing residuals can be used to search for any narrow-band stochastic signals with different correlation properties. As a by-product, parameters of the red noise present in four NANOGrav pulsars (J1713+0747, J2145-0750, B1855+09, J1744-1134) have been evaluated.
Forward citations
Cited by 5 Pith papers
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Using S2 star periastron precession, the work constrains ultralight scalar dark matter mass ratios to below 10^{-3} or 1 and improves quadratic coupling bounds for masses 10^{-20} to 10^{-18} eV.
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Constraints on Ultralight Scalar and Dark Photon Dark Matter from PPTA-DR3 and EPTA-DR2
Bayesian analysis of PPTA-DR3 and EPTA-DR2 finds no statistically significant ULDM signals and sets 95% CL upper limits on scalar and dark photon dark matter, improving prior bounds in most mass ranges.
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The SKAO Pulsar Timing Array
An SKAO PTA with ~174 millisecond pulsars can dominate nanohertz GW sensitivity within four years and enable continuous-wave detections plus anisotropy maps of the gravitational-wave background.
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