TESTING THE SPEED OF GRAVITATIONAL WAVES OVER COSMOLOGICAL DISTANCES

Image: Merging black holes ripple space and time in this artist's concept. Credit: Swinburne Astronomy Productions

On September 14, 2015 at 09:50:45 UTC the two detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) observed a transient gravitational-wave signal from a black hole-black hole binary (BHBH) inspiral.

The Fermi gamma ray burst monitor revealed the presence of a possible electromagnetic counterpart (Connaughton et al. 2016): a weak transient source above 50 keV, 0.4 s after the GW event was detected with a false alarm probability of 0.0022. The spatial location of both events are poorly determined but mutually consistent.

If the EM and GW signals are related to the same transient phenomenon this opens up a new physical window with which to test the relative speeds of light and gravitational waves.

Several of the alternative theories of gravity invoked to explain the accelerated expansion of the Universe predict c_GW ≠ c_light. In a recent paper (Collett & Bacon 2016) the authors assume that the EM and GW are emitted at the same instant and they obtain a constraint on the ratio of the speeds of light and gravitational waves at the level of 10⁻¹⁷.

The assumption that the electromagnetic and gravitational wave emissions are emitted at the same time is a strong one, so they suggest a method that does not make such an assumption using a strongly lensed GW event and EM counterpart. They show that a single strongly lensed GW event would produce robust constraints at the 10⁻⁷ level, if a high energy EM counterpart is observed within the field-of-view of an observing gamma ray burst monitor.

Collett & Bacon 2016 - Testing the speed of gravitational waves over cosmological distances with strong gravitational lensing (arXiv)
Connaughton et al. 2016 - Fermi GBM Observations of LIGO Gravitational Wave event GW150914 (arXiv)

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Figure: False-Colour X-ray and infrared emission image from the core of the infrared shell. The RGB colours correspond to Chandra X-ray 0.2-10 keV (blue), IRAC infrared 8 μm (green), and HPACS 70 μm (red) data. The intensity scale is logarithmic for all channels. Overlaid are equal brightness levels from the MIPS 24 μm band. Note that around the CCO the infrared emission is suppressed in the 70 μm band and enhanced in the 24 μm band suggesting higher dust temperature. Credit: Doroshenko et al 2016 Central compact objects (CCOs) are thought to be young isolated neutron stars that were born during the preceding core-collapse supernova explosion.

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