Abstract
In this article we study gravitational lensing by non-rotating and asymptotically flat black holes in Horndeski theory. By adopting the strong deflection limit, we calculate the deflection angle, from which we obtain the positions and the magnifications of the relativistic images. We compare our results with those corresponding to black holes in General Relativity. We analyze the astrophysical consequences in the case of the nearest supermassive black holes.
Highlights
The unsolved problem of the nature of the dark matter and the dark energy necessary for the explanation of the observed features of the Universe within the context of general relativity has led to a growing interest in modified gravity theories
In this article we study gravitational lensing by non-rotating and asymptotically flat black holes in Horndeski theory
To obtain the image positions, we start by taking the deflection angle in the strong deflection limit approximation and by using the approximate geometric relation b = θ DOL, with DOL the observer-lens distance
Summary
The unsolved problem of the nature of the dark matter and the dark energy necessary for the explanation of the observed features of the Universe within the context of general relativity has led to a growing interest in modified gravity theories. Horndeski [49] found the most general scalar–tensor theory with second-order derivative equations of motion. In this theory, the action has the form. A new class of scalar–tensor theories that extend Horndeski (dubbed “beyond Horndeski”) was introduced, with equations of motion of higher order in the derivatives [52,53], but with the property that the true propagating degrees of freedom obey well-behaved second-order equations, being free from Ostrogradski instabilities.
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