Deflection angle and lensing signature of covariant f(T) gravity. (arXiv:2105.04578v2 [astro-ph.CO] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Ren_X/0/1/0/all/0/1">Xin Ren</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Zhao_Y/0/1/0/all/0/1">Yaqi Zhao</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Saridakis_E/0/1/0/all/0/1">Emmanuel N. Saridakis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cai_Y/0/1/0/all/0/1">Yi-Fu Cai</a>
We calculate the deflection angle, as well as the positions and
magnifications of the lensed images, in the case of covariant $f(T)$ gravity.
We first extract the spherically symmetric solutions for both the pure-tetrad
and the covariant formulation of the theory, since considering spherical
solutions the extension to the latter is crucial, in order for the results not
to suffer from frame-dependent artifacts. Applying the weak-field, perturbative
approximation we extract the deviations of the solutions comparing to General
Relativity. Furthermore, we calculate the deflection angle and then the
differences of the positions and magnifications in the lensing framework. This
effect of consistent $f(T)$ gravity on the lensing features can serve as an
observable signature in the realistic cases where $f(T)$ is expected to deviate
only slightly from General Relativity, since lensing scales in general are not
restricted as in the case of Solar System data, and therefore deviations from
General Relativity could be observed more easily.
We calculate the deflection angle, as well as the positions and
magnifications of the lensed images, in the case of covariant $f(T)$ gravity.
We first extract the spherically symmetric solutions for both the pure-tetrad
and the covariant formulation of the theory, since considering spherical
solutions the extension to the latter is crucial, in order for the results not
to suffer from frame-dependent artifacts. Applying the weak-field, perturbative
approximation we extract the deviations of the solutions comparing to General
Relativity. Furthermore, we calculate the deflection angle and then the
differences of the positions and magnifications in the lensing framework. This
effect of consistent $f(T)$ gravity on the lensing features can serve as an
observable signature in the realistic cases where $f(T)$ is expected to deviate
only slightly from General Relativity, since lensing scales in general are not
restricted as in the case of Solar System data, and therefore deviations from
General Relativity could be observed more easily.
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