http://arxiv.org/abs/1708.06502
To date, the only limit on graviton mass using galaxy clusters was obtained by Goldhaber and Nieto in 1974, using the fact that the orbits of galaxy clusters are bound and closed, and extend up to 580 kpc. From positing that only a Newtonian potential gives rise to such stable bound orbits, a limit on the graviton mass $m_g<10^{-29}$ eV was obtained (PRD 9,1119, 1974). Recently, it has been shown that one can get closed bound orbits for a whole class of non-Newtonian potentials (arXiv:1707.04937 and arXiv:1705.02444), thus invalidating the main \emph{ansatz} used in Goldhaber and Nieto to obtain the graviton mass bound. In order to obtain a revised estimate using galaxy clusters, we use dynamical mass models of the Abell 1689 (A1689) galaxy cluster to check their compatibility with a Yukawa gravitational potential. We assume mass models for the gas, dark matter, and galaxies for A1689 from arXiv:1703.10219 and arXiv:1610.01543, who used this cluster to test various alternate gravity theories, which dispense with the need for dark matter. We quantify the deviations in the acceleration profile using these mass models, assuming a Yukawa potential and that obtained assuming a Newtonian potential, by calculating the $\chi^2$ residuals between the two profiles. The 90\% c.l. upper limit on the graviton mass corresponds to the minimum mass for which $\Delta \chi^2>2.71$. Our estimated 90\% c.l. bound on the graviton mass ($m_g$) is thereby given by, $m_g < 1.64 \times 10^{-29}$ eV or in terms of the graviton Compton wavelength, $\lambda_g>7.6 \times 10^{19}$ km.
S. Desai
Wed, 23 Aug 17
20/45
Comments: 6 pages, 2 figures
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