Stringent bounds to spatial variations of the electron-to-proton mass ratio in the Milky Way

Details Stringent bounds to spatial variations of the electron-to-proton mass ratio in the Milky Way Stringent bounds to spatial variations of the electron-to-proton mass ratio in the Milky Way

2009-07-07

arxiv.org/abs/0907.1192v1

Nucl.Phys.Proc.Suppl.194:287-293,2009

Astronomy and Astrophysics

Astrophysics

Cosmology and Extragalactic Astrophysics

7 pages +2 figures. Galileo Galilei Institute Conferences on Dark Matter and Dark Energy

Scientific paper

10.1016/j.nuclphysbps.2009.07.03

The ammonia method to probe variations of the electron-to-proton mass ratio, Delta_mu/mu, is applied for the first time to dense prestellar molecular clouds in the Milky Way. Carefully selected sample of 21 NH_3/CCS pairs observed in the Perseus molecular cloud provide the offset Delta V (CCS-NH_3)= 36+/-7_{stat}+/-13.5_{sys} m/s . A similar offset of Delta V = 40.8 +/- 12.9_{stat} m/s between NH_3 (J,K) = (1,1) and N_2H+ J = 1-0 has been found in an isolated dense core L183 by Pagani et al. (2009). Overall these observations provide a safe bound of a maximum offset between ammonia and the other molecules at the level of Delta V < 100 m/s. This bound corresponds to Delta_mu/mu < 1E-7, which is an order of magnitude more sensitive than available extragalactic constraints. Taken at face value the measured Delta V shows positive shifts between the line centers of NH_3 and these two other molecules and suggest a real offset, which would imply a Delta_mu/mu about 4E-8. If Delta_mu/mu follows the gradient of the local gravitational potential, then the obtained results are in conflict with laboratory atomic clock experiments in the solar system by 5 orders of magnitude, thus requiring a chameleon-type scalar field model. New measurements involving other molecules and a wider range of objects along with verification of molecular rest frequencies are currently planned to confirm these first indications.

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