The UVES Large Program for Testing Fundamental Physics: I Bounds on a
  change in alpha towards quasar HE 2217-2818
  Absorption line systems detected in quasar spectra can be used to compare the
value of the fine-structure constant, {\alpha}, measured today on Earth with
its value in distant galaxies. In recent years, some evidence has emerged of
small temporal and also spatial variations of {\alpha} on cosmological scales
which may reach a fractional level of ~ 10 ppm (parts per million). To test
these claims we are conducting a Large Program with the VLT UVES . We are
obtaining high-resolution (R ~ 60000 and high signal-to-noise ratio (S/N ~ 100)
UVES spectra calibrated specifically for this purpose. Here we analyse the
first complete quasar spectrum from this Program, that of HE 2217-2818. We
apply the Many Multiplet method to measure {\alpha} in 5 absorption systems
towards this quasar: zabs = 0.7866, 0.9424, 1.5558, 1.6279 and 1.6919. The most
precise result is obtained for the absorber at zabs = 1.6919 where 3 Fe II
transitions and Al II {\lambda}1670 have high S/N and provide a wide range of
sensitivities to {\alpha}. The absorption profile is complex, with several very
narrow features, and requires 32 velocity components to be fitted to the data.
Our final result for the relative variation in {\alpha} in this system is
Delta{\alpha}/{\alpha} = +1.3 +/- 2.4stat +/- 1.0sys ppm. This is one of the
tightest current bounds on {\alpha} variation from an individual absorber. The
absorbers towards quasar HE 2217-2818 reveal no evidence for variation in
{\alpha} at the 3 ppm precision level (1{\sigma} confidence). If the recently
reported 10 ppm dipolar variation of {\alpha} across the sky were correct, the
expectation at this sky position is (3.2-5.4) +/-1.7 ppm depending on dipole
model used . Our constraint of Delta{\alpha}/{\alpha}=+1.3+/-2.4stat +/-1.0sys
ppm is not inconsistent with this expectation.
