Speaker
Description
We present angular diameter distance measurements obtained by locating the
BAO scale in the distribution of galaxies selected from the first year of Dark
Energy Survey data. We consider a sample of over 1.3 million galaxies
distributed over a footprint of 1318 deg$^2$ with $0.6 < z_{\rm photo} < 1$ and
a typical redshift uncertainty of $0.03(1+z)$. This sample was selected using a color/magnitude selection that
optimizes trade-offs between number density and redshift uncertainty. We
investigate the BAO signal in the projected clustering using three conventions,
the angular separation, the co-moving transverse separation, and spherical
harmonics. Further, we compare results obtained from template based and machine
learning photometric redshift determinations. We use 1800 simulations that
approximate our sample in order to produce covariance matrices and allow us to
validate our distance scale measurement methodology. We measure the angular
diameter distance, $D_A$, at the effective redshift of our sample divided by
the true physical scale of the BAO feature, $r_{\rm d}$. We obtain close to a 4
per cent distance measurement of $D_A(z_{\rm eff}=0.81)/r_{\rm d} = 10.75\pm
0.43 $. These results are consistent with the flat $\Lambda$CDM concordance
cosmological model supported by numerous other recent experimental results.
