  We present the first primary transit light curve of the hot Jupiter HAT-P-16b
in the near-UV photometric band. We observed this object on December 29,2012 in
order to update the transit ephemeris, constrain its planetary parameters and
search for magnetic field interference. Vidotto et al. (2011a) postulate that
the magnetic field of HAT-P-16b can be constrained if its near-UV light curve
shows an early ingress compared to its optical light curve, while its egress
remains unchanged. However, we did not detect an early ingress in our night of
observing when using a cadence of 60 seconds and an average photometric
precision of 2.26mmag. We find a near-UV planetary radius of
Rp=1.274+-0.057RJup which is consistent with its near-IR radius of
Rp=1.289+-0.066RJup (Buchhave et al., 2010). We developed an automated
reduction pipeline and modeling package to process our data. The data reduction
package synthesizes a set of IRAF scripts to calibrate images and perform
aperture photometry. The modeling package utilizes the Levenberg-Marquardt
minimization algorithm to find a least-squares best fit and a differential
evolution Markov Chain Monte Carlo algorithm to find the best fit to the light
curve. To constrain the red noise in both fitting models we use the residual
permutation (rosary bead) method and time-averaging method.
