  We examine the properties of the Magellanic Bridge connecting the Large and
Small Magellanic Clouds using ab-type RR Lyrae variables from the extensive
dataset of the Optical Gravitational Lensing Experiment (OGLE), Phase IV data
release. The metallicities of the RR Lyraes are determined from the
characteristics of their light curves, with an average abundance of [Fe/H] =
-1.790 +/- 0.011 (sem) in the Magellanic Bridge. From the individual reddenings
of these stars, derived via their minimum light curve colors, we determined a
median color excess of E(V-I) = 0.101 +/- 0.007 (sem) (implying E(B-V)
$\approx$ 0.077). The peak distance modulus of 18.57 +/- 0.048 (sem) places the
Bridge stars at distances between the two systems. The metallicity and distance
distributions probe the structure of the Magellanic system as a whole,
revealing a smooth transition that connects the galaxies. An examination of the
HI content does not find a clear correlation between HI emission strength and
RR Lyrae spatial distribution, suggesting that the old stellar populations may
trace the overlapping halo distributions of the two Magellanic Clouds.

Astrophysics of Galaxies;Solar and Stellar Astrophysics