  The magnetic field within a few hundred parsecs of the center of the Galaxy
is an essential component of any description of that region. The field has
several pronounced observational manifestations: 1) morphological structures
such as nonthermal radio filaments (NTFs) -- magnetic flux tubes illuminated by
synchrotron emission from relativistic electrons -- and a remarkable,
large-scale, helically wound structure, 2) relatively strong polarization of
thermal dust emission from molecular clouds, presumably resulting from magnetic
alignment of the rotating dust grains, and 3) synchrotron emission from cosmic
rays. Because most of the NTFs are roughly perpendicular to the Galactic plane,
the implied large-scale geometry of the magnetic field is dipolar. Estimates of
the mean field strength vary from tens of microgauss to ~ a milligauss. The
merits and weaknesses of the various estimations are discussed here. If the
field strength is comparable to a milligauss, then the magnetic field is able
to exert a strong influence on the dynamics of molecular clouds, on the
collimation of a Galactic wind, and on the lifetimes and bulk motions of
relativistic particles. Related to the question of field strength is the
question of whether the field is pervasive throughout the central zone of the
Galaxy, or whether its manifestations are predominantly localized phenomena.
Current evidence favors the pervasive model.
