Here we present the fundamental properties of the nuclear cluster of the Milky Way . First , we derive its structural properties by constructing a density map of the central 1000 ” using extinction-corrected star counts . We can describe the data with a two-component model built from Sersic profiles . The inner nearly spherical component is the nuclear cluster . The outer , strongly flattened component can be identified with the stellar component of the circumnuclear zone . Second , we enlarge the radius inside which detailed dynamics are available from 1 pc to 4 pc . We use more than 10000 individual proper motions and more than 2700 radial velocities . We determine the cluster mass by means of isotropic spherical Jeans modeling . We get a nuclear cluster mass within 100 ” of M _ { 100 ^ { \prime \prime } } = ( 6.11 \pm 0.52 | _ { \mathrm { fix } R _ { 0 } } \pm 0.97 | _ { R _ { 0 } } ) % \times 10 ^ { 6 } M _ { \odot } , which corresponds to a total cluster mass of M _ { \mathrm { NC } } = ( 13.08 \pm 2.51 | _ { \mathrm { fix } R _ { 0 } } \pm 2.08 | _ { R _ { 0 } } ) \times 1 % 0 ^ { 6 } M _ { \odot } . By combination of our mass with the flux we calculate M / L = 0.50 \pm 0.12 M _ { \odot } / L _ { \odot, \mathrm { Ks } } for the central 100 ” . That is broadly consistent with a Chabrier IMF . With its mass and a luminosity of M _ { \mathrm { Ks } } = -15.30 \pm 0.26 the nuclear cluster is a bright and massive specimen with a typical size .