We present and analyze a rich dataset including Subaru/SuprimeCam , HST/ACS and WFC3 , Keck/DEIMOS , Chandra/ACIS-I , and JVLA/C and D array for the merging cluster of galaxies ZwCl 0008.8+5215 . With a joint Subaru + HST weak gravitational lensing analysis , we identify two dominant subclusters and estimate the masses to be M _ { \text { 200 } } = \text { 5.7 } ^ { + \text { 2.8 } } _ { - \text { 1.8 } } \times \text { 10 } ^ { \text { 1 % 4 } } \text { M } _ { \odot } and \text { 1.2 } ^ { + \text { 1.4 } } _ { - \text { 0.6 } } \times \text { 10 } ^ { \text { 14 } } \text { M } _ { \odot } . We estimate the projected separation between the two subclusters to be \text { 924 } ^ { + \text { 243 } } _ { - \text { 206 } } \text { kpc } . We perform a clustering analysis of spectroscopically confirmed cluster member galaxies and estimate the line of sight velocity difference between the two subclusters to be \text { 92 } \pm \text { 164 } \text { km } \text { s } ^ { - \text { 1 } } . We further motivate , discuss , and analyze the merger scenario through an analysis of the 42 ks of Chandra/ACIS-I and JVLA/C and D array polarization data . The X-ray surface brightness profile reveals a merging gas-core reminiscent of the Bullet Cluster . The global X-ray luminosity in the 0.5-7.0 keV band is 1.7 \pm 0.1 \times \text { 10 } ^ { \text { 44 } } erg s ^ { - \text { 1 } } and the global X-ray temperature is 4.90 \pm 0.13 keV . The radio relics are polarized up to \text { 40 } \% and along with the masses , velocities , and positions of the two subclusters we input these quantities into a Monte Carlo dynamical analysis and estimate the merger velocity at pericenter to be \text { 1800 } ^ { + \text { 400 } } _ { - \text { 300 } } \text { km } \text { s } ^ { - \text { 1 } } . This is a lower-mass version of the Bullet Cluster and therefore may prove useful in testing alternative models of dark matter . We do not find significant offsets between dark matter and galaxies , but the uncertainties are large with the current lensing data . Furthermore , in the east , the BCG is offset from other luminous cluster galaxies , which poses a puzzle for defining dark matter – galaxy offsets .