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We present a comprehensive view of the W51B HII region complex and the W51Csupernova remnant (SNR) using new radio observations from the VLA, VLBA,MERLIN, JCMT, and CSO along with archival data from Spitzer, ROSAT, ASCA, andChandra. Our VLA data include the first 400 cm (74 MHz) continuum image of W51at high resolution (88 arcsec). The 400 cm image shows non-thermal emissionsurrounding the G49.2-0.3 HII region, and a compact source of non-thermalemission (W51B_NT) coincident with the previously-identified OH (1720 MHz)maser spots, non-thermal 21 and 90 cm emission, and a hard X-ray source.W51B_NT falls within the region of high likelihood for the position of TeVgamma-ray emission. Using the VLBA three OH (1720 MHz) maser spots are detectedin the vicinity of W51B_NT with sizes of 60 to 300 AU and Zeeman effectmagnetic field strengths of 1.5 to 2.2 mG. The multiwavelength data demonstratethat the northern end of the W51B HII region complex has been partly envelopedby the advancing W51C SNR and this interaction explains the presence of W51B_NTand the OH masers. This interaction also appears in the thermal molecular gaswhich partially encircles W51B_NT and exhibits narrow pre-shock (DeltaV 5 km/s)and broad post-shock (DeltaV 20 km/s) velocity components. RADEX radiativetransfer modeling of these two components yield physical conditions consistentwith the passage of a non-dissociative C-type shock. Confirmation of theW51B/W51C interaction provides additional evidence in favor of this regionbeing one of the best candidates for hadronic particle acceleration known thusfar.

OH (1720 MHz) Masers: A Multiwavelength Study of the Interaction between the W51C Supernova Remnant and the W51B Star Forming Region