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We present a new millimeter CO-line observation towards supernova remnant(SNR) CTB 87, which was regarded purely as a pulsar wind nebula (PWN), and anoptical investigation of a coincident surrounding superbubble. The COobservation shows that the SNR delineated by the radio emission is projectivelycovered by a molecular cloud (MC) complex at V$_{\rm {LSR}}$ = $-60$ to $-54$km s$^{-1}$. Both the symmetric axis of the radio emission and the trailingX-ray PWN appear projectively to be along a gap between two molecular gaspatches at $-58$ to $-57$ km s$^{-1}$. Asymmetric broad profiles of $^{12}$COlines peaked at $-58$ km s$^{-1}$ are found at the eastern and southwesternedges of the radio emission. This represents a kinematic signature consistentwith an SNR-MC interaction. We also find that a superbubble, $\sim 37'$ inradius, appears to surround the SNR from HI 21cm (V$_{\rm {LSR}} \sim -61$ to$-68$ km s$^{-1}$), WISE mid-IR, and optical extinction data. We build amulti-band photometric stellar sample of stars within the superbubble regionand find 82 OB star candidates. The likely peak distance in the stars'distribution seems consistent with the distance previously suggested for CTB87. We suggest the arc-like radio emission is mainly the relic of the part ofblastwave that propagates into the MC complex and is now in a radiative stagewhile the other part of blastwave has been expanding into the low-densityregion in the superbubble. This scenario naturally explains the lack of theX-ray emission related to the ejecta and blastwave. The SNR-MC interaction alsofavours a hadronic contribution to the {\gamma}-ray emission from the CTB 87region.

An Investigation of the Interstellar Environment of Supernova Remnant CTB 87