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We present the first spectroscopically resolved \ha\ emission map of theLarge Magellanic Cloud's (LMC) galactic wind. By combining new WisconsinH-alpha Mapper (WHAM) observations ($I_{\rm H\alpha}\gtrsim10~{\rm mR}$) withexisting \hicm\ emission observations, we have (1) mapped the LMC's near-sidegalactic wind over a local standard of rest (LSR) velocity range of $+50\le\rmv_{LSR}\le+250~{\rm km}~{\rm s}^{-1}$, (2) determined its morphology andextent, and (3) estimated its mass, outflow rate, and mass-loading factor. Weobserve \ha\ emission from this wind to typically 1-degree off the LMC's \hi\disk. Kinematically, we find that the diffuse gas in the warm-ionized phase ofthis wind persists at both low ($\lesssim100~{\rm km}~{\rm s}^{-1}$) and high($\gtrsim100~{\rm km}~{\rm s}^{-1}$) velocities, relative to the LMC's \hi\disk. Furthermore, we find that the high-velocity component spatially alignswith the most intense star-forming region, 30~Doradus. We, therefore, concludethat this high-velocity material traces an active outflow. We estimate the massof the warm ($T_e\approx10^4~\rm K$) ionized phase of the near-side LMC outflowto be $\log{\left(M_{\rm ionized}/M_\odot\right)=7.51\pm0.15}$ for the combinedlow and high velocity components. Assuming an ionization fraction of 75\% andthat the wind is symmetrical about the LMC disk, we estimate that its total(neutral and ionized) mass is $\log{\left(M_{\rm total}/M_\odot\right)=7.93}$,its mass-flow rate is $\dot{M}_{\rm outflow}\approx1.43~M_\odot~\rm yr^{-1}$,and its mass-loading factor is $\eta\approx4.54$. Our average mass-loadingfactor results are roughly a factor of 2.5 larger than previous \ha\ imagingand UV~absorption line studies, suggesting that those studies are missingnearly half the gas in the outflows.

Mapping the Supernovae Driven Winds of the Large Magellanic Cloud in H$\alpha$ Emission I