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Abstract We study the spatially resolved outflow properties of CSWA13, an intermediate-mass ( M * = 10 9 M ⊙ ), gravitationally lensed star-forming galaxy at z = 1.87. We use Keck/KCWI to map outflows in multiple rest-frame UV interstellar medium (ISM) absorption lines, along with fluorescent Si ii * emission, and nebular emission from C iii ] tracing the local systemic velocity. The spatial structure of the outflow velocity mirrors that of the nebular kinematics, which we interpret to be a signature of a young galactic wind that is pressurizing the ISM of the galaxy but is yet to burst out. From the radial extent of Si ii * emission, we estimate that the outflow is largely encapsulated within 3.5 kpc. We explore the geometry (e.g., patchiness) of the outflow by measuring the covering fraction at different velocities, finding that the maximum covering fraction is at velocities v ≃ −150 km s −1 . Using the outflow velocity ( v out ), radius ( R ), column density ( N ), and solid angle (Ω) based on the covering fraction, we measure the mass-loss rate log m ̇ out / ( M ⊙ yr − 1 ) = 1.73 ± 0.23 and mass loading factor log η = 0.04 ± 0.34 for the low-ionization outflowing gas in this galaxy. These values are relatively large and the bulk of the outflowing gas is moving with speeds less than the escape velocity of the galaxy halo, suggesting that the majority of the outflowing mass will remain in the circumgalactic medium and/or recycle back into the galaxy. The results support a picture of high outflow rates transporting mass and metals into the inner circumgalactic medium, providing the gas reservoir for future star formation.
C. et al. (Mon,) studied this question.