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In this paper, we present the results from spectroscopic and photometricobservations of the M-type flare star YZ CMi in the framework of the Opticaland Infrared Synergetic Telescopes for Education and Research (OISTER)collaborations during the Transiting Exoplanet Survey Satellite (TESS)observation period. We detected 145 white-light flares from the TESS lightcurve and 4 H$\alpha$ flares from the OISTER observations performed between2019-01-16 and 2019-01-18. Among them, 3 H$\alpha$ flares were associated withwhite-light flares. However, one of them did not show clear brightening incontinuum; during this flare, the H$\alpha$ line exhibited blue-asymmetry whichhas lasted for $\sim 60$ min. The line of sight velocity of the blue-shiftedcomponent is $-80$ - $-100$ km s$^{-1}$. This suggests that there can be upwardflows of chromospheric cool plasma even without detectable red/NIR continuumbrightening. By assuming that the blue-asymmetry in H$\alpha$ line was causedby a prominence eruption on YZ CMi, we estimated the mass and kinetic energy ofthe upward-moving material to be $10^{16}$ - $10^{18}$ g and $10^{29.5}$ -$10^{31.5}$ erg, respectively. The estimated mass is comparable to expectationsfrom the empirical relation between the flare X-ray energy and mass ofupward-moving material for stellar flares and solar CMEs. In contrast, theestimated kinetic energy for the non-white-light flare on YZ CMi is roughly $2$orders of magnitude smaller than that expected from the relation between flareX-ray energy and kinetic energy for solar CMEs. This could be understood by thedifference in the velocity between CMEs and prominence eruptions.

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Time-resolved spectroscopy and photometry of an M dwarf flare star YZ  Canis Minoris with OISTER and TESS: Blue asymmetry in H$\alpha$ line during  the non-white light flare