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Some supernovae (SNe) are powered by collision of the SN ejecta with a densecircumstellar matter (CSM). Their emission spectra show characteristic lineshapes of combined broad emission and narrow P-Cyg lines, which should closelyrelate to the CSM structure and the mass-loss mechanism that creates the denseCSM. We quantitatively investigate the relationship between the line shape andthe CSM structure by Monte Carlo radiative transfer simulations, consideringtwo representative cases of dense CSM formed by steady and eruptive mass loss.Comparing the H$\alpha$ emission between the two cases, we find that a narrowP-Cyg line appears in the eruptive case while it does not appear in the steadycase, due to the difference in the velocity gradient in the dense CSM. We alsoreproduce the blue-shifted photon excess observed in some Type IIn SNe, whichis formed by photon transport across the shock wave and find the relationshipbetween the velocity of the shocked matter and the amount of the blue shift ofthe photon excess. We conclude that the presence or absence of narrow P-Cyglines can distinguish the mass loss mechanism, and suggest high-resolutionspectroscopic observations with $\lambda/ \Delta \lambda \gtrsim 10^4$ afterthe light curve peak for applying this diagnostic method.

Diagnosis of Circumstellar Matter Structure in Interaction-powered Supernovae with Hydrogen Line Feature