2019ApJ...873L...3B

We report distinctly double-peaked Hα and Hβ emission lines in the late-time, nebular-phase spectra (>=200 days) of the otherwise normal at early phases (<=100 days) type IIP supernova ASASSN-16at (SN 2016X). Such distinctly double-peaked nebular Balmer lines have never been observed for a type II SN. The nebular-phase Balmer emission is driven by the radioactive ⁵⁶Co decay, so the observed line profile bifurcation suggests a strong bipolarity in the ⁵⁶Ni distribution or in the line-forming region of the inner ejecta. The strongly bifurcated blueshifted and redshifted peaks are separated by ∼3 x 10³ km s^–1 and are roughly symmetrically positioned with respect to the host-galaxy rest frame, implying that the inner ejecta are composed of two almost-detached blobs. The red peak progressively weakens relative to the blue peak, and disappears in the 740 days spectrum. One possible reason for the line-ratio evolution is increasing differential extinction from continuous formation of dust within the envelope, which is also supported by the near-infrared flux excess that develops after ∼100 days.