  GW190426_152155 was recently reported as one of the 39 candidate
gravitational wave (GW) events in \citet{2020arXiv201014527A}, which has an
unusual source-frame chirp mass $\sim 2.4M_{\odot}$ and may be the first GW
signal from a neutron star-black hole (NSBH) merger. Assuming an astrophysical
origin, we reanalyze GW190426_152155 using several waveforms with different
characteristics, and consider two different priors for the mass ratio of the
binary (Uniform and LogUniform). We find that the results are influenced by the
priors of mass ratio, and this candidate could also be from the merger of two
low mass black holes (BH). In the case for a binary black hole (BBH) merger,
the effective spin is likely negative and the effective precession spin is
non-negligible. As for the NSBH merger, supposing the mass of the light object
follow the distribution of current neutron stars (NSs) with a reasonably
measured/constrained mass, the spin of the low mass BH is so small that is hard
to generate bright electromagnetic emission. Finally, we estimate a merger rate
of GW190426\_152155-like systems to be $59^{+137}_{-51}~{\rm Gpc}^{-3}~{\rm
yr}^{-1}$.

High Energy Astrophysical Phenomena;High Energy Physics - Phenomenology