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The progenitor system of the compact binary merger GW190425 had a total massof $3.4^{+0.3}_{-0.1}$ M$_\odot$ (90th-percentile confidence region) asmeasured from its gravitational wave signal. This mass is significantlydifferent from the Milky Way (MW) population of binary neutron stars (BNSs)that are expected to merge in a Hubble time and from that of the first BNSmerger, GW170817. Here we explore the expected electromagnetic signatures ofsuch a system. We make several astrophysically motivated assumptions to furtherconstrain the parameters of GW190425. By simply assuming that both componentswere NSs, we reduce the possible component masses significantly, finding $m_1 =1.85^{+0.27}_{-0.19}$ M$_\odot$ and $m_2 = 1.47^{+0.16}_{-0.18}$ M$_\odot$.However if the GW190425 progenitor system was a NS-black hole merger, we findbest-fitting parameters $m_1 = 2.19^{+0.21}_{-0.17}$ M$_\odot$ and $m_2 =1.26^{+0.10}_{-0.08}$ M$_\odot$. For a well-motivated BNS system where thelighter NS has a mass similar to the mass of non-recycled NSs in MW BNSsystems, we find $m_1 = 2.03^{+0.15}_{-0.14}$ M$_\odot$ and $m_2 = 1.35 \pm0.09$ M$_\odot$, corresponding to only 7% mass uncertainties. For allscenarios, we expect a prompt collapse of the resulting remnant to a blackhole. Examining detailed models with component masses similar to ourbest-fitting results, we find the electromagnetic counterpart to GW190425 isexpected to be significantly redder and fainter than that of GW170817. We findthat almost all reported observations used to search for an electromagneticcounterpart for GW190425 were too shallow to detect the expected counterpart.If the LIGO-Virgo Collaboration promptly provides the chirp mass, theastronomical community can adapt their observations to improve the likelihoodof detecting a counterpart for similarly "high-mass" BNS systems. (abridged)

Updated Parameter Estimates for GW190425 Using Astrophysical Arguments and Implications for the Electromagnetic Counterpart