The luminous red nova AT 2018bwo in NGC 45 and its binary yellow supergiant progenitor


Abstract in English

Luminous Red Novae (LRNe) are astrophysical transients associated with the partial ejection of a binary systems common envelope (CE) shortly before its merger. Here we present the results of our photometric and spectroscopic follow-up campaign of AT2018bwo (DLT18x), a LRN discovered in NGC45, and investigate its progenitor system using binary stellar-evolution models. The transient reached a peak magnitude of $M_r=-10.97pm0.11$ and maintained this brightness during its optical plateau of $t_p = 41pm5$days. During this phase, it showed a rather stable photospheric temperature of ~3300K and a luminosity of ~$10^{40}$erg/s. The photosphere of AT2018bwo at early times appeared larger and cooler than other similar LRNe, likely due to an extended mass-loss episode before the merger. Towards the end of the plateau, optical spectra showed a reddened continuum with strong molecular absorption bands. The reprocessed emission by the cooling dust was also detected in the mid-infrared bands ~1.5 years after the outburst. Archival Spitzer and Hubble Space Telescope data taken 10-14 years before the transient event suggest a progenitor star with $T_{prog}sim 6500$K, $R_{prog}sim 100R_{odot}$ and $L_{prog}sim 2times10^4L_{odot}$, and an upper limit for optically thin warm (1000 K) dust mass of $M_d<10^{-6}M_{odot}$. Using stellar binary-evolution models, we determined the properties of binary systems consistent with the progenitor parameter space. For AT2018bwo, we infer a primary mass of 12-16 $M_{odot}$, which is 9-45% larger than the ~11$M_{odot}$ obtained using single-star evolution models. The system, consistent with a yellow-supergiant primary, was likely in a stable mass-transfer regime with -2.4<log ($dot{M}/M_{odot}$/yr)<-1.2 a decade before the main instability occurred. During the dynamical merger, the system would have ejected 0.15-0.5$M_{odot}$ with a velocity of ~500 km/s.

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