Panchromatic evolution of three luminous red novae: Forbidden hugs in pandemic times -- IV
Creators: name: Pastorello, A.
name: Valerin, G.
name: Fraser, M.
name: Reguitti, A.
name: Elias-Rosa, N.
name: Filippenko, A. V.
name: Rojas-Bravo, C.
name: Tartaglia, L.
name: Reynolds, T. M.
name: Valenti, S.
name: Andrews, J. E.
name: Ashall, C.
name: Bostroem, K. A.
name: Brink, T. G.
name: Burke, J.
name: Cai, Y. -Z.
name: Cappellaro, E.
name: Coulter, D. A.
name: Dastidar, R.
name: Davis, K. W.
name: Dimitriadis, G.
name: Fiore, A.
name: Foley, R. J.
name: Fugazza, D.
name: Galbany, L.
name: Gangopadhyay, A.
name: Geier, S.
name: Gutierrez, C. P.
name: Haislip, J.
name: Hiramatsu, D.
name: Holmbo, S.
name: Howell, D. A.
name: Hsiao, E. Y.
name: Hung, T.
name: Jha, S. W.
name: Kankare, E.
name: Karamehmetoglu, E.
name: Kilpatrick, C. D.
name: Kotak, R.
name: Kouprianov, V.
name: Kravtsov, T.
name: Kumar, S.
name: Li, Z. -T.
name: Lundquist, M. J.
name: Lundqvist, P.
name: Matilainen, K.
name: Mazzali, P. A.
name: McCully, C.
name: Misra, K.
name: Morales-Garoffolo, A.
name: Moran, S.
name: Morrell, N.
name: Newsome, M.
name: Gonzalez, E. Padilla
name: Pan, Y. -C.
name: Pellegrino, C.
name: Phillips, M. M.
name: Pignata, G.
name: Piro, A. L.
name: Reichart, D. E.
name: Rest, A.
name: Salmaso, I.
name: Sand, D. J.
name: Siebert, M. R.
name: Smartt, S. J.
name: Smith, K. W.
name: Srivastav, S.
name: Stritzinger, M. D.
name: Taggart, K.
name: Tinyanont, S.
name: Yan, S. -Y.
name: Wang, L.
name: Wang, X. -F.
name: Williams, S. C.
name: Wyatt, S.
name: Zhang, T. -M.
name: de Boer, T.
name: Chambers, K.
name: Gao, H.
name: Magnier, E.
Publisher: name: arXiv
Year: 2022
Subjects: subject: Solar and Stellar Astrophysics (astro-ph.SR)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We present photometric and spectroscopic data on three extragalactic luminous red novae (LRNe): AT2018bwo, AT2021afy, and AT2021blu. AT2018bwo was discovered in NGC45 (at 6.8 Mpc) a few weeks after the outburst onset. During the monitoring period, the transient reached a peak luminosity of 10^40 erg/s. AT2021afy, hosted by UGC10043 (49.2 Mpc), showed a double-peaked light curve, with the two peaks reaching a similar luminosity of 2.1(+-0.6)x10^41 erg/s. For AT2021blu in UGC5829, (8.6 Mpc), the pre-outburst phase was well-monitored by several photometric surveys, and the object showed a slow luminosity rise before the outburst. The light curve of AT2021blu was sampled with an unprecedented cadence until the object disappeared behind the Sun, and it was then recovered at late phases. The light curve of AT2021blu shows a double peak, with a prominent early maximum reaching a luminosity of 6.5x10^40 erg/s, which is half of that of AT2021afy. The spectra of AT2021afy and AT2021blu display the expected evolution for LRNe: a blue continuum dominated by prominent Balmer lines in emission during the first peak, and a redder continuum consistent with that of a K-type star with narrow absorption metal lines during the second, broad maximum. The spectra of AT2018bwo are markedly different, with a very red continuum dominated by broad molecular features in absorption. As these spectra closely resemble those of LRNe after the second peak, AT2018bwo was probably discovered at the very late evolutionary stages. This would explain its fast evolution and the spectral properties compatible with that of an M-type star. From the analysis of deep frames of the LRN sites years before the outburst, and considerations of the light curves, the quiescent progenitor systems of the three LRNe were likely massive, with primaries ranging from 13Mo for AT2018bwo, to 13-18Mo for AT2021blu, and over 40Mo for AT2021afy.
description: 33 pages, 19 figures, 7 tables (plus 3 available at the CDS). Accepted for publication in A&amp;A