J/A+A/709/A25ivo://CDS.VizieR/J/A+A/709/A25CDSReguitti A.Pastorello A.Valerin G.Romanov F.D.Siviero A.Cai Y.-Z.,Ciroi S.Elias-Rosa N.Iijima T.Kankare E.Koivisto N.Kravtsov T.,Mason E.Matilainen K.Mura A.C.Ochner P.Reynolds T.M.,Stritzinger M.D.2026-05-19T14:14:26Z2026-04-30T07:58:58ZCDS support team

CDS, Observatoire de Strasbourg, 11 rue de l'Universite, F-67000 Strasbourg, France

cds-question@unistra.frnovaephotometryWe present photometric and spectroscopic observations of the luminous red nova (LRN) AT 2025abao, the fourth discovered in M 31. The LRN, associated with the AGB star WNTR23bzdiq, was discovered during the fast rise following the minimum phase. It reached the peak at g=15.1mag (Mg=-9.5+/-0.1mag), and then it settled onto a long-duration plateau in the red bands, lasting 70 days, while it was slowly linearly declining in the blue bands. The object showed similarities at peak with the canonical LRNe V838 Monocerotis, V1309 Scorpii, and with the faint and fast-evolving AT 2019zhd, the third LRN in M31, though the later evolution is different. Spectroscopically, AT 2025abao evolved as a canonical LRN: the early spectra present a blue continuum with narrow Balmer lines in emission; at peak, the spectral continuum has cooled to a yellow colour, with a photospheric temperature of 6000K. Balmer lines have weakened while absorption lines from metals (FeI, FeII, ScII, BaII, TiII) have developed, and in particular broad (FWHM~700km/s) from the UV CaII H&K lines. Medium- and high-resolution spectra reveal a counter-P Cygni absorption profile in H{alpha}. Finally, late time spectra show an orange continuum (T~4000-5000K), a return in strength of the Balmer lines and the formation of molecular absorption bands. AT 2025abao is the rare case of a LRN with detailed archival information regarding the progenitor system. For the first time, we obtained the spectral energy distribution in the infrared of the precursor of a LRN, which is consistent with that of an M giant/AGB. We propose that the dichotomy of light curve behaviour in LRNe (two peaks vs. plateau) can be explained by the extent and H-richness of the common envelope.2026A&A...709A..25Rhttps://cdsarc.cds.unistra.fr/viz-bin/cat/J/A+A/709/A25CatalogResearchIsServedByTAP VizieR generic servicehttps://cds.unistra.fr/vizier-org/licences_vizier.htmlhttps://vizier.cds.unistra.fr/viz-bin/VizieR-2?-source=J/A+A/709/A25https://vizier.iucaa.in/viz-bin/VizieR-2?-source=J/A+A/709/A25http://vizieridia.saao.ac.za/viz-bin/VizieR-2?-source=J/A+A/709/A25https://vizier.cds.unistra.fr/viz-bin/votable?-source=J/A+A/709/A25https://vizier.iucaa.in/viz-bin/votable?-source=J/A+A/709/A25http://vizieridia.saao.ac.za/viz-bin/votable?-source=J/A+A/709/A25GETtext/xml+votablehttps://tapvizier.cds.unistra.fr/TAPVizieR/tapdefaultJ/A+A/709/A25/tablePhotometry tablerecnoRecord number assigned by the VizieR team. Should Not be used for identification.meta.recordintMJDObservation date (MJD)dtime.epochdoubleFilterFilter (1)instr.bandpasscharSystemMagnitude system, vega or abmeta.notecharmagMagnitude in Flitermagphot.magfloate_magUncertainty in magnitudemagstat.error;phot.magfloatDet[PU] Detection (P=yes, U=no)meta.codecharInstTelescope, Instrumentinstrchar