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The evolution of luminous red nova AT 2017jfs in NGC 4470
Osserv Astron Padova, INAF, Vicolo Osservatorio 5, I-35122 Padua, Italy..
Univ Cadiz, Dept Appl Phys, Campus Puerto Real, Cadiz 11510, Spain..
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2019 (English)In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 625, article id L8Article in journal (Refereed) Published
Abstract [en]

We present the results of our photometric and spectroscopic follow-up of the intermediate-luminosity optical transient AT 2017jfs. At peak, the object reaches an absolute magnitude of M-g = 15.46 +/- 0.15 mag and a bolometric luminosity of 5.5 x 10(41) erg s(-1). Its light curve has the double-peak shape typical of luminous red novae (LRNe), with a narrow first peak bright in the blue bands, while the second peak is longer-lasting and more luminous in the red and near-infrared (NIR) bands. During the first peak, the spectrum shows a blue continuum with narrow emission lines of H and Fe II. During the second peak, the spectrum becomes cooler, resembling that of a K-type star, and the emission lines are replaced by a forest of narrow lines in absorption. About 5 months later, while the optical light curves are characterized by a fast linear decline, the NIR ones show a moderate rebrightening, observed until the transient disappears in solar conjunction. At these late epochs, the spectrum becomes reminiscent of that of M-type stars, with prominent molecular absorption bands. The late-time properties suggest the formation of some dust in the expanding common envelope or an IR echo from foreground pre-existing dust. We propose that the object is a common-envelope transient, possibly the outcome of a merging event in a massive binary, similar to NGC4490-2011OT1.

Place, publisher, year, edition, pages
EDP SCIENCES S A , 2019. Vol. 625, article id L8
Keywords [en]
binaries: close, stars: massive, supernovae: individual: AT 2017jfs, supernovae: individual: NGC440-2011OT1, stars: winds, outflows
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Physical Sciences
Identifiers
URN: urn:nbn:se:kth:diva-252597DOI: 10.1051/0004-6361/201935511ISI: 000468127400002OAI: oai:DiVA.org:kth-252597DiVA, id: diva2:1322620
Note

QC 20190611

Available from: 2019-06-11 Created: 2019-06-11 Last updated: 2019-06-11Bibliographically approved

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