Journal
ASTRONOMY & ASTROPHYSICS
Volume 625, Issue -, Pages -Publisher
EDP SCIENCES S A
DOI: 10.1051/0004-6361/201935511
Keywords
binaries: close; stars: massive; supernovae: individual: AT 2017jfs; supernovae: individual: NGC440-2011OT1; stars: winds, outflows
Categories
Funding
- China Scholarship Council [201606040170]
- Royal Society - Science Foundation Ireland University Research Fellowship
- Spanish MICINN [ESP2017-82674-R]
- FEDER funds [11573003]
- NSFC - National Astronomical Observatories of China
- Chinese Academy of Sciences
- Special Fund for Astronomy from the Ministry of Finance
- PRIN-INAF
- STFC [ST/M005348/1]
- H2020 through an ERC [758638]
- ESO Studentship
- Program of development of M.V. Lomonosov Moscow State University (Leading Scientific School Physics of stars, relativistic objects and galaxies)
- Spanish research project [AYA2017-89384-P]
- Center of Excellence Severo Ochoa award [SEV-2017-0709, RyC-2012-09984, RyC-2012-09975, IJCI-2015-26153, IJCI-2016-30940]
- Max-Planck Society
- Max Planck Institute for Extraterrestrial Physics
- National Central University of Taiwan
- NASA [NN12AR55G]
- NASA Science Mission Directorate
- US NSF [AST-1238877]
- University of Maryland, and Eotvos Lorand University (ELTE)
- NEO Observation Program
- AURA through the National Science Foundation [AST 0132798]
- Instrument Center for Danish Astrophysics (IDA)
- European Organisation for Astronomical Research in the Southern Hemisphere under ESO programmes [199, D-0143]
- LCOGT network
- Nordic Optical Telescope (NOT)
- UK Science and Technology Facilities Council
- Gordon and Betty Moore Foundation [GBMF5490]
- NSF [AST-0908816]
- Mt. Cuba Astronomical Foundation
- Center for Cosmology and AstroParticle Physics at the Ohio State University
- Chinese Academy of Sciences South America Center for Astronomy (CAS-SACA)
- Villum Foundation
- STFC [ST/P006892/1, ST/P000312/1, ST/S006176/1] Funding Source: UKRI
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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.
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