Photometry and spectroscopy of the luminous red nova PSNJ14021678+5426205 in the galaxy M101

Goranskij, V. P.; Barsukova, E. A.; Spiridonova, O. I.; Valeev, A. F.; Фатхуллин, Т. А.; Москвитин, А. С.; Vozyakova, O. V.; Cheryasov, D.; Safonov, Boris; Zharova, A. V.; Hancock, Terry

doi:10.1134/s1990341316010090

Cited by 26 publications

(27 citation statements)

References 26 publications

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“…Some examples are: onset of the CE, similar to the one witnessed for M31 2015LRN (MacLeod et al 2016; mass loss during turbulent phases of the stellar evolution (e.g., during the post He-burning phase); mass-loss events triggered by the passage of a lower-mass companion to the periastron and the subsequent shell-shell collision in very eccentric orbits; swallowing of planets by an expanding red giant (Retter & Marom 2003); mass-transferinduced jets, similar to the ones suggested for M31 2015 LRN and SN2015bh (Soker 2016;Soker & Kashi 2016); a faint terminal explosion or even thermal emission from shocks originated from the mass loss in the binary system (Pejcha et al 2016). The binary merger scenario proposed in this work, has also been presented by Goranskij et al (2016), who interpreted M101-OT as the ejection of a common envelope and the merger of a massive OB binary system.…”

Section: Discussionsupporting

confidence: 68%

Common Envelope Ejection for a Luminous Red Nova in M101

Blagorodnova

Kotak

Polshaw

et al. 2017

ApJ

121

167

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We present the results of optical, near-infrared, and mid-infrared observations of M101 OT2015-1 (PSN J14021678+5426205), a luminous red transient in the Pinwheel galaxy (M101), spanning a total of 16 years. The light curve showed two distinct peaks with absolute magnitudes, on 2014 November 11 and 2015 February 17, respectively. The spectral energy distributions during the second maximum show a cool outburst temperature of »3700 K and low expansion velocities (»-300 kms −1 ) for the H I, Ca II, Ba II, and K I lines. From archival data spanning 15-8 years before the outburst, we find a single source consistent with the optically discovered transient, which we attribute to being the progenitor; it has properties consistent with being an F-type yellow supergiant with L∼8.7´10 4 L e , » T 7000 eff K, and an estimated mass of =  M1 18 1 M e . This star has likely just finished the H-burning phase in the core, started expanding, and is now crossing the Hertzsprung gap. Based on the combination of observed properties, we argue that the progenitor is a binary system, with the more evolved system overfilling the Roche lobe. Comparison with binary evolution models suggests that the outburst was an extremely rare phenomenon, likely associated with the ejection of the common envelope of a massive star. The initial mass of the primary fills the gap between the merger candidates V838 Mon (5−10 M e ) and NGC4490-OT(30 M e ).

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Section: Discussionsupporting

confidence: 68%

Common Envelope Ejection for a Luminous Red Nova in M101

Blagorodnova

Kotak

Polshaw

et al. 2017

ApJ

121

167

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“…The light curve of M101-2015OT1 is extensively described in Goranskij et al (2016) and Blagorodnova et al (2017), and the new data provided here do not change the main outcomes. There are multiple detections of a stellar source before the main outburst, with the earliest detection being over 20 years before the discovery (B ≈ 22 mag, Goranskij et al 2016). A subsequent detection in 2000, shows the object roughly at the same luminosity, and with the following colours: B − V = 0.0 ± 0.3 mag and V − R = 0.7 ± 0.4 mag (Blagorodnova et al 2017).…”

Section: Individual Light Curvesmentioning

confidence: 69%

“…Blagorodnova et al (2017) argued that the progenitor was a binary system with a primary F-type yellow supergiant (T e f f ≈ 7000 K), with a luminosity of 8.7 × 10 4 L ⊙ , hence with M ≈ 16-18 M ⊙ , and a modestmass secondary companion. Goranskij et al (2016), on the basis of its proximity with nearby OB-supergiant associations, proposed a somewhat bluer progenitor. While a common envelope was surely ejected by the binary progenitor of M101-2015OT1, the post-outburst fate is uncertain, as the outcome can be either a merger or a surviving close binary (Blagorodnova et al 2017).…”

Section: Progenitors Of Luminous Double-peaked Transientsmentioning

confidence: 99%

Luminous red novae: Stellar mergers or giant eruptions?

Pastorello

Mason

Taubenberger

et al. 2019

A&A

108

125

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We present extensive datasets for a class of intermediate-luminosity optical transients known as "luminous red novae" (LRNe). They show doublepeaked light curves, with an initial rapid luminosity rise to a blue peak (at −13 to −15 mag), which is followed by a longer-duration red peak that sometimes is attenuated, resembling a plateau. The progenitors of three of them (NGC4490-2011OT1, M101-2015OT1, and SNhunt248), likely relatively massive blue to yellow stars, were also observed in a pre-eruptive stage when their luminosity was slowly increasing. Early spectra obtained during the first peak show a blue continuum with superposed prominent narrow Balmer lines, with P Cygni profiles. Lines of Fe II are also clearly observed, mostly in emission. During the second peak, the spectral continuum becomes much redder, Hα is barely detected, and a forest of narrow metal lines is observed in absorption. Very late-time spectra (∼6 months after blue peak) show an extremely red spectral continuum, peaking in the infrared (IR) domain. Hα is detected in pure emission at such late phases, along with broad absorption bands due to molecular overtones (such as TiO, VO). We discuss a few alternative scenarios for LRNe. Although major instabilities of single massive stars cannot be definitely ruled out, we favour a common envelope ejection in a close binary system, with possibly a final coalescence of the two stars. The similarity between LRNe and the outburst observed a few months before the explosion of the Type IIn SN 2011ht is also discussed.

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“…One of the sources identified as a candidate is PSN J14021678+5426205, which is believed to have been a stellar merger in M101 (Goranskij et al 2016;Blagorodnova et al 2016). PSN J14021678+5426205 satisfied all 3 of the criteria for new candidates (∆νLν < −10 4 L , νLν > 10 5 L for between 3 months and 3 years, and saturated at some point but νLν < 10 4 L in the final two epochs; see Fig.…”

Section: Psn J14021678+5426205mentioning

confidence: 99%

The search for failed supernovae with the Large Binocular Telescope: constraints from 7 yr of data

Adams

Kochanek

Gerke

et al. 2017

Monthly Notices of the Royal Astronomical Society

116

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We report updated results for the first 7 years of our program to monitor 27 galaxies within 10 Mpc using the Large Binocular Telescope to search for failed supernovae (SNe) -core-collapses of massive stars that form black holes without luminous supernovae. In the new data, we identify no new compelling candidates and confirm the existing candidate. Given the 6 successful core-collapse SNe in the sample and one likely failed SN, the implied fraction of core-collapses that result in failed SNe is f = 0.14 +0.33 −0.10 at 90% confidence. If the current candidate is a failed SN, the fraction of failed SN naturally explains the missing high-mass red supergiant SN progenitors and the black hole mass function. If the current candidate is ultimately rejected, the data implies a 90% confidence upper limit on the failed SN fraction of f < 0.35.

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Photometry and spectroscopy of the luminous red nova PSNJ14021678+5426205 in the galaxy M101

Cited by 26 publications

References 26 publications

Common Envelope Ejection for a Luminous Red Nova in M101

Common Envelope Ejection for a Luminous Red Nova in M101

Luminous red novae: Stellar mergers or giant eruptions?

The search for failed supernovae with the Large Binocular Telescope: constraints from 7 yr of data

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