Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631

Cai, Y. -Z.; Pastorello, A.; Fraser, M.; Wang, X. -F.; Filippenko, A. V.; Reguitti, A.; Patra, K. C.; Goranskij, V. P.; Barsukova, E. A.; Brink, T. G.; Elias-Rosa, N.; Zheng, W.; Yang, Y.; Atapin, K. E.; Benetti, S.; Boer, T. J. L. de; Bose, S.; Burke, J.; Byrne, R.; Cappellaro, E.; Chambers, K. C.; Chen, W. -L.; Emami, N.; Gao, H.; Hiramatsu, D.; Howell, D. A.; Huber, M. E.; Kankare, E.; Kelly, P. L.; R., Kotak,; Kravtsov, T.; Lander, V. Yu.; Li, Z. -T.; Lin, C. -C.; Lundqvist, P.; Magnier, E. A.; Malygin, E. A.; Maslennikova, N. A.; Matilainen, K.; Mazzali, P. A.; McCully, C.; Mo, J.; Moran, S.; Newsome, M.; Oparin, D. V.; González, E. P.; Reynolds, T. M.; I., Shatsky, N.; Smartt, S. J.; Smith, K. W.; Stritzinger, Maximilian; Татарников, А. М.; Terreran, G.; Uklein, R. I.; Valerin, G.; Vallely, P. J.; Vozyakova, O. V.; Wainscoat, R.; Yan, S. -Y.; Zhang, J. -J.; Zhang, T. -M.; Желтоухов, С. Г.; Dastidar, R.; Fulton, M.; Galbany, L.; Gangopadhyay, A.; Ge, H. -W.; Gutiérrez, C. P.; H., Lin,; Misra, K.; Ou, Z. -W.; Salmaso, I.; Tartaglia, L.; Xiao, L.; Zhang, X. -H.

doi:10.48550/arxiv.2207.00734

Cited by 7 publications

(23 citation statements)

References 73 publications

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“…Finally, the light curves settle to nearly constant magnitude in all bands (i = 22.80 ± 0.18 mag, hence M i = −6.92 ± 0.23 mag). We note that a similar red hump was observed at late phases in other LRNe, including AT 2021jfs (Pastorello et al 2019b) and AT 2021biy (Cai et al 2022).…”

Section: At 2021blusupporting

confidence: 83%

“…A comparison of the Sloan r absolute light curve for the three LRNe presented in this paper with that of AT 2021biy (Cai et al 2022) is presented in Fig. 6.…”

Section: At 2021blumentioning

confidence: 98%

“…Kochanek et al (2014) noted the existence of a possible correlation between the LRN absolute magnitude at maximum brightness and the progenitor mass, which was later confirmed by Blagorodnova et al (2021) based on a wider compilation of data from the literature. The analysis of Blagorodnova et al (2021) has been recently revised by Cai et al (2022), with different assumptions about the distance and the reddening, and after adopting Johnson-Bessell V as the reference band. Finally, Cai et al (2022) considered the magnitude of the second peak (or the plateau) instead of the magnitude of the first peak, as the former is likely dependent on the mass of the recombining hydrogen, while the latter is probably more sensitive to the parameters (mass and velocity) of the high-velocity gas ejected in the polar direction during the merging process (Metzger & Pejcha 2017).…”

Section: Blagorodnova Et Al (mentioning

confidence: 99%

“…In contrast to the monitoring campaigns of other LRNe in our program (Pastorello et al 2021a,b), the follow-up campaigns of these two objects were not significantly affected by the COVID-19 pandemic restrictions to our access to observational facilities. This study is complemented by a companion paper focused on the detailed analysis of another LRN monitored during the same period, AT 2021biy (Cai et al 2022).…”

Section: Introductionmentioning

confidence: 99%

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Panchromatic evolution of three luminous red novae: Forbidden hugs in pandemic times -- IV

Pastorello¹,

Valerin²,

Fraser³

et al. 2022

Preprint

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We present photometric and spectroscopic data on three extragalactic luminous red novae (LRNe): AT 2018bwo, AT 2021afy, and AT 2021blu. AT 2018bwo was discovered in NGC 45 (at about 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 −1 . AT 2021afy, hosted by UGC 10043 (∼ 49.2 Mpc), showed a double-peaked light curve, with an early maximum reaching a luminosity of 2.1 × 10 41 erg s −1 . Finally, for AT 2021blu in UGC 5829 (∼ 8.6 Mpc), the pre-outburst phase was wellmonitored by several photometric surveys, and the object showed a slow luminosity rise before the outburst. The light curve of AT 2021blu was sampled with an unprecedented cadence until the object disappeared behind the Sun, and was then recovered at late phases. The light curve of LRN AT 2021blu shows a double peak, with a prominent early maximum reaching a luminosity of 6.5 × 10 40 erg s −1 , half that of AT 2021afy. The spectra of AT 2021afy and AT 2021blu 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 AT 2018bwo 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, probably AT 2018bwo was 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 about 13 M ⊙ for AT 2018bwo, to 14 +4 −1 M ⊙ for AT 2021blu, and over 40 M ⊙ for AT 2021afy.

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Section: At 2021blusupporting

confidence: 83%

“…A comparison of the Sloan r absolute light curve for the three LRNe presented in this paper with that of AT 2021biy (Cai et al 2022) is presented in Fig. 6.…”

Section: At 2021blumentioning

confidence: 98%

Section: Blagorodnova Et Al (mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Panchromatic evolution of three luminous red novae: Forbidden hugs in pandemic times -- IV

Pastorello¹,

Valerin²,

Fraser³

et al. 2022

Preprint

Self Cite

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“…Some ILOTs are known to be powered by jets because of their bipolar morphology, e.g., Nova 1670 (CK Vulpec-ulae; Kamiński et al 2021). I therefore raise the possibility that the sharp bump in the light curve of the luminous red novae (ILOT) AT 2021biy at about 330 to 400 days post maximum (Cai et al 2022) was powered by jets.…”

Section: Powering the Bump With Jetsmentioning

confidence: 97%

Pre-explosion, explosion, and post-explosion jets in supernova SN 2019zrk

Soker

2022

Preprint

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I analyse some properties of the luminous transient event SN 2019zrk and conclude that jets were the main powering sources of the pre-explosion outburst (pre-cursor) and ejection of a massive circumstellar matter (CSM), of the very energetic explosion itself, and of the post-explosion bump in the light curve. The pre-explosion energy source is mainly a companion (main sequence, Wolf-Rayet, neutron star or black hole) star that accreted mass and launched jets. I find that the fast expansion of the CSM after acceleration by the explosion ejecta requires the explosion energy to be 10 52 erg. Only jetdriven explosions can supply this energy in such SN 2009ip-like transients. I conclude that ejecta-CSM interaction is extremely unlikely to power the bright bump at about 110 days after explosion. Instead, I show by applying a jet-driven bump toy-model that post-explosion jets are the most likely explanation for the bump. I leave open the question of whether the explosion itself (main outburst) was a core collapse supernova (CCSN) or a common envelope jets supernova (CEJSN). In this study I further connect peculiar transient events, here 2009ip-like transient events, to CCSNe by arguing that jets drive all events, from regular CCSNe through superluminous CCSNe and to many other peculiar and super-energetic transient events, including CEJSNe. Jet-powering cannot be ignored when analyzing all these types of transients.

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An infrared transient from a star engulfing a planet

MacLeod

Karambelkar

et al. 2023

Nature

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It is well known that planets with short orbital periods (≲ 10 days) are common around stars like the Sun 1-3 . Stars expand as they evolve, and thus we expect their close planetary companions to be engulfed [4][5][6] . However, this phase has never been directly observed. Here, we present the discovery of ZTF SLRN-2020, a short-lived optical outburst in the Galactic disk accompanied by bright and long-lived infrared emission. The resulting light curve and spectra share striking similarities with those of red novae 7, 8 -a class of eruptions now confirmed 9 to arise from mergers of binary stars. Its exceptionally low optical luminosity (≈ 10 35 erg s −1 ) and radiated energy (≈ 6.5 × 10 41 erg) point to the engulfment of a planet (of 1 − 10 Jupiter masses) by its Sun-like host star. We estimate the Galactic rate of such Sub-luminous Red Novae (SLRNe) to be ∼ 0.1−few yr −1 . Future Galactic plane surveys are well-poised to routinely identify them, revealing the demographics of planetary engulfment and the ultimate fate of planets in the inner Solar System.Using data from the Zwicky Transient Facility (ZTF) time domain survey 10 , we searched 2 for slowly evolving outbursts near the Galactic plane (Methods). We identified a transient optical source named ZTF 20aazusyv (hereafter ZTF SLRN-2020) that exhibited a fast rise from quiescence to peak outburst flux in ≈ 10 days, subsequently fading by ≈ 10× over six months (Figure 1).The long optical outburst duration together with its faint peak flux distinguishes it from common Galactic plane transients resulting from white dwarfs with close binary companions (the 'dwarf' and 'classical' novae 11 ). The transient also exhibits a mid-IR brightening starting ≈ 7 months prior to the optical outburst, together with bright mid-infrared (IR) emission (> 50× brighter than the optical r-band at ≈ 4 months after optical peak) that lasted for ≳ 15 months. No X-ray emission was detected in follow-up observations during the outburst using the Swift telescope 12 , ruling out an unstable disk accretion episode around a neutron star or black hole 13 (Methods).The bright mid-IR emission during the outburst is suggestive of emission from a warm dust shell surrounding the stellar photosphere. We model the optical to mid-IR spectral energy distribution (SED; Methods) at ≈ 120 days after the optical peak. The analysis reveal a relatively hot inner photosphere (≈ 9000 K) surrounded by a warm dust shell with temperature ≈ 1000 K, located behind a dust visual extinction column of A V ≈ 3.6 mag (Figure 2). Using the 90% confidence interval on the foreground extinction together with three-dimensional Galactic dust distribution maps (Methods), we infer the source to be located at a distance of 2 to 7 kpc. A joint analysis of the overlap between the different dust maps suggests a likely distance of ≈ 4 kpc (Methods). Performing the same analysis at ≈ 320 days after peak, we find the SED to have predominantly shifted into the IR bands caused by an increase in the dust optical depth, that can be att...

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Observations of the luminous red nova AT 2021biy in the nearby galaxy NGC 4631

Cited by 7 publications

References 73 publications

Panchromatic evolution of three luminous red novae: Forbidden hugs in pandemic times -- IV

Panchromatic evolution of three luminous red novae: Forbidden hugs in pandemic times -- IV

Pre-explosion, explosion, and post-explosion jets in supernova SN 2019zrk

An infrared transient from a star engulfing a planet

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