Photometric and spectroscopic evolution of the interacting transient AT 2016jbu(Gaia16cfr)

Brennan, S.; Fraser, M.; Johansson, Joel; Pastorello, A.; Kotak, R.; Stevance, H. F.; Chen, T.-W.; Eldridge, J. J.; Bose, Smarajit; Brown, Pamela J.; Callis, E.; Cartier, R.; Dennefeld, M.; Dong, Subo; Duffy, P.; Elias‐Rosa, N.; Hosseinzadeh, G.; Hsiao, E. Y.; Kuncarayakti, H.; Martín-Carrillo, A.; Monard, B.; Nyholm, A.; Pignata, G.; Sand, David J.; Shappee, B.J.; Smartt, S. J.; Tucker, B. E.; Wyrzykowski, Ł.; Abbot, Harrison; Benetti, S.; Bento, J.; Blondin, S.; Chen, Ping; Delgado, A.; Galbany, L.; Gromadzki, M.; Gutiérrez, C. P.; Hanlon, L.; Harrison, D. L.; Hiramatsu, D.; Hodgkin, S. T.; Holoien, T.; Howell, D. A.; Inserra, C.; Kankare, E.; Lowski, S. Koz; Müller-Bravo, T. E.; Maguire, K.; McCully, C.; Meintjes, P. J.; Morrell, N.; Nicholl, M.; Oneill, D.M.; Pietrukowicz, P.; Poleski, R.; Prieto, J. L.; Rau, A.; Reichart, D.; Schweyer, T.; Shahbandeh, Melissa; Skowron, J.; Sollerman, J.; Soszyński, I.; Stritzinger, M.; Szymański, Mikołaj; Tartaglia, L.; Udalski, A.; Ulaczyk, K.; Young, D. R.; Leeuwen, M. van; Soelen, B. van

doi:10.1093/mnras/stac1243

Cited by 19 publications

(12 citation statements)

References 98 publications

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“…Altogether, these features indicate the continued influence of interaction with asymmetric CSM (Elias-Rosa et al 2016;Thöne et al 2017). Strong Hα emission and signs of CSM interaction at late phases appear to be ubiquitous in objects similar to SN 2015bh, including SN 2009ip through at least 726-1196 days after peak (Fraser et al 2015;Smith et al 2016), AT 2016jbu up to 419 days after peak (Brennan et al 2022a), and SN 2011fh up to 1359 days after peak (Pessi et al 2022). As noted too by Kilpatrick et al (2018), the doublepeaked, asymmetric Hα profiles of AT 2016jbu and SN 2015bh at late times are particularly similar.…”

Section: Ongoing Circumstellar Interactionmentioning

confidence: 82%

Hubble Space Telescope Imaging Reveals that SN 2015bh is Much Fainter than its Progenitor

Jencson,

Sand,

Andrews

et al. 2022

Preprint

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We present Hubble Space Telescope (HST) imaging of the site of SN 2015bh in the nearby spiral galaxy NGC 2770 taken between 2017 and 2019, nearly four years after the peak of the explosion. In 2017-2018, the transient fades steadily in optical filters before declining more slowly to F 814W = −7.2 mag in 2019, nearly 4 mag below the level of its eruptive luminous blue variable (LBV) progenitor observed with HST in 2008-2009. The source fades at a constant color of F 555W − F 814W = 0.3 mag until 2018, similar to SN 2009ip and consistent with a spectrum dominated by continued interaction of the ejecta with circumstellar material (CSM). A deep optical spectrum obtained in 2021 lacks signatures of ongoing interaction (L Hα 10 39 erg s −1 for broadened emission 2000 km s −1 ), but but indicates the presence of a nearby H II region ( 300 pc). The color evolution of the fading source makes it unlikely that emission from a scattered light echo or binary OB companion of the progenitor contributes significantly to the flattening of the late-time light curve. The remaining emission in 2019 may plausibly be attributed to an unresolved ( 3 pc), young stellar cluster. Importantly, the color evolution of SN 2015bh also rules out scenarios in which the surviving progenitor evolves back to a hot, quiescent, optically faint state or is obscured by nascent dust. The simplest explanation is that the massive progenitor did not survive. SN 2015bh, therefore, likely represents a remarkable example of the terminal explosion of a massive star preceded by decades of end-stage eruptive variability.

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Section: Ongoing Circumstellar Interactionmentioning

confidence: 82%

Hubble Space Telescope Imaging Reveals that SN 2015bh is Much Fainter than its Progenitor

Jencson,

Sand,

Andrews

et al. 2022

Preprint

View full text Add to dashboard Cite

show abstract

“…Altogether, these features indicate the continued influence of interaction with asymmetric CSM (Elias-Rosa et al 2016; Thöne et al 2017). Strong Hα emission and signs of CSM interaction at late phases appear to be ubiquitous in objects similar to SN 2015bh, including SN 2009ip through at least 726-1196 days after peak (Fraser et al 2015;Smith et al 2016a), AT 2016jbu up to 419 days after peak (Brennan et al 2022b), and SN 2011fh up to 1359 days after peak (Pessi et al 2022). As noted too by Kilpatrick et al (2018), the doublepeaked asymmetric Hα profiles of AT 2016jbu and SN 2015bh at late times are particularly similar.…”

Section: Ongoing Circumstellar Interactionmentioning

confidence: 93%

“…Monitoring of the event revealed the presence of dense, complex CSM (Graham et al 2014;Margutti et al 2014;Mauerhan et al 2014;Martin et al 2015), possibly with a disk-like geometry pointing to the influence of binary interactions (e.g., Mauerhan et al 2013Mauerhan et al , 2014Levesque et al 2014;Smith 2014;Reilly et al 2017). A class of objects with similar properties has been identified in recent years, including SN 2010mc (Ofek et al 2013;Smith et al 2013), LSQ13zm (Tartaglia et al 2016), AT 2016jbu (or Gaia16crf; Kilpatrick et al 2018;Brennan et al 2022bBrennan et al , 2022c, SN 2016bdu (Pastorello et al 2018), and the main subject of this work, SN 2015bh (Elias-Rosa et al 2016;Ofek et al 2016;Thöne et al 2017).…”

Section: Introductionmentioning

confidence: 95%

Hubble Space Telescope Imaging Reveals That SN 2015bh Is Much Fainter than Its Progenitor

Jencson

Sand

Andrews

et al. 2022

ApJL

View full text Add to dashboard Cite

We present Hubble Space Telescope (HST) imaging of the site of SN 2015bh in the nearby spiral galaxy NGC 2770 taken between 2017 and 2019, nearly four years after the peak of the explosion. In 2017–2018, the transient fades steadily in optical filters before declining more slowly to F814W = −7.1 mag in 2019, ≈4 mag below the level of its eruptive luminous blue variable (LBV) progenitor observed with HST in 2008–2009. The source fades at a constant color of F555W − F814W = 0.4 mag until 2018, similar to SN 2009ip and consistent with a spectrum dominated by interaction of the ejecta with circumstellar material (CSM). A deep optical spectrum obtained in 2021 lacks signatures of ongoing interaction (L Hα ≲ 1038 erg s−1 for broadened emission ≲2000 km s−1), but indicates the presence of a nearby H ii region (≲300 pc). The color evolution of the fading source makes it unlikely that emission from a scattered-light echo or binary OB companion of the progenitor contributes significantly to the flattening of the late-time light curve. The remaining emission in 2019 may plausibly be attributed an evolved/inflated companion or an unresolved (≲3 pc), young stellar cluster. Importantly, the color evolution of SN 2015bh rules out scenarios in which the surviving progenitor is obscured by nascent dust and does not clearly indicate a transition to a hotter, optically faint state. The simplest explanation is that the massive progenitor did not survive. SN 2015bh likely represents a remarkable example of the terminal explosion of a massive star preceded by decades of end-stage eruptive variability.

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“…The late-time decline rate of the light curves is shallower than the one expected from simple 56 Co decay, therefore suggesting the presence of an additional powering source in the form of CSM interaction. Data from Smith and Frew [39], Frew [45], Foley et al [46], Smith et al [47], Pastorello et al [48][49][50][51], Fraser et al [52,53], Brennan et al [54,55], Reguitti et al [56].…”

Section: Supernova Impostorsmentioning

confidence: 99%

Gap Transients Interacting with Circumstellar Medium

2022

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In the last 20 years, modern wide-field surveys discovered a new class of peculiar transients, which lie in the luminosity gap between standard supernovae and classical novae. These transients are often called “intermediate luminosity optical transients” or “gap transients”. They are usually distinguished in subgroups based on their phenomenology, such as supernova impostors, intermediate luminosity red transients, and luminous red novae. In this review, we present a brief overview of their observational features and possible physical scenarios to date, in the attempt to understand their nature.

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Photometric and spectroscopic evolution of the interacting transient AT 2016jbu(Gaia16cfr)

Cited by 19 publications

References 98 publications

Hubble Space Telescope Imaging Reveals that SN 2015bh is Much Fainter than its Progenitor

Hubble Space Telescope Imaging Reveals that SN 2015bh is Much Fainter than its Progenitor

Hubble Space Telescope Imaging Reveals That SN 2015bh Is Much Fainter than Its Progenitor

Gap Transients Interacting with Circumstellar Medium

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