A very luminous jet from the disruption of a star by a massive black hole,Nature

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A very luminous jet from the disruption of a star by a massive black hole
Nature ( IF 64.8 ) Pub Date : 2022-11-30 , DOI: 10.1038/s41586-022-05465-8
Igor Andreoni _{1,

2,

3} , Michael W Coughlin ₄ , Daniel A Perley ₅ , Yuhan Yao ₆ , Wenbin Lu ₇ , S Bradley Cenko _{1,

3} , Harsh Kumar ₈ , Shreya Anand ₆ , Anna Y Q Ho _{9,

10,

11} , Mansi M Kasliwal ₆ , Antonio de Ugarte Postigo ₁₂ , Ana Sagués-Carracedo ₁₃ , Steve Schulze ₁₃ , D Alexander Kann ₁₄ , S R Kulkarni ₆ , Jesper Sollerman ₁₅ , Nial Tanvir ₁₆ , Armin Rest _{17,

18} , Luca Izzo ₁₉ , Jean J Somalwar ₆ , David L Kaplan ₂₀ , Tomás Ahumada ₂ , G C Anupama ₂₁ , Katie Auchettl _{22,

23,

24} , Sudhanshu Barway ₂₁ , Eric C Bellm ₂₅ , Varun Bhalerao ₈ , Joshua S Bloom _{9,

10} , Michael Bremer ₂₆ , Mattia Bulla ₁₅ , Eric Burns ₂₇ , Sergio Campana ₂₈ , Poonam Chandra ₂₉ , Panos Charalampopoulos ₃₀ , Jeff Cooke _{31,

32} , Valerio D'Elia ₃₃ , Kaustav Kashyap Das ₆ , Dougal Dobie _{31,

32} , José Feliciano Agüí Fernández ₁₄ , James Freeburn _{31,

32} , Cristoffer Fremling ₆ , Suvi Gezari ₁₇ , Simon Goode _{31,

32} , Matthew J Graham ₆ , Erica Hammerstein ₂ , Viraj R Karambelkar ₆ , Charles D Kilpatrick ₃₄ , Erik C Kool ₁₅ , Melanie Krips ₂₆ , Russ R Laher ₃₅ , Giorgos Leloudas ₃₀ , Andrew Levan ₃₆ , Michael J Lundquist ₃₇ , Ashish A Mahabal _{6,

38} , Michael S Medford _{9,

10} , M Coleman Miller _{1,

2} , Anais Möller _{31,

32} , Kunal P Mooley ₆ , A J Nayana ₃₉ , Guy Nir ₉ , Peter T H Pang _{40,

41} , Emmy Paraskeva _{42,

43,

44,

45} , Richard A Perley ₄₆ , Glen Petitpas ₄₇ , Miika Pursiainen ₃₀ , Vikram Ravi ₆ , Ryan Ridden-Harper ₄₈ , Reed Riddle ₄₉ , Mickael Rigault ₅₀ , Antonio C Rodriguez ₆ , Ben Rusholme ₃₅ , Yashvi Sharma ₆ , I A Smith ₅₁ , Robert D Stein ₆ , Christina Thöne ₅₂ , Aaron Tohuvavohu ₅₃ , Frank Valdes ₅₄ , Jan van Roestel ₆ , Susanna D Vergani _{55,

56} , Qinan Wang ₁₇ , Jielai Zhang _{31,

32}

Affiliation

Joint Space-Science Institute, University of Maryland, College Park, MD, USA.
Department of Astronomy, University of Maryland, College Park, MD, USA.
Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA.
School of Physics and Astronomy, University of Minnesota, Minneapolis, MN, USA.
Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK.
Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA.
Department of Astrophysical Sciences, Princeton University, Princeton, NJ, USA.
Indian Institute of Technology Bombay, Mumbai, India.
Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.
Lawrence Berkeley National Laboratory, Berkeley, CA, USA.
Miller Institute for Basic Research in Science, Berkeley, CA, USA.
Artemis, Université Côte d'Azur, Observatoire de la Côte d'Azur, CNRS, Nice, France.
The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, Sweden.
Instituto de Astrofísica de Andalucía, Granada, Spain.
The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden.
Department of Physics and Astronomy, University of Leicester, Leicester, UK.
Space Telescope Science Institute, Baltimore, MD, USA.
Department of Physics and Astronomy, The Johns Hopkins University, Baltimore, MD, USA.
DARK, Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark.
Center for Gravitation, Cosmology and Astrophysics, Department of Physics, University of Wisconsin-Milwaukee, Milwaukee, WI, USA.
Indian Institute of Astrophysics, Bangalore, India.
School of Physics, University of Melbourne, Parkville, Victoria, Australia.
ARC Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D), Sydney, Australia.
Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA.
DIRAC Institute, Department of Astronomy, University of Washington, Seattle, WA, USA.
Institut de Radioastronomie Millimétrique (IRAM), Saint Martin d'Hères, France.
Department of Physics & Astronomy, Louisiana State University, Baton Rouge, LA, USA.
INAF-Osservatorio Astronomico di Brera, Merate, Italy.
National Centre for Radio Astrophysics, Tata Institute of Fundamental Research, Pune, India.
DTU Space, National Space Institute, Technical University of Denmark, Kongens Lyngby, Denmark.
Australian Research Council Centre of Excellence for Gravitational Wave Discovery (OzGrav), Swinburne University of Technology, Hawthorn, Victoria, Australia.
Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, Victoria, Australia.
Space Science Data Center - Agenzia Spaziale Italiana, Rome, Italy.
Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA), Northwestern University, Evanston, IL, USA.
IPAC, California Institute of Technology, Pasadena, CA, USA.
Department of Astrophysics, Radboud University, Nĳmegen, The Netherlands.
W. M. Keck Observatory, Kamuela, HI, USA.
Center for Data-Driven Discovery, California Institute of Technology, Pasadena, CA, USA.
Indian Institute of Astrophysics, Bengaluru, India.
Nikhef, Amsterdam, The Netherlands.
Institute for Gravitational and Subatomic Physics (GRASP), Utrecht University, Utrecht, The Netherlands.
IAASARS, National Observatory of Athens, Penteli, Greece.
Department of Astrophysics, Astronomy and Mechanics, Faculty of Physics, National and Kapodistrian University of Athens, Athens, Greece.
Nordic Optical Telescope, Breña Baja, Spain.
Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark.
National Radio Astronomy Observatory, Socorro, NM, USA.
Center for Astrophysics - Harvard & Smithsonian, Cambridge, MA, USA.
School of Physical and Chemical Sciences ∣ Te Kura Matū, University of Canterbury, Christchurch, New Zealand.
Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA.
Université Lyon, Université Claude Bernard Lyon 1, CNRS, IP2I Lyon / IN2P3, IMR 5822, Villeurbanne, France.
Institute for Astronomy, University of Hawai'i, Pukalani, HI, USA.
Astronomical Institute of the Czech Academy of Sciences (ASU-CAS), Ondřejov, Czech Republic.
Department of Astronomy and Astrophysics, University of Toronto, Toronto, Ontario, Canada.
National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ, USA.
GEPI, Observatoire de Paris, PSL University, CNRS, Meudon, France.
Institut d'Astrophysique de Paris, CNRS-UPMC, UMR7095, Paris, France.

Tidal disruption events (TDEs) are bursts of electromagnetic energy that are released when supermassive black holes at the centres of galaxies violently disrupt a star that passes too close¹. TDEs provide a window through which to study accretion onto supermassive black holes; in some rare cases, this accretion leads to launching of a relativistic jet^{2,3,4,5,6,7,8,9}, but the necessary conditions are not fully understood. The best-studied jetted TDE so far is Swift J1644+57, which was discovered in γ-rays, but was too obscured by dust to be seen at optical wavelengths. Here we report the optical detection of AT2022cmc, a rapidly fading source at cosmological distance (redshift z = 1.19325) the unique light curve of which transitioned into a luminous plateau within days. Observations of a bright counterpart at other wavelengths, including X-ray, submillimetre and radio, supports the interpretation of AT2022cmc as a jetted TDE containing a synchrotron ‘afterglow’, probably launched by a supermassive black hole with spin greater than approximately 0.3. Using four years of Zwicky Transient Facility¹⁰ survey data, we calculate a rate of \(0.0{2}_{-0.01}^{+0.04}\) per gigapascals cubed per year for on-axis jetted TDEs on the basis of the luminous, fast-fading red component, thus providing a measurement complementary to the rates derived from X-ray and radio observations¹¹. Correcting for the beaming angle effects, this rate confirms that approximately 1 per cent of TDEs have relativistic jets. Optical surveys can use AT2022cmc as a prototype to unveil a population of jetted TDEs.

中文翻译：

一颗恒星被大质量黑洞破坏后产生的非常明亮的射流

潮汐瓦解事件 (TDE) 是当星系中心的超大质量黑洞猛烈瓦解一颗距离太近的恒星时释放的电磁能量爆发¹。TDE 提供了一个窗口，通过它可以研究超大质量黑洞的吸积；在极少数情况下，这种吸积会导致相对论射流^{2,3,4,5,6,7,8,9}的发射，但必要条件尚不完全清楚。迄今为止研究最好的喷射式 TDE 是 Swift J1644+57，它是在 γ 射线中发现的，但被尘埃遮挡得太多，无法在光学波长下看到。在这里，我们报告了 AT2022cmc 的光学探测，这是一个在宇宙学距离（红移z = 1.19325) 独特的光变曲线在几天内转变为发光平台。对其他波长（包括 X 射线、亚毫米和无线电）的明亮对应物的观察支持将 AT2022cmc 解释为包含同步加速器“余辉”的喷射式 TDE，可能由自旋大于约 0.3 的超大质量黑洞发射。使用四年的 Zwicky 瞬态设施10^调查数据，我们根据发光的、快速消退的红色成分，从而提供与 X 射线和无线电观测^{11得出的速率互补的测量}. 校正光束角效应后，该比率证实大约 1% 的 TDE 具有相对论性喷流。光学调查可以使用 AT2022cmc 作为原型来揭示大量喷射式 TDE。

更新日期：2022-11-30

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