학술논문
The Birth of a Relativistic Jet Following the Disruption of a Star by a Cosmological Black Hole
Document Type
Working Paper
Author
Pasham, Dheeraj R.; Lucchini, Matteo; Laskar, Tanmoy; Gompertz, Benjamin P.; Srivastav, Shubham; Nicholl, Matt; Smartt, Stephen J.; Miller-Jones, James C. A.; Alexander, Kate D.; Fender, Rob; Smith, Graham P.; Fulton, Michael D.; Dewangan, Gulab; Gendreau, Keith; Coughlin, Eric R.; Rhodes, Lauren; Horesh, Assaf; van Velzen, Sjoert; Sfaradi, Itai; Guolo, Muryel; Segura, N. Castro; Aamer, Aysha; Anderson, Joseph P.; Arcavi, Iair; Brennan, Sean J.; Chambers, Kenneth; Charalampopoulos, Panos; Chen, Ting-Wan; Clocchiatti, A.; de Boer, Thomas; Dennefeld, Michel; Ferrara, Elizabeth; Galbany, Lluis; Gao, Hua; Gillanders, James H.; Goodwin, Adelle; Gromadzki, Mariusz; Huber, M; Jonker, Peter G.; Joshi, Manasvita; Kara, Erin; Killestein, Thomas L.; Kosec, Peter; Kocevski, Daniel; Leloudas, Giorgos; Lin, Chien-Cheng; Margutti, Raffaella; Mattila, Seppo; Moore, Thomas; Muller-Bravo, Tomas; Ngeow, Chow-Choong; Oates, Samantha; Onori, Francesca; Pan, Yen-Chen; Perez-Torres, Miguel; Rani, Priyanka; Remillard, Ronald; Ridley, Evan J.; Schulze, Steve; Sheng, Xinyue; Shingles, Luke; Smith, Ken W.; Steiner, James; Wainscoat, Richard; Wevers, Thomas; Yang, Sheng
Source
Subject
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Abstract
A black hole can launch a powerful relativistic jet after it tidally disrupts a star. If this jet fortuitously aligns with our line of sight, the overall brightness is Doppler boosted by several orders of magnitude. Consequently, such on-axis relativistic tidal disruption events (TDEs) have the potential to unveil cosmological (redshift $z>$1) quiescent black holes and are ideal test beds to understand the radiative mechanisms operating in super-Eddington jets. Here, we present multi-wavelength (X-ray, UV, optical, and radio) observations of the optically discovered transient \target at $z=1.193$. Its unusual X-ray properties, including a peak observed luminosity of $\gtrsim$10$^{48}$ erg s$^{-1}$, systematic variability on timescales as short as 1000 seconds, and overall duration lasting more than 30 days in the rest-frame are traits associated with relativistic TDEs. The X-ray to radio spectral energy distributions spanning 5-50 days after discovery can be explained as synchrotron emission from a relativistic jet (radio), synchrotron self-Compton (X-rays), and thermal emission similar to that seen in low-redshift TDEs (UV/optical). Our modeling implies a beamed, highly relativistic jet akin to blazars but requires extreme matter-domination, i.e, high ratio of electron-to-magnetic field energy densities in the jet, and challenges our theoretical understanding of jets.
Comment: To appear in Nature Astronomy on 30th November 2022. Also see here for an animation explaining the result: https://youtu.be/MQHdSbxuznY
Comment: To appear in Nature Astronomy on 30th November 2022. Also see here for an animation explaining the result: https://youtu.be/MQHdSbxuznY