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The peculiar transient AT2018cow: A possible origin of A type Ibn/IIn supernova

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arXiv 2021年

作者： Xiang, Danfeng Wang, Xiaofeng Lin, Weili Mo, Jun Lin, Han Burke, Jamison Hiramatsu, Daichi Hosseinzadeh, Griffin Howell, D. Andrew McCully, Curtis Valenti, Stefan Vinkó, József Wheeler, J. Craig Ehgamberdiev, Shuhrat A. Mirzaqulov, Davron Bódi, Attila Bognár, Zsófia Cseh, Borbála Hanyecz, Ottó Ignácz, Bernadett Kalup, Csilla Könyves-Tóth, Réka Kriskovics, Levente Ordasi, András Pál, András Sárneczky, Krisztián Seli, Bálint Szakáts, Róbert Arranz-Heras, T. Benavides-Palencia, R. Cejudo-Martínez, D. de la Fuente-Fernández, P. Escartín-Pérez, A. la Cuesta, F. García-De González-Carballo, J.L. González-Farfán, R. Limón-Martínez, F. Mantero, A. Naves-Nogués, R. Morales-Aimar, M. Ruíz-Ruíz, V.R. Soldán-Alfaro, F.C. Valero-Pérez, J. Violat-Bordonau, F. Zhang, Tianmeng Zhang, Jujia Li, Xue Chen, Zhihao Sai, Hanna Li, Wenxiong Tsinghua University Beijing100084 China Beijing Planetarium Beijing Academy of Sciences and Technology Beijing100044 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210023 China Las Cumbres Observatory 6740 Cortona Drive Suite 102 GoletaCA93117-5575 United States Department of Physics University of California Santa BarbaraCA93106-9530 United States Center for Astrophysics | Harvard & Smithsonian 60 Garden Street CambridgeMA02138-1516 United States Department of Physics and Astronomy University of California 1 Shields Avenue DavisCA95616-5270 United States Konkoly Observatory Research Centre for Astronomy and Earth Sciences Konkoly-Thege M. út 15-17 Budapest1121 Hungary ELTE Eötvös Loránd University Institute of Physics Pázmany Péter sétány 1/A Budapest1117 Hungary Department of Optics & Quantum Electronics University of Szeged Dóm tér 9 Szeged6720 Hungary Department of Astronomy University of Texas at Austin AustinTX78712 United States Ulugh Beg Astronomical Institute Uzbekistan Academy of Sciences Uzbekistan Tashkent100052 Uzbekistan CSFK Lendület Near-Field Cosmology Research Group Eötvös Loránd University Institute of Physics Pázmany Péter sétány 1/A Budapest1117 Hungary Eötvös Loránd University Department of Astronomy Pázmany Péter sétány 1/A Budapest1117 Hungary Spain Obs. Las Pequeras Navas de Oro Segovia40470 Spain Obs. Posadas MPC J53 Posadas Córdoba14730 Spain Obs. El Gallinero El Berrueco Madrid28192 Spain Obs. Llanes Llanes Asturias33784 Spain Obs. Belako Mungia Vizcaya48100 Spain Obs. La Vara MPC J38 Muñas de Arriba Asturias33784 Spain Obs. Cerro del Viento MPC I84 Badajoz06010 Spain Obs. Uraniborg MPC Z55 Écija Sevilla41400 Spain Obs. Mazariegos MPC I99 Mazariegos Palencia34170 Spain Obs. Bernezzo MPC C77 Bernezzo Cuneo12010 Italy Obs. Montcabrer MPC 213 Cabrils Barcelona08348 Spain Obs. Sencelles MPC K14 Sencelles Islas Baleares07140 Spain New Mexico Skies Unit

We present our photometric and spectroscopic observations on the peculiar transient AT2018cow. The multi-band photometry covers from peak to ∼70 days and the spectroscopy ranges from 5 to ∼50 days. The rapid rise (tr.2.9 days), high luminosity (MVpeak ∼ −20.8 mag) and fast decline after peak make AT2018cow stand out of any other optical transients. While we find that its light curves show high resemblance to those of type Ibn supernovae. Moreover, the spectral energy distribution remains high temperature of ∼14,000 K after ∼15 days since discovery. The spectra are featureless in the first 10 days, while some broad emission lines due to H, He, C and O emerge later, with velocity declining from ∼ 14, 000 km s−1 to ∼3000 km s−1 at the end of our observations. Narrow and weak He I emission lines emerge in the spectra at t >20 days since discovery. These emission lines are reminiscent of the features seen in interacting supernovae like type Ibn and IIn subclasses. We fit the bolometric light curves with a model of circumstellar interaction (CSI) and radioactive decay (RD) of 56Ni and find a good fit with ejecta mass Mej ∼ 3.16 M☉, circumstellar material mass MCSM ∼ 0.04 M☉, and ejected 56Ni mass M56Ni ∼ 0.23 M☉. The CSM shell might be formed in an eruptive mass ejection of the progenitor star. Furthermore, host environment of AT2018cow implies connection of AT2018cow with massive stars. Combining observational properties and the light curve fitting results, we conclude that AT2018cow might be a peculiar interacting supernova originated from a massive star. © 2021, CC BY.

关键词： Electromagnetic wave emission

A 34.5 day quasi-periodic oscillation in γ-ray emission from the blazar PKS 2247–131

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arXiv 2018年

作者： Zhou, Jianeng Wang, Zhongxiang Chen, Liang Wiita, Paul J. Vadakkumthani, Jithesh Morrell, Nidia Zhang, Pengfei Zhang, Jujia Shanghai Astronomical Observatory Chinese Academy of Sciences 80 Nandan Road Shanghai200030 China University of Chinese Academy of Sciences 19A Yuquan Road Beijing100049 China The College of New Jersey 2000 Pennington Road EwingNJ 08628-0718 United States Inter-University Centre for Astronomy and Astrophysics Pune411 007 India Las Campanas Observatory Carnegie Observatories Casilla 601 La Serena 1700000 Chile Purple Mountain Observatory Chinese Academy of Sciences 8 Yuanhua Road Nanjing210034 China Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road BeijingChaoyang District100012 China

Since 2016 October, the active galaxy PKS 2247−131 has undergone a γ-ray outburst, which we studied using data obtained with the Fermi Gamma-ray Space Telescope. The emission arises from a relativistic jet in PKS 2247−131, as an optical spectrum only shows a few weak absorption lines, typical of the BL Lacertae sub-class of the blazar class of active galactic nuclei. Here we report a 34.5 day quasi-periodic oscillation (QPO) in the emission after the initial flux peak of the outburst. Compared to one-year time-scale QPOs, previously identified in blazars in Fermi energies, PKS 2247−131 exhibits the first clear case of a relatively short, month-like oscillation. We show that this QPO can be explained in terms of a helical structure in the jet, where the viewing angle to the dominant emission region in the jet undergoes periodic changes. The time scale of the QPO suggests the presence of binary supermassive black holes in PKS 2247−131. Copyright © 2018, The Authors. All rights reserved.

关键词： Absorption spectroscopy

The extraneous eclipses on binary light curves: KIC 5255552, KIC 10091110, and KIC 11495766

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arXiv 2017年

作者： Zhang, J. Qian, S.B. Wang, S.M. Sun, L.L. Wu, Y. Jiang, L.Q. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of Mathematics and Physics Handan University Handan056005 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Physics and Electronic Engineering Sichuan University of Science ＆Engineering Zigong643000 China

Aims. We aim to find more eclipsing multiple systems and obtain their parameters, thus increasing our understanding of multiple systems. Methods. The extraneous eclipses on the kepler binary light curves indicating extraneous bodies were searched. The binary light curves were analyzed using the binary model, and the extraneous eclipses were studied on their periodicity and shape changes. Results. Three binaries with extraneous eclipses on the binary light curves were found and studied based on the Kepler observations. The object KIC 5255552 is an eclipsing triple system with a fast changing inner binary and an outer companion uncovered by three groups of extraneous eclipses of 862.1(±0.1) d period. The KIC 10091110 is suggested to be a double eclipsing binary system with several possible extraordinary coincidences: the two binaries share similar extremely small mass ratios (0.060(13) and 0.0564(18)), similar mean primary densities (0.3264(42) ρ☉ and 0.3019(28) ρ☉), and, most notably, the ratio of the two binaries’ periods is very close to integer 2 (8.5303353/4.2185174 = 2.022). The KIC 11495766 is a probable triple system with a ∼ 120.73 d period binary and (at least) one non-eclipse companion. Furthermore, very close to it in the celestial sphere, there is a blended background stellar binary of 8.3404432 d period. A first list of 25 eclipsing multiple candidates is presented, with the hope that it will be beneficial for study of eclipsing multiples. Copyright © 2017, The Authors. All rights reserved.

关键词： Stars

Do SN 2002cx-like and SN Ia-CSM objects share the same origin?

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arXiv 2017年

作者： Meng, X. Podsiadlowski, Ph. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Department of Astronomy Oxford University OxfordOX1 3RH United Kingdom

SN 2002cx-like and SN Ia-CSM objects show similar early spectra and both belong to a young stellar population, suggesting that they could share the same progenitor origin. Adopting the framework of the common-envelope-wind (CEW) model developed in Meng & Podsiadlowski (2017), we here propose that both subclasses of SNe Ia are caused by the explosion of hybrid carbon-oxygen-neon white dwarfs (CONe WDs) in single-degenerate systems, where SNe Ia- CSM explode in systems with a massive common envelope (CE) of ∼ 1 Mo, while SN 2002cxlike events correspond to those events where most of the CE has been lost in a wind. Using binary-population-synthesis (BPS) calculations, we estimate a number ratio of SNe Ia-CSM to SN 2002cx-like objects between 1/3 and 2/3 , consistent with observational constraints, and an overall contribution from hybrid CONeWDs to the total SN Ia population that also matches the observed number from these peculiar objects. Our model predicts a statistical sequence of CSM density from SN Ia-CSM to SN 2002cx-like events and normal SNe Ia, consistent with existing radio constraints. We also find a new subclass of hybrid SNe which share the properties of Type II and Type Ia SNe, consistent with some observed SNe, which do not have a surviving companion. In some cases these could even produce SNe Ia from apparently single WDs. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

Two twin binaries with nearly identical components: KIC 4826439 and KIC 6045264

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arXiv 2017年

作者： Zhang, Jia Qian, Sheng-Bang Wang, Shu-Min Wu, Yue Jiang, Lin-Qiao Yunnan Observatories Chinese Academy of Sciences Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China School of Mathematics and Physics Handan University Handan056005 China Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100012 China School of Physics and Electronic Engineering Sichuan University of Science & Engineering Zigong643000 China

Two twin binaries, KIC 4826439 and KIC 6045264, with very similar component stars were found photometrically based on Kepler eclipsing binary light curves. The absolute parameters of the massive components are 1.156(0.03)M☉, 1.881(0.02)R☉, 6065K for KIC 4826439, and 0.874(0.3)M☉, 1.206(0.02)R☉, 6169(30)K for KIC 6045264. The differences between the components are less than two percents for all the parameters. A very low proportion of the twin binaries (2/1592 ≈ 0.13%) was found, which does not support the previous findings of the excesses of twins on binary mass ratio distribution, but support a deficiently low proportion of twins. A new method is practiced to work out the absolute parameters of the two twins without the radial velocities. This method requires the solution of the light curves, the spectra and the evolutionary isochrones of covering the complete stellar parameter space, simultaneously. We also studied their evolution tracks that: KIC 4826439 will experience an unstable mass transfer stage followed by an unclear ending, and KIC 6045264 will become a single star via an over-contact phase. It seems highly unlikely that the two twin binaries will produce twin degenerate binaries, although they have quite similar components. Copyright © 2017, The Authors. All rights reserved.

关键词： Mass transfer

RW Dor: A shallow contact binary with new orbital period investigation

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arXiv 2018年

作者： Sarotsakulchai, T. Qian, S.-B. Soonthornthum, B. Lajus, E. Fernandez Liu, N.-P. Zhou, X. Zhang, J. Liao, W.-P. Reichart, D.E. Haislip, J.B. Kouprianov, V.V. Poshyachinda, S. Yunnan Observatories Chinese Academy of Sciences Kunming650216 China University of Chinese Academy of Sciences 19 A Yuquan Rd. Shijingshan Beijing100049 China National Astronomical Research Institute of Thailand Ministry of Science and Technology Bangkok Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Rd. Chaoyang District Beijing100012 China Facultad de Ciencias Astronómicas y Geofísicas UNLP La Plata Buenos Aires1900 Argentina Instituto de Astrofisica de La Plata CONICET UNLP La PlataProvincia de Buenos Aires Argentina Department of Physics and Astronomy University of North Carolina CB #3255 Chapel HillNC27599 United States

New CCD photometric light curves of short period (P=0.285d) eclipsing binary RW Dor are presented. The observations performed with the PROMPT-8 robotic telescope at CTIO in Chile from March 2015 to March 2017. The other eclipse timings were obtained from the 2.15-m JS telescope at CASLEO, San Juan, Argentina in December 2011. By light-curve analysis, it is found that RW Dor is a W-type shallow contact binary with a fill-out factor f ∼ 11% and high mass ratio q ∼ 1.587 (1/q = 0.63), where the hotter component is the less massive one (M1 ∼ 0.52Mo and M2 ∼ 0.82Mo). For orbital period investigation, the new fifteen eclipse times and those in previous published were compiled. Based on O-C analysis with very weak evidence suggests that a long-term period decrease with a rate of dP/dt =-9.61 × 10-9d yr-1is superimposed on a cyclic variation (A3= 0.0054 days and P3= 49.9 yrs). The long-term period decrease can be interpreted as mass transfer from the more massive component to the less massive one or combine with the angular momentum loss (AML) via magnetic braking. In addition, with the marginal contact phase, high mass ratio (1/q > 0.4) and the long-term period decrease, all suggest that RW Dor is a newly formed contact binary via a Case A mass transfer and it will evolve into a deeper normal contact binary. If the cyclic change is correct, the light-travel time effect via the presence of a cool third body will be more plausible to explain for this. Copyright © 2018, The Authors. All rights reserved.

关键词： Travel time

A new derivation of the relationship between diffusion coefficient and entropy in classical Brownian motion by the ensemble method

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arXiv 2017年

作者： Liao, Yi Gong, Xiao-Bo Department of Physics College of Science Southern University of Science and Technology Shenzhen518055 China Yunnan Observatory and Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of Chinese Academy of Sciences Beijing100049 China

The diffusion coefficient–a measure of dissipation, and the entropy–a measure of fluctuation are found to be intimately correlated in many physical systems. Unlike the fluctuation dissipation theorem in linear response theory, the correlation is often strongly non-linear. To understand this complex dependence, we consider the classical Brownian diffusion in this work. Under certain rational assumption, i.e. in the bi-component fluid mixture, the mass of the Brownian particle M is far greater than that of the bath molecule m, we can adopt the weakly couple limit. Only considering the first-order approximation of the mass ratio m/M, we obtain a linear motion equation in the reference frame of the observer as a Brownian particle. Based on this equivalent equation, we get the Hamiltonian at equilibrium. Finally, using canonical ensemble method, we define a new entropy that is similar to the Kolmogorov-Sinai entropy. Further, we present an analytic expression of the relationship between the diffusion coefficient D and the entropy S in the thermal equilibrium, that is to say, D = eM~ exp [S/(kB d)], where d is the dimension of the space, kB the Boltzmann constant, ~ the reduced Planck constant and e the Euler number. This kind of scaling relation has been well-known and well-tested since the similar one for single component is firstly derived by Rosenfeld with the expansion of volume ratio. Copyright © 2017, The Authors. All rights reserved.

关键词： Entropy

Physical parameters and orbital period variation of a newly discovered cataclysmic variable GSC 4560-02157

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arXiv 2017年

作者： Han, Zhong-Tao Qian, Sheng-Bang Voloshina, Irina Metlov, Vladimir G. Zhu, Li-Ying Li, Lin-Jia P. O. Box 110 Kunming650216 Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 Sternberg Astronomical Institute Moscow State University Universitetskij prospect 13 Moscow119992

GSC 4560-02157 is a new eclipsing cataclysmic variable with an orbital period of 0.265359 days. By using the published V- and R-band data together with our observations, we discovered that the O - C curve of GSC 4560-02157 may shows a cyclic variation with the period of 3.51 years and an amplitude of 1.40 min. If this variation is caused by a light travel-time effect via the existence of a third body, its mass can be derived as M3sini' ≈ 91.08MJup, it should be a low-mass star. In addition, several physical parameters were measured. The colour of the secondary star was determined as V - R = 0.77(±0.03) which corresponds to a spectral type of K2-3. The secondary star's mass was estimated as M2 = 0.73(±0.02)Moby combing the derived V - R value around phase 0 with the assumption that it obeys the mass-luminosity relation of the main sequence stars. This mass is consistent with the mass'period relation of CV donor stars. For the white dwarf, the eclipse durations and contacts of the white dwarf yield an upper limit of the white dwarf's radius corresponding to a lower limit mass of Mi ≈ 0.501Mo. The overestimated radius and previously published spectral data indicate that the boundary layer may has a very high temperature. Copyright © 2017, The Authors. All rights reserved.

关键词： White dwarfs

GRANDMA and HXMT Observations of GRB 221009A - the Standard-Luminosity Afterglow of a Hyper-Luminous Gamma-Ray Burst

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arXiv 2023年

作者： Kann, D.A. Agayeva, S. Aivazyan, V. Alishov, S. Andrade, C.M. Antier, S. Baransky, A. Bendjoya, P. Benkhaldoun, Z. Beradze, S. Berezin, D. Boër, M. Broens, E. Brunier, S. Bulla, M. Burkhonov, O. Burns, E. Chen, Y. Chen, Y.P. Conti, M. Coughlin, M.W. Cui, W.W. Daigne, F. Delaveau, B. Devillepoix, H.A.R. Dietrich, T. Dornic, D. Dubois, F. Ducoin, J.-G. Durand, E. Duverne, P.-A. Eggenstein, H.-B. Ehgamberdiev, S. Fouad, A. Freeberg, M. Froebrich, D. Ge, M.Y. Gervasoni, S. Godunova, V. Gokuldass, P. Gurbanov, E. Han, D.W. Hasanov, E. Hello, P. Hussenot-Desenonges, T. Inasaridze, R. Iskandar, A. Ismailov, N. Janati, A. du Laz, T. Jegou Jia, S.M. Karpov, S. Kaeouach, A. Kiendrebeogo, R.W. Klotz, A. Kneip, R. Kochiashvili, N. Kunert, N. Lekic, A. Leonini, S. Li, C.K. Li, W. Li, X.B. Liao, J.Y. Logie, L. Lu, F.J. Mao, J. Marchais, D. Ménard, R. Morris, D. Natsvlishvili, R. Nedora, V. Noonan, K. Noysena, K. Orange, N.B. Pang, P.T.H. Peng, H.W. Pellouin, C. Peloton, J. Pradier, T. Pyshna, O. Rajabov, Y. Rau, S. Rinner, C. Rivet, J.-P. Romanov, F.D. Rosi, P. Rupchandani, V.A. Serrau, M. Shokry, A. Simon, A. Smith, K. Sokoliuk, O. Soliman, M. Song, L.M. Takey, A. Tillayev, Y. Ramirez, L.M. Tinjaca Melo, I. Tosta e Turpin, D. de Ugarte Postigo, A. Vanaverbeke, S. Vasylenko, V. Vernet, D. Vidadi, Z. Wang, C. Wang, J. Wang, L.T. Wang, X.F. Xiong, S.L. Xu, Y.P. Xue, W.C. Zeng, X. Zhang, S.N. Zhao, H.S. Zhao, X.F. Hessian Research Cluster ELEMENTS Giersch Science Center Goethe University Frankfurt Campus Riedberg Max-von-Laue-Straße 12 Frankfurt am Main60438 Germany N. Tusi Shamakhy Astrophysical Observatory Azerbaijan National Academy of Sciences settl. Y. Mammadaliyev AZ Shamakhi5626 Azerbaijan E. Kharadze Georgian National Astrophysical Observatory Mt. Kanobili Abastumani Adigeni0301 Georgia Samtskhe-Javakheti State University Rustaveli Str. 113 Akhaltsikhe0080 Georgia School of Physics and Astronomy University of Minnesota MinneapolisMN55455 United States Artemis Observatoire de la Côte d’Azur Université Côte d’Azur Boulevard de l’Observatoire Nice06304 France Astronomical Observatory of Taras Shevchenko National University of Kyiv Observatorna Str. 3 Kyiv04053 Ukraine Laboratoire J.-L. Lagrange Université de Nice Sophia-Antipolis CNRS Observatoire de la Côte d’Azur Nice06304 France Oukaimeden Observatory High Energy Physics and Astrophysics Laboratory FSSM Cadi Ayyad University Av. Prince My Abdellah MarrakeshBP 2390 Morocco Main Astronomical Observatory of National Academy of Sciences of Ukraine 27 Acad. Zabolotnoho Str. Kyiv03143 Ukraine Vereniging Voor Sterrenkunde Balen-Neetlaan 18A Mol2400 Belgium Department of Physics and Earth Science University of Ferrara via Saragat 1 FerraraI-44122 Italy INFN Sezione di Ferrara via Saragat 1 FerraraI-44122 Italy INAF Osservatorio Astronomico d’Abruzzo via Mentore Maggini snc TeramoI-64100 Italy Ulugh Beg Astronomical Institute Uzbekistan Academy of Sciences Astronomy Str. 33 Tashkent100052 Uzbekistan Department of Physics & Astronomy Louisiana State University Baton RougeLA70803 United States Key Laboratory of Particle Astrophysics Institute of High Energy Physics Chinese Academy of Sciences Beijing100049 China Montarrenti Observatory S. S. 73 Ponente Sovicille SienaI-53018 Italy Sorbonne Université CNRS UMR 7095 Institut d’Astrophysique de Paris 98 bis bd Arago Paris75014 Fra

GRB 221009A is the brightest Gamma-Ray Burst (GRB) detected in more than 50 years of study. In this paper, we present observations in the X-ray and optical domains ranging from the prompt emission (optical coverage by all-sky cameras) up to 20 days after the GRB obtained by the GRANDMA Collaboration (which includes observations from more than 30 professional and amateur telescopes) and the Insight-HXMT Collaboration operating the X-ray telescope HXMT-LE. We study the optical afterglow with empirical fitting using the GRANDMA+HXMT-LE data sets, augmented with data from the literature up to 60 days. We then model numerically, using a Bayesian approach, the GRANDMA and HXMT-LE afterglow observations, that we augment with Swift-XRT and additional optical/NIR observations reported in the literature. We find that the GRB afterglow, extinguished by a large dust column, is most likely behind a combination of a large Milky-Way dust column combined with moderate low-metallicity dust in the host galaxy. Using the GRANDMA+HXMT-LE+XRT dataset, we find that the simplest model, where the observed afterglow is produced by synchrotron radiation at the forward external shock during the deceleration of a top-hat relativistic jet by a uniform medium, fits the multi-wavelength observations only moderately well, with a tension between the observed temporal and spectral evolution. This tension is confirmed when using the extended dataset. We find that the consideration of a jet structure (Gaussian or power-law), the inclusion of synchrotron self-Compton emission, or the presence of an underlying supernova do not improve the predictions, showing that the modelling of GRB22109A will require going beyond the most standard GRB afterglow model. Placed in the global context of GRB optical afterglows, we find the afterglow of GRB 221009A is luminous but not extraordinarily so, highlighting that some aspects of this GRB do not deviate from the global known sample despite its extreme energetics an

关键词： Dust