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TESS Asteroseismic analysis of the known exoplanet shost star HD 222076

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arXiv 2020年

作者： Jiang, Chen Bedding, Timothy R. Stassun, Keivan G. Veras, Dimitri Corsaro, Enrico Buzasi, Derek L. Mikolajczyk, Przemys law Zhang, Qian-sheng Ou, Jian-wen Campante, Tiago L. Rodrigues, Thaíse S. Nsamba, Benard Bossini, Diego Kane, Stephen R. Ong, Jia Mian Joel Yıldız, Mutlu Orhan, Zeynep Çeiik Örtel, Sibel Wu, Tao Zhang, Xinyi Li, Tanda Basu, Sarbani Cunha, Margarida S. Christensen-Dalsgaard, Jørgen Chaplin, William J. School of Physics and Astronomy Sun Yat-Sen University No. 135 Xingang Xi Road Guangzhou510275 China Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus C8000 Denmark School of Physics University of Sydney NSW2006 Australia Vanderbilt University Department of Physics and Astronomy 6301 Stevenson Center Ln. NashvilleTN37235 United States 6301 Stevenson Center Ln. NashvilleTN37235 United States Centre for Exoplanets and Habitability University of Warwick CoventryCV4 7AL United Kingdom Department of Physics University of Warwick CoventryCV4 7AL United Kingdom INAF — Osservatorio Astrofisico di Catania via S. Sofia 78 Catania95123 Italy Department of Chemistry & Physics Florida Gulf Coast University 10501 FGCU Boulevard S. Fort MyersFL33965 United States Astronomical Institute University of Wroclaw Mikolaja Kopernika 11 Wroclaw51-622 Poland Yunnan Observatories Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences 396 Yangfangwang Guandu District Kunming650216 China University of Chinese Academy of Sciences Beijing100049 China Instituto de Astrofísica e Ciências do Espaço Universidade do Porto Rua das Estrelas Porto4150-762 Portugal Departamento de Física e Astronomia Faculdade de Ciências da Universidade do Porto Rua do Campo Alegre s/n Porto4169-007 Portugal Osservatorio Astronomico di PadovaINAF Vicolo dellOsservatorio 5 PadovaI-35122 Italy Max-Planck-Institut für Astrophysik Karl-Schwarzschild-Str. 1 GarchingD-85748 Germany Department of Earth and Planetary Sciences University of California RiversideCA92521 United States Department of Astronomy Yale University P.O. Box 208101 New HavenCT06520-8101 United States Department of Astronomy and Space Sci

The Transiting Exoplanet Survey Satellite (TESS) is an all-sky survey mission aiming to search for exoplanets that transit bright stars. The high-quality photometric data of TESS are excellent for the asteroseismic study of solar-like stars. In this work, we present an asteroseismic analysis of the red-giant star HD 222076 hosting a long-period (2.4 yr) giant planet discovered through radial velocities. Solar-like oscillations of HD 222076 are detected around 203 µHz by TESS for the first time. Asteroseismic modeling, using global asteroseismic parameters as input, yields a determination of the stellar mass (M? = 1.12 ± 0.12M), radius (R? = 4.34 ± 0.21 R), and age (7.4 ± 2.7 Gyr), with precisions greatly improved from previous studies. The period spacing of the dipolar mixed modes extracted from the observed power spectrum reveals that the star is on the red-giant branch burning hydrogen in a shell surrounding the core. We find that the planet will not escape the tidal pull of the star and be engulfed into it within about 800 Myr, before the tip of the red-giant branch is reached. Copyright © 2020, The Authors. All rights reserved.

关键词： Extrasolar planets

Optical and near-infrared observations of the nearby type Ia supernova 2017cbv

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arXiv 2020年

作者： Wang, Lingzhi Contreras, Carlos Hu, Maokai Hamuy, Mario A. Hsiao, Eric Y. Sand, David J. Anderson, Joseph P. Ashall, Chris Burns, Christopher R. Chen, Juncheng Diamond, Tiara R. Davis, Scott Förster, Francisco Galbany, Lluís González-Gaitán, Santiago Gromadzki, Mariusz Hoeflich, Peter Li, Wenxiong Marion, G.H. Morrell, Nidia Pignata, Giuliano Prieto, Jose L. Phillips, Mark M. Shahbandeh, Melissa Suntzeff, Nicholas Valenti, Stefano Wang, Lifan Wang, Xiaofeng Young, D.R. Yu, Lixin Zhang, Jujia CAS Key Laboratory of Optical Astronomy National Astronomical Observatories Chinese Academy of Sciences Beijing100101 China Chinese Academy of Sciences South America Center for Astronomy National Astronomical Observatories CAS Beijing100101 China Carnegie Observatories Las Campanas Observatory Colina El Pino Casilla601 Chile Purple Mountain Observatory NanjingJiangsu201008 China Departamento de Astronomía Universidad de Chile Camino El Observatorio 1515 Las Condes Santiago Chile Millennium Institute of Astrophysics Santiago Chile Department of Physics Florida State University TallahasseeFL32306 United States Department of Astronomy and Steward Observatory University of Arizona 933 North Cherry Avenue TucsonAZ85721-0065 United States European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States School of Electronics and Information Engineering Wuzhou University Wuzhou543002 China Departamento de Física Teórica y del Cosmos Universidad de Granada GranadaE-18071 Spain CENTRA/COSTAR Instituto Superior Técnico Universidade de Lisboa Av. Rovisco Pais 1 Lisboa1049-001 Portugal Astronomical Observatory University of Warsaw Al. Ujazdowskie 4 Warszawa00-478 Poland Physics Department/Tsinghua Center for Astrophysics Tsinghua University Beijing100084 China Department of Astronomy University of Texas at Austin 1 University Station C1400 AustinTX78712-0259 United States Departamento de Ciencias Físicas Universidad Andres Bello Avda. República 252 Santiago8320000 Chile Núcleo de Astronomía de la Facultad de Ingeniería Universidad Diego Portales Av. Ejército 441 Santiago Chile George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Department of Physics and Astronomy Texas United States A&M University College Station TX77843 United States Department of Physics University of California 1 S

Supernova (SN) 2017cbv in NGC 5643 is one of a handful of type Ia supernovae (SNe Ia) reported to have excess blue emission at early times. This paper presents extensive BV RIY JHKs-band light curves of SN 2017cbv, covering the phase from −16 to +125 days relative to B-band maximum light. SN 2017cbv reached a B-band maximum of 11.710±0.006 mag, with a post-maximum magnitude decline ∆m15(B)=0.990±0.013 mag. The supernova suffered no host reddening based on Phillips intrinsic color, Lira-Phillips relation, and the CMAGIC diagram. By employing the CMAGIC distance modulus µ = 30.58±0.05 mag and assuming H0 = 72 km s−1 Mpc−1, we found that 0.73 Mo56Ni was synthesized during the explosion of SN 2017cbv, which is consistent with estimates using reddening-free and distance-free methods via the phases of the secondary maximum of the NIR-band light curves. We also present 14 near-infrared spectra from −18 to +49 days relative to the B-band maximum light, providing constraints on the amount of swept-up hydrogen from the companion star in the context of the single degenerate progenitor scenario. No Paβ emission feature was detected from our post-maximum NIR spectra, placing a hydrogen mass upper limit of 0.1 Mo. The overall optical/NIR photometric and NIR spectral evolution of SN 2017cbv is similar to that of a normal SN Ia, even though its early evolution is marked by a flux excess no seen in most other well-observed normal SNe Ia. We also compare the exquisite light curves of SN 2017cbv with some Mch DDT models and sub-Mch double detonation models. Copyright © 2020, The Authors. All rights reserved.

关键词： Supernovae

Physical Properties and Catalogue of EW-type Eclipsing Binaries Observed by LAMOST

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arXiv 2017年

作者： Qian, S.-B. He, J.-J. Zhang, J. Zhu, L.-Y. Shi, X.-D. Zhao, E.-G. Zhou, X. P.O. Box 110 Kunming650011 Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang Dis-trict Beijing100012 China University of the Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China

EW-type eclipsing binaries (hereafter EWs) are strong interacting systems where both component stars are usually filling the critical Roche lobes and are sharing a common envelope. Numerous EWs were discovered by several deep photometric survey and there are about 40785 EW-type binary systems listed in the international variable star index (VSX) by March 13, 2017. 7938 of them were observed by LAMOST by November 30, 2016 and their spectral types were given. Stellar atmospheric parameters of 5363 EW-type binary stars were determined based on good spectroscopic observations. In the paper, those EWs were catalogued and their properties are analyzed. The distributions of the orbital period (P), the effect temperature (T), the gravitational acceleration (Log(g)), the metallicity ([Fe/H]) and the radial velocity (RV) are presented for those observed EW-type systems. It is shown that about 80.6% sample stars have metallicity below zero indicating that EW-type systems are old stellar population. This is in agreement with the the conclusion that the EW binaries are formed from moderately close binaries through angular momentum loss via magnetic braking that takes a few hundred million to a few billion years. The unusual high metallicities of a few percent of EWs may be caused by contaminating of material from the evolution of unseen neutron stars and black holes in the systems. The correlations between the orbital period and the effect temperature, the gravitational acceleration and the metallicity are presented and their scatters are mainly caused by (i) the presence of the third bodies and (ii) the wrong determined periods sometimes. It is shown that some EW contain evolved component stars and the physical properties of EWs are mainly depending on their orbital periods. It is found that the extremely short-period EWs may be older than their long-period cousins because they have lower metallicities. This reveals that they have a longer timescale of pre-contact evolution and

关键词： Astrophysics

Cyclic period oscillation of the eclipsing dwarf nova DV UMa

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arXiv 2017年

作者： Han, Z.-T. Qian, S.-B. Voloshina, Irina Zhu, L.-Y. P. O. Box 110 Kunming650216 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P. O. Box 110 Kunming650216 China University of Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China Sternberg Astronomical Institute Moscow State University Universitetskij prospect 13 Moscow119992 Russia

DV UMa is an eclipsing dwarf nova with an orbital period of ~ 2.06 h, which lies just at the bottom edge of the period gap. To detect its orbital period changes we present 12 new mid-eclipse times by using our CCD photometric data and archival data. Combining with the published mid-eclipse times in quiescence, spanning ~ 30 yr, the latest version of the O - C diagram was obtained and analyzed. The best fit to those available eclipse timings shows that the orbital period of DV UMa is undergoing a cyclic oscillation with a period of 17.58(±0.52) yr and an amplitude of 71.1(±6.7) s. The periodic variation most likely arises from the light-travel-time effect via the presence of a circumbinary object because the required energy to drive the Applegate mechanism is too high in this system. The mass of the unseen companion was derived as M3 sin i' = 0.025(±0.004)Mo. If the third body is in the orbital plane (i.e. i' = i = 82.9°) of the eclipsing pair, it would match to a brown dwarf. This hypothetical brown dwarf is orbiting its host star at a separation of ~ 8.6 AU in an eccentric orbit (e = 0.44). Copyright © 2017, The Authors. All rights reserved.

关键词： Stars

Physical properties and evolutionary states of EA-type eclipsing binaries observed by LAMOST

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arXiv 2017年

作者： Qian, S.-B. Zhang, J. He, J.-J. Zhu, L.-Y. Zhao, E.-G. Shi, X.-D. Zhou, X. Han, Z.-T. P.O. Box 110 Kunming650011 China Key Laboratory of the Structure and Evolution of Celestial Objects Chinese Academy of Sciences P.O. Box 110 Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China University of the Chinese Academy of Sciences Yuquan Road 19# Sijingshang Block Beijing100049 China

About 3196 EA-type binaries (EAs) were observed by LAMOST by June 16, 2017 and their spectral types were derived. Meanwhile stellar atmospheric parameters of 2020 EAs were determined. In the paper, those EAs are catalogued and their physical properties and evolutionary states are investigated. The period distribution of EAs suggests that the period limit of tidal locking for the close binaries is about 6 days. It is found that the metallicity of EAs is higher than that of EWs indicating that EAs are generally younger than EWs and they are the progenitors of EWs. The metallicities of long-period EWs (0.4 Copyright © 2017, The Authors. All rights reserved.

关键词： Astrophysics

SN 2021csp - The explosion of a stripped envelope star within a H and He-poor circumstellar medium

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arXiv 2021年

作者： Fraser, Morgan Stritzinger, Maximilian D. Brennan, Seán J. Pastorello, Andrea Cai, Yongzhi Piro, Anthony L. Ashall, Chris Brown, Peter Burns, Christopher R. Elias-Rosa, Nancy Filippenko, Alexei V. Galbany, L. Hsiao, E.Y. Jha, Saurabh W. Kotak, Rubina Moran, Shane Morrell, Nidia Ochner, Paolo Phillips, M.M. Reguitti, Andrea Shappee, B.J. Tomasella, Lina Tucker, Michael Wang, Xiaofeng Zhang, Ju-Jia Anderson, J.P. Barna, Tyler Baron, E. Benetti, Stefano Bersten, Melina C. Brink, Thomas G. Camacho-Neves, Yssavo Davis, Scott Dettman, Kyle G. Folatelli, Gaston Gutiérrez, Claudia P. Höflich, Peter Holoien, Thomas W.-S. Kankare, Erkki Kuncarayakti, Hanindyo Kwok, Lindsey Kumar, Sahana Lu, Jing Mazzali, Paolo Shahbandeh, Melissa Suntzeff, Nicholas B. Taubenberger, Stefan Tinyanont, Samaporn Yan, Shengyu Yang, Yi Zheng, WeiKang School of Physics University College Dublin Dublin 4 Belfield Ireland Department of Physics and Astronomy Aarhus University Ny Munkegade 120 Aarhus CDK-8000 Denmark INAF – Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 PadovaI-35122 Italy Tsinghua University Beijing100084 China The Observatories of the Carnegie Institution for Science 813 Santa Barbara St. PasadenaCA91101 United States Institute for Astronomy University of Hawai’i 2680 Woodlawn Drive HonoluluHI96822 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy Department of Physics and Astronomy Texas A & M University College StationTX77843 United States Campus UAB Carrer de Can Magrans s/n BarcelonaE-08193 Spain Department of Astronomy University of California BerkeleyCA94720-3411 United States Miller Institute for Basic Research in Science University of California BerkeleyCA94720 United States Department of Physics Florida State University 77 Chieftain Way TallahasseeFL32306 United States Department of Physics and Astronomy Rutgers the State University of New Jersey 136 Frelinghuysen Road PiscatawayNJ08854 United States Tuorla Observatory Department of Physics and Astronomy University of Turku Turku20014 Finland Carnegie Observatories Las Campanas Observatory Casilla 601 La Serena Chile Dipartimento di Fisica e Astronomia Università di Padova Vicolo Osservatorio 2 Padova35122 Italy Departamento de Ciencias Fisicas Universidad Andres Bello Avda. Republica 252 Santiago Chile Nuncio Monseñor Sotero Sanz 100 Providencia Santiago Chile Beijing Planetarium Beijing Academy of Science and Technology Beijing100044 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 European Southern Observatory Alonso de Córdova 3107 Casilla 19 Santiago Chile Homer L. Dodge Departme

We present observations of SN 2021csp, a unique supernova (SN) which displays evidence for interaction with H- and He- poor circumstellar material (CSM) at early times. Using high-cadence spectroscopy taken over the first week after explosion, we show that the spectra of SN 2021csp are dominated by C III lines with a velocity of 1800 km s−1. We associate this emission with CSM lost by the progenitor prior to explosion. Subsequently, the SN displays narrow He lines before metamorphosing into a broad-lined Type Ic SN. We model the bolometric light curve of SN 2021csp, and show that it is consistent with the energetic (4 × 1051 erg) explosion of a stripped star, producing 0.4 M of 56Ni within a ∼ 1 M shell of CSM extending out to 400 R. Copyright © 2021, The Authors. All rights reserved.

关键词： Supernovae

Observations of type ia supernova 2014j for nearly 900 days and constraints on its progenitor system

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arXiv 2019年

作者： Li, Wenxiong Wang, Xiaofeng Hu, Maokai Yang, Yi Zhang, Jujia Mo, Jun Chen, Zhihao Zhang, Tianmeng Benetti, Stefano Cappellaro, Enrico Elias-Rosa, Nancy Isern, Jordi Morales-Garoffolo, Antonia Huang, Fang Ochner, Paolo Pastorello, Andrea Reguitti, Andrea Tartaglia, Leonardo Terreran, Giacomo Tomasella, Lina Wang, Lifan Tsinghua University Beijing100084 China Purple Mountain Observatory Chinese Academy of Sciences Nanjing210034 China Department of Particle Physics and Astrophysics Weizmann Institute of Science Rehovot76100 Israel Yunnan Astronomical Observatory of China Chinese Academy of Sciences Kunming650011 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China National Astronomical Observatory of China Chinese Academy of Sciences Beijing100012 China INAF - Osservatorio Astronomico di Padova Vicolo dell’Osservatorio 5 Padova35122 Italy Campus UAB Carrer de Can Magrans s/n Barcelona08193 Spain c/Gran Capitá 2-4 Edif. Nexus 201 Barcelona08034 Spain Department of Applied Physics University of Cádiz Campus of Puerto Real E-11510 Cádiz Spain Department of Astronomy School of Physics and Astronomy Shanghai Jiao Tong University Shanghai200240 China Dipartimento di Fisica e Astronomia G. Galilei Universita’ di Padova Vicolo dell’Osservaotio 3 Padova35122 Italy Departamento de Ciencias Fisicas Universidad Andrés Bello Fernandez Concha Santiago700 Chile Department of Astronomy Stockholm University StockholmSE 10691 Sweden Department of Physics and Astronomy Northwestern University EvanstonIL60208 United States George P. and Cynthia Woods Mitchell Institute for Fundamental Physics & Astronomy Texas A. & M. University Department of Physics and Astronomy 4242 TAMU College StationTX77843 United States

We present extensive ground-based and Hubble Space Telescope (HST) photometry of the highly reddened, very nearby type Ia supernova (SN Ia) 2014J in M82, covering the phases from 9 days before to about 900 days after the B-band maximum. SN 2014J is similar to other normal SNe Ia near the maximum light, but it shows flux excess in the B band in the early nebular phase. This excess flux emission can be due to light scattering by some structures of circumstellar materials located at a few 1017 cm, consistent with a single degenerate progenitor system or a double degenerate progenitor system with mass outflows in the final evolution or magnetically driven winds around the binary system. At t∼+300 to ∼+500 days past the B-band maximum, the light Copyright © 2019, The Authors. All rights reserved.

关键词： Supernovae

Spectropolarimetry and photometry of the early afterglow of the gamma-ray burst GRB 191221B

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arXiv 2020年

作者： Buckley, David A.H. Bagnulo, S. Britto, R.J. Mao, J. Kann, D.A. Cooper, J. Lipunov, V. Hewitt, D.M. Razzaque, S. Kuin, N.P.M. Monageng, I.M. Covino, S. Jakobsson, P. van der Horst, A.J. Wiersema, K. Böttcher, M. Campana, S. D'Elia, V. Gorbovskoy, E.S. Gorbunov, I. Groenewald, D.N. Hartmann, D.H. Kornilov, V.G. Mundell, C.G. Podesta, R. Thomas, J.K. Tyurina, N. Vlasenko, D. van Soelen, B. Xu, D. South African Astronomical Observatory PO Box 9 Observatory Road Observatory Cape Town7935 South Africa Department of Astronomy University of Cape Town Private Bag X3 Rondebosch7701 South Africa Armagh Observatory & Planetarium College Hill ArmaghBT61 9DG United Kingdom Department of Physics University of the Free State PO Box 339 Bloemfontein9300 South Africa Yunnan Observatories Chinese Academy of Sciences Yunnan Province Kunming650011 China Center for Astronomical Mega-Science Chinese Academy of Sciences 20A Datun Road Chaoyang District Beijing100012 China Key Laboratory for the Structure and Evolution of Celestial Objects Chinese Academy of Sciences Kunming650011 China Glorieta de la Astronomía s/n Granada18008 Spain M. V. Lomonosov Moscow State University SAI Physics Department 13 Univeristetskij pr-t Moscow119991 Russia M.V.Lomonosov Moscow State University Physics Department Leninskie gory GSP-1 Moscow119991 Russia Department of Physics University of Johannesburg PO Box 524 Auckland Park2006 South Africa Mullard Space Science Laboratory Dept. of Space and Climate Sciences University College London Holmbury St Mary DorkingRH5 6NT United Kingdom I-23807 Italy Centre for Astrophysics and Cosmology Science Institute University of Iceland Dunhagi 5 Reykjavík107 Iceland Department of Physics The George Washington University 725 21st St. NW WashingtonDC20052 United States The George Washington University WashingtonDC20052 United States Department of Physics University of Warwick Gibbet Hill Road CoventryCV4 7AL United Kingdom Department of Physics and Astronomy University of Leicester LE1 7RH United Kingdom Centre for Space Research North West University Potchefstroom South Africa ASI-Space Science Data Center via del Politecnico snc Rome00133 Italy INAF - Osservatorio Astronomico di Roma via Frascati 33 Monte Porzio Catone00040 Italy Southern African Large Telescope Foundation PO Box 9 Observatory Road Obse

We report on results of spectropolarimetry of the afterglow of the long gamma-ray burst GRB 191221B, obtained with SALT/RSS and VLT/FORS2, as well as photometry from two telescopes in the MASTER Global Robotic Network, at the MASTER-SAAO (South Africa) and MASTER-OAFA (Argentina) stations. Prompt optical emission was detected by MASTER-SAAO 38 s after the alert, which dimmed from a magnitude (white-light) of ∼ 10 to 16.2 mag over a period of ∼10 ks, followed by a plateau phase lasting ∼10 ks and then a decline to ∼18 mag after 80 ks. The light curve shows complex structure, with four or five distinct breaks in the power-law decline rate. SALT/RSS linear spectropolarimetry of the afterglow began ∼ 2.9 h after the burst, during the early part of the plateau phase of the light curve. Absorption lines seen at ∼ 6010 Å and 5490 Å are identified with the Mg II 2799 Å line from the host galaxy at z = 1.15 and an intervening system located at z = 0.96. The mean linear polarisation measured over 3400 − 8000 Å was ∼1.5% and the mean equatorial position angle (θ) ∼65◦. VLT/FORS2 spectropolarimetry was obtained ∼ 10 h postburst, during a period of slow decline (α = −0.44), and the polarisation was measured to be p = 1.2% and θ = 60◦. Two observations with the MeerKAT radio telescope, taken 30 and 444 days after the GRB trigger, detected radio emission from the host galaxy only. We interpret the light curve and polarisation of this long GRB in terms of a slow-cooling forward-shock. Copyright © 2020, The Authors. All rights reserved.

关键词： Stars

Multi-band analyses of the bright GRB 230812B and the associated SN2023pel

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arXiv 2023年

作者： Hussenot-Desenonges, T. Wouters, T. Guessoum, N. Abdi, I. Abulwfa, A. Adami, C. Fernández, J.F. Agüí Ahumada, T. Aivazyan, V. Akl, D. Anand, S. Andrade, C.M. Antier, S. Ata, S.A. D’Avanzo, P. Azzam, Y.A. Baransky, A. Basa, S. Blazek, M. Bendjoya, P. Beradze, S. Boumis, P. Bremer, M. Brivio, R. Buat, V. Bulla, M. Burkhonov, O. Burns, E. Cenko, S.B. Coughlin, M.W. Corradi, W. Daigne, F. Dietrich, T. Dornic, D. Ducoin, J.-G. Duverne, P.-A. Elhosseiny, E.G. Elnagahy, F.I. El-Sadek, M.A. Ferro, M. Le Floc’h, E. Freeberg, M. Fynbo, J.P.U. Götz, D. Gurbanov, E. Hamed, G.M. Hasanov, E. Healy, B.F. Heintz, K.E. Hello, P. Inasaridze, R. Iskandar, A. Ismailov, N. Izzo, L. Jhawar, S. du Laz, T. Jegou Kamel, T.M. Karpov, S. Klotz, A. Koulouridis, E. Kuin, N.P. Kochiashvili, N. Leonini, S. Lu, K.-X. Malesani, D.B. Mašek, M. Mao, J. Melandri, A. Mihov, B.M. Natsvlishvili, R. Navarete, F. Nedora, V. Nicolas, J. Odeh, M. Palmerio, J. Pang, P.T.H. De Pasquale, M. Peng, H.W. Pormente, S. Peloton, J. Pradier, T. Pyshna, O. Rajabov, Y. Rakotondrainibe, N.A. Rivet, J.-P. Rousselot, L. Saccardi, A. Sasaki, N. Schneider, B. Serrau, M. Shokry, A. Slavcheva-Mihova, L. Simon, A. Sokoliuk, O. Srinivasaragavan, G. Strausbaugh, R. Takey, A. Tanvir, N.R. Thöne, C.C. Tillayev, Y. Tosta e Melo, I. Turpin, D. de Ugarte Postigo, A. Vasylenko, V. Vergani, S.D. Vidadi, Z. Xu, D. Wang, L.T. Wang, X.F. Winters, J.M. Zhang, X.-L. Zhu, Z. IJCLab Univ Paris-Saclay CNRS IN2P3 Orsay France Nikhef Science Park 105 Amsterdam1098 XG Netherlands Utrecht University Princetonplein 1 Utrecht3584 CC Netherlands Physics Department American University of Sharjah Sharjah United Arab Emirates 1 El-marsad St. Helwan Cairo11421 Egypt Aix Marseille Univ CNRS CNES LAM Marseille France Instituto de Astrofísica de Andalucía Glorieta de la Astronomía s/n Granada18008 Spain Cahill Center for Astrophysics California Institute of Technology PasadenaCA91125 United States 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 Observatoire de la Côte d’Azur Université Côte d’Azur Boulevard de l’Observatoire Nice06304 France INAF–Osservatorio Astronomico di Brera Via E. Bianchi 46 LC Merate23807 Italy Astronomical Observatory Taras Shevchenko National University of Kyiv Observatorna Str. 3 Kyiv04053 Ukraine CEICO Institute of Physics The Czech Academy of Sciences Na Slovance 1999/2 PrahaCZ-182 21 Czech Republic Centro Astronómico Hispano en Andalucía Observatorio de Calar Alto Sierra de los Filabres Gérgal Almería04550 Spain Laboratoire J.-L. Lagrange Université de Nice Sophia-Antipolis CNRS Observatoire de la Côte d’Azur Nice06304 France National Observatory of Athens Institute for Astronomy Astrophysics Space Applications and Remote Sensing Greece Institut de Radioastronomie Millimétrique France Università degli Studi dell’Insubria Dipartimento di Scienza e Alta Tecnologia Via Valleggio 11 Como22100 Italy 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 Astrono

GRB 230812B is a bright and relatively nearby (z = 0.36) long gamma-ray burst (GRB) that has generated significant interest in the community and has thus been observed over the entire electromagnetic spectrum. We report over 80 observations in X-ray, ultraviolet, optical, infrared, and sub-millimeter bands from the GRANDMA (Global Rapid Advanced Network for Multi-messenger Addicts) network of observatories and from observational partners. Adding complementary data from the literature, we then derive essential physical parameters associated with the ejecta and external properties (i.e. the geometry and environment) of the GRB and compare with other analyses of this event. We spectroscopically confirm the presence of an associated supernova, SN2023pel, and we derive a photospheric expansion velocity of v ∼ 17×103 km s-1. We analyze the photometric data first using empirical fits of the flux and then with full Bayesian Inference. We again strongly establish the presence of a supernova in the data, with a maximum (pseudo-)bolometric luminosity of 5.75×1042 erg/s, at 15.76+0.81-1.21 days (in the observer frame) after the trigger, with a half-max time width of 22.0 days. We compare these values with those of SN1998bw, SN2006aj, and SN2013dx. Our best-fit model favours a very low density environment (log10(nISM/cm-3) = -2.38+1.45-1.60) and small values for the jet’s core angle θcore = 1.54+1.02-0.81 deg and viewing angle θobs = 0.76+1.29-0.76 deg. GRB 230812B is thus one of the best observed afterglows with a distinctive supernova bump. © 2023, CC BY.

关键词： Supernovae