1
|
Li G, Hu M, Li W, Yang Y, Wang X, Yan S, Hu L, Zhang J, Mao Y, Riise H, Gao X, Sun T, Liu J, Xiong D, Wang L, Mo J, Iskandar A, Xi G, Xiang D, Wang L, Sun G, Zhang K, Chen J, Lin W, Guo F, Liu Q, Cai G, Zhou W, Zhao J, Chen J, Zheng X, Li K, Zhang M, Xu S, Lyu X, Castro-Tirado AJ, Chufarin V, Potapov N, Ionov I, Korotkiy S, Nazarov S, Sokolovsky K, Hamann N, Herman E. A shock flash breaking out of a dusty red supergiant. Nature 2024; 627:754-758. [PMID: 38093004 DOI: 10.1038/s41586-023-06843-6] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/14/2023] [Accepted: 11/07/2023] [Indexed: 02/17/2024]
Abstract
Shock-breakout emission is light that arises when a shockwave, generated by the core-collapse explosion of a massive star, passes through its outer envelope. Hitherto, the earliest detection of such a signal was at several hours after the explosion1, although a few others had been reported2-7. The temporal evolution of early light curves should provide insights into the shock propagation, including explosion asymmetry and environment in the vicinity, but this has been hampered by the lack of multiwavelength observations. Here we report the instant multiband observations of a type II supernova (SN 2023ixf) in the galaxy M101 (at a distance of 6.85 ± 0.15 Mpc; ref. 8), beginning at about 1.4 h after the explosion. The exploding star was a red supergiant with a radius of about 440 solar radii. The light curves evolved rapidly, on timescales of 1-2 h, and appeared unusually fainter and redder than predicted by the models9-11 within the first few hours, which we attribute to an optically thick dust shell before it was disrupted by the shockwave. We infer that the breakout and perhaps the distribution of the surrounding dust were not spherically symmetric.
Collapse
Affiliation(s)
- Gaici Li
- Physics Department, Tsinghua University, Beijing, China
| | - Maokai Hu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
| | - Wenxiong Li
- The School of Physics and Astronomy, Tel Aviv University, Tel Aviv, Israel
- Key Laboratory of Optical Astronomy, National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing, China
| | - Yi Yang
- Department of Astronomy, University of California, Berkeley, CA, USA
| | - Xiaofeng Wang
- Physics Department, Tsinghua University, Beijing, China.
- Beijing Planetarium, Beijing Academy of Science and Technology, Beijing, China.
| | - Shengyu Yan
- Physics Department, Tsinghua University, Beijing, China
| | - Lei Hu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA, USA
| | - Jujia Zhang
- Yunnan Observatories, Chinese Academy of Sciences, Kunming, China
- Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China
- International Centre of Supernovae, Yunnan Key Laboratory, Kunming, China
| | - Yiming Mao
- National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing, China
| | | | - Xing Gao
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
| | - Tianrui Sun
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
| | - Jialian Liu
- Physics Department, Tsinghua University, Beijing, China
| | - Dingrong Xiong
- Yunnan Observatories, Chinese Academy of Sciences, Kunming, China
- Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China
| | - Lifan Wang
- Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, College Station, TX, USA
| | - Jun Mo
- Physics Department, Tsinghua University, Beijing, China
| | - Abdusamatjan Iskandar
- Xinjiang Astronomical Observatory, Chinese Academy of Sciences, Urumqi, China
- School of Astronomy and Space Science, University of Chinese Academy of Sciences, Beijing, China
| | - Gaobo Xi
- Physics Department, Tsinghua University, Beijing, China
| | - Danfeng Xiang
- Physics Department, Tsinghua University, Beijing, China
| | - Lingzhi Wang
- Key Laboratory of Optical Astronomy, National Astronomical Observatories of China, Chinese Academy of Sciences, Beijing, China
- South America Center for Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | | | - Keming Zhang
- Department of Astronomy, University of California, Berkeley, CA, USA
| | - Jian Chen
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
| | - Weili Lin
- Physics Department, Tsinghua University, Beijing, China
| | - Fangzhou Guo
- Physics Department, Tsinghua University, Beijing, China
| | - Qichun Liu
- Physics Department, Tsinghua University, Beijing, China
| | | | | | | | - Jin Chen
- Xingming Observatory, Urumqi, China
| | | | | | - Mi Zhang
- Xingming Observatory, Urumqi, China
| | | | | | - Alberto J Castro-Tirado
- Instituto de Astrofisica de Andalucia (IAA-CSIC), Granada, Spain
- Unidad Asociada al CSIC, Departamento de Ingenieria de Sistemas y Automatica, Escuela de Ingenierias, Universidad de Malaga, Malaga, Spain
| | - Vasilii Chufarin
- G. M. Grechko Nizhny Novgorod Planetarium, Nizhny Novgorod, Russia
- Minin University, Nizhny Novgorod, Russia
| | | | | | | | | | - Kirill Sokolovsky
- Department of Astronomy, University of Illinois at Urbana-Champaign, Urbana, IL, USA
- Sternberg Astronomical Institute, Moscow State University, Moscow, Russia
| | | | | |
Collapse
|
2
|
Yang YH, Troja E, O'Connor B, Fryer CL, Im M, Durbak J, Paek GSH, Ricci R, Bom CR, Gillanders JH, Castro-Tirado AJ, Peng ZK, Dichiara S, Ryan G, van Eerten H, Dai ZG, Chang SW, Choi H, De K, Hu Y, Kilpatrick CD, Kutyrev A, Jeong M, Lee CU, Makler M, Navarete F, Pérez-García I. A lanthanide-rich kilonova in the aftermath of a long gamma-ray burst. Nature 2024; 626:742-745. [PMID: 38383623 DOI: 10.1038/s41586-023-06979-5] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 07/31/2023] [Accepted: 12/14/2023] [Indexed: 02/23/2024]
Abstract
Observationally, kilonovae are astrophysical transients powered by the radioactive decay of nuclei heavier than iron, thought to be synthesized in the merger of two compact objects1-4. Over the first few days, the kilonova evolution is dominated by a large number of radioactive isotopes contributing to the heating rate2,5. On timescales of weeks to months, its behaviour is predicted to differ depending on the ejecta composition and the merger remnant6-8. Previous work has shown that the kilonova associated with gamma-ray burst 230307A is similar to kilonova AT2017gfo (ref. 9), and mid-infrared spectra revealed an emission line at 2.15 micrometres that was attributed to tellurium. Here we report a multi-wavelength analysis, including publicly available James Webb Space Telescope data9 and our own Hubble Space Telescope data, for the same gamma-ray burst. We model its evolution up to two months after the burst and show that, at these late times, the recession of the photospheric radius and the rapidly decaying bolometric luminosity (Lbol ∝ t-2.7±0.4, where t is time) support the recombination of lanthanide-rich ejecta as they cool.
Collapse
Affiliation(s)
- Yu-Han Yang
- Department of Physics, University of Rome "Tor Vergata", Rome, Italy.
| | - Eleonora Troja
- Department of Physics, University of Rome "Tor Vergata", Rome, Italy.
- INAF - Istituto Nazionale di Astrofisica, Rome, Italy.
| | - Brendan O'Connor
- Department of Physics, The George Washington University, Washington DC, USA
- Department of Astronomy, University of Maryland, College Park, MD, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Chris L Fryer
- Computer, Computational, and Statistical Sciences Division, Los Alamos National Laboratory, Los Alamos, NM, USA
- Center for Theoretical Astrophysics, Los Alamos National Laboratory, Los Alamos, NM, USA
- The University of Arizona, Tucson, AZ, USA
- Department of Physics and Astronomy, The University of New Mexico, Albuquerque, NM, USA
- The George Washington University, Washington DC, USA
| | - Myungshin Im
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Joe Durbak
- Department of Astronomy, University of Maryland, College Park, MD, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Gregory S H Paek
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Roberto Ricci
- Istituto Nazionale di Ricerca Metrologica, Turin, Italy
- INAF - Istituto di Radioastronomia, Bologna, Italy
| | - Clécio R Bom
- Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, Brazil
- Centro Federal de Educação Tecnológica Celso Suckow da Fonseca, Rodovia Mário Covas, Itaguaí, Brazil
| | | | - Alberto J Castro-Tirado
- Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain
- Unidad Asociada al CSIC Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingenierías Industriales, Universidad de Málaga, Málaga, Spain
| | - Zong-Kai Peng
- Institute for Frontier in Astronomy and Astrophysics, Beijing Normal University, Beijing, China
- Department of Astronomy, Beijing Normal University, Beijing, China
| | - Simone Dichiara
- Department of Astronomy and Astrophysics, The Pennsylvania State University, University Park, PA, USA
| | - Geoffrey Ryan
- Perimeter Institute for Theoretical Physics, Waterloo, Ontario, Canada
| | | | - Zi-Gao Dai
- Department of Astronomy, School of Physical Sciences, University of Science and Technology of China, Hefei, China
| | - Seo-Won Chang
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Hyeonho Choi
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Kishalay De
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Youdong Hu
- Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain
| | - Charles D Kilpatrick
- Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA) and Department of Physics and Astronomy, Northwestern University, Evanston, IL, USA
| | - Alexander Kutyrev
- Department of Astronomy, University of Maryland, College Park, MD, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Mankeun Jeong
- SNU Astronomy Research Center, Astronomy Program, Department of Physics and Astronomy, Seoul National University, Seoul, Republic of Korea
| | - Chung-Uk Lee
- Korea Astronomy and Space Science Institute, Daejeon, Republic of Korea
| | - Martin Makler
- Centro Brasileiro de Pesquisas Físicas, Rio de Janeiro, Brazil
- International Center for Advanced Studies and Instituto de Ciencias Físicas, ECyT-UNSAM and CONICET, Buenos Aires, Argentina
| | | | | |
Collapse
|
3
|
Castro-Tirado AJ, Østgaard N, Göǧüş E, Sánchez-Gil C, Pascual-Granado J, Reglero V, Mezentsev A, Gabler M, Marisaldi M, Neubert T, Budtz-Jørgensen C, Lindanger A, Sarria D, Kuvvetli I, Cerdá-Durán P, Navarro-González J, Font JA, Zhang BB, Lund N, Oxborrow CA, Brandt S, Caballero-García MD, Carrasco-García IM, Castellón A, Castro Tirado MA, Christiansen F, Eyles CJ, Fernández-García E, Genov G, Guziy S, Hu YD, Nicuesa Guelbenzu A, Pandey SB, Peng ZK, Pérez Del Pulgar C, Reina Terol AJ, Rodríguez E, Sánchez-Ramírez R, Sun T, Ullaland K, Yang S. Very-high-frequency oscillations in the main peak of a magnetar giant flare. Nature 2021; 600:621-624. [PMID: 34937892 DOI: 10.1038/s41586-021-04101-1] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/17/2020] [Accepted: 10/06/2021] [Indexed: 11/09/2022]
Abstract
Magnetars are strongly magnetized, isolated neutron stars1-3 with magnetic fields up to around 1015 gauss, luminosities of approximately 1031-1036 ergs per second and rotation periods of about 0.3-12.0 s. Very energetic giant flares from galactic magnetars (peak luminosities of 1044-1047 ergs per second, lasting approximately 0.1 s) have been detected in hard X-rays and soft γ-rays4, and only one has been detected from outside our galaxy5. During such giant flares, quasi-periodic oscillations (QPOs) with low (less than 150 hertz) and high (greater than 500 hertz) frequencies have been observed6-9, but their statistical significance has been questioned10. High-frequency QPOs have been seen only during the tail phase of the flare9. Here we report the observation of two broad QPOs at approximately 2,132 hertz and 4,250 hertz in the main peak of a giant γ-ray flare11 in the direction of the NGC 253 galaxy12-17, disappearing after 3.5 milliseconds. The flare was detected on 15 April 2020 by the Atmosphere-Space Interactions Monitor instrument18,19 aboard the International Space Station, which was the only instrument that recorded the main burst phase (0.8-3.2 milliseconds) in the full energy range (50 × 103 to 40 × 106 electronvolts) without suffering from saturation effects such as deadtime and pile-up. Along with sudden spectral variations, these extremely high-frequency oscillations in the burst peak are a crucial component that will aid our understanding of magnetar giant flares.
Collapse
Affiliation(s)
- A J Castro-Tirado
- Instituto de Astrofísica de Andalucía del Consejo Superior de Investigaciones Científicas (IAA-CSIC), Granada, Spain.,Unidad Asociada al CSIC Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingeniería Industrial, Universidad de Málaga, Málaga, Spain
| | - N Østgaard
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway.
| | - E Göǧüş
- Faculty of Engineering and Natural Sciences, Sabancı University, Istanbul, Turkey.
| | - C Sánchez-Gil
- Departamento de Estadística e Investigación Operativa, Universidad de Cádiz, Puerto Real, Spain
| | - J Pascual-Granado
- Instituto de Astrofísica de Andalucía del Consejo Superior de Investigaciones Científicas (IAA-CSIC), Granada, Spain
| | - V Reglero
- Departamento de Astronomía y Astrofísica, Universitat de València, Valencia, Spain.,Imaging Processing Laboratory, Universitat de València, Valencia, Spain
| | - A Mezentsev
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway.
| | - M Gabler
- Departamento de Astronomía y Astrofísica, Universitat de València, Valencia, Spain.
| | - M Marisaldi
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway. .,National Institute for Astrophysics, Osservatorio di Astrofisica e Scienzia dello Spazio, Bologna, Italy.
| | - T Neubert
- DTU Space, Technical University of Denmark, Kongens Lyngby, Denmark
| | | | - A Lindanger
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway
| | - D Sarria
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway
| | - I Kuvvetli
- DTU Space, Technical University of Denmark, Kongens Lyngby, Denmark
| | - P Cerdá-Durán
- Departamento de Astronomía y Astrofísica, Universitat de València, Valencia, Spain
| | | | - J A Font
- Departamento de Astronomía y Astrofísica, Universitat de València, Valencia, Spain.,Observatori Astronòmic, Universitat de València, Valencia, Spain
| | - B-B Zhang
- School of Astronomy and Space Science, Nanjing University, Nanjing, China.,Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing, China.,Department of Physics and Astronomy, University of Nevada, Las Vegas, Las Vegas, NV, USA
| | - N Lund
- DTU Space, Technical University of Denmark, Kongens Lyngby, Denmark
| | - C A Oxborrow
- DTU Space, Technical University of Denmark, Kongens Lyngby, Denmark
| | - S Brandt
- DTU Space, Technical University of Denmark, Kongens Lyngby, Denmark
| | - M D Caballero-García
- Instituto de Astrofísica de Andalucía del Consejo Superior de Investigaciones Científicas (IAA-CSIC), Granada, Spain
| | | | - A Castellón
- Unidad Asociada al CSIC Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingeniería Industrial, Universidad de Málaga, Málaga, Spain.,Departamento de Álgebra, Geometría y Topología, Facultad de Ciencias, Universidad de Málaga, Málaga, Spain
| | - M A Castro Tirado
- Instituto de Astrofísica de Andalucía del Consejo Superior de Investigaciones Científicas (IAA-CSIC), Granada, Spain.,Escuela Técnica Superior de Arquitectura, Universidad de Málaga, Málaga, Spain
| | - F Christiansen
- DTU Space, Technical University of Denmark, Kongens Lyngby, Denmark
| | - C J Eyles
- Imaging Processing Laboratory, Universitat de València, Valencia, Spain
| | - E Fernández-García
- Instituto de Astrofísica de Andalucía del Consejo Superior de Investigaciones Científicas (IAA-CSIC), Granada, Spain
| | - G Genov
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway
| | - S Guziy
- Astronomical Observatory, Mykolaiv National University, Mykolaiv, Ukraine.,Research Institute, Mykolaiv Astronomical Observatory, Mykolaiv, Ukraine
| | - Y-D Hu
- Instituto de Astrofísica de Andalucía del Consejo Superior de Investigaciones Científicas (IAA-CSIC), Granada, Spain.,Facultad de Ciencias, Universidad de Granada, Granada, Spain
| | | | - S B Pandey
- Aryabhatta Research Institute of Observational Sciences (ARIES), Nainital, India
| | - Z-K Peng
- School of Astronomy and Space Science, Nanjing University, Nanjing, China.,Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing, China
| | - C Pérez Del Pulgar
- Unidad Asociada al CSIC Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingeniería Industrial, Universidad de Málaga, Málaga, Spain
| | - A J Reina Terol
- Unidad Asociada al CSIC Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingeniería Industrial, Universidad de Málaga, Málaga, Spain
| | - E Rodríguez
- Instituto de Astrofísica de Andalucía del Consejo Superior de Investigaciones Científicas (IAA-CSIC), Granada, Spain
| | | | - T Sun
- Instituto de Astrofísica de Andalucía del Consejo Superior de Investigaciones Científicas (IAA-CSIC), Granada, Spain.,Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China.,School of Astronomy and Space Science, University of Science and Technology of China, Hefei, China
| | - K Ullaland
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway
| | - S Yang
- Birkeland Centre for Space Science, Department of Physics and Technology, University of Bergen, Bergen, Norway
| |
Collapse
|
4
|
Lin L, Zhang CF, Wang P, Gao H, Guan X, Han JL, Jiang JC, Jiang P, Lee KJ, Li D, Men YP, Miao CC, Niu CH, Niu JR, Sun C, Wang BJ, Wang ZL, Xu H, Xu JL, Xu JW, Yang YH, Yang YP, Yu W, Zhang B, Zhang BB, Zhou DJ, Zhu WW, Castro-Tirado AJ, Dai ZG, Ge MY, Hu YD, Li CK, Li Y, Li Z, Liang EW, Jia SM, Querel R, Shao L, Wang FY, Wang XG, Wu XF, Xiong SL, Xu RX, Yang YS, Zhang GQ, Zhang SN, Zheng TC, Zou JH. No pulsed radio emission during a bursting phase of a Galactic magnetar. Nature 2020; 587:63-65. [PMID: 33149293 DOI: 10.1038/s41586-020-2839-y] [Citation(s) in RCA: 66] [Impact Index Per Article: 16.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/08/2020] [Accepted: 08/31/2020] [Indexed: 11/10/2022]
Abstract
Fast radio bursts (FRBs) are millisecond-duration radio transients of unknown physical origin observed at extragalactic distances1-3. It has long been speculated that magnetars are the engine powering repeating bursts from FRB sources4-13, but no convincing evidence has been collected so far14. Recently, the Galactic magnetar SRG 1935+2154 entered an active phase by emitting intense soft γ-ray bursts15. One FRB-like event with two peaks (FRB 200428) and a luminosity slightly lower than the faintest extragalactic FRBs was detected from the source, in association with a soft γ-ray/hard-X-ray flare18-21. Here we report an eight-hour targeted radio observational campaign comprising four sessions and assisted by multi-wavelength (optical and hard-X-ray) data. During the third session, 29 soft-γ-ray repeater (SGR) bursts were detected in γ-ray energies. Throughout the observing period, we detected no single dispersed pulsed emission coincident with the arrivals of SGR bursts, but unfortunately we were not observing when the FRB was detected. The non-detection places a fluence upper limit that is eight orders of magnitude lower than the fluence of FRB 200428. Our results suggest that FRB-SGR burst associations are rare. FRBs may be highly relativistic and geometrically beamed, or FRB-like events associated with SGR bursts may have narrow spectra and characteristic frequencies outside the observed band. It is also possible that the physical conditions required to achieve coherent radiation in SGR bursts are difficult to satisfy, and that only under extreme conditions could an FRB be associated with an SGR burst.
Collapse
Affiliation(s)
- L Lin
- Department of Astronomy, Beijing Normal University, Beijing, People's Republic of China
| | - C F Zhang
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - P Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - H Gao
- Department of Astronomy, Beijing Normal University, Beijing, People's Republic of China
| | - X Guan
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J L Han
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China.,University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J C Jiang
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - P Jiang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - K J Lee
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China. .,Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, People's Republic of China.
| | - D Li
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China. .,University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China.
| | - Y P Men
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - C C Miao
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - C H Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J R Niu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - C Sun
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - B J Wang
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - Z L Wang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - H Xu
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J L Xu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - J W Xu
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - Y H Yang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China
| | - Y P Yang
- South-Western Institute for Astronomy Research, Yunnan University, Kunming, People's Republic of China
| | - W Yu
- Shanghai Astronomical Observatory, Chinese Academy of Science, Shanghai, People's Republic of China
| | - B Zhang
- Department of Physics and Astronomy, University of Nevada, Las Vegas, NV, USA.
| | - B-B Zhang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China.,Department of Physics and Astronomy, University of Nevada, Las Vegas, NV, USA.,Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, People's Republic of China
| | - D J Zhou
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China.,University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - W W Zhu
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - A J Castro-Tirado
- Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain.,Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingenierías, Universidad de Málaga, Málaga, Spain
| | - Z G Dai
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China.,Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, People's Republic of China
| | - M Y Ge
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - Y D Hu
- Instituto de Astrofísica de Andalucía (IAA-CSIC), Granada, Spain.,Facultad de Ciencias, Universidad de Granada, Granada, Spain
| | - C K Li
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - Y Li
- University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China.,Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, People's Republic of China
| | - Z Li
- Department of Astronomy, Beijing Normal University, Beijing, People's Republic of China
| | - E W Liang
- Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning, People's Republic of China
| | - S M Jia
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - R Querel
- National Institute of Water and Atmospheric Research (NIWA), Lauder, New Zealand
| | - L Shao
- College of Physics, Hebei Normal University, Shijiazhuang, People's Republic of China
| | - F Y Wang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China.,Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, Nanjing, People's Republic of China
| | - X G Wang
- Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning, People's Republic of China
| | - X F Wu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, People's Republic of China
| | - S L Xiong
- Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - R X Xu
- Department of Astronomy, Peking University, Beijing, People's Republic of China.,Kavli Institute for Astronomy and Astrophysics, Peking University, Beijing, People's Republic of China
| | - Y-S Yang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China
| | - G Q Zhang
- School of Astronomy and Space Science, Nanjing University, Nanjing, People's Republic of China
| | - S N Zhang
- National Astronomical Observatories, Chinese Academy of Sciences, Beijing, People's Republic of China.,University of Chinese Academy of Sciences, Chinese Academy of Sciences, Beijing, People's Republic of China.,Key Laboratory of Particle Astrophysics, Institute of High Energy Physics, Chinese Academy of Sciences, Beijing, People's Republic of China
| | - T C Zheng
- Guangxi Key Laboratory for Relativistic Astrophysics, School of Physical Science and Technology, Guangxi University, Nanning, People's Republic of China
| | - J-H Zou
- College of Physics, Hebei Normal University, Shijiazhuang, People's Republic of China
| |
Collapse
|
5
|
Zhang BB, Zhang B, Sun H, Lei WH, Gao H, Li Y, Shao L, Zhao Y, Hu YD, Lü HJ, Wu XF, Fan XL, Wang G, Castro-Tirado AJ, Zhang S, Yu BY, Cao YY, Liang EW. A peculiar low-luminosity short gamma-ray burst from a double neutron star merger progenitor. Nat Commun 2018; 9:447. [PMID: 29386633 PMCID: PMC5792494 DOI: 10.1038/s41467-018-02847-3] [Citation(s) in RCA: 101] [Impact Index Per Article: 16.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Download PDF] [Figures] [Journal Information] [Subscribe] [Scholar Register] [Received: 12/13/2017] [Accepted: 01/04/2018] [Indexed: 11/11/2022] Open
Abstract
Double neutron star (DNS) merger events are promising candidates of short gamma-ray burst (sGRB) progenitors as well as high-frequency gravitational wave (GW) emitters. On August 17, 2017, such a coinciding event was detected by both the LIGO-Virgo gravitational wave detector network as GW170817 and Gamma-Ray Monitor on board NASA’s Fermi Space Telescope as GRB 170817A. Here, we show that the fluence and spectral peak energy of this sGRB fall into the lower portion of the distributions of known sGRBs. Its peak isotropic luminosity is abnormally low. The estimated event rate density above this luminosity is at least \documentclass[12pt]{minimal}
\usepackage{amsmath}
\usepackage{wasysym}
\usepackage{amsfonts}
\usepackage{amssymb}
\usepackage{amsbsy}
\usepackage{mathrsfs}
\usepackage{upgreek}
\setlength{\oddsidemargin}{-69pt}
\begin{document}$$190_{ - 160}^{ + 440}$$\end{document}190-160+440 Gpc−3 yr−1, which is close to but still below the DNS merger event rate density. This event likely originates from a structured jet viewed from a large viewing angle. There are similar faint soft GRBs in the Fermi archival data, a small fraction of which might belong to this new population of nearby, low-luminosity sGRBs. A short-duration gamma-ray burst was detected along with a double neutron start merger gravitational wave by LIGO-Virgo on August 17th 2017. Here, the authors show that the fluence and spectral peak energy of this event fall into the lower portion of the distribution of known short-duration gamma-ray bursts.
Collapse
Affiliation(s)
- B-B Zhang
- School of Astronomy and Space Science, Nanjing University, 210093, Nanjing, China. .,Instituto de Astrofísica de Andalucía (IAA-CSIC), P.O. Box 03004, E-18080, Granada, Spain. .,Key Laboratory of Modern Astronomy and Astrophysics, Nanjing University, Ministry of Education, Nanjing, 210093, China.
| | - B Zhang
- Department of Physics and Astronomy, University of Nevada, Las Vegas, NV, 89154, USA. .,Department of Astronomy, School of Physics, Peking University, 100871, Beijing, China. .,Kavli Institute for Astronomy and Astrophysics, Peking University, 100871, Beijing, China.
| | - H Sun
- National Astronomical Observatories, Chinese Academy of Sciences, A20 Datun Road, 100012, Beijing, China
| | - W-H Lei
- School of Physics, Huazhong University of Science and Technology, 430074, Wuhan, China
| | - H Gao
- Department of Astronomy, Beijing Normal University, 100875, Beijing, China
| | - Y Li
- Kavli Institute for Astronomy and Astrophysics, Peking University, 100871, Beijing, China
| | - L Shao
- Department of Space Sciences and Astronomy, Hebei Normal University, 050024, Shijiazhuang, China.,Purple Mountain Observatory, Chinese Academy of Sciences, 210008, Nanjing, China
| | - Y Zhao
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL, 32611, USA
| | - Y-D Hu
- Instituto de Astrofísica de Andalucía (IAA-CSIC), P.O. Box 03004, E-18080, Granada, Spain.,Facultad de Ciencias, Campus Fuentenueva s/n, Universidad de Granada, E-18071, Granada, Spain
| | - H-J Lü
- Guangxi Key Laboratory for Relativistic Astrophysics, Department of Physics, Guangxi University, 530004, Nanning, China
| | - X-F Wu
- Purple Mountain Observatory, Chinese Academy of Sciences, 210008, Nanjing, China.,School of Astronomy and Space Science, , University of Science and Technology of China, 230026, Hefei, China
| | - X-L Fan
- School of Physics and Electronics Information, Hubei University of Education, 430205, Wuhan, China
| | - G Wang
- Gran Sasso Science Institute (INFN), Via Francesco Crispi 7, I-67100, LAquila, Italy.,INFN - Sezione di Pisa Edificio C, Largo Bruno Pontecorvo, 3, 56127, Pisa, Italy
| | - A J Castro-Tirado
- Instituto de Astrofísica de Andalucía (IAA-CSIC), P.O. Box 03004, E-18080, Granada, Spain.,Departamento de Ingeniería de Sistemas y Automática, Escuela de Ingenierías, Universidad de Málaga, C. Dr. Ortiz Ramos sn, 29071, Málaga, Spain
| | - S Zhang
- Department of Space Sciences and Astronomy, Hebei Normal University, 050024, Shijiazhuang, China
| | - B-Y Yu
- Department of Space Sciences and Astronomy, Hebei Normal University, 050024, Shijiazhuang, China
| | - Y-Y Cao
- Department of Space Sciences and Astronomy, Hebei Normal University, 050024, Shijiazhuang, China
| | - E-W Liang
- Guangxi Key Laboratory for Relativistic Astrophysics, Department of Physics, Guangxi University, 530004, Nanning, China
| |
Collapse
|
6
|
Dallilar Y, Eikenberry SS, Garner A, Stelter RD, Gottlieb A, Gandhi P, Casella P, Dhillon VS, Marsh TR, Littlefair SP, Hardy L, Fender R, Mooley K, Walton DJ, Fuerst F, Bachetti M, Castro-Tirado AJ, Charcos M, Edwards ML, Lasso-Cabrera NM, Marin-Franch A, Raines SN, Ackley K, Bennett JG, Cenarro AJ, Chinn B, Donoso HV, Frommeyer R, Hanna K, Herlevich MD, Julian J, Miller P, Mullin S, Murphey CH, Packham C, Varosi F, Vega C, Warner C, Ramaprakash AN, Burse M, Punnadi S, Chordia P, Gerarts A, de Paz Martín H, Calero MM, Scarpa R, Acosta SF, Hernández Sánchez WM, Siegel B, Pérez FF, Viera Martín HD, Rodríguez Losada JA, Nuñez A, Tejero Á, Martín González CE, Rodríguez CC, Molgó J, Rodriguez JE, Cáceres JIF, Rodríguez García LA, Lopez MH, Dominguez R, Gaggstatter T, Lavers AC, Geier S, Pessev P, Sarajedini A. A precise measurement of the magnetic field in the corona of the black hole binary V404 Cygni. Science 2017; 358:1299-1302. [PMID: 29217570 DOI: 10.1126/science.aan0249] [Citation(s) in RCA: 19] [Impact Index Per Article: 2.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/22/2017] [Accepted: 11/03/2017] [Indexed: 11/02/2022]
Abstract
Observations of binary stars containing an accreting black hole or neutron star often show x-ray emission extending to high energies (>10 kilo--electron volts), which is ascribed to an accretion disk corona of energetic particles akin to those seen in the solar corona. Despite their ubiquity, the physical conditions in accretion disk coronae remain poorly constrained. Using simultaneous infrared, optical, x-ray, and radio observations of the Galactic black hole system V404 Cygni, showing a rapid synchrotron cooling event in its 2015 outburst, we present a precise 461 ± 12 gauss magnetic field measurement in the corona. This measurement is substantially lower than previous estimates for such systems, providing constraints on physical models of accretion physics in black hole and neutron star binary systems.
Collapse
Affiliation(s)
- Yigit Dallilar
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA.
| | - Stephen S Eikenberry
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA.
| | - Alan Garner
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Richard D Stelter
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Amy Gottlieb
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Poshak Gandhi
- Department of Physics and Astronomy, University of Southampton, Highfield, Southampton SO17 1BJ, UK
| | - Piergiorgio Casella
- Istituto Nazionale di Astrofisica-Osservatorio Astronomico di Roma, Via Frascati 33, I-00040 Monteporzio Catone, Italy
| | - Vik S Dhillon
- Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, UK.,Instituto de Astrofisica de Canarias, 38205 La Laguna, Santa Cruz de Tenerife, Spain
| | - Tom R Marsh
- Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK
| | - Stuart P Littlefair
- Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, UK
| | - Liam Hardy
- Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, UK
| | - Rob Fender
- Division of Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
| | - Kunal Mooley
- Division of Astrophysics, Department of Physics, University of Oxford, Keble Road, Oxford OX1 3RH, UK
| | - Dominic J Walton
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
| | - Felix Fuerst
- Space Radiation Laboratory, California Institute of Technology, Pasadena, CA 91125, USA.,European Space Astronomy Centre, Operations Department, Villanueva de la Cañada, Madrid, Spain
| | - Matteo Bachetti
- Istituto Nazionale di Astrofisica-Osservatorio Astronomico di Cagliari, via della Scienza 5, 09047 Selargius, Italy
| | - A J Castro-Tirado
- Instituto de Astrofísica de Andalucía-Consejo Superior de Investigaciones Científicas, E-18008 Granada, Spain.,Unidad Asociada Departamento de Ingeniería de Sistemas y Automática, Universidad de Málaga, 29071 Malaga, Spain
| | - Miguel Charcos
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Michelle L Edwards
- Large Binocular Telescope Observatory, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA
| | | | | | - S Nicholas Raines
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Kendall Ackley
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - John G Bennett
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - A Javier Cenarro
- Centro de Estudios de Física del Cosmos de Aragón, 44001 Teruel, Aragón, Spain
| | - Brian Chinn
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - H Veronica Donoso
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Raymond Frommeyer
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Kevin Hanna
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Michael D Herlevich
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Jeff Julian
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Paola Miller
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Scott Mullin
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Charles H Murphey
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Chris Packham
- Department of Physics and Astronomy, University of Texas at San Antonio, One UTSA Circle, San Antonio, TX 78249, USA.,National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan
| | - Frank Varosi
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Claudia Vega
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - Craig Warner
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| | - A N Ramaprakash
- Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune-411007, India
| | - Mahesh Burse
- Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune-411007, India
| | - Sujit Punnadi
- Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune-411007, India
| | - Pravin Chordia
- Inter-University Centre for Astronomy and Astrophysics, Post Bag 4, Ganeshkhind, Pune-411007, India
| | - Andreas Gerarts
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Héctor de Paz Martín
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - María Martín Calero
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Riccardo Scarpa
- Instituto de Astrofisica de Canarias, 38205 La Laguna, Santa Cruz de Tenerife, Spain.,Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | | | | | - Benjamin Siegel
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | | | - Himar D Viera Martín
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | | | - Agustín Nuñez
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Álvaro Tejero
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | | | | | - Jordi Molgó
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - J Esteban Rodriguez
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | | | | | - Manuel Huertas Lopez
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Raul Dominguez
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Tim Gaggstatter
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Antonio Cabrera Lavers
- Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Stefan Geier
- Instituto de Astrofisica de Canarias, 38205 La Laguna, Santa Cruz de Tenerife, Spain.,Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Peter Pessev
- Instituto de Astrofisica de Canarias, 38205 La Laguna, Santa Cruz de Tenerife, Spain.,Gran Telescopio de Canarias, Cuesta de San José s/n, E-38712, Breña Baja, La Palma, Spain
| | - Ata Sarajedini
- Department of Astronomy, University of Florida, 211 Bryant Space Science Center, Gainesville, FL 32611, USA
| |
Collapse
|
7
|
Zhang BB, Zhang B, Castro-Tirado AJ. CENTRAL ENGINE MEMORY OF GAMMA-RAY BURSTS AND SOFT GAMMA-RAY REPEATERS. ApJ 2016; 820:L32. [DOI: 10.3847/2041-8205/820/2/l32] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 09/01/2023]
|
8
|
Rabaza O, Jelinek M, Castro-Tirado AJ, Cunniffe R, Zeman J, Hudec R, Sabau-Graziati L, Ruedas-Sánchez J. Compact low resolution spectrograph, an imaging and long slit spectrograph for robotic telescopes. Rev Sci Instrum 2013; 84:114501. [PMID: 24289416 DOI: 10.1063/1.4827895] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/02/2023]
Abstract
The COmpact LOw REsolution Spectrograph (COLORES) is a compact and lightweight (13 kg) f/8 imaging spectrograph designed for robotic telescopes, now installed and operating on the TELMA, a rapid-slewing 60 cm telescope of the BOOTES-2 observatory in Málaga (Spain). COLORES is a multi-mode instrument that enables the observer to seamlessly switch between low-dispersion spectroscopy and direct imaging modes during an observation. In this paper, we describe the instrument and its development, from the initial scientific requirements through the optical design process to final configuration with theoretical performance calculations. The mechanical and electronic design is described, methods of calibration are discussed and early laboratory and scientific results are shown.
Collapse
Affiliation(s)
- O Rabaza
- Department of Civil Engineering, University of Granada, Severo Ochoa Str. s∕n, 18071 Granada, Spain
| | | | | | | | | | | | | | | |
Collapse
|
9
|
Jeong S, Nam JW, Ahn KB, Park IH, Kim SW, Lee J, Lim H, Brandt S, Budtz-Jørgensen C, Castro-Tirado AJ, Chen P, Cho MH, Choi JN, Grossan B, Huang MA, Jung A, Kim JE, Kim MB, Kim YW, Linder EV, Min KW, Na GW, Panasyuk MI, Ripa J, Reglero V, Smoot GF, Suh JE, Svertilov S, Vedenkin N, Yashin I. Slewing Mirror Telescope optics for the early observation of UV/optical photons from Gamma-Ray Bursts. Opt Express 2013; 21:2263-2278. [PMID: 23389206 DOI: 10.1364/oe.21.002263] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [MESH Headings] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/01/2023]
Abstract
We report on design, manufacture, and testing of a Slewing Mirror Telescope (SMT), the first of its kind and a part of Ultra-Fast Flash Observatory-pathfinder (UFFO-p) for space-based prompt measurement of early UV/optical light curves from Gamma-Ray Bursts (GRBs). Using a fast slewing mirror of 150 mm diameter mounted on a 2 axis gimbal stage, SMT can deliver the images of GRB optical counterparts to the intensified CCD detector within 1.5~1.8 s over ± 35 degrees in the slewing field of view. Its Ritchey-Chrétien telescope of 100 mm diameter provides a 17 × 17 arcmin² instantaneous field of view. Technical details of design, construction, the laboratory performance tests in space environments for this unique SMT are described in conjunction with the plan for in-orbit operation onboard the Lomonosov satellite in 2013.
Collapse
Affiliation(s)
- S Jeong
- Department of Physics, Ewha Womans University, 11-1 Daehyun-dong, Seoul 120-750, South Korea
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
10
|
Pian E, Mazzali PA, Masetti N, Ferrero P, Klose S, Palazzi E, Ramirez-Ruiz E, Woosley SE, Kouveliotou C, Deng J, Filippenko AV, Foley RJ, Fynbo JPU, Kann DA, Li W, Hjorth J, Nomoto K, Patat F, Sauer DN, Sollerman J, Vreeswijk PM, Guenther EW, Levan A, O'Brien P, Tanvir NR, Wijers RAMJ, Dumas C, Hainaut O, Wong DS, Baade D, Wang L, Amati L, Cappellaro E, Castro-Tirado AJ, Ellison S, Frontera F, Fruchter AS, Greiner J, Kawabata K, Ledoux C, Maeda K, Møller P, Nicastro L, Rol E, Starling R. An optical supernova associated with the X-ray flash XRF 060218. Nature 2006; 442:1011-3. [PMID: 16943831 DOI: 10.1038/nature05082] [Citation(s) in RCA: 393] [Impact Index Per Article: 21.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 03/20/2006] [Accepted: 07/10/2006] [Indexed: 11/09/2022]
Abstract
Long-duration gamma-ray bursts (GRBs) are associated with type Ic supernovae that are more luminous than average and that eject material at very high velocities. Less-luminous supernovae were not hitherto known to be associated with GRBs, and therefore GRB-supernovae were thought to be rare events. Whether X-ray flashes--analogues of GRBs, but with lower luminosities and fewer gamma-rays--can also be associated with supernovae, and whether they are intrinsically 'weak' events or typical GRBs viewed off the axis of the burst, is unclear. Here we report the optical discovery and follow-up observations of the type Ic supernova SN 2006aj associated with X-ray flash XRF 060218. Supernova 2006aj is intrinsically less luminous than the GRB-supernovae, but more luminous than many supernovae not accompanied by a GRB. The ejecta velocities derived from our spectra are intermediate between these two groups, which is consistent with the weakness of both the GRB output and the supernova radio flux. Our data, combined with radio and X-ray observations, suggest that XRF 060218 is an intrinsically weak and soft event, rather than a classical GRB observed off-axis. This extends the GRB-supernova connection to X-ray flashes and fainter supernovae, implying a common origin. Events such as XRF 060218 are probably more numerous than GRB-supernovae.
Collapse
Affiliation(s)
- E Pian
- Istituto Nazionale di Astrofisica, Trieste Astronomical Observatory, via G. B. Tiepolo 11, I-34131 Trieste, Italy.
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
11
|
Fruchter AS, Levan AJ, Strolger L, Vreeswijk PM, Thorsett SE, Bersier D, Burud I, Castro Cerón JM, Castro-Tirado AJ, Conselice C, Dahlen T, Ferguson HC, Fynbo JPU, Garnavich PM, Gibbons RA, Gorosabel J, Gull TR, Hjorth J, Holland ST, Kouveliotou C, Levay Z, Livio M, Metzger MR, Nugent PE, Petro L, Pian E, Rhoads JE, Riess AG, Sahu KC, Smette A, Tanvir NR, Wijers RAMJ, Woosley SE. Long gamma-ray bursts and core-collapse supernovae have different environments. Nature 2006; 441:463-8. [PMID: 16688183 DOI: 10.1038/nature04787] [Citation(s) in RCA: 614] [Impact Index Per Article: 34.1] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 08/22/2005] [Accepted: 04/05/2006] [Indexed: 11/08/2022]
Abstract
When massive stars exhaust their fuel, they collapse and often produce the extraordinarily bright explosions known as core-collapse supernovae. On occasion, this stellar collapse also powers an even more brilliant relativistic explosion known as a long-duration gamma-ray burst. One would then expect that these long gamma-ray bursts and core-collapse supernovae should be found in similar galactic environments. Here we show that this expectation is wrong. We find that the gamma-ray bursts are far more concentrated in the very brightest regions of their host galaxies than are the core-collapse supernovae. Furthermore, the host galaxies of the long gamma-ray bursts are significantly fainter and more irregular than the hosts of the core-collapse supernovae. Together these results suggest that long-duration gamma-ray bursts are associated with the most extremely massive stars and may be restricted to galaxies of limited chemical evolution. Our results directly imply that long gamma-ray bursts are relatively rare in galaxies such as our own Milky Way.
Collapse
Affiliation(s)
- A S Fruchter
- Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, Maryland 21218, USA.
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
12
|
Haislip JB, Nysewander MC, Reichart DE, Levan A, Tanvir N, Cenko SB, Fox DB, Price PA, Castro-Tirado AJ, Gorosabel J, Evans CR, Figueredo E, MacLeod CL, Kirschbrown JR, Jelinek M, Guziy S, de Ugarte Postigo A, Cypriano ES, LaCluyze A, Graham J, Priddey R, Chapman R, Rhoads J, Fruchter AS, Lamb DQ, Kouveliotou C, Wijers RAMJ, Bayliss MB, Schmidt BP, Soderberg AM, Kulkarni SR, Harrison FA, Moon DS, Gal-Yam A, Kasliwal MM, Hudec R, Vitek S, Kubanek P, Crain JA, Foster AC, Clemens JC, Bartelme JW, Canterna R, Hartmann DH, Henden AA, Klose S, Park HS, Williams GG, Rol E, O'Brien P, Bersier D, Prada F, Pizarro S, Maturana D, Ugarte P, Alvarez A, Fernandez AJM, Jarvis MJ, Moles M, Alfaro E, Ivarsen KM, Kumar ND, Mack CE, Zdarowicz CM, Gehrels N, Barthelmy S, Burrows DN. A photometric redshift of z = 6.39 ± 0.12 for GRB 050904. Nature 2006; 440:181-3. [PMID: 16525465 DOI: 10.1038/nature04552] [Citation(s) in RCA: 97] [Impact Index Per Article: 5.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/23/2005] [Accepted: 12/12/2005] [Indexed: 11/09/2022]
Abstract
Gamma-ray bursts (GRBs) and their afterglows are the most brilliant transient events in the Universe. Both the bursts themselves and their afterglows have been predicted to be visible out to redshifts of z approximately 20, and therefore to be powerful probes of the early Universe. The burst GRB 000131, at z = 4.50, was hitherto the most distant such event identified. Here we report the discovery of the bright near-infrared afterglow of GRB 050904 (ref. 4). From our measurements of the near-infrared afterglow, and our failure to detect the optical afterglow, we determine the photometric redshift of the burst to be z = 6.39 - 0.12 + 0.11 (refs 5-7). Subsequently, it was measured spectroscopically to be z = 6.29 +/- 0.01, in agreement with our photometric estimate. These results demonstrate that GRBs can be used to trace the star formation, metallicity, and reionization histories of the early Universe.
Collapse
Affiliation(s)
- J B Haislip
- Department of Physics and Astronomy, University of North Carolina at Chapel Hill, Campus Box 3255, Chapel Hill, North Carolina 27599, USA
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
13
|
Hjorth J, Sollerman J, Møller P, Fynbo JPU, Woosley SE, Kouveliotou C, Tanvir NR, Greiner J, Andersen MI, Castro-Tirado AJ, Castro Cerón JM, Fruchter AS, Gorosabel J, Jakobsson P, Kaper L, Klose S, Masetti N, Pedersen H, Pedersen K, Pian E, Palazzi E, Rhoads JE, Rol E, van den Heuvel EPJ, Vreeswijk PM, Watson D, Wijers RAMJ. A very energetic supernova associated with the gamma-ray burst of 29 March 2003. Nature 2003; 423:847-50. [PMID: 12815425 DOI: 10.1038/nature01750] [Citation(s) in RCA: 1127] [Impact Index Per Article: 53.7] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/16/2003] [Accepted: 05/20/2003] [Indexed: 11/09/2022]
Abstract
Over the past five years evidence has mounted that long-duration (>2 s) gamma-ray bursts (GRBs)-the most luminous of all astronomical explosions-signal the collapse of massive stars in our Universe. This evidence was originally based on the probable association of one unusual GRB with a supernova, but now includes the association of GRBs with regions of massive star formation in distant galaxies, the appearance of supernova-like 'bumps' in the optical afterglow light curves of several bursts and lines of freshly synthesized elements in the spectra of a few X-ray afterglows. These observations support, but do not yet conclusively demonstrate, the idea that long-duration GRBs are associated with the deaths of massive stars, presumably arising from core collapse. Here we report evidence that a very energetic supernova (a hypernova) was temporally and spatially coincident with a GRB at redshift z = 0.1685. The timing of the supernova indicates that it exploded within a few days of the GRB, strongly suggesting that core-collapse events can give rise to GRBs, thereby favouring the 'collapsar' model.
Collapse
Affiliation(s)
- Jens Hjorth
- Astronomical Observatory, NBIfAFG, University of Copenhagen, Juliane Maries Vej, DK-2100 Copenhagen Ø, Denmark.
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
14
|
Castro-Tirado AJ, Zapatero-Osorio MR, Caon N, Cairos LM, Hjorth J, Pedersen H, Andersen MI, Gorosabel J, Bartolini C, Guarnieri A, Piccioni A, Frontera F, Masetti N, Palazzi E, Pian E, Greiner J, Hudec R, Sagar R, Pandey AK, Mohan V, Yadav RK, Bjornsson C, Jakobsson P, Burud I, Courbin F, Valentini G, Piersimoni A, Aceituno J, Montoya LM, Pedraz S, Gredel R, Claver CF, Rector TA, Rhoads JE, Walter F, Ott J, Hippelein H, Sàsnchez-Bèjar V, Gutiérrez C, Wei J, Zhou A, Guziy S, Shlyapnikov A, Heise J, Costa E, Feroci M, Piro L. Decay of the GRB 990123 optical afterglow: implications for the fireball model. Science 1999; 283:2069-73. [PMID: 10092226 DOI: 10.1126/science.283.5410.2069] [Citation(s) in RCA: 89] [Impact Index Per Article: 3.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Broad-band (ultraviolet to near-infrared) observations of the intense gamma ray burst GRB 990123 started approximately 8.5 hours after the event and continued until 18 February 1999. When combined with other data, in particular from the Robotic Telescope and Transient Source Experiment (ROTSE) and the Hubble Space Telescope (HST), evidence emerges for a smoothly declining light curve, suggesting some color dependence that could be related to a cooling break passing the ultraviolet-optical band at about 1 day after the high-energy event. The steeper decline rate seen after 1.5 to 2 days may be evidence for a collimated jet pointing toward the observer.
Collapse
Affiliation(s)
- A J Castro-Tirado
- Instituto de Astrofisica de Andalucia, IAA-CSIC, Granada, Spain. Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain. Astronomical Observatory, University of Copenhagen, Copenhagen, Denmark. Nordic Optical Telescope, La Palma, T
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|
15
|
Hjorth J, Bjornsson G, Andersen MI, Caon N, Cairos LM, Castro-Tirado AJ, Osorio MR, Pedersen H, Costa E. Polarimetric constraints on the optical afterglow emission from GRB 990123. Science 1999; 283:2073-5. [PMID: 10092227 DOI: 10.1126/science.283.5410.2073] [Citation(s) in RCA: 41] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Polarization of the optical emission from GRB 990123 was measured on 24.17 January 1999 universal time with the Nordic Optical Telescope. An upper limit of 2.3% on the linear polarization was found. Accurate polarization measurements provide important clues to the blast wave geometry and magnetic field structure of gamma-ray bursts (GRBs). The lack of detectable polarization for GRB 990123 indicates that the optical afterglow was produced by a blast wave of unknown geometry with an insignificant coherent magnetic field or by a beamed outflow at high Lorentz factor seen at a small viewing angle. Such a collimated jet would help solve the problem of energy release in this exceptionally luminous cosmological burst.
Collapse
Affiliation(s)
- J Hjorth
- Astronomical Observatory, University of Copenhagen, Juliane Maries Vej 30, DK-2100 Copenhagen O, Denmark. Science Institute, University of Iceland, Dunhaga 3, IS-107 Reykjavik, Iceland. Nordic Optical Telescope, Ap. 474 St. Cruz de La Palma, E-387
| | | | | | | | | | | | | | | | | |
Collapse
|
16
|
Andersen MI, Castro-Tirado AJ, Hjorth J, Moller P, Pedersen H, Caon N, Cairos LM, Korhonen H, Osorio MR, Perez E, Frontera F. Spectroscopic limits on the distance and energy release of GRB 990123. Science 1999; 283:2075-7. [PMID: 10092228 DOI: 10.1126/science.283.5410.2075] [Citation(s) in RCA: 39] [Impact Index Per Article: 1.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
An optical spectrum of the afterglow from the unusually bright gamma-ray burst GRB 990123 obtained on 24.25 January 1999 universal time showed an absorption system at a redshift of z = 1.600. The absence of a hydrogen Lyman alpha forest sets an upper limit of z < 2.17, whereas ultraviolet photometry indicates an upper limit of z < 2.05. The probability of intersecting an absorption system as strong as the one observed along a random line of sight out to this z is at most a few percent, implying that GRB 990123 was probably at z = 1. 600. Currently favored cosmological parameters imply that an isotropic energy release equivalent to the rest mass of 1.8 neutron stars (4.5 x 10(54) erg) was emitted in gamma rays. Nonisotropic emission, such as intrinsic beaming, may resolve this energy problem.
Collapse
Affiliation(s)
- MI Andersen
- Nordic Optical Telescope, Apartado 474 St. Cruz de La Palma, E-38700 Canarias, Spain. Laboratorio de Astrofisica Espacial y Fisica Fundamental, Instituto Nacional de Tecnica Aeroespacial, Post Office Box 50727, E-28080 Madrid, Spain. Insti
| | | | | | | | | | | | | | | | | | | | | |
Collapse
|
17
|
Castro-Tirado AJ, Gorosabel J, Benitez N, Wolf C, Fockenbrock R, Martinez-Gonzalez E, Kristen H, Broeils A, Pedersen H, Greiner J, Costa E, Feroci M, Piro L, Frontera F, Nicastro L, Palazzi E, Bartolini C, Guarnieri A, Masetti N, Piccioni A, Mignoli M, Wold M, Lacy M, Birkle K, Broadhurst T, Brandt S, Lund N. Photometry and spectroscopy of the GRB 970508 optical counterpart. Science 1998; 279:1011-4. [PMID: 9461429 DOI: 10.1126/science.279.5353.1011] [Citation(s) in RCA: 27] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 02/06/2023]
Abstract
An optical transient within the error box of the gamma ray burst GRB 970508 was imaged 4 hours after the event. It displayed a strong ultraviolet excess, and reached maximum brightness 2 days later. The optical spectra did not show any emission lines, and no variations on time scales of minutes were observed for 1 hour during the decline phase. According to the fireball and afterglow models, the intensity should rise monotonically before the observed optical maximum, but the data indicate that another physical mechanism may be responsible for the constant phase seen during the first hours after the burst.
Collapse
Affiliation(s)
- A J Castro-Tirado
- A. J. Castro-Tirado and J. Gorosabel, Laboratorio de Astrofisica Espacial y Fisica Fundamental, INTA, Madrid, Spain. N. Benitez and E. Martinez-Gonzalez, Instituto de Fisica de Cantabria, Santander, Spain. C. Wolf, R. Fockenbrock, K. Birkle, Ma
| | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | | |
Collapse
|