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Wang王 L灵, Hu M, Wang L, Yang 杨 Y轶, Yang J, Gomez H, Chen S, Hu L, Chen TW, Mo J, Wang X, Baade D, Hoeflich P, Wheeler JC, Pignata G, Burke J, Hiramatsu D, Howell DA, McCully C, Pellegrino C, Galbany L, Hsiao EY, Sand DJ, Zhang J, Uddin SA, Anderson JP, Ashall C, Cheng C, Gromadzki M, Inserra C, Lin H, Morrell N, Morales-Garoffolo A, Müller-Bravo TE, Nicholl M, Gonzalez EP, Phillips MM, Pineda-García J, Sai H, Smith M, Shahbandeh M, Srivastav S, Stritzinger MD, Yang S, Young DR, Yu L, Zhang X. Newly formed dust within the circumstellar environment of SN Ia-CSM 2018evt. NATURE ASTRONOMY 2024; 8:504-519. [PMID: 38659610 PMCID: PMC11035149 DOI: 10.1038/s41550-024-02197-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 11/11/2022] [Accepted: 01/05/2024] [Indexed: 04/26/2024]
Abstract
Dust associated with various stellar sources in galaxies at all cosmic epochs remains a controversial topic, particularly whether supernovae play an important role in dust production. We report evidence of dust formation in the cold, dense shell behind the ejecta-circumstellar medium (CSM) interaction in the Type Ia-CSM supernova (SN) 2018evt three years after the explosion, characterized by a rise in mid-infrared emission accompanied by an accelerated decline in the optical radiation of the SN. Such a dust-formation picture is also corroborated by the concurrent evolution of the profiles of the Hα emission line. Our model suggests enhanced CSM dust concentration at increasing distances from the SN as compared to what can be expected from the density profile of the mass loss from a steady stellar wind. By the time of the last mid-infrared observations at day +1,041, a total amount of 1.2 ± 0.2 × 10-2 M⊙ of new dust has been formed by SN 2018evt, making SN 2018evt one of the most prolific dust factories among supernovae with evidence of dust formation. The unprecedented witness of the intense production procedure of dust may shed light on the perceptions of dust formation in cosmic history.
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Grants
- National Natural Science Foundation of China (National Science Foundation of China)
- This work is sponsored (in part) by the Chinese Academy of Sciences (CAS), through a grant to the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile
- the Major Science and Technology Project of Qinghai Province (2019-ZJ-A10) and the Jiangsu Funding Program for Excellent Postdoctoral Talent.
- National Science Foundation (NSF)
- Y.Y. appreciates the generous financial support provided to the supernova group at U.C. Berkeley (PI: Alexei V. Filippenko) by Gary and Cynthia Bengier, Clark and Sharon Winslow, Sanford Robertson, and numerous other donors.
- China Postdoctoral Science Foundation
- L.H. acknowledges support from Jiangsu Funding Program for Excellent Postdoctoral Talent.
- T.W.C. acknowledges the Yushan Young Fellow Program by the Ministry of Education, Taiwan for the financial support.
- a DOE grant to the Wooten Center for Astrophysical Plasma Properties (WCAPP; PI Don Winget), and by grant G09-20065C from the Chandra Observatory.
- Millennium Science Initiative ICN12_009
- Spanish Ministerio de Ciencia e Innovaci\'on (MCIN), the Agencia Estatal de Investigaci\'on (AEI) 10.13039/501100011033, and the European Social Fund (ESF) "Investing in your future" under the 2019 Ram\'on y Cajal program RYC2019-027683-I and the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cient\'ificas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia Mar\'ia de Maeztu CEX2020-001058-M
- EU Horizon 2020 research and innovation programme under grant agreement No 101004719
- European Union under the 2014-2020 ERDF Operational Programme and by the Department of Economic Transformation, Industry, Knowledge, and Universities of the Regional Government of Andalusia through the FEDER-UCA18-107404 grant
- Spanish Ministerio de Ciencia e Innovaci\'on (MCIN), the Agencia Estatal de Investigaci\'on (AEI) 10.13039/501100011033 under the PID2020-115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cient\'ificas (CSIC) under the PIE project 20215AT016 and the I-LINK 2021 LINKA20409, and the program Unidad de Excelencia Mar\'ia de Maeztu CEX2020-001058-M.
- European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement No.~948381) and by a Fellowship from the Alan Turing Institute.
- a visiting astronomer at the Infrared Telescope Facility, which is operated by the University of Hawaii under contract NNH14CK55B with the National Aeronautics and Space Administration
- Chinese Academy of Sciences (CAS), through a grant to the CAS South America Center for Astronomy (CASSACA) in Santiago, Chile
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Affiliation(s)
- Lingzhi 灵芝 Wang王
- Chinese Academy of Sciences South America Center for Astronomy (CASSACA), National Astronomical Observatories, CAS, Beijing, China
- CAS Key Laboratory of Optical Astronomy, National Astronomical Observatories, Chinese Academy of Sciences, Beijing, China
| | - Maokai Hu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
| | - Lifan Wang
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX USA
| | - Yi 轶 Yang 杨
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
- Department of Astronomy, University of California, Berkeley, CA USA
| | - Jiawen Yang
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX USA
| | - Haley Gomez
- Cardiff Hub for Astrophysics Research and Technology, School of Physics & Astronomy, Cardiff University, Cardiff, UK
| | - Sijie Chen
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX USA
| | - Lei Hu
- Purple Mountain Observatory, Chinese Academy of Sciences, Nanjing, China
- McWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University, Pittsburgh, PA USA
| | - Ting-Wan Chen
- Graduate Institute of Astronomy, National Central University, Jhongli, Taiwan
| | - Jun Mo
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
| | - Xiaofeng Wang
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
- Beijing Planetarium, Beijing Academy of Science and Technology, Beijing, China
| | - Dietrich Baade
- European Organisation for Astronomical Research in the Southern Hemisphere (ESO), Garching b. München, Germany
| | - Peter Hoeflich
- Department of Physics, Florida State University, Tallahassee, FL USA
| | | | - Giuliano Pignata
- Instituto de Alta Investigación, Universidad de Tarapacá, Arica, Chile
- Millennium Institute of Astrophysics (MAS), Santiago, Chile
| | - Jamison Burke
- Las Cumbres Observatory, Goleta, CA USA
- Department of Physics, University of California, Santa Barbara, CA USA
| | - Daichi Hiramatsu
- Center for Astrophysics, Harvard & Smithsonian, Cambridge, MA USA
- The NSF AI Institute for Artificial Intelligence and Fundamental Interactions, Alexandria, VA USA
| | - D. Andrew Howell
- Las Cumbres Observatory, Goleta, CA USA
- Department of Physics, University of California, Santa Barbara, CA USA
| | | | - Craig Pellegrino
- Las Cumbres Observatory, Goleta, CA USA
- Department of Physics, University of California, Santa Barbara, CA USA
| | - Lluís Galbany
- Institute of Space Sciences (ICE, CSIC), Barcelona, Spain
- Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona, Spain
| | - Eric Y. Hsiao
- Department of Physics, Florida State University, Tallahassee, FL USA
| | - David J. Sand
- Department of Astronomy and Steward Observatory, University of Arizona, Tucson, AZ USA
| | - Jujia Zhang
- Yunnan Observatories, Chinese Academy of Sciences, Kunming, China
| | - Syed A. Uddin
- George P. and Cynthia Woods Mitchell Institute for Fundamental Physics and Astronomy, Texas A&M University, Department of Physics and Astronomy, College Station, TX USA
| | - J. P. Anderson
- Millennium Institute of Astrophysics (MAS), Santiago, Chile
- European Southern Observatory, Santiago, Chile
| | - Chris Ashall
- Department of Physics, Virginia Tech, Blacksburg, VA USA
| | - Cheng Cheng
- Chinese Academy of Sciences South America Center for Astronomy (CASSACA), National Astronomical Observatories, CAS, Beijing, China
| | | | - Cosimo Inserra
- Cardiff Hub for Astrophysics Research and Technology, School of Physics & Astronomy, Cardiff University, Cardiff, UK
| | - Han Lin
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
| | - N. Morrell
- Carnegie Observatories, Las Campanas Observatory, La Serena, Chile
| | | | - T. E. Müller-Bravo
- Institute of Space Sciences (ICE, CSIC), Barcelona, Spain
- Institut d’Estudis Espacials de Catalunya (IEEC), Barcelona, Spain
| | - Matt Nicholl
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, UK
| | - Estefania Padilla Gonzalez
- Las Cumbres Observatory, Goleta, CA USA
- Department of Physics, University of California, Santa Barbara, CA USA
| | - M. M. Phillips
- Carnegie Observatories, Las Campanas Observatory, La Serena, Chile
| | - J. Pineda-García
- Millennium Institute of Astrophysics (MAS), Santiago, Chile
- Departamento de Ciencias Físicas, Universidad Andres Bello, Santiago, Chile
| | - Hanna Sai
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
| | - Mathew Smith
- Université de Lyon, Université Claude Bernard Lyon 1, Villeurbanne, France
| | - M. Shahbandeh
- Space Telescope Science Institute, Baltimore, MD USA
| | - Shubham Srivastav
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, UK
| | - M. D. Stritzinger
- Department of Physics and Astronomy, Aarhus University, Aarhus, Denmark
| | - Sheng Yang
- Henan Academy of Sciences, Zhengzhou, China
| | - D. R. Young
- Astrophysics Research Centre, School of Mathematics and Physics, Queen’s University Belfast, Belfast, UK
| | - Lixin Yu
- Chinese Academy of Sciences South America Center for Astronomy (CASSACA), National Astronomical Observatories, CAS, Beijing, China
| | - Xinghan Zhang
- Physics Department and Tsinghua Center for Astrophysics (THCA), Tsinghua University, Beijing, China
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2
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Kenworthy M, Lock S, Kennedy G, van Capelleveen R, Mamajek E, Carone L, Hambsch FJ, Masiero J, Mainzer A, Kirkpatrick JD, Gomez E, Leinhardt Z, Dou J, Tanna P, Sainio A, Barker H, Charbonnel S, Garde O, Le Dû P, Mulato L, Petit T, Rizzo Smith M. A planetary collision afterglow and transit of the resultant debris cloud. Nature 2023; 622:251-254. [PMID: 37821589 DOI: 10.1038/s41586-023-06573-9] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 05/05/2023] [Accepted: 08/25/2023] [Indexed: 10/13/2023]
Abstract
Planets grow in rotating disks of dust and gas around forming stars, some of which can subsequently collide in giant impacts after the gas component is removed from the disk1-3. Monitoring programmes with the warm Spitzer mission have recorded substantial and rapid changes in mid-infrared output for several stars, interpreted as variations in the surface area of warm, dusty material ejected by planetary-scale collisions and heated by the central star: for example, NGC 2354-ID8 (refs. 4,5), HD 166191 (ref. 6) and V488 Persei7. Here we report combined observations of the young (about 300 million years old), solar-like star ASASSN-21qj: an infrared brightening consistent with a blackbody temperature of 1,000 Kelvin and a luminosity that is 4 percent that of the star lasting for about 1,000 days, partially overlapping in time with a complex and deep, wavelength-dependent optical eclipse that lasted for about 500 days. The optical eclipse started 2.5 years after the infrared brightening, implying an orbital period of at least that duration. These observations are consistent with a collision between two exoplanets of several to tens of Earth masses at 2-16 astronomical units from the central star. Such an impact produces a hot, highly extended post-impact remnant with sufficient luminosity to explain the infrared observations. Transit of the impact debris, sheared by orbital motion into a long cloud, causes the subsequent complex eclipse of the host star.
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Affiliation(s)
| | - Simon Lock
- School of Earth Sciences, University of Bristol, Bristol, UK
| | - Grant Kennedy
- Department of Physics, University of Warwick, Coventry, UK
- Centre for Exoplanets and Habitability, University of Warwick, Coventry, UK
| | | | - Eric Mamajek
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
- Department of Physics and Astronomy, University of Rochester, Rochester, NY, USA
| | - Ludmila Carone
- Space Research Institute, Austrian Academy of Sciences, Graz, Austria
| | - Franz-Josef Hambsch
- Vereniging Voor Sterrenkunde, Brugge, Belgium
- American Association of Variable Star Observers, Cambridge, MA, USA
- Bundesdeutsche Arbeitsgemeinschaft für Veränderliche Sterne e.V., Berlin, Germany
| | - Joseph Masiero
- IPAC, California Institute of Technology, Pasadena, CA, USA
| | - Amy Mainzer
- Lunar and Planetary Laboratory, University of Arizona, Tucson, AZ, USA
| | | | - Edward Gomez
- Las Cumbres Observatory, Goleta, CA, USA
- School of Physics and Astronomy, Cardiff University, Cardiff, UK
| | - Zoë Leinhardt
- School of Physics, HH Wills Physics Laboratory, University of Bristol, Bristol, UK
| | - Jingyao Dou
- School of Physics, HH Wills Physics Laboratory, University of Bristol, Bristol, UK
| | - Pavan Tanna
- Institute of Astronomy, University of Cambridge, Cambridge, UK
| | | | | | | | - Olivier Garde
- Southern Spectroscopic Project Observatory Team, Chabons, France
| | - Pascal Le Dû
- Southern Spectroscopic Project Observatory Team, Chabons, France
| | - Lionel Mulato
- Southern Spectroscopic Project Observatory Team, Chabons, France
| | - Thomas Petit
- Southern Spectroscopic Project Observatory Team, Chabons, France
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3
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De K, MacLeod M, Karambelkar V, Jencson JE, Chakrabarty D, Conroy C, Dekany R, Eilers AC, Graham MJ, Hillenbrand LA, Kara E, Kasliwal MM, Kulkarni SR, Lau RM, Loeb A, Masci F, Medford MS, Meisner AM, Patel N, Quiroga-Nuñez LH, Riddle RL, Rusholme B, Simcoe R, Sjouwerman LO, Teague R, Vanderburg A. An infrared transient from a star engulfing a planet. Nature 2023; 617:55-60. [PMID: 37138107 DOI: 10.1038/s41586-023-05842-x] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/29/2022] [Accepted: 02/14/2023] [Indexed: 05/05/2023]
Abstract
Planets with short orbital periods (roughly under 10 days) are common around stars like the Sun1,2. Stars expand as they evolve and thus we expect their close planetary companions to be engulfed, possibly powering luminous mass ejections from the host star3-5. However, this phase has never been directly observed. Here we report observations of ZTF SLRN-2020, a short-lived optical outburst in the Galactic disk accompanied by bright and long-lived infrared emission. The resulting light curve and spectra share striking similarities with those of red novae6,7-a class of eruptions now confirmed8 to arise from mergers of binary stars. Its exceptionally low optical luminosity (approximately 1035 erg s-1) and radiated energy (approximately 6.5 × 1041 erg) point to the engulfment of a planet of fewer than roughly ten Jupiter masses by its Sun-like host star. We estimate the Galactic rate of such subluminous red novae to be roughly between 0.1 and several per year. Future Galactic plane surveys should routinely identify these, showing the demographics of planetary engulfment and the ultimate fate of planets in the inner Solar System.
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Affiliation(s)
- Kishalay De
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA.
| | - Morgan MacLeod
- Center for Astrophysics/Harvard & Smithsonian, Cambridge, MA, USA
| | - Viraj Karambelkar
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Jacob E Jencson
- Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD, USA
| | - Deepto Chakrabarty
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Charlie Conroy
- Center for Astrophysics/Harvard & Smithsonian, Cambridge, MA, USA
| | - Richard Dekany
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
| | - Anna-Christina Eilers
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Matthew J Graham
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Lynne A Hillenbrand
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Erin Kara
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Mansi M Kasliwal
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - S R Kulkarni
- Cahill Center for Astrophysics, California Institute of Technology, Pasadena, CA, USA
| | - Ryan M Lau
- NSF's National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ, USA
| | - Abraham Loeb
- Center for Astrophysics/Harvard & Smithsonian, Cambridge, MA, USA
- Black Hole Initiative, Harvard University, Cambridge, MA, USA
| | - Frank Masci
- IPAC, California Institute of Technology, Pasadena, CA, USA
| | - Michael S Medford
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
- Lawrence Berkeley National Laboratory, Berkeley, CA, USA
| | - Aaron M Meisner
- NSF's National Optical-Infrared Astronomy Research Laboratory, Tucson, AZ, USA
| | - Nimesh Patel
- Center for Astrophysics/Harvard & Smithsonian, Cambridge, MA, USA
| | - Luis Henry Quiroga-Nuñez
- Department of Aerospace, Physics and Space Sciences, Florida Institute of Technology, Melbourne, FL, USA
| | - Reed L Riddle
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
| | - Ben Rusholme
- IPAC, California Institute of Technology, Pasadena, CA, USA
| | - Robert Simcoe
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Loránt O Sjouwerman
- National Radio Astronomy Observatory, Array Operations Center, Socorro, NM, USA
| | - Richard Teague
- Center for Astrophysics/Harvard & Smithsonian, Cambridge, MA, USA
- Department of Earth, Atmospheric, and Planetary Sciences, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Andrew Vanderburg
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
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4
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Kool EC, Johansson J, Sollerman J, Moldón J, Moriya TJ, Mattila S, Schulze S, Chomiuk L, Pérez-Torres M, Harris C, Lundqvist P, Graham M, Yang S, Perley DA, Strotjohann NL, Fremling C, Gal-Yam A, Lezmy J, Maguire K, Omand C, Smith M, Andreoni I, Bellm EC, Bloom JS, De K, Groom SL, Kasliwal MM, Masci FJ, Medford MS, Park S, Purdum J, Reynolds TM, Riddle R, Robert E, Ryder SD, Sharma Y, Stern D. A radio-detected type Ia supernova with helium-rich circumstellar material. Nature 2023; 617:477-482. [PMID: 37198310 PMCID: PMC10191849 DOI: 10.1038/s41586-023-05916-w] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 09/30/2022] [Accepted: 03/02/2023] [Indexed: 05/19/2023]
Abstract
Type Ia supernovae (SNe Ia) are thermonuclear explosions of degenerate white dwarf stars destabilized by mass accretion from a companion star1, but the nature of their progenitors remains poorly understood. A way to discriminate between progenitor systems is through radio observations; a non-degenerate companion star is expected to lose material through winds2 or binary interaction3 before explosion, and the supernova ejecta crashing into this nearby circumstellar material should result in radio synchrotron emission. However, despite extensive efforts, no type Ia supernova (SN Ia) has ever been detected at radio wavelengths, which suggests a clean environment and a companion star that is itself a degenerate white dwarf star4,5. Here we report on the study of SN 2020eyj, a SN Ia showing helium-rich circumstellar material, as demonstrated by its spectral features, infrared emission and, for the first time in a SN Ia to our knowledge, a radio counterpart. On the basis of our modelling, we conclude that the circumstellar material probably originates from a single-degenerate binary system in which a white dwarf accretes material from a helium donor star, an often proposed formation channel for SNe Ia (refs. 6,7). We describe how comprehensive radio follow-up of SN 2020eyj-like SNe Ia can improve the constraints on their progenitor systems.
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Affiliation(s)
- Erik C Kool
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden.
| | - Joel Johansson
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden
- The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, Sweden
| | - Jesper Sollerman
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden
| | - Javier Moldón
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
- Jodrell Bank Centre for Astrophysics, School of Physics and Astronomy, The University of Manchester, Manchester, UK
| | - Takashi J Moriya
- National Astronomical Observatory of Japan, National Institutes of Natural Sciences, Mitaka, Japan
- School of Physics and Astronomy, Faculty of Science, Monash University, Clayton, Victoria, Australia
| | - Seppo Mattila
- Tuorla Observatory, Department of Physics and Astronomy, University of Turku, Turku, Finland
- School of Sciences, European University Cyprus, Nicosia, Cyprus
| | - Steve Schulze
- The Oskar Klein Centre, Department of Physics, Stockholm University, AlbaNova, Stockholm, Sweden
| | - Laura Chomiuk
- Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
| | - Miguel Pérez-Torres
- Instituto de Astrofísica de Andalucía, Consejo Superior de Investigaciones Científicas (CSIC), Granada, Spain
- Facultad de Ciencias, Universidad de Zaragoza, Zaragoza, Spain
| | - Chelsea Harris
- Center for Data Intensive and Time Domain Astronomy, Department of Physics and Astronomy, Michigan State University, East Lansing, MI, USA
| | - Peter Lundqvist
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden
| | - Matthew Graham
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Sheng Yang
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden
- Henan Academy of Sciences, Zhengzhou, China
| | - Daniel A Perley
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK
| | - Nora Linn Strotjohann
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Christoffer Fremling
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Avishay Gal-Yam
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - Jeremy Lezmy
- Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, France
| | - Kate Maguire
- School of Physics, Trinity College Dublin, The University of Dublin, Dublin, Ireland
| | - Conor Omand
- The Oskar Klein Centre, Department of Astronomy, Stockholm University, AlbaNova, Stockholm, Sweden
| | - Mathew Smith
- Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, France
- School of Physics and Astronomy, University of Southampton, Southampton, UK
| | - Igor Andreoni
- Joint Space-Science Institute, University of Maryland, College Park, MD, USA
- Department of Astronomy, University of Maryland, College Park, MD, USA
- Astrophysics Science Division, NASA Goddard Space Flight Center, Greenbelt, MD, USA
| | - Eric C Bellm
- DIRAC Institute, Department of Astronomy, University of Washington, Seattle, WA, USA
| | - Joshua S Bloom
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
- Lawrence Berkeley National Laboratory, Berkeley, CA, USA
| | - Kishalay De
- Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, MA, USA
| | - Steven L Groom
- Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Pasadena, CA, USA
| | - Mansi M Kasliwal
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Frank J Masci
- Infrared Processing and Analysis Center (IPAC), California Institute of Technology, Pasadena, CA, USA
| | - Michael S Medford
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
- Lawrence Berkeley National Laboratory, Berkeley, CA, USA
| | - Sungmin Park
- Ulsan National Institute of Science and Technology, Ulsan, South Korea
| | - Josiah Purdum
- Caltech Optical Observatories, California Institute of Technology, Pasadena, CA, USA
| | - Thomas M Reynolds
- The Cosmic Dawn Center (DAWN), Niels Bohr Institute, University of Copenhagen, Copenhagen, Denmark
| | - Reed Riddle
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Estelle Robert
- Univ. Lyon, Univ. Claude Bernard Lyon 1, CNRS/IN2P3, IP2I Lyon, UMR 5822, Villeurbanne, France
| | - Stuart D Ryder
- School of Mathematical and Physical Sciences, Macquarie University, Sydney, New South Wales, Australia
- Astronomy, Astrophysics and Astrophotonics Research Centre, Macquarie University, Sydney, New South Wales, Australia
| | - Yashvi Sharma
- Division of Physics, Mathematics and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Daniel Stern
- Jet Propulsion Laboratory, California Institute of Technology, Pasadena, CA, USA
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5
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Abstract
The radio-loud quasar CTD 135 (2234+282, J2236+2828) has been proposed as a candidate compact symmetric object (CSO), based on its symmetric radio structure revealed by multi-frequency very long baseline interferometry (VLBI) imaging observations on milliarcsec angular scales. CSOs are known as young jetted active galactic nuclei (AGN) whose relativistic plasma jets are misaligned with respect to the line of sight. The peculiarity of CTD 135 as a CSO candidate was its detection in γ-rays, while the vast majority of known γ-ray emitting AGN are blazars with jets pointing close to our viewing direction. Since only a handful of CSOs are known as γ-ray sources, the unambiguous identification of a single candidate is important for studying this rare class of objects. By collecting and interpreting observational data from the recent literature, we revisit the classification of CTD 135. We present evidence that the object, based on its flat-spectrum radio core with high brightness temperature, variability at multiple wavebands, and infrared colours should be classified as a blazar rather than a CSO.
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6
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Gal-Yam A, Bruch R, Schulze S, Yang Y, Perley DA, Irani I, Sollerman J, Kool EC, Soumagnac MT, Yaron O, Strotjohann NL, Zimmerman E, Barbarino C, Kulkarni SR, Kasliwal MM, De K, Yao Y, Fremling C, Yan L, Ofek EO, Fransson C, Filippenko AV, Zheng W, Brink TG, Copperwheat CM, Foley RJ, Brown J, Siebert M, Leloudas G, Cabrera-Lavers AL, Garcia-Alvarez D, Marante-Barreto A, Frederick S, Hung T, Wheeler JC, Vinkó J, Thomas BP, Graham MJ, Duev DA, Drake AJ, Dekany R, Bellm EC, Rusholme B, Shupe DL, Andreoni I, Sharma Y, Riddle R, van Roestel J, Knezevic N. A WC/WO star exploding within an expanding carbon-oxygen-neon nebula. Nature 2022; 601:201-204. [PMID: 35022591 DOI: 10.1038/s41586-021-04155-1] [Citation(s) in RCA: 17] [Impact Index Per Article: 8.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 04/06/2021] [Accepted: 10/15/2021] [Indexed: 11/09/2022]
Abstract
The final fate of massive stars, and the nature of the compact remnants they leave behind (black holes and neutron stars), are open questions in astrophysics. Many massive stars are stripped of their outer hydrogen envelopes as they evolve. Such Wolf-Rayet stars1 emit strong and rapidly expanding winds with speeds greater than 1,000 kilometres per second. A fraction of this population is also helium-depleted, with spectra dominated by highly ionized emission lines of carbon and oxygen (types WC/WO). Evidence indicates that the most commonly observed supernova explosions that lack hydrogen and helium (types Ib/Ic) cannot result from massive WC/WO stars2,3, leading some to suggest that most such stars collapse directly into black holes without a visible supernova explosion4. Here we report observations of SN 2019hgp, beginning about a day after the explosion. Its short rise time and rapid decline place it among an emerging population of rapidly evolving transients5-8. Spectroscopy reveals a rich set of emission lines indicating that the explosion occurred within a nebula composed of carbon, oxygen and neon. Narrow absorption features show that this material is expanding at high velocities (greater than 1,500 kilometres per second), requiring a compact progenitor. Our observations are consistent with an explosion of a massive WC/WO star, and suggest that massive Wolf-Rayet stars may be the progenitors of some rapidly evolving transients.
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Affiliation(s)
- A Gal-Yam
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.
| | - R Bruch
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - S Schulze
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.,The Oskar Klein Centre, Department of Astronomy and Department of Physics, AlbaNova, Stockholm University, Stockholm, Sweden
| | - Y Yang
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.,Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
| | - D A Perley
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK
| | - I Irani
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - J Sollerman
- The Oskar Klein Centre, Department of Astronomy and Department of Physics, AlbaNova, Stockholm University, Stockholm, Sweden
| | - E C Kool
- The Oskar Klein Centre, Department of Astronomy and Department of Physics, AlbaNova, Stockholm University, Stockholm, Sweden
| | - M T Soumagnac
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel.,Lawrence Berkeley National Laboratory, Berkeley, CA, USA
| | - O Yaron
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - N L Strotjohann
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - E Zimmerman
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - C Barbarino
- The Oskar Klein Centre, Department of Astronomy and Department of Physics, AlbaNova, Stockholm University, Stockholm, Sweden
| | - S R Kulkarni
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - M M Kasliwal
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - K De
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Y Yao
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - C Fremling
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - L Yan
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - E O Ofek
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot, Israel
| | - C Fransson
- The Oskar Klein Centre, Department of Astronomy and Department of Physics, AlbaNova, Stockholm University, Stockholm, Sweden
| | - A V Filippenko
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA.,Miller Institute for Basic Research in Science, University of California, Berkeley, Berkeley, CA, USA
| | - W Zheng
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
| | - T G Brink
- Department of Astronomy, University of California, Berkeley, Berkeley, CA, USA
| | - C M Copperwheat
- Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK
| | - R J Foley
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - J Brown
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - M Siebert
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - G Leloudas
- DTU Space, National Space Institute, Technical University of Denmark, Kongens Lyngby, Denmark
| | | | | | | | - S Frederick
- Department of Astronomy, University of Maryland, College Park, MD, USA
| | - T Hung
- Department of Astronomy and Astrophysics, University of California, Santa Cruz, Santa Cruz, CA, USA
| | - J C Wheeler
- Department of Astronomy, University of Texas at Austin, Austin, TX, USA
| | - J Vinkó
- Department of Astronomy, University of Texas at Austin, Austin, TX, USA.,Konkoly Observatory, ELKH CSFK, Budapest, Hungary.,Department of Optics and Quantum Electronics, University of Szeged, Szeged, Hungary.,ELTE Institute of Physics, Eötvös Loránd University, Budapest, Hungary
| | - B P Thomas
- Department of Astronomy, University of Texas at Austin, Austin, TX, USA
| | - M J Graham
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - D A Duev
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - A J Drake
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - R Dekany
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - E C Bellm
- DIRAC Institute, Department of Astronomy, University of Washington, Seattle, WA, USA
| | - B Rusholme
- IPAC, California Institute of Technology, Pasadena, CA, USA
| | - D L Shupe
- IPAC, California Institute of Technology, Pasadena, CA, USA
| | - I Andreoni
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - Y Sharma
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - R Riddle
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - J van Roestel
- Division of Physics, Mathematics, and Astronomy, California Institute of Technology, Pasadena, CA, USA
| | - N Knezevic
- Department of Astronomy, Faculty of Mathematics, University of Belgrade, Belgrade, Serbia
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Our Peculiar Motion Inferred from Number Counts of Mid Infra Red AGNs and the Discordance Seen with the Cosmological Principle. UNIVERSE 2021. [DOI: 10.3390/universe7040107] [Citation(s) in RCA: 7] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/16/2022]
Abstract
According to the Cosmological Principle, the Universe is isotropic and no preferred direction would be seen by an observer that might be stationary with respect to the expanding cosmic fluid. However, because of observer’s partaking in the solar system peculiar motion, there would appear in some of the observed properties of the Cosmos a dipole anisotropy, which could in turn be exploited to determine the peculiar motion of the solar system. The dipole anisotropy in the Cosmic Microwave Background Radiation (CMBR) has given a peculiar velocity vector 370 km s−1 along l=264∘,b=48∘. However, some other dipoles, for instance, from the number counts, sky brightness or redshift distributions in large samples of distant Active Galactic Nuclei (AGNs), have yielded values of the peculiar velocity many times larger than that from the CMBR, though surprisingly, in all cases the directions agreed with the CMBR dipole. Here we determine our peculiar motion from a sample of 0.28 million AGNs, selected from the Mid Infra Red Active Galactic Nuclei (MIRAGN) sample comprising more than a million sources. From this, we find a peculiar velocity, which is more than four times the CMBR value, although the direction seems to be within ∼2σ of the CMBR dipole. A genuine value of the solar peculiar velocity should be the same irrespective of the data or the technique employed to estimate it. Therefore, such discordant dipole amplitudes might mean that the explanation for these dipoles, including that of the CMBR, might in fact be something else. The observed fact that the direction in all cases is the same, though obtained from completely independent surveys using different instruments and techniques, by different sets of people employing different computing routines, might nonetheless indicate that these dipoles are not merely due to some systematics, otherwise why would they all be pointing along the same direction. It might instead suggest a preferred direction in the Universe, implying a genuine anisotropy, which would violate the Cosmological Principle, the core of the modern cosmology.
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Solar System Peculiar Motion from Mid Infra Red AGNs and Its Cosmological Implications. THE 1ST ELECTRONIC CONFERENCE ON UNIVERSE 2021. [DOI: 10.3390/ecu2021-09270] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.7] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
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9
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Dust Reverberation Mapping in Distant Quasars from Optical and Mid-infrared Imaging Surveys. ACTA ACUST UNITED AC 2020. [DOI: 10.3847/1538-4357/aba59b] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.8] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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11
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Expanding the Y Dwarf Census with Spitzer Follow-up of the Coldest CatWISE Solar Neighborhood Discoveries. ACTA ACUST UNITED AC 2020. [DOI: 10.3847/1538-4357/ab6215] [Citation(s) in RCA: 14] [Impact Index Per Article: 3.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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14
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15
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Kennedy GM, Kenworthy MA, Pepper J, Rodriguez JE, Siverd RJ, Stassun KG, Wyatt MC. The transiting dust clumps in the evolved disc of the Sun-like UXor RZ Psc. ROYAL SOCIETY OPEN SCIENCE 2017; 4:160652. [PMID: 28280566 PMCID: PMC5319332 DOI: 10.1098/rsos.160652] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 09/05/2016] [Accepted: 12/21/2016] [Indexed: 06/06/2023]
Abstract
RZ Psc is a young Sun-like star, long associated with the UXor class of variable stars, which is partially or wholly dimmed by dust clumps several times each year. The system has a bright and variable infrared excess, which has been interpreted as evidence that the dimming events are the passage of asteroidal fragments in front of the host star. Here, we present a decade of optical photometry of RZ Psc and take a critical look at the asteroid belt interpretation. We show that the distribution of light curve gradients is non-uniform for deep events, which we interpret as possible evidence for an asteroidal fragment-like clump structure. However, the clumps are very likely seen above a high optical depth midplane, so the disc's bulk clumpiness is not revealed. While circumstantial evidence suggests an asteroid belt is more plausible than a gas-rich transition disc, the evolutionary status remains uncertain. We suggest that the rarity of Sun-like stars showing disc-related variability may arise because (i) any accretion streams are transparent and/or (ii) turbulence above the inner rim is normally shadowed by a flared outer disc.
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Affiliation(s)
- Grant M. Kennedy
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
| | - Matthew A. Kenworthy
- Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands
| | - Joshua Pepper
- Department of Physics, Lehigh University, 16 Memorial Drive East, Bethlehem, PA 18015, USA
| | - Joseph E. Rodriguez
- Harvard-Smithsonian Center for Astrophysics, 60 Garden Street MS-78, Cambridge, MA 02138, USA
- Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN 37235, USA
| | - Robert J. Siverd
- Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Suite 102, Santa Barbara, CA 93117, USA
| | - Keivan G. Stassun
- Department of Physics and Astronomy, Vanderbilt University, 6301 Stevenson Center, Nashville, TN 37235, USA
- Department of Physics, Fisk University, 1000 17th Avenue North, Nashville, TN 37208, USA
| | - Mark C. Wyatt
- Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK
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THE PAN-STARRS1 DISTANT
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> 5.6 QUASAR SURVEY: MORE THAN 100 QUASARS WITHIN THE FIRST GYR OF THE UNIVERSE. ACTA ACUST UNITED AC 2016. [DOI: 10.3847/0067-0049/227/1/11] [Citation(s) in RCA: 212] [Impact Index Per Article: 26.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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Richards GT, Myers AD, Peters CM, Krawczyk CM, Chase G, Ross NP, Fan X, Jiang L, Lacy M, McGreer ID, Trump JR, Riegel RN. BAYESIAN HIGH-REDSHIFT QUASAR CLASSIFICATION FROM OPTICAL AND MID-IR PHOTOMETRY. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0067-0049/219/2/39] [Citation(s) in RCA: 53] [Impact Index Per Article: 5.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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