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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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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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3
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Fraser M. Supernovae and transients with circumstellar interaction. ROYAL SOCIETY OPEN SCIENCE 2020; 7:200467. [PMID: 32874641 PMCID: PMC7428271 DOI: 10.1098/rsos.200467] [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: 03/20/2020] [Accepted: 06/16/2020] [Indexed: 06/11/2023]
Abstract
It is 30 years since the characteristic signatures of interaction with circumstellar material (CSM) were first observed in a core-collapse supernova. Since then, CSM interaction has been observed and inferred across a range of transients, from the low-energy explosions of low-mass stars as likely electron-capture supernovae, through to the brightest superluminous supernovae. In this review, I present a brief overview of some of the interacting supernovae and transients that have been observed to date, and attempt to classify and group them together in a phenomenological framework.
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Affiliation(s)
- Morgan Fraser
- School of Physics, O’Brien Centre for Science North, University College Dublin, Belfield, Dublin 4, Ireland
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4
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The Interaction of Type Ia Supernovae with Planetary Nebulae: The Case of Kepler’s Supernova Remnant. GALAXIES 2020. [DOI: 10.3390/galaxies8020038] [Citation(s) in RCA: 7] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/17/2022]
Abstract
One of the key methods for determining the unknown nature of Type Ia supernovae (SNe Ia) is the search for traces of interaction between the SN ejecta and the circumstellar structures at the resulting supernova remnants (SNRs Ia). So far, the observables that we receive from well-studied SNRs Ia cannot be explained self-consistently by any model presented in the literature. In this study, we suggest that the circumstellar medium (CSM) being observed to surround several SNRs Ia was mainly shaped by planetary nebulae (PNe) that originated from one or both progenitor stars. Performing two-dimensional hydrodynamic simulations, we show that the ambient medium shaped by PNe can account for several properties of the CSM that have been found to surround SNe Ia and their remnants. Finally, we model Kepler’s SNR considering that the SN explosion occurred inside a bipolar PN. Our simulations show good agreement with the observed morphological and kinematic properties of Kepler’s SNR. In particular, our model reproduces the current expansion parameter of Kepler’s SNR, the partial interaction of the remnant with a dense CSM at its northern region and finally the existence of two opposite protrusions (‘ears’) at the equatorial plane of the SNR.
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5
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Variable Hα Emission in the Nebular Spectra of the Low-luminosity Type Ia SN2018cqj/ATLAS18qtd. ACTA ACUST UNITED AC 2020. [DOI: 10.3847/1538-4357/ab6323] [Citation(s) in RCA: 17] [Impact Index Per Article: 4.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
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6
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Pooley D, Wheeler JC, Vinkó J, Dwarkadas VV, Szalai T, Silverman JM, Griesel M, McCullough M, Marion GH, MacQueen P. Interaction of SN Ib 2004dk with a Previously Expelled Envelope. THE ASTROPHYSICAL JOURNAL 2019; 883:120. [PMID: 33324017 PMCID: PMC7735322 DOI: 10.3847/1538-4357/ab3e36] [Citation(s) in RCA: 11] [Impact Index Per Article: 2.2] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 11/18/2022]
Abstract
The interaction between the expanding supernova (SN) ejecta with the circumstellar material (CSM) that was expelled from the progenitor prior to explosion is a long-sought phenomenon, yet observational evidence is scarce. Here we confirm a new example: SN 2004dk, originally a hydrogen-poor, helium-rich Type Ib SN that reappeared as a strong Hα-emitting point source on narrowband Hα images. We present follow-up optical spectroscopy that reveals the presence of a broad Hα component with full width at half maximum of ~ 290 km s-1 in addition to the narrow Hα+[N ii] emission features from the host galaxy. Such a broad component is a clear sign of an ejecta-CSM interaction. We also present observations with the XMM-Newton Observatory, the Swift satellite, and the Chandra X-ray Observatory that span 10 days to 15 years after discovery. The detection of strong radio, X-ray, and Hα emission years after explosion allows various constraints to be put on pre-SN mass-loss processes. We present a wind-bubble model in which the CSM is "pre-prepared" by a fast wind interacting with a slow wind. Much of the outer density profile into which the SN explodes corresponds to no steady-state mass-loss process. We estimate that the shell of compressed slow wind material was ejected ~1400 yr prior to explosion, perhaps during carbon burning, and that the SN shock had swept up about 0.04 M ⊙ of material. The region emitting the Hα has a density of order 10-20 g cm-3.
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Affiliation(s)
- David Pooley
- Department of Physics and Astronomy, Trinity University, San Antonio, TX, USA
- Eureka Scientific, Inc., USA
| | - J Craig Wheeler
- Department of Astronomy, University of Texas at Austin, Austin, TX, USA
| | - Jozsef Vinkó
- Department of Astronomy, University of Texas at Austin, Austin, TX, USA
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, H-1121 Budapest, Hungary
- Department of Optics and Quantum Electronics, University of Szeged, Dóm tér 9, Szeged, 6720, Hungary
| | - Vikram V Dwarkadas
- Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL, USA
| | - Tamas Szalai
- Konkoly Observatory, Research Centre for Astronomy and Earth Sciences, Hungarian Academy of Sciences, H-1121 Budapest, Hungary
- Department of Optics and Quantum Electronics, University of Szeged, Dóm tér 9, Szeged, 6720, Hungary
| | - Jeffrey M Silverman
- Department of Astronomy, University of Texas at Austin, Austin, TX, USA
- Samba TV, San Francisco, CA, USA
| | - Madelaine Griesel
- Department of Physics and Astronomy, Trinity University, San Antonio, TX, USA
| | - Molly McCullough
- Department of Physics and Astronomy, Trinity University, San Antonio, TX, USA
| | - G H Marion
- Department of Astronomy, University of Texas at Austin, Austin, TX, USA
| | - Phillip MacQueen
- Department of Astronomy, University of Texas at Austin, Austin, TX, USA
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7
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Zumalacárregui M, Seljak U. Limits on Stellar-Mass Compact Objects as Dark Matter from Gravitational Lensing of Type Ia Supernovae. PHYSICAL REVIEW LETTERS 2018; 121:141101. [PMID: 30339429 DOI: 10.1103/physrevlett.121.141101] [Citation(s) in RCA: 19] [Impact Index Per Article: 3.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/01/2018] [Revised: 08/14/2018] [Indexed: 06/08/2023]
Abstract
The nature of dark matter (DM) remains unknown despite very precise knowledge of its abundance in the Universe. An alternative to new elementary particles postulates DM as made of macroscopic compact halo objects (MACHO) such as black holes formed in the very early Universe. Stellar-mass primordial black holes (PBHs) are subject to less robust constraints than other mass ranges and might be connected to gravitational-wave signals detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO). New methods are therefore necessary to constrain the viability of compact objects as a DM candidate. Here we report bounds on the abundance of compact objects from gravitational lensing of type Ia supernovae (SNe). Current SNe data sets constrain compact objects to represent less than 35.2% (Joint Lightcurve Analysis) and 37.2% (Union 2.1) of the total matter content in the Universe, at 95% confidence level. The results are valid for masses larger than ∼0.01 M_{⊙} (solar masses), limited by the size SNe relative to the lens Einstein radius. We demonstrate the mass range of the constraints by computing magnification probabilities for realistic SNe sizes and different values of the PBH mass. Our bounds are sensitive to the total abundance of compact objects with M≳0.01 M_{⊙} and complementary to other observational tests. These results are robust against cosmological parameters, outlier rejection, correlated noise, and selection bias. PBHs and other MACHOs are therefore ruled out as the dominant form of DM for objects associated to LIGO gravitational wave detections. These bounds constrain early-Universe models that predict stellar-mass PBH production and strengthen the case for lighter forms of DM, including new elementary particles.
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Affiliation(s)
- Miguel Zumalacárregui
- Berkeley Center for Cosmological Physics, LBNL and University of California at Berkeley, Berkeley, California 94720, USA
- Institut de Physique Théorique, Université Paris Saclay CEA, CNRS, 91191 Gif-sur-Yvette, France
- Nordita, KTH Royal Institute of Technology and Stockholm University, Roslagstullsbacken 23, SE-106 91 Stockholm, Sweden
| | - Uroš Seljak
- Berkeley Center for Cosmological Physics, LBNL and University of California at Berkeley, Berkeley, California 94720, USA
- Physics and Astronomy Department, LBNL, University of California at Berkeley, Berkeley, California 94720, USA
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8
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Kawanaka N, Yanagita S. Cosmic-Ray Lithium Production at the Nova Eruptions Followed by a Type Ia Supernova. PHYSICAL REVIEW LETTERS 2018; 120:041103. [PMID: 29437438 DOI: 10.1103/physrevlett.120.041103] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.2] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/07/2017] [Revised: 11/02/2017] [Indexed: 06/08/2023]
Abstract
Recent measurements of cosmic-ray (CR) light nuclei by AMS-02 have shown that there is an unexpected component of CR lithium whose spectral index is harder than that expected from the secondary production scenario. We propose the nearby type Ia supernova following a nova eruption as the origin of lithium nuclei in the CRs. By fitting the data of CR protons, helium, and lithium fluxes provided by AMS-02 with our theoretical model we show that this scenario is consistent with the observations. The observational tests that can check our hypothesis are briefly discussed.
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Affiliation(s)
- Norita Kawanaka
- Department of Astronomy, Graduate School of Science, Kyoto University, Kitashirakawa Oiwake-cho, Sakyo-ku, Kyoto 606-8502, Japan and Hakubi Center, Yoshida Honmachi, Sakyo-ku, Kyoto 606-8501, Japan
| | - Shohei Yanagita
- College of Science, Ibaraki University, 2-1-1 Bunkyo, Mito, Ibaraki 310-8512, Japan
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Bochenek CD, Dwarkadas VV, Silverman JM, Fox OD, Chevalier RA, Smith N, Filippenko AV. X-ray emission from SN 2012ca: A Type Ia-CSM supernova explosion in a dense surrounding medium. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY 2018; 473:336-344. [PMID: 33293735 PMCID: PMC7720428 DOI: 10.1093/mnras/stx2029] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [Abstract] [Key Words] [Grants] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 05/29/2023]
Abstract
X-ray emission is one of the signposts of circumstellar interaction in supernovae (SNe), but until now, it has been observed only in core-collapse SNe. The level of thermal X-ray emission is a direct measure of the density of the circumstellar medium (CSM), and the absence of X-ray emission from Type Ia SNe has been interpreted as a sign of a very low density CSM. In this paper, we report late-time (500-800 d after discovery) X-ray detections of SN 2012ca in Chandra data. The presence of hydrogen in the initial spectrum led to a classification of Type Ia-CSM, ostensibly making it the first SN Ia detected with X-rays. Our analysis of the X-ray data favours an asymmetric medium, with a high-density component which supplies the X-ray emission. The data suggest a number density >108 cm-3 in the higher density medium, which is consistent with the large observed Balmer decrement if it arises from collisional excitation. This is high compared to most core-collapse SNe, but it may be consistent with densities suggested for some Type IIn or superluminous SNe. If SN 2012ca is a thermonuclear SN, the large CSM density could imply clumps in the wind, or a dense torus or disc, consistent with the single-degenerate channel. A remote possibility for a core-degenerate channel involves a white dwarf merging with the degenerate core of an asymptotic giant branch star shortly before the explosion, leading to a common envelope around the SN.
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Affiliation(s)
- Christopher D. Bochenek
- Department of Astronomy and Astrophysics, University of Chicago, 5640 S Ellis Ave, Chicago, IL 60637, USA
- Astronomy Department, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA
| | - Vikram V. Dwarkadas
- Department of Astronomy and Astrophysics, University of Chicago, 5640 S Ellis Ave, Chicago, IL 60637, USA
| | | | - Ori D. Fox
- Space telescope Science Institute, Baltimore, MD 21218, USA
| | - Roger A. Chevalier
- Department of Astronomy, University of Virginia, Charlottesville, VA 22903, USA
| | - Nathan Smith
- Steward Observatory, 933 N. Cherry Ave., Tucson, AZ 85721, USA
| | - Alexei V. Filippenko
- Department of Astronomy, University of California, Berkeley, CA 94720-3411, USA
- Senior Miller Fellow, Miller Institute for Basic Research in Science, University of California, Berkeley, CA 94720, USA
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Nugent P, Hamuy M. Cosmology with Type IIP Supernovae. HANDBOOK OF SUPERNOVAE 2016:1-18. [DOI: 10.1007/978-3-319-20794-0_108-1] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Subscribe] [Scholar Register] [Received: 07/12/2016] [Accepted: 08/02/2016] [Indexed: 09/02/2023]
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Fisher R, Jumper K. SINGLE-DEGENERATE TYPE Ia SUPERNOVAE ARE PREFERENTIALLY OVERLUMINOUS. ACTA ACUST UNITED AC 2015. [DOI: 10.1088/0004-637x/805/2/150] [Citation(s) in RCA: 36] [Impact Index Per Article: 4.0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/12/2022]
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Justham S. Portrait of a doomed star. Nature 2014; 512:34-5. [DOI: 10.1038/512034a] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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