EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material
We present optical, radio, and X-ray observations of EP250108a/SN 2025kg, a broad-line Type Ic supernova (SN Ic-BL) accompanying an Einstein Probe (EP) fast X-ray transient at z = 0.176. EP250108a/SN 2025kg possesses a double-peaked optical light curve, and its spectrum transitions from a blue under...
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| author | Gokul P. Srinivasaragavan Hamid Hamidani Genevieve Schroeder Nikhil Sarin Anna Y. Q. Ho Anthony L. Piro S. Bradley Cenko Shreya Anand Jesper Sollerman Daniel A. Perley Keiichi Maeda Brendan O’Connor Hanindyo Kuncarayakti M. Coleman Miller Tomás Ahumada Jada L. Vail Paul Duffell Ranadeep Dastidar Igor Andreoni Aleksandra Bochenek Seán. J. Brennan Jonathan Carney Ping Chen James Freeburn Avishay Gal-Yam Wynn Jacobson-Galán Mansi M. Kasliwal Jiaxuan Li Maggie L. Li Niharika Sravan Daniel E. Warshofsky |
| author_facet | Gokul P. Srinivasaragavan Hamid Hamidani Genevieve Schroeder Nikhil Sarin Anna Y. Q. Ho Anthony L. Piro S. Bradley Cenko Shreya Anand Jesper Sollerman Daniel A. Perley Keiichi Maeda Brendan O’Connor Hanindyo Kuncarayakti M. Coleman Miller Tomás Ahumada Jada L. Vail Paul Duffell Ranadeep Dastidar Igor Andreoni Aleksandra Bochenek Seán. J. Brennan Jonathan Carney Ping Chen James Freeburn Avishay Gal-Yam Wynn Jacobson-Galán Mansi M. Kasliwal Jiaxuan Li Maggie L. Li Niharika Sravan Daniel E. Warshofsky |
| author_sort | Gokul P. Srinivasaragavan |
| collection | DOAJ |
| description | We present optical, radio, and X-ray observations of EP250108a/SN 2025kg, a broad-line Type Ic supernova (SN Ic-BL) accompanying an Einstein Probe (EP) fast X-ray transient at z = 0.176. EP250108a/SN 2025kg possesses a double-peaked optical light curve, and its spectrum transitions from a blue underlying continuum to a typical SN Ic-BL spectrum over time. We fit a radioactive decay model to the second peak of the optical light curve and find SN parameters that are consistent with the SN Ic-BL population, while its X-ray and radio properties are consistent with those of low-luminosity GRB (LLGRB) 060218/SN 2006aj. We explore three scenarios to understand the system’s multiwavelength emission: (a) SN ejecta interacting with an extended circumstellar medium (CSM), (b) the shocked cocoon of a collapsar-driven jet choked in its stellar envelope, and (c) the shocked cocoon of a collapsar-driven jet choked in an extended CSM. Models (b) and (c) can explain the optical light curve and are also consistent with the radio and X-ray observations. We favor model (c) because it can self-consistently explain both the X-ray prompt emission and first optical peak, but we do not rule out model (b). From the properties of the first peak in model (c), we find evidence that EP250108a/SN 2025kg interacts with an extended CSM and infer an envelope mass M _e ∼ 0.1 M _⊙ and radius R _e ∼ 4 × 10 ^13 cm. EP250108a/SN 2025kg’s multiwavelength properties make it a close analog to LLGRB 060218/SN 2006aj and highlight the power of early follow-up observations in mapping the environments of massive stars prior to core collapse. |
| format | Article |
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| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
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| series | The Astrophysical Journal Letters |
| spelling | doaj-art-bd7f62c1786f43f5a9d3b068f99ce8452025-07-30T07:10:53ZengIOP PublishingThe Astrophysical Journal Letters2041-82052025-01-019882L6010.3847/2041-8213/ade870EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar MaterialGokul P. Srinivasaragavan0https://orcid.org/0000-0002-6428-2700Hamid Hamidani1https://orcid.org/0000-0003-2866-4522Genevieve Schroeder2https://orcid.org/0000-0001-9915-8147Nikhil Sarin3https://orcid.org/0000-0003-2700-1030Anna Y. Q. Ho4https://orcid.org/0000-0002-9017-3567Anthony L. Piro5https://orcid.org/0000-0001-6806-0673S. Bradley Cenko6https://orcid.org/0000-0003-1673-970XShreya Anand7https://orcid.org/0000-0003-3768-7515Jesper Sollerman8https://orcid.org/0000-0003-1546-6615Daniel A. Perley9https://orcid.org/0000-0001-8472-1996Keiichi Maeda10https://orcid.org/0000-0003-2611-7269Brendan O’Connor11https://orcid.org/0000-0002-9700-0036Hanindyo Kuncarayakti12https://orcid.org/0000-0002-1132-1366M. Coleman Miller13https://orcid.org/0000-0002-2666-728XTomás Ahumada14https://orcid.org/0000-0002-2184-6430Jada L. Vail15https://orcid.org/0009-0000-4044-8799Paul Duffell16https://orcid.org/0000-0001-7626-9629Ranadeep Dastidar17https://orcid.org/0009-0000-6548-6177Igor Andreoni18https://orcid.org/0000-0002-8977-1498Aleksandra Bochenek19https://orcid.org/0009-0008-2714-2507Seán. J. Brennan20https://orcid.org/0000-0003-1325-6235Jonathan Carney21https://orcid.org/0000-0001-8544-584XPing Chen22https://orcid.org/0000-0003-0853-6427James Freeburn23https://orcid.org/0009-0006-7990-0547Avishay Gal-Yam24https://orcid.org/0000-0002-3653-5598Wynn Jacobson-Galán25https://orcid.org/0000-0003-1103-3409Mansi M. Kasliwal26https://orcid.org/0000-0002-5619-4938Jiaxuan Li27https://orcid.org/0000-0001-9592-4190Maggie L. Li28https://orcid.org/0009-0001-6911-9144Niharika Sravan29Daniel E. Warshofsky30Department of Astronomy, University of Maryland , College Park, MD 20742, USA ; gsriniv2@umd.edu; Joint Space-Science Institute, University of Maryland , College Park, MD 20742, USA; Astrophysics Science Division , NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USAAstronomical Institute, Graduate School of Science, Tohoku University , Sendai 980-8578, JapanDepartment of Astronomy, Cornell University , Ithaca, NY 14853, USAOskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University , AlbaNova, Stockholm SE-106 91, Sweden; Nordita, Stockholm University and KTH Royal Institute of Technology , Hannes Alfvéns väg 12, SE-106 91 Stockholm, SwedenDepartment of Astronomy, Cornell University , Ithaca, NY 14853, USAThe Observatories of the Carnegie Institution for Science , 813 Santa Barbara St., Pasadena, CA 91101, USAJoint Space-Science Institute, University of Maryland , College Park, MD 20742, USA; Astrophysics Science Division , NASA Goddard Space Flight Center, 8800 Greenbelt Rd., Greenbelt, MD 20771, USAKavli Institute for Particle Astrophysics and Cosmology, Stanford University , 452 Lomita Mall, Stanford, CA 94305, USA; Department of Astronomy, University of California , Berkeley, CA 94720-3411, USADepartment of Astronomy, The Oskar Klein Center, Stockholm University , AlbaNova, 10691 Stockholm, SwedenAstrophysics Research Institute, Liverpool John Moores University , Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKDepartment of Astronomy, Kyoto University , Kitashirakawa-Oiwake-cho, Sakyo-ku, Kyoto 606-8502, JapanMcWilliams Center for Cosmology, Department of Physics, Carnegie Mellon University , Pittsburgh, PA 15213, USATuorla Observatory, Department of Physics and Astronomy, FI-20014 University of Turku , Finland; Finnish Centre for Astronomy with ESO (FINCA), FI-20014 University of Turku , FinlandDepartment of Astronomy, University of Maryland , College Park, MD 20742, USA ; gsriniv2@umd.edu; Joint Space-Science Institute, University of Maryland , College Park, MD 20742, USADivision of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USADepartment of Astronomy, Cornell University , Ithaca, NY 14853, USADepartment of Physics and Astronomy, Purdue University , 525 Northwestern Ave., West Lafayette, IN 47907, USADepartment of Physics and Astronomy, Purdue University , 525 Northwestern Ave., West Lafayette, IN 47907, USADepartment of Physics and Astronomy, University of North Carolina at Chapel Hill , Chapel Hill, NC 27599-3255, USAAstrophysics Research Institute, Liverpool John Moores University , Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UKThe Oskar Klein Centre, Department of Astronomy, Stockholm University , AlbaNova, SE-10691 Stockholm, SwedenDepartment of Physics and Astronomy, University of North Carolina at Chapel Hill , Chapel Hill, NC 27599-3255, USADepartment of Particle Physics and Astrophysics, Weizmann Institute of Science , 76100 Rehovot, IsraelCentre for Astrophysics and Supercomputing, Swinburne University of Technology , John St., Hawthorn, VIC 3122, Australia; ARC Centre of Excellence for Gravitational Wave Discovery (OzGrav) , John St., Hawthorn, VIC 3122, AustraliaDepartment of Particle Physics and Astrophysics, Weizmann Institute of Science , 76100 Rehovot, IsraelDivision of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USADivision of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USADepartment of Astrophysical Sciences, 4 Ivy Lane, Princeton University , Princeton, NJ 08540, USADivision of Physics, Mathematics and Astronomy, California Institute of Technology , Pasadena, CA 91125, USADepartment of Physics, Drexel University , Philadelphia, PA 19104, USASchool of Physics and Astronomy, University of Minnesota , Minneapolis, MN 55455, USAWe present optical, radio, and X-ray observations of EP250108a/SN 2025kg, a broad-line Type Ic supernova (SN Ic-BL) accompanying an Einstein Probe (EP) fast X-ray transient at z = 0.176. EP250108a/SN 2025kg possesses a double-peaked optical light curve, and its spectrum transitions from a blue underlying continuum to a typical SN Ic-BL spectrum over time. We fit a radioactive decay model to the second peak of the optical light curve and find SN parameters that are consistent with the SN Ic-BL population, while its X-ray and radio properties are consistent with those of low-luminosity GRB (LLGRB) 060218/SN 2006aj. We explore three scenarios to understand the system’s multiwavelength emission: (a) SN ejecta interacting with an extended circumstellar medium (CSM), (b) the shocked cocoon of a collapsar-driven jet choked in its stellar envelope, and (c) the shocked cocoon of a collapsar-driven jet choked in an extended CSM. Models (b) and (c) can explain the optical light curve and are also consistent with the radio and X-ray observations. We favor model (c) because it can self-consistently explain both the X-ray prompt emission and first optical peak, but we do not rule out model (b). From the properties of the first peak in model (c), we find evidence that EP250108a/SN 2025kg interacts with an extended CSM and infer an envelope mass M _e ∼ 0.1 M _⊙ and radius R _e ∼ 4 × 10 ^13 cm. EP250108a/SN 2025kg’s multiwavelength properties make it a close analog to LLGRB 060218/SN 2006aj and highlight the power of early follow-up observations in mapping the environments of massive stars prior to core collapse.https://doi.org/10.3847/2041-8213/ade870Type Ic supernovaeGamma-ray burstsCircumstellar matter |
| spellingShingle | Gokul P. Srinivasaragavan Hamid Hamidani Genevieve Schroeder Nikhil Sarin Anna Y. Q. Ho Anthony L. Piro S. Bradley Cenko Shreya Anand Jesper Sollerman Daniel A. Perley Keiichi Maeda Brendan O’Connor Hanindyo Kuncarayakti M. Coleman Miller Tomás Ahumada Jada L. Vail Paul Duffell Ranadeep Dastidar Igor Andreoni Aleksandra Bochenek Seán. J. Brennan Jonathan Carney Ping Chen James Freeburn Avishay Gal-Yam Wynn Jacobson-Galán Mansi M. Kasliwal Jiaxuan Li Maggie L. Li Niharika Sravan Daniel E. Warshofsky EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material The Astrophysical Journal Letters Type Ic supernovae Gamma-ray bursts Circumstellar matter |
| title | EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material |
| title_full | EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material |
| title_fullStr | EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material |
| title_full_unstemmed | EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material |
| title_short | EP250108a/SN 2025kg: A Jet-driven Stellar Explosion Interacting with Circumstellar Material |
| title_sort | ep250108a sn 2025kg a jet driven stellar explosion interacting with circumstellar material |
| topic | Type Ic supernovae Gamma-ray bursts Circumstellar matter |
| url | https://doi.org/10.3847/2041-8213/ade870 |
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