SN2023fyq: A Type Ibn Supernova with Long-standing Precursor Activity Due to Binary Interaction
We present photometric and spectroscopic observations of SN 2023fyq, a Type Ibn supernova (SN) in the nearby galaxy NGC 4388 ( D ≃ 18 Mpc). In addition, we trace the 3 yr long precursor emission at the position of SN 2023fyq using data from DLT40, ATLAS, Zwicky Transient Facility, ASAS-SN, Swift, an...
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2024-01-01
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| author | Yize Dong Daichi Tsuna Stefano Valenti David J. Sand Jennifer E. Andrews K. Azalee Bostroem Griffin Hosseinzadeh Emily Hoang Saurabh W. Jha Daryl Janzen Jacob E. Jencson Michael Lundquist Darshana Mehta Aravind P. Ravi Nicolas E. Meza Retamal Jeniveve Pearson Manisha Shrestha Alceste Z. Bonanos D. Andrew Howell Nathan Smith Joseph Farah Daichi Hiramatsu Koichi Itagaki Curtis McCully Megan Newsome Estefania Padilla Gonzalez Emmanouela Paraskeva Craig Pellegrino Giacomo Terreran Joshua Haislip Vladimir Kouprianov Daniel E. Reichart |
| author_facet | Yize Dong Daichi Tsuna Stefano Valenti David J. Sand Jennifer E. Andrews K. Azalee Bostroem Griffin Hosseinzadeh Emily Hoang Saurabh W. Jha Daryl Janzen Jacob E. Jencson Michael Lundquist Darshana Mehta Aravind P. Ravi Nicolas E. Meza Retamal Jeniveve Pearson Manisha Shrestha Alceste Z. Bonanos D. Andrew Howell Nathan Smith Joseph Farah Daichi Hiramatsu Koichi Itagaki Curtis McCully Megan Newsome Estefania Padilla Gonzalez Emmanouela Paraskeva Craig Pellegrino Giacomo Terreran Joshua Haislip Vladimir Kouprianov Daniel E. Reichart |
| author_sort | Yize Dong |
| collection | DOAJ |
| description | We present photometric and spectroscopic observations of SN 2023fyq, a Type Ibn supernova (SN) in the nearby galaxy NGC 4388 ( D ≃ 18 Mpc). In addition, we trace the 3 yr long precursor emission at the position of SN 2023fyq using data from DLT40, ATLAS, Zwicky Transient Facility, ASAS-SN, Swift, and amateur astronomer Koichi Itagaki. The double-peaked postexplosion light curve reaches a luminosity of ∼10 ^43 erg s ^−1 . The strong intermediate-width He lines observed in the nebular spectrum imply the interaction is still active at late phases. We found that the precursor activity in SN 2023fyq is best explained by the mass transfer in a binary system involving a low-mass He star and a compact companion. An equatorial disk is likely formed in this process (∼0.6 M _⊙ ), and the interaction of SN ejecta with this disk powers the second peak of the SN. The early SN light curve reveals the presence of dense extended material (∼0.3 M _⊙ ) at ∼3000 R _⊙ ejected weeks before the SN explosion, likely due to final-stage core silicon burning or runaway mass transfer resulting from binary orbital shrinking, leading to rapid-rising precursor emission within ∼30 days prior to explosion. The final explosion could be triggered either by the core collapse of the He star or by the merger of the He star with a compact object. SN 2023fyq, along with SN 2018gjx and SN 2015G, forms a unique class of Type Ibn SNe, which originate in binary systems and are likely to exhibit detectable long-lasting pre-explosion outbursts with magnitudes ranging from −10 to −13. |
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| institution | Kabale University |
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| spelling | doaj-art-53a8ac8782a24bd1b7d62aaea91c381f2025-01-02T15:26:52ZengIOP PublishingThe Astrophysical Journal1538-43572024-01-01977225410.3847/1538-4357/ad8de6SN2023fyq: A Type Ibn Supernova with Long-standing Precursor Activity Due to Binary InteractionYize Dong0https://orcid.org/0000-0002-7937-6371Daichi Tsuna1https://orcid.org/0000-0002-6347-3089Stefano Valenti2https://orcid.org/0000-0001-8818-0795David J. Sand3https://orcid.org/0000-0003-4102-380XJennifer E. Andrews4https://orcid.org/0000-0003-0123-0062K. Azalee Bostroem5https://orcid.org/0000-0002-4924-444XGriffin Hosseinzadeh6https://orcid.org/0000-0002-0832-2974Emily Hoang7https://orcid.org/0000-0003-2744-4755Saurabh W. Jha8https://orcid.org/0000-0001-8738-6011Daryl Janzen9https://orcid.org/0000-0003-0549-3281Jacob E. Jencson10https://orcid.org/0000-0001-5754-4007Michael Lundquist11https://orcid.org/0000-0001-9589-3793Darshana Mehta12https://orcid.org/0009-0008-9693-4348Aravind P. Ravi13https://orcid.org/0000-0002-7352-7845Nicolas E. Meza Retamal14https://orcid.org/0000-0002-7015-3446Jeniveve Pearson15https://orcid.org/0000-0002-0744-0047Manisha Shrestha16https://orcid.org/0000-0002-4022-1874Alceste Z. Bonanos17https://orcid.org/0000-0003-2851-1905D. Andrew Howell18https://orcid.org/0000-0003-4253-656XNathan Smith19https://orcid.org/0000-0001-5510-2424Joseph Farah20https://orcid.org/0000-0003-4914-5625Daichi Hiramatsu21https://orcid.org/0000-0002-1125-9187Koichi Itagaki22Curtis McCully23https://orcid.org/0000-0001-5807-7893Megan Newsome24Estefania Padilla Gonzalez25https://orcid.org/0000-0003-0209-9246Emmanouela Paraskeva26https://orcid.org/0000-0003-2814-4383Craig Pellegrino27https://orcid.org/0000-0002-7472-1279Giacomo Terreran28https://orcid.org/0000-0003-0794-5982Joshua Haislip29https://orcid.org/0000-0002-6703-805XVladimir Kouprianov30https://orcid.org/0000-0003-3642-5484Daniel E. Reichart31https://orcid.org/0000-0002-5060-3673Department of Physics and Astronomy, University of California , 1 Shields Avenue, Davis, CA 95616-5270, USA ; yizdong@ucdavis.eduTAPIR, Mailcode 350-17, California Institute of Technology , Pasadena, CA 91125, USA; Research Center for the Early Universe (RESCEU), School of Science, The University of Tokyo , 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, JapanDepartment of Physics and Astronomy, University of California , 1 Shields Avenue, Davis, CA 95616-5270, USA ; yizdong@ucdavis.eduSteward Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721-0065, USAGemini Observatory , 670 North A‘ohoku Place, Hilo, HI 96720-2700, USASteward Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721-0065, USASteward Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721-0065, USADepartment of Physics and Astronomy, University of California , 1 Shields Avenue, Davis, CA 95616-5270, USA ; yizdong@ucdavis.eduDepartment of Physics and Astronomy, Rutgers, the State University of New Jersey , 136 Frelinghuysen Road, Piscataway, NJ 08854-8019, USADepartment of Physics & Engineering Physics, University of Saskatchewan , 116 Science Place, Saskatoon, SK S7N 5E2, CanadaDepartment of Physics and Astronomy, Johns Hopkins University , 3400 North Charles Street, Baltimore, MD 21218, USA; Space Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USAW. M. Keck Observatory , 65-1120 Māmalahoa Highway, Kamuela, HI 96743-8431, USADepartment of Physics and Astronomy, University of California , 1 Shields Avenue, Davis, CA 95616-5270, USA ; yizdong@ucdavis.eduDepartment of Physics and Astronomy, University of California , 1 Shields Avenue, Davis, CA 95616-5270, USA ; yizdong@ucdavis.eduDepartment of Physics and Astronomy, University of California , 1 Shields Avenue, Davis, CA 95616-5270, USA ; yizdong@ucdavis.eduSteward Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721-0065, USASteward Observatory, University of Arizona , 933 North Cherry Avenue, Tucson, AZ 85721-0065, USAIAASARS, National Observatory of Athens , Metaxa & Vas. Pavlou Street, 15236, Penteli, Athens, GreeceLas Cumbres Observatory , 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA; Department of Physics, University of California , Santa Barbara, CA 93106-9530, USASteward Observatory, University of Arizona , 933 North Cherry Avenue, Rm. N204, Tucson, AZ 85721-0065, USALas Cumbres Observatory , 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA; Department of Physics, University of California , Santa Barbara, CA 93106-9530, USACenter for Astrophysics ∣ Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138-1516, USA; The NSF AI Institute for Artificial Intelligence and Fundamental Interactions , USAItagaki Astronomical Observatory , Yamagata 990-2492, JapanLas Cumbres Observatory , 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA; Department of Physics, University of California , Santa Barbara, CA 93106-9530, USALas Cumbres Observatory , 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA; Department of Physics, University of California , Santa Barbara, CA 93106-9530, USALas Cumbres Observatory , 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA; Department of Physics, University of California , Santa Barbara, CA 93106-9530, USAIAASARS, National Observatory of Athens , Metaxa & Vas. Pavlou Street, 15236, Penteli, Athens, GreeceDepartment of Astronomy, University of Virginia , Charlottesville, VA 22904, USALas Cumbres Observatory , 6740 Cortona Drive, Suite 102, Goleta, CA 93117-5575, USA; Department of Physics, University of California , Santa Barbara, CA 93106-9530, USADepartment of Physics and Astronomy, University of North Carolina , 120 East Cameron Avenue, Chapel Hill, NC 27599, USADepartment of Physics and Astronomy, University of North Carolina , 120 East Cameron Avenue, Chapel Hill, NC 27599, USADepartment of Physics and Astronomy, University of North Carolina , 120 East Cameron Avenue, Chapel Hill, NC 27599, USAWe present photometric and spectroscopic observations of SN 2023fyq, a Type Ibn supernova (SN) in the nearby galaxy NGC 4388 ( D ≃ 18 Mpc). In addition, we trace the 3 yr long precursor emission at the position of SN 2023fyq using data from DLT40, ATLAS, Zwicky Transient Facility, ASAS-SN, Swift, and amateur astronomer Koichi Itagaki. The double-peaked postexplosion light curve reaches a luminosity of ∼10 ^43 erg s ^−1 . The strong intermediate-width He lines observed in the nebular spectrum imply the interaction is still active at late phases. We found that the precursor activity in SN 2023fyq is best explained by the mass transfer in a binary system involving a low-mass He star and a compact companion. An equatorial disk is likely formed in this process (∼0.6 M _⊙ ), and the interaction of SN ejecta with this disk powers the second peak of the SN. The early SN light curve reveals the presence of dense extended material (∼0.3 M _⊙ ) at ∼3000 R _⊙ ejected weeks before the SN explosion, likely due to final-stage core silicon burning or runaway mass transfer resulting from binary orbital shrinking, leading to rapid-rising precursor emission within ∼30 days prior to explosion. The final explosion could be triggered either by the core collapse of the He star or by the merger of the He star with a compact object. SN 2023fyq, along with SN 2018gjx and SN 2015G, forms a unique class of Type Ibn SNe, which originate in binary systems and are likely to exhibit detectable long-lasting pre-explosion outbursts with magnitudes ranging from −10 to −13.https://doi.org/10.3847/1538-4357/ad8de6Core-collapse supernovaeCircumstellar matterStellar mass loss |
| spellingShingle | Yize Dong Daichi Tsuna Stefano Valenti David J. Sand Jennifer E. Andrews K. Azalee Bostroem Griffin Hosseinzadeh Emily Hoang Saurabh W. Jha Daryl Janzen Jacob E. Jencson Michael Lundquist Darshana Mehta Aravind P. Ravi Nicolas E. Meza Retamal Jeniveve Pearson Manisha Shrestha Alceste Z. Bonanos D. Andrew Howell Nathan Smith Joseph Farah Daichi Hiramatsu Koichi Itagaki Curtis McCully Megan Newsome Estefania Padilla Gonzalez Emmanouela Paraskeva Craig Pellegrino Giacomo Terreran Joshua Haislip Vladimir Kouprianov Daniel E. Reichart SN2023fyq: A Type Ibn Supernova with Long-standing Precursor Activity Due to Binary Interaction The Astrophysical Journal Core-collapse supernovae Circumstellar matter Stellar mass loss |
| title | SN2023fyq: A Type Ibn Supernova with Long-standing Precursor Activity Due to Binary Interaction |
| title_full | SN2023fyq: A Type Ibn Supernova with Long-standing Precursor Activity Due to Binary Interaction |
| title_fullStr | SN2023fyq: A Type Ibn Supernova with Long-standing Precursor Activity Due to Binary Interaction |
| title_full_unstemmed | SN2023fyq: A Type Ibn Supernova with Long-standing Precursor Activity Due to Binary Interaction |
| title_short | SN2023fyq: A Type Ibn Supernova with Long-standing Precursor Activity Due to Binary Interaction |
| title_sort | sn2023fyq a type ibn supernova with long standing precursor activity due to binary interaction |
| topic | Core-collapse supernovae Circumstellar matter Stellar mass loss |
| url | https://doi.org/10.3847/1538-4357/ad8de6 |
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