Search for gravitational waves emitted from SN 2023ixf
We present the results of a search for gravitational-wave transients associated with core-collapse supernova SN 2023ixf, which was observed in the galaxy Messier 101 via optical emission on 2023 May 19, during the LIGO-Virgo-KAGRA 15th Engineering Run. We define a five-day on-source window during wh...
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| Hauptverfasser: | , , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
2025 June 1
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| In: |
The astrophysical journal
Year: 2025, Jahrgang: 985, Heft: 2, Pages: 183$p1-23 |
| ISSN: | 1538-4357 |
| DOI: | 10.3847/1538-4357/adc681 |
| Online-Zugang: | Verlag, kostenfrei, Volltext: https://doi.org/10.3847/1538-4357/adc681
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| Verfasserangaben: | A.G. Abac, M. Mapelli, S. Rinaldi [und 1776 weitere] and the LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration |
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| 245 | 1 | 0 | |a Search for gravitational waves emitted from SN 2023ixf |c A.G. Abac, M. Mapelli, S. Rinaldi [und 1776 weitere] and the LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration |
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| 520 | |a We present the results of a search for gravitational-wave transients associated with core-collapse supernova SN 2023ixf, which was observed in the galaxy Messier 101 via optical emission on 2023 May 19, during the LIGO-Virgo-KAGRA 15th Engineering Run. We define a five-day on-source window during which an accompanying gravitational-wave signal may have occurred. No gravitational waves have been identified in data when at least two gravitational-wave observatories were operating, which covered ∼14% of this five-day window. We report the search detection efficiency for various possible gravitational-wave emission models. Considering the distance to M101 (6.7 Mpc), we derive constraints on the gravitational-wave emission mechanism of core-collapse supernovae across a broad frequency spectrum, ranging from 50 Hz to 2 kHz, where we assume the gravitational-wave emission occurred when coincident data are available in the on-source window. Considering an ellipsoid model for a rotating proto-neutron star, our search is sensitive to gravitational-wave energy 1 × 10−4 M⊙c2 and luminosity 2.6 × 10−4 M⊙c2 s−1 for a source emitting at 82 Hz. These constraints are around an order of magnitude more stringent than those obtained so far with gravitational-wave data. The constraint on the ellipticity of the proto-neutron star that is formed is as low as 1.08, at frequencies above 1200 Hz, surpassing past results. | ||
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