We develop and characterize a parameter estimation methodology for rotating core collapse supernovae based on the gravitational wave (GW) core bounce phase and real detector noise. Expanding on the evidence from numerical simulations for the deterministic nature of this GW emission and about the dependence on the ratio β between rotational kinetic to potential energy, we propose an analytical model for the core bounce component which depends on β and one phenomenological parameter. We validate the goodness of the model with a pool of representative waveforms. We use the fitting factor adopted in compact coalescing binary searches as a metric to quantify the goodness of the analytical model and the template bank generated by the model presents an average accuracy of 94.4% when compared with the numerical simulations and is used as the basis for the work. The error for a matched filter frequentist parameter estimation of β is evaluated. The results obtained considering real interferometric noise and a waveform at a distance of 10 kpc and optimal orientation, for one standard deviation estimation error of the rotation parameter β lie in the range of 10−2–10−3 as β increases. The results are also compared to the scenario where Gaussian recolored data is employed. The analytical model also allows for the first time, to compute theoretical minima in the error for β for any type of estimator. Our analysis indicates that the presence of rotation would be detectable at 0.5 Mpc for third generation interferometers like CE or ET.
Parameter estimation from the core-bounce phase of rotating core collapse supernovae in real interferometer noise
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1.
University of Guadalajara
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2.
California Institute of Technology
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3.
Embry–Riddle Aeronautical University
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4.
Monterrey Institute of Technology and Higher Education
Abstract
Copyright and License
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Acknowledgement
The authors thank Professors Abdikamalov and Richers for allowing us to use their CCSNe simulation data. MZ thanks professor Richers for discussions about accuracy of the numerical waveforms. MZ thanks professor Brennan Hughey for feedback on the discussion data quality cuts. This work was supported by CONAHCyT Network Project No. 376127 Sombras, lentes y ondas gravitatorias generadas por objetos compactos astrofísicos. LV acknowledges CONAHCYT scholarship. CM thanks PROSNI-UDG. MAP was supported in part by the Sherman Fairchild Foundation, NSF Grant PHY-2309231, and OAC-2209655 at Caltech. MZ is supported by the National Science Foundation Gravitational Physics Experimental and Data Analysis Program through Awards PHY-2110555 and PHY-2405227. This research has used data or software obtained from the Gravitational Wave Open Science Center (gwosc.org), a service of the LIGO Scientific Collaboration, the Virgo Collaboration, and KAGRA. This material is based upon work supported by NSF's LIGO Laboratory which is a major facility fully funded by the National Science Foundation, as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. Virgo is funded, through the European Gravitational Observatory (EGO), by the French Center National de Recherche Scientifique (CNRS), the Italian Istituto Nazionale di Fisica Nucleare (INFN) and the Dutch Nikhef, with contributions by institutions from Belgium, Germany, Greece, Hungary, Ireland, Japan, Monaco, Poland, Portugal, Spain. KAGRA is supported by Ministry of Education, Culture, Sports, Science and Technology (MEXT), Japan Society for the Promotion of Science (JSPS) in Japan; National Research Foundation (NRF) and Ministry of Science and ICT (MSIT) in Korea; Academia Sinica (AS) and the National Science and Technology Council (NSTC) in Taiwan.
Data Availability
No new data were created in this study, we used catalogs of GW signals from other authors. The data that support the findings of this study are available upon reasonable request from the authors.
Additional details
- Alternative title
- Asymptotic expansions for the maximum likelihood estimation errors of the rotating parameter of the gravitational wave from core-collapse supernovae
- Consejo Nacional de Humanidades, Ciencias y Tecnologías
- 376127
- University of Guadalajara
- PROSNI-UDG -
- Sherman Fairchild Foundation
- National Science Foundation
- PHY-2309231
- National Science Foundation
- OAC-2209655
- National Science Foundation
- PHY-2110555
- National Science Foundation
- PHY-2405227
- Accepted
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2025-04-29
- Available
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2025-05-20Published
- Caltech groups
- LIGO, TAPIR, Division of Physics, Mathematics and Astronomy (PMA)
- Publication Status
- Published