Abstract
The response of the Advanced Laser Interferometer Gravitational-wave Observatory (Advanced LIGO) interferometers is known to vary with time (Tuyenbayev et al 2017 Class. Quantum Grav. 34 015002). Accurate calibration of the interferometers must therefore track and compensate for temporal variations in calibration model parameters. These variations were tracked during the first three Advanced LIGO observing runs, and compensation for some of them has been implemented in the calibration procedure. During the second observing run, multiplicative corrections to the interferometer response were applied while producing calibrated strain data both in real time and in high latency. In a high-latency calibration produced after the second observing run and during the entirety of the third observing run, a correction requiring periodic filter updates was applied to the calibration-the time dependence of the coupled cavity pole frequency f c c . This paper describes the methods developed to compensate for variations in the interferometer response requiring time-dependent filters, including variable zeros, poles, gains, and time delays. The described methods were used to provide compensation for well-modeled time dependence of the interferometer response, which has helped to reduce systematic errors in the calibration to < 2% in magnitude and < 2∘ in phase across LIGO’s most sensitive frequency band of 20-2000 Hz (Sun et al 2020 Class. Quantum Grav. 37 225008; Sun et al 2021 arXiv:2107.00129 [astro-ph.IM]). Additionally, this paper shows how such compensation is relevant for astrophysical inference studies by reducing uncertainty and bias in the sky localization for a simulated binary neutron star merger.
| Original language | English (US) |
|---|---|
| Article number | 035001 |
| Journal | Classical and Quantum Gravity |
| Volume | 40 |
| Issue number | 3 |
| DOIs | |
| State | Published - Feb 2 2023 |
| Externally published | Yes |
Bibliographical note
Funding Information:The authors would like to thank Lilli Sun for her helpful suggestions and careful review of this paper. The authors would like to thank the members of the LIGO calibration team, including Joe Betzwieser, Dripta Bhattacharjee, Jenne Driggers, Evan Goetz, Sudarshan Karki, Jeff Kissel, Antonios Kontos, Greg Mendell, Timesh Mistry, Ethan Payne, Jamie Rollins, Rick Savage, Lilli Sun, and Alan Weinstein. The authors were supported by National Science Foundation Grants PHY-1607178, PHY-1607585, PHY-1506360, and PHY-1847350. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the United States National Science Foundation (NSF), and operates under cooperative Agreement PHY-1764464. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants PHY-0757058 and PHY-0823459. This material is based upon work supported by NSF’s LIGO Laboratory which is a major facility fully funded by the National Science Foundation. Advanced LIGO was built under Award PHY-0823459. The authors gratefully acknowledge the support of the United States NSF for the construction and operation of the LIGO Laboratory and Advanced LIGO 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 (ARC). This paper carries LIGO Document Number LIGO-P1800313.
Funding Information:
The authors would like to thank Lilli Sun for her helpful suggestions and careful review of this paper. The authors would like to thank the members of the LIGO calibration team, including Joe Betzwieser, Dripta Bhattacharjee, Jenne Driggers, Evan Goetz, Sudarshan Karki, Jeff Kissel, Antonios Kontos, Greg Mendell, Timesh Mistry, Ethan Payne, Jamie Rollins, Rick Savage, Lilli Sun, and Alan Weinstein. The authors were supported by National Science Foundation Grants PHY-1607178, PHY-1607585, PHY-1506360, and PHY-1847350. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the United States National Science Foundation (NSF), and operates under cooperative Agreement PHY–1764464. The authors are grateful for computational resources provided by the LIGO Laboratory and supported by National Science Foundation Grants PHY-0757058 and PHY-0823459. This material is based upon work supported by NSF’s LIGO Laboratory which is a major facility fully funded by the National Science Foundation. Advanced LIGO was built under Award PHY–0823459. The authors gratefully acknowledge the support of the United States NSF for the construction and operation of the LIGO Laboratory and Advanced LIGO 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 (ARC). This paper carries LIGO Document Number LIGO-P1800313.
Publisher Copyright:
© 2023 IOP Publishing Ltd.
Keywords
- LIGO
- accuracy
- calibrations
- improving