research article journal article
Open Data from the Third Observing Run of LIGO, Virgo, KAGRA, and GEO
- Publication date
- 28 July 2023
- Publisher
- American Astronomical Society
Abstract
Calibration of the LIGO strain data was performed with
a GstLAL-based calibration software pipeline (Viets et al.
2018). Calibration of the Virgo strain data was performed
with C-based software (Acernese et al. 2022b). Data quality
products and event-validation results were computed using the
DMT (https://labcit.ligo.caltech.edu/~jzweizig/DMT-Project.
html), DQR (https://docs.ligo.org/detchar/data-quality-report/),
DQSEGDB (Fisher et al. 2021), gwdetchar (Macloed et al.
2021a), hveto (Smith et al. 2011), iDQ (Essick et al. 2020), and
Omicron (Robinet et al. 2020) software packages and contribut-
ing software tools. Analyses relied upon the LALSuite software
library (LIGO Scientific Collaboration 2018). PESummary was
used to postprocess and collate parameter estimation results (Hoy
& Raymond 2021). For an exhaustive list of the software used
for searching the GW signals and characterizing their source,
see Abbott et al. (2021c). Plots were prepared with Matplotlib
(Hunter 2007), seaborn (Waskom 2021), GWSumm (Macleod
et al. 2021b), and GWpy (Macleod et al. 2021c). NumPy (Harris
et al. 2020) and SciPy (Virtanen et al. 2020) were used in the
preparation of the manuscript.
This material is based upon work supported by NSF’s LIGO
Laboratory which is a major facility fully funded by the
National Science Foundation. The authors also gratefully
acknowledge the support of 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 GEO 600 detector.
Additional support for Advanced LIGO was provided by the
Australian Research Council. The authors gratefully acknowl-
edge the Italian Istituto Nazionale di Fisica Nucleare (INFN),
the French Centre National de la Recherche Scientifique
(CNRS), and the Netherlands Organization for Scientific
Research (NWO) for the construction and operation of the
Virgo detector and the creation and support of the EGO
consortium. The authors also gratefully acknowledge research
support from these agencies as well as by the Council of
Scientific and Industrial Research of India, the Department of
Science and Technology, India, the Science & Engineering
Research Board (SERB), India, the Ministry of Human
Resource Development, India, the Spanish Agencia Estatal de
Investigación (AEI), the Spanish Ministerio de Ciencia e
Innovación and Ministerio de Universidades, the Conselleria de
Fons Europeus, Universitat i Cultura and the Direcció General
de Política Universitaria i Recerca del Govern de les Illes
Balears, the Conselleria d'Innovació, Universitats, Ciència i
Societat Digital de la Generalitat Valenciana and the CERCA
Programme Generalitat de Catalunya, Spain, the National
Science Centre of Poland and the European Union – European
Regional Development Fund; Foundation for Polish Science
(FNP), the Swiss National Science Foundation (SNSF), the
Russian Foundation for Basic Research, the Russian Science
Foundation, the European Commission, the European Social
Funds (ESF), the European Regional Development Funds
(ERDF), the Royal Society, the Scottish Funding Council, the
Scottish Universities Physics Alliance, the Hungarian Scientific
Research Fund (OTKA), the French Lyon Institute of Origins
(LIO), the Belgian Fonds de la Recherche Scientifique (FRS-
FNRS), Actions de Recherche Concertées (ARC) and Fonds
Wetenschappelijk Onderzoek – Vlaanderen (FWO), Belgium,
the Paris Île-de-France Region, the National Research,
Development and Innovation Office Hungary (NKFIH), the
National Research Foundation of Korea, the Natural Science
and Engineering Research Council Canada, Canadian Founda-
tion for Innovation (CFI), the Brazilian Ministry of Science,
Technology, and Innovations, the International Center for
Theoretical Physics South American Institute for Fundamental
Research (ICTP-SAIFR), the Research Grants Council of Hong
Kong, the National Natural Science Foundation of China
(NSFC), the Leverhulme Trust, the Research Corporation, the
Ministry of Science and Technology (MOST), Taiwan, the
United States Department of Energy, and the Kavli Foundation.
The authors gratefully acknowledge the support of the NSF,
STFC, INFN, and CNRS for provision of computational
resources.
This work was supported by MEXT, JSPS Leading-edge
Research Infrastructure Program, JSPS Grant-in-Aid for
Specially Promoted Research 26000005, JSPS Grant-in-Aid
for Scientific Research on Innovative Areas 2905:
JP17H06358, JP17H06361 and JP17H06364, JSPS Core-to-
Core Program A, Advanced Research Networks, JSPS Grant-
in-Aid for Scientific Research (S) 17H06133 and 20H05639,
JSPS Grant-in-Aid for Transformative Research Areas (A)
20A203: JP20H05854, the joint research program of the
Institute for Cosmic Ray Research, University of Tokyo,
National Research Foundation (NRF), Computing Infrastruc-
ture Project of Global Science experimental Data hub Center
(GSDC) at KISTI, Korea Astronomy and Space Science
Institute (KASI), and Ministry of Science and ICT (MSIT) in
Korea, Academia Sinica (AS), AS Grid Center (ASGC) and the
National Science and Technology Council (NSTC) in Taiwan
under grants including the Rising Star Program and Science
Vanguard Research Program, Advanced Technology Center
(ATC) of NAOJ, and Mechanical Engineering Center of KEK.Peer reviewe
