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Published May 10, 2012 | Published
Journal Article Open

Multimessenger science reach and analysis method for common sources of gravitational waves and high-energy neutrinos


We present the baseline multimessenger analysis method for the joint observations of gravitational waves (GW) and high-energy neutrinos (HEN), together with a detailed analysis of the expected science reach of the joint search. The analysis method combines data from GW and HEN detectors, and uses the blue-luminosity-weighted distribution of galaxies. We derive expected GW+HEN source rate upper limits for a wide range of source parameters covering several emission models. Using published sensitivities of externally triggered searches, we derive joint upper limit estimates both for the ongoing analysis with the initial LIGO-Virgo GW detectors with the partial IceCube detector (22 strings) HEN detector and for projected results to advanced LIGO-Virgo detectors with the completed IceCube (86 strings). We discuss the constraints these upper limits impose on some existing GW+HEN emission models.

Additional Information

© 2012 American Physical Society. Received 5 December 2011; published 10 May 2012. The authors thank Kipp Cannon, Eric Howell, and Eric Thrane for their useful comments. We are grateful for the generous support of Columbia University in the City of New York and the National Science Foundation under cooperative agreements PHY-0847182. The authors are grateful for support from the Swedish Research Council (VR) through the Oskar Klein Centre.We acknowledge the financial support of the National Science Foundation under Grants No. PHY-0855044 and No. PHY-0855313 to the University of Florida, Gainesville, Florida. The authors thank the European Union FP7 (Marie Curie European Reintegration Grant No. NEUTEL-APC 224898). The authors acknowledge financial support from the French Agence Nationale de la Recherche (Contract No. ANR- 08-JCJC-0061-01) and from the EU FP7 (Marie Curie Reintegration Grant). The authors gratefully acknowledge the support of the United States National Science Foundation for the construction and operation of the LIGO Laboratory and the Science and Technology Facilities Council of the United Kingdom, the Max- Planck-Society, and the State of Niedersachsen/Germany for support of the construction and operation of the GEO600 detector. The authors also gratefully acknowledge the support of the research by these agencies and by the Australian Research Council, the Council of Scientific and Industrial Research of India, the Istituto Nazionale di Fisica Nucleare of Italy, the Spanish Ministerio de Educaciόn y Ciencia, the Conselleria d'Economia, Hisenda i Innovaciό of the Govern de les Illes Balears, the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, The National Aeronautics and Space Administration, the Carnegie Trust, the Leverhulme Trust, the David and Lucile Packard Foundation, the Research Corporation, the Alfred P. Sloan Foundation, and the French Centre National de la Recherche Scientifique.

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