Mitigation of the instrumental noise transient in gravitational-wave data surrounding GW170817
In the coming years gravitational-wave detectors will undergo a series of improvements, with an increase in their detection rate by about an order of magnitude. Routine detections of gravitational-wave signals promote novel astrophysical and fundamental theory studies, while simultaneously leading to an increase in the number of detections temporally overlapping with instrumentally- or environmentally-induced transients in the detectors (glitches), often of unknown origin. Indeed, this was the case for the very first detection by the LIGO and Virgo detectors of a gravitational-wave signal consistent with a binary neutron star coalescence, GW170817. A loud glitch in the LIGO-Livingston detector, about one second before the merger, hampered coincident detection (which was initially achieved solely with LIGO-Hanford data). Moreover, accurate source characterization depends on specific assumptions about the behavior of the detector noise that are rendered invalid by the presence of glitches. In this paper, we present the various techniques employed for the initial mitigation of the glitch to perform source characterization of GW170817 and study advantages and disadvantages of each mitigation method. We show that, despite the presence of instrumental noise transients louder than the one affecting GW170817, we are still able to produce unbiased measurements of the intrinsic parameters from simulated injections with properties similar to GW170817.
© 2018 American Physical Society. Received 10 August 2018; published 10 October 2018. The authors are grateful for useful conversations with Duncan Brown and Stanislav Babak in the construction of the manuscript. C. P. is supported by the NSF Grant No. PHY-1607709, and also acknowledges support by the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA). E. A. C. thanks the LSSTC Data Science Fellowship Program; her time as a fellow has benefited this work. E. A. C. also acknowledges support from the Illinois Space Grant Consortium Graduate Fellowship Program. N. C. acknowledges support from the NSF Award No. PHY-1306702. M. E and S. V. acknowledge the support of the National Science Foundation and the Laser Interferometer Gravitational-Wave Observatory (LIGO) Laboratory. LIGO was constructed by the California Institute of Technology and Massachusetts Institute of Technology with funding from the National Science Foundation and operates under cooperative agreement PHY-0757058. The authors thank the LIGO Scientific Collaboration for access to the data and gratefully acknowledge the support of the United States National Science Foundation (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, and the Max-Planck-Society (MPS) for support of the construction of Advanced LIGO. Additional support for Advanced LIGO was provided by the Australian Research Council.
Published - PhysRevD.98.084016.pdf
Submitted - 1808.03619.pdf