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1. Point absorbers in Advanced LIGO

Author: Brooks, Aidan F., Vajente, Gabriele, Yamamoto, Hiro, Abbott, Rich, Adams, Carl, Adhikari, Rana X., Ananyeva, Alena, Appert, Stephen, Arai, Koji, Areeda, Joseph S., Asali, Yasmeen, Aston, Stuart M., Austin, Corey, Baer, Anne M., Ball, Matthew, Ballmer, Stefan W., Banagiri, Sharan, Barker, David, Barsotti, Lisa, Bartlett, Jeffrey, Berger, Beverly K., Betzwieser, Joseph, Bhattacharjee, Dripta, Billingsley, Garilynn, Biscans, Sebastien, Blair, Carl D., Blair, Ryan M., Bode, Nina, Booker, Phillip, Bork, Rolf, Bramley, Alyssa, Brown, Daniel D., Buikema, Aaron, Cahillane, Craig, Cannon, Kipp C., Cao, Huy Tuong, Chen, Xu, Ciobanu, Alexei A., Clara, Filiberto, Compton, Camilla, Cooper, Sam J., Corley, Kenneth R., Countryman, Stefan T., Covas, Pep B., Coyne, Dennis C., Datrier, Laurence E., Davis, Derek, Difronzo, Chiara D., Dooley, Katherine L., Driggers, Jenne C., Dupej, Peter, Dwyer, Sheila E., Effler, Anamaria, Etzel, Todd, Evans, Matthew, Evans, Tom M., Feicht, Jon, Fernandez-Galiana, Alvaro, Fritschel, Peter, Frolov, Valery V., Fulda, Paul, Fyffe, Michael, Giaime, Joe A., Giardina, Dwayne D., Godwin, Patrick, Goetz, Evan, Gras, Slawomir, Gray, Corey, Gray, Rachel, Green, Anna C., Gupta, Anchal, Gustafson, Eric K., Gustafson, Dick, Hall, Evan, Hanks, Jonathan, Hanson, Joe, Hardwick, Terra, Hasskew, Raine K., Heintze, Matthew C., Helmling-Cornell, Adrian F., Holland, Nathan A., Jones, Jeff D., Kandhasamy, Shivaraj, Karki, Sudarshan, Kasprzack, Marie, Kawabe, Keita, Kijbunchoo, Nutsinee, King, Peter J., Kissel, Jeffrey S., Kumar, Rahul, Landry, Michael, Lane, Benjamin B., Lantz, Brian, Laxen, Michael, Lecoeuche, Yannick K., Leviton, Jessica, Jian, Liu, Lormand, Marc, Lundgren, Andrew P., Macas, Ronaldas, Macinnis, Myron, Macleod, Duncan M., Mansell, Georgia L., Marka, Szabolcs, Marka, Zsuzsanna, Martynov, Denis V., Mason, Ken, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCarthy, Richard, McClelland, David E., McCormick, Scott, McCuller, Lee, McIver, Jessica, McRae, Terry, Mendell, Gregory, Merfeld, Kara, Merilh, Edmond L., Meylahn, Fabian, Mistry, Timesh, Mittleman, Richard, Moreno, Gerardo, Mow-Lowry, Conor M., Mozzon, Simone, Mullavey, Adam, Nelson, Timothy J., Nguyen, Philippe, Nuttall, Laura K., Oberling, Jason, Oram, Richard J., Osthelder, Charles, Ottaway, David J., Overmier, Harry, Palamos, Jordan R., Parker, William, Payne, Ethan, Pele, Arnaud, Penhorwood, Reilly, Perez, Carlos J., Pirello, Marc, Radkins, Hugh, Ramirez, Karla E., Richardson, Jonathan W., Riles, Keith, Robertson, Norna A., Rollins, Jameson G., Romel, Chandra L., Romie, Janeen H., Ross, Michael P., Ryan, Kyle, Sadecki, Travis, Sanchez, Eduardo J., Sanchez, Luis E., Tiruppatturrajamanikkam, Saravanan R., Savage, Richard L., Schaetzl, Dean, Schnabel, Roman, Schofield, Robert M., Schwartz, Eyal, Sellers, Danny, Shaffer, Thomas, Sigg, Daniel, Slagmolen, Bram J., Smith, Joshua R., Soni, Siddharth, Sorazu, Borja, Spencer, Andrew P., Strain, Ken A., Sun, Ling, Szczepanczyk, Marek J., Thomas, Michael, Thomas, Patrick, Thorne, Keith A., Toland, Karl, Torrie, Calum I., Traylor, Gary, Tse, Maggie, Urban, Alexander L., Valdes, Guillermo, Vander-Hyde, Daniel C., Veitch, Peter J., Venkateswara, Krishna, Venugopalan, Gautam, Viets, Aaron D., Vo, Thomas, Vorvick, Cheryl, Wade, Madeline, Ward, Robert L., Warner, Jim, Weaver, Betsy, Weiss, Rainer, Whittle, Chris, Willke, Benno, Wipf, Christopher C., Xiao, Liting, Yu, Hang, Yu, Haocun, Zhang, Liyuan, Zucker, Michael E., and Zweizig, John
Subjects: Physics - Instrumentation and Detectors, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Small, highly absorbing points are randomly present on the surfaces of the main interferometer optics in Advanced LIGO. The resulting nano-meter scale thermo-elastic deformations and substrate lenses from these micron-scale absorbers significantly reduces the sensitivity of the interferometer directly though a reduction in the power-recycling gain and indirect interactions with the feedback control system. We review the expected surface deformation from point absorbers and provide a pedagogical description of the impact on power build-up in second generation gravitational wave detectors (dual-recycled Fabry-Perot Michelson interferometers). This analysis predicts that the power-dependent reduction in interferometer performance will significantly degrade maximum stored power by up to 50% and hence, limit GW sensitivity, but suggests system wide corrections that can be implemented in current and future GW detectors. This is particularly pressing given that future GW detectors call for an order of magnitude more stored power than currently used in Advanced LIGO in Observing Run 3. We briefly review strategies to mitigate the effects of point absorbers in current and future GW wave detectors to maximize the success of these enterprises., Comment: 49 pages, 16 figures. -V2: typographical errors in equations B9 and B10 were corrected (stray exponent of "h" was removed). Caption of Figure 9 was corrected to indicate that 40mW was used for absorption in the model, not 10mW as incorrectly indicated in V1
Published: 2021
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2. Vacuum technology

Author: Zucker, Michael E., primary
Published: 2019
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3. Gravitational-wave Constraints on the Equatorial Ellipticity of Millisecond Pulsars

Author: LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Ganapathy, Dhruva, Gopakumar, A., Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Unikrishnan, C. S., Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Ganapathy, Dhruva, Gopakumar, A., Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Unikrishnan, C. S., Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, and Zucker, Michael E
Abstract: We present a search for continuous gravitational waves from five radio pulsars, comprising three recycled pulsars (PSR J0437-4715, PSR J0711-6830, and PSR J0737-3039A) and two young pulsars: the Crab pulsar (J0534+2200) and the Vela pulsar (J0835-4510). We use data from the third observing run of Advanced LIGO and Virgo combined with data from their first and second observing runs. For the first time, we are able to match (for PSR J0437-4715) or surpass (for PSR J0711-6830) the indirect limits on gravitational-wave emission from recycled pulsars inferred from their observed spin-downs, and constrain their equatorial ellipticities to be less than 10-8. For each of the five pulsars, we perform targeted searches that assume a tight coupling between the gravitational-wave and electromagnetic signal phase evolution. We also present constraints on PSR J0711-6830, the Crab pulsar, and the Vela pulsar from a search that relaxes this assumption, allowing the gravitational-wave signal to vary from the electromagnetic expectation within a narrow band of frequencies and frequency derivatives.
Published: 2022

4. All-sky search for continuous gravitational waves from isolated neutron stars using Advanced LIGO O2 data

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019 American Physical Society. We present results of an all-sky search for continuous gravitational waves (CWs), which can be produced by fast spinning neutron stars with an asymmetry around their rotation axis, using data from the second observing run of the Advanced LIGO detectors. Three different semicoherent methods are used to search in a gravitational-wave frequency band from 20 to 1922 Hz and a first frequency derivative from -1×10-8 to 2×10-9 Hz/s. None of these searches has found clear evidence for a CW signal, so upper limits on the gravitational-wave strain amplitude are calculated, which for this broad range in parameter space are the most sensitive ever achieved.
Published: 2022

5. GW190425: Observation of a Compact Binary Coalescence with Total Mass ∼ 3.4 M ⊙

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2020. The Author(s). Published by the American Astronomical Society.. On 2019 April 25, the LIGO Livingston detector observed a compact binary coalescence with signal-to-noise ratio 12.9. The Virgo detector was also taking data that did not contribute to detection due to a low signal-to-noise ratio, but were used for subsequent parameter estimation. The 90% credible intervals for the component masses range from to if we restrict the dimensionless component spin magnitudes to be smaller than 0.05). These mass parameters are consistent with the individual binary components being neutron stars. However, both the source-frame chirp mass and the total mass of this system are significantly larger than those of any other known binary neutron star (BNS) system. The possibility that one or both binary components of the system are black holes cannot be ruled out from gravitational-wave data. We discuss possible origins of the system based on its inconsistency with the known Galactic BNS population. Under the assumption that the signal was produced by a BNS coalescence, the local rate of neutron star mergers is updated to 250-2810.
Published: 2022

6. Search for Multimessenger Sources of Gravitational Waves and High-energy Neutrinos with Advanced LIGO during Its First Observing Run, ANTARES, and IceCube

Author: Massachusetts Institute of Technology. Department of Physics, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Laboratory for Nuclear Science, MIT Kavli Institute for Astrophysics and Space Research, ANTARES Collaboration, IceCube Collaboration, LIGO Scientific Collaboration, Virgo Collaboration, Arguelles Delgado, Carlos A, Axani, Spencer Nicholas, Collin, G. H., Conrad, Janet Marie, Moulai, Marjon H., Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Laboratory for Nuclear Science, MIT Kavli Institute for Astrophysics and Space Research, ANTARES Collaboration, IceCube Collaboration, LIGO Scientific Collaboration, Virgo Collaboration, Arguelles Delgado, Carlos A, Axani, Spencer Nicholas, Collin, G. H., Conrad, Janet Marie, Moulai, Marjon H., Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019. The American Astronomical Society.. Astrophysical sources of gravitational waves, such as binary neutron star and black hole mergers or core-collapse supernovae, can drive relativistic outflows, giving rise to non-thermal high-energy emission. High-energy neutrinos are signatures of such outflows. The detection of gravitational waves and high-energy neutrinos from common sources could help establish the connection between the dynamics of the progenitor and the properties of the outflow. We searched for associated emission of gravitational waves and high-energy neutrinos from astrophysical transients with minimal assumptions using data from Advanced LIGO from its first observing run O1, and data from the Antares and IceCube neutrino observatories from the same time period. We focused on candidate events whose astrophysical origins could not be determined from a single messenger. We found no significant coincident candidate, which we used to constrain the rate density of astrophysical sources dependent on their gravitational-wave and neutrino emission processes.
Published: 2022

7. Search for Gravitational-wave Signals Associated with Gamma-Ray Bursts during the Second Observing Run of Advanced LIGO and Advanced Virgo

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, IPN Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, IPN Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019. The American Astronomical Society.. We present the results of targeted searches for gravitational-wave transients associated with gamma-ray bursts during the second observing run of Advanced LIGO and Advanced Virgo, which took place from 2016 November to 2017 August. We have analyzed 98 gamma-ray bursts using an unmodeled search method that searches for generic transient gravitational waves and 42 with a modeled search method that targets compact-binary mergers as progenitors of short gamma-ray bursts. Both methods clearly detect the previously reported binary merger signal GW170817, with p-values of <9.38 10-6 (modeled) and 3.1 10-4 (unmodeled). We do not find any significant evidence for gravitational-wave signals associated with the other gamma-ray bursts analyzed, and therefore we report lower bounds on the distance to each of these, assuming various source types and signal morphologies. Using our final modeled search results, short gamma-ray burst observations, and assuming binary neutron star progenitors, we place bounds on the rate of short gamma-ray bursts as a function of redshift for z ≤ 1. We estimate 0.07-1.80 joint detections with Fermi-GBM per year for the 2019-20 LIGO-Virgo observing run and 0.15-3.90 per year when current gravitational-wave detectors are operating at their design sensitivities.
Published: 2022

8. Narrow-band search for gravitational waves from known pulsars using the second LIGO observing run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019 us. American Physical Society. American Physical Society. Isolated spinning neutron stars, asymmetric with respect to their rotation axis, are expected to be sources of continuous gravitational waves. The most sensitive searches for these sources are based on accurate matched filtering techniques that assume the continuous wave to be phase locked with the pulsar beamed emission. While matched filtering maximizes the search sensitivity, a significant signal-to-noise ratio loss will happen in the case of a mismatch between the assumed and the true signal phase evolution. Narrow-band algorithms allow for a small mismatch in the frequency and spin-down values of the pulsar while coherently integrating the entire dataset. In this paper, we describe a narrow-band search using LIGO O2 data for the continuous wave emission of 33 pulsars. No evidence of a continuous wave signal is found, and upper limits on the gravitational wave amplitude over the analyzed frequency and spin-down ranges are computed for each of the targets. In this search, we surpass the spin-down limit, namely, the maximum rotational energy loss due to gravitational waves emission for some of the pulsars already present in the LIGO O1 narrow-band search, such as J1400-6325, J1813-1246, J1833-1034, J1952+3252, and for new targets such as J0940-5428 and J1747-2809. For J1400-6325, J1833-1034, and J1747-2809, this is the first time the spin-down limit is surpassed.
Published: 2022

9. Search for Gravitational Waves from a Long-lived Remnant of the Binary Neutron Star Merger GW170817

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Laboratory for Nuclear Science, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, D. V., Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Miller, John, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yam, William, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Laboratory for Nuclear Science, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, D. V., Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Miller, John, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yam, William, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019. The American Astronomical Society. All rights reserved.. One unanswered question about the binary neutron star coalescence GW170817 is the nature of its post-merger remnant. A previous search for post-merger gravitational waves targeted high-frequency signals from a possible neutron star remnant with a maximum signal duration of 500 s. Here, we revisit the neutron star remnant scenario and focus on longer signal durations, up until the end of the second Advanced LIGO-Virgo observing run, which was 8.5 days after the coalescence of GW170817. The main physical scenario for this emission is the power-law spindown of a massive magnetar-like remnant. We use four independent search algorithms with varying degrees of restrictiveness on the signal waveform and different ways of dealing with noise artefacts. In agreement with theoretical estimates, we find no significant signal candidates. Through simulated signals, we quantify that with the current detector sensitivity, nowhere in the studied parameter space are we sensitive to a signal from more than 1 Mpc away, compared to the actual distance of 40 Mpc. However, this study serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity.
Published: 2022

10. A guide to LIGO–Virgo detector noise and extraction of transient gravitational-wave signals

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2020 IOP Publishing Ltd. The LIGO Scientific Collaboration and the Virgo Collaboration have cataloged eleven confidently detected gravitational-wave events during the first two observing runs of the advanced detector era. All eleven events were consistent with being from well-modeled mergers between compact stellar-mass objects: black holes or neutron stars. The data around the time of each of these events have been made publicly available through the gravitational-wave open science center. The entirety of the gravitational-wave strain data from the first and second observing runs have also now been made publicly available. There is considerable interest among the broad scientific community in understanding the data and methods used in the analyses. In this paper, we provide an overview of the detector noise properties and the data analysis techniques used to detect gravitational-wave signals and infer the source properties. We describe some of the checks that are performed to validate the analyses and results from the observations of gravitational-wave events. We also address concerns that have been raised about various properties of LIGO-Virgo detector noise and the correctness of our analyses as applied to the resulting data.
Published: 2022

11. Optically targeted search for gravitational waves emitted by core-collapse supernovae during the first and second observing runs of advanced LIGO and advanced Virgo

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, ASAS-SN Collaboration, DLT40 Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, ASAS-SN Collaboration, DLT40 Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2020 American Physical Society. We present the results from a search for gravitational-wave transients associated with core-collapse supernovae observed within a source distance of approximately 20 Mpc during the first and second observing runs of Advanced LIGO and Advanced Virgo. No significant gravitational-wave candidate was detected. We report the detection efficiencies as a function of the distance for waveforms derived from multidimensional numerical simulations and phenomenological extreme emission models. The sources with neutrino-driven explosions are detectable at the distances approaching 5 kpc, and for magnetorotationally driven explosions the distances are up to 54 kpc. However, waveforms for extreme emission models are detectable up to 28 Mpc. For the first time, the gravitational-wave data enabled us to exclude part of the parameter spaces of two extreme emission models with confidence up to 83%, limited by coincident data coverage. Besides, using ad hoc harmonic signals windowed with Gaussian envelopes, we constrained the gravitational-wave energy emitted during core collapse at the levels of 4.27×10-4 M·c2 and 1.28×10-1 M·c2 for emissions at 235 and 1304 Hz, respectively. These constraints are 2 orders of magnitude more stringent than previously derived in the corresponding analysis using initial LIGO, initial Virgo, and GEO 600 data.
Published: 2022

12. GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

Author: LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Knyazev, E., Lane, B. B., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Noh, M., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Knyazev, E., Lane, B. B., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Noh, M., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2020 authors. Published by the American Physical Society. Published by the American Physical Society under the terms of the "https://creativecommons.org/licenses/by/4.0/"Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO's and Virgo's third observing run. The signal was recorded on April 12, 2019 at 05â¶30â¶44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: A ∼30 MâŠ™ black hole merged with a ∼8 MâŠ™ black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einstein's general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs.
Published: 2022

13. Low-latency Gravitational-wave Alerts for Multimessenger Astronomy during the Second Advanced LIGO and Virgo Observing Run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew Hiram, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gopakumar, Achamveedu, Gras, Slawomir, Hall, E. D, Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Lane, B. B., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mohapatra, S. R. P., Ng, K. Y., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew Hiram, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gopakumar, Achamveedu, Gras, Slawomir, Hall, E. D, Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Lane, B. B., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mohapatra, S. R. P., Ng, K. Y., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019. The American Astronomical Society.. Advanced LIGO's second observing run (O2), conducted from 2016 November 30 to 2017 August 25, combined with Advanced Virgo's first observations in 2017 August, witnessed the birth of gravitational-wave multimessenger astronomy. The first ever gravitational-wave detection from the coalescence of two neutron stars, GW170817, and its gamma-ray counterpart, GRB 170817A, led to an electromagnetic follow-up of the event at an unprecedented scale. Several teams from across the world searched for EM/neutrino counterparts to GW170817, paving the way for the discovery of optical, X-ray, and radio counterparts. In this article, we describe the online identification of gravitational-wave transients and the distribution of gravitational-wave alerts by the LIGO and Virgo collaborations during O2. We also describe the gravitational-wave observables that were sent in the alerts to enable searches for their counterparts. Finally, we give an overview of the online candidate alerts shared with observing partners during O2. Alerts were issued for 14 candidates, 6 of which have been confirmed as gravitational-wave events associated with the merger of black holes or neutron stars. Of the 14 alerts, 8 were issued less than an hour after data acquisition.
Published: 2022

14. Search for Subsolar Mass Ultracompact Binaries in Advanced LIGO’s Second Observing Run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Conrad, Janet Marie, Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Conrad, Janet Marie, Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019 American Physical Society. We present a search for subsolar mass ultracompact objects in data obtained during Advanced LIGO's second observing run. In contrast to a previous search of Advanced LIGO data from the first observing run, this search includes the effects of component spin on the gravitational waveform. We identify no viable gravitational-wave candidates consistent with subsolar mass ultracompact binaries with at least one component between 0.2 Ma-1.0 Ma. We use the null result to constrain the binary merger rate of (0.2 M, 0.2 M) binaries to be less than 3.7×105 Gpc-3 yr-1 and the binary merger rate of (1.0 M, 1.0 M) binaries to be less than 5.2×103 Gpc-3 yr-1. Subsolar mass ultracompact objects are not expected to form via known stellar evolution channels, though it has been suggested that primordial density fluctuations or particle dark matter with cooling mechanisms and/or nuclear interactions could form black holes with subsolar masses. Assuming a particular primordial black hole (PBH) formation model, we constrain a population of merging 0.2 M black holes to account for less than 16% of the dark matter density and a population of merging 1.0 M black holes to account for less than 2% of the dark matter density. We discuss how constraints on the merger rate and dark matter fraction may be extended to arbitrary black hole population models that predict subsolar mass binaries.
Published: 2022

15. All-sky search in early O3 LIGO data for continuous gravitational-wave signals from unknown neutron stars in binary systems

Author: LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, K. Y., Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, K. Y., Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, and Zucker, Michael E
Abstract: Rapidly spinning neutron stars are promising sources of persistent, continuous gravitational waves. Detecting such a signal would allow probing of the physical properties of matter under extreme conditions. A significant fraction of the known pulsar population belongs to binary systems. Searching for unknown neutron stars in binary systems requires specialized algorithms to address unknown orbital frequency modulations. We present a search for continuous gravitational waves emitted by neutron stars in binary systems in early data from the third observing run of the Advanced LIGO and Advanced Virgo detectors using the semicoherent, GPU-accelerated, BinarySkyHough pipeline. The search analyzes the most sensitive frequency band of the LIGO detectors, 50 - 300 Hz. Binary orbital parameters are split into four regions, comprising orbital periods of 3 - 45 days and projected semimajor axes of 2 - 40 light-seconds. No detections are reported. We estimate the sensitivity of the search using simulated continuous wave signals, achieving the most sensitive results to date across the analyzed parameter space.
Published: 2022

16. Quantum correlations between light and the kilogram-mass mirrors of LIGO

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Yu, Haocun, McCuller, Lee P, Tse, Maggie, Barsotti, Lisa, Mavalvala, Nergis, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Matichard, Fabrice, Whittle, Christopher Mark, Buikema, Aaron, Biscans, Sebastien, Gras, Slawomir, Lane, B. B., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Mittleman, Richard K, Weiss, Rainer, Yu, Hang, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Yu, Haocun, McCuller, Lee P, Tse, Maggie, Barsotti, Lisa, Mavalvala, Nergis, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Matichard, Fabrice, Whittle, Christopher Mark, Buikema, Aaron, Biscans, Sebastien, Gras, Slawomir, Lane, B. B., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Mittleman, Richard K, Weiss, Rainer, Yu, Hang, and Zucker, Michael E
Abstract: © 2020, The Author(s), under exclusive licence to Springer Nature Limited. The measurement of minuscule forces and displacements with ever greater precision is inhibited by the Heisenberg uncertainty principle, which imposes a limit to the precision with which the position of an object can be measured continuously, known as the standard quantum limit1–4. When light is used as the probe, the standard quantum limit arises from the balance between the uncertainties of the photon radiation pressure applied to the object and of the photon number in the photoelectric detection. The only way to surpass the standard quantum limit is by introducing correlations between the position/momentum uncertainty of the object and the photon number/phase uncertainty of the light that it reflects5. Here we confirm experimentally the theoretical prediction5 that this type of quantum correlation is naturally produced in the Laser Interferometer Gravitational-wave Observatory (LIGO). We characterize and compare noise spectra taken without squeezing and with squeezed vacuum states injected at varying quadrature angles. After subtracting classical noise, our measurements show that the quantum mechanical uncertainties in the phases of the 200-kilowatt laser beams and in the positions of the 40-kilogram mirrors of the Advanced LIGO detectors yield a joint quantum uncertainty that is a factor of 1.4 (3 decibels) below the standard quantum limit. We anticipate that the use of quantum correlations will improve not only the observation of gravitational waves, but also more broadly future quantum noise-limited measurements.
Published: 2022

17. Searches for Continuous Gravitational Waves from 15 Supernova Remnants and Fomalhaut b with Advanced LIGO

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019. The American Astronomical Society. All rights reserved. We describe directed searches for continuous gravitational waves (GWs) from 16 well-localized candidate neutron stars, assuming none of the stars has a binary companion. The searches were directed toward 15 supernova remnants and Fomalhaut b, a directly imaged extrasolar planet candidate that has been suggested to be a nearby old neutron star. Each search covered a broad band of frequencies and first and second time derivatives. After coherently integrating spans of data from the first Advanced LIGO observing run of 3.5-53.7 days per search, applying data-based vetoes, and discounting known instrumental artifacts, we found no astrophysical signals. We set upper limits on intrinsic GW strain as strict as 1 ×10-25, fiducial neutron star ellipticity as strict as 2 ×10-9, and fiducial r-mode amplitude as strict as 3 ×10-8.
Published: 2022

18. Tests of General Relativity with GW170817

Author: LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Miller, J., Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yam, William, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Miller, J., Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yam, William, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: The recent discovery by Advanced LIGO and Advanced Virgo of a gravitational wave signal from a binary neutron star inspiral has enabled tests of general relativity (GR) with this new type of source. This source, for the first time, permits tests of strong-field dynamics of compact binaries in the presence of matter. In this Letter, we place constraints on the dipole radiation and possible deviations from GR in the post-Newtonian coefficients that govern the inspiral regime. Bounds on modified dispersion of gravitational waves are obtained; in combination with information from the observed electromagnetic counterpart we can also constrain effects due to large extra dimensions. Finally, the polarization content of the gravitational wave signal is studied. The results of all tests performed here show good agreement with GR.
Published: 2022

19. Search for Transient Gravitational-wave Signals Associated with Magnetar Bursts during Advanced LIGO’s Second Observing Run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019. The American Astronomical Society. All rights reserved.. We present the results of a search for short- and intermediate-duration gravitational-wave signals from four magnetar bursts in Advanced LIGO's second observing run. We find no evidence of a signal and set upper bounds on the root sum squared of the total dimensionless strain (h rss ) from incoming intermediate-duration gravitational waves ranging from 1.1 ×10 -22 at 150 Hz to 4.4 ×10 -22 at 1550 Hz at 50% detection efficiency. From the known distance to the magnetar SGR 1806-20 (8.7 kpc), we can place upper bounds on the isotropic gravitational-wave energy of 3.4 ×10 44 erg at 150 Hz assuming optimal orientation. This represents an improvement of about a factor of 10 in strain sensitivity from the previous search for such signals, conducted during initial LIGO's sixth science run. The short-duration search yielded upper limits of 2.1 ×10 44 erg for short white noise bursts, and 2.3 ×10 47 erg for 100 ms long ringdowns at 1500 Hz, both at 50% detection efficiency.
Published: 2022

20. Sensitivity and performance of the Advanced LIGO detectors in the third observing run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Buikema, Aaron, Mansell, Georgia, Barsotti, Lisa, Biscans, Sebastien, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Gras, Slawomir, Lane, B. B., MacInnis, Myron E, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Tse, Maggie, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Buikema, Aaron, Mansell, Georgia, Barsotti, Lisa, Biscans, Sebastien, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Gras, Slawomir, Lane, B. B., MacInnis, Myron E, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Tse, Maggie, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2020 authors. Published by the American Physical Society. On April 1st, 2019, the Advanced Laser Interferometer Gravitational-Wave Observatory (aLIGO), joined by the Advanced Virgo detector, began the third observing run, a year-long dedicated search for gravitational radiation. The LIGO detectors have achieved a higher duty cycle and greater sensitivity to gravitational waves than ever before, with LIGO Hanford achieving angle-averaged sensitivity to binary neutron star coalescences to a distance of 111 Mpc, and LIGO Livingston to 134 Mpc with duty factors of 74.6% and 77.0% respectively. The improvement in sensitivity and stability is a result of several upgrades to the detectors, including doubled intracavity power, the addition of an in-vacuum optical parametric oscillator for squeezed-light injection, replacement of core optics and end reaction masses, and installation of acoustic mode dampers. This paper explores the purposes behind these upgrades, and explains to the best of our knowledge the noise currently limiting the sensitivity of each detector.
Published: 2022

21. All-sky search for continuous gravitational waves from isolated neutron stars in the early O3 LIGO data

Author: LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y.-W., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Nguyen, T., Shinkai, H., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y.-W., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Nguyen, T., Shinkai, H., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, and Zucker, Michael E
Abstract: We report on an all-sky search for continuous gravitational waves in the frequency band 20-2000\,Hz and with a frequency time derivative in the range of $[-1.0, +0.1]\times10^{-8}$\,Hz/s. Such a signal could be produced by a nearby, spinning and slightly non-axisymmetric isolated neutron star in our galaxy. This search uses the LIGO data from the first six months of Advanced LIGO's and Advanced Virgo's third observational run, O3. No periodic gravitational wave signals are observed, and 95\%\ confidence-level (CL) frequentist upper limits are placed on their strengths. The lowest upper limits on worst-case (linearly polarized) strain amplitude $h_0$ are $~1.7\times10^{-25}$ near 200\,Hz. For a circularly polarized source (most favorable orientation), the lowest upper limits are $\sim6.3\times10^{-26}$. These strict frequentist upper limits refer to all sky locations and the entire range of frequency derivative values. For a population-averaged ensemble of sky locations and stellar orientations, the lowest 95\%\ CL upper limits on the strain amplitude are $\sim1.\times10^{-25}$. These upper limits improve upon our previously published all-sky results, with the greatest improvement (factor of $\sim$2) seen at higher frequencies, in part because quantum squeezing has dramatically improved the detector noise level relative to the second observational run, O2. These limits are the most constraining to date over most of the parameter space searched.
Published: 2022

22. A Joint Fermi-GBM and LIGO/Virgo Analysis of Compact Binary Mergers from the First and Second Gravitational-wave Observing Runs

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Fermi Gamma-Ray Burst Monitor, LIGO Scientific Collaboration, Virgo Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Noh, Minkyun, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Fermi Gamma-Ray Burst Monitor, LIGO Scientific Collaboration, Virgo Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Noh, Minkyun, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2020. The American Astronomical Society. All rights reserved We present results from offline searches of Fermi Gamma-ray Burst Monitor (GBM) data for gamma-ray transients coincident with the compact binary coalescences observed by the gravitational-wave (GW) detectors Advanced LIGO and Advanced Virgo during their first and second observing runs. In particular, we perform follow-up for both confirmed events and low significance candidates reported in the LIGO/Virgo catalog GWTC-1. We search for temporal coincidences between these GW signals and GBM-triggered gamma-ray bursts (GRBs). We also use the GBM Untargeted and Targeted subthreshold searches to find coincident gamma-rays below the onboard triggering threshold. This work implements a refined statistical approach by incorporating GW astrophysical source probabilities and GBM visibilities of LIGO/Virgo sky localizations to search for cumulative signatures of coincident subthreshold gamma-rays. All search methods recover the short gamma-ray burst GRB 170817A occurring ∼1.7 s after the binary neutron-star merger GW170817. We also present results from a new search seeking GBM counterparts to LIGO single-interferometer triggers. This search finds a candidate joint event, but given the nature of the GBM signal and localization, as well as the high joint false alarm rate of 1.1 10-6 Hz, we do not consider it an astrophysical association. We find no additional coincidences.
Published: 2022

23. GW190521: A Binary Black Hole Merger with a Total Mass of 150 M ⊙

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Knyazev, E., Lane, B. B., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Noh, Minkyun, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Knyazev, E., Lane, B. B., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Noh, Minkyun, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2020 authors. Published by the American Physical Society. On May 21, 2019 at 03:02:29 UTC Advanced LIGO and Advanced Virgo observed a short duration gravitational-wave signal, GW190521, with a three-detector network signal-to-noise ratio of 14.7, and an estimated false-alarm rate of 1 in 4900 yr using a search sensitive to generic transients. If GW190521 is from a quasicircular binary inspiral, then the detected signal is consistent with the merger of two black holes with masses of 85-14+21 Mm and 66-18+17 Mm (90% credible intervals). We infer that the primary black hole mass lies within the gap produced by (pulsational) pair-instability supernova processes, with only a 0.32% probability of being below 65 Mm. We calculate the mass of the remnant to be 142-16+28 Mm, which can be considered an intermediate mass black hole (IMBH). The luminosity distance of the source is 5.3-2.6+2.4 Gpc, corresponding to a redshift of 0.82-0.34+0.28. The inferred rate of mergers similar to GW190521 is 0.13-0.11+0.30 Gpc-3 yr-1.
Published: 2022

24. Search for gravitational waves from Scorpius X-1 in the second Advanced LIGO observing run with an improved hidden Markov model

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Published: 2022

25. Constraints on Cosmic Strings Using Data from the Third Advanced LIGO–Virgo Observing Run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y.-W., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, K. Y., Nguyen, T., Sekiguchi, Y., Shoemaker, David H, Stover, M., Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Wade, L. E., Wade, M., Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y.-W., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, K. Y., Nguyen, T., Sekiguchi, Y., Shoemaker, David H, Stover, M., Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Wade, L. E., Wade, M., Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, and Zucker, Michael E
Abstract: We search for gravitational-wave signals produced by cosmic strings in the Advanced LIGO and Virgo full O3 data set. Search results are presented for gravitational waves produced by cosmic string loop features such as cusps, kinks and, for the first time, kink-kink collisions.cA template-based search for short-duration transient signals does not yield a detection. We also use the stochastic gravitational-wave background energy density upper limits derived from the O3 data to constrain the cosmic string tension, $G\mu$, as a function of the number of kinks, or the number of cusps, for two cosmic string loop distribution models.cAdditionally, we develop and test a third model which interpolates between these two models. Our results improve upon the previous LIGO-Virgo constraints on $G\mu$ by one to two orders of magnitude depending on the model which is tested. In particular, for one loop distribution model, we set the most competitive constraints to date, $G\mu\lesssim 4\times 10^{-15}$.
Published: 2022

26. All-sky search for short gravitational-wave bursts in the second Advanced LIGO and Advanced Virgo run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019 American Physical Society. We present the results of a search for short-duration gravitational-wave transients in the data from the second observing run of Advanced LIGO and Advanced Virgo. We search for gravitational-wave transients with a duration of milliseconds to approximately one second in the 32-4096 Hz frequency band with minimal assumptions about the signal properties, thus targeting a wide variety of sources. We also perform a matched-filter search for gravitational-wave transients from cosmic string cusps for which the waveform is well modeled. The unmodeled search detected gravitational waves from several binary black hole mergers which have been identified by previous analyses. No other significant events have been found by either the unmodeled search or the cosmic string search. We thus present the search sensitivities for a variety of signal waveforms and report upper limits on the source rate density as a function of the characteristic frequency of the signal. These upper limits are a factor of 3 lower than the first observing run, with a 50% detection probability for gravitational-wave emissions with energies of ∼10-9 Mc2 at 153 Hz. For the search dedicated to cosmic string cusps we consider several loop distribution models, and present updated constraints from the same search done in the first observing run.
Published: 2022

27. Quantum-Enhanced Advanced LIGO Detectors in the Era of Gravitational-Wave Astronomy

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Tse, Maggie, Yu, Haocun, Fernandez Galiana, Alvaro-Miguel, Barsotti, Lisa, Evans, Matthew, Fritschel, Peter K, Mansell, Georgia, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Miller, J., Oelker, Eric Glenn, Phinney, Isabelle Y., Whittle, Christopher Mark, Biscans, Sebastien, Buikema, Aaron, Gras, Slawomir, Lane, B. B., MacInnis, Myron E, Mason, Kenneth R, Massinger, Thomas J., Mittleman, Richard K, Weiss, Rainer, Yu, Hang, Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Tse, Maggie, Yu, Haocun, Fernandez Galiana, Alvaro-Miguel, Barsotti, Lisa, Evans, Matthew, Fritschel, Peter K, Mansell, Georgia, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Miller, J., Oelker, Eric Glenn, Phinney, Isabelle Y., Whittle, Christopher Mark, Biscans, Sebastien, Buikema, Aaron, Gras, Slawomir, Lane, B. B., MacInnis, Myron E, Mason, Kenneth R, Massinger, Thomas J., Mittleman, Richard K, Weiss, Rainer, Yu, Hang, and Zucker, Michael E
Abstract: © 2019 authors. Published by the American Physical Society. Published by the American Physical Society under the terms of the https://creativecommons.org/licenses/by/4.0/ Creative Commons Attribution 4.0 International license. Further distribution of this work must maintain attribution to the author(s) and the published article's title, journal citation, and DOI. The Laser Interferometer Gravitational Wave Observatory (LIGO) has been directly detecting gravitational waves from compact binary mergers since 2015. We report on the first use of squeezed vacuum states in the direct measurement of gravitational waves with the Advanced LIGO H1 and L1 detectors. This achievement is the culmination of decades of research to implement squeezed states in gravitational-wave detectors. During the ongoing O3 observation run, squeezed states are improving the sensitivity of the LIGO interferometers to signals above 50 Hz by up to 3 dB, thereby increasing the expected detection rate by 40% (H1) and 50% (L1).
Published: 2022

28. First Measurement of the Hubble Constant from a Dark Standard Siren using the Dark Energy Survey Galaxies and the LIGO/Virgo Binary–Black-hole Merger GW170814

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, The DES Collaboration, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, The DES Collaboration, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2019. The American Astronomical Society. All rights reserved. We present a multi-messenger measurement of the Hubble constant H 0 using the binary-black-hole merger GW170814 as a standard siren, combined with a photometric redshift catalog from the Dark Energy Survey (DES). The luminosity distance is obtained from the gravitational wave signal detected by the Laser Interferometer Gravitational-Wave Observatory (LIGO)/Virgo Collaboration (LVC) on 2017 August 14, and the redshift information is provided by the DES Year 3 data. Black hole mergers such as GW170814 are expected to lack bright electromagnetic emission to uniquely identify their host galaxies and build an object-by-object Hubble diagram. However, they are suitable for a statistical measurement, provided that a galaxy catalog of adequate depth and redshift completion is available. Here we present the first Hubble parameter measurement using a black hole merger. Our analysis results in , which is consistent with both SN Ia and cosmic microwave background measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20, 140] km s-1 Mpc-1, and it depends on the assumed prior range. If we take a broader prior of [10, 220] km s-1 Mpc-1, we find (57% of the prior range). Although a weak constraint on the Hubble constant from a single event is expected using the dark siren method, a multifold increase in the LVC event rate is anticipated in the coming years and combinations of many sirens will lead to improved constraints on H 0.
Published: 2022

29. Search for continuous gravitational waves from 20 accreting millisecond x-ray pulsars in O3 LIGO data

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Chen, H. Y., Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Chen, H. Y., Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, and Zucker, Michael E
Abstract: Results are presented of searches for continuous gravitational waves from 20 accreting millisecond X-ray pulsars with accurately measured spin frequencies and orbital parameters, using data from the third observing run of the Advanced LIGO and Advanced Virgo detectors. The search algorithm uses a hidden Markov model, where the transition probabilities allow the frequency to wander according to an unbiased random walk, while the $\mathcal{J}$-statistic maximum-likelihood matched filter tracks the binary orbital phase. Three narrow sub-bands are searched for each target, centered on harmonics of the measured spin frequency. The search yields 16 candidates, consistent with a false alarm probability of 30% per sub-band and target searched. These candidates, along with one candidate from an additional target-of-opportunity search done for SAX J1808.4$-$3658, which was in outburst during one month of the observing run, cannot be confidently associated with a known noise source. Additional follow-up does not provide convincing evidence that any are a true astrophysical signal. When all candidates are assumed non-astrophysical, upper limits are set on the maximum wave strain detectable at 95% confidence, $h_0^{95\%}$. The strictest constraint is $h_0^{95\%} = 4.7\times 10^{-26}$ from IGR J17062$-$6143. Constraints on the detectable wave strain from each target lead to constraints on neutron star ellipticity and $r$-mode amplitude, the strictest of which are $\epsilon^{95\%} = 3.1\times 10^{-7}$ and $\alpha^{95\%} = 1.8\times 10^{-5}$ respectively. This analysis is the most comprehensive and sensitive search of continuous gravitational waves from accreting millisecond X-ray pulsars to date.
Published: 2022

30. All-sky search for long-duration gravitational-wave transients in the second Advanced LIGO observing run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, De Pietri, R., Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mohapatra, S. R. P., Ng, K. Y., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Robert F, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, De Pietri, R., Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y., Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mohapatra, S. R. P., Ng, K. Y., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Robert F, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Published: 2022

31. Open data from the first and second observing runs of Advanced LIGO and Advanced Virgo

Author: LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, Evan D., Haster, Carl-Johan, Huang, Yiwen, Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Noh, Minkyun, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, Evan D., Haster, Carl-Johan, Huang, Yiwen, Isi Banales, Maximiliano S, Katsavounidis, Erotokritos, Lane, B. B., Lanza Jr, Robert K, London, L. T., MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Noh, Minkyun, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: © 2021 Advanced LIGO and Advanced Virgo are monitoring the sky and collecting gravitational-wave strain data with sufficient sensitivity to detect signals routinely. In this paper we describe the data recorded by these instruments during their first and second observing runs. The main data products are gravitational-wave strain time series sampled at 16384 Hz. The datasets that include this strain measurement can be freely accessed through the Gravitational Wave Open Science Center at http://gw-openscience.org, together with data-quality information essential for the analysis of LIGO and Virgo data, documentation, tutorials, and supporting software.
Published: 2022

32. Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo’s first three observing runs

Author: LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Fujii, Y., Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y.-W., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, K. Y., Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology. Department of Physics, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Fujii, Y., Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y.-W., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, K. Y., Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, and Zucker, Michael E
Abstract: We report results from searches for anisotropic stochastic gravitational-wave backgrounds using data from the first three observing runs of the Advanced LIGO and Advanced Virgo detectors. For the first time, we include Virgo data in our analysis and run our search with a new efficient pipeline called {\tt PyStoch} on data folded over one sidereal day. We use gravitational-wave radiometry (broadband and narrow band) to produce sky maps of stochastic gravitational-wave backgrounds and to search for gravitational waves from point sources. A spherical harmonic decomposition method is employed to look for gravitational-wave emission from spatially-extended sources. Neither technique found evidence of gravitational-wave signals. Hence we derive 95\% confidence-level upper limit sky maps on the gravitational-wave energy flux from broadband point sources, ranging from $F_{\alpha, \Theta} < {\rm (0.013 - 7.6)} \times 10^{-8} {\rm erg \, cm^{-2} \, s^{-1} \, Hz^{-1}},$ and on the (normalized) gravitational-wave energy density spectrum from extended sources, ranging from $\Omega_{\alpha, \Theta} < {\rm (0.57 - 9.3)} \times 10^{-9} \, {\rm sr^{-1}}$, depending on direction ($\Theta$) and spectral index ($\alpha$). These limits improve upon previous limits by factors of $2.9 - 3.5$. We also set 95\% confidence level upper limits on the frequency-dependent strain amplitudes of quasimonochromatic gravitational waves coming from three interesting targets, Scorpius X-1, SN 1987A and the Galactic Center, with best upper limits range from $h_0 < {\rm (1.7-2.1)} \times 10^{-25},$ a factor of $\geq 2.0$ improvement compared to previous stochastic radiometer searches.
Published: 2022

33. Directional limits on persistent gravitational waves using data from Advanced LIGO’s first two observing runs

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, Aggarwal, Nancy, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Gras, Slawomir, Hall, E. D., Katsavounidis, Erotokritos, Kontos, Antonios, Lane, B. B., Lanza Jr, Robert K, Lynch, Ryan Christopher, MacInnis, Myron E, Mansell, Georgia, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Published: 2022

34. Upper limits on the isotropic gravitational-wave background from Advanced LIGO and Advanced Virgo’s third observing run

Author: LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y.-W., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, Zucker, Michael E, LIGO (Observatory : Massachusetts Institute of Technology), Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, LIGO Scientific Collaboration, Virgo Collaboration, KAGRA Collaboration, Barnum, Sam, Barsotti, Lisa, Biscans, Sebastien, Biscoveanu, Sylvia, Buikema, Aaron, Demos, Nicholas, Donovan, Frederick J, Eisenstein, Robert Alan, Evans, Matthew J, Fernandez Galiana, Alvaro-Miguel, Fishner, Jason M., Fritschel, Peter K, Ganapathy, Dhruva, Gras, Slawomir, Hall, E. D., Haster, Carl-Johan, Huang, Y.-W., Isi Banales, Maximiliano S, Jia, W., Katsavounidis, Erotokritos, Knyazev, E., Komori, Kentaro, Kuns, K., Lane, B. B., Lang, Ryan N., London, L. T., MacInnis, Myron E, Mansell, Georgia, Marx, E. J., Mason, Kenneth R, Massinger, Thomas J., Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Mo, Geoffrey, Ray Pitambar Mohapatra, Satyanarayan, Ng, Kwan Yeung, Nguyen, T., Shoemaker, David H, Sudhir, Vivishek, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Whittle, Christopher Mark, Yu, Haocun, and Zucker, Michael E
Abstract: We report results of a search for an isotropic gravitational-wave background (GWB) using data from Advanced LIGO's and Advanced Virgo's third observing run (O3) combined with upper limits from the earlier O1 and O2 runs. Unlike in previous observing runs in the advanced detector era, we include Virgo in the search for the GWB. The results are consistent with uncorrelated noise, and therefore we place upper limits on the strength of the GWB. We find that the dimensionless energy density $\Omega_{\rm GW}\leq 5.8\times 10^{-9}$ at the 95% credible level for a flat (frequency-independent) GWB, using a prior which is uniform in the log of the strength of the GWB, with 99% of the sensitivity coming from the band 20-76.6 Hz; $\leq 3.4 \times 10^{-9}$ at 25 Hz for a power-law GWB with a spectral index of 2/3 (consistent with expectations for compact binary coalescences), in the band 20-90.6 Hz; and $\leq 3.9 \times 10^{-10}$ at 25 Hz for a spectral index of 3, in the band 20-291.6 Hz. These upper limits improve over our previous results by a factor of 6.0 for a flat GWB. We also search for a GWB arising from scalar and vector modes, which are predicted by alternative theories of gravity; we place upper limits on the strength of GWBs with these polarizations. We demonstrate that there is no evidence of correlated noise of magnetic origin by performing a Bayesian analysis that allows for the presence of both a GWB and an effective magnetic background arising from geophysical Schumann resonances. We compare our upper limits to a fiducial model for the GWB from the merger of compact binaries. Finally, we combine our results with observations of individual mergers andshow that, at design sensitivity, this joint approach may yield stronger constraints on the merger rate of binary black holes at $z \lesssim 2$ than can be achieved with individually resolved mergers alone. [abridged]
Published: 2022

35. LIGO: The Laser Interferometer Gravitational-Wave Observatory

Author: Abramovici, Alex, Althouse, William E., Gürsel, Yekta, Kawamura, Seiji, Raab, Frederick J., Shoemaker, David, Sievers, Lisa, Spero, Robert E., Thorne, Kip S., Vogt, Rochus E., Weiss, Rainer, Whitcomb, Stanley E., and Zucker, Michael E.
Published: 1992

36. Gravitational Wave Observatories

Author: Jeffries, Andrew D., Saulson, Peter R., Spero, Robert E., and Zucker, Michael E.
Published: 1987

37. Predictions for the rates of compact binary coalescences observable by ground-based gravitational-wave detectors

Author: Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Blackburn, Lindy L., Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Evans, M, Fritschel, Peter K, Harry, G. M, Hughey, Barbara, Katsavounidis, Erotokritos, MacInnis, Myron E, Mason, Kenneth R, Mavalvala, Nergis, Mittleman, Richard K, Shapiro, B., Shoemaker, David H, Smith, N. D, Stein, A.J., Stein, Leo Chaim, Waldman, Samuel J., Weiss, R, Wipf, Christopher C., Zucker, Michael E, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Blackburn, Lindy L., Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Evans, M, Fritschel, Peter K, Harry, G. M, Hughey, Barbara, Katsavounidis, Erotokritos, MacInnis, Myron E, Mason, Kenneth R, Mavalvala, Nergis, Mittleman, Richard K, Shapiro, B., Shoemaker, David H, Smith, N. D, Stein, A.J., Stein, Leo Chaim, Waldman, Samuel J., Weiss, R, Wipf, Christopher C., and Zucker, Michael E
Abstract: We present an up-to-date, comprehensive summary of the rates for all types of compact binary coalescence sources detectable by the initial and advanced versions of the ground-based gravitational-wave detectors LIGO and Virgo. Astrophysical estimates for compact-binary coalescence rates depend on a number of assumptions and unknown model parameters and are still uncertain. Themost confident among these estimates are the rate predictions for coalescing binary neutron stars which are based on extrapolations from observed binary pulsars in our galaxy. These yield a likely coalescence rate of 100 Myr -1 per MilkyWay Equivalent Galaxy (MWEG), although the rate could plausibly range from 1 Myr -1 MWEG -1 to 1000 Myr -1 MWEG -1 (Kalogera et al 2004 Astrophys. J. 601 L179; Kalogera et al 2004 Astrophys. J. 614 L137 (erratum)). We convert coalescence rates into detection rates based on data from the LIGO S5 and Virgo VSR2 science runs and projected sensitivities for our advanced detectors. Using the detector sensitivities derived from these data, we find a likely detection rate of 0.02 per year for Initial LIGO-Virgo interferometers, with a plausible range between 2 × 10 -4 and 0.2 per year. The likely binary neutron-star detection rate for the Advanced LIGO-Virgo network increases to 40 events per year, with a range between 0.4 and 400 per year.
Published: 2021

38. Effects of transients in LIGO suspensions on searches for gravitational waves

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Biscans, Sebastien, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K., Gras, Slawomir, MacInnis, Myron E., Martynov, Denis, Mason, K., Matichard, Fabrice, Mavalvala, Nergis, Miller, John, Mittleman, Richard K, Shoemaker, David H, Weiss, Rainer, Yu, Hang, Yu, Haocun, Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Biscans, Sebastien, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K., Gras, Slawomir, MacInnis, Myron E., Martynov, Denis, Mason, K., Matichard, Fabrice, Mavalvala, Nergis, Miller, John, Mittleman, Richard K, Shoemaker, David H, Weiss, Rainer, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: This paper presents an analysis of the transient behavior of the Advanced LIGO (Laser Interferometer Gravitational-wave Observatory) suspensions used to seismically isolate the optics. We have characterized the transients in the longitudinal motion of the quadruple suspensions during Advanced LIGO's first observing run. Propagation of transients between stages is consistent with modeled transfer functions, such that transient motion originating at the top of the suspension chain is significantly reduced in amplitude at the test mass. We find that there are transients seen by the longitudinal motion monitors of quadruple suspensions, but they are not significantly correlated with transient motion above the noise floor in the gravitational wave strain data, and therefore do not present a dominant source of background noise in the searches for transient gravitational wave signals. Using the suspension transfer functions, we compared the transients in a week of gravitational wave strain data with transients from a quadruple suspension. Of the strain transients between 10 and 60 Hz, 84% are loud enough that they would have appeared above the sensor noise in the top stage quadruple suspension monitors if they had originated at that stage at the same frequencies. We find no significant temporal correlation with the suspension transients in that stage, so we can rule out suspension motion originating at the top stage as the cause of those transients. However, only 3.2% of the gravitational wave strain transients are loud enough that they would have been seen by the second stage suspension sensors, and none of them are above the sensor noise levels of the penultimate stage. Therefore, we cannot eliminate the possibility of transient noise in the detectors originating in the intermediate stages of the suspension below the sensing noise.
Published: 2021

39. Point absorbers in Advanced LIGO

Author: Brooks, Aidan F., primary, Vajente, Gabriele, additional, Yamamoto, Hiro, additional, Abbott, Rich, additional, Adams, Carl, additional, Adhikari, Rana X., additional, Ananyeva, Alena, additional, Appert, Stephen, additional, Arai, Koji, additional, Areeda, Joseph S., additional, Asali, Yasmeen, additional, Aston, Stuart M., additional, Austin, Corey, additional, Baer, Anne M., additional, Ball, Matthew, additional, Ballmer, Stefan W., additional, Banagiri, Sharan, additional, Barker, David, additional, Barsotti, Lisa, additional, Bartlett, Jeffrey, additional, Berger, Beverly K., additional, Betzwieser, Joseph, additional, Bhattacharjee, Dripta, additional, Billingsley, Garilynn, additional, Biscans, Sebastien, additional, Blair, Carl D., additional, Blair, Ryan M., additional, Bode, Nina, additional, Booker, Phillip, additional, Bork, Rolf, additional, Bramley, Alyssa, additional, Brown, Daniel D., additional, Buikema, Aaron, additional, Cahillane, Craig, additional, Cannon, Kipp C., additional, Cao, Huy Tuong, additional, Chen, Xu, additional, Ciobanu, Alexei A., additional, Clara, Filiberto, additional, Compton, Camilla, additional, Cooper, Sam J., additional, Corley, Kenneth R., additional, Countryman, Stefan T., additional, Covas, Pep B., additional, Coyne, Dennis C., additional, Datrier, Laurence E., additional, Davis, Derek, additional, Difronzo, Chiara D., additional, Dooley, Katherine L., additional, Driggers, Jenne C., additional, Dupej, Peter, additional, Dwyer, Sheila E., additional, Effler, Anamaria, additional, Etzel, Todd, additional, Evans, Matthew, additional, Evans, Tom M., additional, Feicht, Jon, additional, Fernandez-Galiana, Alvaro, additional, Fritschel, Peter, additional, Frolov, Valery V., additional, Fulda, Paul, additional, Fyffe, Michael, additional, Giaime, Joe A., additional, Giardina, Dwayne D., additional, Godwin, Patrick, additional, Goetz, Evan, additional, Gras, Slawomir, additional, Gray, Corey, additional, Gray, Rachel, additional, Green, Anna C., additional, Gupta, Anchal, additional, Gustafson, Eric K., additional, Gustafson, Dick, additional, Hall, Evan, additional, Hanks, Jonathan, additional, Hanson, Joe, additional, Hardwick, Terra, additional, Hasskew, Raine K., additional, Heintze, Matthew C., additional, Helmling-Cornell, Adrian F., additional, Holland, Nathan A., additional, Izmui, Kiamu, additional, Jia, Wenxuan, additional, Jones, Jeff D., additional, Kandhasamy, Shivaraj, additional, Karki, Sudarshan, additional, Kasprzack, Marie, additional, Kawabe, Keita, additional, Kijbunchoo, Nutsinee, additional, King, Peter J., additional, Kissel, Jeffrey S., additional, Kumar, Rahul, additional, Landry, Michael, additional, Lane, Benjamin B., additional, Lantz, Brian, additional, Laxen, Michael, additional, Lecoeuche, Yannick K., additional, Leviton, Jessica, additional, Jian, Liu, additional, Lormand, Marc, additional, Lundgren, Andrew P., additional, Macas, Ronaldas, additional, Macinnis, Myron, additional, Macleod, Duncan M., additional, Mansell, Georgia L., additional, Marka, Szabolcs, additional, Marka, Zsuzsanna, additional, Martynov, Denis V., additional, Mason, Ken, additional, Massinger, Thomas J., additional, Matichard, Fabrice, additional, Mavalvala, Nergis, additional, McCarthy, Richard, additional, McClelland, David E., additional, McCormick, Scott, additional, McCuller, Lee, additional, McIver, Jessica, additional, McRae, Terry, additional, Mendell, Gregory, additional, Merfeld, Kara, additional, Merilh, Edmond L., additional, Meylahn, Fabian, additional, Mistry, Timesh, additional, Mittleman, Richard, additional, Moreno, Gerardo, additional, Mow-Lowry, Conor M., additional, Mozzon, Simone, additional, Mullavey, Adam, additional, Nelson, Timothy J., additional, Nguyen, Philippe, additional, Nuttall, Laura K., additional, Oberling, Jason, additional, Oram, Richard J., additional, Osthelder, Charles, additional, Ottaway, David J., additional, Overmier, Harry, additional, Palamos, Jordan R., additional, Parker, William, additional, Payne, Ethan, additional, Pele, Arnaud, additional, Penhorwood, Reilly, additional, Perez, Carlos J., additional, Pirello, Marc, additional, Radkins, Hugh, additional, Ramirez, Karla E., additional, Richardson, Jonathan W., additional, Riles, Keith, additional, Robertson, Norna A., additional, Rollins, Jameson G., additional, Romel, Chandra L., additional, Romie, Janeen H., additional, Ross, Michael P., additional, Ryan, Kyle, additional, Sadecki, Travis, additional, Sanchez, Eduardo J., additional, Sanchez, Luis E., additional, Tiruppatturrajamanikkam, Saravanan R., additional, Savage, Richard L., additional, Schaetzl, Dean, additional, Schnabel, Roman, additional, Schofield, Robert M., additional, Schwartz, Eyal, additional, Sellers, Danny, additional, Shaffer, Thomas, additional, Sigg, Daniel, additional, Slagmolen, Bram J., additional, Smith, Joshua R., additional, Soni, Siddharth, additional, Sorazu, Borja, additional, Spencer, Andrew P., additional, Strain, Ken A., additional, Sun, Ling, additional, Szczepanczyk, Marek J., additional, Thomas, Michael, additional, Thomas, Patrick, additional, Thorne, Keith A., additional, Toland, Karl, additional, Torrie, Calum I., additional, Traylor, Gary, additional, Tse, Maggie, additional, Urban, Alexander L., additional, Valdes, Guillermo, additional, Vander-Hyde, Daniel C., additional, Veitch, Peter J., additional, Venkateswara, Krishna, additional, Venugopalan, Gautam, additional, Viets, Aaron D., additional, Vo, Thomas, additional, Vorvick, Cheryl, additional, Wade, Madeline, additional, Ward, Robert L., additional, Warner, Jim, additional, Weaver, Betsy, additional, Weiss, Rainer, additional, Whittle, Chris, additional, Willke, Benno, additional, Wipf, Christopher C., additional, Xiao, Liting, additional, Yu, Hang, additional, Yu, Haocun, additional, Zhang, Liyuan, additional, Zucker, Michael E., additional, and Zweizig, John, additional
Published: 2021
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40. Predictions for the rates of compact binary coalescences observable by ground-based gravitational-wave detectors

Author: Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Blackburn, Lindy L., Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Evans, M, Fritschel, Peter K, Harry, G. M, Hughey, Barbara, Katsavounidis, Erotokritos, MacInnis, Myron E, Mason, Kenneth R, Mavalvala, Nergis, Mittleman, Richard K, Shapiro, B., Shoemaker, David H, Smith, N. D, Stein, A.J., Stein, Leo Chaim, Waldman, Samuel J., Weiss, R, Wipf, Christopher C., Zucker, Michael E, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Blackburn, Lindy L., Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Evans, M, Fritschel, Peter K, Harry, G. M, Hughey, Barbara, Katsavounidis, Erotokritos, MacInnis, Myron E, Mason, Kenneth R, Mavalvala, Nergis, Mittleman, Richard K, Shapiro, B., Shoemaker, David H, Smith, N. D, Stein, A.J., Stein, Leo Chaim, Waldman, Samuel J., Weiss, R, Wipf, Christopher C., and Zucker, Michael E
Abstract: We present an up-to-date, comprehensive summary of the rates for all types of compact binary coalescence sources detectable by the initial and advanced versions of the ground-based gravitational-wave detectors LIGO and Virgo. Astrophysical estimates for compact-binary coalescence rates depend on a number of assumptions and unknown model parameters and are still uncertain. Themost confident among these estimates are the rate predictions for coalescing binary neutron stars which are based on extrapolations from observed binary pulsars in our galaxy. These yield a likely coalescence rate of 100 Myr -1 per MilkyWay Equivalent Galaxy (MWEG), although the rate could plausibly range from 1 Myr -1 MWEG -1 to 1000 Myr -1 MWEG -1 (Kalogera et al 2004 Astrophys. J. 601 L179; Kalogera et al 2004 Astrophys. J. 614 L137 (erratum)). We convert coalescence rates into detection rates based on data from the LIGO S5 and Virgo VSR2 science runs and projected sensitivities for our advanced detectors. Using the detector sensitivities derived from these data, we find a likely detection rate of 0.02 per year for Initial LIGO-Virgo interferometers, with a plausible range between 2 × 10 -4 and 0.2 per year. The likely binary neutron-star detection rate for the Advanced LIGO-Virgo network increases to 40 events per year, with a range between 0.4 and 400 per year. © 2010 IOP Publishing Ltd.
Published: 2020

41. Effects of data quality vetoes on a search for compact binary coalescences in Advanced LIGO’s first observing run

Author: Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, LIGO (Observatory : Massachusetts Institute of Technology), Aggarwal, Nancy, Barsotti, Lisa, Biscans, Sebastien, Brown, N. M., Buikema, Aaron, Donovan, Frederick J, Essick, Reed Clasey, Evans, M., Fritschel, Peter K, Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kontos, Antonios, Libson, Adam A., Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Miller, J., Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Oelker, Eric Glenn, Shoemaker, David H, Tse, Maggie, Vaulin, Ruslan, Vitale, Salvatore, Weiss, Rainer, Yam, William, Yu, H., Zucker, Michael E, LIGO Collaboration, Virgo Collaboration, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, LIGO (Observatory : Massachusetts Institute of Technology), Aggarwal, Nancy, Barsotti, Lisa, Biscans, Sebastien, Brown, N. M., Buikema, Aaron, Donovan, Frederick J, Essick, Reed Clasey, Evans, M., Fritschel, Peter K, Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kontos, Antonios, Libson, Adam A., Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Miller, J., Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Oelker, Eric Glenn, Shoemaker, David H, Tse, Maggie, Vaulin, Ruslan, Vitale, Salvatore, Weiss, Rainer, Yam, William, Yu, H., Zucker, Michael E, LIGO Collaboration, and Virgo Collaboration
Abstract: The first observing run of Advanced LIGO spanned 4 months, from 12 September 2015 to 19 January 2016, during which gravitational waves were directly detected from two binary black hole systems, namely GW150914 and GW151226. Confident detection of gravitational waves requires an understanding of instrumental transients and artifacts that can reduce the sensitivity of a search. Studies of the quality of the detector data yield insights into the cause of instrumental artifacts and data quality vetoes specific to a search are produced to mitigate the effects of problematic data. In this paper, the systematic removal of noisy data from analysis time is shown to improve the sensitivity of searches for compact binary coalescences. The output of the PyCBC pipeline, which is a python-based code package used to search for gravitational wave signals from compact binary coalescences, is used as a metric for improvement. GW150914 was a loud enough signal that removing noisy data did not improve its significance. However, the removal of data with excess noise decreased the false alarm rate of GW151226 by more than two orders of magnitude, from 1 in 770 yr to less than 1 in 186 000 yr. Keywords: LIGO, detector characterization; compact binary coalescences
Published: 2020

42. All-sky search for long-duration gravitational wave transients in the first Advanced LIGO observing run

Author: Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barsotti, Lisa, Biscans, Sebastien, Brown, N. M., Buikema, Aaron, Donovan, Frederick J, Eisenstein, Robert Alan, Essick, Reed Clasey, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Libson, Adam A., Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Miller, John, Mittleman, Richard K, Mohapatra, S. R. P., Oelker, Eric Glenn, Shoemaker, David H, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Yam, William, Yu, Hang, Yu, Haocun, Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barsotti, Lisa, Biscans, Sebastien, Brown, N. M., Buikema, Aaron, Donovan, Frederick J, Eisenstein, Robert Alan, Essick, Reed Clasey, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K, Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Libson, Adam A., Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Miller, John, Mittleman, Richard K, Mohapatra, S. R. P., Oelker, Eric Glenn, Shoemaker, David H, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Yam, William, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: We present the results of a search for long-duration gravitational wave transients in the data of the LIGO Hanford and LIGO Livingston second generation detectors between September 2015 and January 2016, with a total observational time of 49 d. The search targets gravitational wave transients of 10500 s duration in a frequency band of 242048 Hz, with minimal assumptions about the signal waveform, polarization, source direction, time of occurrence. No significant events were observed. As a result we set 90% confidence upper limits on the rate of long-duration gravitational wave transients for different types of gravitational wave signals. We also show that the search is sensitive to sources in the Galaxy emitting at least ∼10[superscript -8] M[subscript ⊙]c[superscript 2] in gravitational waves.
Published: 2019

43. Characterization of transient noise in Advanced LIGO relevant to gravitational wave signal GW150914

Author: Massachusetts Institute of Technology. Center for Theoretical Physics, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barsotti, Lisa, Biscans, Sebastien, Blackburn, Lindy L., Bodiya, Timothy P., Buikema, Aaron, Chatterji, Shourov K., Donovan, Frederick J, Essick, Reed Clasey, Evans, M., Fritschel, Peter K, Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kontos, Antonios, Libson, Adam A., Lynch, Ryan Christopher, MacInnis, Myron E, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Miller, John, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Oelker, Eric Glenn, Shoemaker, David H, Tse, Maggie, Vaulin, Ruslan, Vitale, Salvatore, Weiss, Rainer, Yam, William, Yu, H., Zhang, F., Zucker, Michael E, LIGO Collaboration, Virgo Collaboration, Brown N. M., Massachusetts Institute of Technology. Center for Theoretical Physics, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barsotti, Lisa, Biscans, Sebastien, Blackburn, Lindy L., Bodiya, Timothy P., Buikema, Aaron, Chatterji, Shourov K., Donovan, Frederick J, Essick, Reed Clasey, Evans, M., Fritschel, Peter K, Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kontos, Antonios, Libson, Adam A., Lynch, Ryan Christopher, MacInnis, Myron E, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Miller, John, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Oelker, Eric Glenn, Shoemaker, David H, Tse, Maggie, Vaulin, Ruslan, Vitale, Salvatore, Weiss, Rainer, Yam, William, Yu, H., Zhang, F., Zucker, Michael E, LIGO Collaboration, Virgo Collaboration, and Brown N. M.
Abstract: On 14 September 2015, a gravitational wave signal from a coalescing black hole binary system was observed by the Advanced LIGO detectors. This paper describes the transient noise backgrounds used to determine the significance of the event (designated GW150914) and presents the results of investigations into potential correlated or uncorrelated sources of transient noise in the detectors around the time of the event. The detectors were operating nominally at the time of GW150914. We have ruled out environmental influences and non-Gaussian instrument noise at either LIGO detector as the cause of the observed gravitational wave signal. Keywords: gravitational waves; detector characterization; GW150914
Published: 2019

44. Effects of waveform model systematics on the interpretation of GW150914

Author: Massachusetts Institute of Technology. Department of Physics, MIT Materials Research Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barsotti, Lisa, Biscans, Sebastien, Brown, N. M., Buikema, Aaron, Donovan, Frederick J, Eisenstein, Robert Alan, Essick, Reed Clasey, Evans, Matthew, Fernandez-Galiana, A., Fritschel, Peter K, Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Libson, Adam A., Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Miller, John E, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Oelker, Eric Glenn, Shoemaker, David H, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Yam, William, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO Collaboration, Virgo Collaboration, Massachusetts Institute of Technology. Department of Physics, MIT Materials Research Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Aggarwal, Nancy, Barsotti, Lisa, Biscans, Sebastien, Brown, N. M., Buikema, Aaron, Donovan, Frederick J, Eisenstein, Robert Alan, Essick, Reed Clasey, Evans, Matthew, Fernandez-Galiana, A., Fritschel, Peter K, Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kontos, Antonios, Lanza Jr, Robert K, Libson, Adam A., Lynch, Ryan Christopher, MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Miller, John E, Mittleman, Richard K, Ray Pitambar Mohapatra, Satyanarayan, Oelker, Eric Glenn, Shoemaker, David H, Tse, Maggie, Vitale, Salvatore, Weiss, Rainer, Yam, William, Yu, Hang, Yu, Haocun, Zucker, Michael E, LIGO Collaboration, and Virgo Collaboration
Abstract: Parameter estimates of GW150914 were obtained using Bayesian inference, based on three semi-analytic waveform models for binary black hole coalescences. These waveform models differ from each other in their treatment of black hole spins, and all three models make some simplifying assumptions, notably to neglect sub-dominant waveform harmonic modes and orbital eccentricity. Furthermore, while the models are calibrated to agree with waveforms obtained by full numerical solutions of Einstein's equations, any such calibration is accurate only to some non-zero tolerance and is limited by the accuracy of the underlying phenomenology, availability, quality, and parameter-space coverage of numerical simulations. This paper complements the original analyses of GW150914 with an investigation of the effects of possible systematic errors in the waveform models on estimates of its source parameters. To test for systematic errors we repeat the original Bayesian analysis on mock signals from numerical simulations of a series of binary configurations with parameters similar to those found for GW150914. Overall, we find no evidence for a systematic bias relative to the statistical error of the original parameter recovery of GW150914 due to modeling approximations or modeling inaccuracies. However, parameter biases are found to occur for some configurations disfavored by the data of GW150914: for binaries inclined edge-on to the detector over a small range of choices of polarization angles, and also for eccentricities greater than ∼0.05. For signals with higher signal-to-noise ratio than GW150914, or in other regions of the binary parameter space (lower masses, larger mass ratios, or higher spins), we expect that systematic errors in current waveform models may impact gravitational-wave measurements, making more accurate models desirable for future observations.
Published: 2019

45. First low-latency LIGO+Virgo search for binary inspirals and their electromagnetic counterparts

Author: Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Evans, M., Foley, Stephany, Fritschel, Peter K., Harry, Gregory, Katsavounidis, Erotokritos, Kissel, Jeffrey S., MacInnis, Myron E, Mandel, Ilya, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Mittleman, Richard K, Oelker, Eric Glenn, Shapiro, B., Shoemaker, David H, Soto, J., Stein, A. J., Stein, Leo Chaim, Vaulin, Ruslan, Waldman, Samuel J., Weiss, Rainer, Wipf, Christopher C., Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Evans, M., Foley, Stephany, Fritschel, Peter K., Harry, Gregory, Katsavounidis, Erotokritos, Kissel, Jeffrey S., MacInnis, Myron E, Mandel, Ilya, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Mittleman, Richard K, Oelker, Eric Glenn, Shapiro, B., Shoemaker, David H, Soto, J., Stein, A. J., Stein, Leo Chaim, Vaulin, Ruslan, Waldman, Samuel J., Weiss, Rainer, Wipf, Christopher C., and Zucker, Michael E
Abstract: Aims. The detection and measurement of gravitational-waves from coalescing neutron-star binary systems is an important science goal for ground-based gravitational-wave detectors. In addition to emitting gravitational-waves at frequencies that span the most sensitive bands of the LIGO and Virgo detectors, these sources are also amongst the most likely to produce an electromagnetic counterpart to the gravitational-wave emission. A joint detection of the gravitational-wave and electromagnetic signals would provide a powerful new probe for astronomy. Methods. During the period between September 19 and October 20, 2010, the first low-latency search for gravitational-waves from binary inspirals in LIGO and Virgo data was conducted. The resulting triggers were sent to electromagnetic observatories for followup. We describe the generation and processing of the low-latency gravitational-wave triggers. The results of the electromagnetic image analysis will be described elsewhere. Results. Over the course of the science run, three gravitational-wave triggers passed all of the low-latency selection cuts. Of these, one was followed up by several of our observational partners. Analysis of the gravitational-wave data leads to an estimated false alarm rate of once every 6.4 days, falling far short of the requirement for a detection based solely on gravitational-wave data.
Published: 2019

46. Improving astrophysical parameter estimation via offline noise subtraction for Advanced LIGO

Author: Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Laboratory for Nuclear Science, LIGO (Observatory : Massachusetts Institute of Technology), Vitale, Salvatore, Evans, M., Fritschel, Peter K., Barsotti, Lisa, Biscans, Sebastien, Fernandez-Galiana, A., Gras, Slawomir, Hall, Evan D., MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Shoemaker, David H, Tse, Maggie, Weiss, Rainer, Yu, Hang, Yu, Haocun, Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, Massachusetts Institute of Technology. Laboratory for Nuclear Science, LIGO (Observatory : Massachusetts Institute of Technology), Vitale, Salvatore, Evans, M., Fritschel, Peter K., Barsotti, Lisa, Biscans, Sebastien, Fernandez-Galiana, A., Gras, Slawomir, Hall, Evan D., MacInnis, Myron E, Martynov, Denis, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McCuller, Lee P, Mittleman, Richard K, Shoemaker, David H, Tse, Maggie, Weiss, Rainer, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: The Advanced LIGO detectors have recently completed their second observation run successfully. The run lasted for approximately 10 months and led to multiple new discoveries. The sensitivity to gravitational waves was partially limited by laser noise. Here, we utilize auxiliary sensors that witness these correlated noise sources, and use them for noise subtraction in the time domain data. This noise and line removal is particularly significant for the LIGO Hanford Observatory, where the improvement in sensitivity is greater than 20%. Consequently, we were also able to improve the astrophysical estimation for the location, masses, spins, and orbital parameters of the gravitational wave progenitors.
Published: 2019

47. Effects of transients in LIGO suspensions on searches for gravitational waves

Author: Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Biscans, Sebastien, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K., Gras, Slawomir, MacInnis, Myron E., Martynov, Denis, Mason, K., Matichard, Fabrice, Mavalvala, Nergis, Miller, John, Mittleman, Richard K, Shoemaker, David H, Weiss, Rainer, Yu, Hang, Yu, Haocun, Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Biscans, Sebastien, Evans, M., Fernandez Galiana, Alvaro-Miguel, Fritschel, Peter K., Gras, Slawomir, MacInnis, Myron E., Martynov, Denis, Mason, K., Matichard, Fabrice, Mavalvala, Nergis, Miller, John, Mittleman, Richard K, Shoemaker, David H, Weiss, Rainer, Yu, Hang, Yu, Haocun, and Zucker, Michael E
Abstract: This paper presents an analysis of the transient behavior of the Advanced LIGO (Laser Interferometer Gravitational-wave Observatory) suspensions used to seismically isolate the optics. We have characterized the transients in the longitudinal motion of the quadruple suspensions during Advanced LIGO's first observing run. Propagation of transients between stages is consistent with modeled transfer functions, such that transient motion originating at the top of the suspension chain is significantly reduced in amplitude at the test mass. We find that there are transients seen by the longitudinal motion monitors of quadruple suspensions, but they are not significantly correlated with transient motion above the noise floor in the gravitational wave strain data, and therefore do not present a dominant source of background noise in the searches for transient gravitational wave signals. Using the suspension transfer functions, we compared the transients in a week of gravitational wave strain data with transients from a quadruple suspension. Of the strain transients between 10 and 60 Hz, 84% are loud enough that they would have appeared above the sensor noise in the top stage quadruple suspension monitors if they had originated at that stage at the same frequencies. We find no significant temporal correlation with the suspension transients in that stage, so we can rule out suspension motion originating at the top stage as the cause of those transients. However, only 3.2% of the gravitational wave strain transients are loud enough that they would have been seen by the second stage suspension sensors, and none of them are above the sensor noise levels of the penultimate stage. Therefore, we cannot eliminate the possibility of transient noise in the detectors originating in the intermediate stages of the suspension below the sensing noise.
Published: 2019

48. A gravitational wave observatory operating beyond the quantum shot-noise limit

Author: Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Dwyer, S., Evans, Marshall, Foley, Stephany, Fritschel, Peter K, Harry, Gregory, Katsavounidis, Erotokritos, Kissel, Jeffrey S., MacInnis, Myron E, Mandel, Ilya, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Mittleman, Richard K, Oelker, Eric Glenn, Sankar, S., Shapiro, B., Shoemaker, David H, Smith, N. D., Soto, J., Stein, Abraham, Vaulin, Ruslan, Waldman, Samuel J., Weiss, Rainer, Wipf, Christopher C., Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Dwyer, S., Evans, Marshall, Foley, Stephany, Fritschel, Peter K, Harry, Gregory, Katsavounidis, Erotokritos, Kissel, Jeffrey S., MacInnis, Myron E, Mandel, Ilya, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Mittleman, Richard K, Oelker, Eric Glenn, Sankar, S., Shapiro, B., Shoemaker, David H, Smith, N. D., Soto, J., Stein, Abraham, Vaulin, Ruslan, Waldman, Samuel J., Weiss, Rainer, Wipf, Christopher C., and Zucker, Michael E
Abstract: Around the globe several observatories are seeking the first direct detection of gravitational waves (GWs). These waves are predicted by Einstein's general theory of relativity and are generated, for example, by black-hole binary systems. Present GW detectors are Michelson-type kilometre-scale laser interferometers measuring the distance changes between mirrors suspended in vacuum. The sensitivity of these detectors at frequencies above several hundred hertz is limited by the vacuum (zero-point) fluctuations of the electromagnetic field. A quantum technology - the injection of squeezed light - offers a solution to this problem. Here we demonstrate the squeezed-light enhancement of GEO 600, which will be the GW observatory operated by the LIGO Scientific Collaboration in its search for GWs for the next 3-4 years. GEO 600 now operates with its best ever sensitivity, which proves the usefulness of quantum entanglement and the qualification of squeezed light as a key technology for future GW astronomy.
Published: 2019

49. Enhanced sensitivity of the LIGO gravitational wave detector by using squeezed states of light

Author: Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Biscans, Sebastien, Bodiya, Timothy P., Donovan, Frederick J, Dwyer, S. E., Essick, Reed Clasey, Evans, M., Foley, Stephany, Fritschel, Peter K., Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kissel, Jeffrey S., Kwee, Patrick, MacInnis, Myron E, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Mittleman, Richard K, Oelker, Eric Glenn, Sankar, Shannon Reynier, Shoemaker, David H, Vaulin, Ruslan, Vitale, Salvatore, Waldman, Samuel J., Weiss, Rainer, Wipf, Christopher C., Zhang, F., Zucker, Michael E, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Biscans, Sebastien, Bodiya, Timothy P., Donovan, Frederick J, Dwyer, S. E., Essick, Reed Clasey, Evans, M., Foley, Stephany, Fritschel, Peter K., Gras, Slawomir, Isogai, Tomoki, Katsavounidis, Erotokritos, Kissel, Jeffrey S., Kwee, Patrick, MacInnis, Myron E, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, Mittleman, Richard K, Oelker, Eric Glenn, Sankar, Shannon Reynier, Shoemaker, David H, Vaulin, Ruslan, Vitale, Salvatore, Waldman, Samuel J., Weiss, Rainer, Wipf, Christopher C., Zhang, F., and Zucker, Michael E
Abstract: Nearly a century after Einstein first predicted the existence of gravitational waves, a global network of Earth-based gravitational wave observatories 1-4 is seeking to directly detect this faint radiation using precision laser interferometry. Photon shot noise, due to the quantum nature of light, imposes a fundamental limit on the attometre-level sensitivity of the kilometre-scale Michelson interferometers deployed for this task. Here, we inject squeezed states to improve the performance of one of the detectors of the Laser Interferometer Gravitational-Wave Observatory (LIGO) beyond the quantum noise limit, most notably in the frequency region down to 150 Hz, critically important for several astrophysical sources, with no deterioration of performance observed at any frequency. With the injection of squeezed states, this LIGO detector demonstrated the best broadband sensitivity to gravitational waves ever achieved, with important implications for observing the gravitational-wave Universe with unprecedented sensitivity.
Published: 2019

50. Implementation and testing of the first prompt search for gravitational wave transients with electromagnetic counterparts

Author: Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Dwyer, S., Evans, M., Foley, Stephany, Fridriksson, Joel Karl, Fritschel, Peter K., Harry, Gregory, Homan, Jeroen, Katsavounidis, Erotokritos, Kissel, Jeffrey S., MacInnis, Myron E, Mandel, Ilya, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McDaniel, P., Mittleman, Richard K, Oelker, Eric Glenn, Sankar, Shannon Reynier, Shapiro, B., Shoemaker, David H, Smith, Nicolas de Mateo, Soto, J., Stein, A., Vaulin, Ruslan, Waldman, Samuel J., Weiss, Rainer, Wipf, Christopher C., Zucker, Michael E, LIGO Collaboration, Virgo Collaboration, Massachusetts Institute of Technology. Department of Physics, Lincoln Laboratory, LIGO (Observatory : Massachusetts Institute of Technology), MIT Kavli Institute for Astrophysics and Space Research, Barsotti, Lisa, Bodiya, Timothy P., Corbitt, Thomas R, Donovan, Frederick J, Dwyer, S., Evans, M., Foley, Stephany, Fridriksson, Joel Karl, Fritschel, Peter K., Harry, Gregory, Homan, Jeroen, Katsavounidis, Erotokritos, Kissel, Jeffrey S., MacInnis, Myron E, Mandel, Ilya, Mason, Kenneth R, Matichard, Fabrice, Mavalvala, Nergis, McDaniel, P., Mittleman, Richard K, Oelker, Eric Glenn, Sankar, Shannon Reynier, Shapiro, B., Shoemaker, David H, Smith, Nicolas de Mateo, Soto, J., Stein, A., Vaulin, Ruslan, Waldman, Samuel J., Weiss, Rainer, Wipf, Christopher C., Zucker, Michael E, LIGO Collaboration, and Virgo Collaboration
Abstract: Aims. A transient astrophysical event observed in both gravitational wave (GW) and electromagnetic (EM) channels would yield rich scientific rewards. A first program initiating EM follow-ups to possible transient GW events has been developed and exercised by the LIGO and Virgo community in association with several partners. In this paper, we describe and evaluate the methods used to promptly identify and localize GW event candidates and to request images of targeted sky locations. Methods. During two observing periods (Dec. 17, 2009 to Jan. 8, 2010 and Sep. 2 to Oct. 20, 2010), a low-latency analysis pipeline was used to identify GW event candidates and to reconstruct maps of possible sky locations. A catalog of nearby galaxies and Milky Way globular clusters was used to select the most promising sky positions to be imaged, and this directional information was delivered to EM observatories with time lags of about thirty minutes. A Monte Carlo simulation has been used to evaluate the low-latency GW pipeline's ability to reconstruct source positions correctly. Results. For signals near the detection threshold, our low-latency algorithms often localized simulated GW burst signals to tens of square degrees, while neutron star/neutron star inspirals and neutron star/black hole inspirals were localized to a few hundred square degrees. Localization precision improves for moderately stronger signals. The correct sky location of signals well above threshold and originating from nearby galaxies may be observed with ∼50% or better probability with a few pointings of wide-field telescopes., United States. National Aeronautics and Space Administration (Grant NNX09AL61G)
Published: 2019

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