346 research outputs found
Tuberculous Meningitis: Diagnosis and Treatment Overview
Tuberculous meningitis (TBM) is the most common form of central nervous system tuberculosis (TB) and has very high morbidity and mortality. TBM is typically a subacute disease with symptoms that may persist for weeks before diagnosis. Characteristic cerebrospinal fluid (CSF) findings of TBM include a lymphocytic-predominant pleiocytosis, elevated protein, and low glucose. CSF acid-fast smear and culture have relatively low sensitivity but yield is increased with multiple, large volume samples. Nucleic acid amplification of the CSF by PCR is highly specific but suboptimal sensitivity precludes ruling out TBM with a negative test. Treatment for TBM should be initiated as soon as clinical suspicion is supported by initial CSF studies. Empiric treatment should include at least four first-line drugs, preferably isoniazid, rifampin, pyrazinamide, and streptomycin or ethambutol; the role of fluoroquinolones remains to be determined. Adjunctive treatment with corticosteroids has been shown to improve mortality with TBM. In HIV-positive individuals with TBM, important treatment considerations include drug interactions, development of immune reconstitution inflammatory syndrome, unclear benefit of adjunctive corticosteroids, and higher rates of drug-resistant TB. Testing the efficacy of second-line and new anti-TB drugs in animal models of experimental TBM is needed to help determine the optimal regimen for drug-resistant TB
Search of the early O3 LIGO data for continuous gravitational waves from the Cassiopeia A and Vela Jr. supernova remnants
partially_open1412sĂŹWe present directed searches for continuous gravitational waves from the neutron stars in the Cassiopeia A (Cas A) and Vela Jr. supernova remnants. We carry out the searches in the LIGO detector data from the first six months of the third Advanced LIGO and Virgo observing run using the weave semicoherent method, which sums matched-filter detection-statistic values over many time segments spanning the observation period. No gravitational wave signal is detected in the search band of 20â976 Hz for assumed source ages greater than 300 years for Cas A and greater than 700 years for Vela Jr. Estimates from simulated continuous wave signals indicate we achieve the most sensitive results to date across the explored parameter space volume, probing to strain magnitudes as low as
âŒ6.3Ă10^â26 for Cas A and âŒ5.6Ă10^â26 for Vela Jr. at frequencies near 166 Hz at 95% efficiency.openAbbott, R.; Abbott, T.âD.; Acernese, F.; Ackley, K.; Adams, C.; Adhikari, N.; Adhikari, R.âX.; Adya, V.âB.; Affeldt, C.; Agarwal, D.; Agathos, M.; Agatsuma, K.; Aggarwal, N.; Aguiar, O.âD.; Aiello, L.; Ain, A.; Ajith, P.; Albanesi, S.; Allocca, A.; Altin, P.âA.; Amato, A.; Anand, C.; Anand, S.; Ananyeva, A.; Anderson, S.âB.; Anderson, W.âG.; Andrade, T.; Andres, N.; AndriÄ, T.; Angelova, S.âV.; Ansoldi, S.; Antelis, J.âM.; Antier, S.; Appert, S.; Arai, K.; Araya, M.âC.; Areeda, J.âS.; ArĂšne, M.; Arnaud, N.; Aronson, S.âM.; Arun, K.âG.; Asali, Y.; Ashton, G.; Assiduo, M.; Aston, S.âM.; Astone, P.; Aubin, F.; Austin, C.; Babak, S.; Badaracco, F.; Bader, M.âK.âM.; Badger, C.; Bae, S.; Baer, A.âM.; Bagnasco, S.; Bai, Y.; Baird, J.; Ball, M.; Ballardin, G.; Ballmer, S.âW.; Balsamo, A.; Baltus, G.; Banagiri, S.; Bankar, D.; Barayoga, J.âC.; Barbieri, C.; Barish, B.âC.; Barker, D.; Barneo, P.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barta, D.; Bartlett, J.; Barton, M.âA.; Bartos, I.; Bassiri, R.; Basti, A.; Bawaj, M.; Bayley, J.âC.; Baylor, A.âC.; Bazzan, M.; BĂ©csy, B.; Bedakihale, V.âM.; Bejger, M.; Belahcene, I.; Benedetto, V.; Beniwal, D.; Bennett, T.âF.; Bentley, J.âD.; BenYaala, M.; Bergamin, F.; Berger, B.âK.; Bernuzzi, S.; Bersanetti, D.; Bertolini, A.; Betzwieser, J.; Beveridge, D.; Bhandare, R.; Bhardwaj, U.; Bhattacharjee, D.; Bhaumik, S.; Bilenko, I.âA.; Billingsley, G.; Bini, S.; Birney, R.; Birnholtz, O.; Biscans, S.; Bischi, M.; Biscoveanu, S.; Bisht, A.; Biswas, B.; Bitossi, M.; Bizouard, M.-A.; Blackburn, J.âK.; Blair, C.âD.; Blair, D.âG.; Blair, R.âM.; Bobba, F.; Bode, N.; Boer, M.; Bogaert, G.; Boldrini, M.; Bonavena, L.âD.; Bondu, F.; Bonilla, E.; Bonnand, R.; Booker, P.; Boom, B.âA.; Bork, R.; Boschi, V.; Bose, N.; Bose, S.; Bossilkov, V.; Boudart, V.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Brady, P.âR.; Bramley, A.; Branch, A.; Branchesi, M.; Brau, J.âE.; Breschi, M.; Briant, T.; Briggs, J.âH.; Brillet, A.; Brinkmann, M.; Brockill, P.; Brooks, A.âF.; Brooks, J.; Brown, D.âD.; Brunett, S.; Bruno, G.; Bruntz, R.; Bryant, J.; Bulik, T.; Bulten, H.âJ.; Buonanno, A.; Buscicchio, R.; Buskulic, D.; Buy, C.; Byer, R.âL.; Cadonati, L.; Cagnoli, G.; Cahillane, C.; Bustillo, J. 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Chalathadka; Champion, E.; Chan, C.-H.; Chan, C.; Chan, C.âL.; Chan, K.; Chandra, K.; Chanial, P.; Chao, S.; Charlton, P.; Chase, E.âA.; Chassande-Mottin, E.; Chatterjee, C.; Chatterjee, Debarati; Chatterjee, Deep; Chaturvedi, M.; Chaty, S.; Chen, H.âY.; Chen, J.; Chen, X.; Chen, Y.; Chen, Z.; Cheng, H.; Cheong, C.âK.; Cheung, H.âY.; Chia, H.âY.; Chiadini, F.; Chiarini, G.; Chierici, R.; Chincarini, A.; Chiofalo, M.âL.; Chiummo, A.; Cho, G.; Cho, H.âS.; Choudhary, R.âK.; Choudhary, S.; Christensen, N.; Chu, Q.; Chua, S.; Chung, K.âW.; Ciani, G.; Ciecielag, P.; CieĆlar, M.; Cifaldi, M.; Ciobanu, A.âA.; Ciolfi, R.; Cipriano, F.; Cirone, A.; Clara, F.; Clark, E.âN.; Clark, J.âA.; Clarke, L.; Clearwater, P.; Clesse, S.; Cleva, F.; Coccia, E.; Codazzo, E.; Cohadon, P.-F.; Cohen, D.âE.; Cohen, L.; Colleoni, M.; Collette, C.âG.; Colombo, A.; Colpi, M.; Compton, C.âM.; Constancio, M.; Conti, L.; Cooper, S.âJ.; Corban, P.; Corbitt, T.âR.; Cordero-CarriĂłn, I.; Corezzi, S.; Corley, K.âR.; Cornish, N.; Corre, D.; Corsi, A.; Cortese, S.; Costa, C.âA.; Cotesta, R.; Coughlin, M.âW.; Coulon, J.-P.; Countryman, S.âT.; Cousins, B.; Couvares, P.; Coward, D.âM.; Cowart, M.âJ.; Coyne, D.âC.; Coyne, R.; Creighton, J.âD.âE.; Creighton, T.âD.; Criswell, A.âW.; Croquette, M.; Crowder, S.âG.; Cudell, J.âR.; Cullen, T.âJ.; Cumming, A.; Cummings, R.; Cunningham, L.; Cuoco, E.; CuryĆo, M.; Dabadie, P.; Canton, T. 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Hernandez; Heurs, M.; Hild, S.; Hill, P.; Hines, A.âS.; Hochheim, S.; Hofman, D.; Hohmann, J.âN.; Holcomb, D.âG.; Holland, N.âA.; Hollows, I.âJ.; Holmes, Z.âJ.; Holt, K.; Holz, D.âE.; Hopkins, P.; Hough, J.; Hourihane, S.; Howell, E.âJ.; Hoy, C.âG.; Hoyland, D.; Hreibi, A.; Hsu, Y.; Huang, Y.; HĂŒbner, M.âT.; Huddart, A.âD.; Hughey, B.; Hui, V.; Husa, S.; Huttner, S.âH.; Huxford, R.; Huynh-Dinh, T.; Idzkowski, B.; Iess, A.; Ingram, C.; Isi, M.; Isleif, K.; Iyer, B.âR.; JaberianHamedan, V.; Jacqmin, T.; Jadhav, S.âJ.; Jadhav, S.âP.; James, A.âL.; Jan, A.âZ.; Jani, K.; Janquart, J.; Janssens, K.; Janthalur, N.âN.; Jaranowski, P.; Jariwala, D.; Jaume, R.; Jenkins, A.âC.; Jenner, K.; Jeunon, M.; Jia, W.; Johns, G.âR.; Jones, A.âW.; Jones, D.âI.; Jones, J.âD.; Jones, P.; Jones, R.; Jonker, R.âJ.âG.; Ju, L.; Junker, J.; Juste, V.; Kalaghatgi, C.âV.; Kalogera, V.; Kamai, B.; Kandhasamy, S.; Kang, G.; Kanner, J.âB.; Kao, Y.; Kapadia, S.âJ.; Kapasi, D.âP.; Karat, S.; Karathanasis, C.; Karki, S.; Kashyap, R.; Kasprzack, M.; Kastaun, W.; Katsanevas, S.; Katsavounidis, E.; Katzman, W.; Kaur, T.; Kawabe, K.; KĂ©fĂ©lian, F.; Keitel, D.; Key, J.âS.; Khadka, S.; Khalili, F.âY.; Khan, S.; Khazanov, E.âA.; Khetan, N.; Khursheed, M.; Kijbunchoo, N.; Kim, C.; Kim, J.âC.; Kim, K.; Kim, W.âS.; Kim, Y.-M.; Kimball, C.; Kinley-Hanlon, M.; Kirchhoff, R.; Kissel, J.âS.; Kleybolte, L.; Klimenko, S.; Knee, A.âM.; Knowles, T.âD.; Knyazev, E.; Koch, P.; Koekoek, G.; Koley, S.; Kolitsidou, P.; Kolstein, M.; Komori, K.; Kondrashov, V.; Kontos, A.; Koper, N.; Korobko, M.; Kovalam, M.; Kozak, D.âB.; Kringel, V.; Krishnendu, N.âV.; KrĂłlak, A.; Kuehn, G.; Kuei, F.; Kuijer, P.; Kumar, A.; Kumar, P.; Kumar, Rahul; Kumar, Rakesh; Kuns, K.; Kuwahara, S.; Lagabbe, P.; Laghi, D.; Lalande, E.; Lam, T.âL.; Lamberts, A.; Landry, M.; Lane, B.âB.; Lang, R.âN.; Lange, J.; Lantz, B.; La Rosa, I.; Lartaux-Vollard, A.; Lasky, P.âD.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.; Leavey, S.; Lecoeuche, Y.âK.; Lee, H.âM.; Lee, H.âW.; Lee, J.; Lee, K.; Lehmann, J.; LemaĂźtre, A.; Leroy, N.; Letendre, N.; Levesque, C.; Levin, Y.; Leviton, J.âN.; Leyde, K.; Li, A.âK.âY.; Li, B.; Li, J.; Li, T.âG.âF.; Li, X.; Linde, F.; Linker, S.âD.; Linley, J.âN.; Littenberg, T.âB.; Liu, J.; Liu, K.; Liu, X.; Llamas, F.; Llorens-Monteagudo, M.; Lo, R.âK.âL.; Lockwood, A.; London, L.âT.; Longo, A.; Lopez, D.; Portilla, M. 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Magaña; MagazzĂč, C.; Magee, R.âM.; Maggiore, R.; Magnozzi, M.; Mahesh, S.; Majorana, E.; Makarem, C.; Maksimovic, I.; Maliakal, S.; Malik, A.; Man, N.; Mandic, V.; Mangano, V.; Mango, J.âL.; Mansell, G.âL.; Manske, M.; Mantovani, M.; Mapelli, M.; Marchesoni, F.; Marion, F.; Mark, Z.; MĂĄrka, S.; MĂĄrka, Z.; Markakis, C.; Markosyan, A.âS.; Markowitz, A.; Maros, E.; Marquina, A.; Marsat, S.; Martelli, F.; Martin, I.âW.; Martin, R.âM.; Martinez, M.; Martinez, V.âA.; Martinez, V.; Martinovic, K.; Martynov, D.âV.; Marx, E.âJ.; Masalehdan, H.; Mason, K.; Massera, E.; Masserot, A.; Massinger, T.âJ.; Masso-Reid, M.; Mastrogiovanni, S.; Matas, A.; Mateu-Lucena, M.; Matichard, F.; Matiushechkina, M.; Mavalvala, N.; McCann, J.âJ.; McCarthy, R.; McClelland, D.âE.; McClincy, P.âK.; McCormick, S.; McCuller, L.; McGhee, G.âI.; McGuire, S.âC.; McIsaac, C.; McIver, J.; McRae, T.; McWilliams, S.âT.; Meacher, D.; Mehmet, M.; Mehta, A.âK.; Meijer, Q.; Melatos, A.; Melchor, D.âA.; Mendell, G.; Menendez-Vazquez, A.; 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Rana, J.; Rapagnani, P.; Rapol, U.âD.; Ray, A.; Raymond, V.; Raza, N.; Razzano, M.; Read, J.; Rees, L.âA.; Regimbau, T.; Rei, L.; Reid, S.; Reid, S.âW.; Reitze, D.âH.; Relton, P.; Renzini, A.; Rettegno, P.; Rezac, M.; Ricci, F.; Richards, D.; Richardson, J.âW.; Richardson, L.; Riemenschneider, G.; Riles, K.; Rinaldi, S.; Rink, K.; Rizzo, M.; Robertson, N.âA.; Robie, R.; Robinet, F.; Rocchi, A.; Rodriguez, S.; Rolland, L.; Rollins, J.âG.; Romanelli, M.; Romano, R.; Romel, C.âL.; Romero-RodrĂguez, A.; Romero-Shaw, I.âM.; Romie, J.âH.; Ronchini, S.; Rosa, L.; Rose, C.âA.; RosiĆska, D.; Ross, M.âP.; Rowan, S.; Rowlinson, S.âJ.; Roy, S.; Roy, Santosh; Roy, Soumen; Rozza, D.; Ruggi, P.; Ryan, K.; Sachdev, S.; Sadecki, T.; Sadiq, J.; Sakellariadou, M.; Salafia, O.âS.; Salconi, L.; Saleem, M.; Salemi, F.; Samajdar, A.; Sanchez, E.âJ.; Sanchez, J.âH.; Sanchez, L.âE.; Sanchis-Gual, N.; Sanders, J.âR.; Sanuy, A.; Saravanan, T.âR.; Sarin, N.; Sassolas, B.; Satari, H.; Sathyaprakash, B.âS.; Sauter, O.; Savage, R.âL.; Sawant, D.; Sawant, H.âL.; Sayah, S.; Schaetzl, D.; Scheel, M.; Scheuer, J.; Schiworski, M.; Schmidt, P.; Schmidt, S.; Schnabel, R.; Schneewind, M.; Schofield, R.âM.âS.; Schönbeck, A.; Schulte, B.âW.; Schutz, B.âF.; Schwartz, E.; Scott, J.; Scott, S.âM.; Seglar-Arroyo, M.; Sellers, D.; Sengupta, A.âS.; Sentenac, D.; Seo, E.âG.; Sequino, V.; Sergeev, A.; Setyawati, Y.; Shaffer, T.; Shahriar, M.âS.; Shams, B.; Sharma, A.; Sharma, P.; Shawhan, P.; Shcheblanov, N.âS.; Shikauchi, M.; Shoemaker, D.âH.; Shoemaker, D.âM.; ShyamSundar, S.; Sieniawska, M.; Sigg, D.; Singer, L.âP.; Singh, D.; Singh, N.; Singha, A.; Sintes, A.âM.; Sipala, V.; Skliris, V.; Slagmolen, B.âJ.âJ.; Slaven-Blair, T.âJ.; Smetana, J.; Smith, J.âR.; Smith, R.âJ.âE.; Soldateschi, J.; Somala, S.âN.; Son, E.âJ.; Soni, K.; Soni, S.; Sordini, V.; Sorrentino, F.; Sorrentino, N.; Soulard, R.; Souradeep, T.; Sowell, E.; Spagnuolo, V.; Spencer, A.âP.; Spera, M.; Srinivasan, R.; Srivastava, A.âK.; Srivastava, V.; Staats, K.; Stachie, C.; Steer, D.âA.; Steinlechner, J.; Steinlechner, S.; Stops, D.âJ.; Stover, M.; Strain, K.âA.; Strang, L.âC.; Stratta, G.; Strunk, A.; Sturani, R.; Stuver, A.âL.; Sudhagar, S.; Sudhir, V.; Suh, H.âG.; Summerscales, T.âZ.; Sun, H.; Sun, L.; Sunil, S.; Sur, A.; Suresh, J.; Sutton, P.âJ.; Swinkels, B.âL.; SzczepaĆczyk, M.âJ.; Szewczyk, P.; Tacca, M.; Tait, S.âC.; Talbot, C.âJ.; Talbot, C.; Tanasijczuk, A.âJ.; Tanner, D.âB.; Tao, D.; Tao, L.; MartĂn, E.âN. Tapia San; Taranto, C.; Tasson, J.âD.; Tenorio, R.; Terhune, J.âE.; Terkowski, L.; Thirugnanasambandam, M.âP.; Thomas, M.; Thomas, P.; Thompson, J.âE.; Thondapu, S.âR.; Thorne, K.âA.; Thrane, E.; Tiwari, Shubhanshu; Tiwari, Srishti; Tiwari, V.; Toivonen, A.âM.; Toland, K.; Tolley, A.âE.; Tonelli, M.; Torres-FornĂ©, A.; Torrie, C.âI.; e Melo, I. Tosta; TöyrĂ€, D.; Trapananti, A.; Travasso, F.; Traylor, G.; Trevor, M.; Tringali, M.âC.; Tripathee, A.; Troiano, L.; Trovato, A.; Trozzo, L.; Trudeau, R.âJ.; Tsai, D.âS.; Tsai, D.; Tsang, K.âW.; Tse, M.; Tso, R.; Tsukada, L.; Tsuna, D.; Tsutsui, T.; Turbang, K.; Turconi, M.; Ubhi, A.âS.; Udall, R.âP.; Ueno, K.; Unnikrishnan, C.âS.; Urban, A.âL.; Utina, A.; Vahlbruch, H.; Vajente, G.; Vajpeyi, A.; Valdes, G.; Valentini, M.; Valsan, V.; van Bakel, N.; van Beuzekom, M.; van den Brand, J.âF.âJ.; Van Den Broeck, C.; Vander-Hyde, D.âC.; van der Schaaf, L.; van Heijningen, J.âV.; Vanosky, J.; van Remortel, N.; Vardaro, M.; Vargas, A.âF.; Varma, V.; VasĂșth, M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P.âJ.; Venneberg, J.; Venugopalan, G.; Verkindt, D.; Verma, P.; Verma, Y.; Veske, D.; Vetrano, F.; Vicere', Andrea; Vidyant, S.; Viets, A.âD.; Vijaykumar, A.; Villa-Ortega, V.; Vinet, J.-Y.; Virtuoso, A.; Vitale, S.; Vo, T.; Vocca, H.; von Reis, E.âR.âG.; von Wrangel, J.âS.âA.; Vorvick, C.; Vyatchanin, S.âP.; Wade, L.âE.; Wade, M.; Wagner, K.âJ.; Walet, R.âC.; Walker, M.; Wallace, G.âS.; Wallace, L.; Walsh, S.; Wang, J.âZ.; Wang, W.âH.; Ward, R.âL.; Warner, J.; Was, M.; Washington, N.âY.; Watchi, J.; Weaver, B.; Webster, S.âA.; Weinert, M.; Weinstein, A.âJ.; Weiss, R.; Weldon, G.; Weller, C.âM.; Wellmann, F.; Wen, L.; WeĂels, P.; Wette, K.; Whelan, J.âT.; White, D.âD.; Whiting, B.âF.; Whittle, C.; Wilken, D.; Williams, D.; Williams, M.âJ.; Williamson, A.âR.; Willis, J.âL.; Willke, B.; Wilson, D.âJ.; Winkler, W.; Wipf, C.âC.; Wlodarczyk, T.; Woan, G.; Woehler, J.; Wofford, J.âK.; Wong, I.âC.âF.; Wu, D.âS.; Wysocki, D.âM.; Xiao, L.; Yamamoto, H.; Yang, F.âW.; Yang, L.; Yang, Yang; Yang, Z.; Yap, M.âJ.; Yeeles, D.âW.; Yelikar, A.âB.; Ying, M.; Yoo, J.; Yu, Hang; Yu, Haocun; ZadroĆŒny, A.; Zanolin, M.; Zelenova, T.; Zendri, J.-P.; Zevin, M.; Zhang, J.; Zhang, L.; Zhang, T.; Zhang, Y.; Zhao, C.; Zhao, G.; Zhao, Yue; Zhou, R.; Zhou, Z.; Zhu, X.âJ.; Zimmerman, A.âB.; Zucker, M.âE.; Zweizig, J.Abbott, R.; Abbott, T. âD.; Acernese, F.; Ackley, K.; Adams, C.; Adhikari, N.; Adhikari, R. âX.; Adya, V. âB.; Affeldt, C.; Agarwal, D.; Agathos, M.; Agatsuma, K.; Aggarwal, N.; Aguiar, O. âD.; Aiello, L.; Ain, A.; Ajith, P.; Albanesi, S.; Allocca, A.; Altin, P. âA.; Amato, A.; Anand, C.; Anand, S.; Ananyeva, A.; Anderson, S. âB.; Anderson, W. âG.; Andrade, T.; Andres, N.; AndriÄ, T.; Angelova, S. âV.; Ansoldi, S.; Antelis, J. âM.; Antier, S.; Appert, S.; Arai, K.; Araya, M. âC.; Areeda, J. âS.; ArĂšne, M.; Arnaud, N.; Aronson, S. âM.; Arun, K. âG.; Asali, Y.; Ashton, G.; Assiduo, M.; Aston, S. âM.; Astone, P.; Aubin, F.; Austin, C.; Babak, S.; Badaracco, F.; Bader, M. âK. âM.; Badger, C.; Bae, S.; Baer, A. âM.; Bagnasco, S.; Bai, Y.; Baird, J.; Ball, M.; Ballardin, G.; Ballmer, S. âW.; Balsamo, A.; Baltus, G.; Banagiri, S.; Bankar, D.; Barayoga, J. âC.; Barbieri, C.; Barish, B. âC.; Barker, D.; Barneo, P.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barta, D.; Bartlett, J.; Barton, M. âA.; Bartos, I.; Bassiri, R.; Basti, A.; Bawaj, M.; Bayley, J. âC.; Baylor, A. âC.; Bazzan, M.; BĂ©csy, B.; Bedakihale, V. âM.; Bejger, M.; Belahcene, I.; Benedetto, V.; Beniwal, D.; Bennett, T. âF.; Bentley, J. âD.; Benyaala, M.; Bergamin, F.; Berger, B. âK.; Bernuzzi, S.; Bersanetti, D.; Bertolini, A.; Betzwieser, J.; Beveridge, D.; Bhandare, R.; Bhardwaj, U.; Bhattacharjee, D.; Bhaumik, S.; Bilenko, I. âA.; Billingsley, G.; Bini, S.; Birney, R.; Birnholtz, O.; Biscans, S.; Bischi, M.; Biscoveanu, S.; Bisht, A.; Biswas, B.; Bitossi,
Open Data from the Third Observing Run of LIGO, Virgo, KAGRA, and GEO
The global network of gravitational-wave observatories now includes five detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600. These detectors collected data during their third observing run, O3, composed of three phases: O3a starting in 2019 April and lasting six months, O3b starting in 2019 November and lasting five months, and O3GK starting in 2020 April and lasting two weeks. In this paper we describe these data and various other science products that can be freely accessed through the Gravitational Wave Open Science Center at https://gwosc.org. The main data set, consisting of the gravitational-wave strain time series that contains the astrophysical signals, is released together with supporting data useful for their analysis and documentation, tutorials, as well as analysis software packages
Open data from the third observing run of LIGO, Virgo, KAGRA and GEO
The global network of gravitational-wave observatories now includes five
detectors, namely LIGO Hanford, LIGO Livingston, Virgo, KAGRA, and GEO 600.
These detectors collected data during their third observing run, O3, composed
of three phases: O3a starting in April of 2019 and lasting six months, O3b
starting in November of 2019 and lasting five months, and O3GK starting in
April of 2020 and lasting 2 weeks. In this paper we describe these data and
various other science products that can be freely accessed through the
Gravitational Wave Open Science Center at https://gwosc.org. The main dataset,
consisting of the gravitational-wave strain time series that contains the
astrophysical signals, is released together with supporting data useful for
their analysis and documentation, tutorials, as well as analysis software
packages.Comment: 27 pages, 3 figure
All-sky search for long-duration gravitational-wave bursts in the third Advanced LIGO and Advanced Virgo run
After the detection of gravitational waves from compact binary coalescences, the search for transient gravitational-wave signals with less well-defined waveforms for which matched filtering is not well suited is one of the frontiers for gravitational-wave astronomy. Broadly classified into âshortâ âČ1ââs and âlongâ âł1ââs duration signals, these signals are expected from a variety of astrophysical processes, including non-axisymmetric deformations in magnetars or eccentric binary black hole coalescences. In this work, we present a search for long-duration gravitational-wave transients from Advanced LIGO and Advanced Virgoâs third observing run from April 2019 to March 2020. For this search, we use minimal assumptions for the sky location, event time, waveform morphology, and duration of the source. The search covers the range of 2â500 s in duration and a frequency band of 24â2048 Hz. We find no significant triggers within this parameter space; we report sensitivity limits on the signal strength of gravitational waves characterized by the root-sum-square amplitude hrss as a function of waveform morphology. These hrss limits improve upon the results from the second observing run by an average factor of 1.8
A Joint Fermi-GBM and Swift-BAT Analysis of Gravitational-wave Candidates from the Third Gravitational-wave Observing Run
We present Fermi Gamma-ray Burst Monitor (Fermi-GBM) and Swift Burst Alert Telescope (Swift-BAT) searches for gamma-ray/X-ray counterparts to gravitational-wave (GW) candidate events identified during the third observing run of the Advanced LIGO and Advanced Virgo detectors. Using Fermi-GBM onboard triggers and subthreshold gamma-ray burst (GRB) candidates found in the Fermi-GBM ground analyses, the Targeted Search and the Untargeted Search, we investigate whether there are any coincident GRBs associated with the GWs. We also search the Swift-BAT rate data around the GW times to determine whether a GRB counterpart is present. No counterparts are found. Using both the Fermi-GBM Targeted Search and the Swift- BAT search, we calculate flux upper limits and present joint upper limits on the gamma-ray luminosity of each GW. Given these limits, we constrain theoretical models for the emission of gamma rays from binary black hole mergers
The population of merging compact binaries inferred using gravitational waves through GWTC-3
We report on the population properties of 76 compact binary mergers detected with gravitational waves below a false alarm rate of 1 per year through GWTC-3. The catalog contains three classes of binary mergers: BBH, BNS, and NSBH mergers. We infer the BNS merger rate to be between 10 and 1700 and the NSBH merger rate to be between 7.8 and 140 , assuming a constant rate density versus comoving volume and taking the union of 90% credible intervals for methods used in this work. Accounting for the BBH merger rate to evolve with redshift, we find the BBH merger rate to be between 17.9 and 44 at a fiducial redshift (z=0.2). We obtain a broad neutron star mass distribution extending from to . We can confidently identify a rapid decrease in merger rate versus component mass between neutron star-like masses and black-hole-like masses, but there is no evidence that the merger rate increases again before 10 . We also find the BBH mass distribution has localized over- and under-densities relative to a power law distribution. While we continue to find the mass distribution of a binary's more massive component strongly decreases as a function of primary mass, we observe no evidence of a strongly suppressed merger rate above . The rate of BBH mergers is observed to increase with redshift at a rate proportional to with for . Observed black hole spins are small, with half of spin magnitudes below . We observe evidence of negative aligned spins in the population, and an increase in spin magnitude for systems with more unequal mass ratio
Search for anisotropic gravitational-wave backgrounds using data from Advanced LIGO and Advanced Virgo's first three observing runs
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 and on the
(normalized) gravitational-wave energy density spectrum from extended sources,
ranging from , depending on direction () and spectral index
(). These limits improve upon previous limits by factors of . 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 a factor of
improvement compared to previous stochastic radiometer searches.Comment: 23 Pages, 9 Figure
Population of Merging Compact Binaries Inferred Using Gravitational Waves through GWTC-3
We report on the population properties of compact binary mergers inferred from gravitational-wave observations of these systems during the first three LIGO-Virgo observing runs. The Gravitational-Wave Transient Catalog 3 (GWTC-3) contains signals consistent with three classes of binary mergers: binary black hole, binary neutron star, and neutron star-black hole mergers. We infer the binary neutron star merger rate to be between 10 and 1700 Gpc-3 yr-1 and the neutron star-black hole merger rate to be between 7.8 and 140 Gpc-3 yr-1, assuming a constant rate density in the comoving frame and taking the union of 90% credible intervals for methods used in this work. We infer the binary black hole merger rate, allowing for evolution with redshift, to be between 17.9 and 44 Gpc-3 yr-1 at a fiducial redshift (z=0.2). The rate of binary black hole mergers is observed to increase with redshift at a rate proportional to (1+z)Îș with Îș=2.9-1.8+1.7 for zâČ1. Using both binary neutron star and neutron star-black hole binaries, we obtain a broad, relatively flat neutron star mass distribution extending from 1.2-0.2+0.1 to 2.0-0.3+0.3Mâ. We confidently determine that the merger rate as a function of mass sharply declines after the expected maximum neutron star mass, but cannot yet confirm or rule out the existence of a lower mass gap between neutron stars and black holes. We also find the binary black hole mass distribution has localized over- and underdensities relative to a power-law distribution, with peaks emerging at chirp masses of 8.3-0.5+0.3 and 27.9-1.8+1.9Mâ. While we continue to find that the mass distribution of a binary's more massive component strongly decreases as a function of primary mass, we observe no evidence of a strongly suppressed merger rate above approximately 60Mâ, which would indicate the presence of a upper mass gap. Observed black hole spins are small, with half of spin magnitudes below Ïiâ0.25. While the majority of spins are preferentially aligned with the orbital angular momentum, we infer evidence of antialigned spins among the binary population. We observe an increase in spin magnitude for systems with more unequal-mass ratio. We also observe evidence of misalignment of spins relative to the orbital angular momentum
Constraints on dark photon dark matter using data from LIGO's and Virgo's third observing run
We present a search for dark photon dark matter that could couple to
gravitational-wave interferometers using data from Advanced LIGO and Virgo's
third observing run. To perform this analysis, we use two methods, one based on
cross-correlation of the strain channels in the two nearly aligned LIGO
detectors, and one that looks for excess power in the strain channels of the
LIGO and Virgo detectors. The excess power method optimizes the Fourier
Transform coherence time as a function of frequency, to account for the
expected signal width due to Doppler modulations. We do not find any evidence
of dark photon dark matter with a mass between eV/, which corresponds to frequencies between 10-2000
Hz, and therefore provide upper limits on the square of the minimum coupling of
dark photons to baryons, i.e. dark matter. For the
cross-correlation method, the best median constraint on the squared coupling is
at eV/; for the
other analysis, the best constraint is at eV/. These limits improve upon those obtained
in direct dark matter detection experiments by a factor of for
eV/, and are, in absolute terms, the
most stringent constraint so far in a large mass range eV/.Comment: 20 pages, 7 figure
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