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151. 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: The DES Collaboration, the LIGO Scientific Collaboration, the Virgo Collaboration, Soares-Santos, M., Palmese, A., Hartley, W., Annis, J., Garcia-Bellido, J., Lahav, O., Doctor, Z., Fishbach, M., Holz, D. E., Lin, H., Pereira, M. E. S., Garcia, A., Herner, K., Kessler, R., Peiris, H. V., Sako, M., Allam, S., Brout, D., Rosell, A. Carnero, Chen, H. Y., Conselice, C., deRose, J., deVicente, J., Diehl, H. T., Gill, M. S. S., Gschwend, J., Sevilla-Noarbe, I., Tucker, D. L., Wechsler, R., Berger, E., Cowperthwaite, P. S., Metzger, B. D., Williams, P. K. G., Abbott, T. M. C., Abdalla, F. B., Avila, S., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Kind, M. Carrasco, Carretero, J., Castander, F. J., Crocce, M., Cunha, C. E., D'Andrea, C. B., da Costa, L. N., Davis, C., Desai, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Evrard, A. E., Flaugher, B., Fosalba, P., Frieman, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gruendl, R. A., Gutierrez, G., Hollowood, D. L., Hoyle, B., James, D. J., Jeltema, T., Kuehn, K., Kuropatkin, N., Li, T. S., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Neilsen, E., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Serrano, S., Smith, M., Smith, R. C., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, R. C., Walker, A. R., Wester, W., Zuntz, J., Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arene, M., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Bell, A. S., Beniwal, D., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderon, Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Cannon, K. C., Cao, H., Cao, J., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglia, M., Cavalieri, R., Cella, G., Cerda-Duran, P., Cerretani, G., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Chatziioannou, K., Cheeseboro, B. D., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Colgan, R., Colleoni, M., Collette, C. G., Collins, C., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dalya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davis, D., Daw, E. J., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deleglise, S., Del Pozzo, W., DeMarchi, L. M., Demos, N., Dent, T., De Pietri, R., Derby, J., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., Diaz, M. C., Dietrich, T., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Dmitriev, A., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Giordano, G., Glover, L., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., Gonzalez, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Groot, P., Grote, H., Grunewald, S., Guidi, G. M., Gulati, H. K., Guo, Y., Gupta, A., Gupta, M. K., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannuksela, O. A., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Haster, C. -J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Vivanco, Francisco Hernandez, Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Hreibi, A., Huerta, E. A., Hughey, B., Hulko, M., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kefelian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, H., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnendu, N., Krolak, A., Kuehn, G., Kumar, A., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A., Letendre, N., Levin, Y., Li, J., Li, K. J. L., Li, T. G. F., Li, X., Lin, F., Linde, F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lower, M. E., Luck, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., MacInnis, M., Macleod, D. M., Macquet, A., Hernandez, I. Magana, Magana-Sandoval, F., Zertuche, L. Magana, Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Marka, S., Marka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCann, J. J., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIver, J., McManus, D. J., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muniz, E. A., Muratore, M., Murray, P. G., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O'Brien, B. D., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O'Reilly, B., Ormiston, R. G., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perez, C. J., Perreca, A., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pillant, G., Pinard, L., Pirello, M., Pitkin, M., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Purrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quintero, E. A., Quitzow-James, R., Radkins, H., Radulescu, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romie, J. H., Rose, K., Rosinska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rudiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Santiago, K. A., Sarin, N., Sassolas, B., Saulson, P. R., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schonbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Shaner, M. B., Shao, L., Sharma, P., Shawhan, P., Shen, H., Shink, R., Shoemaker, D. H., Shoemaker, D. M., ShyamSundar, S., Siellez, K., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, N., Singhal, A., Sintes, A. M., Sitmukhambetov, S., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sorazu, B., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stocks, D., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepanczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tapai, M., Taracchini, A., Tasson, J. D., Taylor, R., Thies, F., Thomas, M., Thomas, P., Thondapu, S. R., Thorne, K. A., Thrane, E., Tiwari, Shubhanshu, Tiwari, Srishti, Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forne, A., Torrie, C. I., Toyra, D., Travasso, F., Traylor, G., Tringali, M. C., Trovato, A., Trozzo, L., Trudeau, R., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tuyenbayev, D., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Vahlbruch, H., Vajente, G., Valdes, G., van Bakel, N., van Beuzekom, M., Brand, J. F. J. van den, Broeck, C. Van Den, Vander-Hyde, D. C., van Heijningen, J. V., van der Schaaf, L., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasuth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Vicere, A., Viets, A. D., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Wessels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Yvert, M., Zadrozny, A. K., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A., Zucker, M. E., and Zweizig, J.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: 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 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 $H_0 = 75.2^{+39.5}_{-32.4}~{\rm km~s^{-1}~Mpc^{-1}}$, which is consistent with both SN Ia and CMB measurements of the Hubble constant. The quoted 68% credible region comprises 60% of the uniform prior range [20,140] ${\rm km~s^{-1}~Mpc^{-1}}$, and it depends on the assumed prior range. If we take a broader prior of [10,220] ${\rm km~s^{-1}~Mpc^{-1}}$, we find $H_0 = 78^{+ 96}_{-24}~{\rm km~s^{-1}~Mpc^{-1}}$ ($57\%$ 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 $H_0$., Comment: 18 pages, 2 Figures, submitted to ApJL
Published: 2019
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152. Prospects for observing and localizing gravitational-wave transients with Advanced LIGO, Advanced Virgo and KAGRA

Author: Abbott, BP, Abbott, R, Abbott, TD, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Akutsu, T, Allen, G, Allocca, A, Aloy, MA, Altin, PA, Amato, A, Ananyeva, A, Anderson, SB, Anderson, WG, Ando, M, Angelova, SV, Antier, S, Appert, S, Arai, K, Arai, Koya, Arai, Y, Araki, S, Araya, A, Araya, MC, Areeda, JS, Arène, M, Aritomi, N, Arnaud, N, Arun, KG, Ascenzi, S, Ashton, G, Aso, Y, Aston, SM, Astone, P, Aubin, F, Aufmuth, P, AultONeal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, MKM, Bae, SW, Bae, YB, Baiotti, L, Bajpai, R, Baker, PT, Baldaccini, F, Ballardin, G, Ballmer, SW, Banagiri, S, Barayoga, JC, Barclay, SE, Barish, BC, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Barton, MA, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, JC, Bazzan, M, Bécsy, B, Bejger, M, Belahcene, I, Bell, AS, Beniwal, D, Berger, BK, Bergmann, G, Bernuzzi, S, Bero, JJ, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Bilenko, IA, and Bilgili, SA
Subjects: Gravitational waves, Gravitational-wave detectors, Electromagnetic counterparts, Data analysis, KAGRA Collaboration, LIGO Scientific Collaboration and Virgo Collaboration, Astronomical and Space Sciences, Nuclear & Particles Physics
Abstract: We present our current best estimate of the plausible observing scenarios for the Advanced LIGO, Advanced Virgo and KAGRA gravitational-wave detectors over the next several years, with the intention of providing information to facilitate planning for multi-messenger astronomy with gravitational waves. We estimate the sensitivity of the network to transient gravitational-wave signals for the third (O3), fourth (O4) and fifth observing (O5) runs, including the planned upgrades of the Advanced LIGO and Advanced Virgo detectors. We study the capability of the network to determine the sky location of the source for gravitational-wave signals from the inspiral of binary systems of compact objects, that is binary neutron star, neutron star-black hole, and binary black hole systems. The ability to localize the sources is given as a sky-area probability, luminosity distance, and comoving volume. The median sky localization area (90% credible region) is expected to be a few hundreds of square degrees for all types of binary systems during O3 with the Advanced LIGO and Virgo (HLV) network. The median sky localization area will improve to a few tens of square degrees during O4 with the Advanced LIGO, Virgo, and KAGRA (HLVK) network. During O3, the median localization volume (90% credible region) is expected to be on the order of 105,106,107Mpc3 for binary neutron star, neutron star-black hole, and binary black hole systems, respectively. The localization volume in O4 is expected to be about a factor two smaller than in O3. We predict a detection count of 1-1+12 ( 10-10+52 ) for binary neutron star mergers, of 0-0+19 ( 1-1+91 ) for neutron star-black hole mergers, and 17-11+22 ( 79-44+89 ) for binary black hole mergers in a one-calendar-year observing run of the HLV network during O3 (HLVK network during O4). We evaluate sensitivity and localization expectations for unmodeled signal searches, including the search for intermediate mass black hole binary mergers.
Published: 2020

153. 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: Abbott, BP, Abbott, R, Abbott, TD, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, MA, Altin, PA, Amato, A, Anand, S, Ananyeva, A, Anderson, SB, Anderson, WG, Angelova, SV, Antier, S, Appert, S, Arai, K, Araya, MC, Areeda, JS, Arène, M, Arnaud, N, Aronson, SM, Ascenzi, S, Ashton, G, Aston, SM, Astone, P, Aubin, F, Aufmuth, P, AultONeal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, MKM, Bae, S, Baird, J, Baker, PT, Baldaccini, F, Ballardin, G, Ballmer, SW, Bals, A, Banagiri, S, Barayoga, JC, Barbieri, C, Barclay, SE, Barish, BC, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, JC, Bazzan, M, Bécsy, B, Bejger, M, Belahcene, I, Bell, AS, Beniwal, D, Benjamin, MG, Bergmann, G, Bernuzzi, S, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Biggs, E, Bilenko, IA, Bilgili, SA, Billingsley, G, Birney, IA, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, and Bitossi, M
Subjects: Astronomical Sciences, Physical Sciences, astro-ph.HE, gr-qc
Abstract: 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: 2020

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

Author: Abbott, BP, Abbott, R, Abbott, TD, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, RX, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, MA, Altin, PA, Amato, A, Anand, S, Ananyeva, A, Anderson, SB, Anderson, WG, Angelova, SV, Antier, S, Appert, S, Arai, K, Araya, MC, Areeda, JS, Arène, M, Arnaud, N, Aronson, SM, Arun, KG, Ascenzi, S, Ashton, G, Aston, SM, Astone, P, Aubin, F, Aufmuth, P, AultONeal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, MKM, Bae, S, Baird, J, Baker, PT, Baldaccini, F, Ballardin, G, Ballmer, SW, Bals, A, Banagiri, S, Barayoga, JC, Barbieri, C, Barclay, SE, Barish, BC, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, JC, Baylor, AC, Bazzan, M, Bécsy, B, Bejger, M, Belahcene, I, Bell, AS, Beniwal, D, Benjamin, MG, Berger, BK, Bergmann, G, Bernuzzi, S, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Biggs, E, Bilenko, IA, Bilgili, SA, Billingsley, G, Birney, R, Birnholtz, O, and Biscans, S
Subjects: Astronomical Sciences, Physical Sciences, astro-ph.HE, gr-qc, Astronomical and Space Sciences, Astronomy & Astrophysics, Astronomical sciences, Space sciences
Abstract: 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: 2020

155. Model comparison from LIGOVirgo data on GW170817s binary components and consequences for the merger remnant

Author: Abbott, BP, Abbott, R, Abbott, TD, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, MA, Altin, PA, Amato, A, Anand, S, Ananyeva, A, Anderson, SB, Anderson, WG, Angelova, SV, Antier, S, Appert, S, Arai, K, Araya, MC, Areeda, JS, Arne, M, Arnaud, N, Aronson, SM, Arun, KG, Ascenzi, S, Ashton, G, Aston, SM, Astone, P, Aubin, F, Aufmuth, P, AultONeal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, MKM, Bae, S, Baird, J, Baker, PT, Baldaccini, F, Ballardin, G, Ballmer, SW, Bals, A, Banagiri, S, Barayoga, JC, Barbieri, C, Barclay, SE, Barish, BC, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, JC, Bazzan, M, Bcsy, B, Bejger, M, Belahcene, I, Bell, AS, Beniwal, D, Benjamin, MG, Berger, BK, Bergmann, G, Bernuzzi, S, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Biggs, E, Bilenko, IA, Bilgili, SA, Billingsley, G, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, and Biscoveanu, S
Subjects: Astronomical Sciences, Physical Sciences, neutron stars, neutron star equation of state, gravitational wave astronomy, compact object mergers, gr-qc, astro-ph.HE, Mathematical Sciences, Nuclear & Particles Physics, Mathematical sciences, Physical sciences
Abstract: GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts, and offers an opportunity to directly probe the internal structure of neutron stars. We perform Bayesian model selection on a wide range of theoretical predictions for the neutron star equation of state. For the binary neutron star hypothesis, we find that we cannot rule out the majority of theoretical models considered. In addition, the gravitational-wave data alone does not rule out the possibility that one or both objects were low-mass black holes. We discuss the possible outcomes in the case of a binary neutron star merger, finding that all scenarios from prompt collapse to long-lived or even stable remnants are possible. For long-lived remnants, we place an upper limit of 1.9 kHz on the rotation rate. If a black hole was formed any time after merger and the coalescing stars were slowly rotating, then the maximum baryonic mass of non-rotating neutron stars is at most 3.05M⊙, and three equations of state considered here can be ruled out. We obtain a tighter limit of 2.67M⊙ for the case that the merger results in a hypermassive neutron star.
Published: 2020

156. Model comparison from LIGO-Virgo data on GW170817's binary components and consequences for the merger remnant

Author: Abbott, BP, Abbott, R, Abbott, TD, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adya, VB, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, OD, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, MA, Altin, PA, Amato, A, Anand, S, Ananyeva, A, Anderson, SB, Anderson, WG, Angelova, SV, Antier, S, Appert, S, Arai, K, Araya, MC, Areeda, JS, Arène, M, Arnaud, N, Aronson, SM, Arun, KG, Ascenzi, S, Ashton, G, Aston, SM, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, MKM, Bae, S, Baird, J, Baker, PT, Baldaccini, F, Ballardin, G, Ballmer, SW, Bals, A, Banagiri, S, Barayoga, JC, Barbieri, C, Barclay, SE, Barish, BC, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, JC, Bazzan, M, Bécsy, B, Bejger, M, Belahcene, I, Bell, AS, Beniwal, D, Benjamin, MG, Berger, BK, Bergmann, G, Bernuzzi, S, Berry, CPL, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Biggs, E, Bilenko, IA, Bilgili, SA, Billingsley, G, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, and Biscoveanu, S
Subjects: neutron stars, neutron star equation of state, gravitational wave astronomy, compact object mergers, gr-qc, astro-ph.HE, Nuclear & Particles Physics, Physical Sciences, Mathematical Sciences
Abstract: GW170817 is the very first observation of gravitational waves originating from the coalescence of two compact objects in the mass range of neutron stars, accompanied by electromagnetic counterparts, and offers an opportunity to directly probe the internal structure of neutron stars. We perform Bayesian model selection on a wide range of theoretical predictions for the neutron star equation of state. For the binary neutron star hypothesis, we find that we cannot rule out the majority of theoretical models considered. In addition, the gravitational-wave data alone does not rule out the possibility that one or both objects were low-mass black holes. We discuss the possible outcomes in the case of a binary neutron star merger, finding that all scenarios from prompt collapse to long-lived or even stable remnants are possible. For long-lived remnants, we place an upper limit of 1.9 kHz on the rotation rate. If a black hole was formed any time after merger and the coalescing stars were slowly rotating, then the maximum baryonic mass of non-rotating neutron stars is at most 3.05M⊙, and three equations of state considered here can be ruled out. We obtain a tighter limit of 2.67M⊙ for the case that the merger results in a hypermassive neutron star.
Published: 2020

157. Evaluation of Indoor Paths Based On Indoor Navigation Network Models and Space Syntax Measures

Author: Atakan Bilgili, Alper Sen, and Melih Basaraner
Subjects: indoor navigation, navigation network, wayfinding, indoor path, space syntax, isovist, visibility graph analysis, Geodesy, QB275-343
Abstract: Indoor navigation networks (models) are an essential way to characterize the navigation patterns of pedestrians. To find the most suitable path existing studies concentrate mostly on the minimization of length and turns. However, they alone may fall short to support one in wayfinding as they only consider the spatial structure of a building. Space syntax measures can reveal the interaction among spatial configurations and visibility-based spatial reasoning of pedestrians. In this paper, our original contribution is to adapt them to evaluate indoor paths. To demonstrate our approach, we first conducted a user experiment to collect the navigation patterns. Then, these navigation patterns were compared with the indoor paths through statistical comparison with respect to space syntax measures. Also, all door-from-door paths were compared by traditional and space syntax measures. The findings of the experimental study show that the visibility-based UCN is the more suitable navigation network by traditional measures. However, space syntax measures suggest that centerline-based navigation networks are more suitable. Considering traditional and space syntax measures together, the centerline-based MPRSSE is found to be the more suitable navigation network to assist one in the wayfinding process for our experimental study.
Published: 2023
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158. Machine Learning Approaches for One-Day Ahead Soil Temperature Forecasting

Author: Mehmet Bilgili, Şaban Ünal, Aliihsan Şekertekin, and Cahit Gürlek
Subjects: anfis, daily soil temperature, lstm, elman neural network (enn), feed-forward neural network, Agriculture (General), S1-972
Abstract: Present study investigates the capabilities of six distinct machine learning techniques such as ANFIS network with fuzzy c-means (ANFIS-FCM), grid partition (ANFIS-GP), subtractive clustering (ANFIS-SC), feed-forward neural network (FNN), Elman neural network (ENN), and long short-term memory (LSTM) neural network in one-day ahead soil temperature (ST) forecasting. For this aim, daily ST data gathered at three different depths of 5 cm, 50 cm, and 100 cm from the Sivas meteorological observation station in the Central Anatolia Region of Turkey was used as training and testing datasets. Forecasting values of the machine learning models were compared with actual data by assessing with respect to four statistic metrics such as the mean absolute error, root mean square error (RMSE), Nash−Sutcliffe efficiency coefficient, and correlation coefficient (R). The results showed that the ANFIS-FCM, ANFIS-GP, ANFIS-SC, ENN, FNN and LSTM models presented satisfactory performance in modeling daily ST at all depths, with RMSE values ranging 0.0637-1.3276, 0.0634-1.3809, 0.0643-1.3280, 0.0635-1.3186, 0.0635-1.3281, and 0.0983-1.3256 °C, and R values ranging 0.9910-0.9999, 0.9903-0.9999, 0.9910-0.9999, 0.9911-0.9999, 0.9910-0.9999 and 0.9910-0.9998 °C, respectively.
Published: 2023
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159. The Effects of Different Irrigation Levels and Nitrogen Doses on Growth, Quality and Physiological Parameters of Warm-season Turfgrasses

Author: Müge Kesici, Asuman Cansev, Burak Nazmi Candoğan, Sinem Zere Taşkın, Fikret Yönter, and Ugur Bilgili
Subjects: deficit irrigation, nitrogen fertilization, turf color, turf physiology, Agriculture (General), S1-972
Abstract: This research was conducted to determine to effects of different irrigation levels and nitrogen doses (ND) on the various warm-season turfgrasses at the Agricultural Training and Research Centre of the Bursa Uludag University Faculty of Agriculture for two years in a row. The experimental design was the randomized blocks in a split-split plot design with three replications. The main plot was irrigation levels (I1=25%, I2=50%, I3=75%, and I4=100% of pan evaporation), subplots were turfgrass species [hybrid Bermudagrass (Cynodon transvaalensis x Cynodon dactylon) cv. Tifdwarf, seashore paspalum (Paspalum vaginatum Sw.) cv. Seaspray, zoysiagrass (Zoysia japonica Steud.) cv. Zenit], and sub subplots were ND’s (monthly 0.0, 1.25, 2.5, and 5.0 g N m-²). Visual turfgrass color and quality, clipping yield, leaf relative water content (RWC), loss of turgidity (LT), chlorophyll content (CC), and electrolyte leakage were measured. According to the results, significant differences were determined among irrigation levels, turfgrass species, and ND’s for color, quality, clipping yield and physiological parameters. Turfgrass visual color, quality and clippingyield were shown to decrease significantly with decreases in irrigation water and N fertilizer. The study findings demonstrated that under a non-limiting water supply, irrigation could be decreased by adjusting N fertilizer rates with I3N3 treatments can maintain acceptable turfgrass visual color and quality under Mediterranean climatic conditions. In addition, at 25% (I1) deficit irrigationlevel, leaf RWC, CC decreased significantly, while an increase was determined in LT. This research indicated that under 75% (I3) deficit irrigation and N3 ND, acceptable quality can be maintained with ‘seaspray’ seashore paspalum under Mediterranean climate performed.
Published: 2023
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160. Using Peer Supports to Encourage Adolescents with Autism Spectrum Disorder to Show Interest in Their Conversation Partners

Author: Bambara, Linda M., Cole, Christine L., Telesford, Alana, Bauer, Kathleen, Bilgili-Karabacak, Irem, Weir, Amanda, and Thomas, Amanda
Abstract: Purpose: This study was conducted to evaluate the effects of a multicomponent peer-mediated intervention (PMI) on teaching adolescents with autism spectrum disorder (ASD) how to show interest in peer conversation partners by asking partner-focused questions about the person, their interests, or their experiences and by making partner-focused comments that positively affirm peer statements or express concern. Method: A multiple-baseline design across three verbally fluent high school students with ASD was used to assess the effects of the PMI, which involved training peers (n = 10) to support conversation and the students' use of target skills, and training the students to use partner-focused skills with the aid of a self-reflection cue sheet during conversation with trained peers in a high school cafeteria. Ten-minute samples of student--peer conversations were transcribed and analyzed. Generalization with untrained peers was assessed. Results: The PMI was highly effective in increasing all students' use of partner-focused skills. Gains were maintained by two students in a return-to-baseline condition. Generalization was evident for all students with varied results. Peers and students with ASD perceived the intervention to be beneficial. Conclusions: This study adds to the limited research showing that PMI can be used in high school settings to improve target conversational skills and provides preliminary evidence that PMI can successfully address an underresearched pragmatic language difficulty (i.e., introducing and maintaining topics of conversation of relevance and interest to conversation partners) common among adolescents with ASD. These findings invite replication to extend generality and assess the impact of the intervention on peer relationships.
Published: 2021
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161. Determination of the weights of external conditions for ship resistance

Author: Bilgili, Levent
Published: 2023
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162. Effects of alternative refrigerants on the ejector dimensions for single and dual ejectors enhanced bus air conditioning system

Author: Ünal, Şaban, Erdinç, M. Tahir, Akgün, Hakan, and Bilgili, Mehmet
Published: 2023
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163. The role of solar energy usage in environmental sustainability: Fresh evidence through time-frequency analyses

Author: Kuşkaya, Sevda, Bilgili, Faik, Muğaloğlu, Erhan, Khan, Kamran, Hoque, Mohammad Enamul, and Toguç, Nurhan
Published: 2023
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164. One-hour ahead wind speed forecasting using deep learning approach

Author: Ozbek, Arif, Ilhan, Akin, Bilgili, Mehmet, and Sahin, Besir
Published: 2022
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165. Wavelet coherence analysis and exchange rate movements

Author: Kuşkaya, Sevda, Toğuç, Nurhan, and Bilgili, Faik
Published: 2022
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166. Daily average relative humidity forecasting with LSTM neural network and ANFIS approaches

Author: Ozbek, Arif, Ünal, Şaban, and Bilgili, Mehmet
Published: 2022
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167. The dynamic analysis of renewable energy’s contribution to the dimensions of sustainable development and energy security

Author: Bilgili, Faik and Bağlıtaş, Hayriye Hilal
Published: 2022
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168. Fibular fixation improves ankle functional outcomes and alignment in the intramedullary nailing of distal third tibiofibular diaphyseal fractures

Author: Duramaz, Altuğ, Koluman, Ali Can, Bayrak, Alkan, Ziroğlu, Nezih, Bilgili, Mustafa Gökhan, and Kural, Cemal
Published: 2022
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169. An Advantageous Donor Site Alternative for Preparing Crushed Cartilage Graft: The Postero-inferior Part of the Septal Cartilage

Author: Özkan, Aret Çerçi, Kozanoğlu, Erol, Bilgili, Ahmet Mert, Öngüt, Cüneyt, and Agbulut, Onnik
Published: 2022
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170. Platforms Offered to Human Use in the Process of Information Sharing

Author: Bilgili, Asiye, primary and Ravan Bakhsh, Maziar, additional
Published: 2023
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171. LCA Studies on Marine Alternative Fuels

Author: Bilgili, Levent, primary
Published: 2023
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172. IfNot: An approach towards mitigating interest flooding attacks in Named Data Networking of Things.

Author: Sedat Bilgili, Alper Kamil Demir, and Shahid Alam
Published: 2024
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173. Psychiatrische Ansätze zur Behandlung von sozialem Trauma: Von der normalen Reaktion zur Psychopathologie und psychobiologischen Konzeptionen

Author: Özçürümez Bilgili, Gamze, Hamburger, Andreas, editor, Hancheva, Camellia, editor, and Volkan, Vamık, editor
Published: 2022
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174. Artificial neural network approach for monthly air temperature estimations and maps

Author: Bilgili, Mehmet, Ozbek, Arif, Yildirim, Alper, and Simsek, Erdogan
Published: 2023
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175. Tool flank wear prediction using high-frequency machine data from industrial edge device

Author: Bilgili, Deniz, Kecibas, Gamze, Besirova, Cemile, Chehrehzad, Mohammad Reza, Burun, Gizem, Pehlivan, Toprak, Uresin, Ugur, Emekli, Engin, and Lazoglu, Ismail
Published: 2023
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176. Mycorrhizal species selectivity of sweet sorghum genotypes and their effect on nutrients uptake

Author: Ibrahim Ortas and Gizem Bilgili
Subjects: sweet sorghum genotypes, mycorrhiza species, mycorrhizal dependency, mineral nutrients, root morphology, Plant culture, SB1-1110
Abstract: This study aimed to find the effects of several mycorrhiza species on agronomic characteristics and nutrient uptake of various sweet sorghum genotypes under the semi-arid Mediterranean soil conditions. Four sweet sorghum genotypes were inoculated with three mycorrhiza species under greenhouse conditions. The plants were evaluated for growth parameters such as shoot height, root length, root morphology (root surface, root diameter and volume), shoot and root dry weight, uptake of macro and micro mineral nutrients, root colonisation and mycorrhizal dependency. Mycorrhizal species significantly improved growth and productivity of sorghum genotypes. Inoculation of Funneliformis mosseae, Claroideoglomus claroideum and Claroideoglomus etunicatum resulted in the highest shoot and total dry matter biomass production in Ashana, Hereahri and Yellow genotypes, respectively. Mycorrhiza inoculated white genotype had higher root colonisation and root development, and shoot P, K, Ca and Mg contents. Yellow genotypes produced significantly higher shoot and total dry weight and also were highly mycorrhiza dependent among the four genotypes. Compared to the control treatment mycorrhizal inoculation increased shoot Zn concentration but had non-consistent effects on shoot Cu, Fe and Mn contents. Conclusively, our findings confirmed that sweet sorghum genotypes responded selectively to arbuscular mycorrhizal fungi (AMF) colonisation for their growth parameters and nutrients uptake.
Published: 2022
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177. Evaluation of the Effects of Varicoceles and Fertility Status on Volumetry and Shear-wave Elastography

Author: Mustafa Özdemir, Ali Koç, Mustafa Bilgili, and Gamze Türk
Subjects: infertilite, varikosel, shear-wave elastografi, testis sertliği, testis hacmi, infertility, varicocele, shear-wave elastography, testis stiffness, testis volume, Medicine (General), R5-920
Abstract: Aim: This study aims to compare the volumetry and shear-wave elastography findings in infertile and fertile patients and evaluate the effect of presence of varicoceles on the parameters. Materials-Methods: 40 infertile and 20 fertile patients (120 testes) (mean age 29,3±6,7) between January 2018-November 2018 were included in this prospective study. All patients underwent testicular B-mode and doppler ultrasonography (US) and shear-wave elastography (SWE). Patients were sub-grouped according to fertility status and presence or absence of varicoceles. Results: Testis stiffness was significantly higher in testes without varicoceles than those with varicoceles (p=0.021). It was also higher in fertile patients than infertile patients (p=0.015). Testes volumes were higher in fertile patients and patients with varicoceles (p=0.011 and p=0.028, respectively). Conclusion: SWE is a non-invasive, cheap and reproducible technique with promising results for diagnosis and follow-up in the evaluation of infertility.
Published: 2022
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178. Exploitable Potential of Biomass Energy in Electrical Energy Production in the Mediterranean Region of Turkey

Author: Mehmet Emin Bilgili
Subjects: renewable energy, agricultural residues, biomass potential, energy substitution, Agriculture (General), S1-972
Abstract: Turkey is targeting to generate 30% of its total electricity production from renewable energy sources by 2023. The replacement of electrical energy in the Mediterranean Region of Turkey according to exploitable biomass data was determined in this study. Data from the Ministry of Energy and Natural Resources, the Ministry of Agriculture and Forestry, Turkish Statistical Institute, measurements and literature were used in the study. The technical potential of plant residues and animal-originated biomass in the region was analyzed. It is estimated that the existing plant and animal residues in Turkey correspond to 39% and 9%, respectively. These residues can meet 6.9% of the energy demand of the region, i.e. about 8.3 PJ/year. Employment can be established from the technologies to be used here. By generating electrical energy from biomass, 2 644 302 tons of CO2/year can be reduced by generating electrical energy from biomass. The amount of biofertilizer that can be obtained after biogas production is 1 184 049 ton/year of biofertilizer can be obtained after biogas production. The calorific values measured to determine the energy values of agricultural residues were found to be between 13.0-20.7 MJ/kg.
Published: 2022
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179. Making Sense of the Performance (Dis)Advantage for Immigrant Students across Canada

Author: Volante, Louis, Klinger, Don, Bilgili, Özge, and Siegel, Melissa
Abstract: International achievement measures such as the Programme for International Student Assessment (PISA) have traditionally reported a significant gap between non-migrant and immigrant student groups--a result that is often referred to as the "immigrant performance disadvantage". This article examines first- and second-generation immigrant student achievement results in greater detail across Canada. Overall, Canadian achievement results are atypical in relation to the international community in that immigrant student groups significantly outperform non-migrants in some provincial jurisdictions, and also significantly underperform in other provincial jurisdictions, in relation to reading, mathematics, and scientific literacy. This article examines these diverse results in relation to the available literature and offers a conceptual framework that explains the unique case of Canada. The framework highlights the importance of assessing immigrant student achievement by taking into account the level of individual characteristics, provincial policies, as well as sociocultural and demographic contexts across Canada.
Published: 2017

180. Investigation of the relationship of groundwater quality and irrigation: the case of Mardin Kiziltepe Plain (Mesopotamia) in Turkey

Author: Yenigun, Ibrahim, Bilgili, Ali Volkan, Senol, Halil Ibrahim, and Yenigun, Abdullah
Published: 2023
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181. Modeling and mapping the spatial variability of soil micronutrients in the Tigris basin

Author: Veysel Gökmen, Abdulkadir Sürücü, Mesut Budak, and Ali Volkan Bilgili
Subjects: Geostatistics, Spatial analysis, Variability, Soil micronutrients, Tigris, Science (General), Q1-390
Abstract: Background: Crop production is negatively impacted by excess and lack of soil micronutrients. Due to anthropogenic and natural factors, soil micronutrients vary greatly in space, necessitating time- and money-consuming large-scale sampling. Therefore, modeling their spatial distributions and forecasting in non-sampled areas are essential for high crop production. Methods: In this study, regional variations in soil micronutrient content of the Upper Tigris Basin were modeled to produce local change maps for the development of site-specific nutrient management systems. The concentrations of extractable zinc (Zn), copper (Cu), manganese (Mn), and iron (Fe) in soil samples taken at 388 different sites between 0 and 20 cm deep were determined. Using variogram and kriging analyses, the spatial distribution of the micro element concentrations was modeled and mapped in a GIS environment. Results: The micronutrients demonstrated significant variability with a high coefficient of variation (CV > 35%). It was found that the spatial dependence of the samples ranged from low for Fe and Cu to high for Zn and Mn. The spatial distribution of soil micronutrients was influenced by soil texture in addition to distance. Overall, the results demonstrated that the management of site-specific micronutrients may be aided by the integration of geostatistics and GIS, which is particularly beneficial in terms of effective management of the lands and the optimal use of inputs. Conclusion: Overall, the findings showed that the integration of geostatistics and GIS may be helpful in the management of site-specific micronutrients, which is especially advantageous in terms of efficient management of the lands and the best use of inputs.
Published: 2023
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182. A Novel PBM for Nanomilling of Drugs in a Recirculating Wet Stirred Media Mill: Impacts of Batch Size, Flow Rate, and Back-Mixing

Author: Hamidreza Heidari, Nontawat Muanpaopong, Gulenay Guner, Helen F. Yao, Donald J. Clancy, and Ecevit Bilgili
Subjects: wet stirred media milling, population balance model, drug nanoparticles, breakage kinetics, process development, imperfect mixing, Pharmacy and materia medica, RS1-441
Abstract: We examined the evolution of fenofibrate (FNB, drug) particle size distribution (PSD) during the production of nanosuspensions via wet stirred media milling (WSMM) with a cell-based population balance model (PBM). Our objective was to elucidate the potential impacts of batch size, suspension volumetric flow rate, and imperfect mixing in a recirculating WSMM. Various specific breakage rate functions were fitted to experimental PSD data at baseline conditions assuming perfect mixing. Then, the best function was used to simulate the PSD evolution at various batch sizes and flow rates to validate the model. A novel function, which is a product of power–law and logistic functions, fitted the evolution the best, signifying the existence of a transition particle size commensurate with a grinding limit. Although larger batches yielded coarser and wider PSDs, the suspensions had identical PSDs when milled for the same effective milling time. The flow rate had an insignificant influence on the PSD. Furthermore, the imperfect mixing in the mill chamber was simulated by considering more than one cell and different back-mixing flow ratios. The effects were weak and restricted to the first few turnovers. These insights contribute to our understanding of recirculating WSMM, providing valuable guidance for process development.
Published: 2024
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183. Development of a Semi-Mechanistic Modeling Framework for Wet Bead Milling of Pharmaceutical Nanosuspensions

Author: Donald J. Clancy, Gulenay Guner, Sayantan Chattoraj, Helen Yao, M. Connor Faith, Zahra Salahshoor, Kailey N. Martin, and Ecevit Bilgili
Subjects: milling, wet bead milling, particle size prediction, modeling, semi-mechanistic modeling, microhydrodynamic model, Pharmacy and materia medica, RS1-441
Abstract: This study aimed to develop a practical semi-mechanistic modeling framework to predict particle size evolution during wet bead milling of pharmaceutical nanosuspensions over a wide range of process conditions and milling scales. The model incorporates process parameters, formulation parameters, and equipment-specific parameters such as rotor speed, bead type, bead size, bead loading, active pharmaceutical ingredient (API) mass, temperature, API loading, maximum bead volume, blade diameter, distance between blade and wall, and an efficiency parameter. The characteristic particle size quantiles, i.e., x10, x50, and x90, were transformed to obtain a linear relationship with time, while the general functional form of the apparent breakage rate constant of this relationship was derived based on three models with different complexity levels. Model A, the most complex and general model, was derived directly from microhydrodynamics. Model B is a simpler model based on a power-law function of process parameters. Model C is the simplest model, which is the pre-calibrated version of Model B based on data collected from different mills across scales, formulations, and drug products. Being simple and computationally convenient, Model C is expected to reduce the amount of experimentation needed to develop and optimize the wet bead milling process and streamline scale-up and/or scale-out.
Published: 2024
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184. A New Risk Scoring System to Predict Malignancy in Gallbladder Polyps: a Single-Center Study

Author: Güneş, Yasin, Taşdelen, İksan, Ergin, Anıl, Çakmak, Ahmet, Bilgili, Ali Cihan, Ağar, Mustafa, and Aydın, Mehmet Timuçin
Published: 2022
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185. An Enthalpy-Balance Model for Timewise Evolution of Temperature during Wet Stirred Media Milling of Drug Suspensions

Author: Guner, Gulenay, Elashri, Sherif, Mehaj, Mirsad, Seetharaman, Natasha, Yao, Helen F., Clancy, Donald J., and Bilgili, Ecevit
Published: 2022
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186. Time-series prediction of hourly atmospheric pressure using ANFIS and LSTM approaches

Author: Bilgili, Mehmet, Ilhan, Akın, and Ünal, Şaban
Published: 2022
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187. Global growth in offshore wind turbine technology

Author: Bilgili, Mehmet and Alphan, Hakan
Published: 2022
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188. Effect of different polishing techniques on surface properties and bacterial adhesion on resin-ceramic CAD/CAM materials

Author: Özarslan, Merve, Bilgili Can, Dilber, Avcioglu, Nermin Hande, and Çalışkan, Seçil
Published: 2022
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189. Estimation of aerodynamic coefficients of a non-slender delta wing under ground effect using artificial intelligence techniques

Author: Tumse, Sergen, Bilgili, Mehmet, and Sahin, Besir
Published: 2022
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190. Searches for Continuous Gravitational Waves from Fifteen Supernova Remnants and Fomalhaut b with Advanced LIGO

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Cannon, K. C., Cao, H., Cao, J., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colgan, R., Colleoni, M., Collette, C. G., Collins, C., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrión, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Croquette, M., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, Dálya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., DeBra, D., Deenadayalan, M., Degallaix, J., De Laurentis, M., Deléglise, S., Del Pozzo, W., DeMarchi, L. M., Demos, N., Dent, T., De Pietri, R., Derby, J., De Rosa, R., De Rossi, C., DeSalvo, R., de Varona, O., Dhurandhar, S., Díaz, M. C., Dietrich, T., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Ding, B., Di Pace, S., Di Palma, I., Di Renzo, F., Dmitriev, A., Doctor, Z., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Downes, T. P., Drago, M., Driggers, J. C., Du, Z., Ducoin, J. -G., Dupej, P., Dwyer, S. E., Easter, P. J., Edo, T. B., Edwards, M. C., Effler, A., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenmann, M., Eisenstein, R. A., Essick, R. C., Estelles, H., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fazio, M., Fee, C., Feicht, J., Fejer, M. M., Feng, F., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferreira, T. A., Ferrini, F., Fidecaro, F., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fishner, J. M., Fitz-Axen, M., Flaminio, R., Fletcher, M., Flynn, E., Fong, H., Font, J. A., Forsyth, P. W. F., Fournier, J. -D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Ganija, M. R., Gaonkar, S. G., Garcia, A., García-Quirós, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Giordano, G., Glover, L., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., González, G., Castro, J. M. Gonzalez, Gopakumar, A., Gorodetsky, M. L., Gossan, S. E., Gosselin, M., Gouaty, R., Grado, A., Graef, C., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Gulati, H. K., Guo, Y., Gupta, A., Gupta, M. K., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannuksela, O. A., Hanson, J., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Haster, C. -J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Vivanco, Francisco Hernandez, Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Hreibi, A., Huerta, E. A., Huet, D., Hughey, B., Hulko, M., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. I., Jones, R., Jonker, R. J. G., Ju, L., Junker, J., Kalaghatgi, C. V., Kalogera, V., Kamai, B., Kandhasamy, S., Kang, G., Kanner, J. B., Kapadia, S. J., Karki, S., Karvinen, K. S., Kashyap, R., Kasprzack, M., Katsanevas, S., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Keerthana, N. V., Kéfélian, F., Keitel, D., Kennedy, R., Key, J. S., Khalili, F. Y., Khan, H., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Khursheed, M., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y. -M., Kimball, C., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klika, J. H., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koekoek, G., Koley, S., Kondrashov, V., Kontos, A., Koper, N., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Kringel, V., Krishnendu, N., Królak, A., Kuehn, G., Kumar, A., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Lam, T. L., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Lenon, A., Leroy, N., Letendre, N., Levin, Y., Li, J., Li, K. J. L., Li, T. G. F., Li, X., Lin, F., Linde, F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lower, M. E., Lück, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., MacInnis, M., Macleod, D. M., Macquet, A., Magaña-Sandoval, F., Zertuche, L. Magaña, Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martynov, D. V., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Matone, L., Mavalvala, N., Mazumder, N., McCann, J. J., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIver, J., McManus, D. J., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Meidam, J., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merilh, E. L., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Miao, H., Michel, C., Middleton, H., Mikhailov, E. E., Milano, L., Miller, A. L., Miller, A., Millhouse, M., Mills, J. C., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Moffa, D., Mogushi, K., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Muratore, M., Murray, P. G., Nagar, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, P., Nichols, D., Nissanke, S., Nocera, F., North, C., Nuttall, L. K., Obergaulinger, M., Oberling, J., O'Brien, B. D., O'Dea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., O'Reilly, B., Ormiston, R. G., Ortega, L. F., O'Shaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedersen, C., Pedraza, M., Pedurand, R., Pele, A., Penn, S., Perez, C. J., Perreca, A., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pillant, G., Pinard, L., Pirello, M., Pitkin, M., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasad, J., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Quintero, E. A., Quitzow-James, R., Raab, F. J., Radkins, H., Radulescu, N., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romie, J. H., Rose, K., Rosińska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rüdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salconi, L., Saleem, M., Samajdar, A., Sammut, L., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Santiago, K. A., Sarin, N., Sassolas, B., Saulson, P. R., Sauter, O., Savage, R. L., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. 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E., and Zweizig, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract: We describe directed searches for continuous gravitational waves from sixteen well localized candidate neutron stars assuming none of the stars has a binary companion. The searches were directed toward fifteen supernova remnants and Fomalhaut~b, an extrasolar planet candidate which 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 gravitational wave strain as strict as $1\times10^{-25}$, on fiducial neutron star ellipticity as strict as $2\times10^{-9}$, and on fiducial $r$-mode amplitude as strict as $3\times10^{-8}$., Comment: 21 pages, 22 figures, updated following erratum
Published: 2018
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191. GWTC-1: A Gravitational-Wave Transient Catalog of Compact Binary Mergers Observed by LIGO and Virgo during the First and Second Observing Runs

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology
Abstract: We present the results from three gravitational-wave searches for coalescing compact binaries with component masses above 1$\mathrm{M}_\odot$ during the first and second observing runs of the Advanced gravitational-wave detector network. During the first observing run (O1), from September $12^\mathrm{th}$, 2015 to January $19^\mathrm{th}$, 2016, gravitational waves from three binary black hole mergers were detected. The second observing run (O2), which ran from November $30^\mathrm{th}$, 2016 to August $25^\mathrm{th}$, 2017, saw the first detection of gravitational waves from a binary neutron star inspiral, in addition to the observation of gravitational waves from a total of seven binary black hole mergers, four of which we report here for the first time: GW170729, GW170809, GW170818 and GW170823. For all significant gravitational-wave events, we provide estimates of the source properties. The detected binary black holes have total masses between $18.6_{-0.7}^{+3.2}\mathrm{M}_\odot$, and $84.4_{-11.1}^{+15.8} \mathrm{M}_\odot$, and range in distance between $320_{-110}^{+120}$ Mpc and $2840_{-1360}^{+1400}$ Mpc. No neutron star - black hole mergers were detected. In addition to highly significant gravitational-wave events, we also provide a list of marginal event candidates with an estimated false alarm rate less than 1 per 30 days. From these results over the first two observing runs, which include approximately one gravitational-wave detection per 15 days of data searched, we infer merger rates at the 90% confidence intervals of $110\, -\, 3840$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$ for binary neutron stars and $9.7\, -\, 101$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$ for binary black holes assuming fixed population distributions, and determine a neutron star - black hole merger rate 90% upper limit of $610$ $\mathrm{Gpc}^{-3}\,\mathrm{y}^{-1}$., Comment: Total: 49 pages and 17 figures. Strain data are available from the Gravitational Wave Open Science Center at https://doi.org/10.7935/82H3-HH23. Figures, data behind the figures, including posterior samples, are available from https://dcc.ligo.org/LIGO-P1800307/public
Published: 2018
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192. Binary Black Hole Population Properties Inferred from the First and Second Observing Runs of Advanced LIGO and Advanced Virgo

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., AultONeal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Briggs, J. 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W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Yvert, M., Zadrożny, A. K., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A. B., Zlochower, Y., Zucker, M. E., and Zweizig, J.
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present results on the mass, spin, and redshift distributions with phenomenological population models using the ten binary black hole mergers detected in the first and second observing runs completed by Advanced LIGO and Advanced Virgo. We constrain properties of the binary black hole (BBH) mass spectrum using models with a range of parameterizations of the BBH mass and spin distributions. We find that the mass distribution of the more massive black hole in such binaries is well approximated by models with no more than 1% of black holes more massive than $45\,M_\odot$, and a power law index of $\alpha = {1.3}^{+1.4}_{-1.7}$ (90% credibility). We also show that BBHs are unlikely to be composed of black holes with large spins aligned to the orbital angular momentum. Modelling the evolution of the BBH merger rate with redshift, we show that it is at or increasing with redshift with 93% probability. Marginalizing over uncertainties in the BBH population, we find robust estimates of the BBH merger rate density of $R = {53.2}^{+55.8}_{-28.2}$ Gpc$^{-3}$ yr$^{-1}$ (90% credibility). As the BBH catalog grows in future observing runs, we expect that uncertainties in the population model parameters will shrink, potentially providing insights into the formation of black holes via supernovae, binary interactions of massive stars, stellar cluster dynamics, and the formation history of black holes across cosmic time., Comment: Accepted Manuscript, with content equivalent to the published version
Published: 2018
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193. Tests of General Relativity with GW170817

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calderón, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavaglià, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerdá-Durán, P., Cerretani, G., Cesarini, E., Chaibi, O., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Chia, H. Y., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. 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Subjects: General Relativity and Quantum Cosmology
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 presence of matter. In this paper, 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., Comment: 15 pages, 4 figures. Matches journal submission
Published: 2018
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194. Search for Multi-messenger Sources of Gravitational Waves and High-energy Neutrinos with Advanced LIGO during its first Observing Run, ANTARES and IceCube

Author: ANTARES, IceCube, LIGO, Collaborations, Virgo, Albert, A., Andre, M., Anghinolfi, M., Ardid, M., Aubert, J. -J., Aublin, J., Avgitas, T., Baret, B., Barrios-Marti, J., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bormuth, R., Boumaaza, J., Bourret, S., Bouwhuis, M. C., Brânzas, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chabab, M., Moursli, R. Cherkaoui El, Chiarusi, T., Circella, M., Coelho, J. A. B., Coleiro, A., Colomer, M., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Diaz, A. F., Deschamps, A., Distefano, C., Di Palma, I., Domi, A., Dona, R., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., Bojaddaini, I. El, Khayati, N. El, Elsasser, D., Enzenhofer, A., Ettahiri, A., Fassi, F., Felis, I., Fermani, P., Ferrara, G., Fusco, L., Gay, P., Glotin, H., Gregoire, T., Ruiz, R. Gracia, Graf, K., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernandez-Rey, J. J., Hol, J., Hofestadt, J., Illuminati, G., de Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Khan-Chowdhury, N. R., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefevre, D., Leonora, E., Levi, G., Lotze, M., Loucatos, S., Maggi, G., Marcelin, M., Margiotta, A., Marinelli, A., Martinez-Mora, J. A., Mele, R., Melis, K., Migliozzi, P., Moussa, A., Navas, S., Nezri, E., Nunez, A., Organokov, M., Pavalas, G. E., Pellegrino, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Randazzo, N., Riccobene, G., Sanchez-Losa, A., Saldana, M., Salvadori, I., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schussler, F., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Vallage, B., Van Elewyck, V., Versari, F., Vivolo, D., Wilms, J., Zaborov, D., Zornoza, J. D., Zuniga, J., Aartsen, M. G., Ackermann, M., Adams, J., Aguilar, J. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: 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 origin 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., Comment: 20 pages, 2 figures
Published: 2018
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195. Search for gravitational waves from a long-lived remnant of the binary neutron star merger GW170817

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. 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Subjects: General Relativity and Quantum Cosmology, Astrophysics - High Energy Astrophysical Phenomena
Abstract: 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 with a focus on longer signal durations up until the end of the Second Advanced LIGO-Virgo Observing run, 8.5 days after the coalescence of GW170817. The main physical scenario for such 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 waveformand 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. This study however serves as a prototype for post-merger analyses in future observing runs with expected higher sensitivity., Comment: main paper: 9 pages and 3 figures; total with appendices: 24 pages and 9 figures. Full UL tables available as MRT ancillary files
Published: 2018
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196. A Fermi Gamma-ray Burst Monitor Search for Electromagnetic Signals Coincident with Gravitational-Wave Candidates in Advanced LIGO's First Observing Run

Author: Team, The Fermi Gamma-ray Burst Monitor, Collaboration, The LIGO Scientific, Collaboration, the Virgo, Burns, E., Goldstein, A., Hui, C. M., Blackburn, L., Briggs, M. S., Connaughton, V., Hamburg, R., Kocevski, D., Veres, P., Wilson-Hodge, C. A., Bissaldi, E., Cleveland, W. H., Giles, M. M., Mailyan, B., Meegan, C. A., Paciesas, W. A., Poolakkil, S., Preece, R. D., Racusin, J. L., Roberts, O. J., von Kienlin, A., Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Ar`ene, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., B'ecsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We present a search for prompt gamma-ray counterparts to compact binary coalescence gravitational wave (GW) candidates from Advanced LIGO's first observing run (O1). As demonstrated by the multimessenger observations of GW170817/GRB 170817A, electromagnetic and GW observations provide complementary information about the astrophysical source and, in the case of weaker candidates, may strengthen the case for an astrophysical origin. Here we investigate low-significance GW candidates from the O1 compact-binary coalescence searches using the Fermi Gamma-ray Burst Monitor (GBM), leveraging its all-sky and broad energy coverage. Candidates are ranked and compared to background to measure significance. Those with false alarm rates of less than 10^-5 Hz (about one per day) are used as the search sample for gamma-ray follow-up. No GW candidates were found to be coincident with gamma-ray transients independently identified by blind searches of the GBM data. In addition, GW candidate event times were followed up by a separate targeted search of GBM data. Among the resulting GBM events, the two with lowest false alarm rates were the gamma-ray transient GW150914-GBM presented in Connaughton et al. (2016) and a solar flare in chance coincidence with a GW candidate., Comment: Published in ApJ
Published: 2018
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197. Constraining the p-mode--g-mode tidal instability with GW170817

Author: The LIGO Scientific Collaboration, The Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Arène, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., Bécsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. 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Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: We analyze the impact of a proposed tidal instability coupling $p$-modes and $g$-modes within neutron stars on GW170817. This non-resonant instability transfers energy from the orbit of the binary to internal modes of the stars, accelerating the gravitational-wave driven inspiral. We model the impact of this instability on the phasing of the gravitational wave signal using three parameters per star: an overall amplitude, a saturation frequency, and a spectral index. Incorporating these additional parameters, we compute the Bayes Factor ($\ln B^{pg}_{!pg}$) comparing our $p$-$g$ model to a standard one. We find that the observed signal is consistent with waveform models that neglect $p$-$g$ effects, with $\ln B^{pg}_{!pg} = 0.03^{+0.70}_{-0.58}$ (maximum a posteriori and 90% credible region). By injecting simulated signals that do not include $p$-$g$ effects and recovering them with the $p$-$g$ model, we show that there is a $\simeq 50\%$ probability of obtaining similar $\ln B^{pg}_{!pg}$ even when $p$-$g$ effects are absent. We find that the $p$-$g$ amplitude for 1.4 $M_\odot$ neutron stars is constrained to $\lesssim \text{few}\times10^{-7}$, with maxima a posteriori near $\sim 10^{-7}$ and $p$-$g$ saturation frequency $\sim 70\, \mathrm{Hz}$. This suggests that there are less than a few hundred excited modes, assuming they all saturate by wave breaking. For comparison, theoretical upper bounds suggest a $p$-$g$ amplitude $\lesssim 10^{-6}$ and $\lesssim 10^{3}$ modes saturating by wave breaking. Thus, the measured constraints only rule out extreme values of the $p$-$g$ parameters. They also imply that the instability dissipates $\lesssim 10^{51}\, \mathrm{ergs}$ over the entire inspiral, i.e., less than a few percent of the energy radiated as gravitational waves., Comment: 7 pages, 2 figures
Published: 2018
Full Text: View/download PDF

198. Search for sub-solar mass ultracompact binaries in Advanced LIGO's first observing run

Author: Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Ar`ene, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., B'ecsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buchanan, C. 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A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colla, A., Collette, C. G., Collins, C., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carri'on, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, D'alya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. 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J., Yazback, M., Yu, Hang, Yu, Haocun, Yvert, M., zny, A. Zadro., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, M., Zhang, T., Zhang, Y. -H., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. J., Zhu, X. J., Zucker, M. E., Zweizig, J., and Shandera, S.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics, General Relativity and Quantum Cosmology
Abstract: We present the first Advanced LIGO and Advanced Virgo search for ultracompact binary systems with component masses between 0.2 $M_\odot$ - 1.0 $M_\odot$ using data taken between September 12, 2015 and January 19, 2016. We find no viable gravitational wave candidates. Our null result constrains the coalescence rate of monochromatic (delta function) distributions of non-spinning (0.2 $M_\odot$, 0.2 $M_\odot$) ultracompact binaries to be less than $1.0 \times 10^6 \text{Gpc}^{-3} \text{yr}^{-1}$ and the coalescence rate of a similar distribution of (1.0 $M_\odot$, 1.0 $M_\odot$) ultracompact binaries to be less than $1.9 \times 10^4 \text{Gpc}^{-3} \text{yr}^{-1}$ (at 90 percent confidence). Neither black holes nor neutron stars are expected to form below ~ 1 solar mass through conventional stellar evolution, though it has been proposed that similarly low mass black holes could be formed primordially through density fluctuations in the early universe. Under a particular primordial black hole binary formation scenario, we constrain monochromatic primordial black hole populations of 0.2 $M_\odot$ to be less than $33\%$ of the total dark matter density and monochromatic populations of 1.0 $M_\odot$ to be less than $5\%$ of the dark matter density. The latter strengthens the presently placed bounds from micro-lensing surveys of MAssive Compact Halo Objects (MACHOs) provided by the MACHO and EROS collaborations., Comment: 12 pages, 3 figures
Published: 2018
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199. GW170817: Measurements of Neutron Star Radii and Equation of State

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Ar`ene, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., B'ecsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calder'on, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavagli`a, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerd'a-Dur'an, P., Cerretani, G., Cesarini, E., Chaibi, O., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Chia, H. Y., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. K., Chua, S., Chung, K. W., Chung, S., Ciani, G., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirelli, C. E., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Cocchieri, C., Coccia, E., Cohadon, P. -F., Cohen, D., Colla, A., Collette, C. G., Collins, C., Cominsky, L. R., Constancio Jr., M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carri'on, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Cotesta, R., Coughlin, M. W., Coughlin, S. B., Coulon, J. -P., Countryman, S. T., Couvares, P., Covas, P. B., Cowan, E. E., Coward, D. M., Cowart, M. J., Coyne, D. C., Coyne, R., Creighton, J. D. E., Creighton, T. D., Cripe, J., Crowder, S. G., Cullen, T. J., Cumming, A., Cunningham, L., Cuoco, E., Canton, T. Dal, D'alya, G., Danilishin, S. L., D'Antonio, S., Danzmann, K., Dasgupta, A., Costa, C. F. Da Silva, Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. 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Subjects: General Relativity and Quantum Cosmology, Astrophysics - High Energy Astrophysical Phenomena
Abstract: On 17 August 2017, the LIGO and Virgo observatories made the first direct detection of gravitational waves from the coalescence of a neutron star binary system. The detection of this gravitational-wave signal, GW170817, offers a novel opportunity to directly probe the properties of matter at the extreme conditions found in the interior of these stars. The initial, minimal-assumption analysis of the LIGO and Virgo data placed constraints on the tidal effects of the coalescing bodies, which were then translated to constraints on neutron star radii. Here, we expand upon previous analyses by working under the hypothesis that both bodies were neutron stars that are described by the same equation of state and have spins within the range observed in Galactic binary neutron stars. Our analysis employs two methods: the use of equation-of-state-insensitive relations between various macroscopic properties of the neutron stars and the use of an efficient parametrization of the defining function $p(\rho)$ of the equation of state itself. From the LIGO and Virgo data alone and the first method, we measure the two neutron star radii as $R_1=10.8^{+2.0}_{-1.7}$ km for the heavier star and $R_2= 10.7^{+2.1}_{-1.5}$ km for the lighter star at the 90% credible level. If we additionally require that the equation of state supports neutron stars with masses larger than $1.97 \,M_\odot$ as required from electromagnetic observations and employ the equation-of-state parametrization, we further constrain $R_1= 11.9^{+1.4}_{-1.4}$ km and $R_2= 11.9^{+1.4}_{-1.4}$ km at the 90% credible level. Finally, we obtain constraints on $p(\rho)$ at supranuclear densities, with pressure at twice nuclear saturation density measured at $3.5^{+2.7}_{-1.7}\times 10^{34} \,\mathrm{dyn}/\mathrm{cm}^{2}$ at the 90% level., Comment: 10 pages, 3 figures; v2 matches published version; data associated with the figures can be found at https://dcc.ligo.org/LIGO-P1800115/public
Published: 2018
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200. Properties of the binary neutron star merger GW170817

Author: The LIGO Scientific Collaboration, the Virgo Collaboration, Abbott, B. P., Abbott, R., Abbott, T. D., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Affeldt, C., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Ar`ene, M., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aubin, F., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Banagiri, S., Barayoga, J. C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Batch, J. C., Bawaj, M., Bayley, J. C., Bazzan, M., B'ecsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Bensch, M., Berger, B. K., Bergmann, G., Bernuzzi, S., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bock, O., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Booker, P., Boom, B. A., Booth, C. D., Bork, R., Boschi, V., Bose, S., Bossie, K., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Briant, T., Brighenti, F., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Brooks, A. F., Brown, D. D., Brunett, S., Buchanan, C. C., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. Calder'on, Callister, T. A., Calloni, E., Camp, J. B., Canepa, M., Canizares, P., Cannon, K. C., Cao, H., Cao, J., Capano, C. D., Capocasa, E., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavagli`a, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerd'a-Dur'an, P., Cerretani, G., Cesarini, E., Chaibi, O., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E., Chassande-Mottin, E., Chatterjee, D., Chatziioannou, K., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Chia, H. Y., Chincarini, A., Chiummo, A., Chmiel, T., Cho, H. S., Cho, M., Chow, J. H., Christensen, N., Chu, Q., Chua, A. J. 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A., Vardaro, M., Varma, V., Vass, S., Vas'uth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Vicer'e, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, L., Walsh, S., Wang, G., Wang, H., Wang, J. Z., Wang, W. H., Wang, Y. F., Ward, R. L., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Wessel, E. K., Wessels, P., Westerweck, J., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D., Williams, D., Williams, R. D., Williamson, A. R., Willis, J. L., Willke, B., Wimmer, M. H., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Wong, W. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, S., Yam, W., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yu, Hang, Yu, Haocun, Yvert, M., zny, A. Zadro., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, M., Zhang, T., Zhang, Y. -H., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. J., Zhu, X. J., Zimmerman, A. B., Zlochower, Y., Zucker, M. E., and Zweizig, J.
Subjects: General Relativity and Quantum Cosmology, Astrophysics - High Energy Astrophysical Phenomena
Abstract: On August 17, 2017, the Advanced LIGO and Advanced Virgo gravitational-wave detectors observed a low-mass compact binary inspiral. The initial sky localization of the source of the gravitational-wave signal, GW170817, allowed electromagnetic observatories to identify NGC 4993 as the host galaxy. In this work, we improve initial estimates of the binary's properties, including component masses, spins, and tidal parameters, using the known source location, improved modeling, and recalibrated Virgo data. We extend the range of gravitational-wave frequencies considered down to 23 Hz, compared to 30 Hz in the initial analysis. We also compare results inferred using several signal models, which are more accurate and incorporate additional physical effects as compared to the initial analysis. We improve the localization of the gravitational-wave source to a 90% credible region of $16~\mathrm{deg}^2$. We find tighter constraints on the masses, spins, and tidal parameters, and continue to find no evidence for nonzero component spins. The component masses are inferred to lie between 1.00 and 1.89 $M_\odot$ when allowing for large component spins, and to lie between 1.16 and 1.60 $M_\odot$ (with a total mass $2.73^{+0.04}_{-0.01} \, M_\odot$) when the spins are restricted to be within the range observed in Galactic binary neutron stars. Under minimal assumptions about the nature of the compact objects, our constraints for the tidal deformability parameter $\tilde \Lambda$ are $(0,630)$ when we allow for large component spins, and $300^{+420}_{-230}$ (using a 90% highest posterior density interval) when restricting the magnitude of the component spins, ruling out several equation-of-state models at the 90% credible level. Finally, with LIGO and GEO600 data, we use a Bayesian analysis to place upper limits on the amplitude and spectral energy density of a possible post-merger signal. (Abridged), Comment: 32 pages, 15 figures. Version 3 is the final published version; results are unchanged compared to previous versions. Data behind the figures, including posterior samples, are available at dcc.ligo.org/LIGO-P1800061/public. The gravitational wave strain data for this event are available at the LIGO Open Science Center, gw-openscience.org/events/GW170817
Published: 2018
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