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5. Crowdsourcing quality control for Dark Energy Survey images

Author

Melchior, P., Sheldon, E., Drlica-Wagner, A., Rykoff, E.S., Abbott, T.M.C., Abdalla, F.B., Allam, S., Benoit-Lévy, A., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Crocce, M., D’Andrea, C.B., da Costa, L.N., Desai, S., Doel, P., Evrard, A.E., Finley, D.A., Flaugher, B., Frieman, J., Gaztanaga, E., Gerdes, D.W., Gruen, D., Gruendl, R.A., Honscheid, K., James, D.J., Jarvis, M., Kuehn, K., Li, T.S., Maia, M.A.G., March, M., Marshall, J.L., Nord, B., Ogando, R., Plazas, A.A., Romer, A.K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, R.C., Soares-Santos, M., Suchyta, E., Swanson, M.E.C., Tarle, G., Vikram, V., Walker, A.R., Wester, W., and Zhang, Y.

Published
2016
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8. A gravitational-wave standard siren measurement of the Hubble constant

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., Afrough, M., Agarwal, B., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, B., Allen, G., Allocca, 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., Arnaud, N., Arun, K. G., Ascenzi, S., Ashton, G., Ast, M., Aston, S. M., Astone, P., Atallah, D. V., Aufmuth, P., Aulbert, C., AultONeal, K., Austin, C., Avila-Alvarez, A., Babak, S., Bacon, P., 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., 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., Bcsy, B., Beer, C., Bejger, M., Belahcene, I., Bell, A. S., Berger, B. K., Bergmann, G., Bero, J. J., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhagwat, S., Bhandare, R., Bilenko, I. A., Billingsley, G., Billman, C. R., Birch, J., Birney, R., Birnholtz, O., Biscans, S., Biscoveanu, S., Bisht, A., Bitossi, M., Biwer, C., 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., Bogaert, G., Bohe, A., Bondu, F., Bonilla, E., Bonnand, R., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossie, K., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Branchesi, M., Brau, J. E., Briant, T., Brillet, A., Brinkmann, M., Brisson, V., Brockill, P., Broida, J. E., Brooks, A. F., Brown, D. A., 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. Caldern, 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., Diaz, J. Casanueva, Casentini, C., Caudill, S., Cavagli, M., Cavalier, F., Cavalieri, R., Cella, G., Cepeda, C. B., Cerd-Durn, P., Cerretani, G., Cesarini, E., 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., 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, A. K. W., Chung, S., Ciani, G., Ciolfi, R., 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., Cominsky, L. R., Constancio, M., Jr., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrin, I., Corley, K. R., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., 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., Dal Canton, T., Dlya, G., Danilishin, S. L., DAntonio, S., Danzmann, K., Dasgupta, A., Da Silva Costa, C. F., Datrier, L. E. H., Dattilo, V., Dave, I., Davier, M., Davis, D., Daw, E. J., Day, B., De, S., DeBra, D., Degallaix, J., De Laurentis, M., Delglise, S., Del Pozzo, W., Demos, N., Denker, T., Dent, T., De Pietri, R., Dergachev, V., De Rosa, R., DeRosa, R. T., De Rossi, C., DeSalvo, R., de Varona, O., Devenson, J., Dhurandhar, S., Daz, M. C., Di Fiore, L., Di Giovanni, M., Di Girolamo, T., Di Lieto, A., Di Pace, S., Di Palma, I., Di Renzo, F., Doctor, Z., Dolique, V., Donovan, F., Dooley, K. L., Doravari, S., Dorrington, I., Douglas, R., Dovale lvarez, M., Downes, T. P., Drago, M., Dreissigacker, C., Driggers, J. C., Du, Z., Ducrot, M., Dupej, P., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Eggenstein, H.-B., Ehrens, P., Eichholz, J., Eikenberry, S. S., Eisenstein, R. A., Essick, R. C., Estevez, D., Etienne, Z. B., Etzel, T., Evans, M., Evans, T. M., Factourovich, M., Fafone, V., Fair, H., Fairhurst, S., Fan, X., Farinon, S., Farr, B., Farr, W. M., Fauchon-Jones, E. J., Favata, M., Fays, M., Fee, C., Fehrmann, H., Feicht, J., Fejer, M. M., Fernandez-Galiana, A., Ferrante, I., Ferreira, E. C., Ferrini, F., Fidecaro, F., Finstad, D., Fiori, I., Fiorucci, D., Fishbach, M., Fisher, R. P., Fitz-Axen, M., Flaminio, R., Fletcher, M., Fong, H., Font, J. A., Forsyth, P. W. F., Forsyth, S. S., Fournier, J.-D., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fries, E. M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H., 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., Gehrels, N., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Germain, V., Ghonge, S., Ghosh, Abhirup, Ghosh, Archisman, Ghosh, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Glover, L., Goetz, E., Goetz, R., Gomes, S., Goncharov, B., Gonzlez, 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., Gray, C., Greco, G., Green, A. C., Gretarsson, E. M., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Guo, X., Gupta, A., Gupta, M. K., Gushwa, K. E., Gustafson, E. K., Gustafson, R., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hanson, J., Hardwick, T., Harms, J., Harry, G. M., Harry, I. W., Hart, M. J., Haster, C.-J., Haughian, K., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heptonstall, A. W., Heurs, M., Hild, S., Hinderer, T., Hoak, D., Hofman, D., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Houston, E. A., Howell, E. J., Hreibi, A., Hu, Y. M., Huerta, E. A., Huet, D., Hughey, B., Husa, S., Huttner, S. H., Huynh-Dinh, T., Indik, N., Inta, R., Intini, G., Isa, H. N., Isac, J.-M., Isi, M., Iyer, B. R., Izumi, K., Jacqmin, T., Jani, K., Jaranowski, P., Jawahar, S., Jimnez-Forteza, F., Johnson, W. 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., Kasprzack, M., Katolik, M., Katsavounidis, E., Katzman, W., Kaufer, S., Kawabe, K., Kflian, F., Keitel, D., Kemball, A. J., Kennedy, R., Kent, C., Key, J. S., Khalili, F. Y., Khan, I., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Kim, Chunglee, Kim, J. C., Kim, K., Kim, W., Kim, W. S., Kim, Y.-M., Kimbrell, S. J., King, E. J., King, P. J., Kinley-Hanlon, M., Kirchhoff, R., Kissel, J. S., Kleybolte, L., Klimenko, S., Knowles, T. D., Koch, P., Koehlenbeck, S. M., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Kowalska, I., Kozak, D. B., Krmer, C., Kringel, V., Krishnan, B., Krlak, A., Kuehn, G., Kumar, P., Kumar, R., Kumar, S., Kuo, L., Kutynia, A., Kwang, S., Lackey, B. D., Lai, K. H., Landry, M., 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., Lee, C. H., Lee, H. K., Lee, H. M., Lee, H. W., Lee, K., Lehmann, J., Lenon, A., Leonardi, M., Leroy, N., Letendre, N., Levin, Y., Li, T. G. F., Linker, S. D., Littenberg, T. B., Liu, J., Liu, X., Lo, R. K. L., Lockerbie, N. A., London, L. T., Lord, J. E., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lck, H., Lumaca, D., Lundgren, A. P., Lynch, R., Ma, Y., Macas, R., Macfoy, S., Machenschalk, B., MacInnis, M., Macleod, D. M., Hernandez, I. Magaa, Magaa-Sandoval, F., Zertuche, L. Magaa, Magee, R. M., Majorana, E., Maksimovic, I., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Marchesoni, F., Marion, F., Mrka, S., Mrka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Martelli, F., Martellini, L., 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., McCarthy, R., McClelland, D. E., McCormick, S., McCuller, L., McGuire, S. C., McIntyre, G., McIver, J., McManus, D. J., McNeill, L., McRae, T., McWilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Meidam, J., Mejuto-Villa, E., Melatos, A., Mendell, G., Mercer, R. A., 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, B. B., Miller, J., Millhouse, M., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Ming, J., Mishra, C., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Moffa, D., Moggi, A., Mogushi, K., Mohan, M., Mohapatra, S. R. P., Montani, M., Moore, C. J., Moraru, D., Moreno, G., Morriss, S. R., Mours, B., Mow-Lowry, C. M., Mueller, G., Muir, A. W., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukund, N., Mullavey, A., Munch, J., Muiz, E. A., Muratore, M., Murray, P. G., Napier, K., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Nevin, L., Newport, J. M., Newton, G., Ng, K. K. Y., Nguyen, T. T., Nichols, D., Nielsen, A. B., Nissanke, S., Nitz, A., Noack, A., Nocera, F., Nolting, D., North, C., Nuttall, L. K., Oberling, J., ODea, G. D., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Okada, M. A., Oliver, M., Oppermann, P., Oram, Richard J., OReilly, B., Ormiston, R., Ortega, L. F., OShaughnessy, R., Ossokine, S., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Page, J., Page, M. A., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pal-Singh, A., Pan, Howard, Pan, Huang-Wei, Pang, B., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Papa, M. A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patil, M., Patricelli, B., Pearlstone, B. L., Pedraza, M., Pedurand, R., Pekowsky, L., Pele, A., Penn, S., Perez, C. J., Perreca, A., Perri, L. M., Pfeiffer, H. P., Phelps, M., Piccinni, O. J., Pichot, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Pirello, M., Pitkin, M., Poe, M., Poggiani, R., Popolizio, P., Porter, E. K., Post, A., Powell, J., Prasad, J., Pratt, J. W. W., Pratten, G., Predoi, V., Prestegard, T., Prijatelj, M., Principe, M., Privitera, S., Prodi, G. A., Prokhorov, L. G., Puncken, O., Punturo, M., Puppo, P., Prrer, M., Qi, H., Quetschke, V., Quintero, E. A., Quitzow-James, R., Raab, F. J., Rabeling, D. S., Radkins, H., Raffai, P., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Ren, W., Reyes, S. D., Ricci, F., Ricker, P. M., Rieger, S., Riles, K., Rizzo, M., Robertson, N. A., Robie, R., Robinet, F., Rocchi, A., Rolland, L., Rollins, J. G., Roma, V. J., Romano, J. D., Romano, R., Romel, C. L., Romie, J. H., Rosiska, D., Ross, M. P., Rowan, S., Rdiger, A., Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sadeghian, L., Sakellariadou, M., Salconi, L., Saleem, M., Salemi, F., Samajdar, A., Sammut, L., Sampson, L. M., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sandberg, V., Sanders, J. R., Sassolas, B., Sathyaprakash, B. S., Saulson, P. R., Sauter, O., Savage, R. L., Sawadsky, A., Schale, P., Scheel, M., Scheuer, J., Schmidt, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schnbeck, A., Schreiber, E., Schuette, D., Schulte, B. W., Schutz, B. F., Schwalbe, S. G., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sentenac, D., Sequino, V., Sergeev, A., Shaddock, D. A., Shaffer, T. J., Shah, A. A., Shahriar, M. S., Shaner, M. B., Shao, L., Shapiro, B., Shawhan, P., Sheperd, A., Shoemaker, D. H., Shoemaker, D. M., Siellez, K., Siemens, X., Sieniawska, M., Sigg, D., Silva, A. D., Singer, L. P., Singh, A., Singhal, A., Sintes, A. M., Slagmolen, B. J. J., Smith, B., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Sonnenberg, J. A., Sorazu, B., Sorrentino, F., Souradeep, T., Spencer, A. P., Srivastava, A. K., Staats, K., Staley, A., Steer, D., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S. P., Stone, R., Stops, D. J., Strain, K. A., Stratta, G., Strigin, S. E., Strunk, A., Sturani, R., Stuver, A. L., Summerscales, T. Z., Sun, L., Sunil, S., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepaczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Talukder, D., Tanner, D. B., Tpai, M., Taracchini, A., Tasson, J. D., Taylor, J. A., Taylor, R., Tewari, S. V., Theeg, T., Thies, F., Thomas, E. G., Thomas, M., Thomas, P., Thorne, K. A., Thrane, E., Tiwari, S., Tiwari, V., Tokmakov, K. V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forn, A., Torrie, C. I., Tyr, D., Travasso, F., Traylor, G., Trinastic, J., Tringali, M. C., Trozzo, L., 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., van den Brand, J. F. J., Van Den Broeck, C., Vander-Hyde, D. C., van der Schaaf, L., van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Vetrano, F., Vicer, 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., Wen, L., Wessel, E. K., Weels, P., Westerweck, J., Westphal, T., Wette, K., Whelan, J. T., Whitcomb, S. E., 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., Wong, K. W. K., Worden, J., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, S., Yamamoto, H., Yancey, C. C., Yang, L., Yap, M. J., Yazback, M., Yu, Hang, Yu, Haocun, Yvert, M., Zadrony, A., Zanolin, M., Zelenova, T., Zendri, J.-P., Zevin, M., Zhang, L., Zhang, M., Zhang, T., Zhang, Y.-H., Zhao, C., Zhou, M., Zhou, Z., Zhu, S. J., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., Zweizig, J., Foley, R. J., Coulter, D. A., Drout, M. R., Kasen, D., Kilpatrick, C. D., Madore, B. F., Murguia-Berthier, A., Pan, Y.-C., Piro, A. L., Prochaska, J. X., Ramirez-Ruiz, E., Rest, A., Rojas-Bravo, C., Shappee, B. J., Siebert, M. R., Simon, J. D., Ulloa, N., Annis, J., Soares-Santos, M., Brout, D., Scolnic, D., Diehl, H. T., Frieman, J., Berger, E., Alexander, K. D., Allam, S., Balbinot, E., Blanchard, P., Butler, R. E., Chornock, R., Cook, E. R., Cowperthwaite, P., Drlica-Wagner, A., Durret, F., Eftekhari, T., Finley, D. A., Fong, W., Fryer, C. L., Garca-Bellido, J., Gill, M. S. S., Gruendl, R. A., Hartley, W., Herner, K., Huterer, D., Kessler, R., Li, T. S., Lin, H., Lopes, P. A. A., Loureno, A. C. C., Margutti, R., Marriner, J., Marshall, J. L., Matheson, T., Medina, G. E., Metzger, B. D., Muoz, R. R., Muir, J., Nicholl, M., Nugent, P., Palmese, A., Paz-Chinchn, F., Quataert, E., Sako, M., Sauseda, M., Schlegel, D. J., Secco, L. F., Smith, N., Sobreira, F., Stebbins, A., Villar, V. A., Vivas, A. K., Wester, W., Williams, P. K. G., Yanny, B., Zenteno, A., Abbott, T. M. C., Abdalla, F. B., Bechtol, K., Benoit-Lvy, A., Bertin, E., Bridle, S. L., Brooks, D., Buckley-Geer, E., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., DAndrea, C. B., da Costa, L. N., Davis, C., DePoy, D. L., Desai, S., Dietrich, J. P., Estrada, J., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gutierrez, G., Hartley, W. G., Honscheid, K., Jain, B., James, D. J., Jeltema, T., Johnson, M. W. G., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lahav, O., Lima, M., Maia, M. A. G., March, M., Miller, C. J., Miquel, R., Neilsen, E., Nord, B., Ogando, R. L. C., Plazas, A. A., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R. C., Suchyta, E., Tarle, G., Thomas, D., Thomas, R. C., Troxel, M. A., Tucker, D. L., Vikram, V., Walker, A. R., Weller, J., Zhang, Y., Haislip, J. B., Kouprianov, V. V., Reichart, D. E., Tartaglia, L., Sand, D. J., Valenti, S., Yang, S., Arcavi, Iair, Hosseinzadeh, Griffin, Howell, D. Andrew, McCully, Curtis, Poznanski, Dovi, Vasylyev, Sergiy, Tanvir, N. R., Levan, A. J., Hjorth, J., Cano, Z., Copperwheat, C., de Ugarte-Postigo, A., Evans, P. A., Fynbo, J. P. U., Gonzlez-Fernndez, C., Greiner, J., Irwin, M., Lyman, J., Mandel, I., McMahon, R., Milvang-Jensen, B., OBrien, P., Osborne, J. P., Perley, D. A., Pian, E., Palazzi, E., Rol, E., Rosetti, S., Rosswog, S., Rowlinson, A., Schulze, S., Steeghs, D. T. H., Thne, C. C., Ulaczyk, K., Watson, D., Wiersema, K., Lipunov, V. M., Gorbovskoy, E., Kornilov, V. G., Tyurina, N., Balanutsa, P., Vlasenko, D., Gorbunov, I., Podesta, R., Levato, H., Saffe, C., Buckley, D. A. H., Budnev, N. M., Gress, O., Yurkov, V., Rebolo, R., and Serra-Ricart, M.

Subjects
Gravitational waves -- Measurement, Hubble constant -- Measurement, Environmental issues, Science and technology, Zoology and wildlife conservation
Abstract

Author(s): The LIGO Scientific Collaboration and The Virgo Collaboration; B. P. Abbott [1]; R. Abbott [1]; T. D. Abbott [2]; F. Acernese [3, 4]; K. Ackley [5, 6]; C. Adams [...]

Published
2017
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9. The DES Bright Arcs Survey: Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey 5,000 Sq. Deg. Footprint

Author

O'Donnell, J. H., Wilkinson, R. D., Diehl, H. T., Aros-Bunster, C., Bechtol, K., Birrer, S., Buckley-Geer, E. J., Rosell, A. Carnero, Kind, M. Carrasco, da Costa, L. N., Lozano, S. J. Gonzalez, Gruendl, R. A., Hilton, M., Lin, H., Lindgren, K. A., Martin, J., Pieres, A., Rykoff, E. S., Sevilla-Noarbe, I., Sheldon, E., Sif��n, C., Tucker, D. L., Yanny, B., Abbott, T. M. C., Aguena, M., Allam, S., Andrade-Oliveira, F., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Carretero, J., Costanzi, M., De Vicente, J., Desai, S., Dietrich, J. P., Eckert, K., Everett, S., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Gruen, D., Gschwend, J., Gill, M. S. S., Gutierrez, G., Hinton, S. R., Hollowood, D. L., Honscheid, K., James, D. J., Jeltema, T., Kuehn, K., Lahav, O., Lima, M., Maia, M. A. G., Marshall, J. L., Melchior, P., Menanteau, F., Miquel, R., Morgan, R., Nord, B., Ogando, R. L. C., Paz-Chinch��n, F., Pereira, M. E. S., Malag��n, A. A. Plazas, Rodriguez-Monroy, M., Romer, A. K., Roodman, A., Sanchez, E., Scarpine, V., Schubnell, M., Serrano, S., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., and Varga, T. N.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We report the combined results of eight searches for strong gravitational lens systems in the full 5,000 sq. deg. of Dark Energy Survey (DES) observations. The observations accumulated by the end of the third observing season fully covered the DES footprint in 5 filters (grizY), with an $i-$band limiting magnitude (at $10\sigma$) of 23.44. In four searches, a list of potential candidates was identified using a color and magnitude selection from the object catalogs created from the first three observing seasons. Three other searches were conducted at the locations of previously identified galaxy clusters. Cutout images of potential candidates were then visually scanned using an object viewer. An additional set of candidates came from a data-quality check of a subset of the color-coadd "tiles" created from the full DES six-season data set. A short list of the most promising strong lens candidates was then numerically ranked according to whether or not we judged them to be bona fide strong gravitational lens systems. These searches discovered a diverse set of 247 strong lens candidate systems, of which 81 are identified for the first time. We provide the coordinates, magnitudes, and photometric properties of the lens and source objects, and an estimate of the Einstein radius for 81 new systems and 166 previously reported. This catalog will be of use for selecting interesting systems for detailed follow-up, studies of galaxy cluster and group mass profiles, as well as a training/validation set for automated strong lens searches., Comment: 38 pages, 17 figures, 4 tables, accepted by ApJS

Published
2021

10. KilonovaNet: Surrogate models of kilonova spectra with conditional variational autoencoders.

Author

Lukošiute, K, Raaijmakers, G, Doctor, Z, Soares-Santos, M, and Nord, B

Subjects
RADIATIVE transfer, ASTROPHYSICS, LIGHT curves, EVALUATION methodology, GRAVITATIONAL waves
Abstract

Detailed radiative transfer simulations of kilonova spectra play an essential role in multimessenger astrophysics. Using the simulation results in parameter inference studies requires building a surrogate model from the simulation outputs to use in algorithms requiring sampling. In this work, we present kilonovanet , an implementation of conditional variational autoencoders (cVAEs) for the construction of surrogate models of kilonova spectra. This method can be trained on spectra directly, removing overhead time of pre-processing spectra, and greatly speeds up parameter inference time. We build surrogate models of three state-of-the-art kilonova simulation data sets and present in-depth surrogate error evaluation methods, which can in general be applied to any surrogate construction method. By creating synthetic photometric observations from the spectral surrogate, we perform parameter inference for the observed light-curve data of GW170817 and compare the results with previous analyses. Given the speed with which kilonovanet performs during parameter inference, it will serve as a useful tool in future gravitational wave observing runs to quickly analyse potential kilonova candidates. [ABSTRACT FROM AUTHOR]

Published
2022
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11. Finding quadruply imaged quasars with machine learning – I. Methods.

Author

Akhazhanov, A, More, A, Amini, A, Hazlett, C, Treu, T, Birrer, S, Shajib, A, Liao, K, Lemon, C, Agnello, A, Nord, B, Aguena, M, Allam, S, Andrade-Oliveira, F, Annis, J, Brooks, D, Buckley-Geer, E, Burke, D L, Carnero Rosell, A, and Carrasco Kind, M

Subjects
STELLAR initial mass function, DISTRIBUTION of stars, MACHINE learning, QUASARS, DARK energy, PHYSICAL cosmology
Abstract

Strongly lensed quadruply imaged quasars (quads) are extraordinary objects. They are very rare in the sky and yet they provide unique information about a wide range of topics, including the expansion history and the composition of the Universe, the distribution of stars and dark matter in galaxies, the host galaxies of quasars, and the stellar initial mass function. Finding them in astronomical images is a classic 'needle in a haystack' problem, as they are outnumbered by other (contaminant) sources by many orders of magnitude. To solve this problem, we develop state-of-the-art deep learning methods and train them on realistic simulated quads based on real images of galaxies taken from the Dark Energy Survey, with realistic source and deflector models, including the chromatic effects of microlensing. The performance of the best methods on a mixture of simulated and real objects is excellent, yielding area under the receiver operating curve in the range of 0.86–0.89. Recall is close to 100 per cent down to total magnitude i ∼ 21 indicating high completeness, while precision declines from 85 per cent to 70 per cent in the range i ∼ 17–21. The methods are extremely fast: training on 2 million samples takes 20 h on a GPU machine, and 108 multiband cut-outs can be evaluated per GPU-hour. The speed and performance of the method pave the way to apply it to large samples of astronomical sources, bypassing the need for photometric pre-selection that is likely to be a major cause of incompleteness in current samples of known quads. [ABSTRACT FROM AUTHOR]

Published
2022
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12. Domain adaptation techniques for improved cross-domain study of galaxy mergers

Author

��iprijanovi��, A., Kafkes, D., Jenkins, S., Downey, K., Perdue, G. N., Madireddy, S., Johnston, T., and Nord, B.

Subjects
FOS: Computer and information sciences, Computer Science - Machine Learning, Artificial Intelligence (cs.AI), Computer Science - Artificial Intelligence, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics - Astrophysics of Galaxies, Machine Learning (cs.LG)
Abstract

In astronomy, neural networks are often trained on simulated data with the prospect of being applied to real observations. Unfortunately, simply training a deep neural network on images from one domain does not guarantee satisfactory performance on new images from a different domain. The ability to share cross-domain knowledge is the main advantage of modern deep domain adaptation techniques. Here we demonstrate the use of two techniques - Maximum Mean Discrepancy (MMD) and adversarial training with Domain Adversarial Neural Networks (DANN) - for the classification of distant galaxy mergers from the Illustris-1 simulation, where the two domains presented differ only due to inclusion of observational noise. We show how the addition of either MMD or adversarial training greatly improves the performance of the classifier on the target domain when compared to conventional machine learning algorithms, thereby demonstrating great promise for their use in astronomy., Accepted in: Machine Learning and the Physical Sciences - Workshop at the 34th Conference on Neural Information Processing Systems (NeurIPS); final version

Published
2020

13. CDF Run IIb silicon vertex detector DAQ upgrade

Author

Behari, S., Bacchetta, N., Bolla, G., Cardoso, G., Ciobanu, C.I., Flaugher, B., Garcia-Sciveres, M., Haber, C., Hara, K., Harr, R., Hsiung, T.H., Junk, T., Kim, S., Lu, R.-S., Lujan, P., Maksimovic, P., Merkel, P., Nord, B., Pavlicek, V., Pellett, D., Pursley, J., Schuyler, B., Shenai, A., Treptow, K., Weber, M., and Zimmermann, S.

Subjects
Nuclear physics -- Research, Business, Electronics, Electronics and electrical industries
Abstract

The Collider Detector at Fermilab (CDF) [1] operates in the beamline of the Tevatron proton-antiproton collider at Batavia, IL. The Tevatron is expected to undergo luminosity upgrades (Run IIb) in the future, resulting in a higher number of interactions per beam crossing. To operate in this dense radiation environment, an upgrade of the CDF's silicon vertex detector subsystem and a corresponding upgrade of its VME-based DAQ system has been explored. Prototypes of all the Run IIb SVX DAQ components have been constructed, assembled into a test stand, and operated successfully using an adapted version of the CDF's network-capable DAQ software. In addition, a PCI-based DAQ system has been developed as a fast and inexpensive tool for silicon detector and DAQ component testing in the production phase. In this paper, we present an overview of the Run IIb silicon DAQ upgrade, emphasizing the new features and improvements incorporated into the constituent VME boards and discuss a PCI-based DAQ system developed to facilitate production tests. Index Terms--Collider Detector at Fermilab (CDF) run IIb, data acquisition, PCI, silicon strip detector, VME.

Published
2004

14. Sensors for the CDF Run2b silicon detector

Author

Akimoto, T., Aoki, M., Azzi, P., Bacchetta, N., Behari, S., Benjamin, D., Bisello, D., Bolla, G., Booth, P., Bortoletto, D., Burghard, A., Busetto, G., Cabrera, S., Canepa, A., Cardoso, G., Chertok, M., Ciobanu, C.I., Cooke, P., Derylo, G., Fang, I., Feng, E.J., Fernandez, J.P., Flaugher, B., Freeman, J., Galtieri, L., Galyardt, J., Garcia-Sciveres, M., Giurgiu, G., Gorelov, I., Haber, C., Hale, D., Hara, K., Harr, R., Hill, C., Hoeferkamp, M., Hoff, J., Holbrook, B., Hong, S.C., Hrycyk, M., Hsiung, T.H., Incandela, J., Jeon, E.J., Joo, K.K., Junk, T., Kahkola, H., Karjalainen, S., Kim, S., Kobayashi, K., Kong, D.J., Krieger, B., Kruse, M., Kyre, S., Lander, R., Landry, T., Lauhakangas, R., Lee, J., Lu, R.-S., Lujan, P.J., Lukens, P., Mandelli, E., Manea, C., Maksimovic, P., Merkel, P., Min, S.N., Moccia, S., Nakamura, Y., Nakano, I., Naoumov, D., Nelson, T., Nord, B., Novak, J., Okusawa, T., Orava, R., Orlov, Y., Osterberg, K., Pantano, D., Pavlicek, V., Pellett, D., Pursley, J., Riipinen, P., Schuyler, B., Seidel, S., Shenai, A., Soha, A., Stuart, D., Tanaka, R., Tavi, M., Von der Lippe, H., Walder, J.-P., Wang, Z., Watje, P., Weber, M., Wester, W., Yamamoto, Kenichi, Yang, Y.C., Yao, W., Yarema, R., Yoshitama, H., Yun, J.C., Zetti, F., Zimmerman, T., Zimmermann, S., and Zucchelli, S.

Subjects
Hamamatsu Photonic Systems -- Product development, Silicon diodes -- Product development, Photographic industry -- Product development, Sensors -- Usage, Business, Electronics, Electronics and electrical industries
Abstract

We describe the characteristics of silicon microstrip sensors fabricated by Hamamatsu Photonics for the CDF Run 2b silicon detector. A total of 953 sensors, including 117 prototype sensors, have been produced and tested. Five sensors were irradiated with neutrons up to 1.4 x [10.sup.14] n/[cm.sup.2] as a part of the sensor quality assurance program. The electrical and mechanical characteristics are found to be superior in all aspects and fulfill our specifications. We comment on charge-up susceptibility of the sensors that employ a (100) crystal structure.

Published
2004

15. CDF Run IIb silicon detector: electrical performance and deadtime-less operation

Author

Akimoto, T., Aoki, M., Azzi, P., Bacchetta, N., Behari, S., Benjamin, D., Bisello, D., Bolla, G., Bortoletto, D., Busetto, G., Cabrera, S., Canepa, A., Cardoso, G., Chertok, M., Ciobanu, C.I., Derylo, G., Fang, I., Feng, E.J., Fernandez, J.P., Flaugher, B., Freeman, J., Galtieri, L., Galyardt, J., Garcia-Sciveres, M., Giurgiu, G., Haber, C., Hale, D., Hara, K., Harr, R., Hill, C., Hoff, J., Holbrook, B., Hong, S.C., Hrycyk, M., Hsiung, T.H., Incandela, J., Jeon, E.J., Joo, K.K., Junk, T., Kahkola, H., Karjalainen, S., Kim, S., Kobayashi, K., Kong, D.J., Krieger, B., Kruse, M., Kuznetsova, N., Kyre, S., Lander, R., Landry, T., Lauhakangas, R., Lee, J., Lu, R.-S., Lujan, P., Lukens, P., Mandelli, E., Manea, C., Maksimovic, P., Merkel, P., Min, S.N., Moccia, S., Nakano, I., Nelson, T., Nord, B., Novak, J., Okusawa, T., Orava, R., Orlov, Y., Osterberg, K., Pantano, D., Pavlicek, V., Pellett, D., Pursley, J., Riipinen, P., Schuyler, B., Shenai, A., Soha, A., Stuart, D., Tanaka, R., Tavi, M., Von der Lippe, H., Walder, J.-P., Wang, Z., Weber, Marc, Wester, W., Yamamoto, Kenichi, Yang, Y.C., Yao, W., Yarema, R., Yun, J.C., Zetti, F., Zimmerman, T., Zimmermann, S., and Zucchelli, S.

Subjects
Nuclear physics -- Research, Detectors, Business, Electronics, Electronics and electrical industries
Abstract

The main building block and readout unit of the planned CDF Run IIb silicon detector is a 'stave,' a highly integrated mechanical, thermal, and electrical structure. One of its characteristic features is a copper-on-Kapton flexible cable for power, high voltage, data transmission, and control signals that is placed directly below the silicon microstrip sensors. The dense packaging makes deadtime-less operation of the stave a challenge since coupling of bus cable activity into the silicon sensors must be suppressed efficiently. The stave design features relevant for deadtime-less operation are discussed. The electrical performance achieved with stave prototypes is presented. Index Terms--CDF, deadtime-less, Run IIb, silicon tracker, SVX4.

Published
2004

16. The CDF Run IIb Silicon Detector: Design, preproduction, and performance

Author

Akimoto, T., Aoki, M., Azzi, P., Bacchetta, N., Behari, S., Benjamin, D., Bisello, D., Bolla, G., Bortoletto, D., Burghard, A., Busetto, G., Cabrera, S., Canepa, A., Cardoso, G., Chertok, M., Ciobanu, C.I., Derylo, G., Fang, I., Feng, E.J., Fernandez, J.P., Flaugher, B., Freeman, J., Galtieri, L., Galyardt, J., Garcia-Sciveres, M., Giurgiu, G., Gorelov, I., Haber, C., Hale, D., Hara, K., Harr, R., Hill, C., Hoeferkamp, M., Hoff, J., Holbrook, B., Hong, S.C., Hrycyk, M., Hsiung, T.H., Incandela, J., Jeon, E.J., Joo, K.K., Junk, T., Kahkola, H., Karjalainen, S., Kim, S., Kobayashi, K., Kong, D.J., Krieger, B., Kruse, M., Kuznetsova, N., Kyre, S., Lander, R., Landry, T., Lauhakangas, R., Lee, J., Lu, R.-S., Lujan, P., Lukens, P., Mandelli, E., Manea, C., Maksimovic, P., Merkel, P., Min, S.N., Moccia, S., Nakano, I., Naoumov, D., Nelson, T., Nord, B., Novak, J., Okusawa, T., Orava, R., Orlov, Y., Osterberg, K., Pantano, D., Pavlicek, V., Pellett, D., Pursley, J., Riipinen, P., Schuyler, B., Seidel, S., Shenai, A., Soha, A., Stuart, D., Tanaka, R., Tavi, M., Von der Lippe, H., Walder, J.-P., Wang, Z., Watje, P., Weber, Marc, Wester, W., Yamamoto, K., Yang, Y.C., Yao, W., Yarema, R., Yun, J.C., Zetti, F., Zimmerman, T., Zimmermann, S., and Zucchelli, S.

Published
2006
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17. Expediting DECam Multimessenger Counterpart Searches with Convolutional Neural Networks.

Author

Shandonay, A., Morgan, R., Bechtol, K., Bom, C. R., Nord, B., Garcia, A., Henghes, B., Herner, K., Tabbutt, M., Palmese, A., Santana-Silva, L., Soares-Santos, M., Gill, M. S. S., and GarcĂ-a-Bellido, J.

Subjects
CONVOLUTIONAL neural networks, GRAVITATIONAL wave detectors, INSPECTION & review
Abstract

Searches for counterparts to multimessenger events with optical imagers use difference imaging to detect new transient sources. However, even with existing artifact-detection algorithms, this process simultaneously returns several classes of false positives: false detections from poor-quality image subtractions, false detections from low signal-to-noise images, and detections of preexisting variable sources. Currently, human visual inspection to remove the false positives is a central part of multimessenger follow-up observations, but when next generation gravitational wave and neutrino detectors come online and increase the rate of multimessenger events, the visual inspection process will be prohibitively expensive. We approach this problem with two convolutional neural networks operating on the difference imaging outputs. The first network focuses on removing false detections and demonstrates an accuracy of 92% on our data set. The second network focuses on sorting all real detections by the probability of being a transient source within a host galaxy and distinguishes between various classes of images that previously required additional human inspection. We find the number of images requiring human inspection will decrease by a factor of 1.5 using our approach alone and a factor of 3.6 using our approach in combination with existing algorithms, facilitating rapid multimessenger counterpart identification by the astronomical community. [ABSTRACT FROM AUTHOR]

Published
2022
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18. Dark Energy Survey year 1 results: constraints on extended cosmological models from galaxy clustering and weak lensing

Author

DES Collaboration, Abbott, T. M. C., Abdalla, F. B., Avila, S., Banerji, M., Baxter, E., Bechtol, K., Becker, M. R., Bertin, E., Blazek, J., Bridle, S. L., Brooks, D., Brout, D., Burke, D. L., Campos, A., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, A., Crocce, M., Cunha, C. E., da Costa, L. N., Davis, C., De Vicente, J., DeRose, J., Desai, S., Di Valentino, E., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eifler, T. F., Elvin-Poole, J., Evrard, A. E., Fernandez, E., Fert��, A., Flaugher, B., Fosalba, P., Frieman, J., Garc��a-Bellido, J., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., Jain, B., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kim, A. G., Krause, E., Kuehn, K., Kuropatkin, N., Lahav, O., Lee, S., Lemos, P., Leonard, C. D., Li, T. S., Liddle, A. R., Lima, M., Lin, H., Maia, M. A. G., Marshall, J. L., Martini, P., Menanteau, F., Miller, C. J., Miquel, R., Miranda, V., Mohr, J. J., Muir, J., Nichol, R. C., Nord, B., Ogando, R. L. C., Plazas, A. A., Raveri, M., Rollins, R. P., Romer, A. K., Roodman, A., Rosenfeld, R., Samuroff, S., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Secco, L. F., Serrano, S., Sevilla-Noarbe, I., Smith, M., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., Troxel, M. A., Vikram, V., Walker, A. R., Weaverdyck, N., Wechsler, R. H., Weller, J., Yanny, B., Zhang, Y., Zuntz, J., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, UAM. Departamento de Física Teórica, Natl Opt Astron Observ, UCL, Rhodes Univ, Univ Portsmouth, Univ Cambridge, Univ Penn, LSST, Argonne Natl Lab, Inst Astrophys Paris, UPMC Univ Paris 06, Ohio State Univ, Ecole Polytech Fed Lausanne, Univ Manchester, Stanford Univ, SLAC Natl Accelerator Lab, Universidade Estadual Paulista (Unesp), Carnegie Mellon Univ, Lab Interinst & Astron LIneA, Observ Nacl, Univ Illinois, Natl Ctr Supercomp Applicat, Barcelona Inst Sci & Technol, CSIC, IEEC, Univ Chicago, Univ Michigan, Ctr Invest Energet Medioambientales & Tecnol CIEM, IIT Hyderabad, Fermilab Natl Accelerator Lab, Excellence Cluster Universe, Ludwig Maximilians Univ Munchen, CALTECH, Steward Observ, Univ Edinburgh, Univ Autonoma Madrid, Swiss Fed Inst Technol, Santa Cruz Inst Particle Phys, Max Planck Inst Extraterr Phys, Lawrence Berkeley Natl Lab, Australian Astron Observ, Universidade de São Paulo (USP), Texas A&M Univ, Inst Catalana Recerca & Estudis Avancats, Univ Sussex, Univ Southampton, Brandeis Univ, Universidade Estadual de Campinas (UNICAMP), Oak Ridge Natl Lab, National Optical Astronomy Observatory, University College London, Rhodes University, University of Portsmouth, University of Cambridge, University of Pennsylvania, Argonne National Laboratory, Institut d'Astrophysique de Paris, Ohio State University, Observatoire de Sauverny, University of Manchester, Stanford University, SLAC National Accelerator Laboratory, Universidade Estadual Paulista (UNESP), Carnegie Mellon University, Laboratório Interinstitucional de E-Astronomia - LIneA, Observatório Nacional, University of Illinois at Urbana-Champaign, National Center for Supercomputing Applications, Barcelona Institute of Science and Technology, Institute of Space Sciences (ICE-CSIC), Institut d'Estudis Espacials de Catalunya (IEEC), University of Chicago, University of Michigan, Medioambientales y Tecnológicas (CIEMAT), 382 Via Pueblo Mall, Fermi National Accelerator Laboratory, Ludwig-Maximilians-Universität, California Institute of Technology, University of Edinburgh, Oak Ridge National Laboratory, Universidad Autonoma de Madrid, Ludwig-Maximilians Universität München, ETH Zurich, Santa Cruz Institute for Particle Physics, Max Planck Institute for Extraterrestrial Physics, Lawrence Berkeley National Laboratory, Australian Astronomical Observatory, Texas AandM University, Institució Catalana de Recerca i Estudis Avançats, University of Sussex, University of Southampton, and Physics Department

Subjects
luminous red galaxies, Planck, cosmological model, geometry, MATÉRIA ESCURA, gravitation: model, Cosmic microwave background, Astrophysics, cosmic background radiation, 4/3, des, 01 natural sciences, Cosmology, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), redshift distributions, Weak gravitational lensing, Physics, nucleosynthesis, neutrinos, hep-ph, High Energy Physics - Phenomenology, curvature, astro-ph.CO, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], lambda, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), General relativity, gr-qc, Dark matter, equation of state: time dependence, sloan digital sky survey, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), dark matter, efficient, symbols.namesake, gravitation: lens, 0103 physical sciences, 010306 general physics, STFC, 010308 nuclear & particles physics, Física, RCUK, redshift, Redshift, gravity, Automatic Keywords, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Dark energy, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], sdss, dark energy: equation of state
Abstract

We present constraints on extensions of the minimal cosmological models dominated by dark matter and dark energy, $\Lambda$CDM and $w$CDM, by using a combined analysis of galaxy clustering and weak gravitational lensing from the first-year data of the Dark Energy Survey (DES Y1) in combination with external data. We consider four extensions of the minimal dark energy-dominated scenarios: 1) nonzero curvature $\Omega_k$, 2) number of relativistic species $N_{\rm eff}$ different from the standard value of 3.046, 3) time-varying equation-of-state of dark energy described by the parameters $w_0$ and $w_a$ (alternatively quoted by the values at the pivot redshift, $w_p$, and $w_a$), and 4) modified gravity described by the parameters $\mu_0$ and $\Sigma_0$ that modify the metric potentials. We also consider external information from Planck CMB measurements; BAO measurements from SDSS, 6dF, and BOSS; RSD measurements from BOSS; and SNIa information from the Pantheon compilation. Constraints on curvature and the number of relativistic species are dominated by the external data; when these are combined with DES Y1, we find $\Omega_k=0.0020^{+0.0037}_{-0.0032}$ at the 68% confidence level, and $N_{\rm eff}, Comment: 22 pages, 7 figures, matches the published version

Published
2019

19. First Cosmology Results Using Type Ia Supernovae from the Dark Energy Survey: Photometric Pipeline and Light-curve Data Release

Author

Brout, D, Sako, M, Scolnic, D, Kessler, R, D'Andrea, CB, Davis, TM, Hinton, SR, Kim, AG, Lasker, J, Macaulay, E, Möller, A, Nichol, RC, Smith, M, Sullivan, M, Wolf, RC, Allam, S, Bassett, BA, Brown, P, Castander, FJ, Childress, M, Foley, RJ, Galbany, L, Herner, K, Kasai, E, March, M, Morganson, E, Nugent, P, Pan, YC, Thomas, RC, Tucker, BE, Wester, W, Abbott, TMC, Annis, J, Avila, S, Bertin, E, Brooks, D, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Crocce, M, Cunha, CE, Costa, LND, Davis, C, Vicente, JD, Desai, S, Diehl, HT, Doel, P, Eifler, TF, Flaugher, B, Fosalba, P, Frieman, J, Garcia-Bellido, J, Gaztanaga, E, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Hartley, WG, Hollowood, DL, Honscheid, K, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Lima, M, Marshall, JL, Martini, P, Miquel, R, Nord, B, Plazas, AA, Roodman, A, Rykoff, ES, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Serrano, S, Sevilla-Noarbe, I, Soares-Santos, M, Sobreira, F, Suchyta, E, Swanson, MEC, Tarle, G, Thomas, D, Tucker, DL, Walker, AR, Yanny, B, and Zhang, Y

Subjects
Organic Chemistry, Astrophysics::Instrumentation and Methods for Astrophysics, Molecular, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Physical Chemistry, Atomic, observations [cosmology], photometric [techniques], Particle and Plasma Physics, Affordable and Clean Energy, Astrophysics::Solar and Stellar Astrophysics, Nuclear, general [supernovae], Astrophysics::Galaxy Astrophysics, Astronomical and Space Sciences, astro-ph.IM, Physical Chemistry (incl. Structural)
Abstract

© Contribution of US Department of Energy; not subject to copyright in the United States.. We present griz light curves of 251 SNe Ia from the first 3 years of the Dark Energy Survey Supernova Program's (DES-SN) spectroscopically classified sample. The photometric pipeline described in this paper produces the calibrated fluxes and associated uncertainties used in the cosmological parameter analysis by employing a scene modeling approach that simultaneously models a variable transient flux and temporally constant host galaxy. We inject artificial point sources onto DECam images to test the accuracy of our photometric method. Upon comparison of input and measured artificial supernova fluxes, we find that flux biases peak at 3 mmag. We require corrections to our photometric uncertainties as a function of host galaxy surface brightness at the transient location, similar to that seen by the DES Difference Imaging Pipeline used to discover transients. The public release of the light curves can be found at https://des.ncsa.illinois.edu/releases/sn.

Published
2019

22. Overview of the DESI Legacy Imaging Surveys

Author

Dey, A, Schlegel, DJ, Lang, D, Blum, R, Burleigh, K, Fan, X, Findlay, JR, Finkbeiner, D, Herrera, D, Juneau, S, Landriau, M, Levi, M, McGreer, I, Meisner, A, Myers, AD, Moustakas, J, Nugent, P, Patej, A, Schlafly, EF, Walker, AR, Valdes, F, Weaver, BA, Yeche, C, Zou, H, Zhou, X, Abareshi, B, Abbott, TMC, Abolfathi, B, Aguilera, C, Allen, L, Alvarez, A, Annis, J, Aubert, M, Bell, EF, BenZvi, SY, Bielby, RM, Bolton, AS, Briceno, C, Buckley-Geer, EJ, Butler, K, Calamida, A, Carlberg, RG, Carter, P, Casas, R, Castander, FJ, Choi, Y, Comparat, J, Cukanovaite, E, Delubac, T, DeVries, K, Dey, S, Dhungana, G, Dickinson, M, Ding, Z, Donaldson, JB, Duan, Y, Duckworth, CJ, Eftekharzadeh, S, Eisenstein, DJ, Etourneau, T, Fagrelius, PA, Farihi, J, Fitzpatrick, M, Font-Ribera, A, Fulmer, L, Gansicke, BT, Gaztanaga, E, George, K, Gerdes, DW, Gontcho, SGA, Green, G, Guy, J, Harmer, D, Hernandez, M, Honscheid, K, Lijuan, Huang, James, D, Jannuzi, BT, Jiang, L, Joyce, R, Karcher, A, Karkar, S, Kehoe, R, Kneib, J-P, Kueter-Young, A, Lan, T-W, Lauer, T, Guillou, LL, Suu, ALV, Lee, JH, Lesser, M, Li, TS, Mann, JL, Marshall, B, Martínez-Vázquez, CE, Martini, P, Bourboux, HDMD, McManus, S, Menard, B, Metcalfe, N, Muñoz-Gutiérrez, A, Najita, J, Napier, K, Narayan, G, Newman, JA, Nie, J, Nord, B, Norman, DJ, Olsen, KAG, Paat, A, Palanque-Delabrouille, N, Peng, X, Poppett, CL, Poremba, MR, Prakash, A, Rabinowitz, D, Raichoor, A, Rezaie, M, Robertson, AN, Roe, NA, Ross, AJ, Ross, NP, Rudnick, G, Safonova, S, Saha, A, Sanchez, FJ, Schweiker, H, Scott, A, Seo, H-J, Shan, H, Silva, DR, Soto, C, Sprayberry, D, Staten, R, Stillman, CM, Stupak, RJ, Summers, DL, Tie, SS, Tirado, H, Vargas-Magana, M, Vivas, AK, Wechsler, RH, Williams, D, Yang, J, Yang, Q, Yapici, T, Zaritsky, D, Zenteno, A, Zhang, K, Zhang, T, Zhou, R, and Zhou, Z

Subjects
astro-ph.IM
Abstract

The DESI Legacy Imaging Surveys are a combination of three public projects (the Dark Energy Camera Legacy Survey, the Beijing-Arizona Sky Survey, and the Mayall z-band Legacy Survey) that will jointly image ~14,000 square degrees of the extragalactic sky visible from the northern hemisphere in three optical bands (g, r, and z) using telescopes at the Kitt Peak National Observatory and the Cerro Tololo Inter-American Observatory. The combined survey footprint is split into two contiguous areas by the Galactic plane. The optical imaging is conducted using a unique strategy of dynamic observing that results in a survey of nearly uniform depth. In addition to calibrated images, the project is delivering an inference-based catalog which includes photometry from the grz optical bands and from four mid-infrared bands (at 3.4um, 4.6um, 12um and 22um) observed by the Wide-field Infrared Survey Explorer (WISE) satellite during its full operational lifetime. The project plans two public data releases each year. All the software used to generate the catalogs is also released with the data. This paper provides an overview of the Legacy Surveys project.

Published
2018

23. The Splashback Feature around DES Galaxy Clusters: Galaxy Density and Weak Lensing Profiles

Author

Chang, Chihway, Baxter, E., Jain, B., Sánchez, C., Adhikari, S., Varga, T.N., Fang, Y., Rozo, Eduardo, Rykoff, E.S., Kravtsov, Andrey, Gruen, D., Hartley, W., Huff, E.M., Jarvis, M., Kim, A.G., Prat, J., MacCrann, N., McClintock, T., Palmese, A., Rapetti, D., Rollins, R.P., Samuroff, S., Sheldon, E., Troxel, M.A., Wechsler, R.H., Zhang, Y., Zuntz, J., Abbott, T.M.C., Abdalla, F.B., Allam, S., Annis, J., Bechtol, K., Benoit-Lévy, A., Bernstein, G.M., Brooks, D., Buckley-Geer, E., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., D'Andrea, C.B., Da Costa, L.N., Davis, C., Desai, S., Diehl, H.T., Dietrich, J.P., Drlica-Wagner, A., Eifler, T.F., Flaugher, B., Fosalba, P., Frieman, J., García-Bellido, J., Gaztanaga, E., Gerdes, D.W., Gruendl, R.A., Gschwend, J., Gutierrez, G., Honscheid, K., James, D.J., Jeltema, T., Krause, E., Kuehn, K., Lahav, O., Lima, M., March, M., Marshall, J.L., Martini, P., Melchior, P., Menanteau, F., Miquel, R., Mohr, J.J., Nord, B., Ogando, R.L.C., Plazas, A.A., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R.C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Weller, J., Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and DES

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), galaxies: halos, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, Physical Chemistry, Atomic, 01 natural sciences, Particle and Plasma Physics, gravitational lensing: weak, 0103 physical sciences, Cluster (physics), Nuclear, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Molecular, Astronomy and Astrophysics, Redshift, Galaxy, Dark matter halo, Space and Planetary Science, galaxies: clusters: general, cosmology: observations, Dark energy, Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astronomical and Space Sciences, Physical Chemistry (incl. Structural), Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Splashback refers to the process of matter that is accreting onto a dark matter halo reaching its first orbital apocenter and turning around in its orbit. The cluster-centric radius at which this process occurs, r_sp, defines a halo boundary that is connected to the dynamics of the cluster. A rapid decline in the halo profile is expected near r_sp. We measure the galaxy number density and weak lensing mass profiles around redMaPPer galaxy clusters in the first year Dark Energy Survey (DES) data. For a cluster sample with mean M_200m mass ~2.5 x 10^14 M_sun, we find strong evidence of a splashback-like steepening of the galaxy density profile and measure r_sp=1.13 +/- 0.07 Mpc/h, consistent with earlier SDSS measurements of More et al. (2016) and Baxter et al. (2017). Moreover, our weak lensing measurement demonstrates for the first time the existence of a splashback-like steepening of the matter profile of galaxy clusters. We measure r_sp=1.34 +/- 0.21 Mpc/h from the weak lensing data, in good agreement with our galaxy density measurements. For different cluster and galaxy samples, we find that consistent with LCDM simulations, r_sp scales with R_200m and does not evolve with redshift over the redshift range of 0.3--0.6. We also find that potential systematic effects associated with the redMaPPer algorithm may impact the location of r_sp. We discuss progress needed to understand the systematic uncertainties and fully exploit forthcoming data from DES and future surveys, emphasizing the importance of more realistic mock catalogs and independent cluster samples., Comment: 25 pages, 15 figures; update to journal accepted version

Published
2018

24. COSMOGRAIL: The cosmological monitoring of gravitational lenses

Author

Courbin, F, Bonvin, V, Buckley-Geer, E, Fassnacht, CD, Frieman, J, Lin, H, Marshall, PJ, Suyu, SH, Treu, T, Anguita, T, Motta, V, Meylan, G, Paic, E, Tewes, M, Agnello, A, Chao, DCY, Chijani, M, Gilman, D, Rojas, K, Williams, P, Hempel, A, Kim, S, Lachaume, R, Rabus, M, Abbott, TMC, Allam, S, Annis, J, Banerji, M, Bechtol, K, Benoit-Lévy, A, Brooks, D, Burke, DL, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, D'Andrea, CB, Da Costa, LN, Davis, C, Depoy, DL, Desai, S, Flaugher, B, Fosalba, P, García-Bellido, J, Gaztanaga, E, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, Honscheid, K, James, DJ, Kuehn, K, Kuhlmann, S, Kuropatkin, N, Lahav, O, Lima, M, Maia, MAG, March, M, Marshall, JL, McMahon, RG, Menanteau, F, Miquel, R, Nord, B, Plazas, AA, Sanchez, E, Scarpine, V, Schindler, R, Schubnell, M, Sevilla-Noarbe, I, Smith, M, Soares-Santos, M, Sobreira, F, and Suchyta, E

Subjects
Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

© ESO, 2018. We present time-delay measurements for the new quadruple imaged quasar DES J04085354, the first quadruple imaged quasar found in the Dark Energy Survey (DES). Our result is made possible by implementing a new observational strategy using almost daily observations with the MPIA 2.2 m telescope at La Silla observatory and deep exposures reaching a signal-to-noise ratio of about 1000 per quasar image. This data qualityallows us to catch small photometric variations (a few mmag rms) of the quasar, acting on temporal scales much shorter than microlensing, and hence making the time delay measurement very robust against microlensing. In only seven months we very accurately measured one of the time delays in DES J04085354: - "t(AB) = 112.1 ± 2.1 days (1.8%) using only the MPIA 2.2 m data. In combination with data taken with the 1.2 m Euler Swiss telescope, we also measured two delays involving the D component of the system - "t(AD) = ± 12.8 days (8.2%) and - "t(BD) = 42.4 ± 17.6 days (41%), where all the error bars include systematics. Turning these time delays into cosmological constraints will require deep Hubble Space Telescope (HST) imaging or ground-based adaptive optics (AO), and information on the velocity field of the lensing galaxy.

Published
2018

25. Observation and Confirmation of Six Strong Lensing Systems in The Dark Energy Survey Science Verification Data

Author

Nord, B., Buckley-Geer, E., Lin, H., Diehl, H. T., Helsby, J., Kuropatkin, N., Amara, A., Collett, T., Allam, S., Caminha, G. B., de Bom, C., Desai, S., Dúmet-Montoya, H., Pereira, M. Elidaiana da S., Finley, D. A., Flaugher, B., Furlanetto, C., Gaitsch, H., Gill, M., Merritt, K. W., More, A., Tucker, D., Saro, A., Rykoff, E. S., Rozo, E., Birrer, S., Abdalla, F. B., Agnello, A., Auger, M., Brunner, R. J., Carrasco Kind, M., Castander, F. J., Cunha, C. E., da Costa, L. N., Foley, R. J., Gerdes, D. W., Glazebrook, K., Gschwend, J., Hartley, W., Kessler, R., Lagattuta, D., Lewis, G., Maia, M. A. G., Makler, M., Menanteau, F., Niernberg, A., Scolnic, D., Vieira, J. D., Gramillano, R., Abbott, T. M. C., Banerji, M., Benoit-Lévy, A., Brooks, D., Burke, D. L., Capozzi, D., Carnero Rosell, A., Carretero, J., d'Andrea, C. B., Dietrich, J. P., Doel, P., Evrard, A. E., Frieman, J., Gaztanaga, E., Gruen, D., Honscheid, K., James, D. J., Kuehn, K., Li, T. S., Lima, M., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Neilsen, E., Nichol, R. C., Ogando, R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Walker, A. R., Wester, W., Zhang, Y., Centre de Recherche Astrophysique de Lyon (CRAL), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Nord, B., Buckley-Geer, E., Lin, H., Diehl, H. T., Helsby, J., Kuropatkin, N., Amara, A., Collett, T., Allam, S., Caminha, G. B., De Bom, C., Desai, S., Dumet-Montoya, H., Da Pereira, M. Elidaiana S., Finley, D. A., Flaugher, B., Furlanetto, C., Gaitsch, H., Gill, M., Merritt, K. W., More, A., Tucker, D., Saro, A., Rykoff, E. S., Rozo, E., Birrer, S., Abdalla, F. B., Agnello, A., Auger, M., Brunner, R. J., Kind, M. Carrasco, Castander, F. J., Cunha, C. E., Da Costa, L. N., Foley, R. J., Gerdes, D. W., Glazebrook, K., Gschwend, J., Hartley, W., Kessler, R., Lagattuta, D., Lewis, G., Maia, M. A. G., Makler, M., Menanteau, F., Niernberg, A., Scolnic, D., Vieira, J. D., Gramillano, R., Abbott, T. M. C., Banerji, M., Benoit-Lévy, A., Brooks, D., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Carretero, J., D'Andrea, C. B., Dietrich, J. P., Doel, P., Evrard, A. E., Frieman, J., Gaztanaga, E., Gruen, D., Honscheid, K., James, D. J., Kuehn, K., Li, T. S., Lima, M., Marshall, J. L., Martini, P., Melchior, P., Miquel, R., Neilsen, E., Nichol, R. C., Ogando, R., Plazas, A. A., Romer, A. K., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Walker, A. R., Wester, W., and Zhang, Y.

Subjects
Strong gravitational lensing, observational [methods], Astrophysics, 01 natural sciences, cosmology: observations, galaxies: clusters: general, galaxies: distances and redshifts, gravitational lensing: strong, methods: observational, techniques: spectroscopic, Astronomy and Astrophysics, Space and Planetary Science, Einstein radius, law.invention, law, clusters: general [galaxies], Astrophysics::Solar and Stellar Astrophysics, Surface brightness, 010303 astronomy & astrophysics, QB, Physics, Solar mass, Astrophysics::Instrumentation and Methods for Astrophysics, observations [cosmology], strong [gravitational lensing], astro-ph.CO, spectroscopic [techniques], Astrophysics::Earth and Planetary Astrophysics, observation [cosmology], Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), astro-ph.GA, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Telescope, 0103 physical sciences, distances and redshift [galaxies], Spectrograph, distances and reshifts [galaxies], Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, Astronomy and Astrophysic, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, [SDU]Sciences of the Universe [physics], 13. Climate action, Astrophysics of Galaxies (astro-ph.GA), uploaded-in-3-months-elsewhere
Abstract

We report the observation and confirmation of the first group- and cluster-scale strong gravitational lensing systems found in Dark Energy Survey (DES) data. Through visual inspection of data from the Science Verification (SV) season, we identified 53 candidate systems. We then obtained spectroscopic follow-up of 21 candidates using the Gemini Multi-Object Spectrograph (GMOS) at the Gemini South telescope and the Inamori-Magellan Areal Camera and Spectrograph (IMACS) at the Magellan/Baade telescope. With this follow-up, we confirmed six candidates as gravitational lenses: Three of the systems are newly discovered, and the remaining three were previously known. Of the 21 observed candidates, the remaining 15 were either not detected in spectroscopic observations, were observed and did not exhibit continuum emission (or spectral features), or were ruled out as lensing systems. The confirmed sample consists of one group-scale and five galaxy cluster-scale lenses. The lensed sources range in redshift z ~ 0.80-3.2, and in i-band surface brightness i_{SB} ~ 23-25 mag/sq.-arcsec. (2" aperture). For each of the six systems, we estimate the Einstein radius and the enclosed mass, which have ranges ~ 5.0 - 8.6" and ~ 7.5 x 10^{12} - 6.4 x 10^{13} solar masses, respectively., 17 pages, 7 figures, 4 tables; submitted to ApJ

Published
2015

26. The Electromagnetic Counterpart of the Binary Neutron Star Merger LIGO/Virgo GW170817. I. Discovery of the Optical Counterpart Using the Dark Energy Camera

Author

Soares-Santos, M., Holz, D.E., Annis, J., Chornock, R., Herner, K., Berger, E., Brout, D., Chen, H.-Y., Kessler, R., Sako, M., Allam, S., Tucker, DL., Butler, R. E., Palmese, A., Doctor, Z., Diehl, H.T., Frieman, J., Yanny, B., Lin, H., Scolnic, D., Cowperthwaite, P., Neilsen, E., Marriner, J., Kuropatkin, N., Hartley, W.G., Alexander, K.D., Balbinot, E., Blanchard, P., Brown, D.A., Carlin, J.L., Conselice, Christopher J., Cook, E.R., Drlica-Wagner, A., Drout, M.R., Durret, F., Eftekhari, T., Farr, B., Finley, D.A., Foley, R.J., Fong, W., Fryer, C.L., Gill, M.S.S., Gruendl, R.A., Hanna, C., Kasen, D., Li, T.S., Lopes, P.A.A., Margutti, R., Marshall, J.L., Matheson, T., Medina, G.E., Metzger, B.D., Muir, J., Nicholl, M., Quataert, E., Rest, A., Sauseda, M., Schlegel, D.J., Secco, L.F., Sobreira, F., Stebbins, A., Villar, V.A., Vivas, K., Walker, A.R., Wester, W., Williams, P.K.G., Zenteno, A., Zhang, Y., Abbott, T.M.C., Abdalla, F.B., Banerji, M., Bechtol, K., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D.L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F.J., Crocce, M., Cunha, C.E., Costa, L.N. da, Davis, C., Desai, S., Dietrich, J.P., Doel, P., Eifler, T.F., Fernandez, E., Flaugher, B., Fosalba, P., Gaztanaga, E., Gerdes, D.W., Giannantonio, T., Goldstein, D.A., Gruen, D., Gschwend, J., Gutierrez, G., Honscheid, K., Jain, B., James, D.J., Jeltema, T., Johnson, M.W.G., Johnson, M.D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuhlmann, S., Lahav, O., Lima, M., Maia, M.A.G., March, M., McMahon, R.G., Menanteau, F., Miquel, R., Mohr, J.J., Nichol, R.C., Nord, B., Ogando, R.L C., Petravick, D., Plazas, A.A., Romer, A.K., Roodman, A., Rykoff, E.S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, M., Smith, R.C., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., Thomas, R.C., Troxel, M.A., Vikram, V., Wechsler, R.H., and Weller, J.

Subjects
binaries: close— catalogs— gravitational waves — stars: neutron— surveys
Abstract

We present the Dark Energy Camera (DECam) discovery of the optical counterpart of the first binary neutron star merger detected through gravitational wave emission, GW170817. Our observations commenced 10.5 hours post-merger, as soon as the localization region became accessible from Chile. We imaged 70 deg2 in the i and z bands, covering 93% of the initial integrated localization probability, to a depth necessary to identify likely optical counterparts (e.g., a kilonova). At 11.4 hours post-merger we detected a bright optical transient located 10:600 from the nucleus of NGC4993 at redshift z = 0:0098, consistent (for H0 = 70 km s-1 Mpc-1) with the distance of 40±8 Mpc reported by the LIGO Scientific Collaboration and the Virgo Collaboration (LVC). At detection the transient had magnitudes i=17.3 and z=17.4, and thus an absolute magnitude of Mi = -15.7, in the luminosity range expected for a kilonova. We identified 1,500 potential transient candidates. Applying simple selection criteria aimed at rejecting background events such as supernovae, we find the transient associated with NGC4993 as the only remaining plausible counterpart, and reject chance coincidence at the 99.5% confidence level. We therefore conclude that the optical counterpart we have identified near NGC4993 is associated with GW170817. This discovery ushers in the era of multi-messenger astronomy with gravitational waves, and demonstrates the power of DECam to identify the optical counterparts of gravitational-wave sources.

Published
2017

27. The DES bright arcs survey: hundreds of candidate strongly lensed galaxy systems from the Dark Energy Survey Science Verification and Year 1 observations

Author

Diehl, H.T., Buckley-Geer, E.J., Lindgren, K.A., Nord, B., Gaitsch, H., Gaitsch, S., Lin, H., Allam, S., Collett, T.E., Furlanetto, C., Gill, M.S.S., More, A., Nightingale, J., Odden, C., Pellico, A., Tucker, D.L., Costa, L.N. da, Neto, A.Fausti, Kuropatkin, N., Soares-Santos, M., Welch, B., Zhang, Y., Frieman, J.A., Abdalla, F.B., Annis, J., Bertin, E., Brooks, D., Burke, D. L., Rosell, A.Carnero, Kind, M.Carrasco, Carretero, J., Cunha, C.E., Desai, S., Dietrich, J.P., Drlica-Wagner, A., Evrard, A.E., Finley, D.A., Flaugher, B., Gerdes, D.W., Goldstein, D.A., Gruen, D., Gruendl, R.A., Gschwend, J., Gutierrez, G., James, D.J., Kuehn, K., Kuhlmann, S., Lahav, O., Li, T.S., Lima, M., Maia, M.A.G., Marshall, J.L., Menanteau, F., Miquel, R., Nichol, R.C., Nugent, P., Ogando, R.L.C., Plazas, A.A., Reil, K., Romer, A.K., Sako, M., Sanchez, E., Santiago, B., Scarpine, V., Schindler, R., Schubnell, M., Sevilla-Noarbe, I., Sheldon, E., Smith, M., Sobreira, F., Suchyta, E., Swanson, M.E.C., Tarle, G., Thomas, D., and Walker, A.R.

Subjects
galaxies: high-redshift – gravitational lensing: strong
Abstract

We report the results of searches for strong gravitational lens systems in the Dark Energy Survey (DES) Science Verification and Year 1 observations. The Science Verification data span approximately 250 sq. deg. with a median i-band limiting magnitude for extended objects (10?) of 23.0. The Year 1 data span approximately 2000 sq. deg. and have anti-band limiting magnitude for extended objects (10?) of 22.9. As these data sets are both wide and deep, they are particularly useful for identifying strong gravitational lens candidates. Potential strong gravitational lens candidate systems were initially identified based on a color and magnitude selection in the DES object catalogs or because the system is at the location of a previously identified galaxy cluster. Cutout images of potential candidates were then visually scanned using an object viewer and numerically ranked according to whether or not we judged them to be likely strong gravitational lens systems. Having scanned nearly 400,000 cutouts, we present 374 candidate strong lens systems, of which 348 are identified for the first time. We provide the R.A. and decl., the magnitudes and photometric properties of the lens and source objects, and the distance (radius) of the source(s) from the lens center for each system.

Published
2017

28. The des Bright Arcs Survey: Hundreds of Candidate Strongly Lensed Galaxy Systems from the Dark Energy Survey Science Verification and Year 1 Observations

Author

Diehl, HT, Buckley-Geer, EJ, Lindgren, KA, Nord, B, Gaitsch, H, Gaitsch, S, Lin, H, Allam, S, Collett, TE, Furlanetto, C, Gill, MSS, More, A, Nightingale, J, Odden, C, Pellico, A, Tucker, DL, Costa, LND, Neto, AF, Kuropatkin, N, Soares-Santos, M, Welch, B, Zhang, Y, Frieman, JA, Abdalla, FB, Annis, J, Benoit-Lévy, A, Bertin, E, Brooks, D, Burke, DL, Rosell, AC, Kind, MC, Carretero, J, Cunha, CE, D'Andrea, CB, Desai, S, Dietrich, JP, Drlica-Wagner, A, Evrard, AE, Finley, DA, Flaugher, B, García-Bellido, J, Gerdes, DW, Goldstein, DA, Gruen, D, Gruendl, RA, Gschwend, J, Gutierrez, G, James, DJ, Kuehn, K, Kuhlmann, S, Lahav, O, Li, TS, Lima, M, Maia, MAG, Marshall, JL, Menanteau, F, Miquel, R, Nichol, RC, Nugent, P, Ogando, RLC, Plazas, AA, Reil, K, Romer, AK, Sako, M, Sanchez, E, Santiago, B, Scarpine, V, Schindler, R, Schubnell, M, Sevilla-Noarbe, I, Sheldon, E, Smith, M, Sobreira, F, and Suchyta, E

Abstract

© 2017. The American Astronomical Society. All rights reserved.. We report the results of searches for strong gravitational lens systems in the Dark Energy Survey (DES) Science Verification and Year 1 observations. The Science Verification data span approximately 250 sq. deg. with a median i-band limiting magnitude for extended objects (10σ) of 23.0. The Year 1 data span approximately 2000 sq. deg. and have an i-band limiting magnitude for extended objects (10σ) of 22.9. As these data sets are both wide and deep, they are particularly useful for identifying strong gravitational lens candidates. Potential strong gravitational lens candidate systems were initially identified based on a color and magnitude selection in the DES object catalogs or because the system is at the location of a previously identified galaxy cluster. Cutout images of potential candidates were then visually scanned using an object viewer and numerically ranked according to whether or not we judged them to be likely strong gravitational lens systems. Having scanned nearly 400,000 cutouts, we present 374 candidate strong lens systems, of which 348 are identified for the first time. We provide the R.A. and decl., the magnitudes and photometric properties of the lens and source objects, and the distance (radius) of the source(s) from the lens center for each system.

Published
2017

29. OzDES multifibre spectroscopy for the Dark Energy Survey: Three year results and first data release

Author

Childress, M. J., Lidman, C., Davis, T. M., Tucker, B. E., Asorey, J., Yuan, F., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Banerji, M., Benoit-Levy, A., Stephanie Bernard, Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carollo, D., Carrasco Kind, M., Carretero, J., Castander, F. J., Cunha, C. E., Da Costa, L. N., D Andrea, C. B., Doel, P., Eifler, T. F., Evrard, A. E., Flaugher, B., Foley, R. J., Fosalba, P., Frieman, J., Garcia-Bellido, J., Glazebrook, K., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gschwend, J., Gupta, R. R., Gutierrez, G., Hinton, S. R., Hoormann, J. K., James, D. J., Kessler, R., Kim, A. G., King, A. L., Kovacs, E., Kuehn, K., Kuhlmann, S., Kuropatkin, N., Lagattuta, D. J., Lewis, G. F., Li, T. S., Lima, M., Lin, H., Macaulay, E., Maia, M. A. G., Marriner, J., March, M., Marshall, J. L., Martini, P., Mcmahon, R. G., Menanteau, F., Miquel, R., Moller, A., Morganson, E., Mould, J., Mudd, D., Muthukrishna, D., Nichol, R. C., Nord, B., Ogando, R. L. C., Ostrovski, F., Parkinson, D., Plazas, A. A., Reed, S. L., Reil, K., Romer, A. K., Rykoff, E. S., Sako, M., Sanchez, E., Scarpine, V., Schindler, R., Schubnell, M., Scolnic, D., Sevilla-Noarbe, I., Seymour, N., Sharp, R., Smith, M., Soares-Santos, M., Sobreira, F., Sommer, N. E., Spinka, H., Suchyta, E., Sullivan, M., Swanson, M. E. C., Tarle, G., Uddin, S. A., Walker, A. R., Wester, W., and Zhang, B. R.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present results for the first three years of OzDES, a six-year programme to obtain redshifts for objects in the Dark Energy Survey (DES) supernova fields using the 2dF fibre positioner and AAOmega spectrograph on the Anglo-Australian Telescope. OzDES is a multi-object spectroscopic survey targeting multiple types of targets at multiple epochs over a multi-year baseline, and is one of the first multi-object spectroscopic surveys to dynamically include transients into the target list soon after their discovery. At the end of three years, OzDES has spectroscopically confirmed almost 100 supernovae, and has measured redshifts for 17,000 objects, including the redshifts of 2,566 supernova hosts. We examine how our ability to measure redshifts for targets of various types depends on signal-to-noise, magnitude, and exposure time, finding that our redshift success rate increases significantly at a signal-to-noise of 2 to 3 per 1-Angstrom bin. We also find that the change in signal-to-noise with exposure time closely matches the Poisson limit for stacked exposures as long as 10 hours. We use these results to predict the redshift yield of the full OzDES survey, as well as the potential yields of future surveys on other facilities such as the 4m Multi-Object Spectroscopic Telescope (4MOST), the Subaru Prime Focus Spectrograph (PFS), and the Maunakea Spectroscopic Explorer (MSE). This work marks the first OzDES data release, comprising 14,693 redshifts. OzDES is on target to obtain over a yield of approximately 5,700 supernova host-galaxy redshifts., Accepted for publication in MNRAS. Redshift data release is available at http://www.mso.anu.edu.au/ozdes/DR1

Published
2017

30. Observation and confirmation of nine strong-lensing systems in Dark Energy Survey Year 1 data.

Author

Nord, B, Buckley-Geer, E, Lin, H, Kuropatkin, N, Collett, T, Tucker, D L, Diehl, H T, Agnello, A, Amara, A, Abbott, T M C, Allam, S, Annis, J, Avila, S, Bechtol, K, Brooks, D, Burke, D L, Carnero Rosell, A, Carrasco Kind, M, Carretero, J, and Cunha, C E

Subjects
*DARK energy, *GRAVITATIONAL lenses, *INSPECTION & review, *CLUSTER sampling, *SPECTROGRAPHS, *GALAXY clusters, *GALAXIES
Abstract

We describe the observation and confirmation of nine new strong gravitational lenses discovered in Year 1 data from the Dark Energy Survey (DES). We created candidate lists based on (i) galaxy group and cluster samples, and (ii) photometrically selected galaxy samples. We selected 46 candidates through visual inspection and then used the Gemini Multi-Object Spectrograph (GMOS) at the Gemini South telescope to acquire a spectroscopic follow-up of 21 of these candidates. Through an analysis of these spectroscopic follow-up data, we confirmed nine new lensing systems and rejected two candidates, and the analysis was inconclusive on 10 candidates. For each of the confirmed systems, our report measured spectroscopic properties, estimated source image–lens separations, and estimated enclosed masses as well. The sources that we targeted have an i -band surface brightness range of |$i_{\rm SB} \sim 22\!-\!24\, {\rm mag}\,{\rm arcsec}^{-2}$| and a spectroscopic redshift range of z spec ∼ 0.8−2.6. The lens galaxies have a photometric redshift range of z lens ∼ 0.3−0.7. The lensing systems range in source image–lens separation from 2 to 9 arcsec and in enclosed mass from 1012 to 1013 M⊙. [ABSTRACT FROM AUTHOR]

Published
2020
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31. Galaxy bias from the DES Science Verification data:combining galaxy density maps and weak lensing maps

Author

Chang, C., Pujol, A., Gaztanaga, E., Amara, A., Refregier, A., Bacon, D., Becker, M. R., Bonnett, C., Carretero, J., Castander, F. J., Crocce, M., Fosalba, P., Giannantonio, T., Hartley, W., Jarvis, M., Kacprzak, T., Ross, A. J., Sheldon, E., Troxel, M. A., Vikram, V., Zuntz, J., Abbott, T. M. C., Abdalla, F. B., Allam, S., Annis, J., Benoit-Levy, A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Capozzi, D., Rosell, A. Carnero, Kind, M. Carrasco, Cunha, C. E., D'Andrea, C. B., Costa, L. N. da, Desai, S., Diehl, H. T., Dietrich, J. P., Doel, P., Eifler, T. F., Estrada, J., Evrard, A. E., Flaugher, B., Frieman, J., Goldstein, D. A., Gruen, D., Gruendl, R. A., Gutierrez, G., Honscheid, K., Jain, B., James, D. J., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lima, M., Marshall, J. L., Martini, P., Melchior, P., Miller, C. J., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Romer, A. K., Roodman, A., Rykoff, E. S., Sanchez, E., Scarpine, V., Schubnell, M., Sevilla-Noarbe, I., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., and Walker, A. R.

Subjects
Cosmology and Gravitation, astro-ph.CO, RCUK, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics, STFC
Abstract

We measure the redshift evolution of galaxy bias for a magnitude-limited galaxy sample by combining the galaxy density maps and weak lensing shear maps for a ∼116 deg2 area of the Dark Energy Survey (DES) Science Verification (SV) data. This method was first developed in Amara et al. and later re-examined in a companion paper with rigorous simulation tests and analytical treatment of tomographic measurements. In this work we apply this method to the DES SV data and measure the galaxy bias for a i < 22.5 galaxy sample. We find the galaxy bias and 1σ error bars in four photometric redshift bins to be 1.12 ± 0.19 (z = 0.2–0.4), 0.97 ± 0.15 (z = 0.4–0.6), 1.38 ± 0.39 (z = 0.6–0.8), and 1.45 ± 0.56 (z = 0.8–1.0). These measurements are consistent at the 2σ level with measurements on the same data set using galaxy clustering and cross-correlation of galaxies with cosmic microwave background lensing, with most of the redshift bins consistent within the 1σ error bars. In addition, our method provides the only σ8 independent constraint among the three. We forward model the main observational effects using mock galaxy catalogues by including shape noise, photo-z errors, and masking effects. We show that our bias measurement from the data is consistent with that expected from simulations. With the forthcoming full DES data set, we expect this method to provide additional constraints on the galaxy bias measurement from more traditional methods. Furthermore, in the process of our measurement, we build up a 3D mass map that allows further exploration of the dark matter distribution and its relation to galaxy evolution.

Published
2016

32. DES14X3taz: A TYPE I SUPERLUMINOUS SUPERNOVA SHOWING A LUMINOUS, RAPIDLY COOLING INITIAL PRE-PEAK BUMP

Author

Smith, M, Sullivan, M, D'Andrea, CB, Castander, FJ, Casas, R, Prajs, S, Papadopoulos, A, Nichol, RC, Karpenka, NV, Bernard, SR, Brown, P, Cartier, R, Cooke, J, Curtin, C, Davis, TM, Finley, DA, Foley, RJ, Gal-Yam, A, Goldstein, DA, González-Gaitán, S, Gupta, RR, Howell, DA, Inserra, C, Kessler, R, Lidman, C, Marriner, J, Nugent, P, Pritchard, TA, Sako, M, Smartt, S, Smith, RC, Spinka, H, Thomas, RC, Wolf, RC, Zenteno, A, Abbott, TMC, Benoit-Lévy, A, Bertin, E, Brooks, D, Buckley-Geer, E, Rosell, AC, Kind, MC, Carretero, J, Crocce, M, Cunha, CE, Da Costa, LN, Desai, S, Diehl, HT, Doel, P, Estrada, J, Evrard, AE, Flaugher, B, Fosalba, P, Frieman, J, Gerdes, DW, Gruen, D, Gruendl, RA, James, DJ, Kuehn, K, Kuropatkin, N, Lahav, O, Li, TS, Marshall, JL, Martini, P, Miller, CJ, Miquel, R, Nord, B, Ogando, R, Plazas, AA, Reil, K, Romer, AK, and Roodman, A

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, general [supernovae], Astrophysics::Galaxy Astrophysics
Abstract

© 2016. The American Astronomical Society. All rights reserved. We present DES14X3taz, a new hydrogen-poor superluminous supernova (SLSN-I) discovered by the Dark Energy Survey (DES) supernova program, with additional photometric data provided by the Survey Using DECam for Superluminous Supernovae. Spectra obtained using Optical System for Imaging and low-Intermediate-Resolution Integrated Spectroscopy on the Gran Telescopio CANARIAS show DES14X3taz is an SLSN-I at z = 0.608. Multi-color photometry reveals a double-peaked light curve: a blue and relatively bright initial peak that fades rapidly prior to the slower rise of the main light curve. Our multi-color photometry allows us, for the first time, to show that the initial peak cools from 22,000 to 8000 K over 15 rest-frame days, and is faster and brighter than any published core-collapse supernova, reaching 30% of the bolometric luminosity of the main peak. No physical 56Ni-powered model can fit this initial peak. We show that a shock-cooling model followed by a magnetar driving the second phase of the light curve can adequately explain the entire light curve of DES14X3taz. Models involving the shock-cooling of extended circumstellar material at a distance of ≃400 R⊙ are preferred over the cooling of shock-heated surface layers of a stellar envelope. We compare DES14X3taz to the few double-peaked SLSN-I events in the literature. Although the rise times and characteristics of these initial peaks differ, there exists the tantalizing possibility that they can be explained by one physical interpretation.

Published
2016

33. Supplement: 'Localization and Broadband Follow-up of the Gravitational-wave Transient GW150914' (2016, ApJS, 225, 8)

Author

Abbott, B. P., Abbott, R., Abbott, T. D., Abernathy, M. R., Acernese, F., Ackley, K., Adams, C., Adams, T., Addesso, P., Adhikari, R. X., Adya, V. B., Bodiya, T. P., Goetz, R., Mihara, T., Gondan, L., González, G., Castro, J. M. G., Gopakumar, A., Gordon, N. A., Gorodetsky, M. L., Miao, H., Gossan, S. E., Walsh, S., Johnson, M. D., Aston, S. M., Tomida, H., Gosselin, M., Gouaty, R., Graef, C., Graff, P. B., Granata, M., Grant, A., Gras, S., Wang, G., Michel, C., Gray, C., Greco, G., Ueno, S., Johnson, M. W. G., Green, A. C., Astone, P., Groot, P., Grote, H., Grunewald, S., Vikram, V., Guidi, G. M., Guo, X., Nichol, R. C., Gupta, A., Tsunemi, H., Gupta, M. K., Gushwa, K. E., Karliner, I., Gustafson, E. K., Gustafson, R., Wang, H., Aufmuth, P., Hacker, J. J., Hall, B. R., Hall, E. D., Middleton, H., Cavalier, F., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Wang, M., Braginsky, V. B., Hanna, C., Hannam, M. D., Hanson, J., Aulbert, C., Hardwick, T., Cowperthwaite, P. S., Mikhailov, E. E., Haris, K., Harms, J., Wang, X., Harry, G. M., Harry, I. W., Hart, M. J., Kasen, D., Hartman, M. T., Haster, C. -J., Haughian, K., Matsuoka, M., Heidmann, A., Milano, L., Wang, Y., Babak, S., Heintze, M. C., Heitmann, H., Hello, P., Hemming, G., Hendry, M., Kent, S., Heng, I. S., MAXI Collaboration, Hennig, J., Ward, R. L., Heptonstall, A. W., Miller, J., Heurs, M., Hild, S., Bacon, P., Hoak, D., Hodge, K. A., Hofman, D., Hollitt, S. E., Mason, K., Warner, J., Kessler, R., Holt, K., Holz, D. E., Millhouse, M., Hopkins, P., Hosken, D. J., Hough, J., Houston, E. A., Bader, M. K. M., Howell, E. J., Smith, M., Fraser, M., Croft, S., Hu, Y. M., Huang, S., Kim, A. G., Huerta, E. A., Królak, A., Batch, J. C., Huet, D., Hughey, B., Husa, S., Martini, P., Huttner, S. H., Feng, L., Huynh-Dinh, T., Idrisy, A., Baker, P. T., Indik, N., Ingram, D. R., Carrasco Kind, M., Minenkov, Y., Inta, R., Was, M., Isa, H. N., Isac, J. -M., Franzen, T. M. O., Isi, M., Islas, G., Isogai, T., Iyer, B. R., Izumi, K., Baldaccini, F., Jacqmin, T., Weaver, B., Ming, J., Kuehn, K., Jang, H., Gaensler, B. M., Jani, K., Jaranowski, P., Jawahar, S., Jiménez-Forteza, F., Johnson, W. W., Jones, D. I., Boer, M., Jones, R., Jonker, R. J. G., Mirshekari, S., Ballardin, G., Johnston-Hollitt, M., Kuropatkin, N., Ju, L., Kalaghatgi, C. V., Kalogera, V., Kandhasamy, S., Wei, L. -W., Kang, G., Kanner, J. B., Karki, S., Kasprzack, M., Mishra, C., Kaplan, D. L., Katsavounidis, E., Katzman, W., Lahav, O., Ballmer, S. W., Walker, A. R., Kaufer, S., Kaur, T., Kawabe, K., Kawazoe, F., Kéfélian, F., Kehl, M. S., Morales, M. F., Nord, B., Keitel, D., Kelley, D. B., Weinert, M., Kells, W., Li, T. S., Kennedy, R., Barayoga, J. C., Key, J. S., Khalaidovski, A., Khalili, F. Y., Tingay, S. J., Khan, I., Mitra, S., Weinstein, A. J., Khan, S., Khan, Z., Khazanov, E. A., Kijbunchoo, N., Lima, M., Kim, C., Kim, J., Barclay, S. E., Crocce, M., Kim, K., Weiss, R., Kim, N., Mitrofanov, V. P., Kim, Y. -M., King, E. J., King, P. J., Kinzel, D. L., Kissel, J. S., Branchesi, M., Kleybolte, L., Cavalieri, R., Blackburn, J. K., Welborn, T., Klimenko, S., Koehlenbeck, S. M., Barish, B. C., Mitselmakher, G., Kokeyama, K., Koley, S., Kondrashov, V., Kontos, A., Korobko, M., Korth, W. Z., Martin, R. M., Masserot, A., Mittleman, R., Barker, D., Moggi, A., Mohan, M., Baune, C., Mohapatra, S. R. P., Montani, M., Moore, B. C., Nugent, P., Matone, L., Moore, C. J., Wayth, R. B., Moraru, D., Moreno, G., Krueger, C., Morriss, S. R., Mossavi, K., Mours, B., Mow-Lowry, C. M., Bavigadda, V., Wen, L., Mueller, C. L., Mueller, G., Williams, A., Ogando, R., Muir, A. W., Mukherjee, A., Kuehn, G., Mukherjee, D., Mukherjee, S., Mukund, N., Lord, J. E., Mullavey, A., Munch, J., Murphy, D. J., Murchison Wide-field Array (MWA Collaboration), Bazzan, M., Murray, P. 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C., Estrada, J., Milvang-Jensen, B., Venkateswara, K., Watson, D., Charlton, P., Irwin, M., Fernandez, C. G., McMahon, R. G., Banerji, M., Gonzalez-Solares, E., Bartlett, J., Schulze, S., McIntyre, G., Verkindt, D., de Ugarte Postigo, A., Evrard, A. E., Thoene, C. C., Cano, Z., Rosswog, S., Chassande-Mottin, E., VISTA Collaboration, ASCENZI, STEFANO, Kornilov, V., Barsotti, L., MANGANO, VALERIA, Kowalska, I., McIver, J., MUKHERJEE, DIPANJAN, SALEMI, Filippo, Fernandez, E., SANCHEZ RAMIREZ, RUBEN, DI MAURO, Maria Giuseppina, GIROLETTI, MARCELLO, Balanutsa, P., Vetrano, F., Chen, H. Y., ORIENTI, Monica, Bork, R., STELLA, Luigi, Bradaschia, C., TESTA, Vincenzo, BAZZANO, ANGELA, Chen, Y., Caudill, S., Thomas, R. C., Aiello, L., Cheng, C., Chincarini, A., Chiummo, A., Brau, J. E., Cho, H. S., Cho, M., Chow, J. H., Finley, D. A., Christensen, N., Chen, T. -W., Kuznetsov, A., Chu, Q., Chua, S., Chung, S., Ain, A., Ciani, G., McManus, D. J., Clara, F., Clark, J. A., Cleva, F., Viceré, A., Coccia, E., Buckley, D., Flaugher, B., Cohadon, P. -F., Colla, A., Collette, C. G., Cominsky, L., Constancio, M., Jr., McWilliams, S. T., Ajith, P., Vinciguerra, S., Conte, A., Conti, L., Castander, F. J., Cook, D., Corbitt, T. R., Foley, R. J., Cornish, N., Corsi, A., Cortese, S., Costa, C. A., Vine, D. J., Meacher, D., Coughlin, M. W., Coughlin, S. B., Rebolo, R., Allen, B., Coulon, J. -P., Countryman, S. T., Couvares, P., Fong, W. -F., Cowan, E. E., Vinet, J. -Y., Coward, D. M., Cowart, M. J., Bassiri, R., Coyne, D. C., Serra-Ricart, M., Coyne, R., Craig, K., Creighton, J. D. E., Allocca, A., Cripe, J., Vitale, S., Crowder, S. G., Fosalba, P., Cumming, A., Cunningham, L., Meadors, G. D., Israelian, G., Cuoco, E., Dal Canton, T., Danilishin, S. L., D'Antonio, S., Vo, T., Danzmann, K., Darman, N. S., Altin, P. A., Dattilo, V., Fox, D. B., Dave, I., Budnev, N. M., Meidam, J., Daveloza, H. P., Davier, M., Bock, O., Davies, G. S., Daw, E. J., Day, R., DeBra, D., Debreczeni, G., Degallaix, J., Anderson, S. B., Martynov, D. V., Frieman, J., Melatos, A., Vocca, H., De Laurentis, M., Deléglise, S., Del Pozzo, W., Denker, T., Dent, T., Dereli, H., Dergachev, V., DeRosa, R. T., Gress, O., De Rosa, R., Logue, J., DeSalvo, R., Kozak, D. B., Mendell, G., Fryer, C. L., Anderson, W. G., Dhurandhar, S., Díaz, M. C., Di Fiore, L., Di Giovanni, M., Ivanov, K., Vorvick, C., Di Lieto, A., Di Pace, S., Di Palma, I., Di Virgilio, A., Mendoza-Gandara, D., Dojcinoski, G., Gaztanaga, E., Dolique, V., Arai, K., Donovan, F., DELLA VALLE, Massimo, Poleshuk, V., Dooley, K. L., Doravari, S., Douglas, R., Downes, T. P., Drago, M., Mercer, R. A., Drever, R. W. P., Driggers, J. C., Gerdes, D. W., Voss, D., Du, Z., Tlatov, A., Ducrot, M., Araya, M. C., Dwyer, S. E., Edo, T. B., Edwards, M. C., Effler, A., Neilsen, E., Eggenstein, H. -B., Tucker, D. L., Ehrens, P., Eichholz, J., Cavagliá, M., Brady, P. R., Eikenberry, S. S., Engels, W., Essick, R. C., Arceneaux, C. C., Etzel, T., Evans, M., Vousden, W. D., Merilh, E., Evans, T. M., Everett, R., Yurkov, V., Factourovich, M., Fafone, V., Goldstein, D. A., Fair, H., Fairhurst, S., Fan, X., Vyatchanin, S. P., Fang, Q., Areeda, J. S., Merzougui, M., Farinon, S., Chornock, R., Farr, B., Farr, W. M., Favata, M., Fays, M., Gruen, D., Wade, A. R., Fehrmann, H., Fejer, M. M., Ferrante, I., Ferreira, E. C., Meshkov, S., MASTER Collaboration, Ferrini, F., Arnaud, N., Fidecaro, F., Fiori, I., Wade, L. E., Fiorucci, D., Fisher, R. P., Gruendl, R. A., Flaminio, R., Fletcher, M., Fournier, J. -D., Kawai, N., Messenger, C., Franco, S., Frasca, S., Wade, M., Frasconi, F., Arun, K. G., Frei, Z., Freise, A., Frey, R., Gutierrez, G., Frey, V., Serino, M., Fricke, T. T., Basti, A., Walker, M., Fritschel, P., Frolov, V. V., Fulda, P., Fyffe, M., Gabbard, H. A. G., Ascenzi, S., Gair, J. R., Gammaitoni, L., Marx, J. N., Herner, K., Wallace, L., Gaonkar, S. G., Messick, C., Garufi, F., Gatto, A., Gaur, G., Gehrels, N., Gemme, G., Gendre, B., Genin, E., Negoro, H., Lombardi, A. L., Ashton, G., Gennai, A., Honscheid, K., Kringel, V., Meyers, P. M., George, J., Gergely, L., Germain, V., Ghosh, A., Ghosh, S., ELIAS DE LA ROSA, NANCY DEL CARMEN, Nakahira, S., Giaime, J. A., Giardina, K. D., Giazotto, A., Gill, K., Ast, M., Mezzani, F., James, D. J., Glaefke, A., and Goetz, E.

Abstract

This Supplement provides supporting material for Abbott et al. (2016a). We briefly summarize past electromagnetic (EM) follow-up efforts as well as the organization and policy of the current EM follow-up program. We compare the four probability sky maps produced for the gravitational-wave transient GW150914, and provide additional details of the EM follow-up observations that were performed in the different bands.

Published
2016

34. Eight new Milky Way companions discovered in first-year Dark Energy Survey Data

Author

Des, The Collaboration, Bechtol, K., Drlica-Wagner, A., Balbinot, E., Pieres, A., Simon, J. D., Yanny, B., Santiago, B., Wechsler, R. H., Frieman, J., Walker, A. R., Williams, P., Rozo, E., Rykoff, E. S., Queiroz, A., Luque, E., Benoit-Levy, A., Tucker, D., Sevilla, I., Gruendl, R. A., Da Costa, L. N., Fausti Neto, A., Maia, M. A. G., Abbott, T., Allam, S., Armstrong, R., Bauer, A. H., Bernstein, G. M., Bernstein, R. A., Bertin, E., Brooks, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Castander, F. J., Covarrubias, R., D Andrea, C. B., Depoy, D. L., Desai, S., Diehl, H. T., Eifler, T. F., Estrada, J., August Evrard, Fernandez, E., Finley, D. A., Flaugher, B., Gaztanaga, E., Gerdes, D., Girardi, L., Gladders, M., Gruen, D., Gutierrez, G., Hao, J., Honscheid, K., Jain, B., James, D., Kent, S., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lin, H., Makler, M., March, M., Marshall, J., Martini, P., Merritt, K. W., Miller, C., Miquel, R., Mohr, J., Neilsen, E., Nichol, R., Nord, B., Ogando, R., Peoples, J., Petravick, D., Plazas, A. A., Romer, A. K., Roodman, A., Sako, M., Sanchez, E., Scarpine, V., Schubnell, M., Smith, R. C., Soares-Santos, M., Sobreira, F., Suchyta, E., Swanson, M. E. C., Tarle, G., Thaler, J., Thomas, D., Wester, W., and Zuntz, J.

Subjects
Cosmology and Gravitation, Stellar population, dwarf [galaxies], Milky Way, astro-ph.GA, FOS: Physical sciences, Astrophysics, Galaxia, Astrophysics::Cosmology and Extragalactic Astrophysics, Satellite galaxy, Astrophysics::Solar and Stellar Astrophysics, Eridanus, STFC, Astrophysics::Galaxy Astrophysics, Luminosity function (astronomy), QB, Physics, Aglomerados de galaxias, RCUK, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Stars, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Dark energy, Local Group, Astrophysics::Earth and Planetary Astrophysics
Abstract

We report the discovery of eight new Milky Way companions in ~1,800 deg^2 of optical imaging data collected during the first year of the Dark Energy Survey (DES). Each system is identified as a statistically significant over-density of individual stars consistent with the expected isochrone and luminosity function of an old and metal-poor stellar population. The objects span a wide range of absolute magnitudes (M_V from -2.2 mag to -7.4 mag), physical sizes (10 pc to 170 pc), and heliocentric distances (30 kpc to 330 kpc). Based on the low surface brightnesses, large physical sizes, and/or large Galactocentric distances of these objects, several are likely to be new ultra-faint satellite galaxies of the Milky Way and/or Magellanic Clouds. We introduce a likelihood-based algorithm to search for and characterize stellar over-densities, as well as identify stars with high satellite membership probabilities. We also present completeness estimates for detecting ultra-faint galaxies of varying luminosities, sizes, and heliocentric distances in the first-year DES data., 33 pages, 12 figures, 3 tables. Accepted for publication in ApJ. Readers may be interested in the concurrent work by Koposov, Belokurov, Torrealba, & Evans (http://arxiv.org/abs/1503.02079). Indirect dark matter search results are presented in Drlica-Wagner, Albert, Bechtol, Wood, Strigari, et al. (The LAT and DES Collaborations, http://arxiv.org/abs/1503.02632)

Published
2015

35. The STRong lensing Insights into the Dark Energy Survey (STRIDES) 2016 follow-up campaign – I. Overview and classification of candidates selected by two techniques.

Author

Treu, T, Agnello, A, Baumer, M A, Birrer, S, Buckley-Geer, E J, Courbin, F, Kim, Y J, Lin, H, Marshall, P J, and Nord, B

Subjects
DARK energy, DARK matter, QUASARS, GRAVITATIONAL lenses, GALAXIES
Abstract

The primary goals of the STRong lensing Insights into the Dark Energy Survey (STRIDES) collaboration are to measure the dark energy equation of state parameter and the free streaming length of dark matter. To this aim, STRIDES is discovering strongly lensed quasars in the imaging data of the Dark Energy Survey and following them up to measure time delays, high resolution imaging, and spectroscopy sufficient to construct accurate lens models. In this paper, we first present forecasts for STRIDES. Then, we describe the STRIDES classification scheme, and give an overview of the Fall 2016 follow-up campaign. We continue by detailing the results of two selection methods, the outlier selection technique and a morphological algorithm, and presenting lens models of a system that could possibly be a lensed quasar in an unusual configuration. We conclude with the summary statistics of the Fall 2016 campaign. Including searches presented in companion papers (Anguita et al.; Ostrovski et al.), STRIDES followed up 117 targets identifying 7 new strongly lensed systems, and 7 nearly identical quasars, which could be confirmed as lenses by the detection of the lens galaxy. 76 candidates were rejected and 27 remain otherwise inconclusive, for a success rate in the range of 6–35 per cent. This rate is comparable to that of previous searches like SDSS Quasar Lens Search even though the parent data set of STRIDES is purely photometric and our selection of candidates cannot rely on spectroscopic information. [ABSTRACT FROM AUTHOR]

Published
2018
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36. Effects of Selection and Covariance on X-ray Scaling Relations of Galaxy Clusters

Author

Nord, B., Stanek, R., Rasia, E., and Evrard, A. E.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics
Abstract

We explore how the behavior of galaxy cluster scaling relations are affected by flux-limited selection biases and intrinsic covariance among observable properties. Our models presume log-normal covariance between luminosity (L) and temperature (T) at fixed mass (M), centered on evolving, power-law mean relations as a function of host halo mass. Selection can mimic evolution; the \lm and \lt relations from shallow X-ray flux-limited samples will deviate from mass-limited expectations at nearly all scales while the relations from deep surveys ($10^{-14} \cgsflux$) become complete, and therefore unbiased, at masses above $\sims 2 \times 10^{14} \hinv \msol$. We derive expressions for low-order moments of the luminosity distribution at fixed temperature, and show that the slope and scatter of the \lt relation observed in flux-limited samples is sensitive to the assumed \lt correlation coefficient. In addition, \lt covariance affects the redshift behavior of halo counts and mean luminosity in a manner that is nearly degenerate with intrinsic population evolution., 5pages, 4 Figures, Submitted to MNRAS

Published
2007

37. Generalized Fisher matrices.

Author

Heavens, A. F., Seikel, M., Nord, B. D., Aich, M., Bouffanais, Y., Bassett, B. A., and Hobson, M. P.

Subjects
MATRICES (Mathematics), FISHER information, ERROR analysis in mathematics, SUPERNOVAE, MARKOV processes, ANALYSIS of covariance, PARAMETER estimation
Abstract

The Fisher Information Matrix formalism (Fisher 1935) is extended to cases where the data are divided into two parts (X, Y), where the expectation value of Y depends on X according to some theoretical model, and X and Y both have errors with arbitrary covariance. In the simplest case, (X, Y) represent data pairs of abscissa and ordinate, in which case the analysis deals with the case of data pairs with errors in both coordinates, but X can be any measured quantities on which Y depends. The analysis applies for arbitrary covariance, provided all errors are Gaussian, and provided the errors in X are small, both in comparison with the scale over which the expected signal Y changes, and with the width of the prior distribution. This generalizes the Fisher Matrix approach, which normally only considers errors in the 'ordinate' Y. In this work, we include errors in X by marginalizing over latent variables, effectively employing a Bayesian hierarchical model, and deriving the Fisher Matrix for this more general case. The methods here also extend to likelihood surfaces which are not Gaussian in the parameter space, and so techniques such as DALI (Derivative Approximation for Likelihoods) can be generalized straightforwardly to include arbitrary Gaussian data error covariances. For simple mock data and theoretical models, we compare to Markov Chain Monte Carlo experiments, illustrating the method with cosmological supernova data. We also include the new method in the FISHER4CAST software. [ABSTRACT FROM AUTHOR]

Published
2014
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38. redMaPPer. I. ALGORITHM AND SDSS DR8 CATALOG.

Author

Rykoff, E. S., Rozo, E., Busha, M. T., Cunha, C. E., Finoguenov, A., Evrard, A., Hao, J., Koester, B. P., Leauthaud, A., Nord, B., Pierre, M., Reddick, R., Sadibekova, T., Sheldon, E. S., and Wechsler, R. H.

Subjects
GALAXY clusters, ASTRONOMICAL photometry, GALACTIC redshift, ALGORITHMS, REDSHIFT
Abstract

We describe redMaPPer, a new red sequence cluster finder specifically designed to make optimal use of ongoing and near-future large photometric surveys. The algorithm has multiple attractive features: (1) it can iteratively self-train the red sequence model based on a minimal spectroscopic training sample, an important feature for high-redshift surveys. (2) It can handle complex masks with varying depth. (3) It produces cluster-appropriate random points to enable large-scale structure studies. (4) All clusters are assigned a full redshift probability distribution P(z). (5) Similarly, clusters can have multiple candidate central galaxies, each with corresponding centering probabilities. (6) The algorithm is parallel and numerically efficient: it can run a Dark Energy Survey-like catalog in ∼500 CPU hours. (7) The algorithm exhibits excellent photometric redshift performance, the richness estimates are tightly correlated with external mass proxies, and the completeness and purity of the corresponding catalogs are superb. We apply the redMaPPer algorithm to ∼10, 000 deg2 of SDSS DR8 data and present the resulting catalog of ∼25,000 clusters over the redshift range z ∊ [0.08, 0.55]. The redMaPPer photometric redshifts are nearly Gaussian, with a scatter σz ≈ 0.006 at z ≈ 0.1, increasing to σz ≈ 0.02 at z ≈ 0.5 due to increased photometric noise near the survey limit. The median value for |Δz|/(1 + z) for the full sample is 0.006. The incidence of projection effects is low (⩽5%). Detailed performance comparisons of the redMaPPer DR8 cluster catalog to X-ray and Sunyaev-Zel'dovich catalogs are presented in a companion paper. [ABSTRACT FROM AUTHOR]

Published
2014
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39. A Decam Search for an Optical Counterpart to the Ligo Gravitational-Wave Event Gw151226

Author

Cowperthwaite, Philip Steven, Berger, Edo, Soares-Santos, M., Annis, J., Brout, D., Brown, D. A., Buckley-Geer, E., Cenko, S. B., Chen, H. Y., Chornock, R., Diehl, H. T., Doctor, Z., Drlica-Wagner, A., Drout, M. R., Farr, B., Finley, D. A., Foley, R. J., Fong, W., Fox, D. B., Frieman, J., Garcia-Bellido, J., Gill, M. S. S., Gruendl, R. A., Herner, K., Holz, D. E., Kasen, D., Kessler, R., Lin, H., Margutti, R., Marriner, J., Matheson, T., Metzger, B. D., Neilsen Jr., E. H., Quataert, E., Rest, A., Sako, M., Scolnic, D., Smith, N., Sobreira, F., Strampelli, G. M., Villar, V. A., Walker, A. R., Wester, W., Williams, Preston Noah, Yanny, B., Abbott, T. M. C., Abdalla, F. B., Allam, S., Armstrong, R., Bechtol, K., Benoit-Lévy, A., Bertin, E., Brooks, D., Burke, D. L., Rosell, A. Carnero, Kind, M. Carrasco, Carretero, J., Castander, F. J., Cunha, C. E., D’Andrea, C. B., Costa, L. N. da, Desai, S., Dietrich, J. P., Evrard, A. E., Neto, A. Fausti, Fosalba, P., Gerdes, D. W., Giannantonio, T., Goldstein, D. A., Gruen, D., Gutierrez, G., Honscheid, K., James, D. J., Johnson, M. W. G., Johnson, M. D., Krause, E., Kuehn, K., Kuropatkin, N., Lima, M., Maia, M. A. G., Marshall, J. L., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R., Plazas, A. A., Reil, K., Romer, A. K., Sanchez, E., Scarpine, V., Sevilla-Noarbe, I., Smith, R. C., Suchyta, E., Tarle, G., Thomas, D., Thomas, R. C., Tucker, D. L., and Weller, J.

Subjects
binaries: close, catalogs, gravitational waves, stars: neutron, surveys
Abstract

We report the results of a Dark Energy Camera (DECam) optical follow-up of the gravitational wave (GW) event GW151226, discovered by the Advanced LIGO detectors. Our observations cover 28.8 deg2 of the localization region in the i and z bands (containing 3% of the BAYESTAR localization probability), starting 10 hours after the event was announced and spanning four epochs at 2 −24 days after the GW detection. We achieve 5σ point-source limiting magnitudes of i ≈ 21.7 and z ≈ 21.5, with a scatter of 0.4 mag, in our difference images. Given the two day delay, we search this area for a rapidly declining optical counterpart with & 3σ significance steady decline between the first and final observations. We recover four sources that pass our selection criteria, of which three are cataloged AGN. The fourth source is offset by 5.8 arcsec from the center of a galaxy at a distance of 187 Mpc, exhibits a rapid decline by 0.5 mag over 4 days, and has a red color of i−z ≈ 0.3 mag. These properties could satisfy a set of cuts designed to identify kilonovae. However, this source was detected several times, starting 94 days prior to GW151226, in the Pan-STARRS Survey for Transients (dubbed as PS15cdi) and is therefore unrelated to the GW event. Given its long-term behavior, PS15cdi is likely a Type IIP supernova that transitioned out of its plateau phase during our observations, mimicking a kilonova-like behavior. We comment on the implications of this detection for contamination in future optical follow-up observations., Astronomy

Published
2016
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40. Optical spectroscopy and photometry of SAX J1808.4−3658 in outburst.

Author

Elebert, P., Reynolds, M. T., Callanan, P. J., Hurley, D. J., Ramsay, G., Lewis, F., Russell, D. M., Nord, B., Kane, S. R., DePoy, D. L., and Hakala, P.

Subjects
PULSARS, BINARY stars, OPTICAL spectroscopy, ASTRONOMICAL photometry, NEUTRON stars, BLACK holes, ACCRETION (Astrophysics)
Abstract

We present phase resolved optical spectroscopy and photometry of V4580 Sagittarii, the optical counterpart to the accretion powered millisecond pulsar SAX J1808.4−3658, obtained during the 2008 September/October outburst. Doppler tomography of the N iiiλ4640.64 Bowen blend emission line reveals a focused spot of emission at a location consistent with the secondary star. The velocity of this emission occurs at ; applying a ‘ K-correction’, we find the velocity of the secondary star projected on to the line of sight to be . Based on existing pulse timing measurements, this constrains the mass ratio of the system to be , and the mass function for the pulsar to be . Combining this mass function with various inclination estimates from other authors, we find no evidence to suggest that the neutron star in SAX J1808.4−3658 is more massive than the canonical value of . Our optical light curves exhibit a possible superhump modulation, expected for a system with such a low mass ratio. The equivalent width of the Ca ii H and K interstellar absorption lines suggest that the distance to the source is ∼2.5 kpc. This is consistent with previous distance estimates based on type-I X-ray bursts which assume cosmic abundances of hydrogen, but lower than more recent estimates which assume helium-rich bursts. [ABSTRACT FROM AUTHOR]

Published
2009
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41. The.

Author

Rykoff, E. S., Evrard, A. E., McKay, T. A., Becker, M. R., Johnston, D. E., Koester, B. P., Nord, B., Rozo, E., Sheldon, E. S., Stanek, R., and Wechsler, R. H.

Subjects
X-ray astronomy, X-rays, STELLAR luminosity function, GRAVITATIONAL lenses, MICROLENSING (Astrophysics)
Abstract

We present a new measurement of the scaling relation between X-ray luminosity and total mass for 17 000 galaxy clusters in the maxBCG cluster sample. Stacking subsamples within fixed ranges of optical richness, N200, we measure the mean 0.1–2.4 keV X-ray luminosity, , from the ROSAT All-Sky Survey. The mean mass, , is measured from weak gravitational lensing of SDSS background galaxies. For , the data are well fitted by a power law, . The slope agrees to within 10 per cent with previous estimates based on X-ray selected catalogues, implying that the covariance in and N200 at a fixed halo mass is not large. The luminosity intercept is 30 per cent, or 2σ, lower than that determined from the X-ray flux-limited sample of Reiprich & Böhringer, assuming hydrostatic equilibrium. This slight difference could arise from a combination of Malmquist bias and/or systematic error in hydrostatic mass estimates, both of which are expected. The intercept agrees with that derived by Stanek et al. using a model for the statistical correspondence between clusters and haloes in a WMAP3 cosmology with power spectrum normalization . Similar exercises applied to future data sets will allow constraints on the covariance among optical and hot gas properties of clusters at a fixed mass. [ABSTRACT FROM AUTHOR]

Published
2008
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42. CDF Run IIb Silicon: Design am! Testing.

Author

Lu, R.-S., Akimoto, T., Aoki, M., Hara, K., Kim, S., Azzi, P., Bacchetta, N., Bisello, D., Busetto, G., Cabrera, S., Manea, C., Merkel, P., Pantano, D., Wang, Z., Behari, S., Pursley, J., Maksimovic, P., Schuyler, B., Nord, B., and Benjamin, D.

Subjects
VERTEX detectors, SILICON, NUCLEAR counters, ENGINEERING instruments, RADIOACTIVITY instruments, PROTOTYPES
Abstract

The various generations of Silicon Vertex Detectors (SVX, SVX', SVXII) for Collider Detector at Fermilab (CDF) at the Fermilab Tevatron have been fundamental tools for heavy-flavor tagging via secondary vertex detection. The CDF Run llb Silicon Vertex Detector (SVXIIb) has been designed to be a radiation-tolerant replacement for the currently installed SVXII because SVXII was not expected to survive the Tevatron luminosity anticipated for Run IIb. One major change in the new design is the use of a single mechanical and electrical element throughout the array. This element called a stave, carries six single-sided silicon sensors on each side and is built using carbon fiber skins with a high thermal conductivity on a foam core with a built-In cooling channel. A. Kapton bus cable carries power, data and control signals underneath the silicon sensors on each side of the stave. Sensors are read out in pairs via a ceramic hybrid glued on one of the sensors and equipped with four SVX4 readout chips. This new design concept leads to a very compact mechanical and electrical unit, allowing streamlined production and ease of testing and installation. A description of the design and mechanical performance of the stave is given. Results on the electrical performance obtained using prototype staves are also presented. [ABSTRACT FROM AUTHOR]

Published
2004
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43. Salmonella Isolated from Animals and Feed Production in Sweden Between 1993 and 1997

Author

Tysen E, Noll B, Wahlström H, Hamilton C, Nord Bjerselius U, Hansson I, Boqvist S, and Engvall A

Subjects
animal, cattle, feed, feed production, isolate, poultry, swine, Salmonella, Sweden, Veterinary medicine, SF600-1100
Abstract

This paper presents Salmonella data from animals, feedstuffs and feed mills in Sweden between 1993 and 1997. During that period, 555 isolates were recorded from animals, representing 87 serotypes. Of those, 30 serotypes were found in animals in Sweden for the first time. The majority of all isolates from animals were S. Typhimurium (n = 91), followed by S. Dublin (n = 82). There were 115 isolates from cattle, 21 from broilers, 56 from layers and 18 from swine. The majority of these isolates were from outbreaks, although some were isolated at the surveillance at slaughterhouses. The number of isolates from the feed industry was similar to that of the previous 5-year period. Most of those findings were from dust and scrapings from feed mills, in accordance with the HACCP programme in the feed control programme. It can be concluded that the occurrence of Salmonella in animals and in the feed production in Sweden remained favourable during 1993–97.

Published
2003
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44. IMPACT OF SYSTEMATICS ON SZ-OPTICAL SCALING RELATIONS.

Author

Biesiadzinski, T., McMahon, J., Miller, C. J., Nord, B., and Shaw, L.

Subjects
GALAXY clusters, METAPHYSICAL cosmology, SUNYAEV-Zel'dovich effect, ASTRONOMICAL observations
Abstract

One of the central goals of multi-wavelength galaxy cluster cosmology is to unite all cluster observables to form a consistent understanding of cluster mass. Here, we study the impact of systematic effects from optical cluster catalogs on stacked Sunyaev-Zel'dovich (SZ) signals. We show that the optically predicted Y-decrement can vary by as much as 50% based on the current 2σ systematic uncertainties in the observed mass-richness relationship. Miscentering and impurities will suppress the SZ signal compared to expectations for a clean and perfectly centered optical sample, but to a lesser degree. We show that the levels of these variations and suppression are dependent on the amount of systematics in the optical cluster catalogs. We also study X-ray luminosity-dependent sub-sampling of the optical catalog and find that it creates Malmquist bias, increasing the observed Y-decrement of the stacked signal. We show that the current Planck measurements of the Y-decrement around Sloan Digital Sky Survey optical clusters and their X-ray counterparts are consistent with expectations after accounting for the 1σ optical systematic uncertainties using the Johnston mass-richness relation. [ABSTRACT FROM AUTHOR]

Published
2012
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45. Effects of selection and covariance on X-ray scaling relations of galaxy clusters.

Author

Nord, B., Stanek, R., Rasia, E., and Evrard, A. E.

Subjects
*GALAXY clusters, *SCALING laws (Statistical physics), *STELLAR luminosity function, *RANKING (Statistics), *ANALYSIS of variance, *STATISTICAL physics, *TEMPERATURE effect
Abstract

We explore how the behaviour of galaxy cluster scaling relations are affected by flux-limited selection biases and intrinsic covariance among observable properties. Our models presume log-normal covariance between luminosity ( L) and temperature ( T) at fixed mass ( M), centred on evolving, power-law mean relations as a function of host halo mass. Selection can mimic evolution; the L– M and L– T relations from shallow X-ray flux-limited samples will deviate from mass-limited expectations at nearly all scales while the relations from deep surveys (10−14 erg s−1 cm−2) become complete, and therefore unbiased, at masses above ∼2 × 1014 h−1 M⊙. We derive expressions for low-order moments of the luminosity distribution at fixed temperature, and show that the slope and scatter of the L– T relation observed in flux-limited samples is sensitive to the assumed L– T correlation coefficient. In addition, L– T covariance affects the redshift behaviour of halo counts and mean luminosity in a manner that is nearly degenerate with intrinsic population evolution. [ABSTRACT FROM AUTHOR]

Published
2008
Full Text
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47. DeepZipper II: Searching for Lensed Supernovae in Dark Energy Survey Data with Deep Learning

Author

R. Morgan, B. Nord, K. Bechtol, A. Möller, W. G. Hartley, S. Birrer, S. J. González, M. Martinez, R. A. Gruendl, E. J. Buckley-Geer, A. J. Shajib, A. Carnero Rosell, C. Lidman, T. Collett, T. M. C. Abbott, M. Aguena, F. Andrade-Oliveira, J. Annis, D. Bacon, S. Bocquet, D. Brooks, D. L. Burke, M. Carrasco Kind, J. Carretero, F. J. Castander, C. Conselice, L. N. da Costa, M. Costanzi, J. De Vicente, S. Desai, P. Doel, S. Everett, I. Ferrero, B. Flaugher, D. Friedel, J. Frieman, J. García-Bellido, E. Gaztanaga, D. Gruen, G. Gutierrez, S. R. Hinton, D. L. Hollowood, K. Honscheid, K. Kuehn, N. Kuropatkin, O. Lahav, M. Lima, F. Menanteau, R. Miquel, A. Palmese, F. Paz-Chinchón, M. E. S. Pereira, A. Pieres, A. A. Plazas Malagón, J. Prat, M. Rodriguez-Monroy, A. K. Romer, A. Roodman, E. Sanchez, V. Scarpine, I. Sevilla-Noarbe, M. Smith, E. Suchyta, M. E. C. Swanson, G. Tarle, D. Thomas, T. N. Varga, Morgan, R [0000-0002-7016-5471], Nord, B [0000-0001-6706-8972], Bechtol, K [0000-0001-8156-0429], Möller, A [0000-0001-8211-8608], Birrer, S [0000-0003-3195-5507], González, SJ [0000-0001-7282-3864], Martinez, M [0000-0002-8397-8412], Gruendl, RA [0000-0002-4588-6517], Buckley-Geer, EJ [0000-0002-3304-0733], Shajib, AJ [0000-0002-5558-888X], Rosell, A Carnero [0000-0003-3044-5150], Lidman, C [0000-0003-1731-0497], Collett, T [0000-0001-5564-3140], Aguena, M [0000-0001-5679-6747], Annis, J [0000-0002-0609-3987], Bacon, D [0000-0002-2562-8537], Bocquet, S [0000-0002-4900-805X], Brooks, D [0000-0002-8458-5047], Kind, M Carrasco [0000-0002-4802-3194], Carretero, J [0000-0002-3130-0204], Castander, FJ [0000-0001-7316-4573], Conselice, C [0000-0003-1949-7638], Costanzi, M [0000-0001-8158-1449], De Vicente, J [0000-0001-8318-6813], Desai, S [0000-0002-0466-3288], Flaugher, B [0000-0002-2367-5049], Frieman, J [0000-0003-4079-3263], García-Bellido, J [0000-0002-9370-8360], Gaztanaga, E [0000-0001-9632-0815], Gruen, D [0000-0003-3270-7644], Gutierrez, G [0000-0003-0825-0517], Hinton, SR [0000-0003-2071-9349], Hollowood, DL [0000-0002-9369-4157], Honscheid, K [0000-0002-6550-2023], Kuehn, K [0000-0003-0120-0808], Kuropatkin, N [0000-0003-2511-0946], Lahav, O [0000-0002-1134-9035], Menanteau, F [0000-0002-1372-2534], Miquel, R [0000-0002-6610-4836], Palmese, A [0000-0002-6011-0530], Paz-Chinchón, F [0000-0003-1339-2683], Pieres, A [0000-0001-9186-6042], Malagón, AA Plazas [0000-0002-2598-0514], Romer, AK [0000-0002-9328-879X], Roodman, A [0000-0001-5326-3486], Sanchez, E [0000-0002-9646-8198], Sevilla-Noarbe, I [0000-0002-1831-1953], Smith, M [0000-0002-3321-1432], Suchyta, E [0000-0002-7047-9358], Tarle, G [0000-0003-1704-0781], and Apollo - University of Cambridge Repository

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), FOS: Physical sciences, Física, Astronomy and Astrophysics, 5109 Space Sciences, Basic Behavioral and Social Science, Supernovae, Space and Planetary Science, 5101 Astronomical Sciences, Strong gravitational lensing, Behavioral and Social Science, 7 Affordable and Clean Energy, 51 Physical Sciences, 5107 Particle and High Energy Physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Artículo escrito por un elevado número de autores, solo se referencian el que aparece en primer lugar, el nombre del grupo de colaboración, si le hubiere, y los autores pertenecientes a la UAM, Gravitationally lensed supernovae (LSNe) are important probes of cosmic expansion, but they remain rare and difficult to find. Current cosmic surveys likely contain 5-10 LSNe in total while next-generation experiments are expected to contain several hundred to a few thousand of these systems. We search for these systems in observed Dark Energy Survey (DES) five year SN fields—10 3 sq. deg. regions of sky imaged in the griz bands approximately every six nights over five years. To perform the search, we utilize the DeepZipper approach: a multi-branch deep learning architecture trained on image-level simulations of LSNe that simultaneously learns spatial and temporal relationships from time series of images. We find that our method obtains an LSN recall of 61.13% and a false-positive rate of 0.02% on the DES SN field data. DeepZipper selected 2245 candidates from a magnitude-limited (m i < 22.5) catalog of 3,459,186 systems. We employ human visual inspection to review systems selected by the network and find three candidate LSNe in the DES SN fields, The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016-0597, and MDM-2015-0509, some of which include ERDF funds from the European Union.

Published
2022

48. CMB-S4

Author

Collaboration, The CMB-S4, Abazajian, Kevork, Addison, Graeme E., Adshead, Peter, Ahmed, Zeeshan, Akerib, Daniel, Ali, Aamir, Allen, Steven W., Alonso, David, Alvarez, Marcelo, Amin, Mustafa A., Anderson, Adam, Arnold, Kam S., Ashton, Peter, Baccigalupi, Carlo, Bard, Debbie, Barkats, Denis, Barron, Darcy, Barry, Peter S., Bartlett, James G., Thakur, Ritoban Basu, Battaglia, Nicholas, Bean, Rachel, Bebek, Chris, Bender, Amy N., Benson, Bradford A., Bianchini, Federico, Bischoff, Colin A., Bleem, Lindsey, Bock, James J., Bocquet, Sebastian, Boddy, Kimberly K., Bond, J. Richard, Borrill, Julian, Bouchet, François R., Brinckmann, Thejs, Brown, Michael L., Bryan, Sean, Buza, Victor, Byrum, Karen, Caimapo, Carlos Hervias, Calabrese, Erminia, Calafut, Victoria, Caldwell, Robert, Carlstrom, John E., Carron, Julien, Cecil, Thomas, Challinor, Anthony, Chang, Clarence L., Chinone, Yuji, Cho, Hsiao-Mei Sherry, Cooray, Asantha, Coulton, Will, Crawford, Thomas M., Crites, Abigail, Cukierman, Ari, Cyr-Racine, Francis-Yan, de Haan, Tijmen, Delabrouille, Jacques, Devlin, Mark, Di Valentino, Eleonora, Dierickx, Marion, Dobbs, Matt, Duff, Shannon, Dunkley, Jo, Dvorkin, Cora, Eimer, Joseph, Elleflot, Tucker, Errard, Josquin, Essinger-Hileman, Thomas, Fabbian, Giulio, Feng, Chang, Ferraro, Simone, Filippini, Jeffrey P., Flauger, Raphael, Flaugher, Brenna, Fraisse, Aurelien A., Frolov, Andrei, Galitzki, Nicholas, Gallardo, Patricio A., Galli, Silvia, Ganga, Ken, Gerbino, Martina, Gluscevic, Vera, Goeckner-Wald, Neil, Green, Daniel, Grin, Daniel, Grohs, Evan, Gualtieri, Riccardo, Gudmundsson, Jon E., Gullett, Ian, Gupta, Nikhel, Habib, Salman, Halpern, Mark, Halverson, Nils W., Hanany, Shaul, Harrington, Kathleen, Hasegawa, Masaya, Hasselfield, Matthew, Hazumi, Masashi, Heitmann, Katrin, Henderson, Shawn, Hensley, Brandon, Hill, Charles, Hill, J. Colin, Hlozek, Renée, Ho, Shuay-Pwu Patty, Hoang, Thuong, Holder, Gil, Holzapfel, William, Hood, John, Hubmayr, Johannes, Huffenberger, Kevin M., Hui, Howard, Irwin, Kent, Jeong, Oliver, Johnson, Bradley R., Jones, William C., Kang, Jae Hwan, Karkare, Kirit S., Katayama, Nobuhiko, Keskitalo, Reijo, Kisner, Theodore, Knox, Lloyd, Koopman, Brian J., Kosowsky, Arthur, Kovac, John, Kovetz, Ely D., Kuhlmann, Steve, Kuo, Chao-lin, Kusaka, Akito, Lähteenmäki, Anne, Lawrence, Charles R., Lee, Adrian T., Lewis, Antony, Li, Dale, Linder, Eric, Loverde, Marilena, Lowitz, Amy, Lubin, Phil, Madhavacheril, Mathew S., Mantz, Adam, Marques, Gabriela, Matsuda, Frederick, Mauskopf, Philip, McCarrick, Heather, McMahon, Jeffrey, Meerburg, P. Daniel, Melin, Jean-Baptiste, Menanteau, Felipe, Meyers, Joel, Millea, Marius, Mohr, Joseph, Moncelsi, Lorenzo, Monzani, Maria, Mroczkowski, Tony, Mukherjee, Suvodip, Nagy, Johanna, Namikawa, Toshiya, Nati, Federico, Natoli, Tyler, Newburgh, Laura, Niemack, Michael D., Nishino, Haruki, Nord, Brian, Novosad, Valentine, O'Brient, Roger, Padin, Stephen, Palladino, Steven, Partridge, Bruce, Petravick, Don, Pierpaoli, Elena, Pogosian, Levon, Prabhu, Karthik, Pryke, Clement, Puglisi, Giuseppe, Racine, Benjamin, Rahlin, Alexandra, Rao, Mayuri Sathyanarayana, Raveri, Marco, Reichardt, Christian L., Remazeilles, Mathieu, Rocha, Graca, Roe, Natalie A., Roy, Anirban, Ruhl, John E., Salatino, Maria, Saliwanchik, Benjamin, Schaan, Emmanuel, Schillaci, Alessandro, Schmitt, Benjamin, Schmittfull, Marcel M., Scott, Douglas, Sehgal, Neelima, Shandera, Sarah, Sherwin, Blake D., Shirokoff, Erik, Simon, Sara M., Slosar, Anze, Spergel, David, Germaine, Tyler St., Staggs, Suzanne T., Stark, Antony, Starkman, Glenn D., Stompor, Radek, Stoughton, Chris, Suzuki, Aritoki, Tajima, Osamu, Teply, Grant P., Thompson, Keith, Thorne, Ben, Timbie, Peter, Tomasi, Maurizio, Tristram, Matthieu, Tucker, Gregory, Umiltà, Caterina, van Engelen, Alexander, Vavagiakis, Eve M., Vieira, Joaquin D., Vieregg, Abigail G., Wagoner, Kasey, Wallisch, Benjamin, Wang, Gensheng, Watson, Scott, Westbrook, Ben, Whitehorn, Nathan, Wollack, Edward J., Wu, W. L. Kimmy, Xu, Zhilei, Yang, H. Y. Eric, Yasini, Siavash, Yefremenko, Volodymyr G., Yoon, Ki Won, Young, Edward, Yu, Cyndia, Zonca, Andrea, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), CMB-S4, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris-Sud - Paris 11 (UP11), Apollo - University of Cambridge Repository, Van Swinderen Institute for Particle Physics and G, Cosmic Frontier, Abazajian, K, Addison, G, Adshead, P, Ahmed, Z, Akerib, D, Ali, A, Allen, S, Alonso, D, Alvarez, M, Amin, M, Anderson, A, Arnold, K, Ashton, P, Baccigalupi, C, Bard, D, Barkats, D, Barron, D, Barry, P, Bartlett, J, Basu Thakur, R, Battaglia, N, Bean, R, Bebek, C, Bender, A, Benson, B, Bianchini, F, Bischoff, C, Bleem, L, Bock, J, Bocquet, S, Boddy, K, Richard Bond, J, Borrill, J, Bouchet, F, Brinckmann, T, Brown, M, Bryan, S, Buza, V, Byrum, K, Hervias Caimapo, C, Calabrese, E, Calafut, V, Caldwell, R, Carlstrom, J, Carron, J, Cecil, T, Challinor, A, Chang, C, Chinone, Y, Sherry Cho, H, Cooray, A, Coulton, W, Crawford, T, Crites, A, Cukierman, A, Cyr-Racine, F, De Haan, T, Delabrouille, J, Devlin, M, Di Valentino, E, Dierickx, M, Dobbs, M, Duff, S, Dvorkin, C, Eimer, J, Elleflot, T, Errard, J, Essinger-Hileman, T, Fabbian, G, Feng, C, Ferraro, S, Filippini, J, Flauger, R, Flaugher, B, Fraisse, A, Frolov, A, Galitzki, N, Gallardo, P, Galli, S, Ganga, K, Gerbino, M, Gluscevic, V, Goeckner-Wald, N, Green, D, Grin, D, Grohs, E, Gualtieri, R, Gudmundsson, J, Gullett, I, Gupta, N, Habib, S, Halpern, M, Halverson, N, Hanany, S, Harrington, K, Hasegawa, M, Hasselfield, M, Hazumi, M, Heitmann, K, Henderson, S, Hensley, B, Hill, C, Colin Hill, J, Hlozek, R, Patty Ho, S, Hoang, T, Holder, G, Holzapfel, W, Hood, J, Hubmayr, J, Huffenberger, K, Hui, H, Irwin, K, Jeong, O, Johnson, B, Jones, W, Hwan Kang, J, Karkare, K, Katayama, N, Keskitalo, R, Kisner, T, Knox, L, Koopman, B, Kosowsky, A, Kovac, J, Kovetz, E, Kuhlmann, S, Kuo, C, Kusaka, A, Lahteenmaki, A, Lawrence, C, Lee, A, Lewis, A, Li, D, Linder, E, Loverde, M, Lowitz, A, Lubin, P, Madhavacheril, M, Mantz, A, Marques, G, Matsuda, F, Mauskopf, P, Mccarrick, H, Mcmahon, J, Daniel Meerburg, P, Melin, J, Menanteau, F, Meyers, J, Millea, M, Mohr, J, Moncelsi, L, Monzani, M, Mroczkowski, T, Mukherjee, S, Nagy, J, Namikawa, T, Nati, F, Natoli, T, Newburgh, L, Niemack, M, Nishino, H, Nord, B, Novosad, V, O'Brient, R, Padin, S, Palladino, S, Partridge, B, Petravick, D, Pierpaoli, E, Pogosian, L, Prabhu, K, Pryke, C, Puglisi, G, Racine, B, Rahlin, A, Sathyanarayana Rao, M, Raveri, M, Reichardt, C, Remazeilles, M, Rocha, G, Roe, N, Roy, A, Ruhl, J, Salatino, M, Saliwanchik, B, Schaan, E, Schillaci, A, Schmitt, B, Schmittfull, M, Scott, D, Sehgal, N, Shandera, S, Sherwin, B, Shirokoff, E, Simon, S, Slosar, A, Spergel, D, S, T, Staggs, S, Stark, A, Starkman, G, Stompor, R, Stoughton, C, Suzuki, A, Tajima, O, Teply, G, Thompson, K, Thorne, B, Timbie, P, Tomasi, M, Tristram, M, Tucker, G, Umilta, C, Van Engelen, A, Vavagiakis, E, Vieira, J, Vieregg, A, Wagoner, K, Wallisch, B, Wang, G, Watson, S, Westbrook, B, Whitehorn, N, Wollack, E, Kimmy Wu, W, Xu, Z, Eric Yang, H, Yasini, S, Yefremenko, V, Won Yoon, K, Young, E, Yu, C, Zonca, A, University of California Irvine, Johns Hopkins University, University of Illinois at Urbana-Champaign, SLAC National Accelerator Laboratory, University of California Berkeley, Stanford University, University of Oxford, Rice University, Fermi National Accelerator Laboratory, University of California San Diego, International School for Advanced Studies, Lawrence Berkeley National Laboratory, Harvard University, University of New Mexico, Argonne National Laboratory, Université Paris-Diderot, California Institute of Technology, Cornell University, University of Melbourne, University of Cincinnati, Ludwig Maximilian University of Munich, University of Toronto, UMR7095, Stony Brook University, University of Manchester, Arizona State University, Florida State University, Cardiff University, Dartmouth College, University of Geneva, University of Cambridge, The University of Tokyo, University of Groningen, University of Chicago, University of Pennsylvania, McGill University, National Institute of Standards and Technology, NASA Goddard Space Flight Center, University of Sussex, Princeton University, Simon Fraser University, National Institute for Nuclear Physics, Haverford College, Stockholm University, Case Western Reserve University, University of British Columbia, University of Colorado Boulder, University of Minnesota Twin Cities, University of Michigan, Ann Arbor, Simons Foundation, Columbia University, University of Virginia, University of California Davis, Yale University, University of Pittsburgh, Ben-Gurion University of the Negev, Department of Electronics and Nanoengineering, Jet Propulsion Laboratory, University of California Santa Barbara, Perimeter Institute for Theoretical Physics, Service d'Astrophysique CEA, European Southern Observatory, Washington University St. Louis, University of Milan - Bicocca, University of Southern California, Institute for Advanced Studies, Pennsylvania State University, Brookhaven National Laboratory, Kyoto University, University of Wisconsin-Madison, University of Milano, Université Paris-Saclay, Brown University, Syracuse University, University of California Los Angeles, Aalto-yliopisto, and Aalto University

Subjects
Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cosmology, CMB, Settore FIS/05, Space and Planetary Science, astro-ph.CO, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Galaxies and Cosmology, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

CMB-S4---the next-generation ground-based cosmic microwave background (CMB) experiment---is set to significantly advance the sensitivity of CMB measurements and enhance our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. Among the science cases pursued with CMB-S4, the quest for detecting primordial gravitational waves is a central driver of the experimental design. This work details the development of a forecasting framework that includes a power-spectrum-based semi-analytic projection tool, targeted explicitly towards optimizing constraints on the tensor-to-scalar ratio, $r$, in the presence of Galactic foregrounds and gravitational lensing of the CMB. This framework is unique in its direct use of information from the achieved performance of current Stage 2--3 CMB experiments to robustly forecast the science reach of upcoming CMB-polarization endeavors. The methodology allows for rapid iteration over experimental configurations and offers a flexible way to optimize the design of future experiments given a desired scientific goal. To form a closed-loop process, we couple this semi-analytic tool with map-based validation studies, which allow for the injection of additional complexity and verification of our forecasts with several independent analysis methods. We document multiple rounds of forecasts for CMB-S4 using this process and the resulting establishment of the current reference design of the primordial gravitational-wave component of the Stage-4 experiment, optimized to achieve our science goals of detecting primordial gravitational waves for $r > 0.003$ at greater than $5��$, or, in the absence of a detection, of reaching an upper limit of $r < 0.001$ at $95\%$ CL., 24 pages, 8 figures, 9 tables, submitted to ApJ. arXiv admin note: text overlap with arXiv:1907.04473

Published
2022

49. Dark energy survey year 1 results: Cosmological constraints from cluster abundances and weak lensing

Author

Alex Drlica-Wagner, Dragan Huterer, J. Annis, I. Sevilla-Noarbe, Daniel Scolnic, N. Kuropatkin, Tesla E. Jeltema, F. Paz-Chinchón, K. D. Eckert, T. N. Varga, Brian Nord, Adam Mantz, L. N. da Costa, M. Costanzi, M. A. G. Maia, Michel Aguena, E. Suchyta, August E. Evrard, Brian Yanny, Shantanu Desai, A. Alarcon, M. W. G. Johnson, A. K. Romer, J. Carretero, Paul Martini, V. Scarpine, I. Ferrero, Matt J. Jarvis, Tamara M. Davis, Yanxi Zhang, Tim Eifler, Arya Farahi, David James, Z. Zhang, D. W. Gerdes, Joshua A. Frieman, D. Gruen, R. Cawthon, Antonella Palmese, Pablo Fosalba, Carlos Solans Sanchez, D. H. Brooks, A. R. Walker, B. Flaugher, Risa H. Wechsler, P. Rooney, Keith Bechtol, M. Sako, C. Lidman, A. von der Linden, Erin Sheldon, D. L. Hollowood, M. E. C. Swanson, Huan Lin, Sebastian Bocquet, Julian A. Mayers, Steve Kent, J. De Vicente, Martin Crocce, R. D. Wilkinson, D. L. Burke, Daniel Thomas, E. Buckley-Geer, M. Carrasco Kind, S. Everett, Robert C. Nichol, S. Allam, Robert A. Gruendl, R. L. C. Ogando, J. P. Dietrich, Juan Garcia-Bellido, E. Bertin, Marcos Lima, Michael Troxel, Eduardo Rozo, Jack Elvin-Poole, Enrique Gaztanaga, Peter Doel, Peter Melchior, Ofer Lahav, M. Smith, H. T. Diehl, Douglas L. Tucker, Kyler Kuehn, J. Allyn Smith, Paul Giles, David Bacon, Niall MacCrann, Ami Choi, Ben Hoyle, A. Roodman, Markus Rau, Tommaso Giannantonio, J. Gschwend, Gary Bernstein, Hao-Yi Wu, Tenglin Li, Scott Dodelson, S. W. Allen, Santiago Avila, Chihway Chang, M. D. Johnson, Ramon Miquel, A. Bermeo, Elisabeth Krause, Sebastian Grandis, J. Mena-Fernández, Joe Zuntz, Jochen Weller, F. J. Castander, T. M. C. Abbott, Chun-Hao To, E. J. Sanchez, K. Honscheid, Eli S. Rykoff, Richard G. Kron, A. Carnero Rosell, Felipe Menanteau, S. Samuroff, Gregory Tarle, Santiago Serrano, J. DeRose, D. J. Brout, J. Prat, Samuel Hinton, G. Gutierrez, Xi Chen, A. A. Plazas, Sunayana Bhargava, Joseph J. Mohr, A. Saro, Jennifer L. Marshall, W. G. Hartley, M. Gatti, Juan Estrada, Michael Schubnell, Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, European Commission, European Research Council, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), DES, UAM. Departamento de Física Teórica, Abbott, T. M. C., Aguena, M., Alarcon, A., Allam, S., Allen, S., Annis, J., Avila, S., Bacon, D., Bechtol, K., Bermeo, A., Bernstein, G. M., Bertin, E., Bhargava, S., Bocquet, S., Brooks, D., Brout, D., Buckley-Geer, E., Burke, D. L., Carnero Rosell, A., Carrasco Kind, M., Carretero, J., Castander, F. J., Cawthon, R., Chang, C., Chen, X., Choi, A., Costanzi, M., Crocce, M., Da Costa, L. N., Davis, T. M., De Vicente, J., Derose, J., Desai, S., Diehl, H. T., Dietrich, J. P., Dodelson, S., Doel, P., Drlica-Wagner, A., Eckert, K., Eifler, T. F., Elvin-Poole, J., Estrada, J., Everett, S., Evrard, A. E., Farahi, A., Ferrero, I., Flaugher, B., Fosalba, P., Frieman, J., Garcia-Bellido, J., Gatti, M., Gaztanaga, E., Gerdes, D. W., Giannantonio, T., Giles, P., Grandis, S., Gruen, D., Gruendl, R. A., Gschwend, J., Gutierrez, G., Hartley, W. G., Hinton, S. R., Hollowood, D. L., Honscheid, K., Hoyle, B., Huterer, D., James, D. J., Jarvis, M., Jeltema, T., Johnson, M. W. G., Johnson, M. D., Kent, S., Krause, E., Kron, R., Kuehn, K., Kuropatkin, N., Lahav, O., Li, T. S., Lidman, C., Lima, M., Lin, H., Maccrann, N., Maia, M. A. G., Mantz, A., Marshall, J. L., Martini, P., Mayers, J., Melchior, P., Mena-Fernandez, J., Menanteau, F., Miquel, R., Mohr, J. J., Nichol, R. C., Nord, B., Ogando, R. L. C., Palmese, A., Paz-Chinchon, F., Plazas, A. A., Prat, J., Rau, M. M., Romer, A. K., Roodman, A., Rooney, P., Rozo, E., Rykoff, E. S., Sako, M., Samuroff, S., Sanchez, C., Sanchez, E., Saro, A., Scarpine, V., Schubnell, M., Scolnic, D., Serrano, S., Sevilla-Noarbe, I., Sheldon, E., Smith, J. A., Smith, M., Suchyta, E., Swanson, M. E. C., Tarle, G., Thomas, D., To, C., Troxel, M. A., Tucker, D. L., Varga, T. N., Von Der Linden, A., Walker, A. R., Wechsler, R. H., Weller, J., Wilkinson, R. D., Wu, H., Yanny, B., Zhang, Y., Zhang, Z., and Zuntz, J.

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Software_OPERATINGSYSTEMS, ComputingMethodologies_SIMULATIONANDMODELING, Cosmic microwave background, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Data_CODINGANDINFORMATIONTHEORY, 01 natural sciences, XMM-Newton Telescope, symbols.namesake, 0103 physical sciences, Hardware_INTEGRATEDCIRCUITS, Planck, 010303 astronomy & astrophysics, Weak gravitational lensing, Galaxy cluster, Physics, 010308 nuclear & particles physics, Física, ComputerSystemsOrganization_PROCESSORARCHITECTURES, Galaxies, Cosmos, Redshift, Galaxy, Cosmology, Dark energy, symbols, Baryon acoustic oscillations, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DES Collaboration: et al., We perform a joint analysis of the counts and weak lensing signal of redMaPPer clusters selected from the Dark Energy Survey (DES) Year 1 dataset. Our analysis uses the same shear and source photometric redshifts estimates as were used in the DES combined probes analysis. Our analysis results in surprisingly low values for S8=σ8(Ωm/0.3)0.5=0.65±0.04, driven by a low matter density parameter, Ωm=0.179+0.031−0.038, with σ8−Ωm posteriors in 2.4σ tension with the DES Y1 3x2pt results, and in 5.6σ with the Planck CMB analysis. These results include the impact of post-unblinding changes to the analysis, which did not improve the level of consistency with other data sets compared to the results obtained at the unblinding. The fact that multiple cosmological probes (supernovae, baryon acoustic oscillations, cosmic shear, galaxy clustering and CMB anisotropies), and other galaxy cluster analyses all favor significantly higher matter densities suggests the presence of systematic errors in the data or an incomplete modeling of the relevant physics. Cross checks with x-ray and microwave data, as well as independent constraints on the observable-mass relation from Sunyaev-Zeldovich selected clusters, suggest that the discrepancy resides in our modeling of the weak lensing signal rather than the cluster abundance. Repeating our analysis using a higher richness threshold (λ≥30) significantly reduces the tension with other probes, and points to one or more richness-dependent effects not captured by our model., The DES data management system is supported by the National Science Foundation under Grants No. AST-1138766 and No. AST-1536171. The DES participants from Spanish institutions are partially supported by MINECO under Grants No. AYA2015-71825, No. ESP2015-66861, No. FPA2015-68048, No. SEV2016-0588, No. SEV-2016-0597, and No. MDM-2015-0509, some of which include ERDF funds from the European Union. I. F. A. E. is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Program (FP7/2007-2013) including ERC Grant agreements No. 240672, No. 291329, and No. 306478. We acknowledge support from the Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO), through Project No. CE110001020. This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DEAC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics. The United States Government retains and the publisher, by accepting the article for publication, acknowledges that the United States Government retains a non-exclusive, paid-up, irrevocable, world-wide license to publish or reproduce the published form of this manuscript, or allow others to do so, for United States Government purposes. M. C. and A. S. are supported by the ERC-StG “ClustersXCosmo” Grant agreement No. 716762. A. S. is supported by the FAREMIUR grant “ClustersXEuclid”. E. R. was supported by the DOE Grant No. DE-SC0015975, by the Sloan Foundation, Grant No. FG-2016-6443, and the Cottrell Scholar program of the Research Corporation for Science Advancement. This research used simulations that were performed resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DEAC02-05CH11231.

Published
2020

50. Effect of desensitization in solid organ transplant recipients depends on some cytokines genes polymorphism.

Author

Lobashevsky, A. L., Manwaring, J. E., Travis, M. M., Nord, B. L., Higgins, N. G., Serov, Y. A., Arnoff, T. S., Hommel-Berrey, G. A., Goggins, W. C., Taber, T. E., Carter Sr., C. B., Smith, D. S., Wozniak, T. C., O'Donnell, J. A., and Turrentine, M. W.

Subjects
*DESENSITIZATION (Psychotherapy), *TRANSPLANTATION of organs, tissues, etc., *CYTOKINES, *GENETIC polymorphisms, *IMMUNOGLOBULINS, *IMMUNE response
Abstract

Desensitization (DS) is widely used to decrease PRA in solid organs transplant candidates (IC). Various numbers of cycles of DS are required to reduce or eliminate donor specific antibodies (DSA). The goal of this study was to investigate if there was a correlation between polymorphism (PM) of some cytokine genes and intensity of DS required to make the recipient/donor cross match compatible. Thirty-one TCs were included in the study. Antibody specificity, percent of reactive antibodies (PRA) and serum concentration of cytokines were analyzed using the LUMINEX platform. PCR-SSP method was used for lL-1α, lL-1β, IL-IR, IL-1Rα, IL-4Rα, lL-12, lFNγ, TGFβ1, TNFα, IL-2, IL-4, IL-6 and IL-10 gene PM analysis. Significant relationship between PM of genes encoding IL-4Rα, IFNγ and IL-12 (p70) and susceptibility to DS was demonstrated (p = 0.04, p = 0.01 and p = 0.05 respectively). Correlation between elevated serum level of IL-12 (p70) and A/A or C/A genotype at -1188 position was found in resistant to DS TCs (p = 0.015). These results indicate that analysis PM of genes encoding IL-4Rα, IFNγ and IL-12 enables to define the DS strategy in TCs more accurately regarding the number of plasmapheresis (PP) cycles and dose of intravenous immunoglobulin (IVIG). [ABSTRACT FROM AUTHOR]

Published
2009
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