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973 results on '"Particle Physics and Astrophysics"'

1. Strategies and performance of the CMS silicon tracker alignment during LHC Run 2

Author: Yerevan Physics Institute, Yerevan, Tumasyan Institut für Hochenergiephysik, Armenia A., Vienna, Adam, Austria W., Andrejkovic, J. W., Bergauer, T., Blöch, D., Chatterjee, S., Dragicevic, M., Escalante Del Valle, A., Frühwirth1, R., Hinger, V., Jeitler1, M., Krammer, N., Lechner, L., Liko, D., Mikulec, I., Paulitsch, P., Pitters, F. M., Schieck1, J., Schöfbeck, R., Schwarz, D., Steininger, H., Templ, S., Waltenberger, W., Wulz1 Institute for Nuclear Problems, C. -E., Minsk, Chekhovsky, Belarus V., Litomin, A., Makarenko Universiteit Antwerpen, V., Antwerpen, Beaumont, Belgium W., Darwish2, M. R., De Wolf, E. A., Janssen, T., Kello3, T., Lelek, A., Rejeb Sfar, H., Van Mechelen, P., Van Putte, S., Van Remortel Vrije Universiteit Brussel, N., Brussel, Blekman, Belgium F., Bols, E. S., D’Hondt, J., Delcourt, M., El Faham, H., Lowette, S., Moortgat, S., Morton, A., Muller, D., Sahasransu, A. R., Tavernier, S., Van Doninck, W., Van Mulders Université Libre de Bruxelles, P., Bruxelles, Allard, Belgium Y., Beghin, D., Bilin, B., Clerbaux, B., De Lentdecker, G., Deng, W., Favart, L., Grebenyuk, A., Hohov, D., Kalsi, A. K., Khalilzadeh, A., Lee, K., Mahdavikhorrami, M., Makarenko, I., Moureaux, L., Pétré, L., Popov, A., Postiau, N., Robert, F., Song, Z., Starling, E., Thomas, L., Vanden Bemden, M., Vander Velde, C., Vanlaer, P., Vannerom, D., Wezenbeek, L., Yang Ghent University, Y., Ghent, Cornelis, Belgium T., Dobur, D., Knolle, J., Lambrecht, L., Mestdach, G., Niedziela, M., Roskas, C., Samalan, A., Skovpen, K., Tytgat, M., Ver- massen, B., Vit Université Catholique de Louvain, M., Louvain-la-Neuve, Benecke, Belgium A., Bethani, A., Bruno, G., Bury, F., Caputo, C., David, P., Deblaere, A., Delaere, C., Donertas, I. S., Giammanco, A., Jaffel, K., Jain, Sa., Lemaitre, V., Mondal, K., Prisciandaro, J., Szilasi, N., Taliercio, A., Teklishyn, M., Tran, T. T., Vischia, P., Wertz Centro Brasileiro de Pesquisas Fisicas, S., Rio de Janeiro, Alves, Brazil G. A., Hensel, C., Moraes Universidade do Estado do Rio de Janeiro, A., Aldá Júnior, Brazil W. L., Alves Gallo Pereira, M., Barroso Ferreira Filho, M., Brandao Malbouisson, H., Carvalho, W., Chinellato4, J., Da Costa, E. M., Da Silveira5, G. G., De Jesus Damiao, D., Fonseca De Souza, S., Matos Figueiredo, D., Mora Herrera, C., Mota Amarilo, K., Mundim, L., Nogima, H., Rebello Teles, P., Santoro, A., Silva Do Amaral, S. M., Sznajder, A., Thiel, M., Torres Da Silva De Araujo6, F., Vilela Pereira Universidade Estadual Paulista (a), A., Universidade Federal do ABC (b), São, Paulo, Bernardes5, Brazil C. A., Calligaris, L., Fernandez Perez Tomei, T. R., Gre- gores, E. M., Lemos, D. S., Mercadante, P. G., Novaes, S. F., and Methods in Physics Research, Sandra S. Padula 36 The CMS Collaboration Nuclear Inst., A 1037 (2022) 166795 Institute for Nuclear Research and Nuclear Energy, Bulgarian Academy of Sciences, Sofia, Aleksandrov, Bulgaria A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Rodozov, M., Shopova, M., Sultanov University of Sofia, G., Dimitrov, Bulgaria A., Ivanov, T., Litov, L., Pavlov, B., Petkov, P., Petrov Beihang University, A., Beijing, Cheng, China T., Javaid7, T., Mittal, M., Wang3, H., Yuan Department of Physics, L., Tsinghua, University, Ahmad, China M., Bauer, G., Dozen8, C., Hu, Z., Martins9, J., Wang, Y., Yi10, K., 11 Institute of High Energy Physics, Chapon, China E., Chen7, G. M., Chen7, H. S., Chen, M., Iemmi, F., Kapoor, A., Leggat, D., Liao, H., Liu7, Z. -A., Milosevic, V., Monti, F., Sharma, R., Tao, J., Thomas-Wilsker, J., Wang, J., Zhang, H., Zhao State Key Laboratory of Nuclear Physics and Technology, J., Peking Uni- versity, Agapitos, China A., An, Y., Ban, Y., Chen, C., Levin, A., Li, Q., Lyu, X., Mao, Y., Qian, S. J., Wang, D., Xiao Sun Yat-Sen University, Q. Wang12 J., Guangzhou, China M., Lu, You Institute of Modern Physics and Key Laboratory of Nuclear Physics and Ion-beam Application (MOE) - Fudan University, Z., Shanghai, Gao3, China X., Okawa Zhejiang University, H., Hangzhou, China, Zhejiang, Lin, China Z., Xiao Universidad de Los Andes, M., Bogota, Avila, Colombia C., Cabrera, A., Florez, C., Fraga Universidad de Antioquia, J., Medellin, Mejia Guisao, Colombia J., Ramirez, F., Ruiz Alvarez, J. D., Salazar González University of Split, C. A., Faculty of Electrical Engineering, Mechanical Engi- neering and Naval Architecture, Split, Giljanovic, Croatia D., Godinovic, N., Lelas, D., Puljak University of Split, I., Faculty of Science, Antunovic, Croatia Z., Kovac, M., Sculac Institute Rudjer Boskovic, T., Zagreb, Brigljevic, Croatia V., Ferencek, D., Majumder, D., Mishra, S., Roguljic, M., Starodumov13, A., Susa University of Cyprus, T., Nicosia, Attikis, Cyprus A., Christoforou, K., Erodotou, E., Ioannou, A., Kole, G., Kolosova, M., Konstantinou, S., Mousa, J., Nicolaou, C., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka Charles University, H., Prague, Finger14, Czech Republic M., M. Finger Jr., 14, Kveton Escuela Politecnica Nacional, A., Quito, Ayala Universidad San Francisco de Quito, Ecuador E., Carrera Jarrin Academy of Scientific Research and Technology of the Arab Republic of Egypt, Ecuador E., Egyptian Network of High Energy Physics, Cairo, Abdalla15, Egypt H., Assran16, Y., 17 Center for High Energy Physics (CHEP-FU), Fayoum, University, El-, Fayoum, Mahmoud, Egypt M. A., Mohammed National Institute of Chemical Physics and Biophysics, Y., Tallinn, Ahmed18, Estonia I., Bhowmik, S., Dewanjee, R. K., Ehataht, K., Kadastik, M., Nandan, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken Department of Physics, C., University of Helsinki, Helsinki, Eerola, Finland P., Forthomme, L., Kirschenmann, H., Osterberg, K., Vouti- lainen Helsinki Institute of Physics, M., Bharthuar, Finland S., Brücken, E., Garcia, F., Havukainen, J., Kim, M. S., Kinnunen, R., Lampén, T., Lassila-Perini, K., Lehti, S., Lindén, T., Lotti, M., Martikainen, L., Myllymäki, M., Ott, J., Siikonen, H., Tuominen, E., Tuominiemi Lappeenranta University of Technology, J., Lappeenranta, Luukka, Finland P., Petrow, H., Tuuva IRFU, T., Cea, Université, Paris-Saclay, Gif-sur-Yvette, Amendola, France C., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Givernaud, A., Gras, P., Hamel de Monchenault, G., Jarry, P., Lenzi, B., Locci, E., Malcles, J., Rander, J., Rosowsky, A., Sahin, M. Ö., Savoy-Navarro19, A., Titov, M., Yu Laboratoire Leprince-Ringuet, G. B., Cnrs/in2p3, Ecole, Polytechnique, Insti- tut Polytechnique de Paris, Palaiseau, Ahuja, France S., Beaudette, F., Bonanomi, M., Buchot Perraguin, A., Busson, P., Cappati, A., Charlot, C., Davignon, O., Diab, B., Falmagne, G., Ghosh, S., Granier de Cassagnac, R., Hakimi, A., Kucher, I., Motta, J., Nguyen, M., Ochando, C., Paganini, P., Rembser, J., Salerno, R., Sarkar, U., Sauvan, J. B., Sirois, Y., Tarabini, A., Zabi, A., Zghiche Université de Strasbourg, A., Cnrs, IPHC UMR 7178, Strasbourg, Agram20, France J. -L., Andrea, J., Apparu, D., Bloch, D., Bonnin, C., Bourgatte, G., Brom, J. -M., Chabert, E. C., Charles, L., Collard, C., Dangelser, E., Darej, D., Fontaine20, J. -C., Goerlach, U., Grimault, C., Gross, L., Haas, C., Krauth, M., Le Bihan, A. -C., Nibigira, E., Ollivier-henry, N., Silva Jiménez, E., Van Hove Institut de Physique des 2 Infinis de Lyon (IP2I ), P., Villeurbanne, Asilar, France E., Baulieu, G., Beauceron, S., Bernet, C., Boudoul, G., Camen, C., Caponetto, L., Carle, A., Chanon, N., Contardo, D., Dené, P., Depasse, P., Dupasquier, T., El Mamouni, H., Fay, J., Galbit, G., Gascon, S., Gouze- vitch, M., Ille, B., Laktineh, I. B., Lattaud, H., Lesauvage, A., Lethuillier, M., Lumb, N., Mirabito, L., Nodari, B., Perries, S., Shchablo, K., Sordini, V., Torterotot, L., Touquet, G., Vander Donckt, M., Viret Georgian Technical University, S., Tbilisi, Lomidze, Georgia I., Toriashvili21, T., Tsamalaidze14 RWTH Aachen University, Z., Physikalisches Institut, I., Aachen, Autermann, Germany C., Botta, V., Feld, L., Karpinski, W., Kiesel, M. K., Klein, K., Lipinski, M., Louis, D., Meuser, D., Pauls, A., Pierschel, G., Rauch, M. P., Röwert, N., Schomakers, C., Schulz, J., Teroerde, M., Wlochal RWTH Aachen University, M., Physikalisches Institut A, Iii., Dodonova, Ger- many A., Eliseev, D., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Mastrolorenzo, L., and Methods in Physics Research, M. 37 The CMS Collaboration Nuclear Inst., A 1037 (2022) 166795 Merschmeyer, Meyer, A., Mocellin, G., Mondal, S., Mukherjee, S., Noll, D., Novak, A., Pook, T., Pozdnyakov, A., Rath, Y., Reithler, H., Roemer, J., Schmidt, A., Schuler, S. C., Sharma, A., Vigilante, L., Wiedenbeck, S., Zaleski RWTH Aachen University, S., Physikalisches Institut B, Iii., Dziwok, Ger- many C., Flügge, G., Haj Ahmad22, W., Hlushchenko, O., Kress, T., Nowack, A., Pistone, C., Pooth, O., Roy, D., Sert, H., Stahl18, A., Ziemons, T., Zotz Deutsches Elektronen-Synchrotron, A., Hamburg, Aarup Petersen, Germany H., Aldaya Martin, M., Asmuss, P., Baxter, S., Bayat- makou, M., Behnke, O., Bermúdez Martínez, A., Bertsche, D., Bhattacharya, S., Bin Anuar, A. A., Borras23, K., Brunner, D., Campbell, A., Cardini, A., Cheng, C., Colombina, F., Consuegra Rodríguez, S., Correia Silva, G., Danilov, V., De Silva, M., Didukh, L., Domínguez Damiani, D., Eckerlin, G., Eckstein, D., Estevez Banos, L. I., Filatov, O., Gallo24, E., Geiser, A., Giraldi, A., Grados Luyando, J. M., Grohsjean, A., Guthoff, M., Jafari25, A., Jomhari, N. Z., Jung, H., Kasem23, A., Kasemann, M., Kaveh, H., Kleinwort, C., Krücker, D., Lange, W., Lidrych, J., Lipka, K., Lohmann26, W., Mankel, R., Maser, H., Melzer-Pellmann, I. -A., Mendizabal Morentin, M., Metwally, J., Meyer, A. B., Meyer, M., Mittag, G., Mnich, J., Muhl, C., Mussgiller, A., Otarid, Y., Pérez Adán, D., Pitzl, D., Raspereza, A., Reichelt, O., Ribeiro Lopes, B., Rübenach, J., Saggio, A., Saibel, A., Savitskyi, M., Scham27, M., Scheurer, V., Schütze, P., Schwanenberger24, C., Shchedrolosiev, M., Shevchenko, R., Sosa Ricardo, R. E., Stafford, D., Stever, R., Tonon, N., Van De Klundert, M., Velyka, A., Walsh, R., Walter, D., Wen, Y., Wichmann, K., Wiens, L., Wissing, C., Wuchterl, S., Zuber University of Hamburg, A., Aggleton, Germany R., Albrecht, S., Bein, S., Benato, L., Biskop, H., Buhmann, P., Connor, P., De Leo, K., Eich, M., Feindt, F., Fröhlich, A., Garbers, C., Garutti, E., Gunnellini, P., Hajheidari, M., Haller, J., Hinzmann, A., Jabusch, H. R., Kasieczka, G., Klanner, R., Kogler, R., Kramer, T., Kutzner, V., Lange, J., Lange, T., Lobanov, A., Malara, A., Martens, S., Mrowietz, M., Niemeyer, C. E. N., Nigamova, A., Nissan, Y., Pena Rodriguez, K. J., Rieger, O., Schleper, P., Schröder, M., Schwandt, J., Sonneveld, J., Stadie, H., Steinbrück, G., Tews, A., Vormwald, B., Wellhausen, J., Zoi Karlsruher Institut fuer Technologie, I., Karlsruhe, Ardila-Perez, Germany L. E., Balzer, M., Barvich, T., Bechtel, J., Blank, T., Brom- mer, S., Burkart, M., Butz, E., Caselle, M., Caspart, R., Chwalek, T., De Boer†, W., Dierlamm, A., Droll, A., El Morabit, K., Faltermann, N., Giffels, M., Gosewisch, J. o., Gottmann, A., Hartmann18, F., Heidecker, C., Husemann, U., Keicher, P., Koppenhofer, R., Maier, S., Metzler, M., Mitra, S., Müller, Th., Neufeld, M., Neukum, M., Nürnberg, A., Quast, G., Rabbertz, K., Rauser, J., Sander, O., Savoiu, D., Schell, D., Schnepf, M., Seith, D., Shvetsov, I., Simonis, H. J., Stanulla, J., Steck, P., Ulrich, R., Van Der Linden, J., Von Cube, R. F., Wassmer, M., Weber, M., Weddigen, A., Wieland, S., Wittig, F., Wolf, R., Wozniewski, S., Wunsch Institute of Nuclear and Particle Physics (INPP), S., Ncsr, Demokritos, Aghia, Paraskevi, Anagnostou, Greece G., Assiouras, P., Daskalakis, G., Geralis, T., Kazas, I., Kyriakis, A., Loukas, D., Papadopoulos, A., Stakia National and Kapodistrian University of Athens, A., Athens, Diamantopoulou, Greece M., Karasavvas, D., Karathanasis, G., Kontaxakis, P., Koraka, C. K., Manousakis-Katsikakis, A., Panagiotou, A., Papavergou, I., Saoulidou, N., Theofilatos, K., Tziaferi, E., Vellidis, K., Vourliotis National Technical University of Athens, E., Bakas, Greece G., Kousouris, K., Papakrivopoulos, I., Tsipolitis, G., Zacharopoulou, A., Zografos University of Ioánnina, A., Ioánnina, Adamidis, Greece K., Bestintzanos, I., Evangelou, I., Foudas, C., Gianneios, P., Katsoulis, P., Kokkas, P., Manthos, N., Papadopoulos, I., Strologas MTA-ELTE Lendület CMS Particle and Nuclear Physics Group, J., Eötvös Loránd University, Budapest, Csanad, Hungary M., Farkas, K., Gadallah28, M. M. A., Lökös29, S., Major, P., Mandal, K., Mehta, A., Pasztor, G., Rd ́l, A. J., Surányi, O., Veres Wigner Research Centre for Physics, G. I., Balazs, Hungary T., Bartók30, M., Bencze, G., Hajdu, C., Horvath31, D., Márton, K., Sikler, F., Veszpremi Institute of Nuclear Research ATOMKI, V., Debrecen, Czellar, Hungary S., Karancsi30, J., Molnar, J., Szillasi, Z., Teyssier Institute of Physics, D., University of Debrecen, Raics, Hungary P., Trocsanyi32, Z. L., Ujvari Karoly Robert Campus, B., MATE Institute of Technology, Gyongyos, Csorgo33, Hun- gary T., Nemes33, F., Novak Indian Institute of Science (IISc), T., Bangalore, Choudhury, India S., Komaragiri, J. R., Kumar, D., Panwar, L., Tiwari National Institute of Science Education and Research, P. C., Hbni, Bhubaneswar, Bahinipati34, India S., Das, A. K., Kar, C., Mal, P., Mishra, T., Mohanty, R., Muraleedharan Nair Bindhu35, V. K., Nayak35, A., Saha, P., Sur, N., Swain, S. K., Vats35 Punjab University, D., Chandigarh, Bansal, India S., Beri, S. B., Bhatnagar, V., Chaudhary, G., Chauhan, S., Dhingra36, N., Gupta, R., Kaur, A., Kaur, M., Kaur, S., Kumari, P., Meena, M., Sandeep, K., Singh, J. B., Virdi University of Delhi, A. K., Delhi, Ahmed, India A., Bhardwaj, A., Choudhary, B. C., Gola, M., Jain, C., Jain, G., Keshri, S., Kumar, A., Naimuddin, M., Priyanka, P., Ranjan, K., Saumya, S., Shah Saha Institute of Nuclear Physics, A., Hbni, Kolkata, Bharti37, India M., Bhattacharya, R., Bhowmik, D., Dutta, S., Gomber38, B., Maity39, M., Palit, P., Rout, P. K., Saha, G., Sahu, B., Sarkar, S., Sharan, M., Singh37, B., Thakur37 Indian Institute of Technology Madras, S., Madras, Behera, India P. K., Behera, S. C., Kalbhor, P., Muhammad, A., Pradhan, R., Pujahari, P. R., Sikdar Bhabha Atomic Research Centre, A. K., Mumbai, Dutta, India D., Jha, V., Kumar, V., Mishra, D. K., Naskar40, K., Netrakanti, P. K., Pant, L. M., Shukla Tata Institute of Fundamental Research-A, P., Aziz, India T., Dugad, S., Kumar Tata Institute of Fundamental Research-B, M., Banerjee, India S., Chudasama, R., Guchait, M., Karmakar, S., Kumar, S., Majumder, G., Mazumdar, K., Mukherjee Indian Institute of Science Education and Research (IISER), S., Pune, Alpana, India K., Dube, S., Kansal, B., Laha, A., Pandey, S., Rane, A., Rastogi, A., and Methods in Physics Research, S. Sharma 38 The CMS Collaboration Nuclear Inst., A 1037 (2022) 166795 Isfahan University of Technology, Isfahan, Bakhshiansohi12, Iran H., Khazaie, E., Zeinali41 Institute for Research in Fundamental Sciences (IPM), M., Tehran, Abbas, Iran S. M., Chenarani42, S., Etesami, S. M., Khakzad, M., Mohammadi Najafabadi University College Dublin, M., Dublin, Bari, Italy, Bari, Ramos, D., Bologna, Italy, Bologna, Lo Meoa, S., Grosso, G., Lusiani, E., Pavia, Italy, Pavia, Perugia, Italy, Peru-, Gia, Baldinelli, G., Bianchi, F., Magherinib, M., Pisa, Italy, Italy, Albergo, S., Costa, S., Di Mattia, A., Saizu, M. A., Tricomi, A., Tuve, C., Potenza, R., Catania, Italy, Manca, Mandorli, G., Massa, M., Mazzoni, E., Messineo, A., Scrib- anoa, A., Firenze, Italy, Firenze, Frascati, Benussi, Italy L., Bianco, S., Genova, Italy, Gen-, Ova, Milano, Italy, Milano, Boldrini, G., Pinolini, B. S., Napoli, Italy, Potenza, Italy, Padova, Italy, Trento, Beccherle, R., Rome, Italy, Rome, Torino, Italy, Novara, Coli, S., Rivettia, A., Trieste, Italy, Trieste, Daegu, Dogra, Korea S., Huh, C., Kim, B., Kim, D. H., Kim, G. N., Kim, J., Lee, J., Lee, S. W., Moon, C. S., Y. D., Oh, Pak, S. I., Radburn-Smith, B. C., Sekmen, S., Yang Chonnam National University, Y. C., Institute for Universe and Elementary Particles, Kwangju, Kim, Korea H., D’Amantea, V., Di Domenicoa, M. R., D, A 1037 (2022) 166795 Hanyang University, Seoul, Francois, Korea B., Kim, T. J., Park Korea University, J., Cho, Korea S., Choi, S., Go, Y., Hong, B., Lee, K. S., Lim, J., Park, J., Park, S. K., Yoo Kyung Hee University, J., Department of Physics, Republic of Korea, Goh, Korea J., Gurtu Sejong University, A., Kim, Korea H. S., Kim Seoul National University, Y., Almond, Korea J., Bhyun, J. H., Choi, J., Jeon, S., Kim, J. S., Ko, S., Kwon, H., Lee, H., Lee, S., B. H., Oh, Oh, M., S. B., Oh, Seo, H., Yang, U. K., Yoon University of Seoul, I., Jang, Korea W., Kang, D. Y., Kang, Y., Kim, S., Ko, B., Lee, J. S. H., Lee, Y., Park, I. C., Roh, Y., Ryu, M. S., Song, D., Watson, I. J., Yang Yonsei University, S., Korea S., Ha, Yoo Sungkyunkwan University, H. D., Suwon, Choi, Korea M., Yu College of Engineering and Technology, I., American University of the Middle East (AUM), Egaila, Kuwait, Dasman, Beyrouthy, Kuwait T., Maghrbi Riga Technical University, Y., Riga, Veckalns49 Vilnius University, Latvia V., Vilnius, Ambrozas, Lithuania M., Carvalho Antunes De Oliveira, A., Juodagalvis, A., Rinkevicius, A., Tamulaitis National Centre for Particle Physics, G., Universiti, Malaya, Kuala, Lumpur, Bin Norjoharuddeen, Malaysia N., Wan Abdullah, W. A. T., Yusli, M. N., Zolkapli Universidad de Sonora (UNISON), Z., Hermosillo, Benitez, Mexico J. F., Castaneda Hernandez, A., Coello, M. León., Murillo Quijada, J. A., Sehrawat, A., Valencia Palomo Centro de Investigacion y de Estudios Avanzados del IPN, L., Mexico, City, Ayala, Mexico G., Castilla-Valdez, H., De La Cruz-Burelo, E., Heredia-De La Cruz50, I., Lopezfernandez, R., Mondragon Herrera, C. A., Perez Navarro, D. A., Sánchez Hernández Universidad Iberoamericana, A., Carrillo Moreno, Mexico S., Oropeza Barrera, C., Vazquez Valencia Benemerita Universidad Autonoma de Puebla, F., Puebla, Pedraza, Mexico I., Salazar Ibarguen, H. A., Uribe Estrada University of Montenegro, C., Podgorica, Mijuskovic51, Montenegro J., Raicevic University of Auckland, N., Auckland, Krofcheck University of Canterbury, New Zealand D., Christchurch, Butler National Centre for Physics, New Zealand P. H., Quaid-I-Azam, University, Islamabad, Ahmad, Pak- istan A., Asghar, M. I., Awais, A., Awan, M. I. M., Hoorani, H. R., Khan, W. A., Shah, M. A., Shoaib, M., Waqas AGH University of Science and Technology Faculty of Computer Sci- ence, M., Electronics and Telecommunications, Krakow, Avati, Poland V., Grzanka, L., Malawski National Centre for Nuclear Research, M., Swierk, Bialkowska, Poland H., Bluj, M., Boimska, B., Górski, M., Kazana, M., Szleper, M., Zalewski Institute of Experimental Physics, P., Faculty of Physics, University of Warsaw, Warsaw, Bunkowski, Poland K., Doroba, K., Kalinowski, A., Konecki, M., Krolikowski Laboratório de Instrumentção e Física Experimental de Partículas, J., Lisboa, Araujo, Portugal M., Bargassa, P., Bastos, D., Boletti, A., Faccioli, P., Gallinaro, M., Hollar, J., Leonardo, N., Niknejad, T., Pisano, M., Seixas, J., Toldaiev, O., Varela Joint Institute for Nuclear Research, J., Dubna, Afanasiev, Russia S., Budkouski, D., Golutvin, I., Gorbunov, I., Karjavine, V., Korenkov, V., Lanev, A., Malakhov, A., Matveev52, V., Palichik, V., Perelygin, V., Savina, M., Seitova, D., Shalaev, V., Shmatov, S., Shulha, S., Smirnov, V., Teryaev, O., Voytishin, N., Yuldashev54, B. S., Zarubin, A., Zhizhin Petersburg Nuclear Physics Institute, I., Petersburg), Gatchina (St., Gavrilov, Russia G., Golovtcov, V., Ivanov, Y., Kim55, V., Kuznetsova56, E., Murzin, V., Oreshkin, V., Smirnov, I., Sosnov, D., Sulimov, V., Uvarov, L., Volkov, S., Vorobyev Institute for Nuclear Research, A., Moscow, Andreev, Russia Yu., Dermenev, A., Gninenko, S., Golubev, N., Karneyeu, A., Kirpichnikov, D., Kirsanov, M., Krasnikov, N., Pashenkov, A., Pivovarov, G., Alikhanov of NRC ‘Kurchatov Institute’, A. Toropin Institute for Theoretical and Experimental Physics named by A. I., Epshteyn, Russia V., Gavrilov, V., Lychkovskaya, N., Nikitenko57, A., Popov, V., Stepennov, A., Toms, M., Vlasov, E., Zhokin Moscow Institute of Physics and Technology, A., Aushev National Research Nuclear University ’Moscow Engineering Physics Institute’ (MEPhI), Russia T., Bychkova, Russia O., Chadeeva58, M., Parygin, P., Popova, E., Rusinov, V., Lebedev Physical Institute, D. Selivanova P. 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C., Nabili, S., Palmer, C., Seidel, M., Skuja, A., Wang, L., Wong Massachusetts Institute of Technology, K., Cambridge, Massachusetts, Abercrombie, USA D., Andreassi, G., Bi, R., Brandt, S., Busza, W., Cali, I. A., D’Alfonso, M., Eysermans, J., Freer, C., Gomez Ceballos, G., Goncharov, M., Harris, P., Hu, M., Klute, M., Kovalskyi, D., Krupa, J., Lee, Y. -J., Mironov, C., Paus, C., Rankin, D., Roland, C., Roland, G., Shi, Z., Stephans, G. S. F., Wang, Z., Wyslouch University of Minnesota, B., Minneapolis, Minnesota, Chatterjee, USA R. M., Evans, A., Hansen, P., Hiltbrand, J., Jain, Sh., Krohn, M., Kubota, Y., Mans, J., Revering, M., Rusack, R., Saradhy, R., Schroeder, N., Strobbe, N., Wadud University of Mississippi, M. A., Oxford, Mississippi, Acosta, USA J. G., Cremaldi, L. M., Oliveros, S., Perera, L., Summers† University of Nebraska-Lincoln, D., Lincoln, Nebraska, Avdeeva, USA E., Bloom, K., Bryson, M., Claes, D. R., Fangmeier, C., Finco, L., Golf, F., Joo, C., Kravchenko, I., Meier, F., Musich, M., Reed, I., Siado, J. E., Snow†, G. R., Tabb, W., Yan, F., Zecchinelli State University of New York at Buffalo, A. G., Buffalo, Agarwal, USA G., Bandyopadhyay, H., Hay, L., Iashvili, I., Kharchilava, A., Mclean, C., Nguyen, D., Pekkanen, J., Rappoccio, S., Williams Northeastern University, A., Alverson, USA G., Barberis, E., Haddad, Y., Hortiangtham, A., Li, J., Madi- gan, G., Marzocchi, B., Morse, D. M., Nguyen, V., Orimoto, T., Parker, A., Skinnari, L., Tishelman-Charny, A., Wamorkar, T., Wang, B., Wisecarver, A., Wood Northwestern University, D., Evanston, Illinois, Bhattacharya, USA S., Bueghly, J., Chen, Z., Gilbert, A., Gunter, T., Hahn, K. A., Liu, Y., Odell, N., Schmitt, M. H., Sung, K., Velasco University of Notre Dame, M., Notre, Dame, Indiana, Band, USA R., Bucci, R., Das, A., Dev, N., Goldouzian, R., Hildreth, M., Hurtado Anampa, K., Jessop, C., Lannon, K., Lawrence, J., Loukas, N., Lut- ton, D., Marinelli, N., Mcalister, I., Mccauley, T., Mcgrady, C., Mohrman, K., Musienko52, Y., Ruchti, R., Siddireddy, P., Townsend, A., Wayne, M., Wightman, A., Zarucki, M., Zygala The Ohio State University, L., Columbus, Ohio, Bylsma, USA B., Cardwell, B., Durkin, L. S., Francis, B., Hill, C., Nunez Ornelas, M., Wei, K., Winer, B. L., Yates Princeton University, B. R., Princeton, New, Jersey, Addesa, USA F. M., Bonham, B., Das, P., Dezoort, G., Elmer, P., Frankenthal, A., Greenberg, B., Haubrich, N., Higginbotham, S., Kalogeropoulos, A., Kopp, G., Kwan, S., Lange, D., Marlow, D., Mei, K., Ojalvo, I., Olsen, J., Stickland, D., Tully University of Puerto Rico, C., Mayaguez, Puerto, Rico, Malik, USA S., Norberg, S., Ramirez Vargas Purdue University, J. E., West, Lafayette, Bakshi, USA A. S., Barnes, V. E., Chawla, R., Das, S., Gutay, L., Jones, M., Jung, A. W., Karmarkar, S., Kondratyev, D., Koshy, A. M., Liu, M., Negro, G., Neumeister, N., Paspalaki, G., Piperov, S., Purohit, A., Schulte, J. F., Stojanovic19, M., Thieman, J., Wang, F., Xiao, R., Xie Purdue University Northwest, W., Hammond, Indiana, Dolen, USA J., Parashar Rice University, N., Houston, Texas, Baty, USA A., Decaro, M., Dildick, S., Ecklund, K. M., Freed, S., Gardner, P., Geurts, F. J. M., Li, W., Liu, H., Nussbaum, T., Padley, B. P., Redjimi, R., Shi, W., Stahl Leiton, A. G., Yang, S., Zhang, L., Zhang University of Rochester, Y., Rochester, Bodek, USA A., de Barbaro, P., Demina, R., Dulemba, J. L., Fallon, C., Ferbel, T., Galanti, M., Garcia-Bellido, A., Hindrichs, O., Khukhunaishvili, A., Ranken, E., Taus Rutgers, R., The State University of New Jersey, Piscataway, Bartz, USA E., Chiarito, B., Chou, J. P., Gandrakota, A., Gershtein, Y., Halki- adakis, E., Hart, A., Heindl, M., Karacheban26, O., Laflotte, I., Lath, A., Montalvo, R., Nash, K., Osherson, M., Salur, S., Schnetzer, S., Somalwar, S., Stone, R., Thayil, S. A., Thomas, S., Wang University of Tennessee, H., Knoxville, Tennessee, Acharya, USA H., Delannoy, A. G., Fiorendi, S., Spanier Texas A&, S., University, M, College, Station, Texas, Bouhali98, USA O., Dalchenko, M., Delgado, A., Eusebi, R., Gilmore, J., and Methods in Physics Research, T. 43 The CMS Collaboration Nuclear Inst., A 1037 (2022) 166795 Huang, Kamon99, T., Kim, H., Luo, S., Malhotra, S., Mueller, R., Overton, D., Rathjens, D., Safonov Texas Tech University, A., Lubbock, Texas, Akchurin, USA N., Damgov, J., Hegde, V., Kunori, S., Lamichhane, K., Mengke, T., Muthumuni, S., Peltola, T., Volobouev, I., Whitbeck Vanderbilt University, A., Nashville, Tennessee, Appelt, USA E., D’Angelo, P., Greene, S., Gurrola, A., Johns, W., Melo, A., Ni, H., Padeken, K., Romeo, F., Sheldon, P., Tuo, S., Velkovska University of Virginia, J., Charlottesville, Virginia, Arenton, USA M. W., Cox, B., Cummings, G., Hakala, J., Hirosky, R., Joyce, M., Ledovskoy, A., Li, A., Neu, C., Perez Lara, C. E., Tannenwald, B., White, S., Wolfe Wayne State University, E., Detroit, Michigan, Poudyal University of Wisconsin - Madison, USA N., Madison, Wi, Wisconsin, Black, USA K., Bose, T., Caillol, C., Dasu, S., De Bruyn, I., Everaerts, P., Fienga, F., Galloni, C., He, H., Herndon, M., Hervé, A., Hussain, U., Lanaro, A., Loeliger, A., Loveless, R., Madhusudanan Sreekala, J., Mallampalli, A., Mohammadi, A., Pinna, D., Savin, A., Shang, V., Smith, W. H., Teague, D., Trembath-Reichert, S., Vetens 30 Also at Institute of Physics, W., Hungary 31 Also at Institute of Nuclear Research ATOMKI, Hungary 32 Also at MTA-ELTE Lendület CMS Particle and Nuclear Physics Group, Hungary 33 Also at Wigner Research Centre for Physics, Hungary 34 Also at IIT Bhubaneswar, Bhubaneswar, India 35 Also at Institute of Physics, Khalsa College, India 36 Also at G. H. G., Punjab, India 37 Also at Shoolini University, Solan, India 38 Also at University of Hyderabad, Hyderabad, India 39 Also at University of Visva-Bharati, Santiniketan, India 40 Also at Indian Institute of Technology (IIT), India 41 Also at Sharif University of Technology, Iran 42 Also at Department of Physics, University of Science and Technology of Mazandaran, Behshahr, Iran 43 Now at INFN Sezione di Bari, Università di Bari, Politecnico di Bari, Italy 44 Also at Italian National Agency for New Technologies, Energy and Sustainable Economic Development, Italy 45 Also at Centro Siciliano di Fisica Nucleare, e di Struttura Della Materia, Catania, Italy 46 Also at Horia Hulubei National Institute of Physics and Nuclear Engineering (IFIN-HH), Bucharest, Romania 47 Also at Universita di Napoli ‘Federico II’, Napoli, Italy 48 Also at Consiglio Nazionale delle Ricerche, - Istituto Officina dei Materiali, Perugia, Italy 49 Also at Riga Technical University, Latvia 50 Also at Consejo Nacional de Ciencia, y Tecnología, Mexico 51 Also at IRFU, France 52 Also at Institute for Nuclear Research, Russia 53 Now at National Research Nuclear University ‘Moscow Engineering Physics Institute’ (MEPhI), Russia 54 Also at Institute of Nuclear Physics of the Uzbekistan Academy of Sciences, Tashkent, Petersburg Polytechnic University, Uzbekistan 55 Also at St., Petersburg, St., Russia 56 Also at University of Florida, USA 57 Also at Imperial College, Lebedev Physical Institute, United Kingdom 58 Also at P. N., Russia 59 Also at California Institute of Technology, USA 60 Also at INFN Sezione di Padova, Università di Padova, Università di Trento, Trento, Italy, Padova, Italy 61 Also at Budker Institute of Nuclear Physics, Russia 62 Also at Faculty of Physics, University of Belgrade, Serbia 63 Also at Trincomalee Campus, Eastern, University, Sri, Lanka, Nilaveli, Sri Lanka 64 Also at INFN Sezione di Pavia, Università di Pavia, Italy 65 Also at National and Kapodistrian University of Athens, Greece 66 Also at Ecole Polytechnique Fédérale Lausanne, Lausanne, Switzer- land 67 Also at Universität Zürich, Switzerland 68 Also at Stefan Meyer Institute for Subatomic Physics, Austria 69 Also at Laboratoire d’Annecy-le-Vieux de Physique des Particules, IN2P3-CNRS, Annecyle-Vieux, France 70 Also at Şırnak University, Sirnak, Turkey 71 Also at Near East University, Research Center of Experimental Health Science, Turkey 72 Also at Konya Technical University, Konya, Turkey 73 Also at Piri Reis University, Turkey 74 Also at Adiyaman University, Adiyaman, Turkey 75 Also at Ozyegin University, Turkey 76 Also at Izmir Institute of Technology, Izmir, Turkey 77 Also at Necmettin Erbakan University, Turkey 78 Also at Bozok Universitetesi Rektörlügü, Yozgat, Turkey † Deceased, 1 Also at TU Wien, Wien, Austria, 2 Also at Institute of Basic and Applied Sciences, Faculty of Engineering, Arab Academy for Science, Technology and Maritime Transport, Alexandria, Egypt 3 Also 4 Also 5 Also 6 Also 7 Also 8 Also, 9 Also 10 Also at Nanjing Normal University Department of Physics, Nanjing, China 11 Now at The University of Iowa, USA 12 Also at Deutsches Elektronen-Synchrotron, Alikhanov of NRC ‘Kurchatov Institute’, Germany 13 Also at Institute for Theoretical and Experimental Physics named by A. I., Russia 14 Also at Joint Institute for Nuclear Research, Russia 15 Also at Cairo University, Egypt 16 Also at Suez University, Suez, Egypt 17 Now at British University in Egypt, Egypt 18 Also at CERN, Switzerland 19 Also at Purdue University, USA 20 Also at Université de Haute Alsace, Mulhouse, France 21 Also at Tbilisi State University, Georgia 22 Also at Erzincan Binali Yildirim University, Erzincan, Turkey 23 Also at RWTH Aachen University, Germany 24 Also at University of Hamburg, Germany 25 Also at Isfahan University of Technology, Iran 26 Also at Brandenburg University of Technology, Cottbus, Germany 27 Also at Forschungszentrum Julich, Juelich, Germany 28 Also at Physics Department, Assiut, University, Assiut, Egypt 29 Also at Karoly Robert Campus, Hungary at Université Libre de Bruxelles, Belgium at Universidade Estadual de Campinas, Campinas, Brazil at Federal University of Rio Grande do Sul, Porto, Alegre, Brazil at The University of the State of Amazonas, Manaus, Brazil at University of Chinese Academy of Sciences, China at Department of Physics, China at UFMS, Nova, Andradina, and Methods in Physics Research, Brazil 44 The CMS Collaboration Nuclear Inst., A 1037 (2022) 166795 79 Also at Marmara University, Turkey 80 Also at Milli Savunma University, Turkey 81 Also at Kafkas University, Kars, Turkey 82 Also at Istanbul Bilgi University, Turkey 83 Also at Hacettepe University, Turkey 84 Also at Istanbul University, - Cerrahpasa, Turkey 85 Also at Vrije Universiteit Brussel, Belgium 86 Also at School of Physics and Astronomy, University of Southampton, Southampton, United Kingdom 87 Also at Rutherford Appleton Laboratory, United Kingdom 88 Also at IPPP Durham University, Durham, United Kingdom 89 Also at Monash University, Clayton, Australia 90 Also at Universitá di Torino, Torino, Italy 91 Also at Bethel University, Paul, St., Minneapolis, USA 92 Also at Karamanoğlu Mehmetbey University, Karaman, Turkey 93 Also at Ain Shams University, Egypt 94 Also at Bingol University, Bingol, Turkey 95 Also at Georgian Technical University, Georgia 96 Also at Sinop University, Sinop, Turkey 97 Also at Erciyes University, Kayseri, Turkey 98 Also at Texas A, M University at Qatar, Doha, Qatar 99 Also at Kyungpook National University, Daegu, Korea, Universidad de Cantabria, CMS Collaboration, The CMS Collaboration, Department of Physics, Helsinki Institute of Physics, University of Zurich, Belforte, S., Candelise, V., Casarsa, M., Cossutti, F., DA ROLD, A., DELLA RICCA, G., Sorrentino, G., Vazzoler, F., ET AL (the CMS, Collaboration), Tumasyan, A, Adam, W, Andrejkovic, JW, Bergauer, T, Bloch, D, Chatterjee, S, Dragicevic, M, Del Valle, AE, Fruwirth, R, Hinger, V, Jeitler, M, Krammer, N, Lechner, L, Liko, D, Mikulec, I, Paulitsch, P, Pitters, FM, Schieck, J, Schofbeck, R, Schwarz, D, Steininger, H, Templ, S, Waltenberger, W, Wulz, E, Chekhovsky, V, Litomin, A, Makarenko, V, Beaumont, W, Darwish, MR, De Wolf, EA, Janssen, T, Kello, T, Lelek, A, Sfar, HR, Van Mechelen, P, Van Putte, S, Van Remortel, N, Blekman, F, Bols, ES, D'Hondt, J, Delcourt, M, El Faham, H, Lowette, S, Moortgat, S, Morton, A, Muller, D, Sahasransu, AR, Tavernier, S, Van Doninck, W, Van Mulders, P, Allard, Y, Beghin, D, Bilin, B, Clerbaux, B, De Lentdecker, G, Deng, W, Favart, L, Grebenyuk, A, Hohov, D, Kalsi, AK, Khalilzadeh, A, Lee, K, Mahdavikhorrami, M, Makarenko, I, Moureaux, L, Petre, L, Popov, A, Postiau, N, Robert, F, Song, Z, Starling, E, Thomas, L, Vanden Bemden, M, Vander Velde, C, Vanlaer, P, Vannerom, D, Wezenbeek, L, Yang, Y, Cornelis, T, Dobur, D, Knolle, J, Lambrecht, L, Mestdach, G, Niedziela, M, Roskas, C, Samalan, A, Skovpen, K, Tytgat, M, Vermassen, B, Vit, M, Benecke, A, Bethani, A, Bruno, G, Bury, F, Caputo, C, David, P, Deblaere, A, Delaere, C, Donertas, IS, Giammanco, A, Jaffel, K, Jain, S, Lemaitre, V, Mondal, K, Prisciandaro, J, Szilasi, N, Taliercio, A, Teklishyn, M, Tran, TT, Vischia, P, Wertz, S, Alves, GA, Hensel, C, Moraes, A, Alda, WL, Pereira, MAG, Ferreira, MB, Malbouisson, HB, Carvalho, W, Chinellato, J, Da Costa, EM, Da Silveira, GG, Damiao, DD, De Souza, SF, Figueiredo, DM, Herrera, CM, Amarilo, KM, Mundim, L, Nogima, H, Teles, PR, Santoro, A, Do Amaral, SMS, Sznajder, A, Thiel, M, De Araujo, FTD, Pereira, AV, Bernardes, CA, Calligaris, L, Tomei, TRFP, Gregores, EM, Lemos, DS, Mercadante, PG, Novaes, SF, Padula, SS, Aleksandrov, A, Antchev, G, Hadjiiska, R, Iaydjiev, P, Misheva, M, Rodozov, M, Shopova, M, Sultanov, G, Dimitrov, A, Ivanov, T, Litov, L, Pavlov, B, Petkov, P, Petrov, A, Cheng, T, Javaid, T, Mittal, M, Wang, H, Yuan, L, Ahmad, M, Bauer, G, Dozen, C, Hu, Z, Martins, J, Wang, Y, Yi, K, Chapon, E, Chen, GM, Chen, HS, Chen, M, Iemmi, F, Kapoor, A, Leggat, D, Liao, H, Liu, A, Milosevic, V, Monti, F, Sharma, R, Tao, J, Thomas-Wilsker, J, Wang, J, Zhang, H, Zhao, J, Agapitos, A, An, Y, Ban, Y, Chen, C, Levin, A, Li, Q, Lyu, X, Mao, Y, Qian, SJ, Wang, D, Wang, Q, Lu, M, You, Z, Gao, X, Okawa, H, Lin, Z, Xiao, M, Avila, C, Cabrera, A, Florez, C, Fraga, J, Guisao, JM, Ramirez, F, Alvarez, JDR, Gonzalez, CAS, Giljanovic, D, Godinovic, N, Lelas, D, Puljak, I, Antunovic, Z, Kovac, M, Sculac, T, Brigljevic, V, Ferencek, D, Majumder, D, Mishra, S, Roguljic, M, Starodumov, A, Susa, T, Attikis, A, Christoforou, K, Erodotou, E, Ioannou, A, Kole, G, Kolosova, M, Konstantinou, S, Mousa, J, Nicolaou, C, Ptochos, F, Razis, PA, Rykaczewski, H, Saka, H, Finger, M, Kveton, A, Ayala, E, Jarrin, EC, Abdalla, H, Assran, Y, Mahmoud, MA, Mohammed, Y, Ahmed, I, Bhowmik, S, Dewanjee, RK, Ehataht, K, Kadastik, M, Nandan, S, Nielsen, C, Pata, J, Raidal, M, Tani, L, Veelken, C, Eerola, P, Forthomme, L, Kirschenmann, H, Osterberg, K, Voutilainen, M, Bharthuar, S, Brucken, E, Garcia, F, Havukainen, J, Kim, MS, Kinnunen, R, Lampen, T, Lassila-Perini, K, Lehti, S, Linden, T, Lotti, M, Martikainen, L, Myllymaki, M, Ott, J, Siikonen, H, Tuominen, E, Tuominiemi, J, Luukka, P, Petrow, H, Tuuva, T, Amendola, C, Besancon, M, Couderc, F, Dejardin, M, Denegri, D, Faure, JL, Ferri, F, Ganjour, S, Givernaud, A, Gras, P, de Monchenault, GH, Jarry, P, Lenzi, B, Locci, E, Malcles, J, Rander, J, Rosowsky, A, Sahin, MO, Savoy-Navarro, A, Titov, M, Yu, GB, Ahuja, S, Beaudette, F, Bonanomi, M, Perraguin, AB, Busson, P, Cappati, A, Charlot, C, Davignon, O, Diab, B, Falmagne, G, Ghosh, S, de Cassagnac, RG, Hakimi, A, Kucher, I, Motta, J, Nguyen, M, Ochando, C, Paganini, P, Rembser, J, Salerno, R, Sarkar, U, Sauvan, JB, Sirois, Y, Tarabini, A, Zabi, A, Zghiche, A, Agram, L, Andrea, J, Apparu, D, Bonnin, C, Bourgatte, G, Brom, JM, Chabert, EC, Charles, L, Collard, C, Dangelser, E, Darej, D, Fontaine, C, Goerlach, U, Grimault, C, Gross, L, Haas, C, Krauth, M, Le Bihan, AC, Nibigira, E, Ollivier-henry, N, Jimenez, ES, Van Hove, P, Asilar, E, Baulieu, G, Beauceron, S, Bernet, C, Boudoul, G, Camen, C, Caponetto, L, Carle, A, Chanon, N, Contardo, D, Dene, P, Depasse, P, Dupasquier, T, El Mamouni, H, Fay, J, Galbit, G, Gascon, S, Gouzevitch, M, Ille, B, Laktineh, IB, Lattaud, H, Lesauvage, A, Lethuillier, M, Lumb, N, Mirabito, L, Nodari, B, Perries, S, Shchablo, K, Sordini, V, Torterotot, L, Touquet, G, Vander Donckt, M, Viret, S, Lomidze, I, Toriashvili, T, Tsamalaidze, Z, Autermann, C, Botta, V, Feld, L, Karpinski, W, Kiesel, MK, Klein, K, Lipinski, M, Louis, D, Meuser, D, Pauls, A, Pierschel, G, Rauch, MP, Rowert, N, Schomakers, C, Schulz, J, Teroerde, M, Wlochal, M, Dodonova, A, Eliseev, D, Erdmann, M, Fackeldey, P, Fischer, B, Hebbeker, T, Hoepfner, K, Ivone, F, Mastrolorenzo, L, Merschmeyer, M, Meyer, A, Mocellin, G, Mondal, S, Mukherjee, S, Noll, D, Novak, A, Pook, T, Pozdnyakov, A, Rath, Y, Reithler, H, Roemer, J, Schmidt, A, Schuler, SC, Sharma, A, Vigilante, L, Wiedenbeck, S, Zaleski, S, Dziwok, C, Flugge, G, Ahmad, WH, Hlushchenko, O, Kress, T, Nowack, A, Pistone, C, Pooth, O, Roy, D, Sert, H, Stahl, A, Ziemons, T, Zotz, A, Petersen, HA, Martin, MA, Asmuss, P, Baxter, S, Bayatmakou, M, Behnke, O, Martinez, AB, Bertsche, D, Bhattacharya, S, Bin Anuar, AA, Borras, K, Brunner, D, Campbell, A, Cardini, A, Cheng, C, Colombina, F, Rodriguez, SC, Silva, GC, Danilov, V, De Silva, M, Didukh, L, Damiani, DD, Eckerlin, G, Eckstein, D, Banos, LIE, Filatov, O, Gallo, E, Geiser, A, Giraldi, A, Luyando, JMG, Grohsjean, A, Guthoff, M, Jafari, A, Jomhari, NZ, Jung, H, Kasem, A, Kasemann, M, Kaveh, H, Kleinwort, C, Krucker, D, Lange, W, Lidrych, J, Lipka, K, Lohmann, W, Mankel, R, Maser, H, Melzer-Pellmann, IA, Morentin, MM, Metwally, J, Meyer, AB, Meyer, M, Mittag, G, Mnich, J, Muhl, C, Mussgiller, A, Otarid, Y, Adan, DP, Pitzl, D, Raspereza, A, Reichelt, O, Lopes, BR, Rubenach, J, Saggio, A, Saibel, A, Savitskyi, M, Scham, M, Scheurer, V, Schutze, P, Schwanenberger, C, Shchedrolosiev, M, Shevchenko, R, Ricardo, RES, Stafford, D, Stever, R, Tonon, N, Van De Klundert, M, Velyka, A, Walsh, R, Walter, D, Wen, Y, Wichmann, K, Wiens, L, Wissing, C, Wuchterl, S, Zuber, A, Aggleton, R, Albrecht, S, Bein, S, Benato, L, Biskop, H, Buhmann, P, Connor, P, De Leo, K, Eich, M, Feindt, F, Frohlich, A, Garbers, C, Garutti, E, Gunnellini, P, Hajheidari, M, Haller, J, Hinzmann, A, Jabusch, HR, Kasieczka, G, Klanner, R, Kogler, R, Kramer, T, Kutzner, V, Lange, J, Lange, T, Lobanov, A, Malara, A, Martens, S, Mrowietz, M, Niemeyer, CEN, Nigamova, A, Nissan, Y, Rodriguez, KJP, Rieger, O, Schleper, P, Schroder, M, Schwandt, J, Sonneveld, J, Stadie, H, Steinbruck, G, Tews, A, Vormwald, B, Wellhausen, J, Zoi, I, Ardila-Perez, LE, Balzer, M, Barvich, T, Bechtel, J, Blank, T, Brommer, S, Burkart, M, Butz, E, Caselle, M, Caspart, R, Chwalek, T, De Boer, W, Dierlamm, A, Droll, A, El Morabit, K, Faltermann, N, Giffels, M, Gosewisch, JO, Gottmann, A, Hartmann, F, Heidecker, C, Husemann, U, Keicher, P, Koppenhofer, R, Maier, S, Metzler, M, Mitra, S, Muller, T, Neufeld, M, Neukum, M, Nurnberg, A, Quast, G, Rabbertz, K, Rauser, J, Sander, O, Savoiu, D, Schell, D, Schnepf, M, 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S, Monroy, J, Fuentes, YP, Patterson, JR, Quach, D, Reichert, J, Reid, M, Riley, D, Ryd, A, Smolenski, K, Strohman, C, Sun, W, Thom, J, Wittich, P, Zou, R, Albrow, M, Alyari, M, Apollinari, G, Apresyan, A, Apyan, A, Bakshi, A, Bauerdick, LAT, Berry, D, Berryhill, J, Bhat, PC, Burkett, K, Butler, D, Butler, JN, Canepa, A, Cerati, GB, Cheung, HWK, Chlebana, F, Cremonesi, M, Derylo, G, Di Petrillo, KF, Dickinson, J, Elvira, VD, Feng, Y, Freeman, J, Gecse, Z, Ghosh, A, Gingu, C, Gonzalez, H, Gray, L, Green, D, Grunendahl, S, Gutsche, O, Harris, RM, Heller, R, Herwig, TC, Hirschauer, J, Jayatilaka, B, Jindariani, S, Johnson, M, Joshi, U, Klabbers, P, Klijnsma, T, Klima, B, Kwok, KHM, Lammel, S, Lei, CM, Lincoln, D, Lipton, R, Liu, T, Madrid, C, Maeshima, K, Mantilla, C, Mason, D, McBride, P, Merkel, P, Mrenna, S, Nahn, S, Ngadiuba, J, O'Dell, V, Papadimitriou, V, Pedro, K, Pena, C, Prokofyev, O, Ravera, F, Hall, AR, Ristori, L, Sexton-Kennedy, E, Smith, N, Soha, A, Spalding, WJ, Spiegel, L, Stoynev, S, Strait, J, Taylor, L, Tkaczyk, S, Tran, NV, Uplegger, L, Vaandering, EW, Voirin, E, Weber, HA, Acosta, D, Avery, P, Bourilkov, D, Cadamuro, L, Cherepanov, V, Errico, F, Field, RD, Guerrero, D, Joshi, BM, Kim, M, Koenig, E, Konigsberg, J, Korytov, A, Lo, KH, Matchev, K, Menendez, N, Mitselmakher, G, Madhu, AM, Rawal, N, Rosenzweig, D, Rosenzweig, S, Rotter, J, Shi, K, Sturdy, J, Yigitbasi, E, Zuo, X, Adams, T, Askew, A, Habibullah, R, Hagopian, V, Johnson, KF, Khurana, R, Kolberg, T, Martinez, G, Prosper, H, Schiber, C, Viazlo, O, Yohay, R, Zhang, J, Baarmand, MM, Butalla, S, Elkafrawy, T, Hohlmann, M, Verma, RK, Noonan, D, Rahmani, M, Yumiceva, F, Adams, MR, Gonzalez, HB, Cavanaugh, R, Chen, X, Dittmer, S, Evdokimov, A, Evdokimov, O, Gerber, CE, Hangal, DA, Hofman, DJ, Merrit, AH, Mills, C, Oh, G, Roy, T, Rudrabhatla, S, Tonjes, MB, Varelas, N, Viinikainen, J, Wang, X, Wu, Z, Ye, Z, Alhusseini, M, Dilsiz, K, Durgut, S, Gandrajula, RP, Koseyan, OK, Merlo, JP, Mestvirishvili, A, Nachtman, J, Ogul, H, Onel, Y, Penzo, A, Rude, C, Snyder, C, Tiras, E, Amram, O, Blumenfeld, B, Corcodilos, L, Davis, J, De Havenon, V, Eminizer, M, Feingold, J, Gritsan, AV, Kang, L, Kyriacou, S, Maksimovic, P, Martin, C, Roskes, J, Sullivan, K, Swartz, M, Vami, TA, You, C, Abreu, A, Anguiano, J, Barrera, CB, Baringer, P, Bean, A, Bylinkin, A, Flowers, Z, Isidori, T, Khalil, S, King, J, Krintiras, G, Kropivnitskaya, A, Lazarovits, M, Lindsey, C, Marquez, J, Minafra, N, Murray, M, Nickel, M, Rogan, C, Royon, C, Salvatico, R, Sanders, S, Schmitz, E, Smith, C, Takaki, JDT, Warner, Z, Williams, J, Wilson, G, Duric, S, Ivanov, A, Kaadze, K, Kim, D, Maravin, Y, Mitchell, T, Modak, A, Nam, K, Taylor, R, Rebassoo, F, Wright, D, Adams, E, Baden, A, Baron, O, Belloni, A, Eno, SC, Hadley, NJ, Jabeen, S, Kellogg, RG, Koeth, T, Mignerey, AC, Nabili, S, Palmer, C, Seidel, M, Skuja, A, Wang, L, Wong, K, Abercrombie, D, Andreassi, G, Bi, R, Brandt, S, Busza, W, Cali, IA, D'Alfonso, M, Eysermans, J, Freer, C, Ceballos, GG, Goncharov, M, Harris, P, Hu, M, Klute, M, Kovalskyi, D, Krupa, J, Lee, YJ, Mironov, C, Paus, C, Rankin, D, Roland, C, Roland, G, Shi, Z, Stephans, GSF, Wang, Z, Wyslouch, B, Chatterjee, RM, Evans, A, Hansen, P, Hiltbrand, J, Krohn, M, Kubota, Y, Mans, J, Revering, M, Rusack, R, Saradhy, R, Schroeder, N, Strobbe, N, Wadud, MA, Acosta, JG, Cremaldi, LM, Oliveros, S, Perera, L, Summers, D, Avdeeva, E, Bloom, K, Bryson, M, Claes, DR, Fangmeier, C, Finco, L, Golf, F, Joo, C, Kravchenko, I, Meier, F, Musich, M, Reed, I, Siado, JE, Snow, GR, Tabb, W, Yan, F, Zecchinelli, AG, Agarwal, G, Bandyopadhyay, H, Hay, L, Iashvili, I, Kharchilava, A, McLean, C, Nguyen, D, Pekkanen, J, Rappoccio, S, Williams, A, Alverson, G, Barberis, E, Haddad, Y, Hortiangtham, A, Li, J, Madigan, G, Marzocchi, B, Morse, DM, Nguyen, V, Orimoto, T, Parker, A, Skinnari, L, Tishelman-Charny, A, Wamorkar, T, Wang, B, Wisecarver, A, Wood, D, Bueghly, J, Chen, Z, Gilbert, A, Gunter, T, Hahn, KA, Liu, Y, Odell, N, Schmitt, MH, Sung, K, Velasco, M, Band, R, Bucci, R, Das, A, Dev, N, Goldouzian, R, Hildreth, M, Anampa, KH, Jessop, C, Lannon, K, Lawrence, J, Loukas, N, Lutton, D, Marinelli, N, Mcalister, I, McCauley, T, Mcgrady, C, Mohrman, K, Musienko, Y, Ruchti, R, Siddireddy, P, Townsend, A, Wayne, M, Wightman, A, Zarucki, M, Zygala, L, Bylsma, B, Cardwell, B, Durkin, LS, Francis, B, Hill, C, Ornelas, MN, Wei, K, Winer, BL, Yates, BR, Addesa, FM, Bonham, B, Das, P, Dezoort, G, Elmer, P, Frankenthal, A, Greenberg, B, Haubrich, N, Higginbotham, S, Kalogeropoulos, A, Kopp, G, Kwan, S, Lange, D, Marlow, D, Mei, K, Ojalvo, I, Olsen, J, Stickland, D, Tully, C, Norberg, S, Vargas, JER, Bakshi, AS, Barnes, VE, Chawla, R, Das, S, Gutay, L, Jones, M, Jung, AW, Karmarkar, S, Kondratyev, D, Koshy, AM, Liu, M, Negro, G, Neumeister, N, Paspalaki, G, Piperov, S, Purohit, A, Schulte, JF, Stojanovic, M, Thieman, J, Wang, F, Xiao, R, Xie, W, Dolen, J, Parashar, N, Baty, A, Decaro, M, Dildick, S, Ecklund, KM, Freed, S, Gardner, P, Geurts, FJM, Li, W, Liu, H, Nussbaum, T, Padley, BP, Redjimi, R, Shi, W, Leiton, AGS, Zhang, L, Bodek, A, de Barbaro, P, Demina, R, Dulemba, JL, Fallon, C, Ferbel, T, Galanti, M, Garcia-Bellido, A, Hindrichs, O, Khukhunaishvili, A, Ranken, E, Taus, R, Bartz, E, Chiarito, B, Chou, JP, Gandrakota, A, Gershtein, Y, Halkiadakis, E, Hart, A, Heindl, M, Karacheban, O, Laflotte, I, Lath, A, Montalvo, R, Nash, K, Osherson, M, Salur, S, Schnetzer, S, Somalwar, S, Stone, R, Thayil, SA, Thomas, S, Acharya, H, Delannoy, AG, Fiorendi, S, Spanier, S, Bouhali, O, Dalchenko, M, Delgado, A, Eusebi, R, Gilmore, J, Huang, T, Kamon, T, Luo, S, Malhotra, S, Mueller, R, Overton, D, Rathjens, D, Safonov, A, Akchurin, N, Damgov, J, Hegde, V, Kunori, S, Lamichhane, K, Mengke, T, Muthumuni, S, Peltola, T, Volobouev, I, Whitbeck, A, Appelt, E, D'Angelo, P, Greene, S, Gurrola, A, Johns, W, Melo, A, Ni, H, Padeken, K, Romeo, F, Sheldon, P, Tuo, S, Velkovska, J, Arenton, MW, Cox, B, Cummings, G, Hakala, J, Hirosky, R, Joyce, M, Ledovskoy, A, Li, A, Neu, C, Lara, CEP, Tannenwald, B, White, S, Wolfe, E, Poudyal, N, Black, K, Bose, T, Caillol, C, Dasu, S, De Bruyn, I, Everaerts, P, Fienga, F, Galloni, C, He, H, Herndon, M, Herve, A, Hussain, U, Lanaro, A, Loeliger, A, Loveless, R, Sreekala, JM, Mallampalli, A, Mohammadi, A, Pinna, D, Savin, A, Shang, V, Smith, WH, Teague, D, Trembath-Reichert, S, Vetens, W, Damarseçkin, Serdal, Physics, Elementary Particle Physics, Faculty of Sciences and Bioengineering Sciences, Vriendenkring VUB, and Sağır, Sinan
Subjects: Technology, Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Tracker, Legacy reprocessing, measurement methods, tracking detector, alignment, Settore ING-INF/01 - Elettronica, Physics, Particles & Fields, PARTICLE PHYSICS, LARGE HADRON COLLIDER, CMS, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), tracking detector: alignment, Detector, Alignment, MillePede-II, HipPy, VERTEX, High energy physics, Experimental particle physics, LHC, p p: scattering, p p: colliding beams, B: decay, tau: hadronic decay, interaction: gauge, interaction: model, transverse momentum: missing-energy, new physics: search for, mass spectrum: transverse, black hole: quantum, vector boson: mass, W': leptonic decay, sensitivity, leptoquark: coupling, CERN LHC Coll, leptoquark: mass: lower limit, anomaly, channel cross section: upper limit, effective field theory, Higgs, Detectors and Experimental Techniques, Instruments & Instrumentation, physics.ins-det, Instrumentation, detector, alignment, Physics, Instrumentation and Detectors (physics.ins-det), Nuclear & Particles Physics, Physics, Nuclear, Physical Sciences, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, Engineering sciences. Technology, Particle Physics - Experiment, performance, Nuclear and High Energy Physics, 530 Physics, 0299 Other Physical Sciences, FOS: Physical sciences, 10192 Physics Institute, 114 Physical sciences, 0201 Astronomical and Space Sciences, ddc:530, 3106 Nuclear and High Energy Physics, CMS, performance, Nuclear Science & Technology, numerical calculations, Science & Technology, hep-ex, 3105 Instrumentation, silicon, Physics and Astronomy, alignment [tracking detector], semiconductor detector
Abstract: The strategies for and the performance of the CMS silicon tracking system alignment during the 2015-2018 data-taking period of the LHC are described. The alignment procedures during and after data taking are explained. Alignment scenarios are also derived for use in the simulation of the detector response. Systematic effects, related to intrinsic symmetries of the alignment task or to external constraints, are discussed and illustrated for different scenarios., Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 1037, ISSN:0168-9002, ISSN:1872-9576
Published: 2022
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2. Simulations of solar wind magnetosheath magnetopause interactions

Author: Helsingin yliopisto, matemaattis-luonnontieteellinen tiedekunta, fysiikan laitos, Helsingfors universitet, matematisk-naturvetenskapliga fakulteten, institutionen för fysik, University of Helsinki, Faculty of Science, Department of Physics, Division of Particle Physics and Astrophysics, Finnish Meteorological Institute, Hoilijoki, Sanni, Helsingin yliopisto, matemaattis-luonnontieteellinen tiedekunta, fysiikan laitos, Helsingfors universitet, matematisk-naturvetenskapliga fakulteten, institutionen för fysik, University of Helsinki, Faculty of Science, Department of Physics, Division of Particle Physics and Astrophysics, Finnish Meteorological Institute, and Hoilijoki, Sanni
Abstract: This thesis investigates interactions between solar wind and the magnetosphere of the Earth using two global magnetospheric simulation models, GUMICS-4 and Vlasiator, which are both developed in Finland. The main topic of the thesis is magnetic reconnection at the dayside magnetopause, its drivers and global effects. Magnetosheath mirror mode waves and their evolution, identification and impacts on the local reconnection rates at the magnetopause are also discussed. This thesis consists of four peer-reviewed papers and an introductory part. GUMICS-4 is a magnetohydrodynamic model solving plasma as a single magnetized fluid. Vlasiator is the world s first global magnetospheric hybrid-Vlasov simulation model, which solves the motion of ions by describing them as velocity distribution functions, whereas electrons are described as a charge neutralizing fluid. Vlasiator is able to solve ion scale physics in a global scale simulation. However, it is computationally heavy and the global simulations are currently describing Earth s magnetosphere only in two spatial dimensions, whereas the velocity space is three dimensional. This thesis shows that magnetic reconnection at the dayside magnetopause is controlled by several factors. The impact of dipole tilt angle and sunward component of the interplanetary magnetic field on magnetopause reconnection is investigated with a set of GUMICS-4 simulations. Using Vlasiator simulations, this thesis shows that local reconnection rate is highly variable even during steady solar wind and correlates well with an analytical model for 2D asymmetric reconnection. It is also shown that the local reconnection rate is affected by local variations in the magnetosheath plasma. Fluctuations in the magnetosheath parameters near X-lines are partly generated by mirror mode waves that are observed to grow in the quasi-perpendicular magnetosheath. These results show that that the local reconnection rate at the X-lines is affected not only by the fluct, Aurinkotuuli koostuu plasmasta eli suuresta määrästä sähköisesti varattuja hiukkasia, joita Aurinko jatkuvasti syöksee ympärilleen. Nämä varatut hiukkaset kantavat Auringon magneettikenttää mukanaan planeettojen väliseen avaruuteen. Aurinkotuulen sähkömagneettiset kentät vuorovaikuttavat Maan magneettikentän kanssa muodostaen Maan magnetosfäärin. Vaihtelut aurinkotuulen koostumuksessa, nopeudessa ja magneettikentän suunnassa ja voimakkuudessa aiheuttavat häiriöitä Maan magneetttikentässä. Näitä häiriöitä kutsutaan avaruussääksi. Jotta avaruussään rajuihin muutoksiin voidaan varautua, täytyy aurinkotuulen ja Maan magnetosfäärin vuorovaikutus tuntea. Tärkein vuorovaikutusmekanismi on magneettinen rekonnektio eli magneettisten kenttäviivojen uudelleenkytkeytyminen, jota tapahtuu magnetopausilla eli pinnalla, joka erottaa Maan magnetosfäärin aurinkotuulesta. Rekonnektio avaa Maan kenttäviivoja ja päästää energiaa ja plasmaa virtaamaan sisään ja ulos Maan magnetosfääristä. Tämä väitöskirja koostuu neljästä vertaisarvioidusta julkaisusta ja johdannosta, joissa tutkitaan aurinkotuulen ja Maan magnetosfäärin vuorovaikutusta käyttäen kahta laskennallista mallia. Toinen malli, GUMICS-4, perustuu magnetohydrodynamiikkaan eli plasman kuvailuun yhtenä magneettisena nesteenä. Toinen malli, Vlasiator, on maailman ainoa koko Maan magnetosfääriä kuvaava malli, jossa käytetään hybridi-Vlasov -menetelmää. Vlasiator mallintaa protonien käyttätymisen ratkaisemalla niiden nopeusjakaumien kehityksen, mutta elektronit se mallintaa nesteenä. Tämä metodi mahdollistaa ioniskaalan fysiikan mallintamisen, mutta on laskennallisesti huomattavasti raskaampi kuin plasman kuvaaminen yhtenä nesteenä, mistä johtuen Vlasiator-simulaatiot kuvaavat tällä hetkellä Maan magnetosfääriä ainoastaan kahdessa tilaulottuvuudessa. Ensimmäisessä julkaisussa tutkitaan magneettikentän aaltoja, joita kutsutaan peilimoodiksi, alueessa, joka on Maan magnetopausin ja sen keulashokin väliin jäävä pyörteinen välivyöhyke (
Published: 2017

3. Numerical simulations of semiconductor radiation detectors for high-energy physics and spectroscopy applications

Author: Helsingin yliopisto, matemaattis-luonnontieteellinen tiedekunta, fysiikan laitos, Helsingfors universitet, matematisk-naturvetenskapliga fakulteten, institutionen för fysik, University of Helsinki, Faculty of Science, Department of Physics, Division of Particle Physics and Astrophysics, Peltola, Timo Hannu Tapani, Helsingin yliopisto, matemaattis-luonnontieteellinen tiedekunta, fysiikan laitos, Helsingfors universitet, matematisk-naturvetenskapliga fakulteten, institutionen för fysik, University of Helsinki, Faculty of Science, Department of Physics, Division of Particle Physics and Astrophysics, and Peltola, Timo Hannu Tapani
Abstract: The position sensitive silicon particle detectors are widely used in the tracking systems of High Energy Physics experiments such as the CMS at LHC, the world's largest particle accelerator at CERN. The foreseen upgrade of the LHC to its high luminosity (HL) phase, will enable the use of maximal physics potential of the facility. However, after 10 years of operation the expected fluence will result in a radiation environment that is beyond the capacity of the present tracking system design. The required upgrade of the all-silicon central trackers will include higher granularity and radiation hard sensors that can tolerate the increased occupancy and the higher radiation levels. To address this, extensive measurement and simulation studies have been performed to investigate different designs and silicon materials. The work in this thesis has been carried out within the CMS Tracker Upgrade Project and the multi-experiment RD50 Collaboration. Simulations serve a vital role in device structure optimization and predicting the electric fields and trapping in the silicon sensors. The main objective of device simulations is by using professional software to develop an approach to both model and predict the performance of the irradiated silicon detectors. In the course of this thesis, an effective non-uniform defect model is developed using the Sentaurus TCAD simulation framework. The model reproduces both the observed bulk and surface properties and can predict the performance of strip detectors up to HL-LHC fluences. When applied to measurements of the position dependence of Charge Collection Efficiency, the model can provide a means for the parametrization of oxide charge accumulation at the detector s SiO2/Si interface as a function of irradiation dose. TCAD simulations are also applied for a comparative study of a thin p-on-p pixel sensor and a more conventional p-on-n pixel sensor. The simulations are used to provide an explanation to the measured charge collection beh, Paikkaherkkiä pii-hiukkasilmaisimia käytetään laajalti suurenergia-fysiikan kokeiden jälki-ilmaisin systeemeissä, kuten CMS:ssa LHC:lla, maailman suurimmalla hiukkaskiihdyttimellä CERN:issä. LHC:n edessä oleva päivitys korkean luminositeetin (HL) vaiheeseen tulee mahdollistamaan laitteiston fysiikkapotentiaalin maksimaalisen hyödyntämisen. Kymmenen vuoden toiminnan jälkeen odotettavissa oleva kokonaisannos tulee kuitenkin aiheuttamaan säteily-ympäristön, joka ylittää nykyisen jälki-ilmaisin systeemin kapasiteetin. Kokonaan piistä valmistetuille keskisille jälki-ilmaisimille edellytettyyn päivitykseen tulee kuulumaan suuremman rakeisuuden ja säteilynkestävyyden omaavia ilmaisimia, jotka pystyvät kestämään suurempia hetkellisiä hiukkasannoksia ja korkeampia säteilytasoja. Tämän johdosta on suoritettu laajoja mittaus- ja simulaatiotutkimuksia erilaisilla ilmaisinrakenteilla ja pii-materiaaleilla. Tässä väitöskirjassa esitetetty tutkimus on suoritettu CMS Tracker Upgrade-projektin ja RD50 kollaboraation puitteissa. Simulaatiot ovat oleellisessa osassa ilmaisinrakenteiden optimoinnissa sekä ennakoitaessa sähkökenttiä ja loukkuuntumista pii-ilmaisimissa. Ilmaisinsimulaatioiden pääasiallinen tavoite on kaupallisia ohjelmistoja käyttäen kehittää metodi säteilytettyjen pii-ilmaisimien toiminnan mallintamiseksi ja ennusteiden laatimiseksi. Tässä väitöskirjassa esitellään efektiivisen epäyhtenäisen säteilyvaurio-mallin kehitysprosessi Sentaurus TCAD simulaatio-ohjelmistopakettia käyttäen. Malli toisintaa kokeellisesti havaitut bulkki- ja pintaominaisuudet ja kykenee tuottamaan ennusteita nauhailmaisimille HL-LHC säteilyannoksiin asti. Sovellettuna varauksen keräystehokkuuden paikkariippuvuus mittauksiin, malli voi tarjota keinon oksidivarauksen akkumulaation parametrisointiin annoksen funktiona ilmaisimen pii-oksidi rajapinnalla. TCAD simulaatioita käyttäen on myös suoritettu vertaileva tutkimus ohuen p-on-p pikselisensorin ja tavanomaisemman p-on-n pikselisensorin välillä. Si
Published: 2016

4. Scintillating fiber trackers with optoelectronic readout for the chorus neutrino experiment

Author: UCL - SC/PHYS - Département de physique, Lendermann, Peter, 5th Topical Seminar on Experimental Apparatus for High-energy Particle Physics and Astrophysics, UCL - SC/PHYS - Département de physique, Lendermann, Peter, and 5th Topical Seminar on Experimental Apparatus for High-energy Particle Physics and Astrophysics
Published: 1994

5. Uncovering erosion effects on magnetic flux rope twist

Author: Emilia Kilpua, Simon Good, Jens Pomoell, Sanchita Pal, Daniel Price, University of Helsinki, Particle Physics and Astrophysics, University of Helsinki, Space Physics Research Group, University of Helsinki, Department of Physics, Particle Physics and Astrophysics, Department of Physics, and Space Physics Research Group
Subjects: 010504 meteorology & atmospheric sciences, Field line, Sun: coronal mass ejections (CMEs), HELICITY, Flux, FOS: Physical sciences, Context (language use), CLOUD EROSION, Astrophysics, PROFILE, 01 natural sciences, CORONAL MASS EJECTION, 0103 physical sciences, RECONNECTION, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, TOPOLOGY, LOOP, Sun: heliosphere, 010303 astronomy & astrophysics, Sun: magnetic fields, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, Astronomy and Astrophysics, Magnetic reconnection, solar-terrestrial relations, 115 Astronomy, Space science, Corona, Magnetic flux, MODEL, Solar wind, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, magnetic reconnection, Physics::Space Physics, Astrophysics::Earth and Planetary Astrophysics
Abstract: Magnetic clouds (MCs) are transient structures containing large-scale magnetic flux ropes from solar eruptions. The twist of magnetic field lines around the rope axis reveals information about flux rope formation processes and geoeffectivity. During propagation, MC flux ropes may erode via reconnection with the ambient solar wind. Any erosion reduces the magnetic flux and helicity of the ropes, and changes their cross-sectional twist profiles. This study relates twist profiles in MC flux ropes observed at 1 AU to the amount of erosion undergone by the MCs in interplanetary space. The twist profiles of two well-identified MC flux ropes associated with the clear appearance of post eruption arcades in the solar corona are analysed. To infer the amount of erosion, the magnetic flux content of the ropes in the solar atmosphere is estimated, and compared to estimates at 1 AU. The first MC shows a monotonically decreasing twist from the axis to periphery, while the second displays high twist at the axis, rising twist near the edges, and lower twist in between. The first MC displays a larger reduction in magnetic flux between the Sun and 1 AU, suggesting more erosion, than that seen in the second MC. In the second cloud, rising twist at the rope edges may have been due to an envelope of overlying coronal field lines with relatively high twist, formed by reconnection beneath the erupting flux rope in the low corona. This high-twist envelope remained almost intact from the Sun to 1 AU due to the low erosion levels. In contrast, the high-twist envelope of the first cloud may have been entirely peeled away via erosion by the time it reaches 1 AU., 10 pages, 5 figures, 1 table
Published: 2021

6. iPTF16geu: A multiply imaged, gravitationally lensed type Ia supernova

Author: Yaron, O. [Weizmann Inst. of Science, Rehovot (Israel). Dept. of Particle Physics and Astrophysics] (ORCID:0000000203018017)
Published: 2017
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7. Detection of Lensing Substructure Using Alma Observations of the Dusty Galaxy SDP.81

Author: Wechsler, Risa [Stanford Univ., CA (United States). Kavli Inst. for Particle Astrophysics and Cosmology and Dept. of Physics; SLAC National Accelerator Lab., Menlo Park, CA (United States). Kavli Inst. for Particle Astrophysics and Cosmology and Dept. of Particle Physics and Astrophysics]
Published: 2016
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8. The nature of submillimetre and highly star-forming galaxies in the EAGLE simulation

Author: Tom Theuns, Joop Schaye, James W. Trayford, Ian Smail, Richard G. Bower, Peter Camps, Stuart McAlpine, Robert A. Crain, Maarten Baes, A. M. Swinbank, Particle Physics and Astrophysics, Department of Physics, and University of Helsinki, Particle Physics and Astrophysics
Subjects: formation [galaxies], Population, galaxies: active, REDSHIFT, FOS: Physical sciences, galaxies: starburst, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Star (graph theory), 01 natural sciences, RADIATIVE-TRANSFER CODE, galaxies: high-redshift, 0103 physical sciences, galaxies: formation, DEEP FIELD SOUTH, education, 010303 astronomy & astrophysics, BLACK-HOLES, evolution [galaxies], Astrophysics::Galaxy Astrophysics, POPULATION, Luminosity function (astronomy), QB, ULTRALUMINOUS GALAXIES, Physics, education.field_of_study, starburst [galaxies], 010308 nuclear & particles physics, ALMA SURVEY, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, EVOLUTION, Black hole, STELLAR, Physics and Astronomy, Space and Planetary Science, LUMINOSITY FUNCTION, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], galaxies: evolution, high-redshift [galaxies]
Abstract: We exploit EAGLE, a cosmological hydrodynamical simulation, to reproduce the selection of the observed sub-millimeter (submm) galaxy population by selecting the model galaxies at $z \geq 1$ with mock submm fluxes $S_{850} \geq 1$ mJy. There is a reasonable agreement between the galaxies within this sample and the properties of the observed submm population, such as their star formation rates (SFRs) at $z 1$ mJy. Thus, we investigate the nature of $z \geq 1$ highly star-forming Submm-Faint galaxies (i.e., $\dot M_* \geq 80$ Msol/yr but $S_{850}< 1$ mJy). We find they are similar to the model submm galaxies; being gas rich and hosting undermassive black holes, however they are typically lower mass ($M_* \sim 10^{10}$ Msol) and are at higher redshifts ($z>4$). These typically higher-$z$ galaxies show stronger evidence for having been triggered by major mergers, and critically, they are likely missed by current submm surveys due to their higher dust temperatures. This suggests a potentially even larger contribution to the SFR density at $z > 3$ from dust-obscured systems than implied by current observations., 15 pages, 9 figures, submitted to MNRAS
Published: 2019

9. The gas fractions of dark matter haloes hosting simulated similar to L-star galaxies are governed by the feedback history of their black holes

Author: Davies, Jonathan J., Crain, Robert A., McCarthy, Ian G., Oppenheimer, Benjamin D., Schaye, Joop, Schaller, Matthieu, McAlpine, Stuart, Particle Physics and Astrophysics, Department of Physics, and University of Helsinki, Particle Physics and Astrophysics
Subjects: ACTIVE GALACTIC NUCLEI, AGN FEEDBACK, Astrophysics::High Energy Astrophysical Phenomena, CIRCUMGALACTIC MEDIUM, HOT HALOES, CLUSTER, Astrophysics::Cosmology and Extragalactic Astrophysics, SCALING RELATIONS, 115 Astronomy, Space science, methods: numerical, galaxies: haloes, EAGLE SIMULATIONS, galaxies: formation, STELLAR MASS FUNCTION, GROWTH, HYDRODYNAMICAL SIMULATIONS, galaxies: evolution, Astrophysics::Galaxy Astrophysics
Abstract: We examine the origin of scatter in the relationship between the gas fraction and mass of dark matter haloes hosting present-day similar to L-star central galaxies in the EAGLE simulations. The scatter is uncorrelated with the accretion rate of the central galaxy's black hole (BH), but correlates strongly and negatively with the BH's mass, implicating differences in the expulsion of gas by active galactic nucleus feedback, throughout the assembly of the halo, as the main cause of scatter. Haloes whose central galaxies host undermassive BHs also tend to retain a higher gas fraction, and exhibit elevated star formation rates (SFRs). Diversity in the mass of central BHs stems primarily from diversity in the dark matter halo binding energy, as these quantities are strongly and positively correlated at fixed halo mass, such that similar to L-star galaxies hosted by haloes that are more (less) tightly bound develop central BHs that are more (less) massive than is typical for their halo mass. Variations in the halo gas fraction at fixed halo mass are reflected in both the soft X-ray luminosity and thermal Sunyaev-Zel'dovich flux, suggesting that the prediction of a strong coupling between the properties of galaxies and their halo gas fractions can be tested with measurements of these diagnostics for galaxies with diverse SFRs but similar halo masses.
Published: 2019

10. Barycentric interpolation on Riemannian and semi-Riemannian spaces

Author: Peter H. Johansson, Pauli Pihajoki, Matias Mannerkoski, University of Helsinki, Particle Physics and Astrophysics, University of Helsinki, Department of Physics, Particle Physics and Astrophysics, and Department of Physics
Subjects: SURFACE, black hole physics, FOS: Physical sciences, 010103 numerical & computational mathematics, Barycentric coordinate system, Curvature, 01 natural sciences, methods: numerical, SPHERE, 0103 physical sciences, FOS: Mathematics, Covariant transformation, Mathematics - Numerical Analysis, FIELD, 0101 mathematics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Curvilinear coordinates, CONSTRUCTION, DISKS, SCATTERED DATA, Mathematical analysis, Astronomy and Astrophysics, Numerical Analysis (math.NA), 115 Astronomy, Space science, Surface (topology), Flow (mathematics), Space and Planetary Science, Physics - Data Analysis, Statistics and Probability, MHD-methods: data analysis, Vector field, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Data Analysis, Statistics and Probability (physics.data-an), Interpolation
Abstract: Interpolation of data represented in curvilinear coordinates and possibly having some non-trivial, typically Riemannian or semi-Riemannian geometry is an ubiquitous task in all of physics. In this work we present a covariant generalization of the barycentric coordinates and the barycentric interpolation method for Riemannian and semi-Riemannian spaces of arbitrary dimension. We show that our new method preserves the linear accuracy property of barycentric interpolation in a coordinate-invariant sense. In addition, we show how the method can be used to interpolate constrained quantities so that the given constraint is automatically respected. We showcase the method with two astrophysics related examples situated in the curved Kerr spacetime. The first problem is interpolating a locally constant vector field, in which case curvature effects are expected to be maximally important. The second example is a General Relativistic Magnetohydrodynamics simulation of a turbulent accretion flow around a black hole, wherein high intrinsic variability is expected to be at least as important as curvature effects., Comment: 10 pages, 3 figures. Revised version with small additions, accepted to MNRAS
Published: 2019
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11. Time-dependent data-driven coronal simulations of AR 12673 from emergence to eruption

Author: Erkka Lumme, Emilia Kilpua, Jens Pomoell, Daniel Price, Space Physics Research Group, Particle Physics and Astrophysics, Department of Physics, University of Helsinki, Space Physics Research Group, and University of Helsinki, Particle Physics and Astrophysics
Subjects: 010504 meteorology & atmospheric sciences, Sun: coronal mass ejections (CMEs), Flux, Astrophysics, Solar cycle 24, Space weather, magnetic fields, 01 natural sciences, MAGNETIC-FIELDS, methods: numerical, Magnetogram, Electric field, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, VECTOR MAGNETOGRAM, 0105 earth and related environmental sciences, Physics, Magnetic energy, Sun: corona, SPACE WEATHER, Astronomy and Astrophysics, Magnetic reconnection, 115 Astronomy, Space science, methods: data analysis, Magnetic field, MODEL, 13. Climate action, Space and Planetary Science, magnetic reconnection, 6 SEPTEMBER 2017, Physics::Space Physics
Abstract: Aims. We present a detailed study of the magnetic evolution of AR 12673 using a magnetofrictional modelling approach. Methods. The fully data-driven and time-dependent model was driven with maps of the photospheric electric field, inverted from vector magnetogram observations obtained from the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO). Our analysis was aided by studying the evolution of metrics such as the free magnetic energy and the current-carrying helicity budget of the domain, maps of the squashing factor and twist, and plots of the current density. These allowed us to better understand the dynamic nature of the magnetic topology. Results. Our simulation captured the time-dependent nature of the active region and the erupting flux rope associated with the X-class flares on 6 September 2017, including the largest of solar cycle 24. Additionally, our results suggest a possible threshold for eruptions in the ratio of current-carrying helicity to relative helicity. Conclusion. The flux rope was found to be a combination of two structures that partially combine during the eruption process. Our time-dependent data-driven magnetofrictional model is shown to be capable of generating magnetic fields consistent with extreme ultraviolet (EUV) observations.
Published: 2019
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12. The growth of intermediate mass black holes through tidal captures and tidal disruption events

Author: Francesco Paolo Rizzuto, Thorsten Naab, Antti Rantala, Peter H Johansson, Jeremiah P Ostriker, Nicholas C Stone, Shihong Liao, Dimitrios Irodotou, Particle Physics and Astrophysics, and Department of Physics
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, 114 Physical sciences
Abstract: We present $N\mathrm{-body} $ simulations, including post-Newtonian dynamics, of dense clusters of low-mass stars harbouring central black holes (BHs) with initial masses of 50, 300, and 2000 $\mathrm{M_{\odot}}$. The models are evolved with the $N\mathrm{-body} $ code \textsc{bifrost} to investigate the possible formation and growth of massive BHs by the tidal capture of stars and tidal disruption events (TDEs). We model star-BH tidal interactions using a velocity-dependent drag force, which causes orbital energy and angular momentum loss near the BH. About $\sim 20-30$ per cent of the stars within the spheres of influence of the black holes form Bahcall-Wolf cusps and prevent the systems from core collapse. Within the first 40 Myr of evolution, the systems experience 500 up to 1300 TDEs, depending on the initial cluster structure. Most ($> 95$ per cent) of the TDEs originate from stars in the Bahcall-Wolf cusp. We derive an analytical formula for the TDE rate as a function of the central BH mass, density and velocity dispersion of the clusters ($\dot{N}_{\mathrm{TDE}} \propto M\mathrm{_{BH}} \rho \sigma^{-3}$). We find that TDEs can lead a 300 $\mathrm{M_{\odot}}$ BH to reach $\sim 7000 \mathrm{M_{\odot}}$ within a Gyr. This indicates that TDEs can drive the formation and growth of massive BHs in sufficiently dense environments, which might be present in the central regions of nuclear star clusters., Comment: 17 pages, 18 figures
Published: 2023

13. Transmission of foreshock waves through Earth’s bow shock

Author: L. Turc, O. W. Roberts, D. Verscharen, A. P. Dimmock, P. Kajdič, M. Palmroth, Y. Pfau-Kempf, A. Johlander, M. Dubart, E. K. J. Kilpua, J. Soucek, K. Takahashi, N. Takahashi, M. Battarbee, U. Ganse, Particle Physics and Astrophysics, Space Physics Research Group, and Department of Physics
Subjects: Upstream, Quasi-parallel shocks, Pulsations, General Physics and Astronomy, Magnetosheath, Low-frequency waves, 115 Astronomy, Space science, Fusion, Plasma and Space Physics, Solar-wind, Fusion, plasma och rymdfysik, Astronomi, astrofysik och kosmologi, Magnetosphere, Fluctuations, Astronomy, Astrophysics and Cosmology, Propagation, Simulation
Abstract: The Earth’s magnetosphere and its bow shock, which is formed by the interaction of the supersonic solar wind with the terrestrial magnetic field, constitute a rich natural laboratory enabling in situ investigations of universal plasma processes. Under suitable interplanetary magnetic field conditions, a foreshock with intense wave activity forms upstream of the bow shock. So-called 30 s waves, named after their typical period at Earth, are the dominant wave mode in the foreshock and play an important role in modulating the shape of the shock front and affect particle reflection at the shock. These waves are also observed inside the magnetosphere and down to the Earth’s surface, but how they are transmitted through the bow shock remains unknown. By combining state-of-the-art global numerical simulations and spacecraft observations, we demonstrate that the interaction of foreshock waves with the shock generates earthward-propagating, fast-mode waves, which reach the magnetosphere. These findings give crucial insight into the interaction of waves with collisionless shocks in general and their impact on the downstream medium.
Published: 2022

14. First Light And Reionization Epoch Simulations (FLARES) VII: The star formation and metal enrichment histories of galaxies in the early Universe

Author: Stephen M Wilkins, Aswin P Vijayan, Christopher C Lovell, William J Roper, Erik Zackrisson, Dimitrios Irodotou, Louise T C Seeyave, Jussi K Kuusisto, Peter A Thomas, Joseph Caruana, Christopher J Conselice, Particle Physics and Astrophysics, and Department of Physics
Subjects: Methods: numerical, formation [galaxies], Galaxies: high-redshift, extinction infrared [galaxies], FOS: Physical sciences, Galaxies: evolution, Galaxies: extinction infrared, numerical [methods], Astronomy and Astrophysics, Galaxies: formation, Galaxies, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, galaxies [Infrared], Astronomi, astrofysik och kosmologi, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), galaxies, Astronomy, Astrophysics and Cosmology, evolution [galaxies], high-redshift [galaxies], extinction [Galaxies]
Abstract: The star formation and metal enrichment histories of galaxies - at any epoch - constitute one of the key properties of galaxies, and their measurement is a core aim of observational extragalactic astronomy. The lack of deep rest-frame optical coverage at high-redshift has made robust constraints elusive, but this is now changing thanks to the \emph{James Webb Space Telescope (JWST)}. In preparation for the constraints provided by \emph{JWST} we explore the star formation and metal enrichment histories of galaxies at $z=5-13$ using the First Light And Reionisation Epoch Simulations (FLARES) suite. Built on the EAGLE model, the unique strategy of FLARES allows us to simulate a wide range of stellar masses (and luminosities) and environments. While we predict significant redshift evolution of average ages and specific star formation rates our core result is a mostly flat relationship of age and specific star formation rate with stellar mass. We also find that galaxies in this epoch predominantly have strongly rising star formation histories, albeit with the magnitude dropping with redshift and stellar mass. In terms of chemical enrichment we predict a strong stellar mass - metallicity relation present at $z=10$ and beyond alongside significant $\alpha$-enhancement. Finally, we find no environmental dependence of the relationship between age, specific star formation rate, or metallicity with stellar mass., Comment: To be submitted to MNRAS. Comments welcome
Published: 2022

15. Spatial filtering in a 6D hybrid-Vlasov scheme to alleviate adaptive mesh refinement artifacts: a case study with Vlasiator (versions 5.0, 5.1, and 5.2.1)

Author: Konstantinos Papadakis, Yann Pfau-Kempf, Urs Ganse, Markus Battarbee, Markku Alho, Maxime Grandin, Maxime Dubart, Lucile Turc, Hongyang Zhou, Konstantinos Horaites, Ivan Zaitsev, Giulia Cozzani, Maarja Bussov, Evgeny Gordeev, Fasil Tesema, Harriet George, Jonas Suni, Vertti Tarvus, Minna Palmroth, Department of Physics, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Earths foreshock, General Medicine, 114 Physical sciences, Simulation
Abstract: Numerical simulation models that are used to investigate the near-Earth space plasma environment require sophisticated methods and algorithms as well as high computational power. Vlasiator 5.0 is a hybrid-Vlasov plasma simulation code that is able to perform 6D (3D in ordinary space and 3D in velocity space) simulations using adaptive mesh refinement (AMR). In this work, we describe a side effect of using AMR in Vlasiator 5.0: the heterologous grid approach creates discontinuities due to the different grid resolution levels. These discontinuities cause spurious oscillations in the electromagnetic fields that alter the global results. We present and test a spatial filtering operator for alleviating this artifact without significantly increasing the computational overhead. We demonstrate the operator's use case in large 6D AMR simulations and evaluate its performance with different implementations.
Published: 2022

16. Uncovering the process that transports magnetic helicity to coronal mass ejection flux ropes

Author: Sanchita Pal, Space Physics Research Group, Particle Physics and Astrophysics, and Department of Physics
Subjects: Atmospheric Science, 010504 meteorology & atmospheric sciences, Field line, Aerospace Engineering, Interplanetary medium, Astrophysics, 114 Physical sciences, 01 natural sciences, Magnetic cloud, Magnetic helicity, 0103 physical sciences, Coronal mass ejection, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Flux rope, 0105 earth and related environmental sciences, Physics, Astronomy and Astrophysics, Magnetic reconnection, Corona, Helicity, Interplanetary magnetic field, Geophysics, Space and Planetary Science, Physics::Space Physics, General Earth and Planetary Sciences, Heliosphere
Abstract: Publisher Copyright: © 2021 COSPAR Magnetic helicity, an intrinsic property of eruptive helical flux ropes (FRs) forming coronal mass ejections (CMEs), plays an impor-tant role in determining CME geoeffectiveness. In the solar atmosphere and heliosphere, helicity remains conserved in a closed volume. Considering this fact as a basis of our study, we perform a quantitative comparison between total magnetic helicity and twisted flux in interplanetary CMEs and those transported to CMEs via magnetic reconnection at low corona. At the source, twisted/poloidal flux (/pcme) of CMEs is directly estimated from total reconnection flux, and CME helicity (Hcme) is obtained by combining reconnection flux information with CME physical parameters. At 1 AU, the twisted/poloidal flux (/pmc) and helicity (Hmc) of CMEs are obtained from in situ observations. Considering uncertainties steaming from FR length, reconnection flux and CME physical parameter estimations, poloidal flux and helicity of CMEs at 1 AU are found to be highly relevant ( /pmc /pcme = 0.4-1.5, HHcmemc= 0.3-1) to low-corona magnetic recon-nection at the wake of CMEs. This result remains unchanged despite CME association with pre-existing FRs. We show that a significant reduction in CME helicity during its heliospheric propagation may result from a high rate of FR erosion in the interplanetary medium. Our event analysis confirms that CME's intrinsic magnetic properties are transported to CME FRs during magnetic reconnection at sheared coronal arcades. A one-to-one correspondence between the chirality of 1-AU CMEs and their pre-eruptive structures complies with the fact that the sense of field line rotations in FRs may remain unchanged during coronal reconnection at the source. By connecting intrinsic magnetic properties of FRs through Sun-Earth medium, this study provides important implications for the origin of geoeffec-tiveness in CMEs. (c) 2021 COSPAR. Published by Elsevier B.V. This is an open access article under the CC BY license (http://creativecommons.org/licenses/by/4.0/).
Published: 2022

17. Gravitational wave memory in conformally flat spacetimes

Author: Niko Jokela, K. Kajantie, Miika Sarkkinen, Department of Physics, Helsinki Institute of Physics, and Particle Physics and Astrophysics
Subjects: High Energy Physics - Theory, Nuclear and High Energy Physics, High Energy Physics - Theory (hep-th), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 115 Astronomy, Space science, 114 Physical sciences, General Relativity and Quantum Cosmology
Abstract: We study the gravitational wave memory effect in spacetimes related to flat space by a conformal transformation. The discussion is general but the gravitational wave length scale is assumed to be small compared with the background curvature radius. The general formulas are applied to Friedmann-Robertson-Walker metrics of all spatial curvatures. The effect of new terms stemming from spatial curvature is potentially detectable in future gravitational wave measurements., 27 pages, 1 figure; v2: a new paragraph added at the beginning of Sec. 3, reference to Fig. 1 added in the text, typos corrected, published version
Published: 2023

18. Electroweak sphaleron in a magnetic field

Author: Jaakko Annala, Kari Rummukainen, Department of Physics, Helsinki Institute of Physics, Particle Physics and Astrophysics, and Mind and Matter
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Lattice (hep-lat), Baryon-number nonconservation, FOS: Physical sciences, Phase-transition, Condensate solution, 114 Physical sciences, Point, 3d physics, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Lattice, O(a) errors, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Using lattice simulations we calculate the rate of baryon number violating processes, the sphaleron rate, in the Standard Model with an external (hyper)magnetic field for temperatures across the electroweak cross-over, focusing on the broken phase. Additionally, we compute the Higgs expectation value and the pseudocritical temperature. The electroweak cross-over shifts to lower temperatures with increasing external magnetic field, bringing the onset of the suppression of the baryon number violation with it. When the hypermagnetic field reaches the magitude $B_Y \approx 2 T^2$ the cross-over temperature is reduced from $160$ GeV to $145$ GeV. In the broken phase for small magnetic fields the rate behaves quadratically as a function of the magnetic flux. For stronger magnetic fields the rate reaches a linear regime which lasts until the field gets strong enough to restore the electroweak symmetry where the symmetric phase rate is reached., 15 pages, 16 figures, corrected typos, published version
Published: 2023

19. Modelling the accretion and feedback of supermassive black hole binaries in gas-rich galaxy mergers

Author: Shihong Liao, Peter H Johansson, Matias Mannerkoski, Dimitrios Irodotou, Francesco Paolo Rizzuto, Stuart McAlpine, Antti Rantala, Alexander Rawlings, Till Sawala, Particle Physics and Astrophysics, Department of Physics, and Faculty of Science
Subjects: Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, 114 Physical sciences
Abstract: We introduce a new model for the accretion and feedback of supermassive black hole (SMBH) binaries to the KETJU code, which enables us to resolve the evolution of SMBH binaries down to separations of tens of Schwarzschild radii in gas-rich galaxy mergers. Our subgrid binary accretion model extends the widely used Bondi--Hoyle--Lyttleton accretion into the binary phase and incorporates preferential mass accretion onto the secondary SMBH, which is motivated by results from small-scale hydrodynamical circumbinary disc simulations. We perform idealised gas-rich disc galaxy merger simulations using pure thermal or pure kinetic active galactic nuclei (AGN) feedback. Our binary accretion model provides more physically motivated SMBH mass ratios, which are one of the key parameters for computing gravitational wave (GW) induced recoil velocities. The merger time-scales of our simulated SMBH binaries are in the range $t_{\rm merge}{\sim} 10$--$400$ Myr. Prograde in-plane equal-mass galaxy mergers lead to the shortest merger time-scales, as they experience the strongest starbursts, with the ensuing high stellar density resulting in a rapid SMBH coalescence. Compared to the thermal AGN feedback, the kinetic AGN feedback predicts longer merger time-scales and results in more core-like stellar profiles, as it is more effective in removing gas from the galaxy centre and quenching star formation. This suggests that the AGN feedback implementation plays a critical role in modelling SMBH coalescences. Our model will be useful for improving the modelling of SMBH mergers in gas-rich galaxies, the prime targets for the upcoming LISA GW observatory., 28 pages, 13 main + 6 appendix figures, accepted for publication in MNRAS
Published: 2023

20. The Milky Way's plane of satellites is consistent with ΛCDM

Author: Till Sawala, Marius Cautun, Carlos Frenk, John Helly, Jens Jasche, Adrian Jenkins, Peter H. Johansson, Guilhem Lavaux, Stuart McAlpine, Matthieu Schaller, Faculty of Science, Department of Physics, and Particle Physics and Astrophysics
Subjects: Simulations, Evolution, Astrophysics - astrophysics of galaxies, Astrophysics - cosmology and nongalactic astrophysics, Population, Astronomy and Astrophysics, Mass, 115 Astronomy, Space science, Galaxies, Standard, Depletion, Universe, Substructure, Local group
Abstract: The Milky Way is surrounded by 11 ‘classical’ satellite galaxies in a remarkable configuration: a thin plane that is possibly rotationally supported. Such a structure is thought to be highly unlikely to arise in the standard (ΛCDM) cosmological model (Λ cold dark matter model, where Λ is the cosmological constant). While other apparent discrepancies between predictions and observations of Milky Way satellite galaxies may be explained either through baryonic effects or by invoking alternative forms of dark matter particles, there is no known mechanism for making rotating satellite planes within the dispersion-supported dark matter haloes predicted to surround galaxies such as the Milky Way. This is the so-called ‘plane of satellites problem’, which challenges not only the ΛCDM model but the entire concept of dark matter. Here we show that the reportedly exceptional anisotropy of the Milky Way satellites is explained, in large part, by their lopsided radial distribution combined with the temporary conjunction of the two most distant satellites, Leo I and Leo II. Using Gaia proper motions, we show that the orbital pole alignment is much more common than previously reported, and reveal the plane of satellites to be transient rather than rotationally supported. Comparing with new simulations, where such short-lived planes are common, we find the Milky Way satellites to be compatible with standard model expectations.
Published: 2023

21. The impact of filaments on dwarf galaxy properties in the Auriga simulations

Author: Haonan Zheng, Shihong Liao, Jia Hu, Liang Gao, Robert J J Grand, Qing Gu, Qi Guo, and Particle Physics and Astrophysics
Subjects: Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: With a hydrodynamical simulation using a simple galaxy formation model without taking into account feedback, our previous work has shown that dense and massive filaments at high redshift can provide potential wells to trap and compress gas, and hence affect galaxy formation in their resident low-mass haloes. In this paper, we make use of the Auriga simulations, a suite of high-resolution zoom-in hydrodynamical simulations of Milky Way-like galaxies, to study whether the conclusion still holds in the simulations with a sophisticated galaxy formation model. In agreement with the results of our previous work, we find that, comparing to their counterparts with similar halo masses in field, dwarf galaxies residing in filaments tend to have higher baryonic and stellar fractions. At the fixed parent halo mass, the filament dwarfs tend to have slightly higher star formation rates than those of field ones. But overall we do not find a clear difference in galaxy g - r colours between the filament and field populations. We also show that at high redshifts, the gas components in dwarf galaxies tend to have their spins aligned with the filaments in which they reside. Our results support a picture in which massive filaments at high redshift assist gas accretion and enhance star formation in their resident dwarf sized dark matter haloes., 9 pages, 7 figures, accepted for publication in MNRAS
Published: 2022

22. The Local Group's mass : probably no more than the sum of its parts

Author: Till Sawala, Meri Teeriaho, Peter H Johansson, Faculty of Science, Department of Physics, and Particle Physics and Astrophysics
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Methods: numerical, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Local Group, Dark matter, FOS: Physical sciences, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy: kinematics and dynamics, Methods: statistical, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The total mass of the Local Group (LG) and the masses of its primary constituents, the Milky Way and M31, are important anchors for several cosmological questions. In recent years, independent measurements have consistently yielded halo masses close to $10^{12} \mathrm{M_\odot}$ for the MW, and $1-2 \times 10^{12} \mathrm{M_\odot}$ for M31, while estimates derived from the pair's kinematics via the `timing argument' have yielded a combined mass of around $5 \times 10^{12} \mathrm{M_\odot}$. Here, we analyse the extremely large Uchuu simulation to constrain the mass of the Local Group and its two most massive members. First, we demonstrate the importance of selecting LG analogues whose kinematics are dominated by mutual interactions to a similar extent as the LG. Adopting the observed separation and radial velocity, we obtain a weighted posterior of $75_{-40}^{+65}$ kms$^{-1}$ for the uncertain transverse velocity. Via Gaussian process regression, we infer a total mass of $3.2^{+1.2}_{-0.9} \times 10^{12} \mathrm{M_\odot}$, significantly below the timing argument prediction. Importantly, we show that the remaining uncertainty is not rooted in the analysis or observational errors, but in the irreducible scatter in the kinematics-mass relation. We further find a mass for the less massive halo of $0.9_{-0.3}^{+0.6} \times 10^{12} \mathrm{M_\odot}$ and for the more massive halo of $2.3_{-0.9}^{+1.0} \times 10^{12} \mathrm{M_\odot}$, consistent with independent measurements of the masses of MW and M31, respectively. Incorporating the mass of the MW as an additional prior allows us to further constrain all measurements and determine that the MW is very likely to be the lower mass object of the two., 15 pages, submitted to MNRAS. Full source code provided, comments are welcome
Published: 2023

23. Experimentally accessible nonseparability criteria for multipartite-entanglement-structure detection

Author: Guillermo García-Pérez, Oskari Kerppo, Matteo A. C. Rossi, Sabrina Maniscalco, University of Helsinki, University of Turku, Department of Applied Physics, Centre of Excellence in Quantum Technology, QTF, Aalto-yliopisto, Aalto University, Particle Physics and Astrophysics, Department of Physics, and Mind and Matter
Subjects: General Physics and Astronomy, 114 Physical sciences
Abstract: Funding Information: We acknowledge the use of IBM Quantum services for this work. The views expressed are those of the authors, and do not reflect the official policy or position of IBM or the IBM Quantum team. G.G.-P., O.K., M.A.C.R., and S.M. acknowledge financial support from the Academy of Finland via the Centre of Excellence program (Project no. 336810 and 336814). G.G.-P. acknowledges support from the Academy of Finland via the Postdoctoral Researcher program (Project no. 341985). O.K. acknowledges financial support from the Turku University Foundation. The description of the complex separability structure of quantum states in terms of partially ordered sets has been recently put forward. In this work, we address the question of how to efficiently determine these structures for unknown states. We propose an experimentally accessible and scalable iterative methodology that identifies, on solid statistical grounds, sufficient conditions for nonseparability with respect to certain partitions. In addition, we propose an algorithm to determine the minimal partitions (those that do not admit further splitting) consistent with the experimental observations. We test our methodology experimentally on a 20-qubit IBM quantum computer by inferring the structure of the 4-qubit Smolin and an 8-qubit W state. In the first case, our results reveal that, while the fidelity of the state is low, it nevertheless exhibits the partitioning structure expected from the theory. In the case of the W state, we obtain very disparate results in different runs on the device, which range from nonseparable states to very fragmented minimal partitions with little entanglement in the system. Furthermore, our work demonstrates the applicability of informationally complete positive operator-valued measurements for practical purposes on current noisy intermediate-scale quantum devices.
Published: 2023

24. Quantum Simulation of Dissipative Collective Effects on Noisy Quantum Computers

Author: Marco Cattaneo, Matteo A.C. Rossi, Guillermo García-Pérez, Roberta Zambrini, Sabrina Maniscalco, Mind and Matter, Particle Physics and Astrophysics, Department of Physics, University of the Balearic Islands, Department of Applied Physics, University of Helsinki, Centre of Excellence in Quantum Technology, QTF, Aalto-yliopisto, and Aalto University
Subjects: Quantum Physics, Atoms, General Computer Science, Applied Mathematics, FOS: Physical sciences, General Physics and Astronomy, 114 Physical sciences, Electronic, Optical and Magnetic Materials, Dynamics, Computation, Maps, Electrical and Electronic Engineering, Quantum Physics (quant-ph), Mathematical Physics, State
Abstract: Dissipative collective effects are ubiquitous in quantum physics, and their relevance ranges from the study of entanglement in biological systems to noise mitigation in quantum computers. Here, we put forward the first fully quantum simulation of dissipative collective phenomena on a real quantum computer, based on the recently introduced multipartite collision model. First, we theoretically study the accuracy of this algorithm on near-term quantum computers with noisy gates, and we derive some rigorous error bounds that depend on the timestep of the collision model and on the gate errors. These bounds can be employed to estimate the necessary resources for the efficient quantum simulation of the collective dynamics. Then, we implement the algorithm on some IBM quantum computers to simulate superradiance and subradiance between a pair of qubits. Our experimental results successfully display the emergence of collective effects in the quantum simulation. In addition, we analyze the noise properties of the gates that we employ in the algorithm by means of full process tomography, with the aim of improving our understanding of the errors in the near-term devices that are currently accessible to worldwide researchers. We obtain the values of the average gate fidelity, unitarity, incoherence and diamond error, and we establish a connection between them and the accuracy of the experimentally simulated state. Moreover, we build a noise model based on the results of the process tomography for two-qubit gates and show that its performance is comparable with the noise model provided by IBM. Finally, we observe that the scaling of the error as a function of the number of gates is favorable, but at the same time reaching the threshold of the diamond errors for quantum fault tolerant computation may still be orders of magnitude away in the devices that we employ., Accepted version. We have extensively expanded and modified the experimental noise analysis
Published: 2023

25. Imbalanced Turbulence Modified by Large-scale Velocity Shears in the Solar Wind

Author: Juska E. Soljento, Simon W. Good, Adnane Osmane, Emilia K. J. Kilpua, Department of Physics, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Magnetohydrodynamic turbulence, FOS: Physical sciences, Instability, Astronomy and Astrophysics, Cross-helicity, 115 Astronomy, Space science, 114 Physical sciences, Physics - Plasma Physics, Space Physics (physics.space-ph), Plasma Physics (physics.plasm-ph), Regions, Physics - Space Physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Spectrum, Alfven waves, Fluctuations, Anisotropy, Residual energy, Solar and Stellar Astrophysics (astro-ph.SR), Radial evolution
Abstract: We have investigated how the degree of imbalance in solar wind turbulence is modified by large-scale velocity shears in the solar wind plasma. The balance between counterpropagating Alfv\'enic fluctuations, which interact nonlinearly to generate the turbulence, has been quantified by the cross helicity and Elsasser ratio. Velocity shears at a 30-min timescale were identified, with the shear amplitude defined in terms of the linear Kelvin-Helmholtz (KH) instability threshold. The shears were associated with 74 interplanetary coronal mass ejection (ICME) sheaths observed by the Wind spacecraft at 1 au between 1997 and 2018. Typically weaker shears upstream of the sheaths and downstream in the ICME ejecta were also analyzed. In shears below the KH threshold, imbalance was approximately invariant or weakly rising with shear amplitude. Above the KH threshold, fluctuations tended toward a balanced state with increasing shear amplitude. Magnetic compressibility was also found to increase above the KH threshold. These findings are consistent with velocity shears being local sources of sunward fluctuations that act to reduce net imbalances in the antisunward direction, and suggest that the KH instability plays a role in this process., Comment: 9 pages, 5 figures, accepted for publication in the Astrophysical Journal Letters 2023 March 2
Published: 2023

26. Solar-MACH: An open-source tool to analyze solar magnetic connection configurations

Author: Jan Gieseler, Nina Dresing, Christian Palmroos, Johan L. Freiherr von Forstner, Daniel J. Price, Rami Vainio, Athanasios Kouloumvakos, Laura Rodríguez-García, Domenico Trotta, Vincent Génot, Arnaud Masson, Markus Roth, Astrid Veronig, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Python (programming language), FOS: Physical sciences, Pfss, Astronomy and Astrophysics, Software package, 115 Astronomy, Space science, Space Physics (physics.space-ph), Heliosphere, Astrophysics - Solar and Stellar Astrophysics, Physics - Space Physics, coronal mass ejection (CME), Corona, Spacecraft, Solar and Stellar Astrophysics (astro-ph.SR), solar energetic particle (SEP)
Abstract: The Solar MAgnetic Connection HAUS tool (Solar-MACH) is an open-source tool completely written in Python that derives and visualizes the spatial configuration and solar magnetic connection of different observers (i.e., spacecraft or planets) in the heliosphere at different times. For doing this, the magnetic connection in the interplanetary space is obtained by the classic Parker Heliospheric Magnetic Field (HMF). In close vicinity of the Sun, a Potential Field Source Surface (PFSS) model can be applied to connect the HMF to the solar photosphere. Solar-MACH is especially aimed at providing publication-ready figures for the analyses of Solar Energetic Particle events (SEPs) or solar transients such as Coronal Mass Ejections (CMEs). It is provided as an installable Python package (listed on PyPI and conda-forge), but also as a web tool at solar-mach.github.io that completely runs in any web browser and requires neither Python knowledge nor installation. The development of Solar-MACH is open to everyone and takes place on GitHub, where the source code is publicly available under the BSD 3-Clause License. Established Python libraries like sunpy and pfsspy are utilized to obtain functionalities when possible. In this article, the Python code of Solar-MACH is explained, and its functionality is demonstrated using real science examples. In addition, we introduce the overarching SERPENTINE project, the umbrella under which the recent development took place., 14 pages, 5 figures
Published: 2023

27. Soft photon propagation in a hot and dense medium to next-to-leading order

Author: Tyler Gorda, Aleksi Kurkela, Juuso Österman, Risto Paatelainen, Saga Säppi, Philipp Schicho, Kaapo Seppänen, Aleksi Vuorinen, Helsinki Institute of Physics, Department of Physics, and Particle Physics and Astrophysics
Subjects: High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), FOS: Physical sciences, 114 Physical sciences
Abstract: We present the first complete calculation of the soft photon self-energy to the next-to-leading order in a hot and/or dense ultrarelativistic plasma in Quantum Electrodynamics (QED). The calculation is performed within the real-time formalism utilizing dimensional regularization in $4-2\epsilon$ dimensions, while the result is reported including explicit $O(\epsilon)$ terms in the zero-temperature limit. This information is required to extend the perturbative calculation of the pressure of cold and dense QED matter to partial next-to-next-to-next-to-leading order in a weak-coupling expansion, reported in a companion paper. These results pave the way for a similar future calculation in Quantum Chromodynamics., Comment: 46 pages, 11 figures
Published: 2023

28. Baryonic Effects on Lagrangian Clustering and Angular Momentum Reconstruction

Author: Ming-Jie Sheng, Hao-Ran Yu, Sijia Li, Shihong Liao, Min Du, Yunchong Wang, Peng Wang, Kun Xu, Shy Genel, Dimitrios Irodotou, Particle Physics and Astrophysics, and Department of Physics
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), Matter, Evolution, Stellar, FOS: Physical sciences, Astronomy and Astrophysics, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Galaxy spin, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Halo spin, Illustristng simulations, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: Recent studies illustrate the correlation between the angular momenta of cosmic structures and their Lagrangian properties. However, only baryons are observable and it is unclear whether they reliably trace the cosmic angular momenta. We study the Lagrangian mass distribution, spin correlation, and predictability of dark matter, gas, and stellar components of galaxy-halo systems using IllustrisTNG, and show that the primordial segregations between components are typically small. Their protoshapes are also similar in terms of the statistics of moment of inertia tensors. Under the common gravitational potential they are expected to exert the same tidal torque and the strong spin correlations are not destroyed by the nonlinear evolution and complicated baryonic effects, as confirmed by the high-resolution hydrodynamic simulations. We further show that their late-time angular momenta traced by total gas, stars, or the central galaxies, can be reliably reconstructed by the initial perturbations. These results suggest that baryonic angular momenta can potentially be used in reconstructing the parameters and models related to the initial perturbations., 8 pages, 5 figures, 1 table. Matches the accepted version in ApJ
Published: 2023

29. First light and reionization epoch simulations (FLARES) V : the redshift frontier

Author: Stephen M Wilkins, Aswin P Vijayan, Christopher C Lovell, William J Roper, Dimitrios Irodotou, Joseph Caruana, Louise T C Seeyave, Jussi K Kuusisto, Peter A Thomas, Shedeur A K Parris, Particle Physics and Astrophysics, and Department of Physics
Subjects: Galaxies: general, photometry [Galaxies], Astrophysics::Instrumentation and Methods for Astrophysics, Galaxies: high-redshift, FOS: Physical sciences, Galaxies: evolution, Astronomy and Astrophysics, general [Galaxies], Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies: photometry, Galaxies: formation, evolution [Galaxies], 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, formation [Galaxies], high-redshift [Galaxies], Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Earth and Planetary Astrophysics
Abstract: The James Webb Space Telescope (JWST) is set to transform many areas of astronomy, one of the most exciting is the expansion of the redshift frontier to $z>10$. In its first year alone JWST should discover hundreds of galaxies, dwarfing the handful currently known. To prepare for these powerful observational constraints, we use the First Light And Reionisation Epoch (FLARES) simulations to predict the physical and observational properties of the $z>10$ population of galaxies accessible to JWST. This is the first time such predictions have been made using a hydrodynamical model validated at low redshift. Our predictions at $z=10$ are broadly in agreement with current observational constraints on the far-UV luminosity function and UV continuum slope $β$, though the observational uncertainties are large. We note tension with recent constraints $z\sim 13$ from Harikane et al. 2022 - compared to these constraints, FLARES predicts objects with the same space density should have an order of magnitude lower luminosity, though this is mitigated slightly if dust attenuation is negligible in these systems. Our predictions suggest that in JWST's first cycle alone, around $600$ galaxies should be identified at $z>10$, with the first small samples available at $z>13$., Submitted to MNRAS 20/04/2022
Published: 2023

30. Plasma-neutral interactions in the lower thermosphere-ionosphere : The need for in situ measurements to address focused questions

Author: Sarris, Theodoros, Palmroth, Minna, Aikio, Anita, Buchert, Stephan Christoph, Clemmons, James, Clilverd, Mark, Dandouras, Iannis, Doornbos, Eelco, Goodwin, Lindsay Victoria, Grandin, Maxime, Heelis, Roderick, Ivchenko, Nickolay, Moretto-Jørgensen, Therese, Kervalishvili, Guram, Knudsen, David, Liu, Han-Li, Lu, Gang, Malaspina, David M., Marghitu, Octav, Maute, Astrid, Miloch, Wojciech J., Olsen, Nils, Pfaff, Robert, Stolle, Claudia, Talaat, Elsayed, Thayer, Jeffrey, Tourgaidis, Stelios, Verronen, Pekka T., Yamauchi, Masatoshi, Department of Physics, Space Physics Research Group, and Particle Physics and Astrophysics
Subjects: Altitudes below 200 km, Plasma neutral interactions, Decadal survey, In situ measurements, Ion neutral coupling, Lower thermosphere ionosphere, 115 Astronomy, Space science, LTi, Atmosphere space transition region
Abstract: The lower thermosphere-ionosphere (LTI) is a key transition region between Earth's atmosphere and space. Interactions between ions and neutrals maximize within the LTI and in particular at altitudes from 100 to 200 km, which is the least visited region of the near-Earth environment. The lack of in situ co-temporal and co-spatial measurements of all relevant parameters and their elusiveness to most remote-sensing methods means that the complex interactions between its neutral and charged constituents remain poorly characterized to this date. This lack of measurements, together with the ambiguity in the quantification of key processes in the 100-200 km altitude range affect current modeling efforts to expand atmospheric models upward to include the LTI and limit current space weather prediction capabilities. We present focused questions in the LTI that are related to the complex interactions between its neutral and charged constituents. These questions concern core physical processes that govern the energetics, dynamics, and chemistry of the LTI and need to be addressed as fundamental and long-standing questions in this critically unexplored boundary region. We also outline the range of in situ measurements that are needed to unambiguously quantify key LTI processes within this region, and present elements of an in situ concept based on past proposed mission concepts.
Published: 2023

31. Daedalus MASE (Mission Assessment through Simulation Exercise): a toolset for analysis of in situ missions and for processing global circulation model outputs in the Lower Thermosphere-Ionosphere

Author: Theodore E. Sarris, Stelios Tourgaidis, Panagiotis Pirnaris, Dimitris Baloukidis, Konstantinos Papadakis, Christos Psychalas, Stephan Christoph Buchert, Eelco Doornbos, Mark A. Clilverd, Pekka T. Verronen, David Malaspina, Narghes Ahmadi, Iannis Dandouras, Anna Kotova, Wojciech J. Miloch, David Knudsen, Nils Olsen, Octav Marghitu, Tomoko Matsuo, Gang Lu, Aurélie Marchaudon, Alex Hoffmann, Dulce Lajas, Anja Strømme, Matthew Taylor, Anita Aikio, Minna Palmroth, Roderick Heelis, Nickolay Ivchenko, Claudia Stolle, Guram Kervalishvili, Therese Moretto-Jørgensen, Robert Pfaff, Christian Siemes, Pieter Visser, Jose van den Ijssel, Han-Li Liu, Ingmar Sandberg, Constantinos Papadimitriou, Joachim Vogt, Adrian Blagau, Nele Stachlys, Particle Physics and Astrophysics, Space Physics Research Group, and Department of Physics
Subjects: global circulation model, In situ measurements, Daedalus MASE, daedalus MASE, Astronomy and Astrophysics, in situ measurements, 115 Astronomy, Space science, GCM, 114 Physical sciences, Global circulation model, Lower thermosphere ionosphere, daedalus mission, LTI, lower thermosphere ionosphere, Daedalus mission
Abstract: Daedalus MASE (Mission Assessment through Simulation Exercise) is an open-source package of scientific analysis tools aimed at research in the Lower Thermosphere-Ionosphere (LTI). It was created with the purpose to assess the performance and demonstrate closure of the mission objectives of Daedalus, a mission concept targeting to perform in-situ measurements in the LTI. However, through its successful usage as a mission-simulator toolset, Daedalus MASE has evolved to encompass numerous capabilities related to LTI science and modeling. Inputs are geophysical observables in the LTI, which can be obtained either through in-situ measurements from spacecraft and rockets, or through Global Circulation Models (GCM). These include ion, neutral and electron densities, ion and neutral composition, ion, electron and neutral temperatures, ion drifts, neutral winds, electric field, and magnetic field. In the examples presented, these geophysical observables are obtained through NCAR’s Thermosphere-Ionosphere-Electrodynamics General Circulation Model. Capabilities of Daedalus MASE include: 1) Calculations of products that are derived from the above geophysical observables, such as Joule heating, energy transfer rates between species, electrical currents, electrical conductivity, ion-neutral collision frequencies between all combinations of species, as well as height-integrations of derived products. 2) Calculation and cross-comparison of collision frequencies and estimates of the effect of using different models of collision frequencies into derived products. 3) Calculation of the uncertainties of derived products based on the uncertainties of the geophysical observables, due to instrument errors or to uncertainties in measurement techniques. 4) Routines for the along-orbit interpolation within gridded datasets of GCMs. 5) Routines for the calculation of the global coverage of an in situ mission in regions of interest and for various conditions of solar and geomagnetic activity. 6) Calculations of the statistical significance of obtaining the primary and derived products throughout an in situ mission’s lifetime. 7) Routines for the visualization of 3D datasets of GCMs and of measurements along orbit. Daedalus MASE code is accompanied by a set of Jupyter Notebooks, incorporating all required theory, references, codes and plotting in a user-friendly environment. Daedalus MASE is developed and maintained at the Department for Electrical and Computer Engineering of the Democritus University of Thrace, with key contributions from several partner institutions.
Published: 2023

32. Bulk-preventing actions for SU(N) gauge theories

Author: Tobias Rindlisbacher, Kari Rummukainen, Ahmed Salami, Particle Physics and Astrophysics, Helsinki Institute of Physics, and Department of Physics
Subjects: High Energy Physics::Theory, High Energy Physics - Lattice, High Energy Physics::Lattice, High Energy Physics - Lattice (hep-lat), FOS: Physical sciences, 114 Physical sciences
Abstract: Lattice gauge field theories may suffer from unphysical "bulk" phase transitions at strong lattice gauge coupling. We introduce a one-parameter family of lattice SU(N) gauge actions which, when used in combination with an HMC update algorithm, prevents the appearance of the bulk phase transition. We briefly discuss the (presumed) mechanism behind the prevention of the bulk transition and present test results for different SU(N) gauge groups., Comment: 11 pages, 6 figures
Published: 2023
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33. Direct Observations of Electron Firehose Fluctuations in the Magnetic Reconnection Outflow

Author: G. Cozzani, Yu. V. Khotyaintsev, D. B. Graham, M. André, Department of Physics, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Plasma instabilities, spacecraft observations, plasma instabilities, electron firehose instability, 115 Astronomy, Space science, Fusion, Plasma and Space Physics, Electron firehose instability, Fusion, plasma och rymdfysik, Geophysics, Astronomi, astrofysik och kosmologi, Spacecraft observations, Space and Planetary Science, magnetic reconnection, Magnetic reconnection, Astronomy, Astrophysics and Cosmology, Collisionless plasmas, collisionless plasmas
Abstract: Electron temperature anisotropy-driven instabilities such as the electron firehose instability (EFI) are especially significant in space collisionless plasmas, where collisions are so scarce that wave-particle interactions are the leading mechanisms in the isotropization of the distribution function and energy transfer. Observational statistical studies provided convincing evidence in favor of the EFI constraining the electron distribution function and limiting the electron temperature anisotropy. Magnetic reconnection is characterized by regions of enhanced temperature anisotropy that could drive instabilities-including the electron firehose instability-affecting the particle dynamics and the energy conversion. However, in situ observations of the fluctuations generated by the EFI are still lacking and the interplay between magnetic reconnection and EFI is still largely unknown. In this study, we use high-resolution in situ measurements by the Magnetospheric Multiscale spacecraft to identify and investigate EFI fluctuations in the magnetic reconnection exhaust in the Earth's magnetotail. We find that the wave properties of the observed fluctuations largely agree with theoretical predictions of the non-propagating EF mode. These findings are further supported by comparison with the linear kinetic dispersion relation. Our results demonstrate that the magnetic reconnection outflow can be the seedbed of EFI and provide the first direct in situ observations of EFI-generated fluctuations.
Published: 2023

34. Exploring the optimality of approximate state preparation quantum circuits with a genetic algorithm

Author: Tom Rindell, Berat Yenilen, Niklas Halonen, Arttu Pönni, Ilkka Tittonen, Matti Raasakka, Particle Physics and Astrophysics, Ilkka Tittonen Group, RWTH Aachen University, Aalto University, Department of Electronics and Nanoengineering, and Aalto-yliopisto
Subjects: noisy intermediate-scale quantum, FOS: Computer and information sciences, Quantum Physics, Quantum state preparation, Noisy intermediate-scale quantum, Quantum circuit complexity, Computer Science - Neural and Evolutionary Computing, FOS: Physical sciences, General Physics and Astronomy, 114 Physical sciences, Genetic algorithm, NISQ, Nisq, quantum circuit complexity, genetic algorithm, quantum state preparation, Neural and Evolutionary Computing (cs.NE), Quantum Physics (quant-ph)
Abstract: We study the approximate state preparation problem on noisy intermediate-scale quantum (NISQ) computers by applying a genetic algorithm to generate quantum circuits for state preparation. The algorithm can account for the specific characteristics of the physical machine in the evaluation of circuits, such as the native gate set and qubit connectivity. We use our genetic algorithm to optimize the circuits provided by the low-rank state preparation algorithm introduced by Araujo et al., and find substantial improvements to the fidelity in preparing Haar random states with a limited number of CNOT gates. Moreover, we observe that already for a 5-qubit quantum processor with limited qubit connectivity and significant noise levels (IBM Falcon 5T), the maximal fidelity for Haar random states is achieved by a short approximate state preparation circuit instead of the exact preparation circuit. We also present a theoretical analysis of approximate state preparation circuit complexity to motivate our findings. Our genetic algorithm for quantum circuit discovery is freely available at https://github.com/beratyenilen/qc-ga ., Comment: 22 pages, 4 figures; version 2 changes: title changed, numerical analysis extended to 1000 random states, references added, other minor improvements, conclusions remain unaltered
Published: 2023

35. Measurement of the inclusive and differential t t ¯ $$ \overline{t} $$ γ cross sections in the single-lepton channel and EFT interpretation at s $$ \sqrt{s} $$ = 13 TeV

Author: Tumasyan, A., Adam, W., Andrejkovic, J. W., Bergauer, T., Chatterjee, S., Dragicevic, M., Del Valle, A. Escalante, Fruhwirth, R., Jeitler, M., Krammer, N., Lechner, L., Liko, D., Mikulec, I, Paulitsch, P., Pitters, F. M., Schieck, J., Schofbeck, R., Spanring, M., Templ, S., Waltenberger, W., Wulz, C-E, Chekhovsky, V, Litomin, A., Makarenko, V, Darwish, M. R., De Wolf, E. A., Janssen, X., Kello, T., Lelek, A., Sfar, H. Rejeb, Van Mechelen, P., Van Putte, S., Van Remortel, N., Blekman, F., Bols, E. S., D'Hondt, J., De Clercq, J., Delcourt, M., El Faham, H., Lowette, S., Moortgat, S., Morton, A., Muller, D., Sahasransu, A. R., Tavernier, S., Van Doninck, W., Van Mulders, P., Stylianou, N., Beghin, D., Bilin, B., Clerbaux, B., De Lentdecker, G., Favart, L., Grebenyuk, A., Kalsi, A. K., Lee, K., Mahdavikhorrami, M., Makarenko, I, Moureaux, L., Petre, L., Popov, A., Postiau, N., Starling, E., Thomas, L., V, en Bemden, M., er Velde, C., Vanlaer, P., Vannerom, D., Wezenbeek, L., Gao, X., Cornelis, T., Dobur, D., Knolle, J., Lambrecht, L., Mestdach, G., Niedziela, M., Roskas, C., Samalan, A., Skovpen, K., Tytgat, M., Verbeke, W., Vermassen, B., Vit, M., Bethani, A., Bruno, G., Bury, F., Caputo, C., David, P., Delaere, C., Donertas, I. S., Giammanco, A., Jaffel, K., Jain, Sa, Lemaitre, V, Mondal, K., Prisci, Aro, J., Taliercio, A., Teklishyn, M., Tran, T. T., Vischia, P., Wertz, S., Alves, G. A., Hensel, C., Moraes, A., Alda Junior, W. L., Gallo Pereira, M. Alves, Ferreira Filho, M. Barroso, Malbouisson, H. Br, Carvalho, W., Chinellato, J., Da Costa, E. M., Da Silveira, G. G., Damiao, D. De Jesus, De Souza, S. Fonseca, Figueiredo, D. Matos, Herrera, C. Mora, Amarilo, K. Mota, Mundim, L., Nogima, H., Teles, P. Rebello, Santoro, A., Silva Do Amaral, S. M., Sznajder, A., Thiel, M., Da Silva De Araujo, F. Torres, Pereira, A. Vilela, Bernardes, C. A., Calligaris, L., Fern, ez Perez Tomei, T. R., Gregores, E. M., Lemos, D. S., Mercadante, P. G., Novaes, S. F., Padula, S, Ra, S., Aleks, Rov, A., Antchev, G., Hadjiiska, R., Iaydjiev, P., Misheva, M., Rodozov, M., Shopova, M., Sultanov, G., Dimitrov, A., Ivanov, T., Litov, L., Pavlov, B., Petkov, P., Petrov, A., Cheng, T., Guo, Q., Javaid, T., Mittal, M., Wang, H., Yuan, L., Ahmad, M., Bauer, G., Dozen, C., Hu, Z., Martins, J., Wang, Y., Yi, K., Chapon, E., Chen, G. M., Chen, H. S., Chen, M., Iemmi, F., Kapoor, A., Leggat, D., Liao, H., Liu, Z-A, Milosevic, V, Monti, F., Sharma, R., Tao, J., Thomas-wilsker, J., Wang, J., Zhang, H., Zhang, S., Zhao, J., Agapitos, A., Ban, Y., Chen, C., Huang, Q., Levin, A., Li, Q., Lyu, X., Mao, Y., Qian, S. J., Wang, D., Wang, Q., Xiao, J., Lu, M., You, Z., Okawa, H., Lin, Z., Xiao, M., Avila, C., Cabrera, A., Florez, C., Fraga, J., Sarkar, A., Segura Delgado, M. A., Mejia Guisao, J., Ramirez, F., Ruiz Alvarez, J. D., Salazar Gonzalez, C. A., Giljanovic, D., Godinovic, N., Lelas, D., Puljak, I, Antunovic, Z., Kovac, M., Sculac, T., Brigljevic, V, Ferencek, D., Majumder, D., Roguljic, M., Starodumov, A., Susa, T., Attikis, A., Christoforou, K., Erodotou, E., Ioannou, A., Kole, G., Kolosova, M., Konstantinou, S., Mousa, J., Nicolaou, C., Ptochos, F., Razis, P. A., Rykaczewski, H., Saka, H., Finger, M., Finger Jr, M. Jr, Kveton, A., Ayala, E., Carrera Jarrin, E., Abdalla, H., Khalil, S., Lotfy, A., Mahmoud, M. A., Bhowmik, S., De Oliveira, A. Carvalho Antunes, Dewanjee, R. K., Ehataht, K., Kadastik, M., N, An, S., Nielsen, C., Pata, J., Raidal, M., Tani, L., Veelken, C., Eerola, P., Forthomme, L., Kirschenmann, H., Osterberg, K., Voutilainen, M., Bharthuar, S., Brucken, E., Garcia, F., Havukainen, J., Kim, M. S., Kinnunen, R., Lampen, T., Lassila-Perini, K., Lehti, S., Linden, T., Lotti, M., Martikainen, L., Myllymaki, M., Ott, J., Siikonen, H., Tuominen, E., Tuominiemi, J., Luukka, P., Petrow, H., Tuuva, T., Amendola, C., Besancon, M., Couderc, F., Dejardin, M., Denegri, D., Faure, J. L., Ferri, F., Ganjour, S., Givernaud, A., Gras, P., de Monchenault, G. Hamel, Jarry, P., Lenzi, B., Locci, E., Malcles, J., R, Er, J., Rosowsky, A., Sahin, M. O., Savoy-Navarro, A., Titov, M., G. B., Yu, Mijuskovic, J., Ahuja, S., Beaudette, F., Bonanomi, M., Perraguin, A. Buchot, Busson, P., Cappati, A., Charlot, C., Davignon, O., Diab, B., Falmagne, G., Ghosh, S., de Cassagnac, R. Granier, Hakimi, A., Kucher, I, Nguyen, M., Och, O, C., Paganini, P., Rembser, J., Salerno, R., Sauvan, J. B., Sirois, Y., Zabi, A., Zghiche, A., Agram, J-L, Andrea, J., Apparu, D., Bloch, D., Bourgatte, G., Brom, J-M, Chabert, E. C., Collard, C., Darej, D., Fontaine, J-C, Goerlach, U., Grimault, C., Le Bihan, A-C, Nibigira, E., Van Hove, P., Asilar, E., Beauceron, S., Bernet, C., Boudoul, G., Camen, C., Carle, A., Chanon, N., Contardo, D., Depasse, P., El Mamouni, H., Fay, J., Gascon, S., Gouzevitch, M., Ille, B., Laktineh, I. B., Lattaud, H., Lesauvage, A., Lethuillier, M., Mirabito, L., Perries, S., Shchablo, K., Sordini, V, Torterotot, L., Touquet, G., er Donckt, M., Viret, S., Lomidze, I, Toriashvili, T., Tsamalaidze, Z., Mestvirishvili, A., Feld, L., Klein, K., Lipinski, M., Meuser, D., Pauls, A., Rauch, M. P., Roewert, N., Schulz, J., Teroerde, M., Dodonova, A., Eliseev, D., Erdmann, M., Fackeldey, P., Fischer, B., Hebbeker, T., Hoepfner, K., Ivone, F., Keller, H., Mastrolorenzo, L., Merschmeyer, M., Meyer, A., Mocellin, G., Mondal, S., Mukherjee, S., Noll, D., Novak, A., Pook, T., Pozdnyakov, A., Rath, Y., Reithler, H., Roemer, J., Schmidt, A., Schuler, S. C., Sharma, A., Vigilante, L., Wiedenbeck, S., Zaleski, S., Borras, K., Kasem, A., Coubez, X., Dziwok, C., Fluegge, G., Ahmad, W. Haj, Hlushchenko, O., Kress, T., Nowack, A., Pistone, C., Pooth, O., Roy, D., Sert, H., Stahl, A., Ziemons, T., Petersen, H. Aarup, Martin, M. Aldaya, Asmuss, P., Babounikau, I, Baxter, S., Behnke, O., Martinez, A. Bermudez, Bhattacharya, S., Bin Anuar, A. A., Botta, V, Brunner, D., Campbell, A., Cardini, A., Cheng, C., Colombina, F., Rodriguez, S. Consuegra, Silva, G. Correia, Danilov, V, Didukh, L., Eckerlin, G., Eckstein, D., Banos, L. I. 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Tkaczyk S., Tran N.V., Uplegger L., Vaandering E.W., Weber H.A., Acosta D., Avery P., Bourilkov D., Cadamuro L., Cherepanov V., Errico F., Field R.D., Guerrero D., Joshi B.M., Kim M., Koenig E., Konigsberg J., Korytov A., Lo K.H., Matchev K., Menendez N., Mitselmakher G., Muthirakalayil Madhu A., Rawal N., Rosenzweig D., Rosenzweig S., Shi K., Sturdy J., Yigitbasi E., Zuo X., Adams T., Askew A., Habibullah R., Hagopian V., Johnson K.F., Khurana R., Kolberg T., Martinez G., Prosper H., Schiber C., Viazlo O., Yohay R., Zhang J., Baarmand M.M., Butalla S., Elkafrawy T., Hohlmann M., Kumar Verma R., Noonan D., Rahmani M., Yumiceva F., Adams M.R., Becerril Gonzalez H., Cavanaugh R., Chen X., Dittmer S., Evdokimov O., Gerber C.E., Hangal D.A., Hofman D.J., Merrit A.H., Mills C., Oh G., Roy T., Rudrabhatla S., Tonjes M.B., Varelas N., Viinikainen J., Wang X., Wu Z., Ye Z., Alhusseini M., Dilsiz K., Gandrajula R.P., Koseyan O.K., Merlo J.-P., Mestvirishvili A., Nachtman J., Ogul H., Onel Y., Penzo A., Snyder C., Tiras E., Amram O., Blumenfeld B., Corcodilos L., Davis J., Eminizer M., Gritsan A.V., Kyriacou S., Maksimovic P., Roskes J., Swartz M., Vami T.A., Abreu A., Anguiano J., Baldenegro Barrera C., Baringer P., Bean A., Bylinkin A., Flowers Z., Isidori T., King J., Krintiras G., Kropivnitskaya A., Lazarovits M., Lindsey C., Marquez J., Minafra N., Murray M., Nickel M., Rogan C., Royon C., Salvatico R., Sanders S., Schmitz E., Smith C., Tapia Takaki J.D., Warner Z., Williams J., Wilson G., Duric S., Ivanov A., Kaadze K., Kim D., Maravin Y., Mitchell T., Modak A., Nam K., Rebassoo F., Wright D., Adams E., Baden A., Baron O., Belloni A., Eno S.C., Hadley N.J., Jabeen S., Kellogg R.G., Koeth T., Mignerey A.C., Nabili S., Seidel M., Skuja A., Wang L., Wong K., Abercrombie D., Andreassi G., Bi R., Brandt S., Busza W., Cali I.A., D'Alfonso M., Eysermans J., Freer C., Gomez Ceballos G., Goncharov M., Harris P., Hu M., Klute M., Kovalskyi D., Krupa J., Lee Y.-J., Maier B., Mironov C., Paus C., Rankin D., Roland C., Roland G., Shi Z., Stephans G.S.F., Tatar K., Wang Z., Wyslouch B., Chatterjee R.M., Evans A., Hansen P., Hiltbrand J., Krohn M., Kubota Y., Mans J., Revering M., Rusack R., Saradhy R., Schroeder N., Strobbe N., Wadud M.A., Bloom K., Bryson M., Claes D.R., Fangmeier C., Finco L., Golf F., Joo C., Kravchenko I., Musich M., Reed I., Siado J.E., Snow G.R., Tabb W., Yan F., Agarwal G., Bandyopadhyay H., Hay L., Iashvili I., Kharchilava A., McLean C., Nguyen D., Pekkanen J., Rappoccio S., Williams A., Alverson G., Barberis E., Haddad Y., Hortiangtham A., Li J., Madigan G., Marzocchi B., Morse D.M., Nguyen V., Orimoto T., Parker A., Skinnari L., Tishelman-Charny A., Wamorkar T., Wang B., Wisecarver A., Wood D., Bueghly J., Chen Z., Gilbert A., Gunter T., Hahn K.A., Liu Y., Odell N., Schmitt M.H., Velasco M., Band R., Bucci R., Das A., Dev N., Goldouzian R., Hildreth M., Hurtado Anampa K., Jessop C., Lannon K., Lawrence J., Loukas N., Lutton D., Marinelli N., Mcalister I., McCauley T., Meng F., Mohrman K., Musienko Y., Ruchti R., Siddireddy P., Townsend A., Wayne M., Wightman A., Wolf M., Zarucki M., Zygala L., Bylsma B., Cardwell B., Durkin L.S., Francis B., Hill C., Nunez Ornelas M., Wei K., Winer B.L., Yates B.R., Addesa F.M., Bonham B., Das P., Dezoort G., Elmer P., Frankenthal A., Greenberg B., Haubrich N., Higginbotham S., Kalogeropoulos A., Kopp G., Kwan S., Lange D., Lucchini M.T., Marlow D., Mei K., Ojalvo I., Olsen J., Palmer C., Stickland D., Tully C., Norberg S., Bakshi A.S., Barnes V.E., Chawla R., Das S., Gutay L., Jones M., Jung A.W., Karmarkar S., Liu M., Negro G., Neumeister N., Paspalaki G., Peng C.C., Piperov S., Purohit A., Schulte J.F., Stojanovic M., Thieman J., Wang F., Xiao R., Xie W., Dolen J., Parashar N., Baty A., Decaro M., Dildick S., Ecklund K.M., Freed S., Gardner P., Geurts F.J.M., Li W., Padley B.P., Redjimi R., Shi W., Stahl Leiton A.G., Zhang L., Bodek A., de Barbaro P., Demina R., Dulemba J.L., Fallon C., Ferbel T., Galanti M., Garcia-Bellido A., Hindrichs O., Khukhunaishvili A., Ranken E., Taus R., Chiarito B., Chou J.P., Gandrakota A., Gershtein Y., Halkiadakis E., Hart A., Heindl M., Karacheban O., Laflotte I., Lath A., Montalvo R., Nash K., Osherson M., Salur S., Schnetzer S., Somalwar S., Stone R., Thayil S.A., Thomas S., Acharya H., Delannoy A.G., Spanier S., Bouhali O., Dalchenko M., Delgado A., Eusebi R., Gilmore J., Huang T., Kamon T., Luo S., Malhotra S., Mueller R., Overton D., Rathjens D., Safonov A., Akchurin N., Damgov J., Hegde V., Kunori S., Lamichhane K., Mengke T., Muthumuni S., Peltola T., Volobouev I., Whitbeck A., Appelt E., Greene S., Gurrola A., Johns W., Melo A., Ni H., Padeken K., Romeo F., Sheldon P., Tuo S., Velkovska J., Arenton M.W., Cox B., Cummings G., Hakala J., Hirosky R., Joyce M., Ledovskoy A., Li A., Neu C., Tannenwald B., White S., Wolfe E., Harr R., Poudyal N., Black K., Bose T., Buchanan J., Caillol C., Dasu S., De Bruyn I., Everaerts P., Fienga F., Galloni C., He H., Herndon M., Herve A., Hussain U., Lanaro A., Loeliger A., Loveless R., Madhusudanan Sreekala J., Mallampalli A., Mohammadi A., Pinna D., Savin A., Shang V., Smith W.H., Teague D., Trembath-reichert S., Vetens W., Belforte, S., Candelise, V., Casarsa, M., Cossutti, F., DA ROLD, A., DELLA RICCA, G., Sorrentino, G., Vazzoler, F., ET AL (the CMS, Collaboration), Department of Physics, Helsinki Institute of Physics, Damarseçkin, serdal, Physics, Elementary Particle Physics, Faculty of Sciences and Bioengineering Sciences, Vriendenkring VUB, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), CMS, Yerevan Physics Institute, Institut für Hochenergiephysik, Institute for Nuclear Problems, Universiteit Antwerpen, Vrije Universiteit Brussel, Université Libre de Bruxelles, Ghent University, Université Catholique de Louvain, Centro Brasileiro de Pesquisas Fisicas, Universidade do Estado do Rio de Janeiro (UERJ), Universidade Estadual Paulista (UNESP), Universidade Federal do ABC (UFABC), Bulgarian Academy of Sciences, University of Sofia, Beihang University, Tsinghua University, Institute of High Energy Physics, Peking University, Sun Yat-Sen University, Institute of Modern Physics and Key Laboratory of Nuclear Physics and Ion- beam Application (MOE) — Fudan University, Zhejiang University, Universidad de Los Andes, Universidad de Antioquia, Mechanical Engineering and Naval Architecture, Faculty of Science, Institute Rudjer Boskovic, University of Cyprus, Charles University, Escuela Politecnica Nacional, Universidad San Francisco de Quito, Egyptian Network of High Energy Physics, Fayoum University, National Institute of Chemical Physics and Biophysics, University of Helsinki, Lappeenranta University of Technology, Université Paris-Saclay, Institut Polytechnique de Paris, IPHC UMR 7178, Institut de Physique des 2 Infinis de Lyon (IP2I), Georgian Technical University, I. Physikalisches Institut, III. Physikalisches Institut A, III. Physikalisches Institut B, Deutsches Elektronen-Synchrotron, University of Hamburg, Karlsruher Institut fuer Technologie, NCSR Demokritos, National and Kapodistrian University of Athens, National Technical University of Athens, University of Ioánnina, Eötvös Loránd University, Wigner Research Centre for Physics, Institute of Nuclear Research ATOMKI, University of Debrecen, MATE Institute of Technology, Indian Institute of Science (IISc), HBNI, Panjab University, University of Delhi, Indian Institute of Technology Madras, Bhabha Atomic Research Centre, Tata Institute of Fundamental Research-A, Tata Institute of Fundamental Research-B, Indian Institute of Science Education and Research (IISER), Isfahan University of Technology, Institute for Research in Fundamental Sciences (IPM), University College Dublin, INFN Sezione di Bari, Università di Bari, Politecnico di Bari, INFN Sezione di Bologna, Università di Bologna, INFN Sezione di Catania, Università di Catania, INFN Sezione di Firenze, Università di Firenze, INFN Laboratori Nazionali di Frascati, INFN Sezione di Genova, Università di Genova, INFN Sezione di Milano-Bicocca, Università di Milano-Bicocca, INFN Sezione di Napoli, Università di Napoli ‘Federico II’, Università della Basilicata, Università G. Marconi, INFN Sezione di Padova, Università di Padova, INFN Sezione di Pavia, Università di Pavia, INFN Sezione di Perugia, Università di Perugia, INFN Sezione di Pisa, Università di Pisa, Scuola Normale Superiore di Pisa, Università di Siena, INFN Sezione di Roma, Sapienza Università di Roma, INFN Sezione di Torino, Università di Torino, Università del Piemonte Orientale, INFN Sezione di Trieste, Università di Trieste, Kyungpook National University, Institute for Universe and Elementary Particles, Hanyang University, Korea University, Kyung Hee University, Sejong University, Seoul National University, University of Seoul, Yonsei University, Sungkyunkwan University, American University of the Middle East (AUM), Riga Technical University, Vilnius University, Universiti Malaya, Universidad de Sonora (UNISON), Centro de Investigacion y de Estudios Avanzados del IPN, Universidad Iberoamericana, Benemerita Universidad Autonoma de Puebla, University of Montenegro, University of Auckland, University of Canterbury, Quaid-I-Azam University, Electronics and Telecommunications, National Centre for Nuclear Research, University of Warsaw, Laboratório de Instrumentação e Física Experimental de Partículas, Joint Institute for Nuclear Research, Petersburg Nuclear Physics Institute, Institute for Nuclear Research, Institute for Theoretical and Experimental Physics named by A.I. Alikhanov of NRC ‘Kurchatov Institute’, Moscow Institute of Physics and Technology, National Research Nuclear University ‘Moscow Engineering Physics Institute’ (MEPhI), P.N. Lebedev Physical Institute, Lomonosov Moscow State University, Novosibirsk State University (NSU), Institute for High Energy Physics of National Research Centre ‘Kurchatov Institute’, National Research Tomsk Polytechnic University, Tomsk State University, University of Belgrade: Faculty of Physics and VINCA Institute of Nuclear Sciences, Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT), Universidad Autónoma de Madrid, Instituto Universitario de Ciencias y Tecnologías Espaciales de Asturias (ICTEA), CSIC-Universidad de Cantabria, University of Colombo, University of Ruhuna, European Organization for Nuclear Research, Paul Scherrer Institut, ETH Zurich — Institute for Particle Physics and Astrophysics (IPA), Universität Zürich, National Central University, National Taiwan University (NTU), Science and Art Faculty, Physics Department, Bogazici University, Istanbul Technical University, Istanbul University, Institute for Scintillation Materials of National Academy of Science of Ukraine, Kharkov Institute of Physics and Technology, University of Bristol, Rutherford Appleton Laboratory, Imperial College, Brunel University, Baylor University, Catholic University of America, The University of Alabama, Boston University, Brown University, Davis, University of California, Riverside, San Diego, Santa Barbara — Department of Physics, California Institute of Technology, Carnegie Mellon University, University of Colorado Boulder, Cornell University, Fermi National Accelerator Laboratory, University of Florida, Florida State University, Florida Institute of Technology, University of Illinois at Chicago (UIC), The University of Iowa, Johns Hopkins University, The University of Kansas, Kansas State University, Lawrence Livermore National Laboratory, University of Maryland, Massachusetts Institute of Technology, University of Minnesota, University of Nebraska-Lincoln, State University of New York at Buffalo, Northeastern University, Northwestern University, University of Notre Dame, The Ohio State University, Princeton University, University of Puerto Rico, Purdue University, Purdue University Northwest, Rice University, University of Rochester, The State University of New Jersey, University of Tennessee, Texas A&M University, Texas Tech University, Vanderbilt University, University of Virginia, Wayne State University, University of Wisconsin — Madison, TU Wien, Technology and Maritime Transport, Universidade Estadual de Campinas (UNICAMP), Federal University of Rio Grande do Sul, University of Chinese Academy of Sciences, Universidade Federal de Mato Grosso do Sul (UFMS), Nanjing Normal University Department of Physics, Cairo University, Zewail City of Science and Technology, Université de Haute Alsace, Tbilisi State University, Erzincan Binali Yildirim University, Brandenburg University of Technology, Assiut University, IIT Bhubaneswar, Institute of Physics, G.H.G. Khalsa College, Shoolini University, University of Hyderabad, University of Visva-Bharati, Indian Institute of Technology (IIT), Sharif University of Technology, University of Science and Technology of Mazandaran, Energy and Sustainable Economic Development, Centro Siciliano di Fisica Nucleare e di Struttura Della Materia, Consiglio Nazionale delle Ricerche — Istituto Officina dei Materiali, Consejo Nacional de Ciencia y Tecnología, Institute of Nuclear Physics of the Uzbekistan Academy of Sciences, St. Petersburg State Polytechnical University, Budker Institute of Nuclear Physics, University of Belgrade, Sri Lanka, Ecole Polytechnique Fédérale Lausanne, Stefan Meyer Institute for Subatomic Physics, IN2P3-CNRS, Şırnak University, Research Center of Experimental Health Science, Konya Technical University, Faculty of Engineering, Piri Reis University, Adiyaman University, Ozyegin University, Izmir Institute of Technology, Necmettin Erbakan University, Bozok Universitetesi Rektörlügü, Marmara University, Milli Savunma University, Kafkas University, Istanbul Bilgi University, Hacettepe University, University of Southampton, IPPP Durham University, Bethel University, Karamanoğlu Mehmetbey University, Ain Shams University, Bingol University, Sinop University, Erciyes University, Texas A&M University at Qatar, Università di Trento, CERN, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)
Subjects: transverse momentum [photon], moment: dipole, quark: hadronization, lepton, 13000 GeV-cms, QC770-798, GeV, pair production [top], transverse momentum dependence, 01 natural sciences, High Energy Physics - Experiment, rapidity dependence, Physics, Particles & Fields, effective field theory, Hadron-Hadron scattering (experiments), scattering [p p], [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], dipole [moment], Nuclear Experiment, 0105 Mathematical Physics, CMS, Physics, photon, higher-order: 1, dipole: electromagnetic, perturbation theory: higher-order, hadron-hadron scattering (experiments), TOP, photon: transverse momentum, Nuclear & Particles Physics, dipole, electromagnetic, higher-order, 1, CERN LHC Coll, Top physics, kinematics, associated production [photon], differential cross section, Physical Sciences, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, PARTICLE PHYSICS, colliding beams [p p], top: pair production, Particle Physics - Experiment, 1 [higher-order], ((n)jet lepton) [final state], perturbation theory [quantum chromodynamics], p p: scattering, Nuclear and High Energy Physics, PAIR PRODUCTION, p p, scattering, education, final state: ((n)jet lepton), transverse momentum, electromagnetic [dipole], 114 Physical sciences, differential cross section: measured, measured [differential cross section], Nuclear and particle physics. Atomic energy. Radioactivity, quantum chromodynamics, 0103 physical sciences, TeV, ddc:530, quantum chromodynamics: perturbation theory, 010306 general physics, 0206 Quantum Physics, moment, dipole, Science & Technology, rapidity [photon], hep-ex, LARGE HADRON COLLIDER, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, higher-order [perturbation theory], photon: associated production, hadronization [quark], rapidity, Physics and Astronomy, quark, hadronization, photon: rapidity, High Energy Physics::Experiment, p p: colliding beams, experimental results
Abstract: The production cross section of a top quark pair in association with a photon is measured in proton-proton collisions at a center-of-mass energy of 13 TeV. The data set, corresponding to an integrated luminosity of 137 fb$^{-1}$, was recorded by the CMS experiment during the 2016-2018 data taking of the LHC. The measurements are performed in a fiducial volume defined at the particle level. Events with an isolated, highly energetic lepton, at least three jets from the hadronization of quarks, among which at least one is b tagged, and one isolated photon are selected. The inclusive fiducial $\mathrm{t\overline{t}}\gamma$ cross section, for a photon with transverse momentum greater than 20 GeV and pseudorapidity $\lvert \eta\rvert$ $\lt$ 1.4442, is measured to be 798 $\pm$ 7 (stat) $\pm$ 48 (syst) fb, in good agreement with the prediction from the standard model at next-to-leading order in quantum chromodynamics. The differential cross sections are also measured as a function of several kinematic observables and interpreted in the framework of the standard model effective field theory (EFT), leading to the most stringent direct limits to date on anomalous electromagnetic dipole moment interactions of the top quark and the photon., Comment: Replaced with the published version. Added the journal reference and DOI. All the figures and tables can be found at http://cms-results.web.cern.ch/cms-results/public-results/publications/TOP-18-010 (CMS Public Pages)
Published: 2021

36. ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions – V. Hierarchical fragmentation and gas dynamics in IRDC G034.43+00.24

Author: Ken'ichi Tatematsu, Eswaraiah Chakali, Feng-Wei Xu, Mika Juvela, E. Mannfors, Qiu-Yi Luo, Qizhou Zhang, S. N. Zhang, Sheng-Li Qin, Lokesh K. Dewangan, Ke Wang, L. Viktor Tóth, Junzhi Wang, Tie Liu, Rong Liu, Zhiyuan Ren, Leonardo Bronfman, Paul F. Goldsmith, T. Baug, Jin-Zeng Li, Shanghuo Li, Pak Shing Li, Jianwen Zhou, X.-W. Liu, Xi Chen, Chang Won Lee, Somnath Dutta, Hong-Li Liu, Yong Zhang, Di Li, Anandmayee Tej, Chao Zhang, Archana Soam, Yuefang Wu, Anindya Saha, Amelia M. Stutz, Namitha Issac, Mengyao Tang, Department of Physics, and Particle Physics and Astrophysics
Subjects: ISM: individual objects: G034.43+00.24, Astrophysics::High Energy Astrophysical Phenomena, stars: kinematics and dynamics, Continuum (design consultancy), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Star (graph theory), ISM: clouds, 01 natural sciences, MAGNETIC-FIELDS, Virial theorem, CLUMPS, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, DENSE, Infrared dark cloud, ACCRETION, COLLAPSE, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, stars: formation, 010308 nuclear & particles physics, Star formation, Fragmentation (computing), PROTOSTARS, Astronomy and Astrophysics, DRIVEN, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, Accretion (astrophysics), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Millimeter, MOLECULAR OUTFLOWS
Abstract: We present new 3-mm continuum and molecular lines observations from the ATOMS survey towards the massive protostellar clump, MM1, located in the filamentary infrared dark cloud (IRDC), G034.43+00.24 (G34). The lines observed are the tracers of either dense gas (e.g. HCO+/H13CO+ J = 1-0) or outflows (e.g. CS J = 2-1). The most complete picture to date of seven cores in MM1 is revealed by dust continuum emission. These cores are found to be gravitationally bound, with virial parameter, $\alpha_{vir}, Comment: 14 pages with 6 figures, and in press
Published: 2021

37. First-order electroweak phase transitions : A nonperturbative update

Author: Oliver Gould, Sinan Güyer, Kari Rummukainen, Helsinki Institute of Physics, General Division (Department of Physics) (-2009), Department of Physics, Mind and Matter, and Particle Physics and Astrophysics
Subjects: High Energy Physics - Phenomenology, High Energy Physics - Lattice, Cosmology and Nongalactic Astrophysics (astro-ph.CO), High Energy Physics - Phenomenology (hep-ph), High Energy Physics - Lattice (hep-lat), FOS: Physical sciences, 114 Physical sciences, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We study first-order electroweak phase transitions nonperturbatively, assuming any particles beyond the Standard Model are sufficiently heavy to be integrated out at the phase transition. Utilising high temperature dimensional reduction, we perform lattice Monte-Carlo simulations to calculate the main quantities characterising the transition: the critical temperature, the latent heat, the surface tension and the bubble nucleation rate, updating and extending previous lattice studies. We focus on the region where the theory gives first-order phase transitions due to an effective reduction in the Higgs self-coupling and give a detailed comparison with perturbation theory., Comment: 25 pages, 20 figures, for videos of bubble nucleation see https://doi.org/10.5281/zenodo.6548608, and for the dataset see https://doi.org/10.5281/zenodo.6539259
Published: 2022

38. Solar energetic particle time series analysis with Python

Author: Christian Palmroos, Jan Gieseler, Nina Dresing, Diana E. Morosan, Eleanna Asvestari, Aleksi Yli-Laurila, Daniel J. Price, Saku Valkila, Rami Vainio, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Physics - Space Physics, Astrophysics - Solar and Stellar Astrophysics, FOS: Physical sciences, Astronomy and Astrophysics, 115 Astronomy, Space science, 114 Physical sciences, Space Physics (physics.space-ph), Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: Solar Energetic Particles (SEPs) are charged particles accelerated within the solar atmosphere or the interplanetary space by explosive phenomena such as solar flares or Coronal Mass Ejections (CMEs). Once injected into the interplanetary space, they can propagate towards Earth, causing space weather related phenomena. For their analysis, interplanetary in situ measurements of charged particles are key. The recently expanded spacecraft fleet in the heliosphere not only provides much-needed additional vantage points, but also increases the variety of missions and instruments for which data loading and processing tools are needed. This manuscript introduces a series of Python functions that will enable the scientific community to download, load, and visualize charged particle measurements of the current space missions that are especially relevant to particle research as time series or dynamic spectra. In addition, further analytical functionality is provided that allows the determination of SEP onset times as well as their inferred injection times. The full workflow, which is intended to be run within Jupyter Notebooks and can also be approachable for Python laymen, will be presented with scientific examples. All functions are written in Python, with the source code publicly available at GitHub under a permissive license. Where appropriate, available Python libraries are used, and their application is described.
Published: 2022

39. Euclid preparation : XXI. Intermediate-redshift contaminants in the search for z > 6 galaxies within the Euclid Deep Survey (vol 666, A200, 2022)

Author: Euclid Consortium, Department of Physics, Helsinki Institute of Physics, Doctoral Programme in Particle Physics and Universe Sciences, and Particle Physics and Astrophysics
Subjects: Addenda, Errata, Galaxies: high-redshift, Galaxies: evolution, Galaxies: photometry, 115 Astronomy, Space science, 114 Physical sciences
Abstract: This article is an erratum for: [https://doi.org/10.1051/0004-6361/202243950]
Published: 2022

40. Improved lattice method for determining entanglement measures in SU(N) gauge theories

Author: Tobias Rindlisbacher, Niko Jokela, Arttu Pönni, Kari Rummukainen, Ahmed Salami, Department of Physics, Helsinki Institute of Physics, Mind and Matter, and Particle Physics and Astrophysics
Subjects: High Energy Physics - Lattice, High Energy Physics - Lattice (hep-lat), FOS: Physical sciences, 114 Physical sciences
Abstract: The determination of entanglement measures in SU(N) gauge theories is a non-trivial task. With the so-called "replica trick", a family of entanglement measures, known as "R\'enyi entropies", can be determined with lattice Monte Carlo. Unfortunately, the standard implementation of the replica method for SU(N) lattice gauge theories suffers from a severe signal-to-noise ratio problem, rendering high-precision studies of R\'enyi entropies prohibitively expensive. In this work, we propose a method to overcome the signal-to-noise ratio problem and show some first results for SU(N) in 4 dimensions., Comment: 9 pages, 5 figures, contribution to the proceedings of the 39th International Symposium on Lattice Field Theory, 8th-13th August, 2022, Bonn, Germany
Published: 2022

41. Editorial : Sources and propagation of ultra-low frequency waves in planetary magnetospheres

Author: Turc, Lucile, Takahashi, Kazue, Sandhu, Jasmine K., Volwerk, Martin, Department of Physics, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: 115 Astronomy, Space science
Abstract: Non
Published: 2022

42. Observations of a Solar Energetic Particle Event From Inside and Outside the Coma of Comet 67P

Author: A. Wellbrock, G. H. Jones, N. Dresing, A. J. Coates, C. Simon Wedlund, H. Nilsson, B. Sanchez‐Cano, E. Palmerio, L. Turc, M. Myllys, P. Henri, C. Goetz, O. Witasse, T. A. Nordheim, K. Mandt, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Geophysics, Space and Planetary Science, comets, energetic particles, interactions with solar wind plasma and fields, ionospheres, 115 Astronomy, Space science, 114 Physical sciences, coronal mass ejections, planetary bow shocks
Abstract: Publisher Copyright: ©2022. The Authors. We analyze observations of a solar energetic particle (SEP) event at Rosetta's target comet 67P/Churyumov-Gerasimenko during 6–10 March 2015. The comet was 2.15 AU from the Sun, with the Rosetta spacecraft approximately 70 km from the nucleus placing it deep inside the comet's coma and allowing us to study its response. The Eastern flank of an interplanetary coronal mass ejection (ICME) also encountered Rosetta on 6 and 7 March. Rosetta Plasma Consortium data indicate increases in ionization rates, and cometary water group pickup ions exceeding 1 keV. Increased charge exchange reactions between solar wind ions and cometary neutrals also indicate increased upstream neutral populations consistent with enhanced SEP induced surface activity. In addition, the most intense parts of the event coincide with observations interpreted as an infant cometary bow shock, indicating that the SEPs may have enhanced the formation and/or intensified the observations. These solar transient events may also have pushed the cometopause closer to the nucleus. We track and discuss characteristics of the SEP event using remote observations by SOHO, WIND, and GOES at the Sun, in situ measurements at Solar Terrestrial Relations Observatory Ahead, Mars and Rosetta, and ENLIL modeling. Based on its relatively prolonged duration, gradual and anisotropic nature, and broad angular spread in the heliosphere, we determine the main particle acceleration source to be a distant ICME which emerged from the Sun on 6 March 2015 and was detected locally in the Martian ionosphere but was never encountered by 67P directly. The ICME's shock produced SEPs for several days which traveled to the in situ observation sites via magnetic field line connections.
Published: 2022

43. Interferometric imaging of the type IIIb and U radio bursts observed with LOFAR on 22 August 2017

Author: Bartosz Dabrowski, Katarzyna Mikuła, Paweł Flisek, Christian Vocks, PeiJin Zhang, Jasmina Magdalenić, Alexander Warmuth, Diana E. Morosan, Adam Froń, Richard A. Fallows, Mario M. Bisi, Andrzej Krankowski, Gottfried Mann, Leszek Błaszkiewicz, Eoin P. Carley, Peter T. Gallagher, Pietro Zucca, Paweł Rudawy, Marcin Hajduk, Kacper Kotulak, Tomasz Sidorowicz, Department of Physics, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Sun: radio radiation, Sun, FOS: Physical sciences, Astronomy and Astrophysics, Radio radiation, Sun: UV radiation, 115 Astronomy, Space science, UV radiation, Activity, Methods: observational, Astrophysics - Solar and Stellar Astrophysics, Sun: activity, Space and Planetary Science, Methods, Observational, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The Sun is the source of different types of radio bursts that are associated with solar flares, for example. Among the most frequently observed phenomena are type III solar bursts. Their radio images at low frequencies (below 100 MHz) are relatively poorly studied due to the limitations of legacy radio telescopes. We study the general characteristics of types IIIb and U with stria structure solar radio bursts in the frequency range of 20 - 80 MHz, in particular the source size and evolution in different altitudes, as well as the velocity and energy of electron beams responsible for their generation. In this work types IIIb and U with stria structure radio bursts are analyzed using data from the LOFAR telescope including dynamic spectra and imaging observations, as well as data taken in the X-ray range (GOES and RHESSI satellites) and in the extreme ultraviolet (SDO satellite). In this study we determined the source size limited by the actual shape of the contour at particular frequencies of type IIIb and U solar bursts in a relatively wide frequency band from 20 to 80 MHz. Two of the bursts seem to appear at roughly the same place in the studied active region and their source sizes are similar. It is different in the case of another burst, which seems to be related to another part of the magnetic field structure in this active region. The velocities of the electron beams responsible for the generation of the three bursts studied here were also found to be different., Astronomy & Astrophysics, in press; 9 pages, 6 figures
Published: 2022

44. Shape of the hot topological charge density spectral function

Author: Laine, M., Niemi, L., Procacci, S., Rummukainen, K., Helsinki Institute of Physics, Particle Physics and Astrophysics, Department of Physics, and Mind and Matter
Subjects: High Energy Physics - Phenomenology, Nuclear and High Energy Physics, High Energy Physics - Lattice, High Energy Physics - Phenomenology (hep-ph), 530 Physics, High Energy Physics - Lattice (hep-lat), FOS: Physical sciences, 114 Physical sciences
Abstract: After motivating an interest in the shape of the topological charge density spectral function in hot Yang-Mills theories, we estimate it with the help of thermally averaged classical real-time simulations, for $N_{\rm c} = 2,3$. After subtracting a perturbative contribution at large frequencies, we observe a non-trivial shape at small frequencies (a dip rather than a peak), interpolating smoothly towards the sphaleron rate at zero frequency. Possible frequency scales making an appearance in this shape are discussed. Implications for warm axion inflation and reheating, and for imaginary-time lattice measurements of the strong sphaleron rate, are recapitulated., Comment: 24 pages. v2: clarifications added, published version
Published: 2022

45. Single-spacecraft techniques for shock parameters estimation: A systematic approach

Author: Trotta, Domenico, Vuorinen, Laura, Hietala, Heli, Horbury, Timothy, Dresing, Nina, Gieseler, Jan, Kouloumvakos, Athanasios, Price, Daniel James, Valentini, Francesco, Kilpua, Emilia, Vainio, Rami, Department of Physics, Particle Physics and Astrophysics, Space Physics Research Group, Commission of the European Communities, and The Royal Society
Subjects: Science & Technology, INTERPLANETARY SHOCKS, WAVES, heliosphere, FOS: Physical sciences, Astronomy and Astrophysics, shock waves, spacecraft data, Astronomy & Astrophysics, 115 Astronomy, Space science, PERPENDICULAR SHOCKS, Space Physics (physics.space-ph), SIMULATIONS, REGION, python, space physics, Physics - Space Physics, physics.space-ph, SOLAR-WIND, Physical Sciences, collisionless shocks, 2D
Abstract: Spacecraft missions provide the unique opportunity to study the properties of collisionless shocks utilising in situ measurements. In the past years, several diagnostics have been developed to address key shock parameters using time series of magnetic field (and plasma) data collected by a single spacecraft crossing a shock front. A critical aspect of such diagnostics is the averaging process involved in the evaluation of upstream-downstream quantities. In this work, we discuss several of these techniques, with a particular focus on the shock obliquity (defined as the angle between the upstream magnetic field and the shock normal vector) estimation. We introduce a systematic variation of the upstream/downstream averaging windows, yielding to an ensemble of shock parameters, a useful tool to address the robustness of their estimation. This approach is first tested with a synthetic shock, compliant with the Rankine-Hugoniot jump conditions for a shock, including the presence of noise and disturbances. We then employ self-consistent, hybrid kinetic shock simulations to apply the diagnostics to virtual spacecraft crossing the shock front at various stages of its evolution, highlighting the role of shock-induced fluctuations in the parameters estimation. This approach has the strong advantage of retaining some important properties of collisionless shock while being able to set a known, nominal set of shock parameters. Finally, two recent observations of interplanetary shocks from the Solar Orbiter spacecraft are presented, and the approach is also tested on an interplanetary shock measured by the four spacecraft of the Magnetospheric Multiscale (MMS) mission. All the Python software developed and used for the diagnostics (SerPyShock) is made available for the public, including an example of parameter estimation for a shock wave recently observed in-situ by the Solar Orbiter spacecraft., Published in Frontiers in Astronomy and Space Sciences
Published: 2022

46. Energy Flux Through the Magnetopause During Flux Transfer Events in Hybrid-Vlasov 2D Simulations

Author: Matti Ala‐Lahti, Tuija I. Pulkkinen, Yann Pfau‐Kempf, Maxime Grandin, Minna Palmroth, Department of Physics, Space Physics Research Group, and Particle Physics and Astrophysics
Subjects: Vlasiator, Geophysics, Magnetopause, Reconnection, Solar wind-magnetosphere coupling, Flux transfer events, hybrid-Vlasov, General Earth and Planetary Sciences, 115 Astronomy, Space science, 114 Physical sciences
Abstract: Solar wind-magnetosphere coupling drives magnetospheric dynamic phenomena by enabling energy exchange between magnetospheric and solar wind plasmas. In this study, we examine two-dimensional noon-midnight meridional plane simulation runs of the global hybrid-Vlasov code Vlasiator with southward interplanetary magnetic field driving. We compute the energy flux, which consists of the Poynting flux and hydrodynamic energy flux components, through the Earth's magnetopause during flux transfer events (FTEs). The results demonstrate the spatiotemporal variations of the energy flux along the magnetopause during an FTE, associating the FTE leading (trailing) edge with an energy injection into (escape from) the magnetosphere on the dayside. Furthermore, FTEs traveling along the magnetopause transport energy to the nightside magnetosphere. We identify the tail lobes as a primary entry region for solar wind energy into the magnetosphere, consistent with results from global magnetohydrodynamic simulations and observations.
Published: 2022

47. Synthetic Next Generation Very Large Array line observations of a massive star-forming cloud

Author: M. Juvela, E. Mannfors, T. Liu, L. V. Tóth, Department of Physics, and Particle Physics and Astrophysics
Subjects: radio lines: ISM, Space and Planetary Science, Stars: formation, Astronomy and Astrophysics, 115 Astronomy, Space science, ISM: clouds, ISM: molecules, Stars: protostars
Abstract: Context. Studies of the interstellar medium and the pre-stellar cloud evolution require spectral line observations that have a high sensitivity and high angular and velocity resolution. Regions of high-mass star formation are particularly challenging because of line-of-sight confusion, inhomogeneous physical conditions, and potentially very high optical depths. Aims. We wish to quantify to what accuracy the physical conditions within a massive star-forming cloud can be determined from observations. We are particularly interested in the possibilities offered by the Next Generation Very Large Array (ngVLA) interferometer. Methods. We used data from a magnetohydrodynamic simulation of star formation in a high-density environment. We concentrated on the study of a filamentary structure that has physical properties similar to a small infrared-dark cloud. We produced synthetic observations for spectral lines observable with the ngVLA and analysed these to measure column density, gas temperature, and kinematics. Results were compared to ideal line observations and the actual 3D model. Results. For a nominal cloud distance of 4kpc, ngVLA provides a resolution of ~0.01 pc even in its most compact configuration. For abundant molecules, such as HCO+, NH3, N2H+, and CO isotopomers, cloud kinematics and structure can be mapped down to subarcsecond scales in just a few hours. For NH3, a reliable column density map could be obtained for the entire 15″ × 40″ cloud, even without the help of additional single-dish data, and kinetic temperatures are recovered to a precision of ~1 K. At higher frequencies, the loss of large-scale emission becomes noticeable. The line observations are seen to accurately trace the cloud kinematics, except for the largest scales, where some artefacts appear due to the filtering of low spatial frequencies. The line-of-sight confusion complicates the interpretation of the kinematics, and the usefulness of collapse indicators based on the expected blue asymmetry of optically thick lines is limited. Conclusions. The ngVLA will be able to provide accurate data on the small-scale structure and the physical and chemical state of star-forming clouds, even in high-mass star-forming regions at kiloparsec distances. Complementary single-dish data are still essential for estimates of the total column density and the large-scale kinematics.
Published: 2022

48. 2D Reconstruction of Magnetotail Electron Diffusion Region Measured by MMS

Author: Schroeder, J. M., Egedal, J., Cozzani, G., Khotyaintsev, Yu, Daughton, W., Denton, R. E., Burch, J. L., Khotyaintsev, Yu. V., Department of Physics, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Plasma Physics (physics.plasm-ph), Fusion, plasma och rymdfysik, Geophysics, Geofysik, Physics - Space Physics, Magnetic reconnection, Anomalous resistivity, FOS: Physical sciences, General Earth and Planetary Sciences, 115 Astronomy, Space science, Fusion, Plasma and Space Physics, Physics - Plasma Physics, Space Physics (physics.space-ph)
Abstract: Models for collisionless magnetic reconnection in near-Earth space are distinctly characterized as 2D or 3D. In 2D kinetic models, the frozen-in law for the electron fluid is usually broken by laminar dynamics involving structures set by the electron orbit size, while in 3D models the width of the electron diffusion region is broadened by turbulent effects. We present an analysis of in situ spacecraft observations from the Earth's magnetotail of a fortuitous encounter with an active reconnection region, mapping the observations onto a 2D spatial domain. While the event likely was perturbed by low-frequency 3D dynamics, the structure of the electron diffusion region remains consistent with results from a 2D kinetic simulation. As such, the event represents a unique validation of 2D kinetic, and laminar reconnection models., Comment: Accepted for publication in Geophysical Research Letters. Copyright 2022 American Geophysical Union. Further reproduction or electronic distribution is not permitted. 11 pages. 5 figures
Published: 2022

49. The BepiColombo Environment Radiation Monitor, BERM

Author: Pinto, Marco, Sanchez-Cano, Beatriz, Moissl, Richard, Benkhoff, Johannes, Cardoso, Carlota, Goncalves, Patricia, Assis, Pedro, Vainio, Rami, Oleynik, Philipp, Lehtolainen, Arto, Grande, Manuel, Marques, Arlindo, Department of Physics, and Particle Physics and Astrophysics
Subjects: Radiation monitor, Solar flares, BepiColombo, Berm, Energetic particles, Cruise science, Mercury, 115 Astronomy, Space science
Abstract: The BepiColombo Environment Radiation Monitor (BERM) on board the European Space Agency's Mercury Planetary Orbiter (MPO), is designed to measure the radiation environment encountered by BepiColombo. The instrument measures electrons with energies from similar to 150 keV to similar to 10 MeV, protons with energies from similar to 1.5 MeV to similar to 100 MeV, and heavy ions with Linear Energy Transfer from 1 to 50 MeV.mg(-1).cm(2). BERM is operated continuously, being responsible for monitoring the radiation levels during all phases of the mission, including the cruise, the planetary flybys of Earth, Venus and Mercury, and the Hermean environment. In this paper, we describe the scientific objectives, instrument design and calibration, and the in-flight scientific performance of BERM. Moreover, we provide the first scientific results obtained by BERM during the BepiColombo flyby of Earth in April 2020, and after the impact of a solar energetic particle event during the cruise phase in May 2021. We also discuss the future plans of the instrument including synergies with other instruments on the BepiColombo and on other missions.
Published: 2022

50. Contributions to Loss Across the Magnetopause During an Electron Dropout Event

Author: H. George, G. Reeves, G. Cunningham, M. M. H. Kalliokoski, E. Kilpua, A. Osmane, M. G. Henderson, S. K. Morley, S. Hoilijoki, M. Palmroth, Department of Physics, Particle Physics and Astrophysics, and Space Physics Research Group
Subjects: Drift orbit bifurcation, Geophysics, Space and Planetary Science, Dropout, 115 Astronomy, Space science, Radiation belts, 114 Physical sciences, Radial diffusion
Abstract: Dropout events are dramatic decreases in radiation belt electron populations that can occur in as little as 30 minutes. Loss to magnetopause due to a combination of magnetopause shadowing and outward radial transport plays a significant role in these events. We examine the dropout of relativistic electron populations during the October 2012 geomagnetic storm using simulated electron phase space density, evaluating the contribution of different processes to losses across the magnetopause. We compare loss contribution from outward transport calculated using a standard empirical radial diffusion model that assumes a dipolar geomagnetic field to an event-specific radial diffusion model evaluated with a non-dipolar geomagnetic field. We additionally evaluate the contribution of Shabansky type 1 particles, which bounce along magnetic field lines with local equatorial maxima, to the loss calculated during this event. We find that the empirical radial diffusion model with a dipolar background field underestimates the contribution of radial diffusion to this dropout event by up to 10% when compared to the event-specific, non-dipolar radial diffusion model. We additionally find that including Shabansky type 1 particles in the initial electron phase space density, that is, allowing some magnetic field lines distorted from the typical single-minima configuration in drift shell construction, increases the calculated loss by an average of 0.75%. This shows that the treatment of the geomagnetic field significantly impacts the calculation of electron losses to the magnetopause during dropout events, with the non-dipolar treatment of radial diffusion being essential to accurately quantify the loss of outer radiation belt populations.
Published: 2022

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