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74,424 results on '"Physics"'

1. Decomposition of Benzene during Impacts in N2-dominated Atmospheres

Author: Lukáš Petera, Antonín Knížek, Vojtěch Laitl, and Martin Ferus
Subjects: Space and Planetary Science, Physics, Astronomy and Astrophysics
Abstract: Benzene is a simple neutral aromatic compound found in molecular clouds, comets, and planetary atmospheres. It has been confirmed on Jupiter, Saturn, Titan, and is expected on exoplanets. In this paper, the decomposition of benzene in a simulated asteroid or comet impact into an N2-dominated atmosphere was investigated. The impact plasma was simulated with laser-induced dielectric breakdown and the gas phase decomposition products were observed using high-resolution Fourier transform infrared spectroscopy. The gas phase decomposition products involve mainly HCN, C2H2, and smaller amounts of CH4 with yields of 3.1%–24.0%, 0–11.7%, and 0.5%–3.3%, respectively. Furthermore, in presence of water, benzene also produces CO and CO2 with yields of 2.4%–35.1% and 0.01%–4.8%, respectively. The oxidation state of the product mixture is proportional to the water content. Apart from that, a black-brownish solid phase is formed during the experiments, which makes up about 60% of the original carbon content. Our results therefore show that in anoxic N2-dominated planetary atmospheres, impacts might lead to the depletion of benzene and the formation of HCN, C2H2, and CH4 and, in the presence of water, to the formation of CO and CO2.
Published: 2023

2. A Gravitational-wave Measurement of the Hubble Constant Following the Second Observing Run of Advanced LIGO and Virgo

Author: G. Pagliaroli, Kevin Barkett, Denis Martynov, Marco Bazzan, C. Ingram, L. Pinard, Nicolas Sanchis-Gual, I. Belahcene, A. K. Y. Li, Archana Pai, F. Paoletti, P. Ruggi, G. Vajente, S. M. Gaebel, C. Kr mer, K. W. Chung, I. Dorrington, I. Di Palma, A. Mullavey, T. J. N. Nelson, Filip Morawski, Xiaohui Fan, Richard O'Shaughnessy, B. Barr, B. D. Lackey, G. Eddolls, A. Cumming, P. Grassia, Kipp Cannon, F. Di Renzo, M. Steinke, Francesco Pannarale, Soichiro Morisaki, D. Ugolini, P. Clearwater, M. Haney, T. A. Callister, Zhihui Du, G. Ciani, Alessandro Bertolini, Olivier Minazzoli, M. Razzano, Mairi Sakellariadou, G. Pillant, S. H. R. Yuen, O. de Varona, A. L. Stuver, R. De Rosa, I. Nardecchia, M. Kasprzack, J. Baird, Frances Hellman, M. B. Shaner, Manel Molina-Ruiz, S. B. Coughlin, Jessica Steinlechner, A. Neunzert, M. Heurs, Reed Essick, S. Kandhasamy, B. Sorazu, A. Kutynia, Andrea Chincarini, T. Z. Summerscales, Tenglin Li, Robert J. McCarthy, Linqing Wen, D. Meacher, Leo Tsukada, E. Z. Hamilton, A. Parida, S. S. Eikenberry, E. Genin, D. Estevez, W. Katzman, B. Grace, S. M. Aronson, M. Llorens-Monteagudo, M. Nery, Ryan Lynch, Ettore Majorana, D. M. Wilken, A. Rocchi, B. Goncharov, R. Birney, P. Ehrens, Paul M. Ricker, E. J. Fauchon-Jones, M. Lormand, William Parker, D. J. Stops, J. S. H. Lee, Felix Wellmann, Shreya Anand, D. Huet, S. H. Huttner, Z. Tornasi, Andrew Melatos, M. Lorenzini, M. Bitossi, J.-G. Ducoin, J. Neilson, G. Bergmann, K. Wette, John J. Oh, Timothy Evans, M. G. Benjamin, E. Payne, Rory Smith, C. Adams, R. M. Blair, D. Sigg, S. W. Ballmer, Z. Yang, D. M. Shoemaker, Michelle E. Walker, J. Eichholz, G. Moreno, H. Inchauspe, J. Liu, A. Pasqualetti, M. Tse, D. M. Macleod, B. L. Swinkels, J. Warner, R. Passaquieti, C. Rajan, O. Durante, N. Krupinski, F. Martelli, Karan Jani, Jade Powell, V. Mangano, H. K. Gulati, David H. Reitze, Rahul Kashyap, C. McIsaac, Nergis Mavalvala, A. K. Lenon, S. Mastrogiovanni, P. A. Altin, Piotr Jaranowski, Florent Robinet, J. Zhang, F. Baldaccini, L. F. Ortega, Jerome Degallaix, R. C. Walet, V. P. Mitrofanov, Rosa Poggiani, V. Frey, T. Sadecki, V. Tiwari, Yann Bouffanais, A. C. Green, C. Casentini, R. Shink, E. Goetz, F. Magaña-Sandoval, J. McIver, Sebastian Khan, B. C. Barish, J. H. Briggs, Mark Hannam, L. Rei, Gijs Nelemans, Tanja Hinderer, Alejandro Torres-Forné, A. K. Zadrożny, P.H. Nguyen, V. Boschi, E. J. Son, M. van Beuzekom, S. Grunewald, R. Prasanna, A. Ain, Shubhanshu Tiwari, G. A. Prodi, R. DeSalvo, V. Kondrashov, F. Frasconi, A. K. Mehta, E. D. Hall, S. Farinon, E. Mejuto Villa, D. Barker, A. Samajdar, Jolien D. E. Creighton, A. Pele, D. Singh, Arunava Mukherjee, Fausto Acernese, J. C. Barayoga, B. F. Neil, R. Flaminio, Richard J. Abbott, D. W. Yeeles, Hartmut Grote, D. C. Vander-Hyde, P. Puppo, W. Del Pozzo, Y. Minenkov, P. Bacon, P. F. Cohadon, H. Heitmann, A. Strunk, N. Kijbunchoo, Piero Rettegno, K. A. Santiago, P. J. Sutton, M. Cieślar, Maria Ilaria Del Principe, P. Raffai, J. C. Bayley, H. Wittel, M. Deenadayalan, G. H. Ogin, T. J. Shaffer, Marcus E. Lower, L. Glover, G. Losurdo, S. Biscoveanu, O. V. Palashov, Sean T. McWilliams, F. Piergiovanni, Chang-Hwan Lee, D. E. Cohen, M. Agathos, J. H. Romie, S. Sitmukhambetov, G. Kuehn, K. Merfeld, M. Ar ne, M. Phelps, Archisman Ghosh, R. G. Ormiston, Andrew Matas, A. Chiummo, K. Holt, M. Mantovani, E. A. Huerta, A. Ramos-Buades, S. L. Danilishin, Tristan Briant, R. K. Lanza, P. Dupej, Sheelu Abraham, Eric B. Flynn, J. Betzwieser, Antoine Heidmann, J. Hanks, A. Sur, H. Overmier, R. Goetz, Tarun Souradeep, J. P. Zendri, L. Sun, C. De Rossi, D. Buskulic, Odylio D. Aguiar, James Healy, P. Brockill, Luca Gammaitoni, R. Fittipaldi, C. Horst, Alberto Vecchio, F. Cipriano, Michael Thomas, R. Tenorio, N. A. Holland, D. Sellers, P. Popolizio, Koji Arai, F. J. Raab, Devon S. Johnson, N. Mukund, L. R. Cominsky, Neil J. Cornish, Colm Talbot, Andreas Freise, M. Davier, Sebastiano Bernuzzi, O. Halim, S. Koley, M. Brinkmann, C. Affeldt, S. Appert, Y. Setyawati, E. J. Sanchez, Nicholas Demos, J. D. Lough, D. Pascucci, H. S. Chen, L. E. H. Datrier, M. Bawaj, R. L. Savage, A. S. Bell, M. Laxen, Anchal Gupta, J. Meidam, M. Gosselin, Riccardo Sturani, M. K. M. Bader, O. Chaibi, Wolfango Plastino, R. Taylor, C. L. Romel, Giovanni Carapella, P. Shawhan, I. Ferrante, Soma Mukherjee, Charalampos Markakis, G. Mo, J. K. Blackburn, C. J. Richardson, F. L. Linde, E. Chassande-Mottin, Sylvain Marsat, Sheila Rowan, B. Gateley, Howard Pan, Aaron Buikema, R. Kirchhoff, B. L. Pearlstone, V. Fafone, Paul D. Lasky, R. K. Hasskew, Jordan Camp, D. Tao, M. Muratore, M. C. Heintze, D. Sentenac, F. Carbognani, Patrick Brady, P. Fulda, J. M. Fishner, Will M. Farr, M. Montani, Nancy Aggarwal, R. Gustafson, A. Grimaldi, J. W. Westhouse, Matthew Pitkin, F. Lin, Tania Regimbau, Serena Vinciguerra, F. Garufi, Chandra Kant Mishra, Joseph D. Romano, R. Bhandare, R. Pedurand, Benno Willke, C. C. Wipf, V. Pierro, M. J. Cowart, I. Dave, Lee McCuller, O. J. Piccinni, Takuya Tsutsui, T. D. Abbott, Zoheyr Doctor, M. Fletcher, B. Hughey, K. W. Tsang, P. J. Veitch, M. Rakhmanov, Surendra Nadh Somala, Gregorio Carullo, R. Xu, C. Buy, M. Oliver, Kazuhiro Agatsuma, T. J. Hansen, N. Bode, Christopher P. L. Berry, T. Harder, Rico K. L. Lo, P. Charlton, Kejia Lee, Patrick Das Gupta, S. E. Barclay, J. L. Willis, M. Eisenmann, Ofek Birnholtz, John A. Clark, Ben Farr, W. S. Kim, Christophe Collette, L. Kuo, H. Yamamoto, J. C. Driggers, A. Schönbeck, B. Rajbhandari, Daniel Wysocki, J. Prasad, A. J. Pedersen, S. B. Anderson, Tim Dietrich, M. Pürrer, S. Kwang, Frank Ohme, Vicky Kalogera, K. Rose, M. Tonelli, E. Katsavounidis, Xiuling Li, R. Gray, Patrick Godwin, M. C. Araya, Srishti Tiwari, S. Frasca, Jonathan Richardson, Tyson Littenberg, Kai Staats, L. Conti, M. Chaturvedi, Yu Huang, Geert Raaijmakers, F. Y. Khalili, R. P. Fisher, A. Allocca, D. I. Jones, Guoying Zhao, Kendall Ackley, R. K. Nayak, S. Raja, H. Y. Chia, Sascha Husa, S. E. Strigin, S. Mitra, M. Granata, H. J. Bulten, Minchuan Zhou, Shao-Jiang Wang, T. D. Creighton, S. E. Gossan, Dániel Barta, G. Venugopalan, Karl Gill, V. Srivastava, M. Fays, S. Barnum, S. C. Tait, K. Shukla, Zifan Zhou, I. A. Bilenko, L. Haegel, D.B. DeBra, David J. Ottaway, C. J. Perez, Matthew Evans, B. D. O'Brien, Marek Szczepanczyk, C. Bradaschia, M. Standke, Deep Jariwala, C. Cahillane, Otto A. Hannuksela, C. Gray, H. Estelles, W. A. Campbell, H. Radkins, A. Bozzi, N. N. Janthalur, L. Wallace, A. Królak, R. Frey, E. A. Muñiz, B. Sassolas, S. Brunett, Monica Colpi, Albino Perego, A. Bisht, M. Boer, J. B. Kanner, Andrew Lundgren, S. Xiao, J. V. Vanheijningen, D. Fiorucci, Zachariah B. Etienne, D. Moraru, E. Floden, Jennifer Watchi, A. K. Prajapati, Gianpietro Cagnoli, A. R. Wade, A. Di Lieto, S. J. Chamberlin, M. Vasúth, C. M. Mow-Lowry, Sergey P. Vyatchanin, Jonathan Cripe, V. Bossilkov, A. Paoli, Ik Siong Heng, A. Rüdiger, R. Inta, Steven Bloemen, Jonathan R. Gair, S. Klimenko, Eric Howell, E. Cesarini, S. Márka, N. Sennett, Stephen Fairhurst, Carl Blair, V. Fiumara, M. F. Carney, C. Lazzaro, Patricia Schmidt, Ajay Kumar, Y. K. Lecoeuche, M. J. Yap, C. Whittle, Bala R. Iyer, Stefan Grimm, D. B. Tanner, Kevin M. Ryan, S. McCormick, C. Difronzo, G. M. Harry, C. Palomba, S. Ascenzi, A. L. Miller, K. Venkateswara, L. Aiello, R. Green, Giuseppe Intini, Kenneth A. Strain, Jimin George, M. Sieniawska, Gregory Ashton, K. Chakravarti, G. Valdes, Ken K. Y. Ng, E. E. Cowan, B. D'Angelo, Hongyu Shen, D. C. Coyne, T. Dal Canton, J. Casanueva Diaz, P. Couvares, H. Fong, G. Greco, J. Zweizig, M. S. Shahriar, M. Korobko, J. Brooks, K. Siellez, Shiuh Chao, C. Périgois, P. Astone, Carlos O. Lousto, T. Hardwick, D. Steinmeyer, David Coward, A. Miani, R. Cotesta, Rakesh Kumar, F. Travasso, Yuri Levin, T. P. Downes, Gor Oganesyan, A. F. Brooks, P. J. Quinonez, Fabio Marchesoni, P. Hello, J. Gniesmer, Kyungmin Kim, Debarati Chatterjee, A. Trovato, B. O'Reilly, P. Gruning, Sheon Chua, R. Bonnand, C. North, Mariana Fazio, F. Vetrano, Samuele Cortese, Thomas Dent, P. Corban, S. J. Cooper, S. Leavey, Hai-Ping Cheng, A. Iess, M. Pedraza, M. Chan, Francesco Chiadini, Michał Bejger, Charlie Hoy, P. Schale, J. Jiang, J. Hennig, J. Junker, C. Van Den Broeck, E. Sowell, V. Gayathri, V. Hui, S. Walsh, Miriam Cabero, Alexander C. Jenkins, A. Markowitz, Robert Stone, M. Was, M. M. Hanke, G. Cho, James Whelan, P. Ajith, P. Booker, A. Perreca, G. Gemme, M. Drago, M. Di Giovanni, A. Malik, S. Gaudio, G. Dálya, T. Prestegard, J. Scott, L. K. Nuttall, A. W. Jones, Alessandro Nagar, R. De Pietri, Rocco Romano, M. Kinley-Hanlon, Lindsay DeMarchi, K. A. Thorne, E. L. Merilh, S. E. Dwyer, David Keitel, L. Matone, Mandar Patil, Guenakh Mitselmakher, B. A. Boom, A. M. Sergeev, Karsten Danzmann, A. R. Williamson, H. Vocca, Mario Spera, Peter Aufmuth, Andrea H. Tapia, Hua Wang, F. Cavalier, A. Bals, Yang Yang, S. G. Crowder, J. Bosveld, N. Koper, S. Kaufer, C. I. Torrie, Jan Harms, A. S. Sengupta, Xing-Jiang Zhu, Rana X. Adhikari, R. A. Mercer, S. Ossokine, Jinsook Kim, Om Sharan Salafia, C. K. Cheong, A. Lartaux-Vollard, M. Punturo, Leopoldo Milano, Slawomir Gras, L. Sammut, F. Muciaccia, Anupam Sharma, Lionel London, Moritz Mehmet, S. W. S. Ng, Suvadeep Bose, R. Gouaty, Debnandini Mukherjee, B. Idzkowski, V. Loriette, V. Skliris, R. Macas, G. Billingsley, S. Macfoy, Rainer Weiss, Alessandra Buonanno, R. Metzdorff, Isabel Cordero-Carrión, R. A. Eisenstein, Hee-Suk Cho, Gabrielle Allen, J.-M. Isac, B. Irwin, F. Donovan, S. Doravari, F. Ricci, W. Z. Korth, R. Kennedy, G. Fronz, F. Aubin, G. Stratta, László Á. Gergely, A. Macquet, Jishnu Suresh, G. D. Meadors, P. G. Murray, A. K. Divakarla, S. J. Kapadia, J. M. Gonzalez Castro, Z. Márka, Daichi Tsuna, Geoffrey Lovelace, M. Merzougui, Innocenzo M. Pinto, Haocun Yu, E. Biggs, L. Zhang, T. Zelenova, Riccardo Bassiri, Sebastian Steinlechner, C. A. Rose, X. Liu, Torrey Cullen, Magnus Manske, Bernard F. Whiting, Jesper Munch, Fabien Kéfélian, J. H. Hough, P. W. F. Forsyth, S. R. Thondapu, Chris A. Collins, Achamveedu Gopakumar, M. De Laurentis, M. Bischi, M. C. Milovich-Goff, J. L. Wright, J. R. Palamos, P. T. Baker, Carl-Johan Haster, Alessandra Corsi, D. Laghi, S. D'Antonio, E. Maros, P. B. Covas, L. Rolland, N. Letendre, B. D. Cheeseboro, B. Lantz, David Blair, P. J. Easter, K. Mogushi, Michele Zanolin, I. Magaña Hernandez, T. J. Massinger, Kiran Prasai, M. Khursheed, L. Naticchioni, D. Töyr, G. Vedovato, D. B. Kozak, F. Brighenti, Aniello Grado, D. Stocks, C. Vorvick, T. Vo, E. J. Daw, Salvatore Vitale, P. J. King, G. D. Hammond, K. H. Lai, Aaron Viets, Javed Rana, Abhirup Ghosh, G. Kang, A. L. Urban, Maurizio Canepa, J. Feicht, Satya Mohapatra, Antonio Marquina, L. Errico, T. A. Ferreira, K. D. Giardina, E. M. Santos, Nikhil Sarin, Martin Obergaulinger, M. Mondin, F. Marion, T. Huynh-Dinh, P. Weßels, Joey Shapiro Key, J. R. Sanders, C. F. Da Silva Costa, J. K. Wofford, Vuk Mandic, Chunglee Kim, M. A. Page, J. S. Kissel, H. Cao, D. J. Vine, R. M. S. Schofield, Fabrizio Barone, M. T. Hübner, N. Man, D. Lumaca, Benjamin J. Owen, J. F. J. van den Brand, J. S. Lange, M. A. Okada, E. Cuoco, Binlei Ding, S. Sunil, M. Tacca, Marta Colleoni, Bruno Giacomazzo, A. Gupta, Martin Hendry, Cecilio García-Quirós, J. A. Giaime, M. C. Tringali, K. Haughian, S. Hochheim, N. A. Robertson, D. Corre, Y. M. Kim, B. R. Hall, Maher Yazback, J. G. Bartlett, Márton Tápai, Marc Favata, Matteo Breschi, Fabrizio Bobba, Roger Jones, V. J. Roma, M. C. Díaz, Liam Cunningham, K. Mason, L. Trozzo, Antonios Kontos, S. A. Bilgili, E. C. Ferreira, Albert Lazzarini, A. P. Spencer, Sanjeev Dhurandhar, Jonathan Blackman, D. D. Brown, Anthony A. Amato, N. van Bakel, K. Toland, D. J. Hofman, A. Dmitriev, Samaya Nissanke, Y. Boetzel, S. Meshkov, Seog Oh, M. A. Bizouard, B. K. Berger, N. V. Krishnendu, Alec Mishkin, R. Cavalieri, José A. Font, C. C. Yancey, A. K. Srivastava, A. E. Pace, W. G. Anderson, N. Singh, Subroto Mukherjee, G. Cella, K. Rao, C. Fee, Maya Fishbach, Silvia Corezzi, S. Bae, E. Coccia, S. Katsanevas, M. E. Zucker, B. A. Weaver, J. G. Rollins, L.-W. Wei, Madeline Wade, P. Leaci, G. Rutins, J. D. Jones, T. C. Pechsiri, Graham Woan, Robert L. Byer, Stuart Reid, A. Masserot, K. Kawabe, S. M. Aston, K. Ueno, A. Basti, Ryan N. Lang, Podila Satya Venkata Narasimha Sharma, B. P. Abbott, E. K. Gustafson, Q. Chu, Xin Chen, R. M. Martin, David A. Nichols, A. M. Holgado, K. G. Arun, S. V. Angelova, C. Nguyen, S. Vass, J.-P. Coulon, M. Fitz-Axen, F. J. Hayes, Pablo Cerdá-Durán, Vivien Raymond, Jacob Scheuer, Michael W. Coughlin, I. Khan, G. Pagano, V. Avendano, P. Oppermann, F. Messina, R. Coyne, Fabrice Matichard, E. K. Wessel, E. A. Chase, Z. Frei, Bernard F. Schutz, Daniel E. Holz, B. J. J. Slagmolen, V. Sequino, L. E. Wade, S. Caride, David A. Williams, Samuel Deléglise, A. Fernandez-Galiana, J.-D. Fournier, I. W. Harry, Li Ju, H. Qi, Daniel A. Shaddock, B. Patricelli, Brittany Kamai, C. V. Kalaghatgi, J. Hanson, R. Mittleman, Lili Yang, Philip F. Hopkins, Terry G. McRae, I. Fiori, Shawn Rosofsky, L. G. Prokhorov, T. Di Girolamo, M. Branchesi, C. Pankow, P. M. Meyers, D. Y. T. Pong, H. Masalehdan, E. Massera, Paul J. Groot, M. Zevin, P. Kumar, Edward Seidel, O. E. S. Sauter, J. Woehler, John Veitch, J. Lehmann, S. Chung, N. Arnaud, Vijay Varma, M. MacInnis, S. Penn, S. Caudill, P. Rapagnani, T. Mistry, V. B. Adya, G. L. Mansell, A. Viceré, V. Dattilo, Riccardo Ciolfi, Yi Chen, B. W. Schulte, D. S. Wu, Margaret Millhouse, A. A. Ciobanu, S. G. Gaonkar, Haixing Miao, H. Ohta, Jianfang Wang, F. Di Giovanni, G. Bogaert, Hang Yu, K. L. Dooley, Aaron Zimmerman, Fangchen Feng, Lisa Barsotti, Anirban Dasgupta, A. Effler, R. J. G. Jonker, Nelson Christensen, Z. A. Warden, S. A. Usman, M. Cavagli, D. Tuyenbayev, K. E. Ramirez, S. Ponrathnam, Chunnong Zhao, D. Moffa, David H. Shoemaker, S. Karki, J. J. McCann, T. J. Slaven-Blair, S. ShyamSundar, C. Stachie, S. P. Stevenson, Sebastien Biscans, V. Kringel, R. Tso, S. A. Nichols, M. Kovalam, L. Mereni, D. Passuello, Patrick M. Koch, S. Antier, A. Cirone, S. Banagiri, T. L. Lam, Hyun Lee, Tomasz Bulik, J. Calderón Bustillo, Alessandro Longo, Richard J. Oram, François Bondu, Edward K. Porter, Stefan Hild, Y. Ma, A. Brillet, D. Rose, M. Vardaro, Valérie Martinez, A. Avila-Alvarez, Cesare Barbieri, Walter Winkler, A. S. Markosyan, Harald Lück, L. Nevin, D. Verkindt, M. Cho, J. Cao, G. Gaur, S. C. McGuire, J. F. Read, S. Di Pace, K. Haris, I. Maksimovic, R. L. Ward, G. Hemming, F. Badaracco, C. Messenger, S. M. Koehlenbeck, N. Leroy, B. Bécsy, Des Gibson, Vivishek Sudhir, E. Schreiber, L. Terkowski, Leo Singer, Ryan Magee, Nandita Khetan, Laura Cadonati, D. A. Steer, A. Gennai, L. Kleybolte, Harald P. Pfeiffer, M. Rizzo, I. W. Martin, David E. McClelland, Daniel R. George, Susan M. Scott, Chad Hanna, A. Bramley, C. Kimball, J. Oberling, M. Pirello, Fiodor Sorrentino, P. Thomas, B. U. Gadre, C. Di Giorgio, J. Bidler, F. Nocera, Alicia M. Sintes, Kun Li, Rajesh Kumar, H. Vahlbruch, Gunnar Riemenschneider, J. C. Mills, K. Riles, J. Y. Vinet, H. Middleton, M. Weinert, H. A. G. Gabbard, F. Fidecaro, G. M. Guidi, H. N. Isa, T. Zhang, Thibaut Jacqmin, Roman Schnabel, J. E. Brau, A. A. van Veggel, Efim A. Khazanov, G. Ballardin, M. Saleem, D. J. McManus, S. D. Linker, Douglas Davis, Geraint Pratten, Mark A. Scheel, F. Clara, M. A. Aloy, J. S. Areeda, B. B. Lane, D. Bersanetti, Yu Wang, N. V. Keerthana, Marco Romanelli, G. Koekoek, Francisco Hernandez Vivanco, S. T. Countryman, Christos Karathanasis, Eric Thrane, A. J. Weinstein, Jay D. Tasson, M. Landry, A. Tripathee, L. Di Fiore, B. Mours, F. Meylahn, C. Austin, M. Barsuglia, Hyang Woon Lee, A. Grant, C. Michel, J. H. Klika, T. D. Knowles, Marica Valentini, Surabhi Sachdev, Christopher J. Moore, F. Cleva, M. P. Ross, T. B. Edo, M. Pichot, Maximiliano Isi, M. Croquette, E. M. Gretarsson, Ying Guo, D. Beniwal, Peter Fritschel, Wenxiao Wang, M. Masso-Reid, V. V. Frolov, A. Singhal, J. Petermann, L. E. Sanchez, Enrico Calloni, G. Traylor, S. Soni, Thomas Corbitt, L. Salconi, C. A. Costa, Alena Ananyeva, Stanislav Babak, M. Constancio, P. T.H. Pang, T. Etzel, C. S. Unnikrishnan, B. C. Pant, Sourav Ghosh, Imre Bartos, Prafulla K. Panda, V. Quetschke, Bangalore Suryanarayana Sathyaprakash, Martin M. Fejer, J. R. Smith, R. Bork, S. Ghonge, K. AultONeal, L. van der Schaaf, S. A. Pai, Cody Messick, H. M. Lee, G. Mendell, S. J. Jadhav, K. S. Phukon, Michela Mapelli, J. Li, N. Radulesco, M. Fyffe, Gabriela Gonzalez, K. R. Corley, D. Rosińska, The LIGO Scientific Collaboration, The Virgo Collaboration, Science and Technology Facilities Council (UK), Australian Research Council, Istituto Nazionale di Fisica Nucleare, Council of Science and Technology UP (India), Ministerio de Ciencia, Innovación y Universidades (España), Govern de les Illes Balears, Generalitat Valenciana, National Science Centre (Poland), Russian Foundation for Basic Research, Swiss National Science Foundation, European Commission, Royal Society (UK), Hungarian Scientific Research Fund, National Research Foundation of Korea, Canadian Institute for Advanced Research, Ministry of Science and Technology (Taiwan), Kavli Institute for Particle Astrophysics and Cosmology, Apollo - University of Cambridge Repository, Abbott, B. P., Abbott, R., Abbott, T. D., Abraham, S., Acernese, F., Ackley, K., Adams, C., Adhikari, R. X., Adya, V. B., Affeldt, C., Agathos, M., Agatsuma, K., Aggarwal, N., Aguiar, O. D., Aiello, L., Ain, A., Ajith, P., Allen, G., Allocca, A., Aloy, M. A., Altin, P. A., Amato, A., Anand, S., Ananyeva, A., Anderson, S. B., Anderson, W. G., Angelova, S. V., Antier, S., Appert, S., Arai, K., Araya, M. C., Areeda, J. S., Ar ne, M., Arnaud, N., Aronson, S. M., Arun, K. G., Ascenzi, S., Ashton, G., Aston, S. M., Astone, P., Aubin, F., Aufmuth, P., Aultoneal, K., Austin, C., Avendano, V., Avila-Alvarez, A., Babak, S., Bacon, P., Badaracco, F., Bader, M. K. M., Bae, S., Baird, J., Baker, P. T., Baldaccini, F., Ballardin, G., Ballmer, S. W., Bals, A., Banagiri, S., Barayoga, J. C., Barbieri, C., Barclay, S. E., Barish, B. C., Barker, D., Barkett, K., Barnum, S., Barone, F., Barr, B., Barsotti, L., Barsuglia, M., Barta, D., Bartlett, J., Bartos, I., Bassiri, R., Basti, A., Bawaj, M., Bayley, J. C., Bazzan, M., Becsy, B., Bejger, M., Belahcene, I., Bell, A. S., Beniwal, D., Benjamin, M. G., Berger, B. K., Bergmann, G., Bernuzzi, S., Berry, C. P. L., Bersanetti, D., Bertolini, A., Betzwieser, J., Bhandare, R., Bidler, J., Biggs, E., Bilenko, I. A., Bilgili, S. A., Billingsley, G., Birney, R., Birnholtz, O., Biscans, S., Bischi, M., Biscoveanu, S., Bisht, A., Bitossi, M., Bizouard, M. A., Blackburn, J. K., Blackman, J., Blair, C. D., Blair, D. G., Blair, R. M., Bloemen, S., Bobba, F., Bode, N., Boer, M., Boetzel, Y., Bogaert, G., Bondu, F., Bonnand, R., Booker, P., Boom, B. A., Bork, R., Boschi, V., Bose, S., Bossilkov, V., Bosveld, J., Bouffanais, Y., Bozzi, A., Bradaschia, C., Brady, P. R., Bramley, A., Branchesi, M., Brau, J. E., Breschi, M., Briant, T., Briggs, J. H., Brighenti, F., Brillet, A., Brinkmann, M., Brockill, P., Brooks, A. F., Brooks, J., Brown, D. D., Brunett, S., Buikema, A., Bulik, T., Bulten, H. J., Buonanno, A., Buskulic, D., Buy, C., Byer, R. L., Cabero, M., Cadonati, L., Cagnoli, G., Cahillane, C., Bustillo, J. C., Callister, T. A., Calloni, E., Camp, J. B., Campbell, W. A., Canepa, M., Cannon, K. C., Cao, H., Cao, J., Carapella, G., Carbognani, F., Caride, S., Carney, M. F., Carullo, G., Diaz, J. C., Casentini, C., Caudill, S., Cavagli, M., Cavalier, F., Cavalieri, R., Cella, G., Cerda-Duran, P., Cesarini, E., Chaibi, O., Chakravarti, K., Chamberlin, S. J., Chan, M., Chao, S., Charlton, P., Chase, E. A., Chassande-Mottin, E., Chatterjee, D., Chaturvedi, M., Cheeseboro, B. D., Chen, H. Y., Chen, X., Chen, Y., Cheng, H. -P., Cheong, C. K., Chia, H. Y., Chiadini, F., Chincarini, A., Chiummo, A., Cho, G., Cho, H. S., Cho, M., Christensen, N., Chu, Q., Chua, S., Chung, K. W., Chung, S., Ciani, G., Cieslar, M., Ciobanu, A. A., Ciolfi, R., Cipriano, F., Cirone, A., Clara, F., Clark, J. A., Clearwater, P., Cleva, F., Coccia, E., Cohadon, P. -F., Cohen, D., Colleoni, M., Collette, C. G., Collins, C., Colpi, M., Cominsky, L. R., Constancio, M., Conti, L., Cooper, S. J., Corban, P., Corbitt, T. R., Cordero-Carrion, I., Corezzi, S., Corley, K. 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H., Frasca, S., Frasconi, F., Frei, Z., Freise, A., Frey, R., Frey, V., Fritschel, P., Frolov, V. V., Fronz, G., Fulda, P., Fyffe, M., Gabbard, H. A., Gadre, B. U., Gaebel, S. M., Gair, J. R., Gammaitoni, L., Gaonkar, S. G., Garcia-Quiros, C., Garufi, F., Gateley, B., Gaudio, S., Gaur, G., Gayathri, V., Gemme, G., Genin, E., Gennai, A., George, D., George, J., Gergely, L., Ghonge, S., Ghosh, A., Ghosh, S., Giacomazzo, B., Giaime, J. A., Giardina, K. D., Gibson, D. R., Gill, K., Glover, L., Gniesmer, J., Godwin, P., Goetz, E., Goetz, R., Goncharov, B., Gonzalez, G., Gonzalez Castro, J. M., Gopakumar, A., Gossan, S. E., Gosselin, M., Gouaty, R., Grace, B., Grado, A., Granata, M., Grant, A., Gras, S., Grassia, P., Gray, C., Gray, R., Greco, G., Green, A. C., Green, R., Gretarsson, E. M., Grimaldi, A., Grimm, S. J., Groot, P., Grote, H., Grunewald, S., Gruning, P., Guidi, G. M., Gulati, H. K., Guo, Y., Gupta, A., Gupta, P., Gustafson, E. K., Gustafson, R., Haegel, L., Halim, O., Hall, B. R., Hall, E. D., Hamilton, E. Z., Hammond, G., Haney, M., Hanke, M. M., Hanks, J., Hanna, C., Hannam, M. D., Hannuksela, O. A., Hansen, T. J., Hanson, J., Harder, T., Hardwick, T., Haris, K., Harms, J., Harry, G. M., Harry, I. W., Hasskew, R. K., Haster, C. J., Haughian, K., Hayes, F. J., Healy, J., Heidmann, A., Heintze, M. C., Heitmann, H., Hellman, F., Hello, P., Hemming, G., Hendry, M., Heng, I. S., Hennig, J., Heurs, M., Hild, S., Hinderer, T., Hochheim, S., Hofman, D., Holgado, A. M., Holland, N. A., Holt, K., Holz, D. E., Hopkins, P., Horst, C., Hough, J., Howell, E. J., Hoy, C. G., Huang, Y., Hubner, M. T., Huerta, E. A., Huet, D., Hughey, B., Hui, V., Husa, S., Huttner, S. H., Huynh-Dinh, T., Idzkowski, B., Iess, A., Inchauspe, H., Ingram, C., Inta, R., Intini, G., Irwin, B., Isa, H. N., Isac, J. -M., Isi, M., Iyer, B. R., Jacqmin, T., Jadhav, S. J., Jani, K., Janthalur, N. N., Jaranowski, P., Jariwala, D., Jenkins, A. C., Jiang, J., Johnson, D. S., Jones, A. W., Jones, D. 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M., Xiao, S., Xu, R., Yamamoto, H., Yancey, C. C., Yang, L., Yang, Y., Yang, Z., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, H., Yuen, S. H. R., Zadrozny, A. K., Zadrozny, A., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhao, G., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., Zweizig, J., Van Swinderen Institute for Particle Physics and G, Abbott, B, Abbott, R, Abbott, T, Abraham, S, Acernese, F, Ackley, K, Adams, C, Adhikari, R, Adya, V, Affeldt, C, Agathos, M, Agatsuma, K, Aggarwal, N, Aguiar, O, Aiello, L, Ain, A, Ajith, P, Allen, G, Allocca, A, Aloy, M, Altin, P, Amato, A, Anand, S, Ananyeva, A, Anderson, S, Anderson, W, Angelova, S, Antier, S, Appert, S, Arai, K, Araya, M, Areeda, J, Ar ne, M, Arnaud, N, Aronson, S, Arun, K, Ascenzi, S, Ashton, G, Aston, S, Astone, P, Aubin, F, Aufmuth, P, Aultoneal, K, Austin, C, Avendano, V, Avila-Alvarez, A, Babak, S, Bacon, P, Badaracco, F, Bader, M, Bae, S, Baird, J, Baker, P, Baldaccini, F, Ballardin, G, Ballmer, S, Bals, A, Banagiri, S, Barayoga, J, Barbieri, C, Barclay, S, Barish, B, Barker, D, Barkett, K, Barnum, S, Barone, F, Barr, B, Barsotti, L, Barsuglia, M, Barta, D, Bartlett, J, Bartos, I, Bassiri, R, Basti, A, Bawaj, M, Bayley, J, Bazzan, M, Becsy, B, Bejger, M, Belahcene, I, Bell, A, Beniwal, D, Benjamin, M, Berger, B, Bergmann, G, Bernuzzi, S, Berry, C, Bersanetti, D, Bertolini, A, Betzwieser, J, Bhandare, R, Bidler, J, Biggs, E, Bilenko, I, Bilgili, S, Billingsley, G, Birney, R, Birnholtz, O, Biscans, S, Bischi, M, Biscoveanu, S, Bisht, A, Bitossi, M, Bizouard, M, Blackburn, J, Blackman, J, Blair, C, Blair, D, Blair, R, Bloemen, S, Bobba, F, Bode, N, Boer, M, Boetzel, Y, Bogaert, G, Bondu, F, Bonnand, R, Booker, P, Boom, B, Bork, R, Boschi, V, Bose, S, Bossilkov, V, Bosveld, J, Bouffanais, Y, Bozzi, A, Bradaschia, C, Brady, P, Bramley, A, Branchesi, M, Brau, J, Breschi, M, Briant, T, Briggs, J, Brighenti, F, Brillet, A, Brinkmann, M, Brockill, P, Brooks, A, Brooks, J, Brown, D, Brunett, S, Buikema, A, Bulik, T, Bulten, H, Buonanno, A, Buskulic, D, Buy, C, Byer, R, Cabero, M, Cadonati, L, Cagnoli, G, Cahillane, C, Bustillo, J, Callister, T, Calloni, E, Camp, J, Campbell, W, Canepa, M, Cannon, K, Cao, H, Cao, J, Carapella, G, Carbognani, F, Caride, S, Carney, M, Carullo, G, Diaz, J, Casentini, C, Caudill, S, Cavagli, M, Cavalier, F, Cavalieri, R, Cella, G, Cerda-Duran, P, Cesarini, E, Chaibi, O, Chakravarti, K, Chamberlin, S, Chan, M, Chao, S, Charlton, P, Chase, E, Chassande-Mottin, E, Chatterjee, D, Chaturvedi, M, Cheeseboro, B, Chen, H, Chen, X, Chen, Y, Cheng, H, Cheong, C, Chia, H, Chiadini, F, Chincarini, A, Chiummo, A, Cho, G, Cho, H, Cho, M, Christensen, N, Chu, Q, Chua, S, Chung, K, Chung, S, Ciani, G, Cieslar, M, Ciobanu, A, Ciolfi, R, Cipriano, F, Cirone, A, Clara, F, Clark, J, Clearwater, P, Cleva, F, Coccia, E, Cohadon, P, Cohen, D, Colleoni, M, Collette, C, Collins, C, Colpi, M, Cominsky, L, Constancio, M, Conti, L, Cooper, S, Corban, P, Corbitt, T, Cordero-Carrion, I, Corezzi, S, Corley, K, Cornish, N, Corre, D, Corsi, A, Cortese, S, Costa, C, Cotesta, R, Coughlin, M, Coughlin, S, Coulon, J, Countryman, S, Couvares, P, Covas, P, Cowan, E, Coward, D, Cowart, M, Coyne, D, Coyne, R, Creighton, J, Creighton, T, Cripe, J, Croquette, M, Crowder, S, Cullen, T, Cumming, A, Cunningham, L, Cuoco, E, Dal Canton, T, Dalya, G, D'Angelo, B, Danilishin, S, D'Antonio, S, Danzmann, K, Dasgupta, A, Da Silva Costa, C, Datrier, L, Dattilo, V, Dave, I, Davier, M, Davis, D, Daw, E, Debra, D, Deenadayalan, M, Degallaix, J, De Laurentis, M, Deleglise, S, Pozzo, W, Demarchi, L, Demos, N, Dent, T, De Pietri, R, De Rosa, R, De Rossi, C, Desalvo, R, De Varona, O, Dhurandhar, S, Diaz, M, Dietrich, T, Di Fiore, L, Difronzo, C, Di Giorgio, C, Di Giovanni, F, Di Giovanni, M, Di Girolamo, T, Di Lieto, A, Ding, B, Di Pace, S, Di Palma, I, Di Renzo, F, Divakarla, A, Dmitriev, A, Doctor, Z, Donovan, F, Dooley, K, Doravari, S, Dorrington, I, Downes, T, Drago, M, Driggers, J, Du, Z, Ducoin, J, Dupej, P, Durante, O, Dwyer, S, Easter, P, Eddolls, G, Edo, T, Effler, A, Ehrens, P, Eichholz, J, Eikenberry, S, Eisenmann, M, Eisenstein, R, Errico, L, Essick, R, Estelles, H, Estevez, D, Etienne, Z, Etzel, T, Evans, M, Evans, T, Fafone, V, Fairhurst, S, Fan, X, Farinon, S, Farr, B, Farr, W, Fauchon-Jones, E, Favata, M, Fays, M, Fazio, M, Fee, C, Feicht, J, Fejer, M, Feng, F, Fernandez-Galiana, A, Ferrante, I, Ferreira, E, Ferreira, T, Fidecaro, F, Fiori, I, Fiorucci, D, Fishbach, M, Fisher, R, Fishner, J, Fittipaldi, R, Fitz-Axen, M, Fiumara, V, Flaminio, R, Fletcher, M, Floden, E, Flynn, E, Fong, H, Font, J, Forsyth, P, Fournier, J, Vivanco, F, Frasca, S, Frasconi, F, Frei, Z, Freise, A, Frey, R, Frey, V, Fritschel, P, Frolov, V, Fronz, G, Fulda, P, Fyffe, M, Gabbard, H, Gadre, B, Gaebel, S, Gair, J, Gammaitoni, L, Gaonkar, S, Garcia-Quiros, C, Garufi, F, Gateley, B, Gaudio, S, Gaur, G, Gayathri, V, Gemme, G, Genin, E, Gennai, A, George, D, George, J, Gergely, L, Ghonge, S, Ghosh, A, Ghosh, S, Giacomazzo, B, Giaime, J, Giardina, K, Gibson, D, Gill, K, Glover, L, Gniesmer, J, Godwin, P, Goetz, E, Goetz, R, Goncharov, B, Gonzalez, G, Gonzalez Castro, J, Gopakumar, A, Gossan, S, Gosselin, M, Gouaty, R, Grace, B, Grado, A, Granata, M, Grant, A, Gras, S, Grassia, P, Gray, C, Gray, R, Greco, G, Green, A, Green, R, Gretarsson, E, Grimaldi, A, Grimm, S, Groot, P, Grote, H, Grunewald, S, Gruning, P, Guidi, G, Gulati, H, Guo, Y, Gupta, A, Gupta, P, Gustafson, E, Gustafson, R, Haegel, L, Halim, O, Hall, B, Hall, E, Hamilton, E, Hammond, G, Haney, M, Hanke, M, Hanks, J, Hanna, C, Hannam, M, Hannuksela, O, Hansen, T, Hanson, J, Harder, T, Hardwick, T, Haris, K, Harms, J, Harry, G, Harry, I, Hasskew, R, Haster, C, Haughian, K, Hayes, F, Healy, J, Heidmann, A, Heintze, M, Heitmann, H, Hellman, F, Hello, P, Hemming, G, Hendry, M, Heng, I, Hennig, J, Heurs, M, Hild, S, Hinderer, T, Hochheim, S, Hofman, D, Holgado, A, Holland, N, Holt, K, Holz, D, Hopkins, P, Horst, C, Hough, J, Howell, E, Hoy, C, Huang, Y, Hubner, M, Huerta, E, Huet, D, Hughey, B, Hui, V, Husa, S, Huttner, S, Huynh-Dinh, T, Idzkowski, B, Iess, A, Inchauspe, H, Ingram, C, Inta, R, Intini, G, Irwin, B, Isa, H, Isac, J, Isi, M, Iyer, B, Jacqmin, T, Jadhav, S, Jani, K, Janthalur, N, Jaranowski, P, Jariwala, D, Jenkins, A, Jiang, J, Johnson, D, Jones, A, Jones, D, Jones, J, Jones, R, Jonker, R, Ju, L, Junker, J, Kalaghatgi, C, Kalogera, V, Kamai, B, Kandhasamy, S, Kang, G, Kanner, J, Kapadia, S, Karathanasis, C, Karki, S, Kashyap, R, Kasprzack, M, Katsanevas, S, Katsavounidis, E, Katzman, W, Kaufer, S, Kawabe, K, Keerthana, N, Kefelian, F, Keitel, D, Kennedy, R, Key, J, Khalili, F, Khan, I, Khan, S, Khazanov, E, Khetan, N, Khursheed, M, Kijbunchoo, N, Kim, C, Kim, J, Kim, K, Kim, W, Kim, Y, Kimball, C, King, P, Kinley-Hanlon, M, Kirchhoff, R, Kissel, J, Kleybolte, L, Klika, J, Klimenko, S, Knowles, T, Koch, P, Koehlenbeck, S, Koekoek, G, Koley, S, Kondrashov, V, Kontos, A, Koper, N, Korobko, M, Korth, W, Kovalam, M, Kozak, D, Kr mer, C, Kringel, V, Krishnendu, N, Krolak, A, Krupinski, N, Kuehn, G, Kumar, A, Kumar, P, Kumar, R, Kuo, L, Kutynia, A, Kwang, S, Lackey, B, Laghi, D, Lai, K, Lam, T, Landry, M, Lane, B, Lang, R, Lange, J, Lantz, B, Lanza, R, Lartaux-Vollard, A, Lasky, P, Laxen, M, Lazzarini, A, Lazzaro, C, Leaci, P, Leavey, S, Lecoeuche, Y, Lee, C, Lee, H, Lee, J, Lee, K, Lehmann, J, Lenon, A, Leroy, N, Letendre, N, Levin, Y, Li, A, Li, J, Li, K, Li, T, Li, X, Lin, F, Linde, F, Linker, S, Littenberg, T, Liu, J, Liu, X, Llorens-Monteagudo, M, Lo, R, London, L, Longo, A, Lorenzini, M, Loriette, V, Lormand, M, Losurdo, G, Lough, J, Lousto, C, Lovelace, G, Lower, M, Luck, H, Lumaca, D, Lundgren, A, Lynch, R, Ma, Y, Macas, R, Macfoy, S, Macinnis, M, Macleod, D, Macquet, A, Hernandez, I, Magana-Sandoval, F, Magee, R, Majorana, E, Maksimovic, I, Malik, A, Man, N, Mandic, V, Mangano, V, Mansell, G, Manske, M, Mantovani, M, Mapelli, M, Marchesoni, F, Marion, F, Marka, S, Marka, Z, Markakis, C, Markosyan, A, Markowitz, A, Maros, E, Marquina, A, Marsat, S, Martelli, F, Martin, I, Martin, R, Martinez, V, Martynov, D, Masalehdan, H, Mason, K, Massera, E, Masserot, A, Massinger, T, Masso-Reid, M, Mastrogiovanni, S, Matas, A, Matichard, F, Matone, L, Mavalvala, N, Mccann, J, Mccarthy, R, Mcclelland, D, Mccormick, S, Mcculler, L, Mcguire, S, Mcisaac, C, Mciver, J, Mcmanus, D, Mcrae, T, Mcwilliams, S, Meacher, D, Meadors, G, Mehmet, M, Mehta, A, Meidam, J, Villa, E, Melatos, A, Mendell, G, Mercer, R, Mereni, L, Merfeld, K, Merilh, E, Merzougui, M, Meshkov, S, Messenger, C, Messick, C, Messina, F, Metzdorff, R, Meyers, P, Meylahn, F, Miani, A, Miao, H, Michel, C, Middleton, H, Milano, L, Miller, A, Millhouse, M, Mills, J, Milovich-Goff, M, Minazzoli, O, Minenkov, Y, Mishkin, A, Mishra, C, Mistry, T, Mitra, S, Mitrofanov, V, Mitselmakher, G, Mittleman, R, Mo, G, Moffa, D, Mogushi, K, Mohapatra, S, Molina-Ruiz, M, Mondin, M, Montani, M, Moore, C, Moraru, D, Morawski, F, Moreno, G, Morisaki, S, Mours, B, Mow-Lowry, C, Muciaccia, F, Mukherjee, A, Mukherjee, D, Mukherjee, S, Mukund, N, Mullavey, A, Munch, J, Muniz, E, Muratore, M, Murray, P, Nagar, A, Nardecchia, I, Naticchioni, L, Nayak, R, Neil, B, Neilson, J, Nelemans, G, Nelson, T, Nery, M, Neunzert, A, Nevin, L, Ng, K, Ng, S, Nguyen, C, Nguyen, P, Nichols, D, Nichols, S, Nissanke, S, Nocera, F, North, C, Nuttall, L, Obergaulinger, M, Oberling, J, O'Brien, B, Oganesyan, G, Ogin, G, Oh, J, Oh, S, Ohme, F, Ohta, H, Okada, M, Oliver, M, Oppermann, P, Oram, R, O'Reilly, B, Ormiston, R, Ortega, L, O'Shaughnessy, R, Ossokine, S, Ottaway, D, Overmier, H, Owen, B, Pace, A, Pagano, G, Page, M, Pagliaroli, G, Pai, A, Pai, S, Palamos, J, Palashov, O, Palomba, C, Pan, H, Panda, P, Pang, P, Pankow, C, Pannarale, F, Pant, B, Paoletti, F, Paoli, A, Parida, A, Parker, W, Pascucci, D, Pasqualetti, A, Passaquieti, R, Passuello, D, Patil, M, Patricelli, B, Payne, E, Pearlstone, B, Pechsiri, T, Pedersen, A, Pedraza, M, Pedurand, R, Pele, A, Penn, S, Perego, A, Perez, C, Perigois, C, Perreca, A, Petermann, J, Pfeiffer, H, Phelps, M, Phukon, K, Piccinni, O, Pichot, M, Piergiovanni, F, Pierro, V, Pillant, G, Pinard, L, Pinto, I, Pirello, M, Pitkin, M, Plastino, W, Poggiani, R, Pong, D, Ponrathnam, S, Popolizio, P, Porter, E, Powell, J, Prajapati, A, Prasad, J, Prasai, K, Prasanna, R, Pratten, G, Prestegard, T, Principe, M, Prodi, G, Prokhorov, L, Punturo, M, Puppo, P, Purrer, M, Qi, H, Quetschke, V, Quinonez, P, Raab, F, Raaijmakers, G, Radkins, H, Radulesco, N, Raffai, P, Raja, S, Rajan, C, Rajbhandari, B, Rakhmanov, M, Ramirez, K, Ramos-Buades, A, Rana, J, Rao, K, Rapagnani, P, Raymond, V, Razzano, M, Read, J, Regimbau, T, Rei, L, Reid, S, Reitze, D, Rettegno, P, Ricci, F, Richardson, C, Richardson, J, Ricker, P, Riemenschneider, G, Riles, K, Rizzo, M, Robertson, N, Robinet, F, Rocchi, A, Rolland, L, Rollins, J, Roma, V, Romanelli, M, Romano, J, Romano, R, Romel, C, Romie, J, Rose, C, Rose, D, Rose, K, Rosinska, D, Rosofsky, S, Ross, M, Rowan, S, Rudiger, A, Ruggi, P, Rutins, G, Ryan, K, Sachdev, S, Sadecki, T, Sakellariadou, M, Salafia, O, Salconi, L, Saleem, M, Samajdar, A, Sammut, L, Sanchez, E, Sanchez, L, Sanchis-Gual, N, Sanders, J, Santiago, K, 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Summerscales, T, Sun, L, Sunil, S, Sur, A, Suresh, J, Sutton, P, Swinkels, B, Szczepanczyk, M, Tacca, M, Tait, S, Talbot, C, Tanner, D, Tao, D, Tapai, M, Tapia, A, Tasson, J, Taylor, R, Tenorio, R, Terkowski, L, Thomas, M, Thomas, P, Thondapu, S, Thorne, K, Thrane, E, Tiwari, S, Tiwari, V, Toland, K, Tonelli, M, Tornasi, Z, Torres-Forne, A, Torrie, C, Toyr, D, Travasso, F, Traylor, G, Tringali, M, Tripathee, A, Trovato, A, Trozzo, L, Tsang, K, Tse, M, Tso, R, Tsukada, L, Tsuna, D, Tsutsui, T, Tuyenbayev, D, Ueno, K, Ugolini, D, Unnikrishnan, C, Urban, A, Usman, S, Vahlbruch, H, Vajente, G, Valdes, G, Valentini, M, Bakel, N, Beuzekom, M, Brand, J, Broeck, C, Vander-Hyde, D, Schaaf, L, Vanheijningen, J, Veggel, A, Vardaro, M, Varma, V, Vass, S, Vasuth, M, Vecchio, A, Vedovato, G, Veitch, J, Veitch, P, Venkateswara, K, Venugopalan, G, Verkindt, D, Vetrano, F, Vicere, A, Viets, A, Vinciguerra, S, Vine, D, Vinet, J, Vitale, S, Vo, T, Vocca, H, Vorvick, C, Vyatchanin, S, Wade, A, Wade, L, 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l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Annecy de Physique des Particules (LAPP), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), Institut des Hautes Études Scientifiques (IHES), VIRGO, (Astro)-Particles Physics, COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015 - 2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Spectroscopies optiques des matériaux verres, amorphes et à nanoparticules (SOPRANO), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), 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), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), LIGO Scientific Collaboration, Virgo Collaboration, Arène, M., Bécsy, B., Bustillo, J. Calderón, Diaz, J. Casanueva, Cavaglià, M., Cerdá-Durán, P., Cieślar, M., Cordero-Carrión, I., Dálya, G., D’Angelo, B., D’Antonio, S., Deléglise, S., Pozzo, W. Del, de Varona, O., Díaz, M. C., Vivanco, Francisco Hernandez, Fronzè, G., García-Quirós, C., Ghosh, Abhirup, Ghosh, Archisman, González, G., Gupta, Anchal, Hübner, M. T., Kéfélian, F., Kim, Chunglee, Krämer, C., Królak, A., Kumar, Rahul, Kumar, Rakesh, Lück, H., Hernandez, I. Magaña, Magaña-Sandoval, F., Márka, S., Márka, Z., Villa, E. Mejuto, Mukherjee, Arunava, Mukherjee, Subroto, Muñiz, E. A., O’Brien, B. D., Oram, Richard J., O’Reilly, B., O’Shaughnessy, R., Périgois, C., Pinto, I. M., Pürrer, M., Rana, Javed, Rosińska, D., Rüdiger, A., Schönbeck, A., Szczepańczyk, M. J., Tápai, M., Tiwari, Shubhanshu, Tiwari, Srishti, Torres-Forné, A., Töyrä, D., Bakel, N. van, Beuzekom, M. van, Brand, J. F. J. van den, Broeck, C. Van Den, Schaaf, L. van der, Veggel, A. A. van, Vasúth, M., Viceré, A., Weßels, P., Yu, Hang, Yu, Haocun, Zadrożny, A. K., Zadrożny, A., RS: FSE MSP, Grav. waves and fundamental physics, RS: FSE Grav. waves and fundamental physics, Faculty of Science, Gravitation and Astroparticle Physics Amsterdam, Other Research IHEF (IoP, FNWI), IoP (FNWI), and Astroparticle Physics (IHEF, IoP, FNWI)
Subjects: Gravitació, neutron star: binary, cosmological model, 010504 meteorology & atmospheric sciences, Astronomy, Gravitational Waves, Hubble constant, O2, LIGO, Virgo, detector: network, 01 natural sciences, Cosmology, General Relativity and Quantum Cosmology, LIGO, dark energy, 010303 astronomy & astrophysics, QC, Physics, Settore FIS/01, Hubble constant, Settore FIS/05, CATALOG, Physical Sciences, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), DATA RELEASE, COSMOLOGICAL PARAMETERS, FOS: Physical sciences, O2, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astronomy & Astrophysics, LUMINOSITY FUNCTIONS, gravitational radiation: direct detection, Gravitational-wave astronomy, 1ST, Article, electromagnetic field: production, symbols.namesake, Binary black hole, 0103 physical sciences, DISTRIBUTIONS, K-CORRECTIONS, SDG 7 - Affordable and Clean Energy, Astrophysique, STFC, 0105 earth and related environmental sciences, Gravitational Waves, Science & Technology, Gravitational wave, Virgo, RCUK, Astronomy and Astrophysics, cosmology, gravitational waves, 310 Galaxies and Cosmology, Galaxy, EVOLUTION, Dewey Decimal Classification::500 | Naturwissenschaften::520 | Astronomie, Kartographie, gravitational radiation detector, VIRGO, black hole: binary, Space and Planetary Science, [SDU]Sciences of the Universe [physics], DENSITY, gravitational radiation: emission, Dark energy, Astronomia, ddc:520, galaxy, Gravitational wave astronomy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law
Abstract: This paper presents the gravitational-wave measurement of the Hubble constant (H 0) using the detections from the first and second observing runs of the Advanced LIGO and Virgo detector network. The presence of the transient electromagnetic counterpart of the binary neutron star GW170817 led to the first standard-siren measurement of H 0. Here we additionally use binary black hole detections in conjunction with galaxy catalogs and report a joint measurement. Our updated measurement is H 0 = km s-1 Mpc-1 (68.3% of the highest density posterior interval with a flat-in-log prior) which is an improvement by a factor of 1.04 (about 4%) over the GW170817-only value of km s-1 Mpc-1. A significant additional contribution currently comes from GW170814, a loud and well-localized detection from a part of the sky thoroughly covered by the Dark Energy Survey. With numerous detections anticipated over the upcoming years, an exhaustive understanding of other systematic effects are also going to become increasingly important. These results establish the path to cosmology using gravitational-wave observations with and without transient electromagnetic counterparts., 0, info:eu-repo/semantics/published
Published: 2021

3. GRB 180418A: A Possibly Short Gamma-Ray Burst with a Wide-angle Outflow in a Faint Host Galaxy

Author: Adam Goldstein, Matt Nicholl, B. E. Cobb, E. L. M. Burns, A. J. Levan, Nial R. Tanvir, Nathan Smith, Edo Berger, Kerry Paterson, Brian D. Metzger, P. K. Blanchard, Tanmoy Laskar, Antonino Cucchiara, W. Fong, A. Rouco Escorial, Peter Milne, Raffaella Margutti, A. E. Nugent, D. Cornish, Péter Veres, A. Y. Lien, S. B. Cenko, and M. Lally
Subjects: Physics, astro-ph.HE, 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Space and Planetary Science, 0103 physical sciences, Outflow, Gamma-ray burst, 010303 astronomy & astrophysics, Host (network), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: We present X-ray and multiband optical observations of the afterglow and host galaxy of GRB 180418A, discovered by Swift/BAT and Fermi/GBM. We present a reanalysis of the GBM and BAT data deriving durations of the prompt emission of T 90 ≈ 2.56 and 1.90 s, respectively. Modeling the Fermi/GBM catalog of 1405 bursts (2008–2014) in the hardness–T 90 plane, we obtain a probability of ≈60% that GRB 180418A is a short-hard burst. From a combination of Swift/XRT and Chandra observations, the X-ray afterglow is detected to ≈38.5 days after the burst and exhibits a single power-law decline with F X ∝ t −0.98. Late-time Gemini observations reveal a faint r ≈ 25.69 mag host galaxy at an angular offset of ≈0.″16. At the likely redshift range of z ≈ 1–2.25, we find that the X-ray afterglow luminosity of GRB 180418A is intermediate between short and long gamma-ray bursts (GRBs) at all epochs during which there are contemporaneous data and that GRB 180418A lies closer to the E γ,peak–E γ,iso correlation for short GRBs. Modeling the multiwavelength afterglow with the standard synchrotron model, we derive the burst explosion properties and find a jet opening angle of θ j ≳ 9°–14°. If GRB 180418A is a short GRB that originated from a neutron star merger, it has one of the brightest and longest-lived afterglows along with an extremely faint host galaxy. If, instead, the event is a long GRB that originated from a massive star collapse, it has among the lowest-luminosity afterglows and lies in a peculiar space in terms of the hardness–T 90 and E γ,peak–E γ,iso planes.
Published: 2021

4. Mass, Spin, and Ultralight Boson Constraints from the Intermediate-mass Black Hole in the Tidal Disruption Event 3XMM J215022.4-055108

Author: Sixiang Wen, Nicholas C. Stone, Peter G. Jonker, and Ann I. Zabludoff
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Angular momentum, 010308 nuclear & particles physics, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Sigma, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Accretion (astrophysics), Galaxy, Redshift, Tidal disruption event, Space and Planetary Science, Intermediate-mass black hole, 0103 physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Boson
Abstract: We simultaneously and successfully fit the multi-epoch X-ray spectra of the tidal disruption event (TDE) 3XMM J215022.4-055108 using a modified version of our relativistic slim disk model that now accounts for angular momentum losses from radiation. We explore the effects of different disk properties and of uncertainties in the spectral hardening factor fc and redshift z on the estimation of the black hole mass M and spin a. Across all choices of theoretical priors, we constrain M to less than 2.2e4 Ms at 1 sigma confidence. Assuming that the TDE host is a star cluster associated with the adjacent, brighter, barred lenticular galaxy at z=0.055, we constrain M and a to be (1.75+0.45-0.05)e4 Ms and 0.8+0.12-0.02, respectively, at 1 sigma confidence. The high, but sub-extremal, spin suggests that, if this intermediate mass black hole (IMBH) has grown significantly since formation, it has acquired its last e-fold in mass in a way incompatible with both the standard and chaotic limits of gas accretion. Ours is the first clear IMBH with a spin measurement. As such, this object represents a novel laboratory for astro-particle physics; its M and a place tight limits on the existence of ultralight bosons, ruling out those with masses 1.0e-15 to 1.0e-16 eV., 19 pages, 10 figure and 5 tables. Accepted for publication in Apj
Published: 2021

5. The Nature of Black Hole Shadows

Author: Heino Falcke and Thomas Bronzwaer
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Brightness, Active galactic nucleus, Event horizon, media_common.quotation_subject, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), General Relativity and Quantum Cosmology, Black hole, Projection (mathematics), Space and Planetary Science, Coincident, Sky, Shadow, Astrophysics - High Energy Astrophysical Phenomena, media_common
Abstract: A distinct visual signature occurs in black holes that are surrounded by optically thin and geometrically thick emission regions. This signature is a sharp-edged dip in brightness that is coincident with the black-hole shadow, which is the projection of the black hole's unstable-photon region on the observer's sky. We highlight two key mechanisms responsible for producing the sharp-edged dip: i) the reduction of intensity observed in rays that intersect the unstable-photon region, and thus the perfectly absorbing event horizon, versus rays that do not (blocking), and ii) the increase of intensity observed in rays that travel along extended, horizon-circling paths near the boundary of the unstable-photon region (path-lengthening). We demonstrate that the black-hole shadow is a distinct phenomenon from the photon ring, and that models exist in which the former may be observed, but not the latter. Additionally, we show that the black-hole shadow and its associated visual signature differ from the more model-dependent brightness depressions associated with thin-disk models, because for geometrically thick and optically thin emission regions, the blocking and path-lengthening effects are quite general. Consequentially, the black-hole shadow is a robust and fairly model-independent observable for accreting black holes that are in the deep sub-Eddington regime, such as low-luminosity active galactic nuclei (LLAGN)., Comment: 15 pages, 12 figures, accepted for publication in ApJ (22 July 2021)
Published: 2021

6. Discovery and Characterization of a Rare Magnetic Hybrid beta Cephei Slowly Pulsating B-type Star in an Eclipsing Binary in the Young Open Cluster NGC 6193

Author: Daniel J. Stevens, Marina Kounkel, Dax L. Feliz, Cole Johnston, Luke G. Bouma, Keivan G. Stassun, and Guillermo Torres
Subjects: Physics, Slowly pulsating B-type star, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Binary number, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Characterization (materials science), Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Binary star, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, 010306 general physics, 010303 astronomy & astrophysics, Open cluster
Abstract: As many as 10\% of OB-type stars have global magnetic fields, which is surprising given their internal structure is radiative near the surface. A direct probe of internal structure is pulsations, and some OB-type stars exhibit pressure modes ($\beta$ Cep pulsators) or gravity modes (slowly pulsating B-type stars; SPBs); a few rare cases of hybrid $\beta$ Cep/SPBs occupy a narrow instability strip in the H-R diagram. The most precise fundamental properties of stars are obtained from eclipsing binaries (EBs), and those in clusters with known ages and metallicities provide the most stringent constraints on theory. Here we report the discovery that HD 149834 in the $\sim$5 Myr cluster NGC 6193 is an EB comprising a hybrid $\beta$ Cep/SPB pulsator and a highly irradiated low-mass companion. We determine the masses, radii, and temperatures of both stars; the $\sim$9.7 M$_\odot$ primary resides in the instability strip where hybrid pulsations are theoretically predicted. The presence of both SPB and $\beta$ Cep pulsations indicates that the system has a near-solar metallicity, and is in the second half of the main-sequence lifetime. The radius of the $\sim$1.2 M$_\odot$ companion is consistent with theoretical pre-main-sequence isochrones at 5 Myr, but its temperature is much higher than expected, perhaps due to irradiation by the primary. The radius of the primary is larger than expected, unless its metallicity is super-solar. Finally, the light curve shows residual modulation consistent with the rotation of the primary, and Chandra observations reveal a flare, both of which suggest the presence of starspots and thus magnetism on the primary., Comment: Accepted for publication in The Astrophysical Journal, 15 pages, 14 figures
Published: 2021

7. Diffusive Hydrogenation Reactions of CO Embedded in Amorphous Solid Water at Elevated Temperatures ∼70 K

Author: Naoki Watanabe, Akira Kouchi, Hiroshi Hidaka, and Masashi Tsuge
Subjects: Astrochemistry, 010504 meteorology & atmospheric sciences, Hydrogen, FOS: Physical sciences, chemistry.chemical_element, 01 natural sciences, Mantle (geology), Dense interstellar clouds, chemistry.chemical_compound, Physics - Chemical Physics, 0103 physical sciences, Molecular clouds, Molecule, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Cosmic dust, Chemical Physics (physics.chem-ph), Physics, Laboratory astrophysics, Molecular cloud, Astronomy and Astrophysics, Interstellar molecules, Astrophysics - Astrophysics of Galaxies, Amorphous solid, chemistry, Space and Planetary Science, Chemical physics, Astrophysics of Galaxies (astro-ph.GA), Carbon monoxide, Interstellar dust
Abstract: The surface processes on interstellar dust grains have an important role in the chemical evolution in molecular clouds. Hydrogenation reactions on ice surfaces have been extensively investigated and are known to proceed at low temperatures mostly below 20 K. In contrast, information about the chemical processes of molecules within an ice mantle is lacking. In this work, we investigated diffusive hydrogenation reactions of carbon monoxide (CO) embedded in amorphous solid water (ASW) as a model case and discovered that the hydrogenation of CO efficiently proceeds to yield H2CO and CH3OH even above 20 K when CO is buried beneath ASW. The experimental results suggest that hydrogen atoms diffuse through the cracks of ASW and have a sufficient residence time to react with embedded CO. The hydrogenation reactions occurred even at temperatures up to ~70 K. Cracks collapse at elevated temperatures but the occurrence of hydrogenation reactions means that the cracks would not completely disappear and remain large enough for penetration by hydrogen atoms. Considering the hydrogen-atom fluence in the laboratory and molecular clouds, we suggest that the penetration of hydrogen and its reactions within the ice mantle occur in astrophysical environments. Unified Astronomy
Published: 2020

8. Faraday Dispersion Function of Disk Galaxies with Axisymmetric Global Magnetic Fields. I

Author: Haruya Eguchi, Keitaro Takahashi, Shinsuke Ideguchi, Masaki Suzuki, and Yoshimitsu Miyashita
Subjects: Physics, 010504 meteorology & atmospheric sciences, Turbulence, Astronomy, Rotational symmetry, Astronomy and Astrophysics, 01 natural sciences, Galaxy, law.invention, Magnetic field, Computational physics, Space and Planetary Science, law, 0103 physical sciences, Pitch angle, Dispersion (water waves), Faraday cage, 010303 astronomy & astrophysics, Beam (structure), 0105 earth and related environmental sciences
Abstract: Faraday tomography is a novel method to probe 3-dimensional structure of magnetic fields of polarized radio sources. In this paper, we investigate Faraday dispersion function (FDF) of disk galaxies extending a simple analytic model of galactic magnetic fields developed in Ideguchi et al. (2017). The model consists of axisymmetric coherent fields and turbulent fields and we consider the effects of inclination, relative amplitude of coherent and turbulent magnetic fields and pitch angle of coherent fields. Our simple model makes it easy to obtain physical interpretation of FDFs and helps understanding observational results. We find FDFs have two peaks when galaxies are observed with non zero inclination. The gap and relative height of two peaks are dependent on the inclination angle and pitch angle but are not affected by relative amplitude of coherent and turbulent magnetic fields so much. These findings give us an important caution that two peaks in observed FDFs do not necessarily imply the presence of two separate radio sources within a beam.
Published: 2020

9. Implications from Late-time X-Ray Detections of Optically Selected Tidal Disruption Events: State Changes, Unification, and Detection Rates

Author: Peter G. Jonker, Brian D. Metzger, Nicholas C. Stone, S. van Velzen, and A. Generozov
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Brightness, 010504 meteorology & atmospheric sciences, Astronomy, media_common.quotation_subject, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Observable, Astrophysics, 01 natural sciences, Power law, Asymmetry, Luminosity, Black hole, 13. Climate action, Space and Planetary Science, 0103 physical sciences, Detection rate, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, media_common
Abstract: We present Chandra X-ray observations of four optically-selected tidal disruption events (TDEs) obtained 4-9 years after discovery. Three sources were detected with luminosities between 9X10^40 and 3X10^42 erg/s. The spectrum of PTF09axc is consistent with a power law of index 2.5+-0.1, whereas the spectrum of PTF09ge is very soft. The power law spectrum of PTF09axc and prior literature findings, provide evidence that TDEs transition from an early-time soft state to a late-time hard state many years after disruption. We propose that the time to peak luminosity for optical and X-ray emission may differ substantially in TDEs, with X-rays being produced or becoming observable later. This delay helps explain the differences in observed properties such as L_opt/L_ X of optically and X-ray selected TDEs. We update TDE rate predictions for the eROSITA instrument: it ranges from 3 per yr to 990 per yr, depending sensitively on the distribution of black hole spins and the time delay between disruption and peak X-ray brightness. We further predict an asymmetry in the number of retrograde and prograde disks in samples of optically and X-ray selected TDEs. The details of the observational biases can contribute to observed differences between optically and X-ray selected TDEs (with optically selected TDEs being fainter in X-rays for retrograde TDE disks)., Comment: Accepted for publication to ApJ, 18 pages, 4 figures
Published: 2020

10. The Intriguing Parsec-scale Radio Structure in the 'Offset AGN' KISSR 102

Author: Mousumi Das, Z. Paragi, D. Lena, S. Vaddi, R. Khatun, Preeti Kharb, and Smitha Subramanian
Subjects: Physics, Offset (computer science), Space and Planetary Science, Astronomy, Astrophysics of Galaxies (astro-ph.GA), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We report the detection of an intriguing parsec-scale radio source in the "offset AGN" candidate, KISSR 102. The elliptical host galaxy includes two optical nuclei at a projected separation of 1.54 kpc, N1 and N2, to the south-east and north-west, respectively. Phase-referenced VLBA observations at 1.5 and 4.9 GHz of this LINER galaxy, have detected double radio components (A and B) at a projected separation of 4.8 parsec at 1.5 GHz, and another partially-resolved double radio structure at 4.9 GHz coincident with the brighter radio component A. These radio detections are confined to the optical nucleus N1. The brightness temperatures of all the detected radio components are high, $\gtrsim10^8$ K, consistent with them being components of a radio AGN. The 1.5-4.9 GHz spectral index is inverted ($\alpha\sim+0.64\pm0.08$) for component A and steep for component B ($\alpha \lesssim-1.6$). The dramatic change in the spectral indices of A and B is inconsistent with it being a typical "core-jet" structure from a single AGN or the mini-lobes of a compact symmetric object. To be consistent with a "core-jet" structure, the jet in KISSR 102 would need to be undergoing strong jet-medium interaction with dense surrounding media resulting in a drastic spectral steepening of the jet. Alternatively, the results could be consistent with the presence of a parsec-scale binary radio AGN, which is the end result of a three-body interaction involving three supermassive black holes in the centre of KISSR 102., Comment: 11 pages, 6 figures, ApJ accepted
Published: 2020

11. Cosmic-Ray Anisotropies in Right Ascension Measured by the Pierre Auger Observatory

Author: The Pierre Auger Collaboration, Aab, A., Abreu, P., Aglietta, M., Albuquerque, I. F. M., Albury, J. M., Allekotte, I., Almela, A., Castillo, J. Alvarez, Alvarez-Mu��iz, J., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Ferreira, P. R. Ara��jo, Asorey, H., Assis, P., Avila, G., Badescu, A. M., Bakalova, A., Balaceanu, A., Barbato, F., Luz, R. J. Barreira, Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Bister, T., Biteau, J., Blanco, A., Blazek, J., Bleve, C., Boh��ov��, M., Boncioli, D., Bonifazi, C., Arbeletche, L. Bonneau, Borodai, N., Botti, A. M., Brack, J., Bretz, T., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero-Mora, K. S., Caccianiga, L., Calcagni, L., Cancio, A., Canfora, F., Caracas, I., Carceller, J. M., Caruso, R., Castellina, A., Catalani, F., Cataldi, G., Cazon, L., Cerda, M., Chinellato, J. A., Choi, K., Chudoba, J., Chytka, L., Clay, R. W., Cerutti, A. C. Cobos, Colalillo, R., Coleman, A., Coluccia, M. R., Concei��o, R., Condorelli, A., Consolati, G., Contreras, F., Convenga, F., Covault, C. E., Dasso, S., Daumiller, K., Dawson, B. R., Day, J. A., de Almeida, R. M., de Jes��s, J., de Jong, S. J., De Mauro, G., Neto, J. R. T. de Mello, De Mitri, I., de Oliveira, J., Franco, D. de Oliveira, de Souza, V., Debatin, J., del R��o, M., Deligny, O., Dhital, N., Di Matteo, A., Castro, M. L. D��az, Dobrigkeit, C., D'Olivo, J. C., Dorosti, Q., Anjos, R. C. dos, Dova, M. T., Ebr, J., Engel, R., Epicoco, I., Erdmann, M., Escobar, C. O., Etchegoyen, A., Falcke, H., Farmer, J., Farrar, G., Fauth, A. C., Fazzini, N., Feldbusch, F., Fenu, F., Fick, B., Figueira, J. M., Filip��i��, A., Freire, M. M., Fujii, T., Fuster, A., Galea, C., Galelli, C., Garc��a, B., Vegas, A. L. Garcia, Gemmeke, H., Gesualdi, F., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Glombitza, J., Gobbi, F., Golup, G., Berisso, M. G��mez, Vitale, P. F. G��mez, Gongora, J. P., Gonz��lez, N., Goos, I., G��ra, D., Gorgi, A., Gottowik, M., Grubb, T. D., Guarino, F., Guedes, G. P., Guido, E., Hahn, S., Halliday, R., Hampel, M. R., Hansen, P., Harari, D., Harvey, V. M., Haungs, A., Hebbeker, T., Heck, D., Hill, G. C., Hojvat, C., H��randel, J. R., Horvath, P., Hrabovsk��, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Johnsen, J. A., Jurysek, J., K��p��, A., Kampert, K. H., Keilhauer, B., Kemp, J., Klages, H. O., Kleifges, M., Kleinfeller, J., K��pke, M., Mezek, G. Kukec, Awad, A. Kuotb, Lago, B. L., LaHurd, D., Lang, R. G., de Oliveira, M. A. Leigui, Lenok, V., Letessier-Selvon, A., Lhenry-Yvon, I., Presti, D. Lo, Lopes, L., L��pez, R., Casado, A. L��pez, Lorek, R., Luce, Q., Lucero, A., Payeras, A. Machado, Malacari, M., Mancarella, G., Mandat, D., Manning, B. C., Manshanden, J., Mantsch, P., Mariazzi, A. G., Mari��, I. C., Marsella, G., Martello, D., Martinez, H., Bravo, O. Mart��nez, Mastrodicasa, M., Mathes, H. J., Matthews, J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K. -D., Michal, S., Micheletti, M. I., Miramonti, L., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Morlino, G., Mostaf��, M., M��ller, A. L., Muller, M. A., M��ller, S., Mussa, R., Muzio, M., Namasaka, W. M., Nellen, L., Niculescu-Oglinzanu, M., Niechciol, M., Nitz, D., Nosek, D., Novotny, V., No��ka, L., Nucita, A, N��ez, L. A., Palatka, M., Pallotta, J., Panetta, M. P., Papenbreer, P., Parente, G., Parra, A., Pech, M., Pedreira, F., P��kala, J., Pelayo, R., Pe��a-Rodriguez, J., Pereira, L. A. S., Armand, J. Perez, Perlin, M., Perrone, L., Peters, C., Petrera, S., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Pont, B., Pothast, M., Privitera, P., Prouza, M., Puyleart, A., Querchfeld, S., Rautenberg, J., Ravignani, D., Reininghaus, M., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., de Carvalho, W. Rodrigues, Rojo, J. Rodriguez, Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Salina, G., Gomez, J. D. Sanabria, S��nchez, F., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Savina, P., Sch��fer, C., Scherini, V., Schieler, H., Schimassek, M., Schimp, M., Schl��ter, F., Schmidt, D., Scholten, O., Schov��nek, P., Schr��der, F. G., Schr��der, S., Sciutto, S. J., Scornavacche, M., Shellard, R. C., Sigl, G., Silli, G., Sima, O., ��m��da, R., Sommers, P., Soriano, J. F., Souchard, J., Squartini, R., Stadelmaier, M., Stanca, D., Stani��, S., Stasielak, J., Stassi, P., Streich, A., Su��rez-Dur��n, M., Sudholz, T., Suomij��rvi, T., Supanitsky, A. D., ��up��k, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Tapia, A., Timmermans, C., Tobiska, P., Peixoto, C. J. Todero, Tom��, B., Elipe, G. Torralba, Travaini, A., Travnicek, P., Trimarelli, C., Trini, M., Tueros, M., Ulrich, R., Unger, M., Urban, M., Vaclavek, L., Galicia, J. F. Vald��s, Vali��o, I., Valore, L., van Vliet, A., Varela, E., C��rdenas, B. Vargas, V��squez-Ram��rez, A., Veberi��, D., Ventura, C., Quispe, I. D. Vergara, Verzi, V., Vicha, J., Villase��or, L., Vink, J., Vorobiov, S., Wahlberg, H., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczy��ski, H., Winchen, T., Wirtz, M., Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zehrer, L., Zepeda, A., Ziolkowski, M., Zuccarello, F., Aab, A., Abreu, P., Aglietta, M., Albuquerque, I. F. M., Albury, J. M., Allekotte, I., Almela, A., Castillo, J. A., Alvarez-Muiz, J., Anastasi, G. A., Anchordoqui, L., Andrada, B., Andringa, S., Aramo, C., Ferreira, P. R. A., Asorey, H., Assis, P., Avila, G., Badescu, A. M., Bakalova, A., Balaceanu, A., Barbato, F., Luz, R. J. B., Becker, K. H., Bellido, J. A., Berat, C., Bertaina, M. E., Bertou, X., Biermann, P. L., Bister, T., Biteau, J., Blanco, A., Blazek, J., Bleve, C., Bohacova, M., Boncioli, D., Bonifazi, C., Arbeletche, L. B., Borodai, N., Botti, A. M., Brack, J., Bretz, T., Briechle, F. L., Buchholz, P., Bueno, A., Buitink, S., Buscemi, M., Caballero-Mora, K. S., Caccianiga, L., Calcagni, L., Cancio, A., Canfora, F., Caracas, I., Carceller, J. M., Caruso, R., Castellina, A., Catalani, F., Cataldi, G., Cazon, L., Cerda, M., Chinellato, J. A., Choi, K., Chudoba, J., Chytka, L., Clay, R. W., Cerutti, A. C. C., Colalillo, R., Coleman, A., Coluccia, M. R., Conceica¸o, R., Condorelli, A., Consolati, G., Contreras, F., Convenga, F., Covault, C. E., Dasso, S., Daumiller, K., Dawson, B. R., Day, J. A., De Almeida, R. M., De Jesus, J., De Jong, S. J., De Mauro, G., De Mello Neto, J. R. T., De Mitri, I., De Oliveira, J., De Oliveira Franco, D., De Souza, V., Debatin, J., Del Rio, M., Deligny, O., Dhital, N., Di Matteo, A., Castro, M. L. D., Dobrigkeit, C., D'Olivo, J. C., Dorosti, Q., Dos Anjos, R. C., Dova, M. T., Ebr, J., Engel, R., Epicoco, I., Erdmann, M., Escobar, C. O., Etchegoyen, A., Falcke, H., Farmer, J., Farrar, G., Fauth, A. C., Fazzini, N., Feldbusch, F., Fenu, F., Fick, B., Figueira, J. M., Filipcic, A., Freire, M. M., Fujii, T., Fuster, A., Galea, C., Galelli, C., Garcia, B., Vegas, A. L. G., Gemmeke, H., Gesualdi, F., Gherghel-Lascu, A., Ghia, P. L., Giaccari, U., Giammarchi, M., Giller, M., Glombitza, J., Gobbi, F., Golup, G., Berisso, M. G., Vitale, P. F. G., Gongora, J. P., Gonzalez, N., Goos, I., Gora, D., Gorgi, A., Gottowik, M., Grubb, T. D., Guarino, F., Guedes, G. P., Guido, E., Hahn, S., Halliday, R., Hampel, M. R., Hansen, P., Harari, D., Harvey, V. M., Haungs, A., Hebbeker, T., Heck, D., Hill, G. C., Hojvat, C., Horandel, J. R., Horvath, P., Hrabovsky, M., Huege, T., Hulsman, J., Insolia, A., Isar, P. G., Johnsen, J. A., Jurysek, J., Kaapa, A., Kampert, K. H., Keilhauer, B., Kemp, J., Klages, H. O., Kleifges, M., Kleinfeller, J., Kopke, M., Mezek, G. K., Awad, A. K., Lago, B. L., Lahurd, D., Lang, R. G., Leigui De Oliveira, M. A., Lenok, V., Letessier-Selvon, A., Lhenry-Yvon, I., Presti, D. L., Lopes, L., Lopez, R., Casado, A. L., Lorek, R., Luce, Q., Lucero, A., Payeras, A. M., Malacari, M., Mancarella, G., Mandat, D., Manning, B. C., Manshanden, J., Mantsch, P., Mariazzi, A. G., Maris, I. C., Marsella, G., Martello, D., Martinez, H., Bravo, O. M., Mastrodicasa, M., Mathes, H. J., Matthews, J., Matthiae, G., Mayotte, E., Mazur, P. O., Medina-Tanco, G., Melo, D., Menshikov, A., Merenda, K. -D., Michal, S., Micheletti, M. I., Miramonti, L., Mockler, D., Mollerach, S., Montanet, F., Morello, C., Morlino, G., Mostafa, M., Muller, A. L., Muller, M. A., Muller, S., Mussa, R., Muzio, M., Namasaka, W. M., Nellen, L., Niculescu-Oglinzanu, M., Niechciol, M., Nitz, D., Nosek, D., Novotny, V., Nozka, L., Nucita, A., Nuez, L. A., Palatka, M., Pallotta, J., Panetta, M. P., Papenbreer, P., Parente, G., Parra, A., Pech, M., Pedreira, F., Pkala, J., Pelayo, R., Pea-Rodriguez, J., Pereira, L. A. S., Armand, J. P., Perlin, M., Perrone, L., Peters, C., Petrera, S., Pierog, T., Pimenta, M., Pirronello, V., Platino, M., Pont, B., Pothast, M., Privitera, P., Prouza, M., Puyleart, A., Querchfeld, S., Rautenberg, J., Ravignani, D., Reininghaus, M., Ridky, J., Riehn, F., Risse, M., Ristori, P., Rizi, V., Carvalho, W. R. D., Rojo, J. R., Roncoroni, M. J., Roth, M., Roulet, E., Rovero, A. C., Ruehl, P., Saffi, S. J., Saftoiu, A., Salamida, F., Salazar, H., Salina, G., Gomez, J. D. S., Sanchez, F., Santos, E. M., Santos, E., Sarazin, F., Sarmento, R., Sarmiento-Cano, C., Sato, R., Savina, P., Schafer, C., Scherini, V., Schieler, H., Schimassek, M., Schimp, M., Schluter, F., Schmidt, D., Scholten, O., Schovanek, P., Schroder, F. G., Schroder, S., Sciutto, S. J., Scornavacche, M., Shellard, R. C., Sigl, G., Silli, G., Sima, O., Smida, R., Sommers, P., Soriano, J. F., Souchard, J., Squartini, R., Stadelmaier, M., Stanca, D., Stanic, S., Stasielak, J., Stassi, P., Streich, A., Suarez-Duran, M., Sudholz, T., Suomijarvi, T., Supanitsky, A. D., Supik, J., Szadkowski, Z., Taboada, A., Taborda, O. A., Tapia, A., Timmermans, C., Tobiska, P., Peixoto, C. J. T., Tome, B., Elipe, G. T., Travaini, A., Travnicek, P., Trimarelli, C., Trini, M., Tueros, M., Ulrich, R., Unger, M., Urban, M., Vaclavek, L., Galicia, J. F. V., Valio, I., Valore, L., Van Vliet, A., Varela, E., Cardenas, B. V., Vasquez-Ramirez, A., Veberic, D., Ventura, C., Quispe, I. D. V., Verzi, V., Vicha, J., Villaseor, L., Vink, J., Vorobiov, S., Wahlberg, H., Watson, A. A., Weber, M., Weindl, A., Wiencke, L., Wilczynski, H., Winchen, T., Wirtz, M., Wittkowski, D., Wundheiler, B., Yushkov, A., Zas, E., Zavrtanik, D., Zavrtanik, M., Zehrer, L., Zepeda, A., Ziolkowski, M., Zuccarello, F., Astronomy, Research unit Astroparticle Physics, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Pierre Auger, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Aab A., Abreu P., Aglietta M., Albuquerque I.F.M., Albury J.M., Allekotte I., Almela A., Castillo J.A., Alvarez-Muiz J., Anastasi G.A., Anchordoqui L., Andrada B., Andringa S., Aramo C., Ferreira P.R.A., Asorey H., Assis P., Avila G., Badescu A.M., Bakalova A., Balaceanu A., Barbato F., Luz R.J.B., Becker K.H., Bellido J.A., Berat C., Bertaina M.E., Bertou X., Biermann P.L., Bister T., Biteau J., Blanco A., Blazek J., Bleve C., Bohacova M., Boncioli D., Bonifazi C., Arbeletche L.B., Borodai N., Botti A.M., Brack J., Bretz T., Briechle F.L., Buchholz P., Bueno A., Buitink S., Buscemi M., Caballero-Mora K.S., Caccianiga L., Calcagni L., Cancio A., Canfora F., Caracas I., Carceller J.M., Caruso R., Castellina A., Catalani F., Cataldi G., Cazon L., Cerda M., Chinellato J.A., Choi K., Chudoba J., Chytka L., Clay R.W., Cerutti A.C.C., Colalillo R., Coleman A., Coluccia M.R., Conceica¸o R., Condorelli A., Consolati G., Contreras F., Convenga F., Covault C.E., Dasso S., Daumiller K., Dawson B.R., Day J.A., De Almeida R.M., De Jesus J., De Jong S.J., De Mauro G., De Mello Neto J.R.T., De Mitri I., De Oliveira J., De Oliveira Franco D., De Souza V., Debatin J., Del Rio M., Deligny O., Dhital N., Di Matteo A., Castro M.L.D., Dobrigkeit C., D'Olivo J.C., Dorosti Q., Dos Anjos R.C., Dova M.T., Ebr J., Engel R., Epicoco I., Erdmann M., Escobar C.O., Etchegoyen A., Falcke H., Farmer J., Farrar G., Fauth A.C., Fazzini N., Feldbusch F., Fenu F., Fick B., Figueira J.M., Filipcic A., Freire M.M., Fujii T., Fuster A., Galea C., Galelli C., Garcia B., Vegas A.L.G., Gemmeke H., Gesualdi F., Gherghel-Lascu A., Ghia P.L., Giaccari U., Giammarchi M., Giller M., Glombitza J., Gobbi F., Golup G., Berisso M.G., Vitale P.F.G., Gongora J.P., Gonzalez N., Goos I., Gora D., Gorgi A., Gottowik M., Grubb T.D., Guarino F., Guedes G.P., Guido E., Hahn S., Halliday R., Hampel M.R., Hansen P., Harari D., Harvey V.M., Haungs A., Hebbeker T., Heck D., Hill G.C., Hojvat C., Horandel J.R., Horvath P., Hrabovsky M., Huege T., Hulsman J., Insolia A., Isar P.G., Johnsen J.A., Jurysek J., Kaa¨pa A., Kampert K.H., Keilhauer B., Kemp J., Klages H.O., Kleifges M., Kleinfeller J., Kopke M., Mezek G.K., Awad A.K., Lago B.L., Lahurd D., Lang R.G., Leigui De Oliveira M.A., Lenok V., Letessier-Selvon A., Lhenry-Yvon I., Presti D.L., Lopes L., Lopez R., Casado A.L., Lorek R., Luce Q., Lucero A., Payeras A.M., Malacari M., Mancarella G., Mandat D., Manning B.C., Manshanden J., Mantsch P., Mariazzi A.G., Maris I.C., Marsella G., Martello D., Martinez H., Bravo O.M., Mastrodicasa M., Mathes H.J., Matthews J., Matthiae G., Mayotte E., Mazur P.O., Medina-Tanco G., Melo D., Menshikov A., Merenda K.-D., Michal S., Micheletti M.I., Miramonti L., Mockler D., Mollerach S., Montanet F., Morello C., Morlino G., Mostafa M., Muller A.L., Muller M.A., Muller S., Mussa R., Muzio M., Namasaka W.M., Nellen L., Niculescu-Oglinzanu M., Niechciol M., Nitz D., Nosek D., Novotny V., Nozka L., Nucita A., Nuez L.A., Palatka M., Pallotta J., Panetta M.P., Papenbreer P., Parente G., Parra A., Pech M., Pedreira F., Pkala J., Pelayo R., Pea-Rodriguez J., Pereira L.A.S., Armand J.P., Perlin M., Perrone L., Peters C., Petrera S., Pierog T., Pimenta M., Pirronello V., Platino M., Pont B., Pothast M., Privitera P., Prouza M., Puyleart A., Querchfeld S., Rautenberg J., Ravignani D., Reininghaus M., Ridky J., Riehn F., Risse M., Ristori P., Rizi V., Carvalho W.R.D., Rojo J.R., Roncoroni M.J., Roth M., Roulet E., Rovero A.C., Ruehl P., Saffi S.J., Saftoiu A., Salamida F., Salazar H., Salina G., Gomez J.D.S., Sanchez F., Santos E.M., Santos E., Sarazin F., Sarmento R., Sarmiento-Cano C., Sato R., Savina P., Schafer C., Scherini V., Schieler H., Schimassek M., Schimp M., Schluter F., Schmidt D., Scholten O., Schovanek P., Schroder F.G., Schroder S., Sciutto S.J., Scornavacche M., Shellard R.C., Sigl G., Silli G., Sima O., Smida R., Sommers P., Soriano J.F., Souchard J., Squartini R., Stadelmaier M., Stanca D., Stanic S., Stasielak J., Stassi P., Streich A., Suarez-Duran M., Sudholz T., Suomijarvi T., Supanitsky A.D., Supik J., Szadkowski Z., Taboada A., Taborda O.A., Tapia A., Timmermans C., Tobiska P., Peixoto C.J.T., Tome B., Elipe G.T., Travaini A., Travnicek P., Trimarelli C., Trini M., Tueros M., Ulrich R., Unger M., Urban M., Vaclavek L., Galicia J.F.V., Valio I., Valore L., Van Vliet A., Varela E., Cardenas B.V., Vasquez-Ramirez A., Veberic D., Ventura C., Quispe I.D.V., Verzi V., Vicha J., Villaseor L., Vink J., Vorobiov S., Wahlberg H., Watson A.A., Weber M., Weindl A., Wiencke L., Wilczynski H., Winchen T., Wirtz M., Wittkowski D., Wundheiler B., Yushkov A., Zas E., Zavrtanik D., Zavrtanik M., Zehrer L., Zepeda A., Ziolkowski M., Zuccarello F., Physics, and Elementary Particle Physics
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, Astrophysics, anisotropy [cosmic radiation], Amplitude, 01 natural sciences, surface [detector], 010303 astronomy & astrophysics, Right ascension, astro-ph.HE, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), OBSERVATÓRIOS, Galactic Center, Astrophysics::Instrumentation and Methods for Astrophysics, Cosmic Rays, Auger, observatory, Physics::Space Physics, Astrophysics - High Energy Astrophysical Phenomena, Extragalactic cosmic ray, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Cosmic ray, cosmic radiation: anisotropy, Galactic center, 0103 physical sciences, High Energy Physics, Pierre auger observatory, 0105 earth and related environmental sciences, Pierre Auger Observatory, detector: surface, Física, Astronomy and Astrophysics, efficiency [trigger], Galaxy, Dipole, Automatic Keywords, Space and Planetary Science, Experimental High Energy Physics, trigger: efficiency, ddc:520, galaxy, Observatory, Energy (signal processing), anisotropies, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], dipole
Abstract: We present measurements of the large-scale cosmic-ray anisotropies in right ascension, using data collected by the surface detector array of the Pierre Auger Observatory over more than 14 years. We determine the equatorial dipole component, ~d⊥, through a Fourier analysis in right ascension that includes weights for each event so as to account for the main detector-induced systematic effects. For the energies at which the trigger efficiency of the array is small, the “East-West” method is employed. Besides using the data from the array with detectors separated by 1500 m, we also include data from the smaller but denser sub-array of detectors with 750 m separation, which allows us to extend the analysis down to ∼ 0.03 EeV. The most significant equatorial dipole amplitude obtained is that in the cumulative bin above 8 EeV, d⊥ = 6.0 +1.0 −0.9%, which is inconsistent with isotropy at the 6σ level. In the bins below 8 EeV, we obtain 99% CL upper-bounds on d⊥ at the level of 1 to 3 percent. At energies below 1 EeV, even though the amplitudes are not significant, the phases determined in most of the bins are not far from the right ascension of the Galactic center, at αGC = −94◦ , suggesting a predominantly Galactic origin for anisotropies at these energies. The reconstructed dipole phases in the energy bins above 4 EeV point instead to right ascensions that are almost opposite to the Galactic center one, indicative of an extragalactic cosmic ray origin., La lista completa de autores puede verse en el archivo asociado., Instituto de Física La Plata
Published: 2020
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12. BAYESIAN ANALYSIS OF COSMIC RAY PROPAGATION: EVIDENCE AGAINST HOMOGENEOUS DIFFUSION

Author: Aaron C. Vincent, T. A. Porter, Michael P. Hobson, Gudlaugur Johannesson, Elena Orlando, Roberto Ruiz de Austri, Igor V. Moskalenko, Roberto Trotta, Farhan Feroz, P. B. Graff, Andrew W. Strong, Johannesson, G, de Austri, Rr, Vincent, Ac, Moskalenko, Iv, Orlando, E, Porter, Ta, Strong, Aw, Trotta, R, Feroz, F, Graff, P, Hobson, Mp, Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], and Science and Technology Facilities Council
Subjects: astroparticle physics, cosmic rays, diffusion, Galaxy: general, ISM: general, methods: statistical, Parameter space, 01 natural sciences, Diffusion (business), 010303 astronomy & astrophysics, cosmic ray, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, 0306 Physical Chemistry (incl. Structural), SUPERNOVA-REMNANTS, general [ISM], SECONDARY, ELEMENTAL COMPOSITION, astroparticle physic, Physical Sciences, 0202 Atomic, Molecular, Nuclear, Particle and Plasma Physics, Astrophysics - High Energy Astrophysical Phenomena, Bar (music), astro-ph.GA, Bayesian probability, statistical [methods], FOS: Physical sciences, Cosmic ray, FERMI-LAT OBSERVATIONS, Astronomy & Astrophysics, Article, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, 0201 Astronomical and Space Sciences, Calibration, ENERGY-SPECTRA, Nested sampling algorithm, general [Galaxy], Science & Technology, NUCLEI, 010308 nuclear & particles physics, CONSTRAINTS, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Computational physics, Interstellar medium, MODEL, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), SOLAR MODULATION, EMISSION
Abstract: We present the results of the most complete ever scan of the parameter space for cosmic ray (CR) injection and propagation. We perform a Bayesian search of the main GALPROP parameters, using the MultiNest nested sampling algorithm, augmented by the BAMBI neural network machine learning package. This is the first such study to separate out low-mass isotopes ($p$, $\bar p$ and He) from the usual light elements (Be, B, C, N, O). We find that the propagation parameters that best fit $p$, $\bar p$, He data are significantly different from those that fit light elements, including the B/C and $^{10}$Be/$^9$Be secondary-to-primary ratios normally used to calibrate propagation parameters. This suggests each set of species is probing a very different interstellar medium, and that the standard approach of calibrating propagation parameters using B/C can lead to incorrect results. We present posterior distributions and best fit parameters for propagation of both sets of nuclei, as well as for the injection abundances of elements from H to Si. The input GALDEF files with these new parameters will be included in an upcoming public GALPROP update., Comment: 20 pages, 10 figures, 5 tables. v2 accepted for publication in ApJ
Published: 2021

13. Beyond the Detector Horizon

Author: Wierda, A. Renske A.C., Wempe, Ewoud, Hannuksela, Otto A., Koopmans, Léon V.E., Van Den Broeck, Chris, Sub Subatomic Physics (SAP), Subatomic Physics, Astronomy, Kapteyn Astronomical Institute, Sub Subatomic Physics (SAP), and Subatomic Physics
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Gravitational wave, Horizon, FOS: Physical sciences, Astronomy and Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Galaxy, Redshift, LIGO, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, False alarm, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Galaxy cluster, Event (probability theory)
Abstract: When gravitational waves pass near massive astrophysical objects, they can be gravitationally lensed. The lensing can split them into multiple wave-fronts, magnify them, or imprint beating patterns on the waves. Here we focus on the multiple images produced by strong lensing. In particular, we investigate strong lensing forecasts, the rate of lensing, and the role of lensing statistics in strong lensing searches. Overall, we find a reasonable rate of lensed detections for double, triple, and quadruple images at the LIGO--Virgo--KAGRA design sensitivity. We also report the rates for A+ and LIGO Voyager and briefly comment on potential improvements due to the inclusion of sub-threshold triggers. We find that most galaxy-lensed events originate from redshifts $z \sim 1-4$ and report the expected distribution of lensing parameters for the observed events. Besides forecasts, we investigate the role of lensing forecasts in strong lensing searches, which explore repeated event pairs. One problem associated with the searches is the rising number of event pairs, which leads to a rapidly increasing false alarm probability. We show how knowledge of the expected galaxy lensing time delays in our searches allow us to tackle this problem. Once the time delays are included, the false alarm probability increases linearly (similar to non-lensed searches) instead of quadratically with time, significantly improving the search. For galaxy cluster lenses, the improvement is less significant. The main uncertainty associated with these forecasts are the merger-rate density estimates at high redshift, which may be better resolved in the future.
Published: 2021

14. Cosmic-Ray Propagation in Light of the Recent Observation of Geminga

Author: G. Jóhannesson, Igor V. Moskalenko, and T. A. Porter
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Astronomy and Astrophysics, Cosmic ray, Astrophysics, 01 natural sciences, Article, Interstellar medium, Pulsar, Space and Planetary Science, 0103 physical sciences, Diffusion (business), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Fermi Gamma-ray Space Telescope
Abstract: The High Altitude Water Cherenkov (HAWC) telescope recently observed extended emission around the Geminga and PSR~B0656+14 pulsar wind nebulae (PWNe). These observations have been used to estimate cosmic-ray (CR) diffusion coefficients near the PWNe that appear to be more than two orders of magnitude smaller than that typically derived for the interstellar medium from the measured abundances of secondary species in CRs. Two-zone diffusion models have been proposed as a solution to this discrepancy, where the slower diffusion zone (SDZ) is confined to a small region around the PWN. Such models are shown to successfully reproduce the HAWC observations of the Geminga PWN while retaining consistency with other CR data. It is found that the size of the SDZ influences the predicted positron flux and the spectral shape of the extended $\gamma$-ray emission at lower energies that can be observed with the {\it Fermi} Large Area Telescope ({\it Fermi} LAT). If the two observed PWNe are not unique, then it is likely that there are similar pockets of slow diffusion around many CR sources elsewhere in the Milky Way. The consequences of such picture for Galactic CR propagation is explored., Comment: 13 pages, 9 figures, submitted to ApJ
Published: 2021

15. The Discovery of a Low-energy Excess in Cosmic-Ray Iron: Evidence of the Past Supernova Activity in the Local Bubble

Author: D. Grandi, Massimo Gervasi, Igor V. Moskalenko, N. Masi, Pier-Giorgio Rancoita, Lucio Quadrani, Davide Rozza, G. Jóhannesson, Mauro Tacconi, Matteo Boschini, S. Pensotti, T. A. Porter, S. Della Torre, G. La Vacca, Boschini, M, Della Torre, S, Gervasi, M, Grandi, D, Jóhannesson, G, La Vacca, G, Masi, N, Moskalenko, I, Pensotti, S, Porter, T, Quadrani, L, Rancoita, P, Rozza, D, and Tacconi, M
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Physics, FOS: Physical sciences, Interplanetary medium, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Spectral line, Article, Galactic cosmic ray, Interstellar medium, Supernova, Heliosphere, FIS/05 - ASTRONOMIA E ASTROFISICA, Local Bubble, FIS/01 - FISICA SPERIMENTALE, Space and Planetary Science, Cosmic ray detector, Cosmic ray source, Ionization energy, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Since its launch, the Alpha Magnetic Spectrometer - 02 (AMS-02) has delivered outstanding quality measurements of the spectra of cosmic-ray (CR) species, $\bar{p}$, $e^{\pm}$, and nuclei, $_1$H-$_8$O, $_{10}$Ne, $_{12}$Mg, $_{14}$Si, which resulted in a number of breakthroughs. One of the latest long awaited surprises is the spectrum of $_{26}$Fe just published by AMS-02. Because of the large fragmentation cross section and large ionization energy losses, most of CR iron at low energies is local, and may harbor some features associated with relatively recent supernova (SN) activity in the solar neighborhood. Our analysis of new iron spectrum together with Voyager 1 and ACE-CRIS data reveals an unexpected bump in the iron spectrum and in the Fe/He, Fe/O, and Fe/Si ratios at 1-2 GV, while a similar feature in the spectra of He, O, Si, and in their ratios is absent, hinting at a local source of low-energy CRs. The found excess fits well with recent discoveries of radioactive $^{60}$Fe deposits in terrestrial and lunar samples, and in CRs. We provide an updated local interstellar spectrum (LIS) of iron in the energy range from 1 MeV nucleon$^{-1}$ to $\sim$10 TeV nucleon$^{-1}$. Our calculations employ the GalProp-HelMod framework that is proved to be a reliable tool in deriving the LIS of CR $\bar{p}$, $e^{-}$, and nuclei $Z\le28$., 12 pages, 9 figures, 5 tables; Accepted for publication in the Astrophysical Journal. arXiv admin note: text overlap with arXiv:2006.01337
Published: 2021

16. High-energy Gamma Rays from the Milky Way: Three-dimensional Spatial Models for the Cosmic-Ray and Radiation Field Densities in the Interstellar Medium

Author: Igor V. Moskalenko, T. A. Porter, and Gudlaugur Johannesson
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astroparticle physics, Physics, Spiral galaxy, 010308 nuclear & particles physics, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Galaxy, Article, Luminosity, Interstellar medium, Space and Planetary Science, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Fermi Gamma-ray Space Telescope
Abstract: High-energy gamma rays of interstellar origin are produced by the interaction of cosmic-ray (CR) particles with the diffuse gas and radiation fields in the Galaxy. The main features of this emission are well understood and are reproduced by existing CR propagation models employing 2D Galactocentric cylindrically symmetrical geometry. However, the high-quality data from instruments like the Fermi Large Area Telescope reveal significant deviations from the model predictions on few to tens of degree scales indicating the need to include the details of the Galactic spiral structure and thus require 3D spatial modelling. In this paper the high-energy interstellar emissions from the Galaxy are calculated using the new release of the GALPROP code employing 3D spatial models for the CR source and interstellar radiation field (ISRF) densities. Three models for the spatial distribution of CR sources are used that are differentiated by their relative proportion of input luminosity attributed to the smooth disc or spiral arms. Two ISRF models are developed based on stellar and dust spatial density distributions taken from the literature that reproduce local near- to far-infrared observations. The interstellar emission models that include arms and bulges for the CR source and ISRF densities provide plausible physical interpretations for features found in the residual maps from high-energy gamma-ray data analysis. The 3D models for CR and ISRF densities provide a more realistic basis that can be used for the interpretation of the non-thermal interstellar emissions from the Galaxy., 23 pages, 14 figures, 1 appendix. ApJ in press
Published: 2021

17. A Statistical Study of Propagating MHD Kink Waves in the Quiescent Corona

Author: Ajay K. Tiwari, Richard Morton, James McLaughlin, and Centrum Wiskunde & Informatica, Amsterdam (CWI), The Netherlands
Subjects: Physics, 010308 nuclear & particles physics, Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Plasma, Coronal loop, F500, 01 natural sciences, Corona, Computational physics, Transverse plane, Amplitude, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, 0103 physical sciences, Physics::Space Physics, Astrophysics::Solar and Stellar Astrophysics, Magnetohydrodynamics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Wave power
Abstract: The Coronal Multi-channel Polarimeter (CoMP) has opened up exciting opportunities to probe transverse MHD waves in the Sun's corona. The archive of CoMP data is utilised to generate a catalogue of quiescent coronal loops that can be used for studying propagating kink waves. The catalogue contains 120 loops observed between 2012-2014. This catalogue is further used to undertake a statistical study of propagating kink waves in the quiet regions of the solar corona, investigating phase speeds, loop lengths, footpoint power ratio and equilibrium parameter values. The statistical study enables us to establish the presence of a relationship between the rate of damping and the length of the coronal loop, with longer coronal loops displaying weaker wave damping. We suggest the reason for this behaviour is related to a decreasing average density contrast between the loop and ambient plasma as loop length increases. The catalogue presented here will provide the community with the foundation for the further study of propagating kink waves in the quiet solar corona., Comment: Submitted to ApJ
Published: 2021
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18. The Physical Properties of Low-redshift FeLoBAL Quasars. I. Spectral-synthesis Analysis of the Broad Absorption-line (BAL) Outflows Using SimBAL

Author: Hyunseop Choi, Karen M. Leighly, Donald M. Terndrup, Collin Dabbieri, Sarah C. Gallagher, and Gordon T. Richards
Subjects: Astrophysics and Astronomy, Space and Planetary Science, Physics, Astronomy and Astrophysics
Abstract: We present the first systematic study of 50 low-redshift (0.66 < z < 1.63) iron low-ionization broad absorption-line quasars (FeLoBALQs) using SimBAL, which represents a more than five-fold increase in the number of FeLoBALQs with detailed absorption line spectral analyses. We found the outflows have a wide range of ionization parameters, − 4 ≲ log U ≲ 1.2 and densities, 2.8 ≲ log n ≲ 8 [ cm − 3 ] . The objects in our sample showed FeLoBAL gas located at a wide range of distances 0 ≲ log R ≲ 4.4 [pc], although we do not find any evidence for disk winds (with R ≪ 0.01 pc) in our sample. The outflow strength primarily depends on the outflow velocity with faster outflows found in quasars that are luminous or that have flat or redder spectral energy distributions. We found that ∼18% of the FeLoBALQs in the sample have the significantly powerful outflows needed for quasar feedback. Eight objects showed overlapping troughs in the spectra, and we identified eleven loitering outflow objects, a new class of FeLoBALQs that are characterized by low outflow velocities and high column density winds located log R ≲ 1 [pc] from the central engine. The FeLoBALs in loitering outflows objects do not show properties expected for radiatively driven winds, and these objects may represent a distinct population among FeLoBALQs. We discuss how the potential acceleration mechanisms and the origins of the FeLoBAL winds may differ for outflows at different locations in quasars.
Published: 2022

19. The Physical Properties of Low-redshift FeLoBAL Quasars. III. The Location and Geometry of the Outflows

Author: Hyunseop Choi, Karen M. Leighly, Collin Dabbieri, Donald M. Terndrup, Sarah C. Gallagher, and Gordon T. Richards
Subjects: Active galactic nuclei, Astrophysics and Astronomy, Broad-absorption line quasar, Space and Planetary Science, Physics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Quasars, Astrophysics - Astrophysics of Galaxies
Abstract: We present continued analysis of a sample of low-redshift iron low-ionization broad absorption-line quasars (FeLoBALQs). Choi et al. (2022) presented $SimBAL$ spectral analysis of BAL outflows in 50 objects. Leighly et al. (2022) analyzed optical emission lines of 30 of those 50 objects and found that they are characterized by either a high accretion rate ($L_\mathrm{Bol}/L_\mathrm{Edd}>0.3$) or low accretion rate ($0.03, Comment: Resubmitted to ApJ after review
Published: 2022

20. NuSTAR Observations of Intrinsically X-Ray Weak Quasar Candidates: An Obscuration-only Scenario

Author: Chaojun Wang, B. Luo, W. N. Brandt, D. M. Alexander, F. E. Bauer, S. C. Gallagher, Jian Huang, Hezhen Liu, and D. Stern
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Space and Planetary Science, Physics, Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We utilize recent NuSTAR observations (co-added depth $\approx55$-120 ks) of PG $1001+054$, PG $1254+047$, and PHL 1811 to constrain their hard X-ray ($\gtrsim5$ keV) weakness and spectral shapes, and thus to investigate the nature of their extreme X-ray weakness. These quasars showed very weak soft X-ray emission, and they were proposed to be intrinsically X-ray weak, with the X-ray coronae producing weak continuum emission relative to their optical/UV emission. However, the new observations suggest an alternative explanation. The NuSTAR 3-24 keV spectral shapes for PG $1001+054$ and PHL 1811 are likely flat (effective power-law photon indices $\Gamma_{\rm eff}=1.0^{+0.5}_{-0.6}$ and $\Gamma_{\rm eff}=1.4^{+0.8}_{-0.7}$, respectively), while the shape is nominal for PG $1254+047$ ($\Gamma_{\rm eff}=1.8\pm0.3$). PG $1001+054$ and PHL 1811 are significantly weak at hard X-ray energies (by factors of $\approx26$-74 at rest-frame 8 keV) compared to the expectations from their optical/UV emission, while PG $1254+047$ is only hard X-ray weak by a factor of $\approx3$. We suggest that X-ray obscuration is present in all three quasars. We propose that, as an alternative to the intrinsic X-ray weakness + X-ray obscuration scenario, the soft and hard X-ray weakness of these quasars can be uniformly explained under an obscuration-only scenario. This model provides adequate descriptions of the multi-epoch soft and hard X-ray data of these quasars, with variable column density and leaked fraction of the partial-covering absorber. We suggest that the absorber is the clumpy dust-free wind launched from the accretion disk. These quasars probably have super-Eddington accretion rates that drive powerful and high-density winds., Comment: 21 pages, 8 figures, accepted for publication in ApJ
Published: 2022

21. A Giant Loop of Ionized Gas Emerging from the Tumultuous Central Region of IC 5063

Author: Luis C. Ho, A. Travascio, W. Peter Maksym, William C. Keel, Travis C. Fischer, Tom Oosterloo, Giuseppina Fabbiano, Jingzhe Ma, Martin Elvis, and Astronomy
Subjects: Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Doubly ionized oxygen, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, symbols.namesake, Astrophysics::Galaxy Astrophysics, Line (formation), High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Seyfert galaxies, Accretion (meteorology), Balmer series, Astronomy and Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, Galaxy, Interstellar medium, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), symbols, Active galaxies, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The biconical radiation pattern extending from an active galactic nucleus (AGN) may strongly photoionize the circumnuclear interstellar medium (ISM) and stimulate emission from the narrow line region (NLR). Observations of the NLR may provide clues to the structure of dense material that preferentially obscures the bicone at certain angles, and may reveal the presence of processes in the ISM tied to AGN accretion and feedback. Ground-based integral field units (IFUs) may study these processes via well-understood forbidden diagnostic lines such as [O III] and [S II], but scales of $\sim10$s of pc remain challenging to spatially resolve at these wavelengths for all but the nearest AGN. We present recent narrow filter Hubble Space Telescope (HST) observations of diagnostic forbidden ([O III], [S II]) and Balmer (H$\alpha$, H$\beta$) lines in the NLR of IC 5063. This AGN's jet inclination into the plane of the galaxy provides an important laboratory for strong AGN-host interactions. We find evidence for a low-ionization loop which emits brightly in [S II] and [N II], and which may arise from plume-like hot outflows that ablate ISM from the galactic plane before escaping laterally. We also present spatially resolved Baldwin-Phillips-Terlevich diagnostic maps of the IC 5063 NLR. These maps suggest a sharp transition to lower-ionization states outside the jet path, and that such emission is dominated by $\sim10-40$ pc clumps and filamentary structure at large (>>25{\deg}) angles from the bicone axis. Such emission may arise from precursorless shocks when AGN outflows impact low-density hot plasma in the cross-cone., Comment: Accepted by ApJ. 18 pages, 8 figures. Follow-up paper to arXiv:2009.10153
Published: 2021

22. Zero-metallicity Hypernova Uncovered by an Ultra-metal-poor Star in the Sculptor Dwarf Spheroidal Galaxy

Author: Lorenzo Posti, Eline Tolstoy, Davide Massari, Else Starkenburg, Pascale Jablonka, Anish M. Amarsi, Stefania Salvadori, Giuseppina Battaglia, Á. Skúladóttir, Amina Helmi, Mike Irwin, Vanessa Hill, Astronomy, Kapteyn Astronomical Institute, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Observatoire astronomique de Strasbourg (ObAS), and Université de Strasbourg (UNISTRA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Metallicity, Milky Way, Population, FOS: Physical sciences, Astrophysics, 01 natural sciences, 0103 physical sciences, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, 010308 nuclear & particles physics, carbon, abundance patterns, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Dwarf spheroidal galaxy, Stars, Supernova, draco, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), high-resolution spectroscopy, chemical evolution, Hypernova, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena
Abstract: Although true metal-free "Population III" stars have so-far escaped discovery, their nature, and that of their supernovae, is revealed in the chemical products left behind in the next generations of stars. Here we report the detection of an ultra-metal poor star in the Sculptor dwarf spheroidal galaxy, AS0039. With [Fe/H]$_{\rm LTE}=-4.11$, it is the most metal-poor star so far discovered in any external galaxy. Contrary to the majority of Milky Way stars at this metallicity, AS0039 is clearly not enhanced in carbon, with [C/Fe]$_{\rm LTE}=-0.75$ and A(C)=+3.60, making it the lowest detected carbon abundance in any star to date. It furthermore lacks $\alpha$-element uniformity, having extremely low [Mg/Ca]$_{\rm NLTE}=-0.60$ and [Mg/Ti]$_{\rm NLTE}=-0.86$, in stark contrast with the near solar ratios observed in C-normal stars within the Milky Way halo. The unique abundance pattern indicates that AS0039 formed out of material that was predominantly enriched by a $\sim$20$ M_\odot$ progenitor star with an unusually high explosion energy $E=10\times10^{51}$ erg. The star AS0039 is thus one of the first observational evidence for zero-metallicity hypernovae and provides a unique opportunity to investigate the diverse nature of Population III stars., Comment: Accepted in ApJL, 7 pages, 3 figures, 1 table, and an appendix (1 figure and 3 tables)
Published: 2021

23. A Detailed Kinematic Study of 3C 84 and Its Connection to γ-Rays

Author: Junghwan Oh, Alan P. Marscher, Sung-Bo Lee, Svetlana G. Jorstad, Yosuke Mizuno, Jongho Park, Sascha Trippe, Jeffrey A. Hodgson, Bindu Rani, Florent Mertens, and Kapteyn Astronomical Institute
Subjects: High energy, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Kinematics, Wavelet analysis, 01 natural sciences, Wavelet, 0103 physical sciences, Very-long-baseline interferometry, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Very long baseline interferometry, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Gamma-ray astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Connection (mathematics), 13. Climate action, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, High energy astrophysics
Abstract: 3C 84 (NGC 1275) is the bright radio core of the Perseus Cluster. Even in the absence of strong relativistic effects, the source has been detected at Gamma-rays up to TeV energies. Despite its intensive study, the physical processes responsible for the high-energy emission in the source remain unanswered. We present a detailed kinematics study of the source and its connection to Gamma-ray emission. The sub-parsec scale radio structure is dominated by slow-moving features in both the eastern and western lanes of the jet. The jet appears to have accelerated to its maximum speed within less than 125 000 gravitational radii. The fastest reliably detected speed in the jet was ~0.9 c. This leads to a minimum Lorentz factor of ~1.35. Our analysis suggests the presence of multiple high-energy sites in the source. If Gamma-rays are associated with kinematic changes in the jet, they are being produced in both eastern and western lanes in the jet. Three Gamma-ray flares are contemporaneous with epochs where the slowly moving emission region splits into two sub-regions. We estimate the significance of these events being associated as ~2-3 sigma. We tested our results against theoretical predictions for magnetic reconnection-induced mini-jets and turbulence and find them compatible., 15 pages, 21 figures, 13 tables, Accepted to ApJ
Published: 2021

24. Testing General Relativity with NuSTAR Data of Galactic Black Holes

Author: Askar B. Abdikamalov, Dimitry Ayzenberg, Ashutosh Tripathi, Jiachen Jiang, Menglei Zhou, Cosimo Bambi, Yuexin Zhang, Honghui Liu, and Astronomy
Subjects: 010504 meteorology & atmospheric sciences, General relativity, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitation, symbols.namesake, 0103 physical sciences, Einstein, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, X-ray astronomy, Spacetime, Gravitational wave, Astronomy and Astrophysics, Rotating black hole, Space and Planetary Science, symbols, Reflection (physics), Astrophysics - High Energy Astrophysical Phenomena
Abstract: Einstein's theory of General Relativity predicts that the spacetime metric around astrophysical black holes is described by the Kerr solution. In this work, we employ state-of-the-art in relativistic reflection modeling to analyze a selected set of NuSTAR spectra of Galactic black holes to obtain the most robust and precise constraints on the Kerr black hole hypothesis possible today. Our constraints are much more stringent than those from other electromagnetic techniques, and with some sources we get stronger constraints than those currently available from gravitational waves., 15 pages, 11 figures. v2: refereed version
Published: 2021

25. Erratum

Author: Christopher D. Fassnacht, Olivier Le Fèvre, Roy R. Gal, Denise Hung, Brian C. Lemaux, O. Cucciati, John McKean, Guilin Liu, Daniela Vergani, Nimish P. Hathi, Lori M. Lubin, Adam Tomczak, D. Pelliccia, Lu Shen, Wenjuan Fang, S. Bardelli, N. Miller, and E. Zucca
Subjects: Physics, Active galactic nucleus, Space and Planetary Science, Astronomy and Astrophysics, Astrophysics
Published: 2021

26. Interactions of Atomic and Molecular Hydrogen with a Diamond-like Carbon Surface: H2 Formation and Desorption

Author: Yuki Kimura, Naoki Watanabe, Tetsuya Hama, Akira Kouchi, and Masashi Tsuge
Subjects: Physics, Number density, 010504 meteorology & atmospheric sciences, Diffusion, chemistry.chemical_element, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Amorphous solid, chemistry, Space and Planetary Science, Chemical physics, Desorption, Ionization, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Kinetic isotope effect, Molecule, 010303 astronomy & astrophysics, Carbon, 0105 earth and related environmental sciences
Abstract: The interactions of atomic and molecular hydrogen with bare interstellar dust grain surfaces are important for understanding H2 formation at relatively high temperatures (>20 K). We investigate the diffusion of physisorbed H atoms and the desorption energetics of H2 molecules on an amorphous diamond-like carbon (DLC) surface. From temperature-programmed desorption experiments with a resonance-enhanced multiphoton ionization (REMPI) method for H2 detection, the H2 coverage-dependent activation energies for H2 desorption are determined. The activation energies decrease with increasing H2 coverage and are centered at 30 meV with a narrow distribution. Using a combination of photostimulated desorption and REMPI methods, the time variations of the surface number density of H2 following atomic and molecular hydrogen depositions are studied. From these measurements, we show that H2 formation on a DLC surface is quite efficient, even at 20 K. A significant kinetic isotope effect for H2 and D2 recombination reactions suggests that H-atom diffusion on a DLC surface is mediated by quantum mechanical tunneling. In astrophysically relevant conditions, H2 recombination due to physisorbed H-atoms is unlikely to occur at 20 K, suggesting that chemisorbed H atoms might play a role in H2 formation at relatively high temperatures., 33 pages, 8 figures, Accepted for publication in ApJ
Published: 2019

27. BAT AGN Spectroscopic Survey. XI. The Covering Factor of Dust and Gas in Swift/BAT Active Galactic Nuclei

Author: David J. Rosario, Lindsay Fuller, Kohei Ichikawa, Franz E. Bauer, Benny Trakhtenbrot, T. Taro Shimizu, Yoshihiro Ueda, Marko Stalevski, Chris Packham, Claudio Ricci, Taiki Kawamuro, Kyuseok Oh, and Michael Koss
Subjects: Active galactic nucleus, 010504 meteorology & atmospheric sciences, INFRARED-EMISSION, Astrophysics::High Energy Astrophysical Phenomena, nuclei [galaxies], FOS: Physical sciences, SPECTRAL ENERGY-DISTRIBUTIONS, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, galaxies [infrared], 01 natural sciences, STAR-FORMATION, Luminosity, SUPERMASSIVE BLACK-HOLES, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Absorption (logic), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Luminosity function (astronomy), Physics, Luminous infrared galaxy, High Energy Astrophysical Phenomena (astro-ph.HE), Supermassive black hole, Spectral density, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Physics and Astronomy, LUMINOSITY FUNCTION, Space and Planetary Science, NGC 1068, Astrophysics of Galaxies (astro-ph.GA), active [galaxies], COSMOLOGICAL EVOLUTION, ASTRONOMICAL DATA, STATISTICAL-METHODS, Astrophysics::Earth and Planetary Astrophysics, SUBARCSECOND MIDINFRARED VIEW, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We quantify the luminosity contribution of active galactic nuclei (AGN) to the 12 $\mu$m, mid-infrared (MIR; 5-38 $\mu$m), and the total IR (5-1000 $\mu$m) emission in the local AGN detected in the all-sky 70-month Swift/Burst Alert Telescope (BAT) ultra hard X-ray survey. We decompose the IR spectral energy distributions (SEDs) of 587 objects into AGN and starburst components using AGN torus and star-forming galaxy templates. This enables us to recover the AGN torus emission also for low-luminosity end, down to $\log (L_{14-150}/{\rm erg}~{\rm s}^{-1}) \simeq 41$, which typically have significant host galaxy contamination. We find that the luminosity contribution of the AGN to the 12 $\mu$m, the MIR, and the total IR band is an increasing function of the 14-150 keV luminosity. We also find that for the most extreme cases, the IR pure-AGN emission from the torus can extend up to 90 $\mu$m. The obtained total IR AGN luminosity through the IR SED decomposition enables us to estimate the fraction of the sky obscured by dust, i.e., the dust covering factor. We demonstrate that the median of the dust covering factor is always smaller than that of the X-ray obscuration fraction above the AGN bolometric luminosity of $\log (L_{\rm bol}/{\rm erg}~{\rm s}^{-1}) \simeq 42.5$. Considering that X-ray obscuration fraction is equivalent to the covering factor coming from both the dust and gas, it indicates that an additional neutral gas component, along with the dusty torus, is responsible for the absorption of X-ray emission., Comment: 21 pages, 15 figures, accepted for publication in ApJ. The full list of Table 1 is available at http://www.kusastro.kyoto-u.ac.jp/~ichikawa/Table1_MR_20181107.txt
Published: 2019

28. Populations of Stellar-mass Black Holes from Binary Systems

Author: Łukasz Wyrzykowski, Grzegorz Wiktorowicz, Krzysztof Belczynski, Krzysztof A. Rybicki, Martyna Chruslinska, and Jakub Klencki
Subjects: Initial mass function, 010504 meteorology & atmospheric sciences, Stellar mass, Metallicity, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Gravitational microlensing, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Star formation, Astronomy and Astrophysics, Galaxy, Black hole, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: In large and complicated stellar systems like galaxies it is difficult to predict the number and characteristics of a black hole population. Such populations may be modelled as an aggregation of homogeneous (i.e. having uniform star formation history and the same initial chemical composition) stellar populations. Using realistic evolutionary models we predict the abundances and properties of black holes formed from binaries in these environments. We show that the black hole population will be dominated by single black holes originating from binary disruptions and stellar mergers. Furthermore, we discuss how black hole populations are influenced by such factors as initial parameters, metallicity, initial mass function, and natal kick models. As an example application of our results, we estimate that about 26 microlensing events to happen every year in the direction of the Galactic Bulge due to black holes in a survey like OGLE-IV. Our results may be used to perform in-depth studies related to realistic black hole populations, e.g. observational predictions for space survey missions like Gaia, or Einstein Probe. We prepared a publicly available database with the raw data from our simulations to be used for more in-depth studies., Comment: 20 pages, 16 figures, revised version
Published: 2019

29. Orion SrcI's Disk Is Salty

Author: Adam Ginsburg, Richard Plambeck, Melvyn Wright, Brett A. McGuire, Ciriaco Goddi, and John Bally
Subjects: Physics, Astrochemistry, Space and Planetary Science, Astronomy, Astronomy and Astrophysics
Abstract: Contains fulltext : 201308.pdf (Publisher’s version ) (Open Access)
Published: 2019

30. EHT-HOPS Pipeline for Millimeter VLBI Data Reduction

Author: Michael D. Johnson, Kazunori Akiyama, Sheperd S. Doeleman, Maciek Wielgus, Michael Janssen, Katherine L. Bouman, Roger J. Cappallo, Lindy Blackburn, Vincent L. Fish, John E. Barrett, Andrew Chael, Geoffrey B. Crew, Colin J. Lonsdale, Sara Issaoun, and Chi-kwan Chan
Subjects: 010504 meteorology & atmospheric sciences, Astronomy, Pipeline (computing), Global Arrays, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Submillimeter Array, 0103 physical sciences, Very-long-baseline interferometry, Calibration, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Remote sensing, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Interferometry, Space and Planetary Science, Millimeter, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Data reduction
Abstract: We present the design and implementation of an automated data calibration and reduction pipeline for very-long-baseline interferometric (VLBI) observations taken at millimeter wavelengths. These short radio-wavelengths provide the best imaging resolution available from ground-based VLBI networks such as the Event Horizon Telescope (EHT) and the Global Millimeter VLBI Array (GMVA), but require specialized processing due to the strong effects from atmospheric opacity and turbulence as well as the heterogeneous nature of existing global arrays. The pipeline builds upon a calibration suite (HOPS) originally designed for precision geodetic VLBI. To support the reduction of data for astronomical observations, we have developed an additional framework for global phase and amplitude calibration which provides output in a standard data format for astronomical imaging and analysis. We test the pipeline on observations taken at 3.5 mm (86 GHz) by the GMVA joined by the phased Atacama Large Millimeter/submillimeter Array in April 2017, and demonstrate the benefits from the specialized processing of high frequency VLBI data with respect to classical analysis techniques.
Published: 2019

31. Gravity-dominated Collisions: A Model for the Largest Remnant Masses with Treatment for 'Hit and Run' and Density Stratification

Author: Martin Jutzi, Willy Benz, A. Reufer, Travis Gabriel, Erik Asphaug, and Alan Jackson
Subjects: Planetesimal, 010504 meteorology & atmospheric sciences, Hydrodynamical simulations (767), Impact phenomena (779), Planet formation (1241), 01 natural sciences, Article, Smoothed-particle hydrodynamics, Planet, 0103 physical sciences, Transition zone, Thermal, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Hydrodynamics (1963), 520 Astronomy, Astronomy and Astrophysics, Mechanics, Planetary science (1255), Collision, 620 Engineering, Inner planets (797), Planetary science, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics, Formation and evolution of the Solar System
Abstract: We develop empirical relationships for the accretion and erosion of colliding gravity-dominated bodies of various compositions under conditions expected in late-stage solar system formation. These are fast, easily coded relationships based on a large database of smoothed particle hydrodynamics (SPH) simulations of collisions between bodies of different compositions, including those that are water rich. The accuracy of these relations is also comparable to the deviations of results between different SPH codes and initial thermal/rotational conditions. We illustrate the paucity of disruptive collisions between major bodies, as compared to collisions between less massive planetesimals in late-stage planet formation, and thus focus on more probable, low-velocity collisions, though our relations remain relevant to disruptive collisions as well. We also pay particular attention to the transition zone between merging collisions and those where the impactor does not merge with the target, but continues downrange, a “hit-and-run” collision. We find that hit-and-run collisions likely occur more often in density-stratified bodies and across a wider range of impact angles than suggested by the most commonly used analytic approximation. We also identify a possible transitional zone in gravity-dominated collisions where larger bodies may undergo more disruptive collisions when the impact velocity exceeds the sound speed, though understanding this transition warrants further study. Our results are contrary to the commonly assumed invariance of total mass (scale), density structure, and material composition on the largest remnants of giant impacts. We provide an algorithm for adopting our model into N-body planet formation simulations, so that the mass of growing planets and debris can be tracked.
Published: 2021

32. The Stars of the HETDEX Survey. I. Radial Velocities and Metal-Poor Stars from Low-Resolution Stellar Spectra

Author: Karl Gebhardt, Keith Hawkins, Christopher Sneden, Dustin Davis, Barbara G. Castanheira, Donald P. Schneider, Caitlin M. Casey, Andreas Kelz, J. Craig Wheeler, Steven L. Finkelstein, Daniel J. Farrow, Gary J. Hill, Erin Mentuch Cooper, Andreia Carrillo, Howard E. Bond, Robin Ciardullo, Greg Zeimann, Matthias Steinmetz, Matthew Shetrone, Chenxu Liu, Else Starkenburg, and Astronomy
Subjects: Physics, 010308 nuclear & particles physics, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Segue, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Astronomical spectroscopy, Spectral line, law.invention, LAMOST, Telescope, Stars, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, law, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Dark energy, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract: The Hobby-Eberly Telescope Dark Energy Experiment (HETDEX) is an unbiased, massively multiplexed spectroscopic survey, designed to measure the expansion history of the universe through low-resolution ($R\sim750$) spectra of Lyman-Alpha Emitters. In its search for these galaxies, HETDEX will also observe a few 10$^{5}$ stars. In this paper, we present the first stellar value-added catalog within the internal second data release of the HETDEX Survey (HDR2). The new catalog contains 120,571 low-resolution spectra for 98,736 unique stars between $10 < G < 22$ spread across the HETDEX footprint at relatively high ($b\sim60^\circ$) Galactic latitudes. With these spectra, we measure radial velocities (RVs) for $\sim$42,000 unique FGK-type stars in the catalog and show that the HETDEX spectra are sufficient to constrain these RVs with a 1$��$ precision of 28.0 km/s and bias of 3.5 km/s with respect to the LAMOST surveys and 1$��$ precision of 27.5 km/s and bias of 14.0 km/s compared to the SEGUE survey. Since these RVs are for faint ($G\geq16$) stars, they will be complementary to Gaia. Using t-Distributed Stochastic Neighbor Embedding (t-SNE), we also demonstrate that the HETDEX spectra can be used to determine a star's T${\rm{eff}}$, and log g and its [Fe/H]. With the t-SNE projection of the FGK-type stars with HETDEX spectra we also identify 416 new candidate metal-poor ([Fe/H] $< -1$~dex) stars for future study. These encouraging results illustrate the utility of future low-resolution stellar spectroscopic surveys., 18 Pages, 11 Figures, 2 Tables. Accepted to ApJ
Published: 2021

33. The Relativistic Jet Orientation and Host Galaxy of the Peculiar Blazar PKS 1413+135

Author: T. J. Pearson, Anne Lähteenmäki, Ian Browne, Keith Grainge, A. L. Peirson, Matthew L. Lister, J. A. Zensus, B. T. Soifer, Vikram Ravi, Talvikki Hovatta, Mark Gurwell, Vikram Singh, Peter N. Wilkinson, Margo F. Aller, A. C. S. Readhead, Sebastian Kiehlmann, G. B. Taylor, Michael Werner, Eric S. Perlman, Thomas Mcaloone, Ioannis Liodakis, Harish Vedantham, Varoujan Gorjian, Rodrigo Reeves, M. Hodges, Merja Tornikoski, Walter Max-Moerbeck, Vasiliki Pavlidou, Roger Blandford, and Astronomy
Subjects: Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysical jet, 0103 physical sciences, Blazar, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Jet (fluid), Spiral galaxy, Seyfert galaxies, 010308 nuclear & particles physics, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Redshift, Galaxy, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Radio active galactic nuclei, Strong gravitational lensing, Relativistic jets, Astrophysics - High Energy Astrophysical Phenomena, Blazars, BL Lac object, Apparent superluminal motion
Abstract: PKS 1413+135 is one of the most peculiar blazars known. Its strange properties led to the hypothesis almost four decades ago that it is gravitationally lensed by a mass concentration associated with an intervening galaxy. It exhibits symmetric achromatic variability, a rare form of variability that has been attributed to gravitational milli-lensing. It has been classified as a BL Lac object, and is one of the rare objects in this class with a visible counterjet. BL Lac objects have jet axes aligned close to the line of sight. It has also been classified as a compact symmetric object, which have jet axes not aligned close to the line of sight. Intensive efforts to understand this blazar have hitherto failed to resolve even the questions of the orientation of the relativistic jet, and the host galaxy. Answering these two questions is important as they challenge our understanding of jets in active galactic nuclei and the classification schemes we use to describe them. We show that the jet axis is aligned close to the line of sight and PKS 1413+135 is almost certainly not located in the apparent host galaxy, but is a background object in the redshift range $0.247 < z < 0.5$. The intervening spiral galaxy at $z = 0.247$ provides a natural host for the putative lens responsible for symmetric achromatic variability and is shown to be a Seyfert 2 galaxy. We also show that, as for the radio emission, a "multizone" model is needed to account for the high-energy emission., Accepted for publication in The Astrophysical Journal. 28 pages, 15 figures
Published: 2021

34. Ring Formation by Coagulation of Dust Aggregates in the Early Phase of Disk Evolution around a Protostar

Author: Hauyu Baobab Liu, Hiroshi Kobayashi, Yichen Zhang, Nami Sakai, Koji Murakawa, Satoshi Okuzumi, Hidekazu Tanaka, Satoshi Ohashi, and Riouhei Nakatani
Subjects: Physics, Earth and Planetary Astrophysics (astro-ph.EP), Star formation, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Ring (chemistry), Circumstellar disk, Interstellar medium, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Coagulation (water treatment), Protostar, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Early phase, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: Ring structures are observed by (sub-)millimeter dust continuum emission in various circumstellar disks from early stages of Class 0 and I to late stage of Class II young stellar objects (YSOs). In this paper, we study one of the possible scenarios of such ring formation in early stage, which is coagulation of dust aggregates. The dust grains grow in an inside-out manner because the growth timescale is roughly proportional to the orbital period. The boundary of the dust evolution can be regarded as the growth front, where the growth time is comparable to the disk age. With radiative transfer calculations based on the dust coagulation model, we find that the growth front can be observed as a ring structure because dust surface density is sharply changed at this position. Furthermore, we confirm that the observed ring positions in the YSOs with an age of $\lesssim1$ Myr are consistent with the growth front. The growth front could be important to create the ring structure in particular for early stage of the disk evolution such as Class 0 and I sources., 15 pages, 12 figures, 1 table, accepted for publication in ApJ
Published: 2021

35. A Test of the Hadronic Origin of γ-Rays from Blazars with Follow-up up to a Month Later of IceCube Alerts with Imaging Air Cherenkov Telescopes

Author: Damiano Fiorillo, Chun Fai Tung, Konstancja Satalecka, and I. Taboada
Subjects: Physics, 03 medical and health sciences, 0302 clinical medicine, Space and Planetary Science, 0103 physical sciences, Hadron, Astronomy and Astrophysics, Astrophysics, Blazar, 010303 astronomy & astrophysics, 030226 pharmacology & pharmacy, 01 natural sciences, Cherenkov radiation
Published: 2021
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36. The Observability of Plasmoid-powered γ-Ray Flares with the Fermi Large Area Telescope

Author: Maria Petropoulou, Ian Christie, and Manuel Meyer
Subjects: Physics, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Astronomy and Astrophysics, Quasar, Magnetic reconnection, Plasmoid, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Gamma-ray astronomy, 01 natural sciences, Relativistic particle, Astrophysical jet, Space and Planetary Science, Physics::Space Physics, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Blazar, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Fermi Gamma-ray Space Telescope
Abstract: The exact mechanism for the production of fast $\gamma$-ray variability in blazars remains debated. Magnetic reconnection, in which plasmoids filled with relativistic particles and magnetic fields are formed, is a viable candidate to explain the broadband electromagnetic spectrum and variability of these objects. Using state-of-the-art magnetic reconnection simulations, we generate realistic $\gamma$-ray light curves that would be observed with the Fermi Large Area Telescope. A comparison with observed $\gamma$-ray flares from flat spectrum radio quasars (FSRQs) reveals that magnetic reconnection events lead to comparable flux levels and variability patterns, in particular when the reconnection layer is slightly misaligned with the line of sight. Emission from fast plasmoids moving close to the line of sight could explain fast variability on the time scales of minutes for which evidence has been found in observations of FSRQs. Our results motivate improvements in existing radiative transfer simulations as well as dedicated searches for fast variability as evidence for magnetic reconnection events., Comment: 19 pages, 6 Figures. Accepted in ApJ. Matches published version
Published: 2021
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37. Where Have All the Solar-like Stars Gone? Rotation Period Detectability at Various Inclinations and Metallicities

Author: Emre Işık, V. Witzke, Timo Reinhold, Alexander Shapiro, N.-E. Nèmec, Sami K. Solanki, TAÜ, Mühendislik Fakültesi, Bilgisayar Mühendisliği Bölümü, and Işık, Emre
Subjects: Rotation period, 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, G-type Stars, 010502 geochemistry & geophysics, Rotation, Stellar classification, 01 natural sciences, Spitzer Space Telescope, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences, Physics, G-Sterne, Stellar rotation, G-tipi Yıldızlar, Astronomy and Astrophysics, Light curve, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Solar rotation, Astrophysics::Earth and Planetary Astrophysics
Abstract: The plethora of photometric data collected by the Kepler space telescope has promoted the detection of tens of thousands of stellar rotation periods. However, these periods are not found to an equal extent among different spectral types. Interestingly, early G-type stars with near-solar rotation periods are strongly underrepresented among those stars with known rotation periods. In this study we investigate whether the small number of such stars can be explained by difficulties in the period determination from photometric time series. For that purpose, we generate model light curves of early G-type stars with solar rotation periods for different inclination angles, metallicities and (magnitude-dependent) noise levels. We find that the detectability is determined by the predominant type of activity (i.e. spot or faculae domination) on the surface, which defines the degree of irregularity of the light curve, and further depends on the level of photometric noise. These two effects significantly complicate the period detection and explain the lack of solar-like stars with known near-solar rotation periods. We conclude that the rotation periods of the majority of solar-like stars with near-solar rotation periods remain undetected to date. Finally, we promote the use of new techniques to recover more periods of near-solar rotators., Comment: 14 pages, 7 figures, accepted for publication in ApJL
Published: 2021
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38. Classification of High-resolution Solar H α Spectra Using t -distributed Stochastic Neighbor Embedding

Author: Robert Kamlah, Christoph Kuckein, Andrea Diercke, Horst Balthasar, Ioannis Kontogiannis, Meetu Verma, Carsten Denker, Partha Sarathi Pal, Ekaterina Dineva, and Gal Matijevic
Subjects: Physics, 010504 meteorology & atmospheric sciences, High resolution, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Spectral line, Computational physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, t-distributed stochastic neighbor embedding, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, Spectroscopy, Astrophysics - Instrumentation and Methods for Astrophysics, 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences
Abstract: The H{\alpha} spectral line is a well-studied absorption line revealing properties of the highly structured and dynamic solar chromosphere. Typical features with distinct spectral signatures in H{\alpha} include filaments and prominences, bright active-region plages, superpenumbrae around sunspots, surges, flares, Ellerman bombs, filigree, and mottles and rosettes, among others. This study is based on high-spectral resolution H{\alpha} spectra obtained with the echelle spectrograph of the Vacuum Tower Telescope (VTT) located at Observatorio del Teide (ODT), Tenerife, Spain. The t-distributed Stochastic Neighbor Embedding (t-SNE) is a machine learning algorithm, which is used for nonlinear dimensionality reduction. In this application, it projects H{\alpha} spectra onto a two-dimensional map, where it becomes possible to classify the spectra according to results of Cloud Model (CM) inversions. The CM parameters optical depth, Doppler width, line-of-sight velocity, and source function describe properties of the cloud material. Initial results of t-SNE indicate its strong discriminatory power to separate quiet-Sun and plage profiles from those that are suitable for CM inversions. In addition, a detailed study of various t-SNE parameters is conducted, the impact of seeing conditions on the classification is assessed, results for various types of input data are compared, and the identified clusters are linked to chromospheric features. Although t-SNE proves to be efficient in clustering high-dimensional data, human inference is required at each step to interpret the results. This exploratory study provides a framework and ideas on how to tailor a classification scheme towards specific spectral data and science questions., Comment: 16 pages, 14 figures, Accepted to be published in Astrophysical Journal
Published: 2021
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39. A New Cosmic-Ray-driven Instability

Author: Christoph Pfrommer, Timon Thomas, and Mohamad Shalaby
Subjects: 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Cosmic ray, 01 natural sciences, Instability, Acceleration, 0103 physical sciences, Pitch angle, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Galaxy cluster, 0105 earth and related environmental sciences, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, Astronomy and Astrophysics, Computational Physics (physics.comp-ph), Astrophysics - Astrophysics of Galaxies, Galaxy, Physics - Plasma Physics, Computational physics, Plasma Physics (physics.plasm-ph), Particle acceleration, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - High Energy Astrophysical Phenomena, Physics - Computational Physics
Abstract: Cosmic ray (CR)-driven instabilities play a decisive role during particle acceleration at shocks and CR propagation in galaxies and galaxy clusters. These instabilities amplify magnetic fields and modulate CR transport so that the intrinsically collisionless CR population is tightly coupled to the thermal plasma and provides dynamical feedback. Here, we show that CRs with a finite pitch angle drive electromagnetic waves (along the background magnetic field) unstable on intermediate scales between the gyro-radii of CR ions and electrons as long as CRs are drifting with a velocity less than half of the Alfv\'en speed of electrons. By solving the linear dispersion relation, we show that this new instability typically grows faster by more than an order of magnitude in comparison to the commonly discussed resonant instability at the ion gyroscale. We find the growth rate for this intermediate-scale instability and identify the growing modes as background ion-cyclotron modes in the frame that is comoving with the CRs. We confirm the theoretical growth rate with a particle-in-cell (PIC) simulation and study the non-linear saturation of this instability. We identify three important astro-physical applications of this intermediate-scale instability, which is expected to 1. modulate CR transport and strengthen CR feedback in galaxies and galaxy clusters, 2. enable electron injection into the diffusive shock acceleration process, and 3. decelerate CR escape from the sites of particle acceleration which would generate gamma-ray halos surrounding CR sources such as supernova remnants., Comment: 16 pages, 13 figures, 2 tables. Accepted to ApJ. Comments are welcome. An animation for the growth of the new instability can be found at http://www.youtube.com/watch?v=yP2dBCPOQYc
Published: 2021
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40. Orbital Migration and Circularization of Tidal Debris by Alfvén-wave Drag: Circumstellar Debris and Pollution around White Dwarfs

Author: Douglas N. C. Lin, Shang-Fei Liu, and Yun Zhang
Subjects: Pollution, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Alfvén wave, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, media_common, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, White dwarf, Astronomy, Astronomy and Astrophysics, Debris, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Drag, Asteroid, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract: A significant fraction of white dwarfs (WDs) exhibit signs of ongoing accretion of refractory elements at rates $\sim10^3$--$10^7$ kg s$^{-1}$, among which, 37 WDs were detected to harbor dusty debris disks. Such a concurrence requires not only fertile reservoirs of planetary material, but also a high duty cycle of metal delivery. It has been commonly suggested that this material could be supplied by Solar System analogs of Main Belt asteroids or Kuiper Belt objects. Here we consider the primary progenitors of WD pollutants as a population of residual high-eccentricity planetesimals, de-volatilized during the stellar giant phases. Equivalent to the Solar System's long-period comets, they are scattered to the proximity of WDs by perturbations from remaining planets, Galactic tides, passing molecular clouds, and nearby stars. These objects undergo downsizing when they venture within the tidal disruption limit. We show quantitatively how the breakup condition and fragment sizes are determined by material strength and gravity. Thereafter, the fragments' semi-major axes need to decay by at least $\sim$6 orders of magnitude before their constituents are eventually accreted onto the surface of WDs. We investigate the orbital evolution of these fragments around WDs and show that WDs' magnetic fields induce an Alfv\'en-wave drag during their periastron passages and rapidly circularize their orbits. This process could be responsible for the observed accretion rates of heavy-elements and the generation of circum-WD debris disks. A speculative implication is that giant planets may be common around WDs' progenitors and they may still be bound to some WDs today., Comment: Accepted for publication in ApJ. 16 pages, 4 figures and 1 table
Published: 2021
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41. ALMA and IRIS Observations of the Solar Chromosphere. I. An On-disk Type II Spicule

Author: Viggo Hansteen, Sven Wedemeyer, Alberto Sainz Dalda, Bart De Pontieu, T. S. Bastian, Jaime de la Cruz Rodríguez, Shahin Jafarzadeh, Juan Martinez-Sykora, Georgios Chintzoglou, and Mikolaj Szydlarski
Subjects: 010504 meteorology & atmospheric sciences, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Submillimeter Array, 0103 physical sciences, Radiative transfer, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Chromosphere, Spectrograph, Solar and Stellar Astrophysics (astro-ph.SR), Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Plage, Solar transition region, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Solar physics, Convection zone, Astrophysics - Solar and Stellar Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics::Earth and Planetary Astrophysics
Abstract: We present observations of the solar chromosphere obtained simultaneously with the Atacama Large Millimeter/submillimeter Array (ALMA) and the Interface Region Imaging Spectrograph (IRIS). The observatories targeted a chromospheric plage region of which the spatial distribution (split between strongly and weakly magnetized regions) allowed the study of linear-like structures in isolation, free of contamination from background emission. Using these observations in conjunction with a radiative magnetohydrodynamic 2.5D model covering the upper convection zone all the way to the corona that considers non-equilibrium ionization effects, we report the detection of an on-disk chromospheric spicule with ALMA and confirm its multithermal nature., 29 pages, 9 figures, Accepted for publication in the Astrophysical Journal. This version replaces the previous submission, which is now split into two companion papers
Published: 2021
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42. SN 2013ai: A Link between Hydrogen-rich and Hydrogen-poor Core-collapse Supernovae

Author: Melina C. Bersten, Melissa Shahbandeh, J. Serón, Nicholas B. Suntzeff, Tao Chen, B. Englert, George H Marion, Scott C. Davis, Lluís Galbany, J. D. Lyman, Adam Fisher, Mark M. Phillips, E. E. Falco, Christopher R. Burns, Justyn R. Maund, Chris Ashall, Peter Hoeflich, A. Bunzel, Gastón Folatelli, Sanjay Kumar, Stefano Benetti, L. Martinez, Nidia Morrell, K. Ertini, Seppo Mattila, David Young, Carlos Contreras, Mark Sullivan, Nancy Elias-Rosa, Jessica R. Lu, M. D. Stritzinger, Joseph P. Anderson, Morgan Fraser, Eric Hsiao, Robert P. Kirshner, P. J. Pessi, National Science Foundation (US), Danish Agency for Science, Technology and Innovation, Royal Society (UK), National Aeronautics and Space Administration (US), European Commission, Ministerio de Ciencia, Innovación y Universidades (España), and Villum Fonden
Subjects: Absolute magnitude, 010504 meteorology & atmospheric sciences, Hydrogen, chemistry.chemical_element, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, purl.org/becyt/ford/1 [https], 0103 physical sciences, Core-collapse supernovae, 010303 astronomy & astrophysics, Helium, 0105 earth and related environmental sciences, Envelope (waves), Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Late stellar evolution, Astronomy and Astrophysics, purl.org/becyt/ford/1.3 [https], Light curve, Type II supernova, Supernova, chemistry, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, type II supernovae
Abstract: Davis, S., et al., We present a study of the optical and near-infrared (NIR) spectra of SN 2013ai along with its light curves. These data range from discovery until 380 days after explosion. SN 2013ai is a fast declining Type II supernova (SN II) with an unusually long rise time, 18.9 2.7 days in the V-band, and a bright V-band peak absolute magnitude of -18.7 0.06 mag. The spectra are dominated by hydrogen features in the optical and NIR. The spectral features of SN 2013ai are unique in their expansion velocities, which, when compared to large samples of SNe II, are more than 1,000 km s-1 faster at 50 days past explosion. In addition, the long rise time of the light curve more closely resembles SNe IIb rather than SNe II. If SN 2013ai is coeval with a nearby compact cluster, we infer a progenitor zero-age main-sequence mass of ∼17 M o˙. After performing light-curve modeling, we find that SN 2013ai could be the result of the explosion of a star with little hydrogen mass, a large amount of synthesized 56Ni, 0.3-0.4 M o˙, and an explosion energy of 2.5-3.0 1051 erg. The density structure and expansion velocities of SN 2013ai are similar to those of the prototypical SN IIb, SN 1993J. However, SN 2013ai shows no strong helium features in the optical, likely due to the presence of a dense core that prevents the majority of γ-rays from escaping to excite helium. Our analysis suggests that SN 2013ai could be a link between SNe II and stripped-envelope SNe., The work of the CSP-II has been generously supported by the National Science Foundation under grants AST-1008343, AST1613426, AST-1613455, and AST1613472. The CSP-II was also supported in part by the Danish Agency for Science and Technology and Innovation through a Sapere Aude Level 2 grant. M.F. is supported by a Royal Society—Science Foundation Ireland University Research Fellowship. P.H. acknowledges support by grants of the NSF AST-1008962 and NASA’s ATP1909476. L.G. was funded by the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement No. 839090. This work has been partially supported by the Spanish grant PGC2018-095317- B-C21 within the European Funds for Regional Development (FEDER). T.W.C. acknowledges the EU Funding under Marie Skłodowska-Curie grant agreement No 842471. M.S. is supported by generous grants from Villum FONDEN (13261, 28021) and by a project grant (8021-00170B) awarded by the Independent Research Fund Denmark.
Published: 2021
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43. The Post-impact Evolution of the X-Ray-emitting Gas in SNR 1987A as Viewed by XMM-Newton

Author: L. Sun, Dmitry Prokhorov, Jacco Vink, Yang Chen, Denys Malyshev, Gerd Pühlhofer, Ping Zhou, and High Energy Astrophys. & Astropart. Phys (API, FNWI)
Subjects: High Energy Astrophysical Phenomena (astro-ph.HE), SHARP, Physics, Horizon 2020, X-ray astronomy, Supernova remnants, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, X-ray, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Interstellar medium, Supernova, Supernovae, 13. Climate action, Space and Planetary Science, 0103 physical sciences, European Union (EU), Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Since 1996 the blast wave driven by SN 1987A has been interacting with the dense circumstellar material, which provides us with a unique opportunity to study the early evolution of a newborn supernova remnant (SNR). Based on the XMM-Newton RGS and EPIC-pn X-ray observations from 2007 to 2019, we investigated the post-impact evolution of the X-ray emitting gas in SNR 1987A. The hot plasma is represented by two non-equilibrium ionization components with temperature of $\sim0.6$ keV and $\sim2.5$ keV. The low-temperature plasma has a density $\sim2400$ cm$^{-3}$, which is likely dominated by the lower density gas inside the equatorial ring (ER). The high-temperature plasma with a density $\sim550$ cm$^{-3}$ could be dominated by the H II region and the high-latitude material beyond the ring. In the last few years, the emission measure of the low-temperature plasma has been decreasing, indicating that the blast wave has left the main ER. But the blast wave is still propagating into the high-latitude gas, resulting in the steadily increase of the high-temperature emission measure. In the meantime, the average abundances of N, O, Ne, and Mg are found to be declining, which may reflect the different chemical compositions between two plasma components. We also detected the Fe K lines in most of the observations, showing increasing flux and centroid energy. We interpret the Fe K lines as from a third hot component, which may come from the reflected shock-heated gas or originate from Fe-rich ejecta clumps, shocked by the reverse shock., Comment: 33 pages, 10 figures, accepted for publication in ApJ
Published: 2021
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44. Ultramassive Black Holes in the Most Massive Galaxies: M BH – σ versus M BH – R b

Author: Armando Gil de Paz, Johan H. Knapen, and Bililign T. Dullo
Subjects: Physics, Supermassive black hole, 010504 meteorology & atmospheric sciences, Velocity dispersion, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Black hole, Space and Planetary Science, 0103 physical sciences, Elliptical galaxy, 010303 astronomy & astrophysics, Lenticular galaxy, 0105 earth and related environmental sciences
Abstract: We investigate the nature of the relations between black hole (BH) mass (M BH) and the central velocity dispersion (σ) and, for core-Sérsic galaxies, the size of the depleted core (R b). Our sample of 144 galaxies with dynamically determined M BH encompasses 24 core-Sérsic galaxies, thought to be products of gas-poor mergers, and reliably identified based on high-resolution Hubble Space Telescope imaging. For core-Sérsic galaxies, i.e., combining normal-core (R b R b ≳ 0.5 kpc), we find that M BH correlates remarkably well with R b such that M BH ∝ R b 1.20 ± 0.14 (rms scatter in log M BH of Δrms ∼ 0.29 dex), confirming previous works on the same galaxies apart from three new ones. Separating the sample into Sérsic, normal-core and large-core galaxies, we find that Sérsic and normal-core galaxies jointly define a single log-linear M BH–σ relation M BH ∝ σ 4.88±0.29 with Δrms ∼ 0.47 dex; however, at the high-mass end, large-core galaxies (four with measured M BH) are offset upward from this relation by (2.5–4) × σ s, explaining the previously reported steepening of the M BH–σ relation for massive galaxies. Large-core spheroids have magnitudes M V ≲ −23.50 mag, half-light radii R e ≳ 10 kpc, and are extremely massive, M * ≳ 1012 M ☉. Furthermore, these spheroids tend to host ultramassive BHs (M BH ≳ 1010 M ☉) tightly connected with their R b rather than σ. The less popular M BH–R b relation exhibits ∼62% less scatter in log M BH than the M BH–σ relations. Our findings suggest that large-core spheroids form via multiple major “dry” merger events involving super/ultramassive BHs, consistent with the flattening of the σ–L V relation observed at M V ≲ −23.5 mag.
Published: 2021
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45. Spatially Resolved RGS Analysis of Kepler's Supernova Remnant

Author: Aya Bamba, Jacco Vink, Hiroyuki Uchida, John P. Hughes, Tomoaki Kasuga, Satoru Katsuda, Toshiki Sato, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Gravitation and Astroparticle Physics Amsterdam
Subjects: Physics, High Energy Astrophysical Phenomena (astro-ph.HE), X-ray astronomy, Line-of-sight, Astrophysics::High Energy Astrophysical Phenomena, White dwarf, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, General Medicine, Astrophysics::Cosmology and Extragalactic Astrophysics, Supernova, Space and Planetary Science, Reflection (physics), Asymptotic giant branch, Astrophysics::Solar and Stellar Astrophysics, Satellite, Astrophysics::Earth and Planetary Astrophysics, Supernova remnant, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract: The distribution and kinematics of the circumstellar medium (CSM) around a supernova remnant (SNR) tell us useful information about the explosion of its natal supernova (SN). Kepler's SNR, the remnant of SN1604, is widely regarded to be of Type Ia origin. Its shock is moving through a dense, asymmetric CSM. The presence of this dense gas suggests that its parent progenitor system consisted of a white dwarf and an asymptotic giant branch (AGB) star. In this paper, we analyze a new and long observation with the reflection grating spectrometers (RGS) on board the XMM-Newton satellite, spatially resolving the remnant emission in the cross-dispersion direction. We find that the CSM component is blue-shifted with velocities in the general range 0-500 km/s. We also derive information on the central bar structure and find that the northwest half is blue-shifted, while the southeast half is red-shifted. Our result is consistent with a picture proposed by previous studies, in which a "runaway" AGB star moved to the north-northwest and toward us in the line of sight, although it is acceptable for both single-degenerate and core-degenerate scenarios for the progenitor system., Comment: 19 pages, 5 figures, accepted for publication in ApJ
Published: 2021
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46. Cepheids with Giant Companions. I. Revealing a Numerous Population of Double-lined Binary Cepheids* †

Author: W. Narloch, Jesper Storm, Bogumił Pilecki, Richard I. Anderson, Grzegorz Pietrzyński, Nancy Remage Evans, Mónica Taormina, and Wolfgang Gieren
Subjects: Physics, education.field_of_study, 010504 meteorology & atmospheric sciences, Cepheid variable, Milky Way, Population, Binary number, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, 01 natural sciences, Galaxy, Stars, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, Stellar physics, 0103 physical sciences, education, 010303 astronomy & astrophysics, Solar and Stellar Astrophysics (astro-ph.SR), 0105 earth and related environmental sciences
Abstract: Masses of classical Cepheids of 3 to 11 M$\odot$ are predicted by theory but those measured, clump between 3.6 and 5 M$\odot$. As a result, their mass-luminosity relation is poorly constrained, impeding our understanding of basic stellar physics and the Leavitt Law. All Cepheid masses come from the analysis of 11 binary systems, including only 5 double-lined and well-suited for accurate dynamical mass determination. We present a project to analyze a new, numerous group of Cepheids in double-lined binary (SB2) systems to provide mass determinations in a wide mass interval and study their evolution. We analyze a sample of 41 candidate binary LMC Cepheids spread along the P-L relation, that are likely accompanied by luminous red giants, and present indirect and direct indicators of their binarity. In a spectroscopic study of a subsample of 18 brightest candidates, for 16 we detected lines of two components in the spectra, already quadrupling the number of Cepheids in SB2 systems. Observations of the whole sample may thus lead to quadrupling all the Cepheid mass estimates available now. For the majority of our candidates, erratic intrinsic period changes dominate over the light travel-time effect due to binarity. However, the latter may explain the periodic phase modulation for 4 Cepheids. Our project paves the way for future accurate dynamical mass determinations of Cepheids in the LMC, Milky Way, and other galaxies, which will potentially increase the number of known Cepheid masses even 10-fold, hugely improving our knowledge about these important stars., 12 pages, 7 figures, 3 tables, accepted for publication in ApJ
Published: 2021
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47. Interaction of Large- and Small-scale Dynamos in Isotropic Turbulent Flows from GPU-accelerated Simulations

Author: Ruben Krasnopolsky, Matthias Rheinhardt, Hsien Shang, Johannes Pekkilä, Miikka S. Väisälä, Maarit J. Käpylä, Academia Sinica, Professorship Korpi-Lagg Maarit, Department of Computer Science, Aalto-yliopisto, and Aalto University
Subjects: FOS: Physical sciences, Probability density function, 010103 numerical & computational mathematics, 01 natural sciences, symbols.namesake, 0103 physical sciences, Magnetic Prandtl number, 0101 mathematics, Scaling, Solar and Stellar Astrophysics (astro-ph.SR), Physics, 010308 nuclear & particles physics, Turbulence, Isotropy, Fluid Dynamics (physics.flu-dyn), Reynolds number, Astronomy and Astrophysics, Physics - Fluid Dynamics, Computational Physics (physics.comp-ph), Computational physics, Astrophysics - Solar and Stellar Astrophysics, Space and Planetary Science, symbols, Magnetohydrodynamics, Physics - Computational Physics, Dynamo
Abstract: Magnetohydrodynamical (MHD) dynamos emerge in many different astrophysical situations where turbulence is present, but the interaction between large-scale (LSD) and small-scale dynamos (SSD) is not fully understood. We performed a systematic study of turbulent dynamos driven by isotropic forcing in isothermal MHD with magnetic Prandtl number of unity, focusing on the exponential growth stage. Both helical and non-helical forcing was employed to separate the effects of LSD and SSD in a periodic domain. Reynolds numbers (Rm) up to $\approx 250$ were examined and multiple resolutions used for convergence checks. We ran our simulations with the Astaroth code, designed to accelerate 3D stencil computations on graphics processing units (GPUs) and to employ multiple GPUs with peer-to-peer communication. We observed a speedup of $\approx 35$ in single-node performance compared to the widely used multi-CPU MHD solver Pencil Code. We estimated the growth rates both from the averaged magnetic fields and their power spectra. At low Rm, LSD growth dominates, but at high Rm SSD appears to dominate in both helically and non-helically forced cases. Pure SSD growth rates follow a logarithmic scaling as a function of Rm. Probability density functions of the magnetic field from the growth stage exhibit SSD behaviour in helically forced cases even at intermediate Rm. We estimated mean-field turbulence transport coefficients using closures like the second-order correlation approximation (SOCA). They yield growth rates similar to the directly measured ones and provide evidence of $\alpha$ quenching. Our results are consistent with the SSD inhibiting the growth of the LSD at moderate Rm, while the dynamo growth is enhanced at higher Rm., Comment: 22 pages, 23 figures, 2 tables, Accepted for publication in the Astrophysical Journal
Published: 2021
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48. GASP XXXII. Measuring the diffuse ionized gas fraction in ram-pressure stripped galaxies

Author: Jacopo Fritz, Ariel Werle, Callum Bellhouse, Matilde Mingozzi, Neven Tomičić, Bianca M. Poggianti, Andrea Franchetto, Marco Gullieuszik, Daniela Bettoni, Benedetta Vulcani, and Alessia Moretti
Subjects: Physics, 010504 meteorology & atmospheric sciences, Stellar population, Stellar mass, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Condensed Matter::Mesoscopic Systems and Quantum Hall Effect, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Ram pressure, Space and Planetary Science, Galaxy group, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Surface brightness, 010303 astronomy & astrophysics, Equivalent width, Galaxy cluster, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences
Abstract: The diffuse ionized gas (DIG) is an important component of the interstellar medium and it can be affected by many physical processes in galaxies. Measuring its distribution and contribution in emission allows us to properly study both its ionization and star formation in galaxies. Here, we measure for the first time the DIG emission in 38 gas-stripped galaxies in local clusters drawn from the GAs Stripping Phenomena in galaxies with MUSE survey (GASP). These galaxies are at different stages of stripping. We also compare the DIG properties to those of 33 normal galaxies from the same survey. To estimate the DIG fraction (C$_{DIG}$) and derive its maps, we combine attenuation corrected H$\alpha$ surface brightness with $\rm [SII]/H\alpha$ line ratio. Our results indicate that we cannot use neither a single H$\alpha$ or $\rm [SII]/H\alpha$ value, nor a threshold in equivalent width of H$\alpha$ emission line to separate spaxels dominated by DIG and non-DIG emission. Assuming a constant surface brightness of the DIG across galaxies underestimates C$_{DIG}$. Contrasting stripped and non-stripped galaxies, we find no clear differences in C$_{DIG}$. The DIG emission contributes between 20\% and 90\% of the total integrated flux, and does not correlate with the galactic stellar mass and star-formation rate (SFR). The C$_{DIG}$ anti-correlates with the specific SFR, which may indicate an older ($>10^8$ yr) stellar population as ionizing source of the DIG. The DIG fraction shows anti-correlations with the SFR surface density, which could be used for a robust estimation of integrated C$_{DIG}$ in galaxies., Comment: This article is currently in press for the ApJ. 28 pages of which the main text is 21 pages, 17 figures of which 11 are in the main text, 2 tables, Appendix on the end (with 6 figures)
Published: 2021
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49. 3D Convection-resolving Model of Temperate, Tidally Locked Exoplanets

Author: Martin Turbet, Maxence Lefèvre, and Raymond T. Pierrehumbert
Subjects: Convection, Physics, Earth and Planetary Astrophysics (astro-ph.EP), 010504 meteorology & atmospheric sciences, Cloud cover, FOS: Physical sciences, Astronomy and Astrophysics, Atmospheric sciences, 01 natural sciences, Exoplanet, Tidal locking, Physics::Geophysics, 13. Climate action, Space and Planetary Science, Planet, 0103 physical sciences, Cloud albedo, Radiative transfer, Climate model, Astrophysics::Earth and Planetary Astrophysics, 010303 astronomy & astrophysics, Physics::Atmospheric and Oceanic Physics, 0105 earth and related environmental sciences, Astrophysics - Earth and Planetary Astrophysics
Abstract: A large fraction of known terrestrial-size exoplanets located in the Habitable Zone of M-dwarfs are expected to be tidally-locked. Numerous efforts have been conducted to study the climate of such planets, using in particular 3-D Global Climate Models (GCM). One of the biggest challenges in simulating such an extreme environment is to properly represent the effects of sub-grid convection. Most GCMs use either a simplistic convective-adjustment parametrization or sophisticated (e.g., mass flux scheme) Earth-tuned parametrizations. One way to improve the representation of convection is to study convection using Convection Resolving numerical Models (CRMs), with an fine spatial resolution . In this study, we developed a CRM coupling the non-hydrostatic dynamical core WRF with the radiative transfer and cloud/precipitation models of the LMD-Generic climate model to study convection and clouds on tidally-locked planets, with a focus on Proxima b. Simulations were performed for a set of 3 surface temperatures (corresponding to three different incident fluxes) and 2 rotation rates, assuming an Earth-like atmosphere. The main result of our study is that while we recover the prediction of GCMs that (low-altitude) cloud albedo increases with increasing stellar flux, the cloud feedback is much weaker due to transient aggregation of convection leading to low partial cloud cover., Accepted for publications in The Astrophysical Journal. 42 pages, 14 figures, 1 table
Published: 2021
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50. Inspecting the Cepheid Distance Ladder: the Hubble Space Telescope Distance to the SN Ia Host Galaxy NGC 5584

Author: V. Hocdé, Pierre Kervella, Behnam Javanmardi, L. Breuval, Nicolas Nardetto, Antoine Mérand, Grzegorz Pietrzyński, Wolfgang Gieren, Alexandre Gallenne, Simon Borgniet, Laboratoire Energie Signal Images et Automatique [Univ Ngaoundéré] (LESIA), Université de Ngaoundéré/University of Ngaoundéré [Cameroun] (UN), Laboratoire d'études spatiales et d'instrumentation en astrophysique (LESIA (UMR_8109)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)
Subjects: Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010504 meteorology & atmospheric sciences, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Cepheid variable, Milky Way, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Observational cosmology, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, Cosmic distance ladder, Astronomy and Astrophysics, Light curve, Astrophysics - Astrophysics of Galaxies, Galaxy, Distance modulus, Supernova, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: The current tension between the direct and the early Universe measurements of the Hubble Constant, $H_0$, requires detailed scrutiny of all the data and methods used in the studies on both sides of the debate. The Cepheids in the type Ia supernova (SNIa) host galaxy NGC 5584 played a key role in the local measurement of $H_0$. The SH0ES project used the observations of this galaxy to derive a relation between Cepheids' periods and ratios of their amplitudes in different optical bands of the Hubble Space Telescope (HST), and used these relations to analyse the light curves of the Cepheids in around half of the current sample of local SNIa host galaxies. In this work, we present an independent detailed analysis of the Cepheids in NGC 5584. We employ different tools for our photometric analysis and a completely different method for our light curve analysis, and we do not find a systematic difference between our period and mean magnitude measurements compared to those reported by SH0ES. By adopting a period-luminosity relation calibrated by the Cepheids in the Milky Way, we measure a distance modulus $\mu=31.810\pm0.047$ (mag) which is in agreement with $\mu=31.786\pm0.046$ (mag) measured by SH0ES. In addition, the relations we find between periods and amplitude ratios of the Cepheids in NGC 5584 are significantly tighter than those of SH0ES and their potential impact on the direct $H_0$ measurement will be investigated in future studies., Comment: Accepted for publication in The Astrophysical Journal on 17-Feb-2021
Published: 2021
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