Attenzione: i dati modificati non sono ancora stati salvati. Per confermare inserimenti o cancellazioni di voci è necessario confermare con il tasto SALVA/INSERISCI in fondo alla pagina
UNICA IRIS Institutional Research Information System
In a companion paper, we present the first spatially resolved polarized image of Sagittarius A* on event horizon scales, captured using the Event Horizon Telescope, a global very long baseline interferometric array operating at a wavelength of 1.3 mm. Here we interpret this image using both simple analytic models and numerical general relativistic magnetohydrodynamic (GRMHD) simulations. The large spatially resolved linear polarization fraction (24%-28%, peaking at similar to 40%) is the most stringent constraint on parameter space, disfavoring models that are too Faraday depolarized. Similar to our studies of M87*, polarimetric constraints reinforce a preference for GRMHD models with dynamically important magnetic fields. Although the spiral morphology of the polarization pattern is known to constrain the spin and inclination angle, the time-variable rotation measure (RM) of Sgr A* (equivalent to approximate to 46 degrees +/- 12 degrees rotation at 228 GHz) limits its present utility as a constraint. If we attribute the RM to internal Faraday rotation, then the motion of accreting material is inferred to be counterclockwise, contrary to inferences based on historical polarized flares, and no model satisfies all polarimetric and total intensity constraints. On the other hand, if we attribute the mean RM to an external Faraday screen, then the motion of accreting material is inferred to be clockwise, and one model passes all applied total intensity and polarimetric constraints: a model with strong magnetic fields, a spin parameter of 0.94, and an inclination of 150 degrees. We discuss how future 345 GHz and dynamical imaging will mitigate our present uncertainties and provide additional constraints on the black hole and its accretion flow.
First Sagittarius A* Event Horizon Telescope Results. VIII. Physical Interpretation of the Polarized Ring
The Event Horizon Telescope Collaboration, null;Akiyama, Kazunori;Alberdi, Antxon;Alef, Walter;Algaba, Juan Carlos;Anantua, Richard;Asada, Keiichi;Azulay, Rebecca;Bach, Uwe;Baczko, Anne-Kathrin;Ball, David;Baloković, Mislav;Bandyopadhyay, Bidisha;Barrett, John;Bauböck, Michi;Benson, Bradford A.;Bintley, Dan;Blackburn, Lindy;Blundell, Raymond;Bouman, Katherine L.;Bower, Geoffrey C.;Boyce, Hope;Bremer, Michael;Brinkerink, Christiaan D.;Brissenden, Roger;Britzen, Silke;Broderick, Avery E.;Broguiere, Dominique;Bronzwaer, Thomas;Bustamante, Sandra;Byun, Do-Young;Carlstrom, John E.;Ceccobello, Chiara;Chael, Andrew;Chan, Chi-kwan;Chang, Dominic O.;Chatterjee, Koushik;Chatterjee, Shami;Chen, Ming-Tang;Chen 陈, Yongjun 永军;Cheng, Xiaopeng;Cho, Ilje;Christian, Pierre;Conroy, Nicholas S.;Conway, John E.;Cordes, James M.;Crawford, Thomas M.;Crew, Geoffrey B.;Cruz-Osorio, Alejandro;Cui 崔, Yuzhu 玉竹;Dahale, Rohan;Davelaar, Jordy;De Laurentis, Mariafelicia;Deane, Roger;Dempsey, Jessica;Desvignes, Gregory;Dexter, Jason;Dhruv, Vedant;Dihingia, Indu K.;Doeleman, Sheperd S.;Dougall, Sean;Dzib, Sergio A.;Eatough, Ralph P.;Emami, Razieh;Falcke, Heino;Farah, Joseph;Fish, Vincent L.;Fomalont, Edward;Ford, H. Alyson;Foschi, Marianna;Fraga-Encinas, Raquel;Freeman, William T.;Friberg, Per;Fromm, Christian M.;Fuentes, Antonio;Galison, Peter;Gammie, Charles F.;García, Roberto;Gentaz, Olivier;Georgiev, Boris;Goddi, Ciriaco;Gold, Roman;Gómez-Ruiz, Arturo I.;Gómez, José L.;Gu 顾, Minfeng 敏峰;Gurwell, Mark;Hada, Kazuhiro;Haggard, Daryl;Haworth, Kari;Hecht, Michael H.;Hesper, Ronald;Heumann, Dirk;Ho 何, Luis C. 子山;Ho, Paul;Honma, Mareki;Huang, Chih-Wei L.;Huang 黄, Lei 磊;Hughes, David H.;Ikeda, Shiro;Impellizzeri, C. M. Violette;Inoue, Makoto;Issaoun, Sara;James, David J.;Jannuzi, Buell T.;Janssen, Michael;Jeter, Britton;Jiang 江, Wu 悟;Jiménez-Rosales, Alejandra;Johnson, Michael D.;Jorstad, Svetlana;Joshi, Abhishek V.;Jung, Taehyun;Karami, Mansour;Karuppusamy, Ramesh;Kawashima, Tomohisa;Keating, Garrett K.;Kettenis, Mark;Kim, Dong-Jin;Kim, Jae-Young;Kim, Jongsoo;Kim, Junhan;Kino, Motoki;Koay, Jun Yi;Kocherlakota, Prashant;Kofuji, Yutaro;Koch, Patrick M.;Koyama, Shoko;Kramer, Carsten;Kramer, Joana A.;Kramer, Michael;Krichbaum, Thomas P.;Kuo, Cheng-Yu;La Bella, Noemi;Lauer, Tod R.;Lee, Daeyoung;Lee, Sang-Sung;Leung, Po Kin;Levis, Aviad;Li 李, Zhiyuan 志远;Lico, Rocco;Lindahl, Greg;Lindqvist, Michael;Lisakov, Mikhail;Liu 刘, Jun 俊;Liu, Kuo;Liuzzo, Elisabetta;Lo, Wen-Ping;Lobanov, Andrei P.;Loinard, Laurent;Lonsdale, Colin J.;Lowitz, Amy E.;Lu 路, Ru-Sen 如森;MacDonald, Nicholas R.;Mao 毛, Jirong 基荣;Marchili, Nicola;Markoff, Sera;Marrone, Daniel P.;Marscher, Alan P.;Martí-Vidal, Iván;Matsushita, Satoki;Matthews, Lynn D.;Medeiros, Lia;Menten, Karl M.;Michalik, Daniel;Mizuno, Izumi;Mizuno, Yosuke;Moran, James M.;Moriyama, Kotaro;Moscibrodzka, Monika;Mulaudzi, Wanga;Müller, Cornelia;Müller, Hendrik;Mus, Alejandro;Musoke, Gibwa;Myserlis, Ioannis;Nadolski, Andrew;Nagai, Hiroshi;Nagar, Neil M.;Nakamura, Masanori;Narayanan, Gopal;Natarajan, Iniyan;Nathanail, Antonios;Navarro Fuentes, Santiago;Neilsen, Joey;Neri, Roberto;Ni, Chunchong;Noutsos, Aristeidis;Nowak, Michael A.;Oh, Junghwan;Okino, Hiroki;Olivares, Héctor;Ortiz-León, Gisela N.;Oyama, Tomoaki;Özel, Feryal;Palumbo, Daniel C. M.;Paraschos, Georgios Filippos;Park, Jongho;Parsons, Harriet;Patel, Nimesh;Pen, Ue-Li;Pesce, Dominic W.;Piétu, Vincent;Plambeck, Richard;PopStefanija, Aleksandar;Porth, Oliver;Pötzl, Felix M.;Prather, Ben;Preciado-López, Jorge A.;Psaltis, Dimitrios;Pu, Hung-Yi;Ramakrishnan, Venkatessh;Rao, Ramprasad;Rawlings, Mark G.;Raymond, Alexander W.;Rezzolla, Luciano;Ricarte, Angelo;Ripperda, Bart;Roelofs, Freek;Rogers, Alan;Romero-Cañizales, Cristina;Ros, Eduardo;Roshanineshat, Arash;Rottmann, Helge;Roy, Alan L.;Ruiz, Ignacio;Ruszczyk, Chet;Rygl, Kazi L. J.;Sánchez, Salvador;Sánchez-Argüelles, David;Sánchez-Portal, Miguel;Sasada, Mahito;Satapathy, Kaushik;Savolainen, Tuomas;Schloerb, F. Peter;Schonfeld, Jonathan;Schuster, Karl-Friedrich;Shao, Lijing;Shen 沈, Zhiqiang 志强;Small, Des;Sohn, Bong Won;SooHoo, Jason;Sosapanta Salas, León David;Souccar, Kamal;Stanway, Joshua S.;Sun 孙, He 赫;Tazaki, Fumie;Tetarenko, Alexandra J.;Tiede, Paul;Tilanus, Remo P. J.;Titus, Michael;Torne, Pablo;Toscano, Teresa;Traianou, Efthalia;Trent, Tyler;Trippe, Sascha;Turk, Matthew;van Bemmel, Ilse;van Langevelde, Huib Jan;van Rossum, Daniel R.;Vos, Jesse;Wagner, Jan;Ward-Thompson, Derek;Wardle, John;Washington, Jasmin E.;Weintroub, Jonathan;Wharton, Robert;Wielgus, Maciek;Wiik, Kaj;Witzel, Gunther;Wondrak, Michael F.;Wong, George N.;Wu 吴, Qingwen 庆文;Yadlapalli, Nitika;Yamaguchi, Paul;Yfantis, Aristomenis;Yoon, Doosoo;Young, André;Young, Ken;Younsi, Ziri;Yu 于, Wei 威;Yuan 袁, Feng 峰;Yuan 袁, Ye-Fei 业飞;Zensus, J. Anton;Zhang, Shuo;Zhao, Guang-Yao;Zhao 赵, Shan-Shan 杉 杉;Najafi-Ziyazi, Mahdi
2024-01-01
Abstract
In a companion paper, we present the first spatially resolved polarized image of Sagittarius A* on event horizon scales, captured using the Event Horizon Telescope, a global very long baseline interferometric array operating at a wavelength of 1.3 mm. Here we interpret this image using both simple analytic models and numerical general relativistic magnetohydrodynamic (GRMHD) simulations. The large spatially resolved linear polarization fraction (24%-28%, peaking at similar to 40%) is the most stringent constraint on parameter space, disfavoring models that are too Faraday depolarized. Similar to our studies of M87*, polarimetric constraints reinforce a preference for GRMHD models with dynamically important magnetic fields. Although the spiral morphology of the polarization pattern is known to constrain the spin and inclination angle, the time-variable rotation measure (RM) of Sgr A* (equivalent to approximate to 46 degrees +/- 12 degrees rotation at 228 GHz) limits its present utility as a constraint. If we attribute the RM to internal Faraday rotation, then the motion of accreting material is inferred to be counterclockwise, contrary to inferences based on historical polarized flares, and no model satisfies all polarimetric and total intensity constraints. On the other hand, if we attribute the mean RM to an external Faraday screen, then the motion of accreting material is inferred to be clockwise, and one model passes all applied total intensity and polarimetric constraints: a model with strong magnetic fields, a spin parameter of 0.94, and an inclination of 150 degrees. We discuss how future 345 GHz and dynamical imaging will mitigate our present uncertainties and provide additional constraints on the black hole and its accretion flow.
I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11584/406604
Citazioni
ND
1
2
social impact
Conferma cancellazione
Sei sicuro che questo prodotto debba essere cancellato?
simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 589/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.