TY - JOUR

T1 - The Variability of the Black Hole Image in M87 at the Dynamical Timescale

AU - Satapathy, Kaushik

AU - Psaltis, Dimitrios

AU - Özel, Feryal

AU - Medeiros, Lia

AU - Dougall, Sean T.

AU - Chan, Chi-Kwan

AU - Wielgus, Maciek

AU - Prather, Ben S.

AU - Wong, George N.

AU - Gammie, Charles F.

AU - Akiyama, Kazunori

AU - Alberdi, Antxon

AU - Alef, Walter

AU - Algaba, Juan Carlos

AU - Anantua, Richard

AU - Asada, Keiichi

AU - Azulay, Rebecca

AU - Baczko, Anne-Kathrin

AU - Ball, David

AU - Baloković, Mislav

AU - Barrett, John

AU - Benson, Bradford A.

AU - Bintley, Dan

AU - Blackburn, Lindy

AU - Blundell, Raymond

AU - Boland, Wilfred

AU - Bouman, Katherine L.

AU - Bower, Geoffrey C.

AU - Boyce, Hope

AU - Bremer, Michael

AU - Brinkerink, Christiaan D.

AU - Brissenden, Roger

AU - Britzen, Silke

AU - Broderick, Avery E.

AU - Broguiere, Dominique

AU - Bronzwaer, Thomas

AU - Bustamente, Sandra

AU - Byun, Do-Young

AU - Carlstrom, John E.

AU - Chael, Andrew

AU - Chatterjee, Koushik

AU - Chatterjee, Shami

AU - Chen, Ming-Tang

AU - Chen, Yongjun

AU - Cho, Ilje

AU - Christian, Pierre

AU - Conway, John E.

AU - Cordes, James M.

AU - Crawford, Thomas M.

AU - Crew, Geoffrey B.

AU - Cruz-Osorio, Alejandro

AU - Cui, Yuzhu

AU - Davelaar, Jordy

AU - De Laurentis, Mariafelicia

AU - Deane, Roger

AU - Dempsey, Jessica

AU - Desvignes, Gregory

AU - Dexter, Jason

AU - Doeleman, Sheperd S.

AU - Eatough, Ralph P.

AU - Falcke, Heino

AU - Farah, Joseph

AU - Fish, Vincent L.

AU - Fomalont, Ed

AU - Ford, H. Alyson

AU - Fraga-Encinas, Raquel

AU - Friberg, Per

AU - Fromm, Christian M.

AU - Fuentes, Antonio

AU - Galison, Peter

AU - García, Roberto

AU - Gentaz, Olivier

AU - Georgiev, Boris

AU - Goddi, Ciriaco

AU - Gold, Roman

AU - Gómez-Ruiz, Arturo I.

AU - Gómez, José L.

AU - Gu, Minfeng

AU - Gurwell, Mark

AU - Hada, Kazuhiro

AU - Haggard, Daryl

AU - Hecht, Michael H.

AU - Hesper, Ronald

AU - Ho, Luis C.

AU - Ho, Paul

AU - Honma, Mareki

AU - Huang, Chih-Wei L.

AU - Huang, Lei

AU - Hughes, David H.

AU - Ikeda, Shiro

AU - Inoue, Makoto

AU - Issaoun, Sara

AU - James, David J.

AU - Jannuzi, Buell T.

AU - Janssen, Michael

AU - Jeter, Britton

AU - Jiang, Wu

AU - Jimenez-Rosales, Alejandra

AU - Johnson, Michael D.

AU - Jorstad, Svetlana

AU - Jung, Taehyun

AU - Karami, Mansour

AU - Karuppusamy, Ramesh

AU - Kawashima, Tomohisa

AU - Keating, Garrett K.

AU - Kettenis, Mark

AU - Kim, Dong-Jin

AU - Kim, Jae-Young

AU - Kim, Jongsoo

AU - Kim, Junhan

AU - Kino, Motoki

AU - Koay, Jun Yi

AU - Kofuji, Yutaro

AU - Koch, Patrick M.

AU - Koyama, Shoko

AU - Kramer, Carsten

AU - Kramer, Michael

AU - Krichbaum, Thomas P.

AU - Kuo, Cheng-Yu

AU - Lauer, Tod R.

AU - Lee, Sang-Sung

AU - Levis, Aviad

AU - Li, Yan-Rong

AU - Li, Zhiyuan

AU - Lindqvist, Michael

AU - Lico, Rocco

AU - Lindahl, Greg

AU - Liu, Jun

AU - Liu, Kuo

AU - Liuzzo, Elisabetta

AU - Lo, Wen-Ping

AU - Lobanov, Andrei P.

AU - Loinard, Laurent

AU - Lonsdale, Colin

AU - Lu, Ru-Sen

AU - MacDonald, Nicholas R.

AU - Mao, Jirong

AU - Marchili, Nicola

AU - Markoff, Sera

AU - Marrone, Daniel P.

AU - Marscher, Alan P.

AU - Martí-Vidal, Iván

AU - Matsushita, Satoki

AU - Matthews, Lynn D.

AU - Menten, Karl M.

AU - Mizuno, Izumi

AU - Mizuno, Yosuke

AU - Moran, James M.

AU - Moriyama, Kotaro

AU - Moscibrodzka, Monika

AU - Müller, Cornelia

AU - Mejías, Alejandro Mus

AU - Musoke, Gibwa

AU - Nagai, Hiroshi

AU - Nagar, Neil M.

AU - Nakamura, Masanori

AU - Narayan, Ramesh

AU - Narayanan, Gopal

AU - Natarajan, Iniyan

AU - Nathanail, Antonios

AU - Neilsen, Joey

AU - Neri, Roberto

AU - Ni, Chunchong

AU - Noutsos, Aristeidis

AU - Nowak, Michael A.

AU - Okino, Hiroki

AU - Olivares, Héctor

AU - Ortiz-León, Gisela N.

AU - Oyama, Tomoaki

AU - Palumbo, Daniel C. M.

AU - Park, Jongho

AU - Patel, Nimesh

AU - Pen, Ue-Li

AU - Pesce, Dominic W.

AU - Piétu, Vincent

AU - Plambeck, Richard

AU - PopStefanija, Aleksandar

AU - Porth, Oliver

AU - Pötzl, Felix M.

AU - Preciado-López, Jorge A.

AU - Pu, Hung-Yi

AU - Ramakrishnan, Venkatessh

AU - Rao, Ramprasad

AU - Rawlings, Mark G.

AU - Raymond, Alexander W.

AU - Rezzolla, Luciano

AU - Ripperda, Bart

AU - Roelofs, Freek

AU - Rogers, Alan

AU - Ros, Eduardo

AU - Rose, Mel

AU - Roshanineshat, Arash

AU - Rottmann, Helge

AU - Roy, Alan L.

AU - Ruszczyk, Chet

AU - Rygl, Kazi L. J.

AU - Sánchez, Salvador

AU - Sánchez-Arguelles, David

AU - Sasada, Mahito

AU - Savolainen, Tuomas

AU - Schloerb, F. Peter

AU - Schuster, Karl-Friedrich

AU - Shao, Lijing

AU - Shen, Zhiqiang

AU - Small, Des

AU - Sohn, Bong Won

AU - SooHoo, Jason

AU - Sun, He

AU - Tazaki, Fumie

AU - Tetarenko, Alexandra J.

AU - Tiede, Paul

AU - Tilanus, Remo P. J.

AU - Titus, Michael

AU - Toma, Kenji

AU - Torne, Pablo

AU - Traianou, Efthalia

AU - Trent, Tyler

AU - Trippe, Sascha

AU - van Bemmel, Ilse

AU - van Langevelde, Huib Jan

AU - van Rossum, Daniel R.

AU - Wagner, Jan

AU - Ward-Thompson, Derek

AU - Wardle, John

AU - Weintroub, Jonathan

AU - Wex, Norbert

AU - Wharton, Robert

AU - Wiik, Kaj

AU - Wu, Qingwen

AU - Yoon, Doosoo

AU - Young, André

AU - Young, Ken

AU - Younsi, Ziri

AU - Yuan, Feng

AU - Yuan, Ye-Fei

AU - Zensus, J. Anton

AU - Zhao, Guang-Yao

AU - Zhao, Shan-Shan

PY - 2022

Y1 - 2022

N2 - The black hole images obtained with the Event Horizon Telescope (EHT) are expected to be variable at the dynamical timescale near their horizons. For the black hole at the center of the M87 galaxy, this timescale (5–61 days) is comparable to the 6 day extent of the 2017 EHT observations. Closure phases along baseline triangles are robust interferometric observables that are sensitive to the expected structural changes of the images but are free of station-based atmospheric and instrumental errors. We explored the day-to-day variability in closure-phase measurements on all six linearly independent nontrivial baseline triangles that can be formed from the 2017 observations. We showed that three triangles exhibit very low day-to-day variability, with a dispersion of ∼3°–5°. The only triangles that exhibit substantially higher variability (∼90°–180°) are the ones with baselines that cross the visibility amplitude minima on the u–v plane, as expected from theoretical modeling. We used two sets of general relativistic magnetohydrodynamic simulations to explore the dependence of the predicted variability on various black hole and accretion-flow parameters. We found that changing the magnetic field configuration, electron temperature model, or black hole spin has a marginal effect on the model consistency with the observed level of variability. On the other hand, the most discriminating image characteristic of models is the fractional width of the bright ring of emission. Models that best reproduce the observed small level of variability are characterized by thin ring-like images with structures dominated by gravitational lensing effects and thus least affected by turbulence in the accreting plasmas.

AB - The black hole images obtained with the Event Horizon Telescope (EHT) are expected to be variable at the dynamical timescale near their horizons. For the black hole at the center of the M87 galaxy, this timescale (5–61 days) is comparable to the 6 day extent of the 2017 EHT observations. Closure phases along baseline triangles are robust interferometric observables that are sensitive to the expected structural changes of the images but are free of station-based atmospheric and instrumental errors. We explored the day-to-day variability in closure-phase measurements on all six linearly independent nontrivial baseline triangles that can be formed from the 2017 observations. We showed that three triangles exhibit very low day-to-day variability, with a dispersion of ∼3°–5°. The only triangles that exhibit substantially higher variability (∼90°–180°) are the ones with baselines that cross the visibility amplitude minima on the u–v plane, as expected from theoretical modeling. We used two sets of general relativistic magnetohydrodynamic simulations to explore the dependence of the predicted variability on various black hole and accretion-flow parameters. We found that changing the magnetic field configuration, electron temperature model, or black hole spin has a marginal effect on the model consistency with the observed level of variability. On the other hand, the most discriminating image characteristic of models is the fractional width of the bright ring of emission. Models that best reproduce the observed small level of variability are characterized by thin ring-like images with structures dominated by gravitational lensing effects and thus least affected by turbulence in the accreting plasmas.

U2 - 10.3847/1538-4357/ac332e

DO - 10.3847/1538-4357/ac332e

M3 - статья

VL - 925

JO - Astrophysical Journal

JF - Astrophysical Journal

SN - 0004-637X

IS - 1

ER -