J 2024

Ordered magnetic fields around the 3C 84 central black hole

PARASCHOS, G. F., J-Y KIM, Maciek WIELGUS, J. ROEDER, T. P. KRICHBAUM et. al.

Základní údaje

Originální název

Ordered magnetic fields around the 3C 84 central black hole

Autoři

PARASCHOS, G. F., J-Y KIM, Maciek WIELGUS (616 Polsko, domácí), J. ROEDER, T. P. KRICHBAUM, E. ROS, I. AGUDO, I. MYSERLIS, M. MOSCIBRODZKA, E. TRAIANOU, J. A. ZENSUS, L. BLACKBURN, C-K CHAN, S. ISSAOUN, M. JANSSEN, M. D. JOHNSON, V. L. FISH, K. AKIYAMA, A. ALBERDI, W. ALEF, J. C. ALGABA, R. ANANTUA, K. ASADA, R. AZULAY, U. BACH, A-K BACZKO, D. BALL, M. BALOKOVIC, J. BARRETT, M. BAUBOCK, B. A. BENSON, D. BINTLEY, R. BLUNDELL, K. L. BOUMAN, G. C. BOWER, H. BOYCE, M. BREMER, C. D. BRINKERINK, R. BRISSENDEN, S. BRITZEN, A. E. BRODERICK, D. BROGUIERE, T. BRONZWAER, S. BUSTAMANTE, D-Y BYUN, J. E. CARLSTROM, C. CECCOBELLO, A. CHAEL, D. O. CHANG, K. CHATTERJEE, S. CHATTERJEE, M. T. CHEN, Y. CHEN, X. CHENG, I. CHO, P. CHRISTIAN, N. S. CONROY, J. E. CONWAY, J. M. CORDES, T. M. CRAWFORD, G. B. CREW, A. CRUZ-OSORIO, Y. CUI, R. DAHALE, J. DAVELAAR, M. DE LAURENTIS, R. DEANE, J. DEMPSEY, G. DESVIGNES, J. DEXTER, V. DHRUV, S. S. DOELEMAN, S. DOUGAL, S. A. DZIB, R. P. EATOUGH, R. EMAMI, H. FALCKE, J. FARAH, E. FOMALONT, H. A. FORD, M. FOSCHI, R. FRAGA-ENCINAS, W. T. FREEMAN, P. FRIBERG, C. M. FROMM, A. FUENTES, P. GALISON, C. F. GAMMIE, R. GARCIA, O. GENTAZ, B. GEORGIEV, C. GODDI, R. GOLD, A. I. GOMEZ-RUIZ, J. L. GOMEZ, M. GU, M. GURWELL, K. HADA, D. HAGGARD, K. HAWORTH, M. H. HECHT, R. HESPER, D. HEUMANN, L. C. HO, P. HO, M. HONMA, C. L. HUANG, L. HUANG, D. H. HUGHES, S. IKEDA, C. M. V. IMPELLIZZERI, M. INOUE, D. J. JAMES, B. T. JANNUZI, B. JETER, W. JAING, A. JIMENEZ-ROSALES, S. JORSTAD, A. V. JOSHI, T. JUNG, M. KARAMI, R. KARUPPUSAMY, T. KAWASHIMA, G. K. KEATING, M. KETTENIS, D-J KIM, J. KIM, J. KIM, M. KINO, J. Y. KOAY, P. KOCHERLAKOTA, Y. KOFUJI, P. M. KOCH, S. KOYAMA, C. KRAMER, J. A. KRAMER, M. KRAMER, C-Y KUO, N. LA BELLA, T. R. LAUER, D. LEE, S-S LEE, P. K. LEUNG, A. LEVIS, Z. LI, R. LICO, G. LINDAHL, M. LINDQVIST, M. LISAKOV, J. LIU, K. LIU, E. LIUZZO, W-P LO, A. P. LOBANOV, L. LOINARD, C. J. LONSDALE, A. E. LOWITZ, R-S LU, N. R. MACDONALD, J. MAO, N. MARCHILI, S. MARKOFF, D. P. MARRONE, A. P. MARSCHER, I. MARTI-VIDAL, S. MATSUSHITA, L. D. MATTHEWS, L. MEDEIROS, K. M. MENTEN, D. MICHALIK, I.. MIZUNO, Y. MIZUNO, J. M. MORAN, K. MORIYAMA, W. MULAUDZI, C. MUELLER, H. MUELLER, A. MUS, G. MUSOKE, A. NADOLSKI, H. NAGAI, N. M. NAGAR, M. NAKAMURA, G. NARAYANAN, I. NATARAJAN, A. NATHANAIL, S. NAVARRO FUENTES, J. NEILSEN, R. NERI, C. NI, A. NOUTSOS, M. A. NOWAK, J. OH, H. OKINO, H. OLIVARES, G. N. ORTIZ-LEON, T. OYAMA, F. OZEL, D. C. M. PALUMBO, J. PARK, H. PARSONS, N. PATEL, U-L PEN, V. PIETU, R. PLAMBECK, A. POPSTEFANIJA, O. PORTH, F. M. POTZL, B. PRATHER, J. A. PRECIADO-LOPEZ, D. PSALTIS, H-Y PU, V. RAMAKRISHNAN, R.. RAO, M. G. RAWLINGS, A. W. RAYMOND, L. REZZOLLA, A. RICARTE, B. RIPPERDA, F. ROELOFS, A. ROGERS, C. ROMERO-CANIZALES, A. ROSHANINESHAT, H. ROTTMANN, A. L. ROY, I. RUIZ, C. RUSZCZYK, K. L. J. RYGL, S. SANCHEZ, D. SANCHEZ-ARGUELLES, M. SANCHEZ-PORTAL, M. SASADA, K. SATAPATHY, T. SAVOLAINEN, F. P. SCHLOERB, J. SCHONFELD, K. SCHUSTER, L. SHAO, Z. SHEN, D. SMALL, B. W. SOHN, J. SOOHOO, L. D. Sosapanta SALAS, K. SOUCCAR, H. SUN, F. TAZAKI, A. J. TETARENKO, P. TIEDE, R. P. J. TILANUS, M. TITUS, P. TORNE, T. TOSCANO, T. TRENT, S. TRIPPE, M. TURK, I. VAN BEMMEL, J. H. VAN LANGEVELDE, R. D. VAN ROSSUM, J. VOS, J. WAGNER, D. WARD-THOMPSON, J. WARDLE, J. E. WASHINGTON, J. WEINTROUB, R. WHARTON, K. WIIK, G. WITZEL, M. F. WONDRAK, G. N. WONG, Q. WU, N. YADLAPALLI, P. YAMAGUCHI, A. YFANTIS, D. YOON, A. YOUNG, K. YOUNG, Z. YOUNSI, W. YU, F. YUAN, Y-F YUAN, S. ZHANG, G. Y. ZHAO a S-S ZHAO

Vydání

ASTRONOMY & ASTROPHYSICS, LES ULIS CEDEX A, EDP SCIENCES S A, 2024, 0004-6361

Další údaje

Jazyk

angličtina

Typ výsledku

Článek v odborném periodiku

Obor

10308 Astronomy

Stát vydavatele

Francie

Utajení

není předmětem státního či obchodního tajemství

Odkazy

Impakt faktor

Impact factor: 6.500 v roce 2022

Organizační jednotka

Fyzikální ústav v Opavě

UT WoS

001187956400001

Klíčová slova anglicky

techniques: high angular resolution;techniques: interferometric;galaxies: active;galaxies: individual: NGC 1275;galaxies: jets

Štítky

Příznaky

Mezinárodní význam, Recenzováno
Změněno: 5. 2. 2025 13:24, Mgr. Pavlína Jalůvková

Anotace

V originále

Context. 3C 84 is a nearby radio source with a complex total intensity structure, showing linear polarisation and spectral patterns. A detailed investigation of the central engine region necessitates the use of very-long-baseline interferometry (VLBI) above the hitherto available maximum frequency of 86 GHz. Aims. Using ultrahigh resolution VLBI observations at the currently highest available frequency of 228 GHz, we aim to perform a direct detection of compact structures and understand the physical conditions in the compact region of 3C 84. Methods. We used Event Horizon Telescope (EHT) 228 GHz observations and, given the limited (u; v)-coverage, applied geometric model fitting to the data. Furthermore, we employed quasi-simultaneously observed, ancillary multi-frequency VLBI data for the source in order to carry out a comprehensive analysis of the core structure. Results. We report the detection of a highly ordered, strong magnetic field around the central, supermassive black hole of 3C 84. The brightness temperature analysis suggests that the system is in equipartition. We also determined a turnover frequency of gamma(m) = (113 +/- 4) GHz, a corresponding synchrotron self-absorbed magnetic field of B-SSA = (2.9 +/- 1.6) G, and an equipartition magnetic field of B-eq = (5.2 +/- 0.6) G. Three components are resolved with the highest fractional polarisation detected for this object (m(net) = (17.0 +/- 3.9)%). The positions of the components are compatible with those seen in low-frequency VLBI observations since 2017-2018. We report a steeply negative slope of the spectrum at 228 GHz. We used these findings to test existing models of jet formation, propagation, and Faraday rotation in 3C 84. Conclusions. The findings of our investigation into di fferent flow geometries and black hole spins support an advection-dominated accretion flow in a magnetically arrested state around a rapidly rotating supermassive black hole as a model of the jet-launching system in the core of 3C 84. However, systematic uncertainties due to the limited (u, v)-coverage, however, cannot be ignored. Our upcoming work using new EHT data, which o ffer full imaging capabilities, will shed more light on the compact region of 3C 84.