Details

Autor(en) / Beteiligte

• Jiménez-Rosales, A.
• Dexter, J.
• Widmann, F.
• Bauböck, M.
• Abuter, R.
• Amorim, A.
• Berger, J. P.
• Bonnet, H.
• Brandner, W.
• Clénet, Y.
• de Zeeuw, P. T.
• Eckart, A.
• Eisenhauer, F.
• Förster Schreiber, N. M.
• Garcia, P.
• Gao, F.
• Gendron, E.
• Genzel, R.
• Gillessen, S.
• Habibi, M.
• Haubois, X.
• Heißel, G.
• Henning, T.
• Hippler, S.
• Horrobin, M.
• Jochum, L.
• Jocou, L.
• Kaufer, A.
• Kervella, P.
• Lacour, S.
• Lapeyrère, V.
• Le Bouquin, J.-B.
• Léna, P.
• Nowak, M.
• Ott, T.
• Paumard, T.
• Perraut, K.
• Perrin, G.
• Pfuhl, O.
• Rodríguez-Coira, G.
• Shangguan, J.
• Scheithauer, S.
• Stadler, J.
• Straub, O.
• Straubmeier, C.
• Sturm, E.
• Tacconi, L. J.
• Vincent, F.
• von Fellenberg, S.
• Waisberg, I.
• Wieprecht, E.
• Wiezorrek, E.
• Woillez, J.
• Yazici, S.
• Zins, G.

Titel

Dynamically important magnetic fields near the event horizon of Sgr A

Ist Teil von

• Astronomy and astrophysics (Berlin), 2020-11, Vol.643, p.A56

Ort / Verlag

Heidelberg: EDP Sciences

Erscheinungsjahr

2020

Quelle

EZB Electronic Journals Library

Beschreibungen/Notizen

• We study the time-variable linear polarisation of Sgr A* during a bright near-infrared flare observed with the GRAVITY instrument on July 28, 2018. Motivated by the time evolution of both the observed astrometric and polarimetric signatures, we interpret the data in terms of the polarised emission of a compact region (“hotspot”) orbiting a black hole in a fixed, background magnetic field geometry. We calculated a grid of general relativistic ray-tracing models, created mock observations by simulating the instrumental response, and compared predicted polarimetric quantities directly to the measurements. We take into account an improved instrument calibration that now includes the instrument’s response as a function of time, and we explore a variety of idealised magnetic field configurations. We find that the linear polarisation angle rotates during the flare, which is consistent with previous results. The hotspot model can explain the observed evolution of the linear polarisation. In order to match the astrometric period of this flare, the near horizon magnetic field is required to have a significant poloidal component, which is associated with strong and dynamically important fields. The observed linear polarisation fraction of ≃30% is smaller than the one predicted by our model (≃50%). The emission is likely beam depolarised, indicating that the flaring emission region resolves the magnetic field structure close to the black hole.