Constraining particle acceleration in Sgr A(*) with simultaneous GRAVITY, 
Spitzer, NuSTAR, and Chandra observations

Abuter, R.; Amorim, A.; Bauböck, M.; Bagano, F.; Berger, J. P.; Boyce, H.; Bonnet, H.; Brandner, W.; Clénet, Y.; Davies, R.; de Zeeuw, P. T.; Dexter, J.; Dallilar, Y.; Drescher, A.; Eckart, A.; Eisenhauer, F.; Fazio, G. G.; Förster Schreiber, N. M.; Foster, K.; Gammie, C.; Garcia, P.; Gao, F.; Gendron, E.; Genzel, R.; Ghisellini, G.; Gillessen, S.; Gurwell, M. A.; Habibi, M.; Haggard, D.; Hailey, C.; Harrison, F. A.; Haubois, X.; Heißel, G.; Henning, T.; Hippler, S.; Hora, J. L.; Horrobin, M.; Jiménez-Rosales, A.; Jochum, L.; Jocou, L.; Kaufer, A.; Kervella, P.; Lacour, S.; Lapeyrère, V.; Le Bouquin, J.-B.; Léna, P.; Lowrance, P. J.; Lutz, D.; Marko, S.; Mori, K.; Morris, M. R.; Neilsen, J.; Nowak, M.; Ott, T.; Paumard, T.; Perraut, K.; Perrin, G.; Ponti, G.; Pfuhl, O.; Rabien, S.; Rodríguez-Coira, G.; Shangguan, J.; Shimizu, T.; Scheithauer, S.; Smith, H. A.; Stadler, J.; Stern, D. K.; Straub, O.; Straubmeier, C.; Sturm, E.; Tacconi, L. J.; Vincent, F.; Fellenberg, S. D. von; Waisberg, I.; Widmann, F.; Wieprecht, E.; Wiezorrek, E.; Willner, S. P.; Witzel, G.; Woillez, J.; Yazici, S.; Young, A.; Zhang, S.; Zins, G.

doi:10.1051/0004-6361/202140981

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Constraining particle acceleration in Sgr A(*) with simultaneous GRAVITY, Spitzer, NuSTAR, and Chandra observations

MPG-Autoren

/persons/resource/persons216131

Bauböck, M.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons208361

Davies, R.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons225865

de Zeeuw, P. T.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons146381

Dexter, J.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons250315

Dallilar, Y.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4766

Eisenhauer, F.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4923

Förster Schreiber, N. M.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons214427

Gao, F.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4590

Genzel, R.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4768

Gillessen, S.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons181377

Habibi, M.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons216133

Jiménez-Rosales, A.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4584

Lutz, D.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons16190

Ott, T.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons82450

Ponti, G.
High Energy Astrophysics, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4782

Pfuhl, O.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4786

Rabien, S.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons232571

Shangguan, J.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons206401

Shimizu, T.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons248280

Stadler, J.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons232635

Straub, O.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4650

Sturm, E.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons4582

Tacconi, L. J.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons206120

Fellenberg, S. D. von
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons214431

Widmann, F.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons16329

Wieprecht, E.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons16335

Wiezorrek, E.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

/persons/resource/persons203013

Yazici, S.
Infrared and Submillimeter Astronomy, MPI for Extraterrestrial Physics, Max Planck Society;

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Zitation

Abuter, R., Amorim, A., Bauböck, M., Bagano, F., Berger, J. P., Boyce, H., et al. (2021). Constraining particle acceleration in Sgr A(*) with simultaneous GRAVITY, Spitzer, NuSTAR, and Chandra observations. Astronomy and Astrophysics, 654: A22. doi:10.1051/0004-6361/202140981.

Zitierlink: https://hdl.handle.net/21.11116/0000-0009-A041-8

Zusammenfassung

We report the time-resolved spectral analysis of a bright near-infrared and moderate X-ray flare of Sgr A^⋆. We obtained light curves in the M, K, and H bands in the mid- and near-infrared and in the 2 − 8 keV and 2 − 70 keV bands in the X-ray. The observed spectral slope in the near-infrared band is νL_ν ∝ ν^{0.5 ± 0.2}; the spectral slope observed in the X-ray band is νL_ν ∝ ν^{−0.7 ± 0.5}. Using a fast numerical implementation of a synchrotron sphere with a constant radius, magnetic field, and electron density (i.e., a one-zone model), we tested various synchrotron and synchrotron self-Compton scenarios. The observed near-infrared brightness and X-ray faintness, together with the observed spectral slopes, pose challenges for all models explored. We rule out a scenario in which the near-infrared emission is synchrotron emission and the X-ray emission is synchrotron self-Compton. Two realizations of the one-zone model can explain the observed flare and its temporal correlation: one-zone model in which the near-infrared and X-ray luminosity are produced by synchrotron self-Compton and a model in which the luminosity stems from a cooled synchrotron spectrum. Both models can describe the mean spectral energy distribution (SED) and temporal evolution similarly well. In order to describe the mean SED, both models require specific values of the maximum Lorentz factor γ_max, which differ by roughly two orders of magnitude. The synchrotron self-Compton model suggests that electrons are accelerated to γ_max ∼ 500, while cooled synchrotron model requires acceleration up to γ_max ∼ 5 × 10⁴. The synchrotron self-Compton scenario requires electron densities of 10¹⁰ cm⁻³ that are much larger than typical ambient densities in the accretion flow. Furthermore, it requires a variation of the particle density that is inconsistent with the average mass-flow rate inferred from polarization measurements and can therefore only be realized in an extraordinary accretion event. In contrast, assuming a source size of 1 R_S, the cooled synchrotron scenario can be realized with densities and magnetic fields comparable with the ambient accretion flow. For both models, the temporal evolution is regulated through the maximum acceleration factor γ_max, implying that sustained particle acceleration is required to explain at least a part of the temporal evolution of the flare.