J 2019

Multi-wavelength torus-jet model for Sagittarius A*

VINCENT, Frédéric H., Marek ABRAMOWICZ, Andrzej A. ZDZIARSKI, Maciej Iek WIELGUS, Thibaut PAUMARD et. al.

Basic information

Original name

Multi-wavelength torus-jet model for Sagittarius A*

Authors

VINCENT, Frédéric H. (250 France), Marek ABRAMOWICZ (616 Poland, guarantor, belonging to the institution), Andrzej A. ZDZIARSKI (616 Poland), Maciej Iek WIELGUS (616 Poland), Thibaut PAUMARD (250 France), Guy S. PERRIN (250 France) and Odelle STRAUB (756 Switzerland)

Edition

Astronomy & Astrophysics, 2019, 0004-6361

Other information

Language

English

Type of outcome

Článek v odborném periodiku

Field of Study

10308 Astronomy

Country of publisher

France

Confidentiality degree

není předmětem státního či obchodního tajemství

References:

RIV identification code

RIV/47813059:19240/19:A0000437

Organization unit

Faculty of Philosophy and Science in Opava

UT WoS

000463695200002

Keywords in English

Galaxy: center; accretion: accretion disks; black hole physics; relativistic processes

Tags

International impact, Reviewed

Links

GA17-16287S, research and development project.
Změněno: 21/4/2020 10:33, Ing. Petra Skoumalová

Abstract

V originále

Context. The properties of the accretion/ejection flow surrounding the supermassive central black hole of the Galaxy Sgr A* will be scrutinized by the new-generation instrument GRAVITY and the Event Horizon Telescope (EHT). Developing fast, robust, and simple models of such flows is therefore important and very timely. Aims. We want to model the quiescent emission of Sgr A* from radio to mid-infrared wavelengths, using thermal and nonthermal synchrotron. The radiation is emitted by the overlay of a magnetized compact torus close to the black hole, and a large-scale magnetized jet. We compare model spectra and images to the multi-wavelength observable constraints available to date. We simulate EHT observations at 1.3 mm of the best-fit model for different inclinations. Methods. We use a simple analytic description for the geometry of the torus and jet. We model their emission by thermal synchrotron and kappa-distribution synchrotron, respectively. We use relativistic ray tracing to compute simulated spectra and images, restricting our analysis to the Schwarzschild (zero spin) case. A best-fit is found by adjusting the simulated spectra to the latest observed data, and we check the consistency of our spectral best fits with the radio-image sizes and infrared spectral index constraints. We use the open-source eht-imaging library to generate EHT-reconstructed images. Results. We find perfect spectral fit (chi^(2)_(red) approximate to 1)both for nearly face-on and nearly edge-on views. These best fits give parameter values very close to those found by the most recent numerical simulations, which are much more complex than our model. The intrinsic radio size of Sgr A* is found to be in reasonable agreement with the centimetric observed constraints. Our best-fit infrared spectral index is in perfect agreement with the latest constraints. Our emission region at 1.3 mm, although larger than the early-EHT Gaussian best fit, does contain bright features at the less than or similar to 40 mu as scale. EHT-reconstructed images show that torus/jet-specific features persist after the reconstruction procedure, and that these features are sensitive to inclination. Conclusions. The main interest of our model is to provide a simple and fast model of the quiescent state of Sgr A*, which gives extremely similar results to those of state-of-the-art numerical simulations. Our model is easy to use and we publish all the material necessary to reproduce our spectra and images, meaning that anyone interested can use our results relatively straightforwardly. We hope that such a public tool will be useful in the context of the recent and near-future GRAVITY and EHT results.