PoS - Proceedings of Science
Volume 395 - 37th International Cosmic Ray Conference (ICRC2021) - CRI - Cosmic Ray Indirect
New Constraints on Cosmic Particle Populations at the Galactic Center using X-ray Observations of the Molecular Cloud Sagittarius B2
F. Rogers*, S. Zhang, K. Perez, M. Clavel and A. Taylor
Full text: pdf
Pre-published on: August 03, 2021
Published on: March 18, 2022
Located $\sim100$ pc from the dynamic center of the Milky Way, the molecular cloud Sagittarius B2 (Sgr B2) is the most massive such object in the Galactic Center region.
In X-rays, Sgr B2 shows a prominent neutral Fe K$\alpha$ line at 6.4 keV and continuum emission beyond 10 keV, indicating high-energy, non-thermal processes in the cloud.
The Sgr B2 complex is an X-ray reflection nebula whose total emissions have decreased since the year 2001 as it reprocesses what are likely one or more past energetic outbursts from the supermassive black hole Sagittarius A*. The X-ray reflection model explains the observed time-variability of the Fe K$\alpha$ and hard X-ray emissions, and it provides a window into the luminous history of our nearest supermassive black hole.
In light of evidence of elevated cosmic particle populations in the Galactic Center, recent interest has also focused on X-rays from Sgr B2 as a probe of low-energy (sub-GeV) cosmic particles.
In contrast to X-ray reflection, in this case we can assume that the X-ray flux contribution from ionization by low-energy cosmic particles is constant in time, such that upper limits on low-energy cosmic particle populations may be obtained using the lowest flux levels observed from the cloud.
Here, we present the most recent and correspondingly dimmest NuSTAR and XMM-Newton observations of Sgr B2, from 2018.
These reveal small-scale variations within lower density portions of the Sgr B complex, including brightening features, and enable the best upper limits on ionization of molecular clouds by low-energy cosmic particles in the inner $\sim100$ pc of the Galaxy.
DOI: https://doi.org/10.22323/1.395.0288
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