Abstract
The rapidly varying (~10 min timescale) non-thermal X-ray emission observed from Sgr A implies that particle acceleration is occuring close to the event horizon of the supermassive black hole. The TeV γ-ray source HESSJ1745-290 is coincident with Sgr A* and may be closely related to its X-ray emission. Simultaneous X-ray and TeV observations are required to elucidate the relationship between these objects. We report on joint HESS/Chandra observations performed in July 2005, during which an X-ray flare was detected. Despite a factor of ≈9 increase in the X-ray flux of Sgr A*, no evidence is found for an increase in the TeV γ-ray flux from this region. We find that an increase in the γ-ray flux of a factor of 2 or greater can be excluded at a confidence level of 99%. This finding disfavours scenarios in which the keV and TeV emission are associated with the same population of accelerated particles and in which the bulk of the γ-ray emission is produced within ∼ cm (∼100 Rs) of the supermassive black hole.
Original language | English (US) |
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Pages (from-to) | L25-L28 |
Journal | Astronomy and Astrophysics |
Volume | 492 |
Issue number | 1 |
DOIs | |
State | Published - Dec 1 2008 |
Externally published | Yes |
Keywords
- Gamma rays: observations
- X-rays: individuals: Sgr A
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science