Please use this identifier to cite or link to this item:
https://hdl.handle.net/2440/50810
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DC Field | Value | Language |
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dc.contributor.author | Aharonian, F. | - |
dc.contributor.author | Akhperjanian, A. | - |
dc.contributor.author | Barres de Almaida, U. | - |
dc.contributor.author | Bazer-Bachi, A. | - |
dc.contributor.author | Becherini, Y. | - |
dc.contributor.author | Behera, B. | - |
dc.contributor.author | Benbow, W. | - |
dc.contributor.author | Bernlohr, K. | - |
dc.contributor.author | Boisson, C. | - |
dc.contributor.author | Bochow, A. | - |
dc.contributor.author | Borrel, V. | - |
dc.contributor.author | Braun, I. | - |
dc.contributor.author | Brion, E. | - |
dc.contributor.author | Brucker, J. | - |
dc.contributor.author | Brun, P. | - |
dc.contributor.author | Buhler, R. | - |
dc.contributor.author | Bulik, T. | - |
dc.contributor.author | Busching, I. | - |
dc.contributor.author | Boutelier, T. | - |
dc.contributor.author | Carrigan, S. | - |
dc.contributor.author | et al. | - |
dc.date.issued | 2008 | - |
dc.identifier.citation | Astronomy and Astrophysics: a European journal, 2008; 492(1):L25-L28 | - |
dc.identifier.issn | 0004-6361 | - |
dc.identifier.issn | 1432-0746 | - |
dc.identifier.uri | http://hdl.handle.net/2440/50810 | - |
dc.description | Copyright © ESO 2008 | - |
dc.description.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 HESS J1745−290 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 ∼1014 cm (∼100 RS) of the supermassive black hole. | - |
dc.description.statementofresponsibility | F. Aharonian, A. G. Akhperjanian, U. Barres de Almeida, A. R. Bazer-Bachi, Y. Becherini ... Gavin P. Rowell ... et al. | - |
dc.language.iso | en | - |
dc.publisher | EDP Sciences | - |
dc.rights | Copyright © ESO 2008 | - |
dc.source.uri | http://dx.doi.org/10.1051/0004-6361:200810912 | - |
dc.subject | gamma rays: observations | - |
dc.subject | X-rays: individuals: Sgr A* | - |
dc.title | Simultaneous HESS and Chandra observations of Sagitarius A(star) during an X-ray flare | - |
dc.type | Journal article | - |
dc.identifier.doi | 10.1051/0004-6361:200810912 | - |
pubs.publication-status | Published | - |
dc.identifier.orcid | Rowell, G. [0000-0002-9516-1581] | - |
Appears in Collections: | Aurora harvest Chemistry and Physics publications |
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File | Description | Size | Format | |
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hdl_50810.pdf | Published version | 101.86 kB | Adobe PDF | View/Open |
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