Sökning: onr:"swepub:oai:DiVA.org:lnu-39562" > Diffuse Galactic ga...
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000 | 12196naa a2203061 4500 | |
001 | oai:DiVA.org:lnu-39562 | |
003 | SwePub | |
008 | 150129s2014 | |||||||||||000 ||eng| | |
009 | oai:DiVA.org:su-113564 | |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-395622 URI |
024 | 7 | a https://doi.org/10.1103/PhysRevD.90.1220072 DOI |
024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1135642 URI |
040 | a (SwePub)lnud (SwePub)su | |
041 | a engb eng | |
042 | 9 SwePub | |
072 | 7 | a ref2 swepub-contenttype |
072 | 7 | a art2 swepub-publicationtype |
100 | 1 | a Abramowski, A.u Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germany,Natl Acad Sci Republ Armenia, Yerevan 0019, Armenia,Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, NL-1098 XH Amsterdam, Netherlands,Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland4 aut |
245 | 1 0 | a Diffuse Galactic gamma-ray emission with HESS |
264 | 1 | c 2014 |
338 | a print2 rdacarrier | |
500 | a AuthorCount:226; | |
520 | a Diffuse gamma-ray emission is the most prominent observable signature of celestial cosmic-ray interactions at high energies. While already being investigated at GeVenergies over several decades, assessments of diffuse gamma-ray emission at TeVenergies remain sparse. After completion of the systematic survey of the inner Galaxy, the H.E.S.S. experiment is in a prime position to observe large-scale diffuse emission at TeVenergies. Data of the H.E.S.S. Galactic Plane Survey are investigated in regions off known gamma-ray sources. Corresponding gamma-ray flux measurements were made over an extensive grid of celestial locations. Longitudinal and latitudinal profiles of the observed gamma-ray fluxes show characteristic excess emission not attributable to known gamma-ray sources. For the first time large-scale gamma-ray emission along the Galactic plane using imaging atmospheric Cherenkov telescopes has been observed. While the background subtraction technique limits the ability to recover modest variation on the scale of the H.E.S.S. field of view or larger, which is characteristic of the inverse Compton scatter-induced Galactic diffuse emission, contributions of neutral pion decay as well as emission from unresolved gamma-ray sources can be recovered in the observed signal to a large fraction. Calculations show that the minimum gamma-ray emission from pi(0) decay represents a significant contribution to the total signal. This detection is interpreted as a mix of diffuse Galactic gamma-ray emission and unresolved sources. | |
650 | 7 | a NATURVETENSKAPx Fysikx Astronomi, astrofysik och kosmologi0 (SwePub)103052 hsv//swe |
650 | 7 | a NATURAL SCIENCESx Physical Sciencesx Astronomy, Astrophysics and Cosmology0 (SwePub)103052 hsv//eng |
653 | a Astropartikelfysik | |
653 | a Astroparticle Physics | |
700 | 1 | a Aharonian, F.u Max Planck Inst Kernphys, D-69029 Heidelberg, Germany4 aut |
700 | 1 | a Benkhali, F. Aitu Max Planck Inst Kernphys, D-69029 Heidelberg, Germany4 aut |
700 | 1 | a Akhperjanian, A. G.u Natl Acad Sci Republ Armenia, Yerevan 0019, Armenia4 aut |
700 | 1 | a Anguener, E. O.u Humboldt Univ, Inst Phys, D-12489 Berlin, Germany4 aut |
700 | 1 | a Backes, M.u Univ Namibia, Dept Phys, Windhoek, Namibia4 aut |
700 | 1 | a Balenderan, S.u Univ Durham, Dept Phys, Durham DH1 3LE, England4 aut |
700 | 1 | a Balzer, A.u Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, NL-1098 XH Amsterdam, Netherlands4 aut |
700 | 1 | a Barnacka, A.u Uniwersytet Jagiellonski, Obserwatorium Astron, PL-30244 Krakow, Poland4 aut |
700 | 1 | a Becherini, Yvonneu Linnéuniversitetet,Institutionen för fysik och elektroteknik (IFE)4 aut0 (Swepub:lnu)yvbeaa |
700 | 1 | a Tjus, J. Becker4 aut |
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710 | 2 | a Univ Hamburg, Inst Expt Phys, D-22761 Hamburg, Germanyb Natl Acad Sci Republ Armenia, Yerevan 0019, Armenia4 org |
773 | 0 | t Physical Review Dg 90:12, s. Article ID: 122007-q 90:12<Article ID: 122007-x 1550-7998x 1550-2368 |
856 | 4 | u https://arxiv.org/abs/1411.7568y arXiv:1411.7568 |
856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-39562 |
856 | 4 8 | u https://doi.org/10.1103/PhysRevD.90.122007 |
856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-113564 |
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