WFRF:(Taylor Hugh S.)
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| Fältnamn | Indikatorer | Metadata |
|---|---|---|
| 000 | 13298naa a2203157 4500 | |
| 001 | oai:DiVA.org:lnu-41395 | |
| 003 | SwePub | |
| 008 | 150326s2015 | |||||||||||000 ||eng| | |
| 009 | oai:DiVA.org:su-115931 | |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-413952 URI |
| 024 | 7 | a https://doi.org/10.1051/0004-6361/2013226942 DOI |
| 024 | 7 | a https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-1159312 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, Germany,Natl Acad Sci Republ Armenia, Armenia ; Yerevan Phys Inst, Armenia,DESY, Germany ; Univ Potsdam, Germany,Nicolaus Copernicus Astron Ctr, Poland4 aut |
| 245 | 1 0 | a Probing the gamma-ray emission from HESS J1834-087 using HESS and Fermi LAT observations |
| 264 | c 2015-01-20 | |
| 264 | 1 | b EDP Sciences,c 2015 |
| 338 | a print2 rdacarrier | |
| 500 | a AuthorCount:228; | |
| 520 | a Aims. Previous observations with the High Energy Stereoscopic System (H.E.S.S.) have revealed an extended very-high-energy (VHE; E > 100 GeV) gamma-ray source, HESS J1834-087, coincident with the supernova remnant (SNR) W41. The origin of the gamma-ray emission was investigated in more detail with the H.E.S.S. array and the Large Area Telescope (LAT) onboard the Fermi Gamma-ray Space Telescope. Methods. The gamma-ray data provided by 61 h of observations with H.E.S.S., and four years with the Fermi LAT were analyzed, covering over five decades in energy from 1.8 GeV up to 30 TeV. The morphology and spectrum of the TeV and GeV sources were studied and multiwavelength data were used to investigate the origin of the gamma-ray emission toward W41. Results. The TeV source can be modeled with a sum of two components: one point-like and one significantly extended (sigma(TeV) = 0.17 degrees +/- 0.01 degrees), both centered on SNR W41 and exhibiting spectra described by a power law with index Gamma(TeV) similar or equal to 2.6. The GeV source detected with Fermi LAT is extended (sigma(GeV) = 0.15 degrees +/- 0.03 degrees) and morphologically matches the VHE emission. Its spectrum can be described by a power-law model with an index Gamma(GeV) = 2.15 +/- 0.12 and smoothly joins the spectrum of the whole TeV source. A break appears in the gamma-ray spectra around 100 GeV. No pulsations were found in the GeV range. Conclusions. Two main scenarios are proposed to explain the observed emission: a pulsar wind nebula (PWN) or the interaction of SNR W41 with an associated molecular cloud. X-ray observations suggest the presence of a point-like source (a pulsar candidate) near the center of the remnant and nonthermal X-ray diffuse emission that could arise from the possibly associated PWN. The PWN scenario is supported by the compatible positions of the TeV and GeV sources with the putative pulsar. However, the spectral energy distribution from radio to gamma-rays is reproduced by a one-zone leptonic model only if an excess of low-energy electrons is injected following a Maxwellian distribution by a pulsar with a high spin-down power (> 10(37) erg s(-1)). This additional low-energy component is not needed if we consider that the point-like TeV source is unrelated to the extended GeV and TeV sources. The interacting SNR scenario is supported by the spatial coincidence between the gamma-ray sources, the detection of OH (1720 MHz) maser lines, and the hadronic modeling. | |
| 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 acceleration of particles | |
| 653 | a ISM: supernova remnants | |
| 653 | a ISM: clouds | |
| 653 | a cosmic rays | |
| 653 | a Astropartikelfysik | |
| 653 | a Astroparticle Physics | |
| 700 | 1 | a Aharonian, F.u Max Planck Inst Kernphys,Germany ; Dublin Inst Adv Studies, Ireland ; Natl Acad Sci Republ Armenia, Armenia4 aut |
| 700 | 1 | a Benkhali, F. Aitu Max Planck Inst Kernphys,Germany4 aut |
| 700 | 1 | a Akhperjanian, A. G.u Natl Acad Sci Republ Armenia, Armenia ; Yerevan Phys Inst, Armenia,Univ Erlangen Nurnberg, Germany4 aut |
| 700 | 1 | a Angüner, E. O.u Humboldt Univ, Germany4 aut |
| 700 | 1 | a Anton, G.u Univ Erlangen Nurnberg, Germany4 aut |
| 700 | 1 | a Backes, M.u Univ Namibia, Namibia4 aut |
| 700 | 1 | a Balenderans, S.u Univ Durham, UK4 aut |
| 700 | 1 | a Balzer, A.u DESY, Germany ; Univ Potsdam, Germany4 aut |
| 700 | 1 | a Barnacka, A.u Nicolaus Copernicus Astron Ctr, 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 |
| 700 | 1 | a Bernloehr, K.4 aut |
| 700 | 1 | a Birsin, E.4 aut |
| 700 | 1 | a Bissaldi, E.4 aut |
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| 700 | 1 | a Meyer, Manuelu Stockholms universitet,Fysikum,Oskar Klein-centrum för kosmopartikelfysik (OKC)4 aut0 (Swepub:su)rwagner |
| 700 | 1 | a Chalme-Calvet, R.4 aut |
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| 700 | 1 | a Cheesebrough, A.4 aut |
| 700 | 1 | a Chretien, M.4 aut |
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| 700 | 1 | a Cologna, G.4 aut |
| 700 | 1 | a Conrad, Janu Stockholms universitet,Fysikum,Oskar Klein-centrum för kosmopartikelfysik (OKC),Wallenberg Academy Fellow, Sweden4 aut0 (Swepub:su)conrad |
| 700 | 1 | a Couturier, C.4 aut |
| 700 | 1 | a Cui, Y.4 aut |
| 700 | 1 | a Dalton, M.4 aut |
| 700 | 1 | a Daniel, M. K.4 aut |
| 700 | 1 | a Davids, I. D.4 aut |
| 700 | 1 | a Degrange, B.4 aut |
| 700 | 1 | a Deil, C.4 aut |
| 700 | 1 | a deWilt, P.4 aut |
| 700 | 1 | a Dickinson, Hugh J.u Stockholms universitet,Fysikum,Oskar Klein-centrum för kosmopartikelfysik (OKC)4 aut0 (Swepub:su)hdick |
| 700 | 1 | a Djannati-Atai, A.4 aut |
| 700 | 1 | a Domainko, W.4 aut |
| 700 | 1 | a Drury, L. O 'C.4 aut |
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| 700 | 1 | a Fegan, S.4 aut |
| 700 | 1 | a Feinstein, F.4 aut |
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| 700 | 1 | a Giebels, B.4 aut |
| 700 | 1 | a Glicenstein, J. F.4 aut |
| 700 | 1 | a Grondin, M. -H4 aut |
| 700 | 1 | a Grudzinska, M.4 aut |
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| 700 | 1 | a Wagner, R. M.4 aut |
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| 700 | 1 | a Weidinger, M.4 aut |
| 700 | 1 | a Weitzel, Q.4 aut |
| 700 | 1 | a White, R.4 aut |
| 700 | 1 | a Wierzcholska, A.4 aut |
| 700 | 1 | a Willmann, P.4 aut |
| 700 | 1 | a Woernlein, A.4 aut |
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| 700 | 1 | a Yang, R.4 aut |
| 700 | 1 | a Zabalza, V.4 aut |
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| 700 | 1 | a Zdziarski, A. A.4 aut |
| 700 | 1 | a Zech, A.4 aut |
| 700 | 1 | a Zechlin, H. -S4 aut |
| 700 | 1 | a Acero, F.4 aut |
| 700 | 1 | a Casandjian, J. M.4 aut |
| 700 | 1 | a Cohen-Tanugi, J.4 aut |
| 700 | 1 | a Giordano, F.4 aut |
| 700 | 1 | a Guillemot, L.4 aut |
| 700 | 1 | a Lande, J.4 aut |
| 700 | 1 | a Pletsch, H.4 aut |
| 700 | 1 | a Uchiyama, Y.4 aut |
| 710 | 2 | a Univ Hamburg, Germanyb Natl Acad Sci Republ Armenia, Armenia ; Yerevan Phys Inst, Armenia4 org |
| 773 | 0 | t Astronomy and Astrophysicsd : EDP Sciencesg 574q 574x 0004-6361x 1432-0746 |
| 856 | 4 | u https://www.aanda.org/articles/aa/pdf/2015/02/aa22694-13.pdf |
| 856 | 4 | u https://doi.org/10.1051/0004-6361/201322694y Fulltext |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:lnu:diva-41395 |
| 856 | 4 8 | u https://doi.org/10.1051/0004-6361/201322694 |
| 856 | 4 8 | u https://urn.kb.se/resolve?urn=urn:nbn:se:su:diva-115931 |
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