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  • 6951.
    Abramowski, A.
    et al.
    University of Hamburg, Germany.
    Aharonian, F.
    Max Planck Inst Kernphys, Germany ; Dublin Inst Adv Studies, Ireland ; Natl Acad Sci Republ Armenia, Armenia.
    Benkhali, F. Ait
    Max Planck Inst Kernphys, Germany.
    Akhperjanian, A. G.
    Natl Acad Sci Republ Armenia, Armenia ; Yerevan Phys Inst, Armenia.
    Anguner, E. O.
    Humboldt Univ, Germany.
    Backes, M.
    Univ Namibia, Namibia.
    Balenderans, S.
    Univ Durham, UK.
    Balzer, A.
    Univ Amsterdam, Netherlands.
    Barnacka, A.
    Uniwersytet Jagiellonski, Poland.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Berge, D.
    Bernhard, S.
    Bernloehr, K.
    Birsin, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Bregeon, J.
    Brun, F.
    Brun, P.
    Bryan, M.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Chadwick, P. M.
    Chatraborty, N.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Cui, Y.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Djannati-Atai, A.
    Domainko, W.
    Donath, A.
    Drury, L. O ' C
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gabici, S.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Gottschall, D.
    Grondin, M. -H
    Grudzinska, M.
    Hadasch, D.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Ivascenko, A.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung-Richardt, O.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kolitzus, D.
    Komin, Nu
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lefranc, V.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. P.
    Lohse, T.
    Lopatin, A.
    Lu, C-C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Mitchell, A. M. W.
    Moderski, R.
    Mohamed, M.
    Mora, K.
    Moulin, E.
    Murach, T.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Odaka, H.
    Ohm, S.
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Anibas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Petrucci, P-O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Université Paris Diderot, France.
    Quirrenbach, A.
    Raab, S.
    Reichardt, I.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Salek, D.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spanier, F.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Tavernet, J-P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Veh, J.
    Venter, C.
    Viana, A.
    Vincent, P.
    Vink, J.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Wagner, R. M.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Yang, R.
    Zabalza, V.
    Zaborov, D.
    Zacharias, M.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H-S
    H.E.S.S. detection of TeV emission from the interaction region between the supernova remnant G349.7+0.2 and a molecular cloud2015In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 574, p. 1-7, article id A100Article in journal (Refereed)
    Abstract [en]

    G349.7+0.2 is a young Galactic supernova remnant (SNR) located at the distance of 11.5 kpc and observed across the entire electromagnetic spectrum from radio to high energy (HE; 0.1 GeV < E < 100 GeV) gamma-rays. Radio and infrared observations indicate that the remnant is interacting with a molecular cloud. In this paper, the detection of very high energy (VHE, E > 100 GeV) gamma-ray emission coincident with this SNR with the High Energy Stereoscopic System (HESS.) is reported. This makes it one of the farthest Galactic SNR ever detected in this domain. An integral flux F(E > 400 GeV) = (6.5 +/- 1.1(stat) +/- 1.3(syst)) x 10-11 ph cm(-2) s(-1) corresponding to similar to 0.7% of that of the Crab Nebula and to a luminosity of similar to 10(34) erg s(-1) above the same energy threshold, and a steep photon index Gamma(VHE) = 2.8 +/- 0.27(stat) +/- 0.20(syst) are measured. The analysis of more than 5 yr of Fermi-LAT data towards this source shows a power-law like spectrum with a best-fit photon index Gamma(HE) = 2.2 +/- 0.04.2(stat-0.31sys)(+0.13), The combined gamma-ray spectrum of 0349.7+0.2 can be described by either a broken power law (I3PL) or a power law with exponential (or sub exponential) cutoff (PLC). In the former case, the photon break energy is found at E-br,E-gamma = 551(-30)(+70) GeV, slightly higher than what is usually observed in the HE/VHE gamma-ray emitting middle-aged SNRs known to be interacting with molecular clouds. In the latter case. the exponential (respectively sub-exponential) cutoff energy is measured at E-cat,E-gamma = 1.4(-0.55)(+1.6) (respectively 0.35(-0.21)(+0.75)) TeV. A pion decay process resulting from the interaction of the accelerated protons and nuclei with the dense surrounding medium is clearly the preferred scenario to explain the gamma-ray emission. The BPL with a spectral steepening of 0.5-1 and the PLC provide equally good fits to the data. The product or the average gas density and the total energy content of accelerated protons and nuclei amounts to nu W-p similar to 5 x 10(51) erg cm(-3)

  • 6952.
    Abramowski, A.
    et al.
    University of Hamburg, Germany.
    Aharonian, F.
    Max Planck Institute for Nuclear Physics, Germany ; Dublin Institute for Advanced Studies, Ireland ; National Academy of Sciences of the Republic of Armenia, Armenia.
    Benkhali, F. Ait
    Max Planck Institute for Nuclear Physics, Germany.
    Akhperjanian, A. G.
    National Academy of Sciences of the Republic of Armenia, Armenia ; Yerevan Physics Institute, Armenia.
    Angüner, E.
    Humboldt-Universität zu Berlin, Germany.
    Anton, G.
    Friedrich-Alexander-Universität Erlangen-Nürnberg, Germany.
    Balenderan, S.
    University of Durham, UK.
    Balzer, A.
    DESY, Germany ; University of Potsdam, Germany.
    Barnacka, A.
    Nicolaus Copernicus Astronomical Center, Poland.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Cerruti, M.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, H. J.
    Djannati-Ataie, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Grondin, M. -H
    Grudzinska, M.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lennarz, D.
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Université Paris Diderot, France.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Rob, L.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Szostek, A.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Vink, J.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Zabalza, V.
    Zacharias, M.
    Zajczyk, A.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    HESS J1640-465-an exceptionally luminous TeV gamma-ray supernova remnant2014In: Monthly notices of the Royal Astronomical Society, ISSN 0035-8711, E-ISSN 1365-2966, Vol. 439, no 3, p. 2828-2836Article in journal (Refereed)
    Abstract [en]

    The results of follow-up observations of the TeV gamma-ray source HESS J1640-465 from 2004 to 2011 with the High Energy Stereoscopic System (HESS) are reported in this work. The spectrum is well described by an exponential cut-off power law with photon index Gamma = 2.11 +/- 0.09(stat) +/- 0.10(sys), and a cut-off energy of E-2 = 6.0(-1.2)(+2.0) TeV. The TeV emission is significantly extended and overlaps with the northwestern part of the shell of the SNR G338.3-0.0. The new HESS results, a re-analysis of archival XMM-Newton data and multiwavelength observations suggest that a significant part of the gamma-ray emission from HESS J1640-465 originates in the supernova remnant shell. In a hadronic scenario, as suggested by the smooth connection of the GeV and TeV spectra, the product of total proton energy and mean target density could be as high as W(p)n(H) similar to 4 x 10(52)(d/10kpc)(2) erg cm(-3).

  • 6953.
    Abramowski, A.
    et al.
    Univ Hamburg, Germany.
    Aharonian, F.
    Max Planck Inst Kernphys,Germany ; Dublin Inst Adv Studies, Ireland ; Natl Acad Sci Republ Armenia, Armenia.
    Benkhali, F. Ait
    Max Planck Inst Kernphys,Germany.
    Akhperjanian, A. G.
    Natl Acad Sci Republ Armenia, Armenia ; Yerevan Phys Inst, Armenia.
    Angüner, E. O.
    Humboldt Univ, Germany.
    Anton, G.
    Univ Erlangen Nurnberg, Germany.
    Backes, M.
    Univ Namibia, Namibia.
    Balenderans, S.
    Univ Durham, UK.
    Balzer, A.
    DESY, Germany ; Univ Potsdam, Germany .
    Barnacka, A.
    Nicolaus Copernicus Astron Ctr, Poland.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Bernloehr, K.
    Birsin, E.
    Bissaldi, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Brucker, J.
    Brun, F.
    Brun, P.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Chadwick, P. M.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Cheesebrough, A.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Daniel, M. K.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Dickinson, H. J.
    Djannati-Atai, A.
    Domainko, W.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Grondin, M. -H
    Grudzinska, M.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kneiske, T.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Moderski, R.
    Mohamed, M.
    Moulin, E.
    Murach, T.
    Naumann, C. L.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Odaka, H.
    Ohm, S.
    Wilhelmi, E. de Ona
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Perez, J.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Univ Paris Diderot, APC, AstroParticule & Cosmology, CNRS,IN2P3,CEA,Irfu, Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
    Quirrenbach, A.
    Raab, S.
    Raue, M.
    Reichardt, I.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    Reyes, R. de los
    Rieger, F.
    Rob, L.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Venter, C.
    Viana, A.
    Vincent, P.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Wagner, R. M.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Yang, R.
    Zabalza, V.
    Zacharias, M.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    Acero, F.
    Casandjian, J. M.
    Cohen-Tanugi, J.
    Giordano, F.
    Guillemot, L.
    Lande, J.
    Pletsch, H.
    Uchiyama, Y.
    Probing the gamma-ray emission from HESS J1834-087 using HESS and Fermi LAT observations2015In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 574, article id A27Article in journal (Refereed)
    Abstract [en]

    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.

  • 6954.
    Abramowski, A.
    et al.
    Univ Hamburg, Germany.
    Aharonian, F.
    Max Planck Inst Kernphys,Germany ; Dublin Inst Adv Studies, Ireland ; Natl Acad Sci Republ Armenia, Armenia.
    Benkhali, F. Ait
    Max Planck Inst Kernphys,Germany.
    Akhperjanian, A. G.
    Natl Acad Sci Republ Armenia, Armenia ; Yerevan Phys Inst, Armenia.
    Angüner, E. O.
    Humboldt Univ, Germany.
    Backes, M.
    Univ Namibia, Namibia.
    Balenderans, S.
    Univ Durham, UK.
    Balzer, A.
    Univ Amsterdam, Netherlands.
    Barnacka, A.
    Uniwersytet Jagiellonski, Poland.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Berge, D.
    Bernhard, S.
    Bernloehr, K.
    Birsin, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Bregeon, J.
    Brun, F.
    Brun, P.
    Bryan, M.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Chadwick, P. M.
    Chakraborty, N.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Cui, Y.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Djannati-Atai, A.
    Domainko, W.
    Donath, A.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gabici, S.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Gottschall, D.
    Grondin, M. -H
    Grudzinska, M.
    Hadasch, D.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Ivascenko, A.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung-Richardt, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kolitzus, D.
    Komin, Nu
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lefaucheur, J.
    Lefranc, V.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Mitchell, A. M. W.
    Moderski, R.
    Mohamed, M.
    Mora, K.
    Moulin, E.
    Murach, T.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Odaka, H.
    Ohm, S.
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Univ Paris Diderot, APC, AstroParticule & Cosmology, CNRS,IN2P3,CEA,Irfu, Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
    Quirrenbach, A.
    Raab, S.
    Reichardt, I.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    de los Reyes, R.
    Rieger, F.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Salek, D.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spanier, F.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Veh, J.
    Venter, C.
    Viana, A.
    Vincent, P.
    Vink, J.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Wagner, R. M.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Yang, R.
    Zabalza, V.
    Zaborov, D.
    Zacharias, M.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    Constraints on an Annihilation Signal from a Core of Constant Dark Matter Density around the Milky Way Center with HESS2015In: Physical Review Letters, ISSN 0031-9007, E-ISSN 1079-7114, Vol. 114, no 8, article id 081301Article in journal (Refereed)
    Abstract [en]

    An annihilation signal of dark matter is searched for from the central region of the Milky Way. Data acquired in dedicated on-off observations of the Galactic center region with H.E.S.S. are analyzed for this purpose. No significant signal is found in a total of similar to 9 h of on-off observations. Upper limits on the velocity averaged cross section, <sigma upsilon >, for the annihilation of dark matter particles with masses in the range of similar to 300 GeV to similar to 10 TeV are derived. In contrast to previous constraints derived from observations of the Galactic center region, the constraints that are derived here apply also under the assumption of a central core of constant dark matter density around the center of the Galaxy. Values of <sigma upsilon > that are larger than 3 x 10(-24) cm(3)/s are excluded for dark matter particles with masses between similar to 1 and similar to 4 TeV at 95% C.L. if the radius of the central dark matter density core does not exceed 500 pc. This is the strongest constraint that is derived on <sigma upsilon > for annihilating TeV mass dark matter without the assumption of a centrally cusped dark matter density distribution in the search region.

  • 6955.
    Abramowski, A.
    et al.
    University of Hamburg, Germany.
    Aharonian, F.
    Max Planck Institute for Nuclear Physics, Germany ; Dublin Institute for Advanced Studies, Ireland ; National Academy of Sciences of the Republic of Armenia, Armenia.
    Benkhali, F. Ait
    Max Planck Institute for Nuclear Physics, Germany.
    Akhperjanian, A. G.
    Yerevan Physics Institute, Armenia ; National Academy of Sciences of the Republic of Armenia, Armenia.
    Angüner, E. O.
    Humboldt University of Berlin, Germany.
    Backes, M.
    University of Namibia, Namibia.
    Balzer, A.
    University of Amsterdam, Netherlands.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Ruhr University Bochum, Germany.
    Berge, D.
    University of Amsterdam, Netherlands.
    Bernhard, S.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Bernloehr, K.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Birsin, E.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Blackwell, R.
    Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia..
    Boettcher, M.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Boisson, C.
    Univ Paris Diderot, CNRS, Observ Paris, LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Bolmont, J.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Bordas, P.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Bregeon, J.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Brun, F.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Brun, P.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Bryan, M.
    Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Bulik, T.
    Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland..
    Carr, J.
    Aix Marseille Univ, CNRS, IN2P3, CPPM UMR 7346, F-13288 Marseille, France..
    Casanova, S.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;PAN, Inst Fizyki Jadrowej, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Chakraborty, N.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Chalme-Calvet, R.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Chaves, R. C. G.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Chen, A.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Chevalier, J.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Chretien, M.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Colafrancesco, S.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Cologna, G.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Condon, B.
    Univ Bordeaux, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France..
    Conrad, J.
    Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden..
    Couturier, C.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Cui, Y.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Davids, I. D.
    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia.;North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Degrange, B.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Deil, C.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    deWilt, P.
    Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia..
    Djannati-Atai, A.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Domainko, W.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Donath, A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Drury, L. O 'C.
    Dubus, G.
    Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.;CNRS, IPAG, F-38000 Grenoble, France..
    Dutson, K.
    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
    Dyks, J.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Dyrda, M.
    PAN, Inst Fizyki Jadrowej, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Edwards, T.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Egberts, K.
    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
    Eger, P.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Ernenwein, J. -P
    Espigat, P.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Farnier, C.
    Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden..
    Fegan, S.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Feinstein, F.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Fernandes, M. V.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Fernandez, D.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Fiasson, A.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Fontaine, G.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Foerster, A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Fuessling, M.
    DESY, D-15738 Zeuthen, Germany..
    Gabici, S.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Gajdus, M.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Gallant, Y. A.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Garrigoux, T.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Giavitto, G.
    DESY, D-15738 Zeuthen, Germany..
    Giebels, B.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Glicenstein, J. F.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Gottschall, D.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Goyal, A.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Grondin, M. -H
    Grudzinska, M.
    Univ Warsaw, Astron Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland..
    Hadasch, D.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Haeffner, S.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Hahn, J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Hawkes, J.
    Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia..
    Heinzelmann, G.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Henri, G.
    Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.;CNRS, IPAG, F-38000 Grenoble, France..
    Hermann, G.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Hervet, O.
    Univ Paris Diderot, CNRS, Observ Paris, LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Hillert, A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Hinton, J. A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
    Hofmann, W.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Hofverberg, P.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Hoischen, C.
    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany..
    Holler, M.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Horns, D.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Ivascenko, A.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Jacholkowska, A.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Jamrozy, M.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Janiak, M.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Jankowsky, F.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Jung-Richardt, I.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Kastendieck, M. A.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Katarzynski, K.
    Nicolaus Copernicus Univ, Fac Phys Astron & Informat, Ctr Astron, Grudziadzka 5, PL-87100 Torun, Poland..
    Katz, U.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Kerszberg, D.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Khelifi, B.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Kieffer, M.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Klepser, S.
    DESY, D-15738 Zeuthen, Germany..
    Klochkov, D.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Kluzniak, W.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Kolitzus, D.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Komin, Nu.
    Univ Witwatersrand, Sch Phys, 1 Jan Smuts Ave, ZA-2050 Johannesburg, South Africa..
    Kosack, K.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Krakau, S.
    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
    Krayzel, F.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Krueger, P. P.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Laffon, H.
    Univ Bordeaux, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France..
    Lamanna, G.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Lau, J.
    Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia..
    Lefaucheur, J.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Lefranc, V.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Lemiere, A.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Lemoine-Goumard, M.
    Univ Bordeaux, CNRS, IN2P3, Ctr Etud Nucl Bordeaux Gradignan, F-33175 Gradignan, France..
    Lenain, J. -P
    Lohse, T.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Lopatin, A.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Lorentz, M.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Lu, C. -C
    Lui, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Marandon, V.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Marcowith, A.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Mariaud, C.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Marx, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Maurin, G.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Maxted, N.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Mayer, M.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Meintjes, P. J.
    Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa..
    Menzler, U.
    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
    Meyer, M.
    Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden..
    Mitchell, A. M. W.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Moderski, R.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Mohamed, M.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Mora, K.
    Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden..
    Moulin, E.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Murach, T.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    de Naurois, M.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Niemiec, J.
    PAN, Inst Fizyki Jadrowej, Ul Radzikowskiego 152, PL-31342 Krakow, Poland..
    Oakes, L.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Odaka, H.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Oettl, S.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Ohm, S.
    DESY, D-15738 Zeuthen, Germany..
    Opitz, B.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Ostrowski, M.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Oya, I.
    DESY, D-15738 Zeuthen, Germany..
    Panter, M.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Parsons, R. D.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Arribas, M. Paz
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Pekeur, N. W.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Pelletier, G.
    Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.;CNRS, IPAG, F-38000 Grenoble, France..
    Petrucci, P. -O
    Peyaud, B.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Pita, S.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Poon, H.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Prokhorov, Dmitry
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Prokoph, Heike
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Puehlhofer, G.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Punch, M.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Quirrenbach, A.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Raab, S.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Reichardt, I.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Reimer, A.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Reimer, O.
    Leopold Franzens Univ Innsbruck, Inst Astro & Teilchenphys, A-6020 Innsbruck, Austria..
    Renaud, M.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    de los Reyes, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Rieger, F.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;Heidelberg Univ, ITA, DFG, D-69117 Heidelberg, Germany..
    Romoli, C.
    Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland..
    Rosier-Lees, S.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Rowell, G.
    Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia..
    Rudak, B.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Rulten, C. B.
    Univ Paris Diderot, CNRS, Observ Paris, LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Sahakian, V.
    Natl Acad Sci Republ Armenia, Marshall Baghramian Ave 24, Yerevan 0019, Armenia.;Yerevan Phys Inst, 2 Alikhanian Bros St, Yerevan 375036, Armenia..
    Salek, D.
    Univ Amsterdam, Inst High Energy Phys, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Sanchez, D. A.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Santangelo, A.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Sasaki, M.
    Univ Tubingen, Inst Astron & Astrophys, Sand 1, D-72076 Tubingen, Germany..
    Schlickeiser, R.
    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
    Schuessler, F.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Schulz, A.
    DESY, D-15738 Zeuthen, Germany..
    Schwanke, U.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Schwemmer, S.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Seyffert, A. S.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Simoni, R.
    Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Sol, H.
    Univ Paris Diderot, CNRS, Observ Paris, LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Spanier, F.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Spengler, G.
    Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden..
    Spies, F.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Stawarz, L.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Steenkamp, R.
    Univ Namibia, Dept Phys, Private Bag 13301, Windhoek, Namibia..
    Stegmann, C.
    Univ Potsdam, Inst Phys & Astron, Karl Liebknecht Str 24-25, D-14476 Potsdam, Germany.;DESY, D-15738 Zeuthen, Germany..
    Stinzing, F.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Stycz, K.
    DESY, D-15738 Zeuthen, Germany..
    Sushch, I.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Tavernet, J. -P
    Tavernier, T.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Taylor, A. M.
    Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin 2, Ireland..
    Terrier, R.
    Univ Paris Diderot, CNRS, IN2P3, CEA Irfu,Observ Paris,Sorbonne Paris Cite,APC,Ast, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France..
    Tluczykont, M.
    Univ Hamburg, Inst Expt Phys, Luruper Chaussee 149, D-22761 Hamburg, Germany..
    Trichard, C.
    Univ Savoie Mt Blanc, CNRS, IN2P3, Lab Annecy Le Vieux Phys Particules, F-74941 Annecy Le Vieux, France..
    Tuffs, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Valerius, K.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    van der Walt, J.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    van Eldik, C.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    van Soelen, B.
    Univ Free State, Dept Phys, POB 339, ZA-9300 Bloemfontein, South Africa..
    Vasileiadis, G.
    Univ Montpellier 2, CNRS, IN2P3, Lab Universe & Particules Montpellier, CC 72,Pl Eugene Bataillon, F-34095 Montpellier 5, France..
    Veh, J.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Venter, C.
    North West Univ, Ctr Space Res, ZA-2520 Potchefstroom, South Africa..
    Viana, A.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Vincent, P.
    Univ Pierre & Marie Curie Paris 6, Univ Denis Diderot Paris 7, CNRS, IN2P3,LPNHE, 4 Pl Jussieu, F-75252 Paris 5, France..
    Vink, J.
    Univ Amsterdam, Astron Inst Anton Pannekoek, GRAPPA, Sci Pk 904, NL-1098 XH Amsterdam, Netherlands..
    Voisin, F.
    Univ Adelaide, Sch Chem & Phys, Adelaide, SA 5005, Australia..
    Voelk, H. J.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Vuillaume, T.
    Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.;CNRS, IPAG, F-38000 Grenoble, France..
    Wagner, S. J.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Wagner, P.
    Humboldt Univ, Inst Phys, Newtonstr 15, D-12489 Berlin, Germany..
    Wagner, R. M.
    Stockholm Univ, Albanova Univ Ctr, Oskar Klein Ctr, Dept Phys, S-10691 Stockholm, Sweden..
    Weidinger, M.
    Ruhr Univ Bochum, Inst Theoret Phys, Lehrstuhl Weltraum & Astrophys 4, D-44780 Bochum, Germany..
    White, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany.;Univ Grenoble Alpes, IPAG, F-38000 Grenoble, France.;CNRS, IPAG, F-38000 Grenoble, France..
    Wierzcholska, A.
    PAN, Inst Fizyki Jadrowej, Ul Radzikowskiego 152, PL-31342 Krakow, Poland.;Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Willmann, P.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Woernlein, A.
    Univ Erlangen Nurnberg, Phys Inst, Erwin Rommel Str 1, D-91058 Erlangen, Germany..
    Wouters, D.
    CEA Saclay, DSM Irfu, F-91191 Gif Sur Yvette, France..
    Yang, R.
    Max Planck Inst Kernphys, POB 103980, D-69029 Heidelberg, Germany..
    Zabalza, V.
    Univ Leicester, Dept Phys & Astron, Univ Rd, Leicester LE1 7RH, Leics, England..
    Zaborov, D.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Zacharias, M.
    Heidelberg Univ, Landessternwarte, D-69117 Heidelberg, Germany..
    Zdziarski, A. A.
    Nicolaus Copernicus Astron Ctr, Ul Bartycka 18, PL-00716 Warsaw, Poland..
    Zech, A.
    Univ Paris Diderot, CNRS, Observ Paris, LUTH, 5 Pl Jules Janssen, F-92190 Meudon, France..
    Zefi, F.
    Ecole Polytech, CNRS, IN2P3, Lab Leprince Ringuet, F-91128 Palaiseau, France..
    Zywucka, N.
    Uniwersytet Jagiellonski, Obserwatorium Astron, Ul Orla 171, PL-30244 Krakow, Poland..
    Detailed spectral and morphological analysis of the shell type supernova remnant RCW 862018In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 612, article id A4Article in journal (Refereed)
    Abstract [en]

    Aims. We aim for an understanding of the morphological and spectral properties of the supernova remnant RCW 86 and for insights into the production mechanism leading to the RCW 86 very high-energy gamma-ray emission. Methods. We analyzed High Energy Spectroscopic System (H.E.S.S.) data that had increased sensitivity compared to the observations presented in the RCW 86 H.E.S.S. discovery publication. Studies of the morphological correlation between the 0.5-1 keV X-ray band, the 2-5 keV X-ray band, radio, and gamma-ray emissions have been performed as well as broadband modeling of the spectral energy distribution with two different emission models. Results. We present the first conclusive evidence that the TeV gamma-ray emission region is shell-like based on our morphological studies. The comparison with 2-5 keV X-ray data reveals a correlation with the 0.4-50 TeV gamma-ray emission. The spectrum of RCW 86 is best described by a power law with an exponential cutoff at E-cut = (3.5 +/- 1.2(stat)) TeV and a spectral index of Gamma approximate to 1.6 +/- 0.2. A static leptonic one-zone model adequately describes the measured spectral energy distribution of RCW 86, with the resultant total kinetic energy of the electrons above 1 GeV being equivalent to similar to 0.1% of the initial kinetic energy of a Type Ia supernova explosion (10(51) erg). When using a hadronic model, a magnetic field of B approximate to 100 mu G is needed to represent the measured data. Although this is comparable to formerly published estimates, a standard E-2 spectrum for the proton distribution cannot describe the gamma-ray data. Instead, a spectral index of Gamma(p) approximate to 1.7 would be required, which implies that similar to 7 x 10(49)/n(cm-3) erg has been transferred into high-energy protons with the effective density n(cm-3) = n/1 cm(-3). This is about 10% of the kinetic energy of a typical Type Ia supernova under the assumption of a density of 1 cm(-3).

  • 6956. Abramowski, A.
    et al.
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    Barnacka, A.
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    Tjus, J. Becker
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    Bernloehr, K.
    Birsin, E.
    Biteau, J.
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    Boisson, C.
    Bolmont, J.
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    Bregeon, J.
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    Bulik, T.
    Carrigan, S.
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    Chadwick, P. M.
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    Chalme-Calvet, R.
    Chaves, R. C. G.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, Jan
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Davids, I. D.
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    Djannati-Atai, A.
    Domainko, W.
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    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, Christian
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
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    Krueger, P. P.
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    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, Manuel
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Mitchell, A. M. W.
    Moderski, R.
    Mohamed, M.
    Morå, Knut
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Moulin, E.
    Murach, T.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Odaka, H.
    Ohm, S.
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, M.
    Quirrenbach, A.
    Raab, S.
    Reichardt, I.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    Reyes, R. de Los
    Rieger, F.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Salek, D.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spanier, F.
    Spengler, Gerrit
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    Van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Veh, J.
    Venter, C.
    Viana, A.
    Vincent, P.
    Vink, J.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Wagner, Robert M.
    Stockholm University, Faculty of Science, Department of Physics. Stockholm University, Faculty of Science, The Oskar Klein Centre for Cosmo Particle Physics (OKC).
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Yang, R.
    Zabalza, V.
    Zaborov, D.
    Zacharias, M.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    Fukui, Y.
    Sano, H.
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    Yoshiike, S.
    DISCOVERY OF THE HARD SPECTRUM VHE gamma-RAY SOURCE HESS J1641-4632014In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 794, no 1, p. L1-Article in journal (Refereed)
    Abstract [en]

    This Letter reports the discovery of a remarkably hard spectrum source, HESS J1641-463, by the High Energy Stereoscopic System (H.E.S.S.) in the very high energy (VHE) domain. HESS J1641-463 remained unnoticed by the usual analysis techniques due to confusion with the bright nearby source HESS J1640-465. It emerged at a significance level of 8.5 standard deviations after restricting the analysis to events with energies above 4 TeV. It shows a moderate flux level of phi(E > 1TeV) = (3.64 +/- 0.44(stat)+/- 0.73(sys)) x 10(-13) cm(-2) s(-1), corresponding to 1.8% of the Crab Nebula flux above the same energy, and a hard spectrum with a photon index of Gamma = 2.07 +/- 0.11(stat)+/- 0.20(sys). It is a point-like source, although an extension up to a Gaussian width of sigma = 3 arcmin cannot be discounted due to uncertainties in the H.E.S.S. point-spread function. The VHE gamma-ray flux of HESS J1641-463 is found to be constant over the observed period when checking time binnings from the year-by-year to the 28 minute exposure timescales. HESS J1641-463 is positionally coincident with the radio supernova remnant SNR G338.5+0.1. No X-ray candidate stands out as a clear association; however, Chandra and XMM-Newton data reveal some potential weak counterparts. Various VHE gamma-ray production scenarios are discussed. If the emission from HESS J1641-463 is produced by cosmic ray protons colliding with the ambient gas, then their spectrum must extend close to 1 PeV. This object may represent a source population contributing significantly to the galactic cosmic ray flux around the knee.

  • 6957.
    Abramowski, A.
    et al.
    Univ Hamburg.
    Aharonian, F.
    Max Planck Inst Kernphys, Heidelberg, Germany.
    Benkhali, F. Ait
    Max Planck Inst Kernphys, Heidelberg, Germany.
    Akhperjanian, A. G.
    Natl Acad Sci Republ Armenia.
    Uner, E. O. Ang
    Humboldt Univ.
    Backes, M.
    Univ Namibia.
    Balenderan, S.
    Univ Durham.
    Balzer, A.
    Univ Amsterdam.
    Barnacka, A.
    Uniwersytet Jagiello, Poland.
    Becherini, Yvonne
    Linnaeus University, Faculty of Technology, Department of Physics and Electrical Engineering.
    Tjus, J. Becker
    Berge, D.
    Bernhard, S.
    Bernloehr, K.
    Birsin, E.
    Biteau, J.
    Boettcher, M.
    Boisson, C.
    Bolmont, J.
    Bordas, P.
    Bregeon, J.
    Brun, F.
    Brun, P.
    Bryan, M.
    Bulik, T.
    Carrigan, S.
    Casanova, S.
    Chadwick, P. M.
    Chakraborty, N.
    Chalme-Calvet, R.
    Chaves, R. C. G.
    Chretien, M.
    Colafrancesco, S.
    Cologna, G.
    Conrad, J.
    Couturier, C.
    Cui, Y.
    Dalton, M.
    Davids, I. D.
    Degrange, B.
    Deil, C.
    deWilt, P.
    Djannati-Atai, A.
    Domainko, W.
    Donath, A.
    Drury, L. O 'C.
    Dubus, G.
    Dutson, K.
    Dyks, J.
    Dyrda, M.
    Edwards, T.
    Egberts, K.
    Eger, P.
    Espigat, P.
    Farnier, C.
    Fegan, S.
    Feinstein, F.
    Fernandes, M. V.
    Fernandez, D.
    Fiasson, A.
    Fontaine, G.
    Foerster, A.
    Fuessling, M.
    Gabici, S.
    Gajdus, M.
    Gallant, Y. A.
    Garrigoux, T.
    Giavitto, G.
    Giebels, B.
    Glicenstein, J. F.
    Gottschall, D.
    Grondin, M. -H
    Grudzinska, M.
    Hadasch, D.
    Haeffner, S.
    Hahn, J.
    Harris, J.
    Heinzelmann, G.
    Henri, G.
    Hermann, G.
    Hervet, O.
    Hillert, A.
    Hinton, J. A.
    Hofmann, W.
    Hofverberg, P.
    Holler, M.
    Horns, D.
    Ivascenko, A.
    Jacholkowska, A.
    Jahn, C.
    Jamrozy, M.
    Janiak, M.
    Jankowsky, F.
    Jung-Richardt, I.
    Kastendieck, M. A.
    Katarzynski, K.
    Katz, U.
    Kaufmann, S.
    Khelifi, B.
    Kieffer, M.
    Klepser, S.
    Klochkov, D.
    Kluzniak, W.
    Kolitzus, D.
    Komin, Nu.
    Kosack, K.
    Krakau, S.
    Krayzel, F.
    Krueger, P. P.
    Laffon, H.
    Lamanna, G.
    Lau, J.
    Lefaucheur, J.
    Lefranc, V.
    Lemiere, A.
    Lemoine-Goumard, M.
    Lenain, J. -P
    Lohse, T.
    Lopatin, A.
    Lu, C. -C
    Marandon, V.
    Marcowith, A.
    Marx, R.
    Maurin, G.
    Maxted, N.
    Mayer, M.
    McComb, T. J. L.
    Mehault, J.
    Meintjes, P. J.
    Menzler, U.
    Meyer, M.
    Mitchell, A. M. W.
    Moderski, R.
    Mohamed, M.
    Mora, K.
    Moulin, E.
    Murach, T.
    de Naurois, M.
    Niemiec, J.
    Nolan, S. J.
    Oakes, L.
    Odaka, H.
    Ohm, S.
    Opitz, B.
    Ostrowski, M.
    Oya, I.
    Panter, M.
    Parsons, R. D.
    Arribas, M. Paz
    Pekeur, N. W.
    Pelletier, G.
    Petrucci, P. -O
    Peyaud, B.
    Pita, S.
    Poon, H.
    Puehlhofer, G.
    Punch, Michael
    Univ Paris Diderot, APC, AstroParticule & Cosmology, CNRS,IN2P3,CEA,Irfu, Observ Paris,Sorbonne Paris C, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France.
    Quirrenbach, A.
    Raab, S.
    Reichardt, I.
    Reimer, A.
    Reimer, O.
    Renaud, M.
    Reyes, R. de Los
    Rieger, F.
    Romoli, C.
    Rosier-Lees, S.
    Rowell, G.
    Rudak, B.
    Rulten, C. B.
    Sahakian, V.
    Salek, D.
    Sanchez, D. A.
    Santangelo, A.
    Schlickeiser, R.
    Schuessler, F.
    Schulz, A.
    Schwanke, U.
    Schwarzburg, S.
    Schwemmer, S.
    Sol, H.
    Spanier, F.
    Spengler, G.
    Spies, F.
    Stawarz, L.
    Steenkamp, R.
    Stegmann, C.
    Stinzing, F.
    Stycz, K.
    Sushch, I.
    Tavernet, J. -P
    Tavernier, T.
    Taylor, A. M.
    Terrier, R.
    Tluczykont, M.
    Trichard, C.
    Valerius, K.
    Van Eldik, C.
    van Soelen, B.
    Vasileiadis, G.
    Veh, J.
    Venter, C.
    Viana, A.
    Vincent, P.
    Vink, J.
    Voelk, H. J.
    Volpe, F.
    Vorster, M.
    Vuillaume, T.
    Wagner, S. J.
    Wagner, P.
    Wagner, R. M.
    Ward, M.
    Weidinger, M.
    Weitzel, Q.
    White, R.
    Wierzcholska, A.
    Willmann, P.
    Woernlein, A.
    Wouters, D.
    Yang, R.
    Zabalza, V.
    Zaborov, D.
    Zacharias, M.
    Zdziarski, A. A.
    Zech, A.
    Zechlin, H. -S
    Fukui, Y.
    Sano, H.
    Fukuda, T.
    Yoshiike, S.
    Discovery of the Hard Spectrum VHE γ-Ray Source HESS J1641–4632014In: Astrophysical Journal Letters, ISSN 2041-8205, E-ISSN 2041-8213, Vol. 794, no 1, p. Article ID: L1-Article in journal (Refereed)
    Abstract [en]

    This Letter reports the discovery of a remarkably hard spectrum source, HESS J1641-463, by the High Energy Stereoscopic System (H.E.S.S.) in the very high energy (VHE) domain. HESS J1641-463 remained unnoticed by the usual analysis techniques due to confusion with the bright nearby source HESS J1640-465. It emerged at a significance level of 8.5 standard deviations after restricting the analysis to events with energies above 4 TeV. It shows a moderate flux level of phi(E > 1TeV) = (3.64 +/- 0.44(stat)+/- 0.73(sys)) x 10(-13) cm(-2) s(-1), corresponding to 1.8% of the Crab Nebula flux above the same energy, and a hard spectrum with a photon index of Gamma = 2.07 +/- 0.11(stat)+/- 0.20(sys). It is a point-like source, although an extension up to a Gaussian width of sigma = 3 arcmin cannot be discounted due to uncertainties in the H.E.S.S. point-spread function. The VHE gamma-ray flux of HESS J1641-463 is found to be constant over the observed period when checking time binnings from the year-by-year to the 28 minute exposure timescales. HESS J1641-463 is positionally coincident with the radio supernova remnant SNR G338.5+0.1. No X-ray candidate stands out as a clear association; however, Chandra and XMM-Newton data reveal some potential weak counterparts. Various VHE gamma-ray production scenarios are discussed. If the emission from HESS J1641-463 is produced by cosmic ray protons colliding with the ambient gas, then their spectrum must extend close to 1 PeV. This object may represent a source population contributing significantly to the galactic cosmic ray flux around the knee.

  • 6958. Abramowski, A.
    et al.
    Conrad, Jan
    Dickinson, Hugh
    Ripken, Joachim
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Zechlin, H-S
    et al.,
    HESS OBSERVATIONS OF THE GLOBULAR CLUSTERS NGC 6388 AND M15 AND SEARCH FOR A DARK MATTER SIGNAL2011In: Astrophysical Journal, ISSN 0004-637X, E-ISSN 1538-4357, Vol. 735, no 1Article in journal (Refereed)
    Abstract [en]

    Observations of the globular clusters (GCs) NGC 6388 and M15 were carried out by the High Energy Stereoscopic System array of Cherenkov telescopes for a live time of 27.2 and 15.2 hr, respectively. No gamma-ray signal is found at the nominal target position of NGC 6388 and M15. In the primordial formation scenario, GCs are formed in a dark matter (DM) halo and DM could still be present in the baryon-dominated environment of GCs. This opens the possibility of observing a DM self-annihilation signal. The DM content of the GCs NGC 6388 and M15 is modeled taking into account the astrophysical processes that can be expected to influence the DM distribution during the evolution of the GC: the adiabatic contraction of DM by baryons, the adiabatic growth of a black hole in the DM halo, and the kinetic heating of DM by stars. Ninety-five percent confidence level exclusion limits on the DM particle velocity-weighted annihilation cross section are derived for these DM halos. In the TeV range, the limits on the velocity-weighted annihilation cross section are derived at the 10(-25) cm(3) s(-1) level and a few 10(-24) cm(3) s(-1) for NGC 6388 and M15, respectively.

  • 6959. Abramowski, A.
    et al.
    Jacholkowska, A.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    et al.,
    Search for Lorentz Invariance breaking with a likelihood fit of the PKS 2155-304 flare data taken on MJD 539442011In: Astroparticle physics, ISSN 0927-6505, E-ISSN 1873-2852, Vol. 34, no 9, p. 738-747Article in journal (Refereed)
    Abstract [en]

    Several models of Quantum Gravity predict Lorentz Symmetry breaking at energy scales approaching the Planck scale (similar to 10(19) GeV). With present photon data from the observations of distant astrophysical sources, it is possible to constrain the Lorentz Symmetry breaking linear term in the standard photon dispersion relations. Gamma Ray Bursts (GRB) and flaring Active Galactic Nuclei (AGN) are complementary to each other for this purpose, since they are observed at different distances in different energy ranges and with different levels of variability. Following a previous publication of the High Energy Stereoscopic System (H.E.S.S.) collaboration [1], a more sensitive event-by-event method consisting of a likelihood fit is applied to PKS 2155-304 flare data of MJD 53944 (July 28, 2006) as used in the previous publication. The previous limit on the linear term is improved by a factor of similar to 3 up to M-QG(1), > 2.1 X 10(1B) GeV and is currently the best result obtained with blazars. The sensitivity to the quadratic term is lower and provides a limit of M-QG(q) > 6.4 x 10(10) GeV, which is the best value obtained so far with an AGN and similar to the best limits obtained with GRB.

  • 6960. Abramowski, A.
    et al.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    et. al.,
    HESS J1943+213: a candidate extreme BL Lacertae object2011In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 529, no A49Article in journal (Refereed)
    Abstract [en]

    ontext. The H.E.S.S. Cherenkov telescope array has been surveying the Galactic plane for new VHE (>100 GeV) gamma-ray sources.

    Aims. We report on a newly detected point-like source, HESS J1943+213. This source coincides with an unidentified hard X-ray source IGR J19443+2117, which was proposed to have radio and infrared counterparts.

    Methods. We combine new H.E.S.S., Fermi/LAT and Nançay Radio Telescope observations with pre-existing non-simultaneous multi-wavelength observations of IGR J19443+2117 and discuss the likely source associations as well as the interpretation as an active galactic nucleus, a gamma-ray binary or a pulsar wind nebula.

    Results. HESS J1943+213 is detected at the significance level of 7.9σ (post-trials) at RA(J2000) = , Dec(J2000) = . The source has a soft spectrum with photon index Γ = 3.1 ± 0.3stat ± 0.2sys and a flux above 470 GeV of (1.3 ± 0.2stat ± 0.3sys) × 10-12 cm-2 s-1. There is no Fermi/LAT counterpart down to a flux limit of 6 × 10-9 cm-2 s-1 in the 0.1–100 GeV energy range (95% confidence upper limit calculated for an assumed power-law model with a photon index Γ = 2.0). The data from radio to VHE gamma-rays do not show any significant variability.

    Conclusions. The lack of a massive stellar counterpart disfavors the binary hypothesis, while the soft VHE spectrum would be very unusual in case of a pulsar wind nebula. In addition, the distance estimates for Galactic counterparts places them outside of the Milky Way. All available observations favor an interpretation as an extreme, high-frequency peaked BL Lac object with a redshift z > 0.14. This would be the first time a blazar is detected serendipitously from ground-based VHE observations, and the first VHE AGN detected in the Galactic Plane.

  • 6961. Abramowski, A.
    et al.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    HESS Collaboration,
    et. al.,
    VHE gamma-ray emission of PKS 2155-304: spectral and temporal variability2010In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 520, p. A83-Article in journal (Refereed)
    Abstract [en]

    Context. Observations of very high-energy.-rays from blazars provide information about acceleration mechanisms occurring in their innermost regions. Studies of variability in these objects lead to a better understanding of the mechanisms in play.

    Aims. To investigate the spectral and temporal variability of VHE (>100 GeV) gamma-rays of the well-known high-frequency-peaked BL Lac object PKS 2155-304 with the HESS imaging atmospheric Cherenkov telescopes over a wide range of flux states.

    Methods. Data collected from 2005 to 2007 were analyzed. Spectra were derived on time scales ranging from 3 years to 4 min. Light curve variability was studied through doubling timescales and structure functions and compared with red noise process simulations.

    Results. The source was found to be in a low state from 2005 to 2007, except for a set of exceptional flares that occurred in July 2006. The quiescent state of the source is characterized by an associated mean flux level of (4.32 +/- 0.09(stat) +/- 0.86(syst)) x 10(-11) cm(-2) s(-1) above 200 GeV, or approximately 15% of the Crab Nebula, and a power-law photon index of Gamma = 3.53 +/- 0.06(stat) +/- 0.10(syst). During the flares of July 2006, doubling timescales of similar to 2 min are found. The spectral index variation is examined over two orders of magnitude in flux, yielding different behavior at low and high fluxes, which is a new phenomenon in VHE gamma-ray emitting blazars. The variability amplitude characterized by the fractional rms F-var is strongly energy-dependent and is proportional to E-0.19 +/- 0.01. The light curve rms correlates with the flux. This is the signature of a multiplicative process that can be accounted for as a red noise with a Fourier index of similar to 2.

    Conclusions. This unique data set shows evidence of a low-level.-ray emission state from PKS 2155-304 that possibly has a different origin than the outbursts. The discovery of the light curve ognormal behavior might be an indicator of the origin of aperiodic variability in blazars.

  • 6962. Abramowski, A
    et al.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Kawamura, A.
    et. al.,
    Revisiting the Westerlund 2 field with the HESS telescope array2011In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 525, p. A46-Article in journal (Refereed)
    Abstract [en]

    Aims. Previous observations with the HESS telescope array revealed the existence of extended very-high-energy (VHE; E > 100 GeV) gamma-ray emission, HESS J1023-575, coincident with the young stellar cluster Westerlund 2. At the time of discovery, the origin of the observed emission was not unambiguously identified, and follow-up observations have been performed to further investigate the nature of this gamma-ray source. Methods. The Carina region towards the open cluster Westerlund 2 has been re-observed, increasing the total exposure to 45.9 h. The combined dataset includes 33 h of new data and now permits a search for energy-dependent morphology and detailed spectroscopy. Results. A new, hard spectrum VHE gamma-ray source, HESS J1026-582, was discovered with a statistical significance of 7 sigma. It is positionally coincident with the Fermi LAT pulsar PSRJ1028-5819. The positional coincidence and radio/gamma-ray characteristics of the LAT pulsar favors a scenario where the TeV emission originates from a pulsar wind nebula. The nature of HESS J1023-575 is discussed in light of the deep HESS observations and recent multi-wavelength discoveries, including the Fermi LAT pulsar PSRJ1022-5746 and giant molecular clouds in the region. Despite the improved VHE dataset, a clear identification of the object responsible for the VHE emission from HESS J1023-575 is not yet possible, and contribution from the nearby high-energy pulsar and/or the open cluster remains a possibility.

  • 6963. Abramowski, A.
    et al.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Zechlin, H. -S.
    et al.,
    A new SNR with TeV shell-type morphology: HESS J1731-3472011In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 531, p. A81-Article in journal (Refereed)
    Abstract [en]

    Aims. The recent discovery of the radio shell-type supernova remnant (SNR), G353.6-0.7, in spatial coincidence with the unidentified TeV source HESS J1731-347 has motivated further observations of the source with the High Energy Stereoscopic System (HESS) Cherenkov telescope array to test a possible association of the gamma-ray emission with the SNR.

    Methods. With a total of 59 h of observation, representing about four times the initial exposure available in the discovery paper of HESS J1731-347, the gamma-ray morphology is investigated and compared with the radio morphology. An estimate of the distance is derived by comparing the interstellar absorption derived from X-rays and the one obtained from (12)CO and HI observations.

    Results. The deeper gamma-ray observation of the source has revealed a large shell-type structure with similar position and extension (r similar to 0.25 degrees) as the radio SNR, thus confirming their association. By accounting for the HESS angular resolution and projection effects within a simple shell model, the radial profile is compatible with a thin, spatially unresolved, rim. Together with RX J1713.7-3946, RX J0852.0-4622 and SN 1006, HESS J1731-347 is now the fourth SNR with a significant shell morphology at TeV energies. The derived lower limit on the distance of the SNR of 3.2 kpc is used together with radio and X-ray data to discuss the possible origin of the gamma-ray emission, either via inverse Compton scattering of electrons or the decay of neutral pions resulting from proton-proton interaction.

  • 6964. Abramowski, A.
    et al.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Zechlin, H. -S.
    et al.,
    HESS constraints on dark matter annihilations towards the sculptor and carina dwarf galaxies2011In: Astroparticle physics, ISSN 0927-6505, E-ISSN 1873-2852, Vol. 34, no 8, p. 608-616Article in journal (Refereed)
    Abstract [en]

    The Sculptor and Carina dwarf spheroidal galaxies were observed with the H.E.S.S. Cherenkov telescope array between January 2008 and December 2009. The data sets consist of a total of 11.8 h and 14.811 of high quality data, respectively. No gamma-ray signal was detected at the nominal positions of these galaxies above 220 GeV and 320 GeV, respectively. Upper limits on the gamma-ray fluxes at 95% CL assuming two forms for the spectral energy distribution (a power law shape and one derived from dark matter annihilation) are obtained at the level of 10(-13)-10(-12) cm(-2) s(-1) in the TeV range. Constraints on the velocity weighted dark matter particle annihilation cross section for both Sculptor and Carina dwarf galaxies range from <sigma v > 10(-21) cm(3) s(-1) down to <sigma v > similar to 10(-2)2 cm(3) s(-1) on the dark matter halo model used. Possible enhancements of the gamma-ray flux are studied: the Sommerfeld effect, which is found to exclude some dark matter particle masses, the internal Bremsstrahlung and clumps in the dark-matter halo distributions.

  • 6965. Abramowski, A.
    et al.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Zechlin, H-S.
    et al.,
    Very-high-energy gamma-ray emission from the direction of the Galactic globular cluster Terzan 52011In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 531, p. L18-Article in journal (Refereed)
    Abstract [en]

    The HESS very-high-energy (VHE, E > 0.1 TeV) gamma-ray telescope system has discovered a new source, HESS J1747-248. The measured integral flux is (1.2 +/- 0.3) x 10(-12) cm(-2) s(-1) above 440 GeV for a power-law photon spectral index of 2.5 +/- 0.3(stat) +/- 0.2(sys). The VHE gamma-ray source is located in the close vicinity of the Galactic globular cluster Terzan 5 and extends beyond the HESS point spread function (0.07 degrees). The probability of a chance coincidence with Terzan 5 and an unrelated VHE source is quite low (similar to 10(-4)). With the largest population of identified millisecond pulsars (msPSRs), a very high core stellar density and the brightest GeV range flux as measured by Fermi-LAT, Terzan 5 stands out among Galactic globular clusters. The properties of the VHE source are briefly discussed in the context of potential emission mechanisms, notably in relation to msPSRs. Interpretation of the available data accommodates several possible origins for this VHE gamma-ray source, although none of them offers a satisfying explanation of its peculiar morphology.

  • 6966. Abramowski, A.
    et al.
    Ryde, Felix
    KTH, School of Engineering Sciences (SCI), Physics, Particle and Astroparticle Physics.
    Ziegler, M.
    et al.,
    Simultaneous multi-wavelength campaign on PKS 2005-489 in a high state2011In: Astronomy and Astrophysics, ISSN 0004-6361, E-ISSN 1432-0746, Vol. 533, p. A110-Article in journal (Refereed)
    Abstract [en]

    The high-frequency peaked BL Lac object PKS 2005-489 was the target of a multi-wavelength campaign with simultaneous observations in the TeV gamma-ray (H.E.S.S.), GeV gamma-ray (Fermi/LAT), X-ray (RXTE, Swift), UV (Swift) and optical (ATOM, Swift) bands. This campaign was carried out during a high flux state in the synchrotron regime. The flux in the optical and X-ray bands reached the level of the historical maxima. The hard GeV spectrum observed with Fermi/LAT connects well to the very high energy (VHE, E > 100 GeV) spectrum measured with H.E.S.S. with a peak energy between similar to 5 and 500 GeV. Compared to observations with contemporaneous coverage in the VHE and X-ray bands in 2004, the X-ray flux was similar to 50 times higher during the 2009 campaign while the TeV gamma-ray flux shows marginal variation over the years. The spectral energy distribution during this multi-wavelength campaign was fit by a one zone synchrotron self-Compton model with a well determined cutoff in X-rays. The parameters of a one zone SSC model are inconsistent with variability time scales. The variability behaviour over years with the large changes in synchrotron emission and small changes in the inverse Compton emission does not warrant an interpretation within a one-zone SSC model despite an apparently satisfying fit to the broadband data in 2009.

  • 6967. Abrams, P
    et al.
    Cardozo, L
    Fall, M
    Griffiths, D
    Rosier, P
    Ulmsten, U
    Uppsala University, Medicinska vetenskapsområdet, Faculty of Medicine, Department of Women's and Children's Health.
    Van Kerrebroeck, P
    Victor, A
    Wein, A
    The standardisation of terminology in lower urinary tract function: reportfrom the standardisation sub-committee of the International ContinenceSociety.2003In: Urology, Vol. 61, p. 37-Article in journal (Refereed)
  • 6968. Abrams, P
    et al.
    Cardozo, L
    Fall, M
    Griffiths, D
    Rosier, P
    Ulmsten, U
    Uppsala University, Medicinska vetenskapsområdet, Faculty of Medicine, Department of Women's and Children's Health.
    van Kerrebroeck, P
    Victor, A
    Wein, A
    The standardisation of terminology of lower urinary tract function: Report from the standardistation sub-committee of the International Continence Society.2002In: Neurourology and Urodynamics, Vol. 21, p. 167-Article in journal (Refereed)
  • 6969. Abrams, Pascale
    et al.
    Boquete, Hugo
    Fideleff, Hugo
    Feldt-Rasmussen, Ulla
    Jonsson, J
    Koltowska-Häggström, Maria
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Pharmacy, Department of Pharmacy.
    Wilton, Patrick
    Abs, Roger
    GH replacement in hypopituitarism improves lipid profile and quality of life independently of changes in obesity variables2008In: European Journal of Endocrinology, ISSN 0804-4643, E-ISSN 1479-683X, Vol. 159, no 6, p. 825-832Article in journal (Refereed)
    Abstract [en]

    Objective: GH deficiency (GHD) in adults is characterized by elevated body mass index (BMI), increased waist girth (WG) and increased fat mass (FM). Information about how these indicators of obesity affect the lipid profile and quality of life (QoL) of GHD subjects is scarce. It is also unclear how changes in these indicators brought about by GH replacement influence lipids and QoL. Design and methods: Adult GHD Subjects from the Pfizer International Metabolic Database were grouped according to BMI (n = 291 with BMI < 25 kg/m(2), n = 372 with BMI 25-30 kg/m(2), n = 279 with BMI > 30 kg/m(2)), WG (n = 508 with normal WG, n = 434 with increased WG) and FM (n = 357) and according to changes in these variables after 1 year of GH replacement. Serum IGF-1 concentrations, lipid concentrations and QoL using the QoL Assessment of GHD in Adults questionnaire were assessed at baseline and after 1 year of treatment. Results: At baseline, total and low-density lipoprotein (LDL) cholesterol were similarly elevated in the BMI and WG groups, but high-density lipoprotein (HDL) cholesterol decreased and triglycerides increased with increasing BMI and WG. QoL was progressively poorer with increasing BMI and WG. After 1 year of GH replacement, total and LDL cholesterol and QoL improved in all BMI, WG and FM groups. Conclusions: Variables of obesity adversely affect the already unfavourable lipid profile in GHD Subjects by decreasing HDL cholesterol, but do not counteract the positive effect of GH replacement on LDL cholesterol. Similarly, QoL is influenced by obesity, but responds equally well to GH treatment independent of BMI, WG and FM.

  • 6970.
    Abramson, Jeff
    Uppsala University, Teknisk-naturvetenskapliga vetenskapsområdet, Chemistry, Department of Biochemistry.
    Structural studies on the integral membrane protein, ubiquinol oxidase from Escherichia coli2001Doctoral thesis, comprehensive summary (Other academic)
    Abstract [en]

    Heme-copper oxidases are redox-driven proton pumps that couple the reduction of molecular oxygen to water with the vectorial translocation of protons across the membrane. The proton gradient generated by heme-copper oxidases and the other members of the aerobic respiratory chain is ultimately used to drive the synthesis of ATP. There are two main branches of the heme-copper oxidases that are characterized by the electron donating substrate; the cytochrome c oxidases, which use cytochrome c as the electron donor, and the ubiquinol oxidases, which use a lipid-soluble molecule, ubiquinol, as their electron donor. These enzymes share important structural and functional features.

    This thesis presents the procedures that have led to the first crystal structure of a ubiquinol oxidase, cytochrome bo, oxidase from Escherichia coli, at a resolution of 3.5 Å. The overall structure of the enzyme is similar to those of cytochrome c oxidases; however the membrane spanning region of subunit I contains a cluster of polar residues exposed to the interior of the lipid bilayer. No such structural feature is present in cytochrome c oxidases. Mutagenesis studies on residues in this region strongly suggest that this area forms a ubiquinone binding site. A comparison of this region with known ubiquinone binding sites shows remarkable similarities. In light of these findings specific roles for these polar residues is proposed in electron and proton transfer in ubiquinol oxidase.

    A fusion protein of cytochrome bo3-Protein Z was generated in an attempt to increase the hydrophilic surface of the protein, thus extending protein-protein contacts within the crystal lattice structure. Such an approach can be used to facilitate crystallization.

  • 6971.
    Abramson, Jonas
    et al.
    Halmstad University, School of Business and Engineering (SET).
    Andersson, Magnus
    Halmstad University, School of Business and Engineering (SET).
    Examensarbete Sko- och vagntvätt2006Independent thesis Basic level (degree of Bachelor)Student thesis
    Abstract [sv]
    Range Servant som är ett företag som tillverkar olika typer av golfprodukter har gett oss i uppdrag att ta fram en förbättrad modell av deras luftrengörings enhet. Den nuvarande används av golfare för att blåsa av gräs och annan smuts som har kommit på kläder, skor och vagn. Den skall användas i första hand innan man går in i lokaler vid golfbanan som t. ex klubbhus eller restauranger. Smutsen skall samlas upp i en låda som är lätt att tömma. Produkten ska bestå av två moduler så att man kan anpassa den efter kundens behov. Huvuddelen består av en fot tvätt som vid behov kan byggas på med ett vagnsdel. Detta för att man ska kunna samla upp gräset även från vagnen. Vi har gjort 8 st. principförslag som företaget har gått igenom tillsammans med marknadsavdelning och konstruktörer. De har även visat den för kunder och har därefter bestämt sig för vilken vi skall fortsätta med.
  • 6972. Abramson, N. I.
    Lemmings of Palaearctic tundra (morphological variation, distribution patterns, taxonomy and zoogeography)1995In: Swedish-Russian Tundra Ecology-expedition-94. Tundra Ecology-94. A Cruise Report, Stockholm: Swedish Polar Research Secretariat , 1995, , p. 111-117Chapter in book (Other academic)
  • 6973. Abramson, Nataliya
    Morphometric variation in true lemmings (Lemmus) from the Eurasian Arctic1999In: Ambio, Vol. 28, no 3, p. 256-260Article in journal (Refereed)
  • 6974.
    Abramson, Nils
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering, Metrology and Optics.
    Article may have left false impression that light-in-flight method is new2008In: Laser Focus World, ISSN 1043-8092, Vol. 44, no 4, p. 10-10Article in journal (Other academic)
  • 6975.
    Abramson, Nils
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering, Metrology and Optics.
    FEMTOSECOND IMAGING Motion picture of short pulses2011In: Nature Photonics, ISSN 1749-4885, E-ISSN 1749-4893, Vol. 5, no 7, p. 389-390Article in journal (Refereed)
  • 6976.
    Abramson, Nils
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering.
    Holography, relativity and the spooky ellipsoids2006In: Proceedings of the 7th International Symposium on Display Holography: Advances In Display Holography / [ed] Bjelkhagen, HI, 2006, p. 228-235Conference paper (Refereed)
    Abstract [en]

    The further away from a house we move, the smaller it appears. We could say that we are in the centre of a "sphere of observation", which must reach the house before we can see it. The larger that sphere is, the smaller the house appears. This is natural to us and not difficult to understand. In Einstein's Special Relativity it is stated that the faster we move past a house, the shorter it appears. We state in this paper that this is because the faster we travel, the more our "sphere of observation" is elongated into an "ellipsoid of observation". The longer that ellipsoid is, the shorter the house appears. This contraction is not so natural to us, because to be observable the velocity has to be extremely high, almost close to the velocity of light. A similar phenomenon can, however, be studied when holography with ultrashort pulses is used for measurement. In this case the sphere of observation is also transformed into an ellipsoid of observation. Thus, according to our approach objects appear shorter because the definition of length (the metre) becomes longer, just as time moves slower because the definition of time (the second) becomes longer. The transformation of the sphere into an ellipsoid is however hidden to the observer both in the case of holography and in relativity. This spooky behaviour of the ellipsoid has resulted in a new mathematical theorem.

  • 6977.
    Abramson, Nils
    et al.
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering.
    Boman, J.
    Bonnevier, Björn
    KTH, School of Electrical Engineering (EES), Centres, Alfvén Laboratory Centre for Space and Fusion Plasma Physics.
    Plane intersections of rotational ellipsoids2006In: The American mathematical monthly, ISSN 0002-9890, E-ISSN 1930-0972, Vol. 113, no 4, p. 336-339Article in journal (Refereed)
  • 6978.
    Abramson, Nils H.
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering, Metrology and Optics.
    Appearance of Objects at Relativistic Velocities, a Holographic Approach2010In: SEARCH FOR FUNDAMENTAL THEORY / [ed] Amoroso RL, Rowlands P, Jeffers S, MELVILLE, NY: AMER INST PHYSICS , 2010, Vol. 1316, p. 118-124Conference paper (Refereed)
    Abstract [en]

    A diagram borrowed from holographic interferometry has been applied to visualize phenomena in Special Relativity. It displays how a sphere of observation is by velocity elongated into an ellipsoid of observation and produces graphically all the well accepted equations of Einsteins Special Relativity. The Lorentz contraction, however, is explained as an elongation of the measuring rod, the meter, which by definition is based on either a specific number of wavelengths or the velocity of light multiplied by time. The diagram displays the total apparent object distortions including not only the Lorentz contraction but also larger apparent contractions and elongations caused by the classic Doppler Effect. The reasons of these deformations are the delays caused by variations in distance from observer to different parts of the moving object. In this paper we do not discuss the meaning of apparent, as compared to real, deformation.

  • 6979.
    Abramson, Nils H.
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering.
    Elliptic visualizing optical resolution and kinetic energy2017In: Applied Optics, ISSN 1559-128X, E-ISSN 2155-3165, Vol. 56, no 5, p. 1413-1416Article in journal (Refereed)
    Abstract [en]

    Diffraction limited resolution as introduced by Abbe is well established, but interference limited resolution was not well known until holographic interferometry was introduced. The holodiagram is used to simplify holography and in a new way visualize the distribution, ratio, and relation among resolutions of different optical techniques, including relativistic phenomena. Resolution, when measured by optical methods based on the number of wavelengths of light, is defined in the following as the minimum distance between resolvable points, or the largest object needed to be resolved. Everywhere in the diagram this resolution is represented by two orthogonal diagonals of rhombs.

  • 6980.
    Abramson, Nils H.
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering, Metrology and Optics.
    Holodiagram: elliptic visualizing interferometry, relativity, and light-in-flight2014In: Applied Optics, ISSN 1559-128X, E-ISSN 2155-3165, Vol. 53, no 11, p. 2398-2404Article in journal (Refereed)
    Abstract [en]

    In holographic interferometry, there is usually a static distance separating the point of illumination and the point of observation. In Special Relativity, this separation is dynamic and is caused by the velocity of the observer. The corrections needed to compensate for these separations are similar in the two fields. We use the ellipsoids of the holodiagram for measurement and in a graphic way to explain and evaluate optical resolution, gated viewing, radar, holography, three-dimensional interferometry, Special Relativity, and light-in-flight recordings. Lorentz contraction together with time dilation is explained as the result of the eccentricity of the measuring ellipsoid, caused by its velocity. The extremely thin ellipsoid of the very first light appears as a beam aimed directly at the observer, which might explain the wave or ray duality of light and entanglement. Finally, we introduce the concept of ellipsoids of observation.

  • 6981.
    Abramson, Nils H.
    KTH, School of Industrial Engineering and Management (ITM).
    Holographic Metrology and Basic Physics2013In: Journal of Physics, Conference Series, ISSN 1742-6588, E-ISSN 1742-6596, Vol. 415, no 1, p. 012030-Article in journal (Refereed)
    Abstract [en]

    A short pulse of light is emitted from one point followed by a short observation from another point separated in space and time from the first. Even if space is full of scattering particles no sphere of expanding light is seen from outside by the observer, instead he finds himself inside an ellipsoid of light. We use this ellipsoid for measurement and in a graphic way to explain and evaluate optical resolution, gated viewing, radar, holography, 3-D interferometry and Special Relativity. In the later case the Lorentz Contraction together with the Time Dilation are explained as results of the eccentricity of the measuring ellipsoid, caused by its velocity. Finally, the extremely thin ellipsoid of the very first light appears as a beam aimed directly at the observer which might explain the wave or ray duality of light and entanglement.

  • 6982.
    Abramson, Nils H.
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering, Metrology and Optics.
    INSTANT RANDOM INFORMATION2010In: SEARCH FOR FUNDAMENTAL THEORY / [ed] Amoroso RL, Rowlands P, Jeffers S, MELVILLE, NY: AMER INST PHYSICS , 2010, Vol. 1316, p. 113-117Conference paper (Refereed)
    Abstract [en]

    Information is carried by matter or by energy and thus Einstein stated that "no information can travel faster than light." He also was very critical to the "Spooky action at distance" as described in Quantum Physics. However, many verified experiments have proven that the "Spooky actions" not only work at distance but also that they travel at a velocity faster than light, probably at infinite velocity. Examples are Young's fringes at low light levels or entanglements. My explanation is that this information is without energy. In the following I will refer to this spooky information as exformation, where "ex-" refers to existence, the information is not transported in any way, it simply exists. Thus Einstein might have been wrong when he stated that no information can travel faster than light. But he was is right in that no detectable information can travel faster than light. Phenomena connected to entanglement appear at first to be exceptions, but in those cases the information can not be reconstructed until energy is later sent in the form of correlation using ordinary information at the velocity of light. In entanglement we see that even if the exformation can not be detected directly because its luck of energy it still can influence what happens at random, bemuse in Quantum Physics there is by definition no energy difference between two states that happen randomly.

  • 6983.
    Abramson, Nils H.
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering.
    Lorentz contraction, apparent or real2013In: Progress In Electromagnetics Research Symposium Proceedings, Stockholm, Sweden, Aug. 12-15, 2013, 2013, p. 1547-1549Conference paper (Refereed)
    Abstract [en]

    The Michelson Morley interference experiment of 1887 indicated that the velocity of light is independent of the velocities of source and observer. This surprising result was in conflict with earlier calculations. To make theory and experiment in agreement Lorentz stated a contraction of rigid objects parallel to velocity. We discuss if this contraction is real or caused by the interference method of measurement. Our approach is to introduce a sphere of observation based on ultra short light pulses combined to ultra short observations. When the experimenter travels at high velocity this sphere is according to Lorentz contracted into an oblate ellipsoid. According to our proposed theory the sphere is instead elongated into a prolate ellipsoid. The result of this effect is that stationary objects appear contracted. Our results are in full agreement to Einsteins Special Theory of Relativity. To support our statements we introduce a novel method to measure the length of a travelling object that is independent of interferometry.

  • 6984.
    Abramson, Nils H.
    KTH, School of Industrial Engineering and Management (ITM), Production Engineering, Metrology and Optics.
    Optical resolution and the duality of light2008In: Applied Optics, ISSN 1559-128X, E-ISSN 2155-3165, Vol. 47, no 19, p. D1-D5Article in journal (Refereed)
    Abstract [en]

    For 15 years, lensless microscopes have been constructed based on the use of holography, a digital CCD detector, and a computer for image reconstruction by use of, e.g., Fourier transformation. Thus, no lens is involved and therefore the conventional resolution limit of half the wavelength no longer applies. Instead of being limited by the wavelength, the resolution is in this case limited by how exact one can measure the phases of the light. It is remarkable that the interference-limited resolution is approximately 0.01X, whereas the diffraction-limited resolution is only of the order of 0.5X. It is my hope that by combining these two techniques it will be possible to increase the magnification in optical systems by at least an order of magnitude. The calculations at so indicate that information does not necessarily decrease with distance.

  • 6985.
    Abramson, Norman
    et al.
    Department of Electrical Engineering, University of Hawaii, USA.
    Sacchi, Claudio
    Information Engineering and Computer Science Department, University of Trento, Italy.
    Bellalta, Boris
    Department of Information and Communication Technologies, Universitat Pompeu Fabra, Spain.
    Vinel, Alexey
    Saint-Petersburg Institute for Informatics and Automation, Russian Academy of Sciences, Russia.
    Multiple access communications in future-generation wireless networks2012In: EURASIP Journal on Wireless Communications and Networking, ISSN 1687-1472, E-ISSN 1687-1499, p. Art nr 45-Article in journal (Refereed)
  • 6986.
    Abramson, Alex
    et al.
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA..
    Caffarel-Salvador, Ester
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA.;MIT, Inst Med Engn & Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA..
    Khang, Minsoo
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA..
    Dellal, David
    MIT, Inst Med Engn & Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA..
    Silverstein, David
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA..
    Gao, Yuan
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA..
    Frederiksen, Morten Revsgaard
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Vegge, Andreas
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Hubalek, Frantisek
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Water, Jorrit J.
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Friderichsen, Anders V.
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Fels, Johannes
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Kirk, Rikke Kaae
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Cleveland, Cody
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA.;Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Collins, Joy
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA..
    Tamang, Siddartha
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA..
    Hayward, Alison
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA.;MIT, Div Comparat Med, Cambridge, MA 02139 USA..
    Landh, Tomas
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Buckley, Stephen T.
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Roxhed, Niclas
    KTH, School of Electrical Engineering and Computer Science (EECS), Micro and Nanosystems.
    Rahbek, Ulrik
    Novo Nordisk AS, Global Res Technol, Global Drug Discovery & Device R&D, Copenhagen, Denmark..
    Langer, Robert
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA.;MIT, Inst Med Engn & Sci, 77 Massachusetts Ave, Cambridge, MA 02139 USA.;MIT, Media Lab, Cambridge, MA 02139 USA..
    Traverso, Giovanni
    MIT, Dept Chem Engn, Cambridge, MA 02139 USA.;MIT, David H Koch Inst Integrat Canc Res, Cambridge, MA 02139 USA.;MIT, Dept Mech Engn, Cambridge, MA 02139 USA.;Harvard Med Sch, Brigham & Womens Hosp, Div Gastroenterol, Boston, MA 02115 USA..
    An ingestible self-orienting system for oral delivery of macromolecules2019In: Science, ISSN 0036-8075, E-ISSN 1095-9203, Vol. 363, no 6427, p. 611-+Article in journal (Refereed)
    Abstract [en]

    Biomacromolecules have transformed our capacity to effectively treat diseases; however, their rapid degradation and poor absorption in the gastrointestinal (GI) tract generally limit their administration to parenteral routes. An oral biologic delivery system must aid in both localization and permeation to achieve systemic drug uptake. Inspired by the leopard tortoise's ability to passively reorient, we developed an ingestible self-orienting millimeter-scale applicator (SOMA) that autonomously positions itself to engage with GI tissue. It then deploys milliposts fabricated from active pharmaceutical ingredients directly through the gastric mucosa while avoiding perforation. We conducted in vivo studies in rats and swine that support the applicator's safety and, using insulin as a model drug, demonstrated that the SOMA delivers active pharmaceutical ingredient plasma levels comparable to those achieved with subcutaneous millipost administration.

  • 6987.
    Abramsson, Alexander
    et al.
    Örebro University, Örebro University School of Business.
    Happonen, Anna
    Örebro University, Örebro University School of Business.
    Malmsten, Dennis
    Örebro University, Örebro University School of Business.
    Aktieindexobligationer: En studie om struktur och prissättning av produkter på den svenska marknaden2013Independent thesis Basic level (degree of Bachelor), 10 credits / 15 HE creditsStudent thesis
  • 6988. Abramsson, Alexandra
    et al.
    Kurup, Sindhulakshmi
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Medical Biochemistry and Microbiology.
    Yamada, Shuhei
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Medical Biochemistry and Microbiology.
    Lindblom, Per
    Schallmeiner, Edith
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Genetics and Pathology.
    Ledin, Johan
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Medical Biochemistry and Microbiology.
    Ringvall, Maria
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Medical Biochemistry and Microbiology.
    Landegren, Ulf
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Genetics and Pathology.
    Kjellén, Lena
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Medical Biochemistry and Microbiology.
    Bondjers, Göran
    Li, Jin-Ping
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Medical Biochemistry and Microbiology.
    Lindahl, Ulf
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Medical Biochemistry and Microbiology.
    Spillmann, Dorothe
    Uppsala University, Disciplinary Domain of Medicine and Pharmacy, Faculty of Medicine, Department of Medical Biochemistry and Microbiology.
    Gerhardt, Holger
    Defective N-sulfation of heparan sulfate proteoglycans limits PDGF-BB binding and pericyte recruitment in vascular development2007In: Genes & Development, ISSN 0890-9369, E-ISSN 1549-5477, Vol. 21, no 3, p. 316-331Article in journal (Refereed)
    Abstract [en]

    During vascular development, endothelial platelet-derived growth factor B (PDGF-B) is critical for pericyte recruitment. Deletion of the conserved C-terminal heparin-binding motif impairs PDGF-BB retention and pericyte recruitment in vivo, suggesting a potential role for heparan sulfate (HS) in PDGF-BB function during vascular development. We studied the participation of HS chains in pericyte recruitment using two mouse models with altered HS biosynthesis. Reduction of N-sulfation due to deficiency in N-deacetylase/N-sulfotransferase-1 attenuated PDGF-BB binding in vitro, and led to pericyte detachment and delayed pericyte migration in vivo. Reduced N-sulfation also impaired PDGF-BB signaling and directed cell migration, but not proliferation. In contrast, HS from glucuronyl C5-epimerase mutants, which is extensively N- and 6-O-sulfated, but lacks 2-O-sulfated L-iduronic acid residues, retained PDGF-BB in vitro, and pericyte recruitment in vivo was only transiently delayed. These observations were supported by in vitro characterization of the structural features in HS important for PDGF-BB binding. We conclude that pericyte recruitment requires HS with sufficiently extended and appropriately spaced N-sulfated domains to retain PDGF-BB and activate PDGF receptor β (PDGFRβ) signaling, whereas the detailed sequence of monosaccharide and sulfate residues does not appear to be important for this interaction.

  • 6989.
    Abramsson, Andreas
    et al.
    Umeå University, Faculty of Science and Technology, Department of Science and Mathematics Education.
    Karlsson, David
    Umeå University, Faculty of Science and Technology, Department of Science and Mathematics Education.
    Pojkar som skriver: En kvalitativ studie om vad som utmärker mer avancerade skrivare2017Independent thesis Advanced level (professional degree), 20 credits / 30 HE creditsStudent thesis
    Abstract [sv]

    Syftet med denna studie är att öka kunskapen om vad som utmärker mer avancerade manliga skrivare på mellanstadiet. Genom en enkätundersökning av pojkars attityder till skrivande samt observationer av pojkars skrivpraktiker före och under ett längre skrivprojekt studerades aspekter som utmärker dessa skrivare gentemot övriga elever. Studien fann att de mer avancerade manliga skrivarna kommer från högutbildade familjer samt att de avancerade skrivarnas positiva attityder till skrivandet var väl förankrade i hemmet. Studien fann också att dessa pojkar i högre uträckning anstränger sig för sin egen, lärarens och sina vårdnadshavares skull än deras klasskamrater. Slutsatsen är att vårdnadshavares värderingar samt att läraren har höga förväntningar på pojkarna avspeglar sig i en vilja att anstränga sig för att lära – vilket i studien visade sig vara nyckeln till att bli en mer avancerad skrivare

  • 6990.
    Abramsson, Andreas
    et al.
    Kristianstad University College, School of Teacher Education.
    Nilsson, Daniel
    Kristianstad University College, School of Teacher Education.
    Minskar fysisk aktivitet självupplevda hälsobesvär?: En kvantitativ studie angående vilka eventuella samband som finns mellan gymnasiekillars självupplevda hälsobesvär och skattade fysiska aktivitetsnivå2009Independent thesis Basic level (university diploma), 10 credits / 15 HE creditsStudent thesis
    Abstract [sv]

    Forskning har visat att oro, ångest, stress och dålig sömn är åkommor som blivit allt vanligare och symptomen sjunker allt lägre ned i åldrarna. Med detta som utgångspunkt har vi valt en surveyundersökning i form av enkäter för att se vilka eventuella samband som fanns mellan gymnasiekillars självupplevda hälsobesvär och deras skattade fysiska aktivitetsnivå. I undersökningen har 96 gymnasiekillars svar behandlats för att ta del av deras upplevda hälsa och skattade fysiska aktivitetsnivå. Enligt Lpf 94 är syftet med undervisningen i Idrott och hälsa bland annat att utveckla elevernas kunskap om hur olika faktorer kan påverka det fysiska, psykiska och sociala välbefinnandet. Regelbunden fysisk aktivitet kan motverka bland annat stress, oro och depression. Resultatet av undersökningen visade att det fanns samband mellan gymnasiekillars självupplevda hälsobesvär och deras skattade fysiska aktivitetsnivå. Slutsatsen med studien är att lärare i Idrott och hälsa med hjälp av resultatet kan ge sina elever en insikt i vilka positiva effekter fysisk aktivitet har på eventuella besvär med hälsan. Därmed kan de även motivera dem till en framtida regelbunden fysisk aktivitet. Studien ämnar väcka läsarens intresse för ämnet och ge en insikt i sambanden mellan självupplevda hälsobesvär och fysisk aktivitet.

  • 6991.
    Abramsson, Anna
    et al.
    Umeå University, Faculty of Social Sciences, Department of Informatics.
    Pursiainen, Peter
    Umeå University, Faculty of Social Sciences, Department of Informatics.
    Sandman, Jonas
    Umeå University, Faculty of Social Sciences, Department of Informatics.
    Systemutveckling som designarbete – En studie av en systemutvecklingsprocess 2003Independent thesis Basic level (degree of Bachelor), 15 credits / 22,5 HE creditsStudent thesis
  • 6992.
    Abramsson, Anna
    et al.
    Umeå University, Faculty of Social Sciences, Department of Informatics.
    Sandman, Jonas
    Umeå University, Faculty of Social Sciences, Department of Informatics.
    Överlever Internet? En granskning av hoten mot Internets infrastruktur2004Independent thesis Advanced level (degree of Master (One Year)), 10 credits / 15 HE creditsStudent thesis
  • 6993. Abramsson, Erika
    et al.
    Strömbäck, Jesper
    Mid Sweden University, Faculty of Science, Technology and Media, Department of Information Technology and Media.
    EU-parlamentsvalet: En god eller dålig nyhet?2004Report (Other academic)
  • 6994.
    Abramsson, Evelina
    et al.
    Umeå University, Faculty of Social Sciences, Umeå School of Business and Economics (USBE), Statistics.
    Grind, Kajsa
    Umeå University, Faculty of Social Sciences, Umeå School of Business and Economics (USBE), Statistics.
    Skattning av kausala effekter med matchat fall-kontroll data2017Independent thesis Basic level (degree of Bachelor), 10 credits / 15 HE creditsStudent thesis
  • 6995.
    Abramsson, Heidi
    et al.
    Örebro University, School of Law, Psychology and Social Work.
    Hummerhielm, Michaela
    Örebro University, School of Law, Psychology and Social Work.
    Barn till missbrukande föräldrar: En studie om påverkan och en stödgruppsverksamhet2010Independent thesis Basic level (degree of Bachelor), 10 credits / 15 HE creditsStudent thesis
  • 6996. Abramsson, Ida
    et al.
    Johansson, Krister
    Internet - informationskälla och kommunikationsmedel: ett försök att utveckla elevernas förmåga att använda Internet i skolarbetet1999Independent thesis Basic level (professional degree), 10 credits / 15 HE creditsStudent thesis
  • 6997.
    Abramsson, Johannes
    et al.
    Karlstad University.
    Cederwall, Albert
    Karlstad University.
    Samskapandets påverkan på varumärkesupplevelsen: -      I en hyresvärd-hyresgäst kontext2018Independent thesis Basic level (degree of Bachelor), 180 HE creditsStudent thesis
  • 6998.
    Abramsson, Jonatan
    Linköping University, The Department of Physics, Chemistry and Biology.
    First-principle of Sc / Cr multilayers for x-ray mirrors applications2008Independent thesis Basic level (professional degree), 20 points / 30 hpStudent thesis
    Abstract [en]

    In order to produce x-ray mirrors the Thin Film Physics group at IFM grows Cr/Sc multilayers, with a typical thickness of the individual layers in the range 5-20 Å, and with as many periods as possible (a few hundred).

    The quality of the multilayer interfaces is crucial for their performance as mirrors. For thick layers poly-crystalline multilayers form with an interface quality that is too poor for the use as x-ray mirrors. For thinner layers, however, amorphous layers are formed with a much better quality of the interface.

    The goal of this project was to understand the formation of amorphous multilayers. Unfortunately it is impossible with the present day's theoretical tools to determine the structure of amorph interfaces. It is also impossible to calculate the interface structure for elements with large mismatch in size.

    So we have to construct interface models that are both simple and based on physical arguments.

  • 6999.
    Abramsson, Linnea
    Umeå University, Faculty of Medicine, Department of Pharmacology and Clinical Neuroscience, Pharmacology.
    Följsamhet till behandling med bisfosfonater: En intervjustudie på ortopedavdelningen vid Norrlands Universitetssjukhus, Umeå2017Independent thesis Basic level (degree of Bachelor), 10 credits / 15 HE creditsStudent thesis
  • 7000.
    Abramsson, Linnea
    et al.
    Umeå University, Faculty of Medicine, Department of Pharmacology and Clinical Neuroscience.
    Gustafsson, Maria
    Umeå University, Faculty of Medicine, Department of Pharmacology and Clinical Neuroscience, Pharmacology.
    Adherence to Bisphosphonates among People Admitted to an Orthopaedic and Geriatric Ward at a University Hospital in Sweden2018In: Pharmacy, ISSN 2226-4787, E-ISSN 1913-4711, Vol. 6, no 1, article id 20Article in journal (Refereed)
    Abstract [en]

    Oral bisphosphonates are the first choice of therapy to reduce the risk of osteoporotic fractures. These medications have generally poor oral bioavailability, which may further be reduced by concomitant intake of certain foods and drugs; therefore, it is vital to follow specific instructions. The aim with this study was to assess general adherence to oral bisphosphonates and adherence to specific administration instructions among people admitted to two wards at Umeå University hospital in Sweden. This interview study focuses on elderly patients living at home and prescribed oral bisphosphonates. Invited were 27 patients admitted to an orthopaedic ward and a geriatric ward during the period 28 March 2017 and 5 December 2017. In total, 21 patients were interviewed regarding their adherence to oral bisphosphonates. Out of 21 patients, 13 (62%) were considered non-adherent. The most common reason was calcium intake less than 2 h after oral administration of bisphosphonate (54%). The number of regularly prescribed drugs was significantly higher among patients rated non-adherent to bisphosphonates compared to those rated adherent (p = 0.004). Adherence to bisphosphonates administration instruction among elderly people living at home was limited. More research is needed to confirm these results and to investigate the reasons for non-adherence and how adherence to bisphosphonates can be improved.

137138139140141142143 6951 - 7000 of 1157239
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