Dokument-ID Dokumenttyp Verfasser/Autoren Herausgeber Haupttitel Abstract Auflage Verlagsort Verlag Erscheinungsjahr Seitenzahl Schriftenreihe Titel Schriftenreihe Bandzahl ISBN Quelle der Hochschulschrift Konferenzname Quelle:Titel Quelle:Jahrgang Quelle:Heftnummer Quelle:Erste Seite Quelle:Letzte Seite URN DOI Abteilungen OPUS4-50973 Wissenschaftlicher Artikel Abdalla, Hassan E.; Adam, R.; Aharonian, Felix A.; Benkhali, F. Ait; Angüner, Ekrem Oǧuzhan; Arakawa, M.; Arcaro, C.; Armand, C.; Ashkar, H.; Backes, M.; Martins, V. Barbosa; Barnard, M.; Becherini, Y.; Berge, D.; Bernloehr, K.; Bissaldi, E.; Blackwell, R.; Boettcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus, M.; Brun, F.; Brun, P.; Bryan, M.; Buechele, M.; Bulik, T.; Bylund, T.; Capasso, M.; Caroff, S.; Carosi, A.; Casanova, Sabrina; Cerruti, M.; Chand, T.; Chandra, S.; Chen, A.; Colafrancesco, S.; Curylo, M.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V; Dyks, J.; Egberts, Kathrin; Emery, G.; Ernenwein, J-P; Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Fussling, Matthias; Gabici, S.; Gallant, Y. A.; Gate, F.; Giavitto, G.; Giunti, L.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M-H; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, J. A.; Hofmann, W.; Hoischen, Clemens; Holch, T. L.; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq, A.; Jung-Richardt, I; Kastendieck, M. A.; Katarzynski, K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Kluzniak, W.; Komin, Nu; Kosack, K.; Kostunin, D.; Kreter, M.; Lamanna, G.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J-P; Leser, Eva; Levy, C.; Lohse, T.; Lypova, I; Mackey, J.; Majumdar, J.; Malyshev, D.; Marandon, V; Marcowith, A.; Mares, A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; Odaka, H.; Ohm, S.; Wilhelmi, E. de Ona; Ostrowski, M.; Oya, I; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P-O; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V; Noel, A. Priyana; Prokhorov, D. A.; Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V; Sailer, S.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schussler, F.; Schulz, A.; Schutte, H. M.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, Christian; Steppa, Constantin Beverly; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voelk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, Alraune; Ziegler, A.; Zorn, J.; Zywucka, N.; de Palma, F.; Axelsson, M.; Roberts, O. J. A very-high-energy component deep in the gamma-ray burst afterglow Gamma-ray bursts (GRBs) are brief flashes of gamma-rays and are considered to be the most energetic explosive phenomena in the Universe(1). The emission from GRBs comprises a short (typically tens of seconds) and bright prompt emission, followed by a much longer afterglow phase. During the afterglow phase, the shocked outflow-produced by the interaction between the ejected matter and the circumburst medium-slows down, and a gradual decrease in brightness is observed(2). GRBs typically emit most of their energy via.-rays with energies in the kiloelectronvolt-to-megaelectronvolt range, but a few photons with energies of tens of gigaelectronvolts have been detected by space-based instruments(3). However, the origins of such high-energy (above one gigaelectronvolt) photons and the presence of very-high-energy (more than 100 gigaelectronvolts) emission have remained elusive(4). Here we report observations of very-high-energy emission in the bright GRB 180720B deep in the GRB afterglow-ten hours after the end of the prompt emission phase, when the X-ray flux had already decayed by four orders of magnitude. Two possible explanations exist for the observed radiation: inverse Compton emission and synchrotron emission of ultrarelativistic electrons. Our observations show that the energy fluxes in the X-ray and gamma-ray range and their photon indices remain comparable to each other throughout the afterglow. This discovery places distinct constraints on the GRB environment for both emission mechanisms, with the inverse Compton explanation alleviating the particle energy requirements for the emission observed at late times. The late timing of this detection has consequences for the future observations of GRBs at the highest energies. London Nature Publ. Group 2019 12 Nature : the international weekly journal of science 575 7783 464 + 10.1038/s41586-019-1743-9 Institut für Physik und Astronomie OPUS4-48806 Wissenschaftlicher Artikel Abdalla, Hassan E.; Adam, R.; Aharonian, Felix A.; Benkhali, F. Ait; Angüner, Ekrem Oǧuzhan; Arakawa, M.; Arcaro, C.; Armand, C.; Ashkar, H.; Backes, M.; Martins, V. Barbosa; Barnard, M.; Becherini, Y.; Berge, D.; Bernloehr, K.; Blackwell, R.; Böttcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus, M.; Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Bylund, T.; Capasso, M.; Caroff, S.; Carosi, A.; Casanova, Sabrina; Cerruti, M.; Chand, T.; Chandra, S.; Chen, A.; Colafrancesco, S.; Curylo, M.; Davids, I. D.; Deil, C.; Devin, J.; DeWilt, P.; Dirson, L.; Djannati-Ata, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V; Dyks, J.; Egberts, Kathrin; Emery, G.; Ernenwein, J-P; Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Füßling, Matthias; Gabici, S.; Gallant, Y. A.; Gate, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M-H; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, James Anthony; Hofmann, W.; Hoischen, Clemens; Holch, Tim Lukas; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jardin-Blicq, A.; Jung-Richardt, I; Kastendieck, M. A.; Katarzynski, K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Kluzniak, W.; Komin, Nu; Kosack, K.; Kostunin, D.; Kraus, M.; Lamanna, G.; Lau, J.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J-P; Leser, Eva; Levy, C.; Lohse, T.; Lypova, I; Mackey, J.; Majumdar, J.; Malyshev, D.; Marandon, V; Marcowith, A.; Mares, A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Moulin, E.; Muller, J.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; Odaka, H.; Ohm, S.; Wilhelmi, E. de Ona; Ostrowski, M.; Oya, I; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P-O; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V; Priyana Noel, A.; Prokhorov, D. A.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V; Saito, S.; Sanchez, David M.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schutte, H.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, Christian; Steppa, Constantin Beverly; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van Der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voisin, F.; Voelk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zacharias, Michael; Zanin, R.; Zdziarski, A. A.; Zech, Alraune; Ziegler, A.; Zorn, J.; Zywucka, N.; Meyer, M. Constraints on the emission region of 3C 279 during strong flares in 2014 and 2015 through VHE gamma-ray observations with HESS The flat spectrum radio quasar 3C 279 is known to exhibit pronounced variability in the high-energy (100MeV < E < 100 GeV) gamma-ray band, which is continuously monitored with Fermi-LAT. During two periods of high activity in April 2014 and June 2015 target-of-opportunity observations were undertaken with the High Energy Stereoscopic System (H.E.S.S.) in the very-high-energy (VHE, E > 100 GeV) gamma-ray domain. While the observation in 2014 provides an upper limit, the observation in 2015 results in a signal with 8 : 7 sigma significance above an energy threshold of 66 GeV. No VHE variability was detected during the 2015 observations. The VHE photon spectrum is soft and described by a power-law index of 4.2 +/- 0.3. The H.E.S.S. data along with a detailed and contemporaneous multiwavelength data set provide constraints on the physical parameters of the emission region. The minimum distance of the emission region from the central black hole was estimated using two plausible geometries of the broad-line region and three potential intrinsic spectra. The emission region is confidently placed at r greater than or similar to 1 : 7 X 1017 cm from the black hole, that is beyond the assumed distance of the broad-line region. Time-dependent leptonic and lepto-hadronic one-zone models were used to describe the evolution of the 2015 flare. Neither model can fully reproduce the observations, despite testing various parameter sets. Furthermore, the H.E.S.S. data were used to derive constraints on Lorentz invariance violation given the large redshift of 3C 279. Les Ulis EDP Sciences 2019 19 Astronomy and astrophysics : an international weekly journal 627 10.1051/0004-6361/201935704 Institut für Physik und Astronomie OPUS4-49065 Wissenschaftlicher Artikel Abdalla, Hassan E.; Aharonian, Felix A.; Benkhali, F. Ait; Anguener, E. O.; Arakawa, M.; Arcaro, C.; Armand, C.; Ashkar, H.; Backes, M.; Martins, V. Barbosa; Barnard, M.; Becherini, Y.; Berge, D.; Bernloehr, K.; Blackwell, R.; Boettcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Breuhaus, M.; Brun, F.; Brun, P.; Bryan, M.; Buechele, M.; Bulik, T.; Bylund, T.; Capasso, M.; Caroff, S.; Carosi, A.; Casanova, Sabrina; Cerruti, M.; Chakraborty, N.; Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco, S.; Curylo, M.; Davids, I. D.; Deil, C.; Devin, J.; de Wilt, P.; Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V; Dyks, J.; Egberts, Kathrin; Emery, G.; Ernenwein, J-p; Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Fuessling, M.; Gabici, S.; Gallant, Y. A.; Gate, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M-H; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, James Anthony; Hofmann, W.; Hoischen, Clemens; Holch, Tim Lukas; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jung-Richardt, I; Kastendieck, M. A.; Katarzynski, K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Kluzniak, W.; Komin, Nu; Kosack, K.; Kostunin, D.; Kraus, M.; Lamanna, G.; Lau, J.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J-P; Leser, Eva; Levy, C.; Lohse, T.; Lopez-Coto, R.; Lypova, I; Mackey, J.; Majumdar, J.; Malyshev, D.; Marandon, V; Marcowith, A.; Mares, A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Muller, J.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; Odaka, H.; Ohm, S.; Wilhelmi, E. de Ona; Ostrowski, M.; Oya, I; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P-O; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V; Noel, A. Priyana; Prokhorov, D. A.; Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V; Saito, S.; Sanchez, David M.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schussler, F.; Schulz, A.; Schutte, H.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, Christian; Steppa, Constantin Beverly; Takahashi, T.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voisin, F.; Voelk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, Alraune; Ziegler, A.; Zorn, J.; Zywucka, N.; Maxted, N. Upper limits on very-high-energy gamma-ray emission from core-collapse supernovae observed with H.E.S.S. Young core-collapse supernovae with dense-wind progenitors may be able to accelerate cosmic-ray hadrons beyond the knee of the cosmic-ray spectrum, and this may result in measurable gamma-ray emission. We searched for gamma-ray emission from ten super- novae observed with the High Energy Stereoscopic System (H.E.S.S.) within a year of the supernova event. Nine supernovae were observed serendipitously in the H.E.S.S. data collected between December 2003 and December 2014, with exposure times ranging from 1.4 to 53 h. In addition we observed SN 2016adj as a target of opportunity in February 2016 for 13 h. No significant gamma-ray emission has been detected for any of the objects, and upper limits on the >1 TeV gamma-ray flux of the order of similar to 10(-13) cm(-)(2)s(-1) are established, corresponding to upper limits on the luminosities in the range similar to 2 x 10(39) to similar to 1 x 10(42) erg s(-1). These values are used to place model-dependent constraints on the mass-loss rates of the progenitor stars, implying upper limits between similar to 2 x 10(-5) and similar to 2 x 10(-3) M-circle dot yr(-1) under reasonable assumptions on the particle acceleration parameters. Les Ulis EDP Sciences 2019 11 Astronomy and astrophysics : an international weekly journal 626 10.1051/0004-6361/201935242 Institut für Physik und Astronomie OPUS4-50453 Wissenschaftlicher Artikel Abdalla, Hassan E.; Aharonian, Felix A.; Benkhali, F. Ait; Angüner, Ekrem Oǧuzhan; Arakawa, M.; Arcaro, C.; Armand, C.; Arrieta, M.; Backes, M.; Barnard, M.; Becherini, Y.; Tjus, J. Becker; Berge, D.; Bernhard, S.; Bernloehr, K.; Blackwell, R.; Bottcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bordas, Pol; Bregeon, J.; Brun, F.; Brun, P.; Bryan, M.; Buechele, M.; Bulik, T.; Bylund, T.; Capasso, M.; Caroff, S.; Carosi, A.; Cerruti, M.; Chakraborty, N.; Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco, S.; Condon, B.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V; Dyks, J.; Egberts, Kathrin; Emery, G.; Ernenwein, J-P; Eschbach, S.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Fuessling, M.; Gabici, S.; Gallant, Y. A.; Gate, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M-H; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, James Anthony; Hofmann, W.; Hoischen, Clemens; Holch, Tim Lukas; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jouvin, L.; Jung-Richardt, I; Kastendieck, M. A.; Katarzynski, K.; Katsuragawa, M.; Katz, U.; Kerszberg, D.; Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Kluzniak, W.; Komin, Nu; Kosack, K.; Krakau, S.; Kraus, M.; Kruger, P. P.; Lamanna, G.; Lau, J.; Lefaucheur, J.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J-P; Leser, Eva; Lohse, T.; Lorentz, M.; Lopez-Coto, R.; Lypova, I; Malyshev, D.; Marandon, V; Marcowith, A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moulin, E.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; Odaka, H.; Ohm, S.; Ostrowski, M.; Oya, I; Padovani, M.; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P-O; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V; Noel, A. Priyana; Prokhorov, D.; Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V; Saito, S.; Sanchez, David M.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schussler, F.; Schulz, A.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shilon, I; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Spanier, F.; Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, Christian; Steppa, Constantin Beverly; Takahashi, T.; Tavernet, J-P; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tibaldo, L.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voisin, F.; Voelk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; Wagner, R. M.; White, R.; Wierzcholska, A.; Yang, R.; Zaborov, D.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, Alraune; Zefi, F.; Ziegler, A.; Zorn, J.; Zywucka, N. The 2014TeV gamma-Ray Flare of Mrk 501 Seen with HESS The blazar Mrk 501 (z = 0.034) was observed at very-high-energy (VHE, E greater than or similar to 100 GeV) gamma-ray wavelengths during a bright flare on the night of 2014 June 23-24 (MJD 56832) with the H.E.S.S. phase-II array of Cherenkov telescopes. Data taken that night by H.E.S.S. at large zenith angle reveal an exceptional number of gamma-ray photons at multi-TeV energies, with rapid flux variability and an energy coverage extending significantly up to 20 TeV. This data set is used to constrain Lorentz invariance violation (LIV) using two independent channels: a temporal approach considers the possibility of an energy dependence in the arrival time of gamma-rays, whereas a spectral approach considers the possibility of modifications to the interaction of VHE gamma-rays with extragalactic background light (EBL) photons. The non-detection of energy-dependent time delays and the non-observation of deviations between the measured spectrum and that of a supposed power-law intrinsic spectrum with standard EBL attenuation are used independently to derive strong constraints on the energy scale of LIV (E-QG) in the subluminal scenario for linear and quadratic perturbations in the dispersion relation of photons. For the case of linear perturbations, the 95% confidence level limits obtained are E-QG,E-1 > 3.6 x 10(17) GeV using the temporal approach and E-QG,E-1 > 2.6 x 10(19) GeV using the spectral approach. For the case of quadratic perturbations, the limits obtained are E-QG,E-2 > 8.5 x 10(10) GeV using the temporal approach and E-QG,E-2 > 7.8 x 10(11) GeV using the spectral approach. Bristol IOP Publ. Ltd. 2019 9 The astrophysical journal : an international review of spectroscopy and astronomical physics 870 2 10.3847/1538-4357/aaf1c4 Institut für Physik und Astronomie OPUS4-48936 Wissenschaftlicher Artikel Abdalla, Hassan E.; Aharonian, Felix A.; Benkhali, F. Ait; Angüner, Ekrem Oǧuzhan; Arakawa, M.; Arcaro, C.; Armand, C.; Arrieta, M.; Backes, M.; Barnard, M.; Becherini, Y.; Tjus, J. Becker; Berge, D.; Bernloehr, K.; Blackwell, R.; Bottcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bordas, Pol; Bregeon, J.; Brun, F.; Brun, P.; Bryan, M.; Buchele, M.; Bulik, T.; Bylund, T.; Capasso, M.; Caroff, S.; Carosi, A.; Casanova, Sabrina; Cerruti, M.; Chakraborty, N.; Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco, S.; Condon, B.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V.; Dyks, J.; Egberts, Kathrin; Emery, G.; Ernenwein, J. -P.; Eschbach, S.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Fuessling, M.; Gabici, S.; Gallant, Y. A.; Gate, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, James Anthony; Hofmann, W.; Hoischen, Clemens; Holch, Tim Lukas; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jouvin, L.; Jung-Richardt, I.; Kastendieck, M. A.; Katarzynski, K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Kluzniak, W.; Komin, Nu.; Kosack, K.; Kraus, M.; Lamanna, G.; Lau, J.; Lefaucheur, J.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J. -P.; Leser, Eva; Lohse, T.; Lopez-Coto, R.; Lorentz, M.; Lypova, I.; Malyshev, D.; Marandon, V.; Marcowith, A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; Odaka, H.; Ohm, S.; Ostrowski, M.; Oya, I.; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V.; Noel, A. Priyana; Prokhorov, D. A.; Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V.; Saito, S.; Sanchez, David M.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schussler, F.; Schulz, A.; Schutte, H.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shilon, I.; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, Christian; Steppa, Constantin Beverly; Takahashi, T.; Tavernet, J. -P.; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voisin, F.; Voelk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; Wagner, R. M.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zaborov, D.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, Alraune; Ziegler, A.; Zorn, J.; Zywucka, N. H.E.S.S. observations of the flaring gravitationally lensed galaxy PKS 1830-211 PKS 1830-211 is a known macrolensed quasar located at a redshift of z = 2.5. Its highenergy gamma-ray emission has been detected with the Fermi-Large Area Telescope (LAT) instrument and evidence for lensing was obtained by several authors from its high-energy data. Observations of PKS 1830-211 were taken with the High Energy Stereoscopic System (H.E.S.S.) array of Imaging Atmospheric Cherenkov Telescopes in 2014 August, following a flare alert by the Fermi-LAT Collaboration. The H.E.S.S observations were aimed at detecting a gamma-ray flare delayed by 20-27 d from the alert flare, as expected from observations at other wavelengths. More than 12 h of good-quality data were taken with an analysis threshold of similar to 67 GeV. The significance of a potential signal is computed as a function of the date and the average significance over the whole period. Data are compared to simultaneous observations by Fermi-LAT. No photon excess or significant signal is detected. An upper limit on PKS 1830-211 flux above 67 GeV is computed and compared to the extrapolation of the Fermi-LAT flare spectrum. Oxford Oxford Univ. Press 2019 6 Monthly notices of the Royal Astronomical Society 486 3 3886 3891 10.1093/mnras/stz1031 Institut für Physik und Astronomie OPUS4-50442 Wissenschaftlicher Artikel Abdalla, Hassan E.; Aharonian, Felix A.; Benkhali, F. Ait; Angüner, Ekrem Oǧuzhan; Arakawa, M.; Arcaro, C.; Armand, C.; Arrieta, M.; Backes, M.; Barnard, M.; Becherini, Y.; Tjus, J. Becker; Berge, D.; Bernloehr, K.; Blackwell, R.; Bottcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bordas, Pol; Bregeon, J.; Brun, F.; Brun, P.; Bryan, M.; Buechele, M.; Bulik, T.; Bylund, T.; Capasso, M.; Caroff, S.; Carosi, A.; Casanova, Sabrina; Cerruti, M.; Chakraborty, N.; Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco, S.; Condon, B.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V; Dyks, J.; Egberts, Kathrin; Emery, G.; Ernenwein, J-P; Eschbach, S.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Fuessling, M.; Gabici, S.; Gallant, Y. A.; Gate, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M-H; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, James Anthony; Hofmann, W.; Hoischen, Clemens; Holch, Tim Lukas; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jouvin, L.; Jung-Richardt, I; Kastendieck, M. A.; Katarzynski, K.; Katsuragawa, M.; Katz, U.; Kerszberg, D.; Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Kluzniak, W.; Komin, Nu; Kosack, K.; Kraus, M.; Lamanna, G.; Lau, J.; Lefaucheur, J.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J-P; Leser, Eva; Lohse, T.; Lopez-Coto, R.; Lypova, I; Malyshev, D.; Marandon, V; Marcowith, A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; Odaka, H.; Ohm, S.; Ostrowski, M.; Oya, I; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P-O; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V; Noel, A. Priyana; Prokhorov, D. A.; Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V; Saito, S.; Sanchez, David M.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schussler, F.; Schulz, A.; Schutte, H.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shilon, I; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, Christian; Steppa, Constantin Beverly; Takahashi, T.; Tavernet, J-P; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tibaldo, L.; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voisin, F.; Voelk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; Wagner, R. M.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zaborov, D.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, Alraune; Zefi, F.; Ziegler, A.; Zorn, J.; Zywucka, N. Particle transport within the pulsar wind nebula HESS J1825-137 Context. We present a detailed view of the pulsar wind nebula (PWN) HESS J1825-137. We aim to constrain the mechanisms dominating the particle transport within the nebula, accounting for its anomalously large size and spectral characteristics. Aims. The nebula was studied using a deep exposure from over 12 years of H.E.S.S. I operation, together with data from H.E.S.S. II that improve the low-energy sensitivity. Enhanced energy-dependent morphological and spatially resolved spectral analyses probe the very high energy (VHE, E > 0.1 TeV) gamma-ray properties of the nebula. Methods. The nebula emission is revealed to extend out to 1.5 degrees from the pulsar, similar to 1.5 times farther than previously seen, making HESS J1825-137, with an intrinsic diameter of similar to 100 pc, potentially the largest gamma-ray PWN currently known. Characterising the strongly energy-dependent morphology of the nebula enables us to constrain the particle transport mechanisms. A dependence of the nebula extent with energy of R proportional to E alpha with alpha = -0.29 +/- 0.04(stat) +/- 0.05(sys) disfavours a pure diffusion scenario for particle transport within the nebula. The total gamma-ray flux of the nebula above 1 TeV is found to be (1.12 +/- 0.03(stat) +/- 0.25(sys)) +/- 10(-11) cm(-2) s(-1), corresponding to similar to 64% of the flux of the Crab nebula. Results. HESS J1825-137 is a PWN with clearly energy-dependent morphology at VHE gamma-ray energies. This source is used as a laboratory to investigate particle transport within intermediate-age PWNe. Based on deep observations of this highly spatially extended PWN, we produce a spectral map of the region that provides insights into the spectral variation within the nebula. Les Ulis EDP Sciences 2019 18 Astronomy and astrophysics : an international weekly journal 621 10.1051/0004-6361/201834335 Institut für Physik und Astronomie OPUS4-48817 Wissenschaftlicher Artikel Abdalla, Hassan E.; Aharonian, Felix A.; Benkhali, F. Ait; Angüner, Ekrem Oǧuzhan; Arakawa, M.; Arcaro, C.; Armand, C.; Backes, M.; Barnard, M.; Becherini, Y.; Berge, D.; Bernloehr, K.; Blackwell, R.; Bottcher, M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bregeon, J.; Brun, F.; Brun, P.; Bryan, M.; Buechele, M.; Bulik, T.; Bylund, T.; Capasso, M.; Caroff, S.; Carosi, A.; Casanova, Sabrina; Cerruti, M.; Chakraborty, N.; Chand, T.; Chandra, S.; Chaves, R. C. G.; Chen, A.; Colafrancesco, S.; Condon, B.; Davids, I. D.; Deil, C.; Devin, J.; deWilt, P.; Dirson, L.; Djannati-Atai, A.; Dmytriiev, A.; Donath, A.; Doroshenko, V; Dyks, J.; Egberts, Kathrin; Emery, G.; Ernenwein, J-P; Eschbach, S.; Feijen, K.; Fegan, S.; Fiasson, A.; Fontaine, G.; Funk, S.; Fuessling, M.; Gabici, S.; Gallant, Y. A.; Gate, F.; Giavitto, G.; Glawion, D.; Glicenstein, J. F.; Gottschall, D.; Grondin, M-H; Hahn, J.; Haupt, M.; Heinzelmann, G.; Henri, G.; Hermann, G.; Hinton, James Anthony; Hofmann, W.; Hoischen, Clemens; Holch, Tim Lukas; Holler, M.; Horns, D.; Huber, D.; Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.; Jankowsky, D.; Jankowsky, F.; Jouvin, L.; Jung-Richardt, I; Kastendieck, M. A.; Katarzynski, K.; Katsuragawa, M.; Katz, U.; Khangulyan, D.; Khelifi, B.; King, J.; Klepser, S.; Kluzniak, W.; Komin, Nu; Kosack, K.; Kostunin, D.; Kraus, M.; Lamanna, G.; Lau, J.; Lemiere, A.; Lemoine-Goumard, M.; Lenain, J-P; Leser, Eva; Lohse, T.; Lopez-Coto, R.; Lypova, I; Malyshev, D.; Marandon, V; Marcowith, A.; Mariaud, C.; Marti-Devesa, G.; Marx, R.; Maurin, G.; Maxted, N.; Meintjes, P. J.; Mitchell, A. M. W.; Moderski, R.; Mohamed, M.; Mohrmann, L.; Moore, C.; Moulin, E.; Murach, T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.; Niemiec, J.; Oakes, L.; Odaka, H.; Ohm, S.; Wilhelmi, E. de Ona; Ostrowski, M.; Oya, I; Panter, M.; Parsons, R. D.; Perennes, C.; Petrucci, P-O; Peyaud, B.; Piel, Q.; Pita, S.; Poireau, V; Noel, A. Priyana; Prokhorov, D. A.; Prokoph, H.; Puehlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth, R.; Reimer, A.; Reimer, O.; Renaud, M.; Rieger, F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Ruiz-Velasco, E.; Sahakian, V; Saito, S.; Sanchez, David M.; Santangelo, A.; Sasaki, M.; Schlickeiser, R.; Schussler, F.; Schulz, A.; Schutte, H.; Schwanke, U.; Schwemmer, S.; Seglar-Arroyo, M.; Senniappan, M.; Seyffert, A. S.; Shafi, N.; Shilon, I; Shiningayamwe, K.; Simoni, R.; Sinha, A.; Sol, H.; Specovius, A.; Spir-Jacob, M.; Stawarz, L.; Steenkamp, R.; Stegmann, Christian; Steppa, Constantin Beverly; Takahashi, T.; Tavernet, J-P; Tavernier, T.; Taylor, A. M.; Terrier, R.; Tibaldo, Luigi; Tiziani, D.; Tluczykont, M.; Trichard, C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt, D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis, G.; Veh, J.; Venter, C.; Vincent, P.; Vink, J.; Voisin, F.; Voelk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.; White, R.; Wierzcholska, A.; Yang, R.; Yoneda, H.; Zaborov, D.; Zacharias, M.; Zanin, R.; Zdziarski, A. A.; Zech, Alraune; Ziegler, A.; Zorn, J.; Zywucka, N. H.E.S.S. and Suzaku observations of the Vela X pulsar wind nebula Context. Pulsar wind nebulae (PWNe) represent the most prominent population of Galactic very-high-energy gamma-ray sources and are thought to be an efficient source of leptonic cosmic rays. Vela X is a nearby middle-aged PWN, which shows bright X-ray and TeV gamma-ray emission towards an elongated structure called the cocoon. Aims. Since TeV emission is likely inverse-Compton emission of electrons, predominantly from interactions with the cosmic microwave background, while X-ray emission is synchrotron radiation of the same electrons, we aim to derive the properties of the relativistic particles and of magnetic fields with minimal modelling. Methods. We used data from the Suzaku XIS to derive the spectra from three compact regions in Vela X covering distances from 0.3 to 4 pc from the pulsar along the cocoon. We obtained gamma-ray spectra of the same regions from H.E.S.S. observations and fitted a radiative model to the multi-wavelength spectra. Results. The TeV electron spectra and magnetic field strengths are consistent within the uncertainties for the three regions, with energy densities of the order 10(-12) erg cm(-3). The data indicate the presence of a cutoff in the electron spectrum at energies of similar to 100 TeV and a magnetic field strength of similar to 6 mu G. Constraints on the presence of turbulent magnetic fields are weak. Conclusions. The pressure of TeV electrons and magnetic fields in the cocoon is dynamically negligible, requiring the presence of another dominant pressure component to balance the pulsar wind at the termination shock. Sub-TeV electrons cannot completely account for the missing pressure, which may be provided either by relativistic ions or from mixing of the ejecta with the pulsar wind. The electron spectra are consistent with expectations from transport scenarios dominated either by advection via the reverse shock or by diffusion, but for the latter the role of radiative losses near the termination shock needs to be further investigated in the light of the measured cutoff energies. Constraints on turbulent magnetic fields and the shape of the electron cutoff can be improved by spectral measurements in the energy range greater than or similar to 10 keV. Les Ulis EDP Sciences 2019 16 Astronomy and astrophysics : an international weekly journal 627 10.1051/0004-6361/201935458 Institut für Physik und Astronomie OPUS4-48554 Wissenschaftlicher Artikel Abebe, Zeweter; Haki, Gulelat Desse; Schweigert, Florian J.; Henkel, Ina M.; Baye, Kaleab Low breastmilk vitamin A concentration is prevalent in rural Ethiopia Background There is scant information on the breastmilk vitamin A (BMVA) concentration of lactating women in developing countries, partly due to lack of methods applicable in-field. Objective To assess BMVA concentrations of samples collected from lactating women of children aged 6-23 months, in Mecha district, Ethiopia. Subjects/methods Data on socio-demographic and anthropometric characteristics were collected from randomly selected lactating women (n = 104). Breast milk samples were collected and vitamin A concentrations were analyzed using HPLC and iCheck FLUORO then the two measurements were compared. Results The prevalence of underweight (BMI < 18.5 kg/m(2)) among lactating women was 17%. Seventy six percent of the BMVA values were < 1.05 mu mol/l and 81% were < 8 mu g/g fat. The mean BMVA concentration accounted to 41% of the estimated average value for mothers in developing countries. The BMVA values from HPLC and iCheck were correlated (r = 0.59, p = < 0.001), but it was not strong. Conclusions The result indicates the low vitamin A status of the lactating women and their children. It further indicates that intake assessments should not use average BMVA composition. The possibility of using iCheck for monitoring interventions designed to improve vitamin A status of lactating women with low BMVA requires further investigation. London Nature Publ. Group 2019 7 European journal of clinical nutrition 73 8 1110 1116 10.1038/s41430-018-0334-4 Institut für Ernährungswissenschaft OPUS4-48358 Wissenschaftlicher Artikel Abeysekara, A. U.; Archer, A.; Benbow, Wystan; Bird, Ralph; Brill, A.; Brose, Robert; Buchovecky, M.; Calderon-Madera, D.; Christiansen, J. L.; Cui, W.; Daniel, M. K.; Falcone, A.; Feng, Q.; Fernandez-Alonso, M.; Finley, J. P.; Fortson, Lucy; Furniss, Amy; Gent, A.; Giuri, C.; Gueta, O.; Hanna, David; Hassan, T.; Hervet, Oliver; Holder, J.; Hughes, G.; Humensky, T. B.; Johnson, Caitlin A.; Kaaret, P.; Kertzman, M.; Kieda, David; Krause, Maria; Krennrich, F.; Kumar, S.; Lang, M. J.; Maier, Gernot; Moriarty, P.; Mukherjee, Reshmi; Nievas-Rosillo, M.; Ong, R. A.; Pfrang, Konstantin Johannes; Pohl, Martin; Prado, R. R.; Pueschel, Elisa; Quinn, J.; Ragan, K.; Reynolds, P. T.; Ribeiro, D.; Richards, G. T.; Roache, E.; Rovero, A. C.; Sadeh, Iftach; Santander, M.; Sembroski, G. H.; Shahinyan, Karlen; Sushch, Iurii; Svraka, T.; Weinstein, A.; Wells, R. M.; Wilcox, Patrick; Wilhelm, Alina; Williams, David Arnold; Williamson, T. J.; Zitzer, B. Measurement of the Extragalactic Background Light Spectral Energy Distribution with VERITAS The extragalactic background light (EBL), a diffuse photon field in the optical and infrared range, is a record of radiative processes over the universe?s history. Spectral measurements of blazars at very high energies (>100 GeV) enable the reconstruction of the spectral energy distribution (SED) of the EBL, as the blazar spectra are modified by redshift- and energy-dependent interactions of the gamma-ray photons with the EBL. The spectra of 14 VERITAS-detected blazars are included in a new measurement of the EBL SED that is independent of EBL SED models. The resulting SED covers an EBL wavelength range of 0.56?56 ?m, and is in good agreement with lower limits obtained by assuming that the EBL is entirely due to radiation from cataloged galaxies. Bristol IOP Publ. Ltd. 2019 8 The astrophysical journal : an international review of spectroscopy and astronomical physics 885 2 10.3847/1538-4357/ab4817 Institut für Physik und Astronomie OPUS4-43970 Wissenschaftlicher Artikel Adam, Berit Öffentliches Rechnungswesen 5., vollständig überarb. Aufl. Wiesbaden Springer 2019 13 Handbuch zur Verwaltungsreform 978-3-658-21562-0 443 456 Wirtschaftswissenschaften