TY  - JOUR
A1  - Abramowski, A.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Akhperjanian, A. G.
A1  - Anguener, E. O.
A1  - Backes, M.
A1  - Balzer, A.
A1  - Becherini, Y.
A1  - Tjus, J. Becker
A1  - Berge, D.
A1  - Bernhard, S.
A1  - Bernloehr, K.
A1  - Birsin, E.
A1  - Blackwell, R.
A1  - Boettcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Bulik, T.
A1  - Carr, J.
A1  - Casanova, Sabrina
A1  - Chakraborty, N.
A1  - Chalme-Calvet, R.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Chevalier, J.
A1  - Chretien, M.
A1  - Colafrancesco, S.
A1  - Cologna, G.
A1  - Condon, B.
A1  - Conrad, J.
A1  - Couturier, C.
A1  - Cui, Y.
A1  - Davids, I. D.
A1  - Degrange, B.
A1  - Deil, C.
A1  - deWilt, P.
A1  - Djannati-Atai, A.
A1  - Domainko, W.
A1  - Donath, A.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Dyrda, M.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Ernenwein, J. -P.
A1  - Espigat, P.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Feinstein, F.
A1  - Fernandes, M. V.
A1  - Fernandez, D.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Goyal, A.
A1  - Grondin, M. -H.
A1  - Grudzinska, M.
A1  - Hadasch, D.
A1  - Haeffner, S.
A1  - Hahn, J.
A1  - Hawkes, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hillert, A.
A1  - Hinton, J. A.
A1  - Hofmann, W.
A1  - Hofverberg, P.
A1  - Hoischen, Clemens
A1  - Holler, M.
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, F.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kerszberg, D.
A1  - Khelifi, B.
A1  - Kieffer, M.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kolitzus, D.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Krayzel, F.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lefaucheur, J.
A1  - Lefranc, V.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Lohse, T.
A1  - Lopatin, A.
A1  - Lorentz, M.
A1  - Lu, C. -C.
A1  - Lui, R.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - Meintjes, P. J.
A1  - Menzler, U.
A1  - Meyer, M.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - de Naurois, M.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Oettl, S.
A1  - Ohm, S.
A1  - Opitz, B.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Arribas, M. Paz
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Pita, S.
A1  - Poon, H.
A1  - Prokhorov, D.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Reichardt, I.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Romoli, C.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Salek, D.
A1  - Sanchez, D. A.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schuessler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seyffert, A. S.
A1  - Simoni, R.
A1  - Sol, H.
A1  - Spanier, F.
A1  - Spengler, G.
A1  - Spies, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, I.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tuffs, R.
A1  - Valerius, K.
A1  - van der Walt, J.
A1  - van Eldik, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - Weidinger, M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zabalza, V.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Zywucka, N.
T1  - Detailed spectral and morphological analysis of the shell type supernova remnant RCW 86
JF  - Astronomy and astrophysics : an international weekly journal
N2  - 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).
KW  - astroparticle physics
KW  - gamma rays: general
KW  - ISM: supernova remnants
KW  - cosmic rays
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201526545
SN  - 1432-0746
VL  - 612
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Abramowski, A.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Akhperjanian, A. G.
A1  - Andersson, T.
A1  - Anguener, E. O.
A1  - Arakawa, M.
A1  - Arrieta, M.
A1  - Aubert, P.
A1  - Backes, M.
A1  - Balzer, A.
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Tjus, J. Becker
A1  - Berge, D.
A1  - Bernhard, S.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Boettcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Bilchele, M.
A1  - Bulik, T.
A1  - Capasso, M.
A1  - Carr, J.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chalme-Calvet, R.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Chevalier, J.
A1  - Chretien, M.
A1  - Coffaro, M.
A1  - Colafrancesco, S.
A1  - Cologna, G.
A1  - Condon, B.
A1  - Conrad, J.
A1  - Cui, Y.
A1  - Davids, I. D.
A1  - Decock, J.
A1  - Degrange, B.
A1  - Deil, C.
A1  - Devin, J.
A1  - deWilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Domainko, W.
A1  - Donath, A.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Ernenwein, J. -P.
A1  - Eschbach, S.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Fernandes, M. V.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Funk, S.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Goya, A.
A1  - Grondin, M. -H.
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Hawkes, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hinton, J. A.
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holler, M.
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Iwasaki, H.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jingo, M.
A1  - Jogler, T.
A1  - Jouvin, L.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Kerszberg, D.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - Kieffer, M.
A1  - King, J.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kolitzus, D.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Kraus, M.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lees, J. -P.
A1  - Lefaucheur, J.
A1  - Lefranc, V.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Leser, Eva
A1  - Lohse, T.
A1  - Lorentz, M.
A1  - Liu, R.
A1  - Lopez-Coto, R.
A1  - Lypova, I.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - Meintjes, P. J.
A1  - Meyer, M.
A1  - Mitche, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Nakashima, S.
A1  - de Naurois, M.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Oettl, S.
A1  - Ohm, S.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Padovani, M.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Arribas, M. Paz
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perennes, C.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poon, H.
A1  - Prokhorov, D.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Richter, S.
A1  - Rieger, F.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Saito, S.
A1  - Salek, D.
A1  - Sanchez, D. A.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schuessler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Settimo, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I.
A1  - Simoni, R.
A1  - Sol, H.
A1  - Spanier, F.
A1  - Spengler, G.
A1  - Spies, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stycz, K.
A1  - Sushch, I.
A1  - Takahashi, T.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tibaldo, L.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van der Walt, D. J.
A1  - van Eldik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zabalza, V.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Ziegler, A.
A1  - Zywucka, N.
T1  - Deeper HESS observations of Vela Junior (RX J0852.0-4622)
BT  - Morphology studies and resolved spectroscopy
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Aims. We study gamma-ray emission from the shell-type supernova remnant (SNR) RXJ0852.0-4622 to better characterize its spectral properties and its distribution over the SNR. Methods. The analysis of an extended High Energy Spectroscopic System (H.E.S.S.) data set at very high energies (E > 100 GeV) permits detailed studies, as well as spatially resolved spectroscopy, of the morphology and spectrum of the whole RXJ0852.0-4622 region. The H.E.S.S. data are combined with archival data from other wavebands and interpreted in the framework of leptonic and hadronic models. The joint Fermi-LAT-H.E.S.S. spectrum allows the direct determination of the spectral characteristics of the parent particle population in leptonic and hadronic scenarios using only GeV-TeV data. Results. An updated analysis of the H.E.S.S. data shows that the spectrum of the entire SNR connects smoothly to the high-energy spectrum measured by Fermi-LAT. The increased data set makes it possible to demonstrate that the H.E.S.S. spectrum deviates significantly from a power law and is well described by both a curved power law and a power law with an exponential cutoff at an energy of E-cut = (6.7 +/- 1.2(stat) +/- 1.2(syst)) TeV. The joint Fermi-LAT-H.E.S.S. spectrum allows the unambiguous identification of the spectral shape as a power law with an exponential cutoff. No significant evidence is found for a variation of the spectral parameters across the SNR, suggesting similar conditions of particle acceleration across the remnant. A simple modeling using one particle population to model the SNR emission demonstrates that both leptonic and hadronic emission scenarios remain plausible. It is also shown that at least a part of the shell emission is likely due to the presence of a pulsar wind nebula around PSR J0855-4644.
KW  - astroparticle physics
KW  - gamma rays: general
KW  - acceleration of particles
KW  - cosmic rays
KW  - ISM: supernova remnants
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201630002
SN  - 1432-0746
VL  - 612
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Abramowski, A.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Akhperjanian, A. G.
A1  - Andersson, T.
A1  - Anguener, E. O.
A1  - Arakawa, M.
A1  - Arrieta, M.
A1  - Aubert, P.
A1  - Backes, M.
A1  - Balzer, A.
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Tjus, J. Becker
A1  - Berge, D.
A1  - Bernhard, S.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Boettcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bonnefoy, S.
A1  - Bordas, Pol
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Buechele, M.
A1  - Bulik, T.
A1  - Capasso, M.
A1  - Carr, J.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Chevalier, J.
A1  - Coffaro, M.
A1  - Colafrancesco, S.
A1  - Cologna, G.
A1  - Condon, B.
A1  - Conrad, J.
A1  - Cui, Y.
A1  - Davids, I. D.
A1  - Decock, J.
A1  - Degrange, B.
A1  - Deil, C.
A1  - Devin, J.
A1  - deWilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Domainko, W.
A1  - Donath, A.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Ernenwein, J. -P.
A1  - Eschbach, S.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Fernandes, M. V.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Funk, S.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Goyal, A.
A1  - Grondin, M. -H.
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Hawkes, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hinton, J. A.
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holch, T. L.
A1  - Holler, M.
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Iwasaki, H.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jingo, M.
A1  - Jogler, T.
A1  - Jouvin, L.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Kerszberg, D.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - King, J.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kolitzus, D.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Kraus, M.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lees, J. -P.
A1  - Lefaucheur, J.
A1  - Lefranc, V.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Leser, Eva
A1  - Lohse, T.
A1  - Lorentz, M.
A1  - Liu, R.
A1  - Lopez-Coto, R.
A1  - Lypova, I.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - Meintjes, P. J.
A1  - Meyer, M.
A1  - Mitche, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Nakashima, S.
A1  - de Naurois, M.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Oettl, S.
A1  - Ohm, S.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Padovani, M.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perennes, C.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poon, H.
A1  - Prokhorov, D.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Richter, S.
A1  - Rieger, F.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Saito, S.
A1  - Salek, D.
A1  - Sanchez, D. A.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schuessler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Settimo, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I.
A1  - Simoni, R.
A1  - Sol, H.
A1  - Spanier, F.
A1  - Spengler, G.
A1  - Spies, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stycz, K.
A1  - Sushch, I.
A1  - Takahashi, T.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tibaldo, L.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van der Wale, D. J.
A1  - van Eldik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zabalza, V.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Ziegler, A.
A1  - Zywucka, N.
A1  - Bamba, A.
A1  - Fukui, Y.
A1  - Sano, H.
A1  - Yoshiike, S.
T1  - A search for new supernova remnant shells in the Galactic plane with HESS
JF  - Astronomy and astrophysics : an international weekly journal
N2  - A search for new supernova remnants (SNRs) has been conducted using TeV gamma-ray data from the H.E.S.S. Galactic plane survey. As an identification criterion, shell morphologies that are characteristic for known resolved TeV SNRs have been used. Three new SNR candidates were identified in the H.E.S.S. data set with this method. Extensive multiwavelength searches for counterparts were conducted. A radio SNR candidate has been identified to be a counterpart to HESS J1534-571. The TeV source is therefore classified as a SNR. For the other two sources, HESS J1614-518 and HESS J1912 + 101, no identifying counterparts have been found, thus they remain SNR candidates for the time being. TeV-emitting SNRs are key objects in the context of identifying the accelerators of Galactic cosmic rays. The TeV emission of the relativistic particles in the new sources is examined in view of possible leptonic and hadronic emission scenarios, taking the current multiwavelength knowledge into account.
KW  - astroparticle physics
KW  - ISM: supernova remnants
KW  - cosmic rays
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201730737
SN  - 1432-0746
VL  - 612
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Abramowski, A.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Akhperjanian, A. G.
A1  - Andersson, T.
A1  - Anguener, E. O.
A1  - Arrieta, M.
A1  - Aubert, P.
A1  - Backes, M.
A1  - Balzer, A.
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Tjus, J. Becker
A1  - Berge, D.
A1  - Bernhard, S.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Boettcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Bulik, T.
A1  - Capasso, M.
A1  - Carr, J.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chalme-Calvet, R.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Chevalier, J.
A1  - Chretien, M.
A1  - Colafrancesco, S.
A1  - Cologna, G.
A1  - Condon, B.
A1  - Conrad, J.
A1  - Cui, Y.
A1  - Davids, I. D.
A1  - Decock, J.
A1  - Degrange, B.
A1  - Dei, C.
A1  - Devin, J.
A1  - deWilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Domainko, W.
A1  - Donath, A.
A1  - Dubus, G.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Ernenwein, J. -P.
A1  - Eschbach, S.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Fernandes, M. V.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Foerster, A.
A1  - Fukuyama, T.
A1  - Funk, S.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Goyal, A.
A1  - Grondin, M. -H.
A1  - Hadasch, D.
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Hawkes, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hinton, J. A.
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holler, M.
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jingo, M.
A1  - Jogler, T.
A1  - Jouvin, L.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katz, U.
A1  - Kerszberg, D.
A1  - Khelifi, B.
A1  - Kieffer, M.
A1  - King, J.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Kolitzus, D.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Kraus, M.
A1  - Krayzel, F.
A1  - Krueger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lees, J. -P.
A1  - Lefaucheur, J.
A1  - Lefranc, V.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Leser, Eva
A1  - Lohse, T.
A1  - Lorentz, M.
A1  - Liu, R.
A1  - Lopez-Coto, R.
A1  - Lypova, I.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - Meintjes, P. J.
A1  - Meyer, M.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - de Naurois, M.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Oettl, S.
A1  - Ohm, S.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Padovani, M.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perennes, C.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poon, H.
A1  - Prokhorov, D.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Romoli, C.
A1  - Rosier-Lees, S.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Salek, D.
A1  - Sanchez, D. A.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schuessler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Settimo, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I.
A1  - Simoni, R.
A1  - Sol, H.
A1  - Spanie, F.
A1  - Spengler, G.
A1  - Spies, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stinzing, F.
A1  - Stycz, K.
A1  - Sushch, I.
A1  - Takahashi, T.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tibaldo, L.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van der Walt, D. J.
A1  - van Edik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Volpe, F.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zabalza, V.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Ziegler, A.
A1  - Zywucka, N.
T1  - HESS observations of RX J1713.7-3946 with improved angular and spectral resolution
BT  - Evidence for gamma-ray emission extending beyond the X-ray emitting shell
JF  - Astronomy and astrophysics : an international weekly journal
KW  - acceleration of particles
KW  - cosmic rays
KW  - ISM: supernova remnants
KW  - gamma rays: general
KW  - astroparticle physic
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201629790
SN  - 1432-0746
VL  - 612
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - De Angelis, A.
A1  - Tatischeff, V.
A1  - Grenier, I. A.
A1  - McEnery, J.
A1  - Mallamaci, Manuela
A1  - Tavani, M.
A1  - Oberlack, U.
A1  - Hanlon, L.
A1  - Walter, R.
A1  - Argan, A.
A1  - Von Ballmoos, P.
A1  - Bulgarelli, A.
A1  - Bykov, A.
A1  - Hernanz, M.
A1  - Kanbach, G.
A1  - Kuvvetli, I.
A1  - Pearce, M.
A1  - Zdziarski, A.
A1  - Conrad, J.
A1  - Ghisellini, G.
A1  - Harding, A.
A1  - Isern, J.
A1  - Leising, M.
A1  - Longo, F.
A1  - Madejski, G.
A1  - Martinez, M.
A1  - Mazziotta, Mario Nicola
A1  - Paredes, J. M.
A1  - Pohl, Martin
A1  - Rando, R.
A1  - Razzano, M.
A1  - Aboudan, A.
A1  - Ackermann, M.
A1  - Addazi, A.
A1  - Ajello, M.
A1  - Albertus, C.
A1  - Alvarez, J. M.
A1  - Ambrosi, G.
A1  - Anton, S.
A1  - Antonelli, L. A.
A1  - Babic, A.
A1  - Baibussinov, B.
A1  - Balbom, M.
A1  - Baldini, L.
A1  - Balman, S.
A1  - Bambi, C.
A1  - Barres de Almeida, U.
A1  - Barrio, J. A.
A1  - Bartels, R.
A1  - Bastieri, D.
A1  - Bednarek, W.
A1  - Bernard, D.
A1  - Bernardini, E.
A1  - Bernasconi, T.
A1  - Bertucci, B.
A1  - Biland, A.
A1  - Bissaldi, E.
A1  - Boettcher, M.
A1  - Bonvicini, V.
A1  - Bosch-Ramon, V.
A1  - Bottacini, E.
A1  - Bozhilov, V.
A1  - Bretz, T.
A1  - Branchesi, M.
A1  - Brdar, V.
A1  - Bringmann, T.
A1  - Brogna, A.
A1  - Jorgensen, C. Budtz
A1  - Busetto, G.
A1  - Buson, S.
A1  - Busso, M.
A1  - Caccianiga, A.
A1  - Camera, S.
A1  - Campana, R.
A1  - Caraveo, P.
A1  - Cardillo, M.
A1  - Carlson, P.
A1  - Celestin, S.
A1  - Cermeno, M.
A1  - Chen, A.
A1  - Cheung, C. C.
A1  - Churazov, E.
A1  - Ciprini, S.
A1  - Coc, A.
A1  - Colafrancesco, S.
A1  - Coleiro, A.
A1  - Collmar, W.
A1  - Coppi, P.
A1  - Curado da Silva, R.
A1  - Cutini, S.
A1  - De Lotto, B.
A1  - de Martino, D.
A1  - De Rosa, A.
A1  - Del Santo, M.
A1  - Delgado, L.
A1  - Diehl, R.
A1  - Dietrich, S.
A1  - Dolgov, A. D.
A1  - Dominguez, A.
A1  - Prester, D. Dominis
A1  - Donnarumma, I.
A1  - Dorner, D.
A1  - Doro, M.
A1  - Dutra, M.
A1  - Elsaesser, D.
A1  - Fabrizio, M.
A1  - Fernandez-Barral, A.
A1  - Fioretti, V.
A1  - Foffano, L.
A1  - Formato, V.
A1  - Fornengo, N.
A1  - Foschini, L.
A1  - Franceschini, A.
A1  - Franckowiak, A.
A1  - Funk, S.
A1  - Fuschino, F.
A1  - Gaggero, D.
A1  - Galanti, G.
A1  - Gargano, F.
A1  - Gasparrini, D.
A1  - Gehrz, R.
A1  - Giammaria, P.
A1  - Giglietto, N.
A1  - Giommi, P.
A1  - Giordano, F.
A1  - Giroletti, M.
A1  - Ghirlanda, G.
A1  - Godinovic, N.
A1  - Gouiffes, C.
A1  - Grove, J. E.
A1  - Hamadache, C.
A1  - Hartmann, D. H.
A1  - Hayashida, M.
A1  - Hryczuk, A.
A1  - Jean, P.
A1  - Johnson, T.
A1  - Jose, J.
A1  - Kaufmann, S.
A1  - Khelifi, B.
A1  - Kiener, J.
A1  - Knodlseder, J.
A1  - Kolem, M.
A1  - Kopp, J.
A1  - Kozhuharov, V.
A1  - Labanti, C.
A1  - Lalkovski, S.
A1  - Laurent, P.
A1  - Limousin, O.
A1  - Linares, M.
A1  - Lindfors, E.
A1  - Lindner, M.
A1  - Liu, J.
A1  - Lombardi, S.
A1  - Loparco, F.
A1  - Lopez-Coto, R.
A1  - Lopez Moya, M.
A1  - Lott, B.
A1  - Lubrano, P.
A1  - Malyshev, D.
A1  - Mankuzhiyil, N.
A1  - Mannheim, K.
A1  - Marcha, M. J.
A1  - Marciano, A.
A1  - Marcote, B.
A1  - Mariotti, M.
A1  - Marisaldi, M.
A1  - McBreen, S.
A1  - Mereghetti, S.
A1  - Merle, A.
A1  - Mignani, R.
A1  - Minervini, G.
A1  - Moiseev, A.
A1  - Morselli, A.
A1  - Moura, F.
A1  - Nakazawa, K.
A1  - Nava, L.
A1  - Nieto, D.
A1  - Orienti, M.
A1  - Orio, M.
A1  - Orlando, E.
A1  - Orleanski, P.
A1  - Paiano, S.
A1  - Paoletti, R.
A1  - Papitto, A.
A1  - Pasquato, M.
A1  - Patricelli, B.
A1  - Perez-Garcia, M. A.
A1  - Persic, M.
A1  - Piano, G.
A1  - Pichel, A.
A1  - Pimenta, M.
A1  - Pittori, C.
A1  - Porter, T.
A1  - Poutanen, J.
A1  - Prandini, E.
A1  - Prantzos, N.
A1  - Produit, N.
A1  - Profumo, S.
A1  - Queiroz, F. S.
A1  - Raino, S.
A1  - Raklev, A.
A1  - Regis, M.
A1  - Reichardt, I.
A1  - Rephaeli, Y.
A1  - Rico, J.
A1  - Rodejohann, W.
A1  - Fernandez, G. Rodriguez
A1  - Roncadelli, M.
A1  - Roso, L.
A1  - Rovero, A.
A1  - Ruffini, R.
A1  - Sala, G.
A1  - Sanchez-Conde, M. A.
A1  - Santangelo, Andrea
A1  - Parkinson, P. Saz
A1  - Sbarrato, T.
A1  - Shearer, A.
A1  - Shellard, R.
A1  - Short, K.
A1  - Siegert, T.
A1  - Siqueira, C.
A1  - Spinelli, P.
A1  - Stamerra, A.
A1  - Starrfield, S.
A1  - Strong, A.
A1  - Strumke, I.
A1  - Tavecchio, F.
A1  - Taverna, R.
A1  - Terzic, T.
A1  - Thompson, D. J.
A1  - Tibolla, O.
A1  - Torres, D. F.
A1  - Turolla, R.
A1  - Ulyanov, A.
A1  - Ursi, A.
A1  - Vacchi, A.
A1  - Van den Abeele, J.
A1  - Vankova-Kirilovai, G.
A1  - Venter, C.
A1  - Verrecchia, F.
A1  - Vincent, P.
A1  - Wang, X.
A1  - Weniger, C.
A1  - Wu, X.
A1  - Zaharijas, G.
A1  - Zampieri, L.
A1  - Zane, S.
A1  - Zimmer, S.
A1  - Zoglauer, A.
T1  - Science with e-ASTROGAM A space mission for MeV-GeV gamma-ray astrophysics
JF  - Journal of High Energy Astrophysics
Y1  - 2018
U6  - https://doi.org/10.1016/j.jheap.2018.07.001
SN  - 2214-4048
SN  - 2214-4056
VL  - 19
SP  - 1
EP  - 106
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - JOUR
A1  - Gorski, Mathias
A1  - Jung, Bettina
A1  - Li, Yong
A1  - Matias-Garcia, Pamela R.
A1  - Wuttke, Matthias
A1  - Coassin, Stefan
A1  - Thio, Chris H. L.
A1  - Kleber, Marcus E.
A1  - Winkler, Thomas W.
A1  - Wanner, Veronika
A1  - Chai, Jin-Fang
A1  - Chu, Audrey Y.
A1  - Cocca, Massimiliano
A1  - Feitosa, Mary F.
A1  - Ghasemi, Sahar
A1  - Hoppmann, Anselm
A1  - Horn, Katrin
A1  - Li, Man
A1  - Nutile, Teresa
A1  - Scholz, Markus
A1  - Sieber, Karsten B.
A1  - Teumer, Alexander
A1  - Tin, Adrienne
A1  - Wang, Judy
A1  - Tayo, Bamidele O.
A1  - Ahluwalia, Tarunveer S.
A1  - Almgren, Peter
A1  - Bakker, Stephan J. L.
A1  - Banas, Bernhard
A1  - Bansal, Nisha
A1  - Biggs, Mary L.
A1  - Boerwinkle, Eric
A1  - Böttinger, Erwin
A1  - Brenner, Hermann
A1  - Carroll, Robert J.
A1  - Chalmers, John
A1  - Chee, Miao-Li
A1  - Chee, Miao-Ling
A1  - Cheng, Ching-Yu
A1  - Coresh, Josef
A1  - de Borst, Martin H.
A1  - Degenhardt, Frauke
A1  - Eckardt, Kai-Uwe
A1  - Endlich, Karlhans
A1  - Franke, Andre
A1  - Freitag-Wolf, Sandra
A1  - Gampawar, Piyush
A1  - Gansevoort, Ron T.
A1  - Ghanbari, Mohsen
A1  - Gieger, Christian
A1  - Hamet, Pavel
A1  - Ho, Kevin
A1  - Hofer, Edith
A1  - Holleczek, Bernd
A1  - Foo, Valencia Hui Xian
A1  - Hutri-Kahonen, Nina
A1  - Hwang, Shih-Jen
A1  - Ikram, M. Arfan
A1  - Josyula, Navya Shilpa
A1  - Kahonen, Mika
A1  - Khor, Chiea-Chuen
A1  - Koenig, Wolfgang
A1  - Kramer, Holly
A1  - Kraemer, Bernhard K.
A1  - Kuehnel, Brigitte
A1  - Lange, Leslie A.
A1  - Lehtimaki, Terho
A1  - Lieb, Wolfgang
A1  - Loos, Ruth J. F.
A1  - Lukas, Mary Ann
A1  - Lyytikainen, Leo-Pekka
A1  - Meisinger, Christa
A1  - Meitinger, Thomas
A1  - Melander, Olle
A1  - Milaneschi, Yuri
A1  - Mishra, Pashupati P.
A1  - Mononen, Nina
A1  - Mychaleckyj, Josyf C.
A1  - Nadkarni, Girish N.
A1  - Nauck, Matthias
A1  - Nikus, Kjell
A1  - Ning, Boting
A1  - Nolte, Ilja M.
A1  - O'Donoghue, Michelle L.
A1  - Orho-Melander, Marju
A1  - Pendergrass, Sarah A.
A1  - Penninx, Brenda W. J. H.
A1  - Preuss, Michael H.
A1  - Psaty, Bruce M.
A1  - Raffield, Laura M.
A1  - Raitakari, Olli T.
A1  - Rettig, Rainer
A1  - Rheinberger, Myriam
A1  - Rice, Kenneth M.
A1  - Rosenkranz, Alexander R.
A1  - Rossing, Peter
A1  - Rotter, Jerome
A1  - Sabanayagam, Charumathi
A1  - Schmidt, Helena
A1  - Schmidt, Reinhold
A1  - Schoettker, Ben
A1  - Schulz, Christina-Alexandra
A1  - Sedaghat, Sanaz
A1  - Shaffer, Christian M.
A1  - Strauch, Konstantin
A1  - Szymczak, Silke
A1  - Taylor, Kent D.
A1  - Tremblay, Johanne
A1  - Chaker, Layal
A1  - van der Harst, Pim
A1  - van der Most, Peter J.
A1  - Verweij, Niek
A1  - Voelker, Uwe
A1  - Waldenberger, Melanie
A1  - Wallentin, Lars
A1  - Waterworth, Dawn M.
A1  - White, Harvey D.
A1  - Wilson, James G.
A1  - Wong, Tien-Yin
A1  - Woodward, Mark
A1  - Yang, Qiong
A1  - Yasuda, Masayuki
A1  - Yerges-Armstrong, Laura M.
A1  - Zhang, Yan
A1  - Snieder, Harold
A1  - Wanner, Christoph
A1  - Boger, Carsten A.
A1  - Kottgen, Anna
A1  - Kronenberg, Florian
A1  - Pattaro, Cristian
A1  - Heid, Iris M.
T1  - Meta-analysis uncovers genome-wide significant variants for rapid kidney function decline
JF  - Kidney international : official journal of the International Society of Nephrology
N2  - Rapid decline of glomerular filtration rate estimated from creatinine (eGFRcrea) is associated with severe clinical endpoints. In contrast to cross-sectionally assessed eGFRcrea, the genetic basis for rapid eGFRcrea decline is largely unknown. To help define this, we meta-analyzed 42 genome-wide association studies from the Chronic Kidney Diseases Genetics Consortium and United Kingdom Biobank to identify genetic loci for rapid eGFRcrea decline. Two definitions of eGFRcrea decline were used: 3 mL/min/1.73m(2)/year or more ("Rapid3"; encompassing 34,874 cases, 107,090 controls) and eGFRcrea decline 25% or more and eGFRcrea under 60 mL/min/1.73m(2) at follow-up among those with eGFRcrea 60 mL/min/1.73m(2) or more at baseline ("CKDi25"; encompassing 19,901 cases, 175,244 controls). Seven independent variants were identified across six loci for Rapid3 and/or CKDi25: consisting of five variants at four loci with genome-wide significance (near UMOD-PDILT (2), PRKAG2, WDR72, OR2S2) and two variants among 265 known eGFRcrea variants (near GATM, LARP4B). All these loci were novel for Rapid3 and/or CKDi25 and our bioinformatic follow-up prioritized variants and genes underneath these loci. The OR2S2 locus is novel for any eGFRcrea trait including interesting candidates. For the five genome-wide significant lead variants, we found supporting effects for annual change in blood urea nitrogen or cystatin-based eGFR, but not for GATM or (LARP4B). Individuals at high compared to those at low genetic risk (8-14 vs. 0-5 adverse alleles) had a 1.20-fold increased risk of acute kidney injury (95% confidence interval 1.08-1.33). Thus, our identified loci for rapid kidney function decline may help prioritize therapeutic targets and identify mechanisms and individuals at risk for sustained deterioration of kidney function.
KW  - acute kidney injury
KW  - end-stage kidney disease
KW  - genome-wide association
KW  - study
KW  - rapid eGFRcrea decline
Y1  - 2020
U6  - https://doi.org/10.1016/j.kint.2020.09.030
SN  - 0085-2538
SN  - 1523-1755
VL  - 99
IS  - 4
SP  - 926
EP  - 939
PB  - Elsevier
CY  - New York
ER  - 
TY  - JOUR
A1  - Vladova, Gergana
A1  - Gronau, Norbert
T1  - KI-basierte Assistenzsysteme in betrieblichen Lernprozessen
JF  - Industrie 4.0 Management : Gegenwart und Zukunft industrieller Geschäftsprozesse
N2  - Assistenzsysteme finden im Kontext der digitalen Transformation immer mehr Einsatz. Sie können Beschäftigte in industriellen Produktionsprozessen sowohl in der Anlern- als auch in der aktiven Arbeitsphase unterstützen. Kompetenzen können so arbeitsplatz- und prozessnah sowie bedarfsorientiert aufgebaut werden. In diesem Beitrag wird der aktuelle Forschungsstand zu den Einsatzmöglichkeiten dieser Assistenzsysteme diskutiert und mit Beispielen illustriert. Es werden unter anderem auch Herausforderungen für den Einsatz aufgezeigt. Am Ende des Beitrags werden Potenziale für die zukünftige Nutzung von AS in industriellen Lernprozessen und für die Forschung identifiziert.
KW  - KI
KW  - kognitive Assistenzsysteme
KW  - betriebliche Lernprozesse
KW  - Weiterbildung
Y1  - 2022
U6  - https://doi.org/10.30844/I40M_22-2_11-14
SN  - 2364-9216
SN  - 2364-9208
VL  - 38
IS  - 2
SP  - 11
EP  - 14
PB  - GITO mbH Verlag für Industrielle Informationstechnik und Organisation
CY  - Berlin
ER  - 
TY  - JOUR
A1  - Ahnen, M. L.
A1  - Ansoldi, S.
A1  - Antonelli, L. A.
A1  - Arcaro, C.
A1  - Babie, A.
A1  - Banerjee, B.
A1  - Bangale, P.
A1  - de Almeida, U. Barres
A1  - Barrio, J. A.
A1  - Gonzalez, J. Becerra
A1  - Bednarek, W.
A1  - Bernardini, E.
A1  - Berti, A.
A1  - Biasuzzi, B.
A1  - Biland, A.
A1  - Blanch, O.
A1  - Bonnefoy, S.
A1  - Bonnoli, G.
A1  - Borracci, F.
A1  - Carosi, R.
A1  - Carosi, A.
A1  - Chatterjee, A.
A1  - Colin, P.
A1  - Colombo, E.
A1  - Contreras, J. L.
A1  - Cortina, J.
A1  - Covino, S.
A1  - Cumani, P.
A1  - Da Vela, P.
A1  - Dazzi, F.
A1  - De Angelis, A.
A1  - De Lotto, B.
A1  - Wilhelmi, E. de Ona
A1  - Di Pierro, F.
A1  - Doert, M.
A1  - Dominguez, A.
A1  - Prester, D. Dominis
A1  - Dorner, D.
A1  - Doro, M.
A1  - Einecke, S.
A1  - Glawion, D. Eisenacher
A1  - Elsaesser, D.
A1  - Engelkemeier, M.
A1  - Ramazani, V. Fallah
A1  - Fernandez-Barra, A.
A1  - Fidalgo, D.
A1  - Fonseca, M. V.
A1  - Font, L.
A1  - Fruck, C.
A1  - Galindo, D.
A1  - Lopez, R. J. Garcia
A1  - Garczarczyk, M.
A1  - Gaug, M.
A1  - Giammaria, P.
A1  - Godinovie, N.
A1  - Gora, D.
A1  - Griffiths, S.
A1  - Guberman, D.
A1  - Hadasch, D.
A1  - Hahn, A.
A1  - Hassan, T.
A1  - Hayashida, M.
A1  - Herrera, J.
A1  - Hose, J.
A1  - Hrupec, D.
A1  - Hughes, G.
A1  - Ishio, K.
A1  - Konno, Y.
A1  - Kubo, H.
A1  - Kushida, J.
A1  - Kuvezdie, D.
A1  - Lelas, D.
A1  - Lindfors, E.
A1  - Lombardi, S.
A1  - Longo, F.
A1  - Lopez, M.
A1  - Lopez-Oramas, A.
A1  - Majumdar, P.
A1  - Makariev, M.
A1  - Maneva, G.
A1  - Manganaro, M.
A1  - Mannheim, K.
A1  - Maraschi, L.
A1  - Mariotti, M.
A1  - Martinez, M.
A1  - Mazin, D.
A1  - Menzel, U.
A1  - Minev, M.
A1  - Mirzoyan, R.
A1  - Moralejo, A.
A1  - Moreno, V.
A1  - Moretti, E.
A1  - Munar-Adrover, P.
A1  - Neustroev, V.
A1  - Niedzwiecki, A.
A1  - Rosillo, M. Nievas
A1  - Nilsson, K.
A1  - Nishijima, K.
A1  - Noda, K.
A1  - Nogues, L.
A1  - Paiano, S.
A1  - Palacio, J.
A1  - Paneque, D.
A1  - Paoletti, R.
A1  - Paredes, J. M.
A1  - Paredes-Fortuny, X.
A1  - Pedaletti, G.
A1  - Peresano, M.
A1  - Perri, L.
A1  - Persic, M.
A1  - Moroni, P. G. Prada
A1  - Prandini, E.
A1  - Puljak, I.
A1  - Garcia, J. R.
A1  - Reichardt, I.
A1  - Rhode, W.
A1  - Riti, M.
A1  - Rico, J.
A1  - Saito, T.
A1  - Satalecka, K.
A1  - Schroeder, S.
A1  - Schweizer, T.
A1  - Shore, S. N.
A1  - Sillanpaa, A.
A1  - Sitarek, J.
A1  - Sobczynskall, D.
A1  - Stamerra, A.
A1  - Strzys, M.
A1  - Surie, T.
A1  - Takalo, L.
A1  - Tavecchio, F.
A1  - Temnikov, P.
A1  - Terzie, T.
A1  - Tescaro, D.
A1  - Teshima, M.
A1  - Torres, D. F.
A1  - Torres-Alla, N.
A1  - Treves, A.
A1  - Vanzo, G.
A1  - Acosta, M. Vazquez
A1  - Vovk, I.
A1  - Ward, J. E.
A1  - Will, M.
A1  - Wu, M. H.
A1  - Zarie, D.
A1  - Abdalla, Hassan E.
A1  - Abramowski, A.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Akhperjanian, A. G.
A1  - Andersson, T.
A1  - Angüner, Ekrem Oǧuzhan
A1  - Arakawa, M.
A1  - Arrieta, M.
A1  - Aubert, P.
A1  - Backes, M.
A1  - Balzer, A.
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Tjus, J. Becker
A1  - Berge, D.
A1  - Bernhard, S.
A1  - Bernlohr, K.
A1  - Blackwell, R.
A1  - Bottcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bordas, Pol
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Btichele, M.
A1  - Bulik, T.
A1  - Capasso, M.
A1  - Carr, J.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chalme-Calvet, R.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Chevalier, J.
A1  - Chretien, M.
A1  - Coffaro, M.
A1  - Colafrancesco, S.
A1  - Cologna, G.
A1  - Condon, B.
A1  - Conrad, J.
A1  - Cui, Y.
A1  - Davids, I. D.
A1  - Decock, J.
A1  - Degrange, B.
A1  - Dei, C.
A1  - Devin, J.
A1  - Dewilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Domainko, W.
A1  - Donath, A.
A1  - Dutson, K.
A1  - Dyks, J.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Eger, P.
A1  - Ernenwein, J. -P.
A1  - Eschbach, S.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Fernandes, M. V.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Forster, A.
A1  - Funk, S.
A1  - Ftifiling, M.
A1  - Gabici, S.
A1  - Gajdus, M.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Giavitto, G.
A1  - Giebels, B.
A1  - Glicenstein, J. F.
A1  - Gottschal, D.
A1  - Goya, A.
A1  - Grondin, M. -H.
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Hawkes, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hervet, O.
A1  - Hinton, J. A.
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holler, M.
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Iwasaki, H.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Janiak, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jingo, M.
A1  - Jogler, T.
A1  - Jouvin, L.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzyfiski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Kerszberg, D.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - Kieffer, M.
A1  - King, J.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluiniak, W.
A1  - Kolitzus, D.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Kraus, M.
A1  - Krtiger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lees, J. -P.
A1  - Lefaucheur, J.
A1  - Lefranc, V.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Leser, Eva
A1  - Lohse, T.
A1  - Lorentz, M.
A1  - Liu, R.
A1  - Lopez-Coto, R.
A1  - Lypova, I.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - Meintjes, P. J.
A1  - Meyer, M.
A1  - Mitche, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Nakashima, S.
A1  - De Naurois, M.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Ott, S.
A1  - Ohm, S.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Padovani, M.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perennes, C.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Pie, Q.
A1  - Pita, S.
A1  - Poon, H.
A1  - Prokhorov, D.
A1  - Prokoph, H.
A1  - Ptffilhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - De Los Reyes, R.
A1  - Richter, S.
A1  - Rieger, F.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Safi-Harb, S.
A1  - Sahakian, V.
A1  - Saito, S.
A1  - Salek, D.
A1  - Sanchez, D. A.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schtissler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Settimo, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I.
A1  - Simoni, R.
A1  - So, H.
A1  - Spanier, F.
A1  - Spengler, G.
A1  - Spies, F.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Stycz, K.
A1  - Sushch, I.
A1  - Takahashi, T.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tibaldo, L.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - Van der Walt, D. J.
A1  - Van Eldik, C.
A1  - Van Rensburg, C.
A1  - Van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Vok, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Wornlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zabalza, V.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Ziegler, A.
A1  - Zywuckan, N.
T1  - Constraints on particle acceleration in SS433/W50 from MAGIC and HESS observations
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. The large jet kinetic power and non-thermal processes occurring in the microquasar SS 433 make this source a good candidate for a very high-energy (VHE) gamma-ray emitter. Gamma-ray fluxes above the sensitivity limits of current Cherenkov telescopes have been predicted for both the central X-ray binary system and the interaction regions of SS 433 jets with the surrounding W50 nebula. Non-thermal emission at lower energies has been previously reported, indicating that efficient particle acceleration is taking place in the system. Aims. We explore the capability of SS 433 to emit VHE gamma rays during periods in which the expected flux attenuation due to periodic eclipses (P-orb similar to 13.1 days) and precession of the circumstellar disk (P-pre similar to 162 days) periodically covering the central binary system is expected to be at its minimum. The eastern and western SS 433/W50 interaction regions are also examined using the whole data set available. We aim to constrain some theoretical models previously developed for this system with our observations. Methods. We made use of dedicated observations from the Major Atmospheric Gamma Imaging Cherenkov telescopes (MAGIC) and High Energy Spectroscopic System (H.E.S.S.) of SS 433 taken from 2006 to 2011. These observation were combined for the first time and accounted for a total effective observation time of 16.5 h, which were scheduled considering the expected phases of minimum absorption of the putative VHE emission. Gamma-ray attenuation does not affect the jet/medium interaction regions. In this case, the analysis of a larger data set amounting to similar to 40-80 h, depending on the region, was employed. Results. No evidence of VHE gamma-ray emission either from the central binary system or from the eastern/western interaction regions was found. Upper limits were computed for the combined data set. Differential fluxes from the central system are found to be less than or similar to 10(-12)-10(-13) TeV-1 cm(-2) s(-1) in an energy interval ranging from similar to few x 100 GeV to similar to few TeV. Integral flux limits down to similar to 10(-12)-10(-13) ph cm(-2) s(-1) and similar to 10(-13)-10(-14) ph cm(-2) s(-1) are obtained at 300 and 800 GeV, respectively. Our results are used to place constraints on the particle acceleration fraction at the inner jet regions and on the physics of the jet/medium interactions. Conclusions. Our findings suggest that the fraction of the jet kinetic power that is transferred to relativistic protons must be relatively small in SS 433, q(p) <= 2.5 x 10(-5), to explain the lack of TeV and neutrino emission from the central system. At the SS 433/W50 interface, the presence of magnetic fields greater than or similar to 10 mu G is derived assuming a synchrotron origin for the observed X-ray emission. This also implies the presence of high-energy electrons with E-e up to 50 TeV, preventing an efficient production of gamma-ray fluxes in these interaction regions.
KW  - gamma rays: general
KW  - stars: black holes
KW  - X-rays: binaries
KW  - ISM: jets and outflows
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201731169
SN  - 1432-0746
VL  - 612
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Abdalla, Hassan E.
A1  - Collaboration, H. E. S. S.
A1  - Abramowski, A.
A1  - Aharonian, Felix A.
A1  - Benkhali, F. Ait
A1  - Angüner, Ekrem Oǧuzhan
A1  - Arakawa, M.
A1  - Armand, C.
A1  - Arrieta, M.
A1  - Backes, M.
A1  - Balzer, A.
A1  - Barnard, M.
A1  - Becherini, Y.
A1  - Tjus, J. Becker
A1  - Berge, D.
A1  - Bernhard, S.
A1  - Bernloehr, K.
A1  - Blackwell, R.
A1  - Bottcher, M.
A1  - Boisson, C.
A1  - Bolmont, J.
A1  - Bonnefoy, S.
A1  - Bordas, Pol
A1  - Bregeon, J.
A1  - Brun, F.
A1  - Brun, P.
A1  - Bryan, M.
A1  - Buechele, M.
A1  - Bulik, T.
A1  - Capasso, M.
A1  - Caroff, S.
A1  - Carosi, A.
A1  - Casanova, Sabrina
A1  - Cerruti, M.
A1  - Chakraborty, N.
A1  - Chaves, R. C. G.
A1  - Chen, A.
A1  - Chevalier, J.
A1  - Colafrancesco, S.
A1  - Condon, B.
A1  - Conrad, J.
A1  - Davids, I. D.
A1  - Decock, J.
A1  - Deil, C.
A1  - Devin, J.
A1  - deWilt, P.
A1  - Dirson, L.
A1  - Djannati-Atai, A.
A1  - Donath, A.
A1  - Dyks, J.
A1  - Edwards, T.
A1  - Egberts, Kathrin
A1  - Emery, G.
A1  - Ernenwein, J. -P.
A1  - Eschbach, S.
A1  - Farnier, C.
A1  - Fegan, S.
A1  - Fernandes, M. V.
A1  - Fiasson, A.
A1  - Fontaine, G.
A1  - Funk, S.
A1  - Fuessling, M.
A1  - Gabici, S.
A1  - Gallant, Y. A.
A1  - Garrigoux, T.
A1  - Gate, F.
A1  - Giavitto, G.
A1  - Glawion, D.
A1  - Glicenstein, J. F.
A1  - Gottschall, D.
A1  - Grondin, M. -H.
A1  - Hahn, J.
A1  - Haupt, M.
A1  - Hawkes, J.
A1  - Heinzelmann, G.
A1  - Henri, G.
A1  - Hermann, G.
A1  - Hinton, J. A.
A1  - Hofmann, W.
A1  - Hoischen, Clemens
A1  - Holch, T. L.
A1  - Holler, M.
A1  - Horns, D.
A1  - Ivascenko, A.
A1  - Iwasaki, H.
A1  - Jacholkowska, A.
A1  - Jamrozy, M.
A1  - Jankowsky, D.
A1  - Jankowsky, F.
A1  - Jingo, M.
A1  - Jouvin, L.
A1  - Jung-Richardt, I.
A1  - Kastendieck, M. A.
A1  - Katarzynski, K.
A1  - Katsuragawa, M.
A1  - Katz, U.
A1  - Kerszberg, D.
A1  - Khangulyan, D.
A1  - Khelifi, B.
A1  - King, J.
A1  - Klepser, S.
A1  - Klochkov, D.
A1  - Kluzniak, W.
A1  - Komin, Nu.
A1  - Kosack, K.
A1  - Krakau, S.
A1  - Kraus, M.
A1  - Kruger, P. P.
A1  - Laffon, H.
A1  - Lamanna, G.
A1  - Lau, J.
A1  - Lefaucheur, J.
A1  - Lemiere, A.
A1  - Lemoine-Goumard, M.
A1  - Lenain, J. -P.
A1  - Leser, Eva
A1  - Lohse, T.
A1  - Lorentz, M.
A1  - Liu, R.
A1  - Lopez-Coto, R.
A1  - Lypova, I.
A1  - Malyshev, D.
A1  - Marandon, V.
A1  - Marcowith, Alexandre
A1  - Mariaud, C.
A1  - Marx, R.
A1  - Maurin, G.
A1  - Maxted, N.
A1  - Mayer, M.
A1  - Meintjes, P. J.
A1  - Meyer, M.
A1  - Mitchell, A. M. W.
A1  - Moderski, R.
A1  - Mohamed, M.
A1  - Mohrmann, L.
A1  - Mora, K.
A1  - Moulin, Emmanuel
A1  - Murach, T.
A1  - Nakashima, S.
A1  - de Naurois, M.
A1  - Ndiyavala, H.
A1  - Niederwanger, F.
A1  - Niemiec, J.
A1  - Oakes, L.
A1  - Odaka, H.
A1  - Ohm, S.
A1  - Ostrowski, M.
A1  - Oya, I.
A1  - Padovani, M.
A1  - Panter, M.
A1  - Parsons, R. D.
A1  - Pekeur, N. W.
A1  - Pelletier, G.
A1  - Perennes, C.
A1  - Petrucci, P. -O.
A1  - Peyaud, B.
A1  - Piel, Q.
A1  - Pita, S.
A1  - Poireau, V.
A1  - Prokhorov, D. A.
A1  - Prokoph, H.
A1  - Puehlhofer, G.
A1  - Punch, M.
A1  - Quirrenbach, A.
A1  - Raab, S.
A1  - Rauth, R.
A1  - Reimer, A.
A1  - Reimer, O.
A1  - Renaud, M.
A1  - de los Reyes, R.
A1  - Rieger, F.
A1  - Rinchiuso, L.
A1  - Romoli, C.
A1  - Rowell, G.
A1  - Rudak, B.
A1  - Rulten, C. B.
A1  - Sahakian, V.
A1  - Saito, S.
A1  - Sanchez, D. A.
A1  - Santangelo, Andrea
A1  - Sasaki, M.
A1  - Schlickeiser, R.
A1  - Schussler, F.
A1  - Schulz, A.
A1  - Schwanke, U.
A1  - Schwemmer, S.
A1  - Seglar-Arroyo, M.
A1  - Seyffert, A. S.
A1  - Shafi, N.
A1  - Shilon, I.
A1  - Shiningayamwe, K.
A1  - Simoni, R.
A1  - Sol, H.
A1  - Spanier, F.
A1  - Spir-Jacob, M.
A1  - Stawarz, L.
A1  - Steenkamp, R.
A1  - Stegmann, Christian
A1  - Steppa, Constantin Beverly
A1  - Sushch, I.
A1  - Takahashi, T.
A1  - Tavernet, J. -P.
A1  - Tavernier, T.
A1  - Taylor, A. M.
A1  - Terrier, R.
A1  - Tibaldo, L.
A1  - Tiziani, D.
A1  - Tluczykont, M.
A1  - Trichard, C.
A1  - Tsirou, M.
A1  - Tsuji, N.
A1  - Tuffs, R.
A1  - Uchiyama, Y.
A1  - van der Walt, D. J.
A1  - van Eldik, C.
A1  - van Rensburg, C.
A1  - van Soelen, B.
A1  - Vasileiadis, G.
A1  - Veh, J.
A1  - Venter, C.
A1  - Viana, A.
A1  - Vincent, P.
A1  - Vink, J.
A1  - Voisin, F.
A1  - Voelk, H. J.
A1  - Vuillaume, T.
A1  - Wadiasingh, Z.
A1  - Wagner, S. J.
A1  - Wagner, P.
A1  - Wagner, R. M.
A1  - White, R.
A1  - Wierzcholska, A.
A1  - Willmann, P.
A1  - Woernlein, A.
A1  - Wouters, D.
A1  - Yang, R.
A1  - Zaborov, D.
A1  - Zacharias, M.
A1  - Zanin, R.
A1  - Zdziarski, A. A.
A1  - Zech, Alraune
A1  - Zefi, F.
A1  - Ziegler, A.
A1  - Zorn, J.
A1  - Zywucka, N.
T1  - Detection of variable VHE gamma-ray emission from the extra-galactic gamma-ray binary LMC P3
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Recently, the high-energy (HE, 0.1-100 GeV) gamma-ray emission from the object LMC P3 in the Large Magellanic Cloud (LMC) has been discovered to be modulated with a 10.3-day period, making it the first extra-galactic gamma-ray binary. Aims. This work aims at the detection of very-high-energy (VHE, >100 GeV) gamma-ray emission and the search for modulation of the VHE signal with the orbital period of the binary system. Methods. LMC P3 has been observed with the High Energy Stereoscopic System (H.E.S.S.); the acceptance-corrected exposure time is 100 h. The data set has been folded with the known orbital period of the system in order to test for variability of the emission. Results. VHE gamma-ray emission is detected with a statistical significance of 6.4 sigma. The data clearly show variability which is phase-locked to the orbital period of the system. Periodicity cannot be deduced from the H.E.S.S. data set alone. The orbit-averaged luminosity in the 1-10 TeV energy range is (1.4 +/- 0.2) x 10(35) erg s(-1). A luminosity of (5 +/- 1) x 10(35) erg s(-1) is reached during 20% of the orbit. HE and VHE gamma-ray emissions are anti-correlated. LMC P3 is the most luminous gamma-ray binary known so far.
KW  - gamma rays: stars
KW  - binaries: general
KW  - stars: massive
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201732426
SN  - 1432-0746
VL  - 610
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - GEN
A1  - Braun, David R.
A1  - Aldeias, Vera
A1  - Archer, Will
A1  - Arrowsmith, J. Ramon
A1  - Baraki, Niguss
A1  - Campisano, Christopher J.
A1  - Deino, Alan L.
A1  - DiMaggio, Erin N.
A1  - Dupont-Nivet, Guillaume
A1  - Engda, Blade
A1  - Feary, David A.
A1  - Garello, Dominique I.
A1  - Kerfelew, Zenash
A1  - McPherron, Shannon P.
A1  - Patterson, David B.
A1  - Reeves, Jonathan S.
A1  - Thompson, Jessica C.
A1  - Reed, Kaye E.
T1  - Reply to Sahle and Gossa: Technology and geochronology at the earliest known Oldowan site at Ledi-Geraru, Ethiopia
T2  - Proceedings of the National Academy of Sciences of the United States of America
Y1  - 2019
U6  - https://doi.org/10.1073/pnas.1911952116
SN  - 0027-8424
N1  - Letter
VL  - 116
IS  - 41
SP  - 20261
EP  - 20262
PB  - National Acad. of Sciences
CY  - Washington
ER  - 
TY  - JOUR
A1  - Bender, Benedict
A1  - Lewandowski, Stefanie
T1  - Potenziale plattformbasierter Geschäftsmodelle im Kunststoffspritzguss
T1  - Potential of platform-based business models in the plastics industry
JF  - Industrie 4.0 Management : Gegenwart und Zukunft industrieller Geschäftsprozesse
N2  - Die Potenziale plattformbasierter Geschäftsmodelle im Kontext von Industrie 4.0 sind bisher nicht vollständig erschlossen. Ansatzpunkte für Plattformen und ökosystembasierte Wertschöpfung variieren zwischen Industrien. Die Kunststoffindustrie ist dahingehend bisher weitestgehend unberücksichtigt. Aufgrund der Industriestruktur, insb. der einheitlichen Wertschöpfungsstrukturen eignet sich die Kunststoffindustrie für den Einsatz digitaler Plattformen. Neben Ansätzen für Plattformen in der Spritzgussindustrie bietet der Beitrag ein Vorgehensmodell für die Erweiterung etablierte Geschäftsmodelle. Somit kann der Einstieg in plattformbasierte Geschäftsmodelle für KMUs erleichtert werden.
N2  - The potential of platform-based business models in the context of Industry 4.0 has not yet been fully realized. Approaches for platforms and ecosystem-based value creation vary between industries. The plastics industry has so far been widely ignored in this respect. Due to its industrial structure, in particular the uniform value creation structures, the plastics industry is suitable for digital platforms. In addition to approaches for platforms in the injection molding industry, the article offers a procedure model for the expansion of established business models. This can facilitate the entry into the field of platform-based business models for SMEs.
KW  - Digitale Plattformen
KW  - plattformbasierte Geschäftsmodelle
KW  - Kunststoffindustrie
KW  - Plattform Ökosystem
KW  - Potenziale
KW  - Industrie 4.0
KW  - digital platforms
KW  - platform-based business models
KW  - plastics industry
KW  - platform ecosystem
KW  - potentials
KW  - Industry 4.0
Y1  - 2022
U6  - https://doi.org/10.30844/IM_22-6_14-18
SN  - 2364-9208
SN  - 2364-9216
VL  - 38
IS  - 6
SP  - 14
EP  - 18
PB  - GITO mbH Verlag
CY  - Berlin
ER  - 
TY  - JOUR
A1  - Ganghof, Steffen
A1  - Eppner, Sebastian
A1  - Pörschke, Alexander
T1  - Australian bicameralism as semi-parliamentarism
BT  - patterns of majority formation in 29 democracies
JF  - Australian Journal of Political Science
N2  - The article analyses the type of bicameralism we find in Australia as a distinct executive-legislative system – a hybrid between parliamentary and presidential government – which we call ‘semi-parliamentary government’. We argue that this hybrid presents an important and underappreciated alternative to pure parliamentary government as well as presidential forms of the power-separation, and that it can achieve a certain balance between competing models or visions of democracy. We specify theoretically how the semi-parliamentary separation of powers contributes to the balancing of democratic visions and propose a conceptual framework for comparing democratic visions. We use this framework to locate the Australian Commonwealth, all Australian states and 22 advanced democratic nation-states on a two-dimensional empirical map of democratic patterns for the period from 1995 to 2015.
KW  - Executive-legislative relations
KW  - bicameralism
KW  - parliamentary government
KW  - presidential government
KW  - visions of democracy
Y1  - 2018
U6  - https://doi.org/10.1080/10361146.2018.1451487
SN  - 1036-1146
SN  - 1363-030X
VL  - 53
IS  - 2
SP  - 211
EP  - 233
PB  - Routledge, Taylor & Francis Group
CY  - Abingdon
ER  - 
TY  - JOUR
A1  - Deino, Alan L.
A1  - Sier, Mark Jan
A1  - Garello, Dominique
A1  - Keller, B.
A1  - Kingston, John
A1  - Scott, Jennifer J.
A1  - Dupont-Nivet, Guillaume
A1  - Cohen, Andrew
T1  - Chronostratigraphy of the Baringo-Tugen-Barsemoi (HSPDP-BTB13-1A) core-Ar-40/Ar-39 dating, magnetostratigraphy, tephrostratigraphy, sequence stratigraphy and Bayesian age modeling
JF  - Palaeogeography, palaeoclimatology, palaeoecology : an international journal for the geo-sciences
N2  - The Baringo-Tugen-Barsemoi 2013 drillcore (BTB13), acquired as part of the Hominin Sites and Paleolakes Drilling Project, recovered 228 m of fluviolacustrine sedimentary rocks and tuffs spanning a similar to 3.29-2.56 Ma interval of the highly fossiliferous and hominin-bearing Chemeron Formation, Tugen Hills, Kenya. Here we present a Bayesian stratigraphic age model for the core employing chronostratigraphic control points derived from Ar-40/Ar-39 dating of tuffs from core and outcrop, Ar-40/Ar-39 age calibration of related outcrop diatomaceous units, and core magnetostratigraphy. The age model reveals three main intervals with distinct sediment accumulation rates: an early rapid phase from 3.2 to 2.9 Ma; a relatively slow phase from 2.9 to 2.7 Ma; and the highest rate of accumulation from 2.7 to 2.6 Ma. The intervals of rapid accumulation correspond to periods of high Earth orbital eccentricity, whereas the slow accumulation interval corresponds to low eccentricity at 2.9-2.7 Ma, suggesting that astronomically mediated climate processes may be responsible for the observed changes in sediment accumulation rate. Lacustrine transgression-regression events, as delineated using sequence stratigraphy, dominantly operate on precession scale, particularly within the high eccentricity periods. A set of erosively based fluvial conglomerates correspond to the 2.9-2.7 Ma interval, which could be related to either the depositional response to low eccentricity or to the development of unconformities due to local tectonic activity. Age calibration of core magnetic susceptibility and gamma density logs indicates a close temporal correspondence between a shift from high- to low-frequency signal variability at similar to 3 Ma, approximately coincident the end of the mid-Piacenzian Warm Period, and the beginning of the cooling of world climate leading to the initiation of Northern Hemispheric glaciation c. 2.7 Ma. BTB13 and the Baringo Basin records may thus provide evidence of a connection between high-latitude glaciation and equatorial terrestrial climate toward the end of the Pliocene.
KW  - Chemeron Formation
KW  - Pliocene
KW  - Eccentricity
KW  - Precession
KW  - Paleoclimate
KW  - Paleolimnology
Y1  - 2019
U6  - https://doi.org/10.1016/j.palaeo.2019.109258
SN  - 0031-0182
SN  - 1872-616X
VL  - 532
PB  - Elsevier
CY  - Amsterdam
ER  - 
TY  - JOUR
A1  - Mühlenbruch, Marco
A1  - Grossart, Hans-Peter
A1  - Eigemann, Falk
A1  - Voss, Maren
T1  - Mini-review: Phytoplankton-derived polysaccharides in the marine environment and their interactions with heterotrophic bacteria
JF  - Environmental microbiology
N2  - Within the wealth of molecules constituting marine dissolved organic matter, carbohydrates make up the largest coherent and quantifiable fraction. Their main sources are from primary producers, which release large amounts of photosynthetic products – mainly polysaccharides – directly into the surrounding water via passive and active exudation. The organic carbon and other nutrients derived from these photosynthates enrich the ‘phycosphere’ and attract heterotrophic bacteria. The rapid uptake and remineralization of dissolved free monosaccharides by heterotrophic bacteria account for the barely detectable levels of these compounds. By contrast, dissolved combined polysaccharides can reach high concentrations, especially during phytoplankton blooms. Polysaccharides are too large to be taken up directly by heterotrophic bacteria, instead requiring hydrolytic cleavage to smaller oligo- or monomers by bacteria with a suitable set of exoenzymes. The release of diverse polysaccharides by various phytoplankton taxa is generally interpreted as the deposition of excess organic material. However, these molecules likely also fulfil distinct, yet not fully understood functions, as inferred from their active modulation in terms of quality and quantity when phytoplankton becomes nutrient limited or is exposed to heterotrophic bacteria. This minireview summarizes current knowledge regarding the exudation and composition of phytoplankton-derived exopolysaccharides and acquisition of these compounds by heterotrophic bacteria.
Y1  - 2018
U6  - https://doi.org/10.1111/1462-2920.14302
SN  - 1462-2912
SN  - 1462-2920
VL  - 20
IS  - 8
SP  - 2671
EP  - 2685
PB  - Wiley
CY  - Hoboken
ER  - 
TY  - JOUR
A1  - Rojas-Jimenez, Keilor
A1  - Fonvielle, Jeremy Andre
A1  - Ma, Hua
A1  - Grossart, Hans-Peter
T1  - Transformation of humic substances by the freshwater Ascomycete Cladosporium sp.
JF  - Waterbird
N2  - The ecological relevance of fungi in freshwater ecosystems is becoming increasingly evident, particularly in processing the extensive amounts of polymeric organic carbon such as cellulose, chitin, and humic substances (HS). We isolated several fungal strains from oligo-mesotrophic Lake Stechlin, Brandenburg, Germany, and analyzed their ability to degrade polymeric-like substrates. Using liquid chromatography-organic carbon detection, we determined the byproducts of HS transformation by the freshwater fungus Cladosporium sp. KR14. We demonstrate the ability of this fungus to degrade and simultaneously synthesize HS, and that transformation processes were intensified when iron, as indicator of the occurrence of Fenton reactions, was present in the medium. Furthermore, we showed that structural complexity of the HS produced changed with the availability of other polymeric substances in the medium. Our study highlights the contribution of freshwater Ascomycetes to the transformation of complex organic compounds. As such, it has important implications for understanding the ecological contribution of fungi to aquatic food webs and related biogeochemical cycles.
Y1  - 2017
U6  - https://doi.org/10.1002/lno.10545
SN  - 1524-4695
SN  - 1938-5390
VL  - 40
SP  - 282
EP  - 288
PB  - Waterbird SOC
CY  - Washington
ER  - 
TY  - JOUR
A1  - Perscheid, Michael
A1  - Plattner, Hasso
A1  - Ritter, Daniel
A1  - Schlosser, Rainer
A1  - Teusner, Ralf
T1  - Enterprise platform and integration concepts research at HPI
JF  - SIGMOD record
N2  - The Hasso Plattner Institute (HPI), academically structured as the independent Faculty of Digital Engineering at the University of Potsdam, unites computer science research and teaching with the advantages of a privately financed institute and a tuition-free study program. Founder and namesake of the institute is the SAP co-founder Hasso Plattner, who also heads the Enterprise Platform and Integration Concepts (EPIC) research center which focuses on the technical aspects of business software with a vision to provide the fastest way to get insights out of enterprise data. Founded in 2006, the EPIC combines three research groups comprising autonomous data management, enterprise software engineering, and data-driven decision support.
Y1  - 2023
U6  - https://doi.org/10.1145/3582302.3582322
SN  - 0163-5808
SN  - 1943-5835
VL  - 51
IS  - 4
SP  - 68
EP  - 73
PB  - Association for Computing Machinery
CY  - New York
ER  - 
TY  - JOUR
A1  - Schmalzgruber, Hedwig
T1  - Niklas Holzberg, Avian/Romulus. Fabelsammlungen der Spätantike, lateinisch – deutsch, Sammlung Tusculum, Berlin-Boston: De Gruyter, 2022, 237
pp., 39.95 €, ISBN 978-3-11-075705-7, https://doi.org/10.1515/9783110757064
JF  - Exemplaria classica
Y1  - 2022
SN  - 1699-3225
SN  - 2173-6839
VL  - 26
SP  - 390
EP  - 397
PB  - Universidad de Huelva
CY  - Huelva
ER  - 
TY  - GEN
A1  - Brand, Ralf
A1  - Timme, Sinika
T1  - Physical inactivity or exercise? A simple decision test predicts exercise behavior over the next 14 days
T2  - Journal of sport & exercise psychology
Y1  - 2022
U6  - https://doi.org/10.1123/jsep.2022-0071
SN  - 0895-2779
SN  - 1543-2904
VL  - 44
IS  - S1
SP  - S68
EP  - S68
PB  - Human Kinetics Publishing
CY  - Champaign
ER  - 
TY  - RPRT
A1  - Angenendt, Steffen
A1  - Koch, Anne
A1  - Tjaden, Jasper
T1  - Predicting irregular migration
BT  - SWP research paper
T2  - high hopes, meagre results
N2  - German and European migration policy operates in permanent crisis mode. Sudden increases in irregular immigration create a sense of loss of control, which is instrumentalised by populist forces. This has generated great interest in quantitative migration predictions. High expectations are placed in the AI-based tools currently under devel&#x00ad;op&#x00ad;ment for forecasting irregular migration. The potential applications of these tools are manifold. They range from managing and strengthening the EU's reception capacity and border protections to configuring humanitarian aid provision and longer-term planning of development programmes. There is a significant gap between the expectations placed in the new instruments and their practical utility. Technical limits exist, medium-term forecasts are methodologically implausible, and channels for feeding the results into political decision-making processes are lacking. The great demand for predictions is driven by the political functions of migration prediction, which include its uses in political communication, funding acquisition and legitimisation of political decisions. Investment in the quality of the underlying data will be more productive than developing a succession of new prediction tools. Funding for applications in emergency relief and development cooperation should be prioritised. Crisis early warning and risk analysis should also be strengthened and their networking improved.
KW  - Migration
KW  - Migrationspolitik
KW  - Wanderungsprognosen
KW  - Vorhersage
KW  - Vorausschau
KW  - displacement forecasting
KW  - Krisenfrüherkennung
KW  - Risikoanalyse
KW  - Künstliche Intelligenz
KW  - maschinelles Lernen
KW  - Agentenbasierte Modellierung
KW  - predicting irregular migration
KW  - forecast
KW  - quantitative migration prediction
KW  - UNHCR
KW  - IOM
KW  - Frontex Risk Analysis Network (FRAN)
KW  - Common Integrated Risk Analysis Model (CIRAM)
KW  - Emergency Response Coordination Centre (ERCC)
KW  - Frontex
KW  - Pact on Migration and Asylum
Y1  - 2023
U6  - https://doi.org/10.18449/2023RP11
SN  - 2747-5115
SN  - 1611-6372
VL  - 11
PB  - Stiftung Wissenschaft und Politik (SWP)
CY  - Berlin
ER  - 
TY  - RPRT
A1  - Angenendt, Steffen
A1  - Koch, Anne
A1  - Tjaden, Jasper
T1  - Die Prognose ungeregelter Wanderungen
BT  - große Erwartungen, begrenzter Nutzen
T2  - SWP-Studie
N2  - Die deutsche und europäische Migrationspolitik befindet sich im permanenten Krisenmodus. Plötzliche Anstiege ungeregelter Zuwanderung nähren ein Gefühl von Kontrollverlust, das wiederum von populistischen Kräften instrumentalisiert wird. Daher hat die Politik großes Interesse an quantitativen Migrationsprognosen. Besondere Erwartungen wecken KI-gestützte Instrumente zur Vorhersage ungeregelter Wanderungsbewegungen, wie sie zurzeit entwickelt werden. Die Anwendungsfelder dieser Instrumente sind vielfältig. Sie reichen von einer Stärkung der Aufnahmekapazitäten in der EU über die präventive Verschärfung von Grenzschutzmaßnahmen und eine bedarfsgerechte Bereitstellung von Ressourcen in humanitären Krisen bis zur längerfristigen entwicklungspolitischen Programmplanung. Allerdings besteht eine deutliche Kluft zwischen den Erwartungen an die neuen Instrumente und ihrem praktischen Mehrwert. Zum einen sind die technischen Möglichkeiten begrenzt, und mittelfristige Vorhersagen zu ungeregelten Wanderungen sind methodisch kaum möglich. Zum anderen mangelt es an Verfahren, um die Ergebnisse in politische Entscheidungsprozesse einfließen zu lassen. Die hohe Nachfrage nach Prognosen erklärt sich aus den politischen Funktionen quantitativer Migrationsvorhersage - beispielsweise ihrem Potential für die politische Kommunikation, die Mitteleinwerbung und die Legitimierung politischer Entscheidungen. Investitionen in die Qualität der den Prognosen zugrunde liegenden Daten sind sinnvoller als die Entwicklung immer neuer Instrumente. Bei der Mittelvergabe für Prognosen sollten Anwendungen in der Nothilfe und der Entwicklungszusammenarbeit priorisiert werden. Zudem sollten die Krisenfrüherkennung und die Risikoanalyse gestärkt werden, und die beteiligten Akteure sollten sich besser vernetzen.
KW  - Migration
KW  - Migrationspolitik
KW  - Wanderungsprognosen
KW  - Vorhersage
KW  - Vorausschau
KW  - Displacement Forecasting
KW  - Krisenfrüherkennung
KW  - Risikoanalyse
KW  - Künstliche Intelligenz
KW  - maschinelles Lernen
KW  - Agentenbasierte Modellierung
Y1  - 2023
U6  - https://doi.org/10.18449/2023S10
SN  - 2747-5115
SN  - 1611-6372
VL  - 10
PB  - Stiftung Wissenschaft und Politik (SWP)
CY  - Berlin
ER  - 
TY  - JOUR
A1  - Zhu, Hui
A1  - Chen, Lunjin
A1  - Liu, Xu
A1  - Shprits, Yuri
T1  - Modulation of locally generated equatorial noise by ULF wave
JF  - Journal of geophysical research : Space physics
N2  - In this paper we report a rare and fortunate event of fast magnetosonic (MS, also called equatorial noise) waves modulated by compressional ultralow frequency (ULF) waves measured by Van Allen Probes. The characteristics of MS waves, ULF waves, proton distribution, and their potential correlations are analyzed. The results show that ULF waves can modulate the energetic ring proton distribution and in turn modulate the MS generation. Furthermore, the variation of MS intensities is attributed to not only ULF wave activities but also the variation of background parameters, for example, number density. The results confirm the opinion that MS waves are generated by proton ring distribution and propose a new modulation phenomenon.
Y1  - 2019
U6  - https://doi.org/10.1029/2018JA026199
SN  - 2169-9380
SN  - 2169-9402
VL  - 124
IS  - 4
SP  - 2779
EP  - 2787
PB  - American Geophysical Union
CY  - Washington
ER  - 
TY  - JOUR
A1  - Cabalar, Pedro
A1  - Kaminski, Roland
A1  - Schaub, Torsten
A1  - Schuhmann, Anna
T1  - Temporal answer set programming on finite traces
JF  - Theory and practice of logic programming
N2  - In this paper, we introduce an alternative approach to Temporal Answer Set Programming that relies on a variation of Temporal Equilibrium Logic (TEL) for finite traces. This approach allows us to even out the expressiveness of TEL over infinite traces with the computational capacity of (incremental) Answer Set Programming (ASP). Also, we argue that finite traces are more natural when reasoning about action and change. As a result, our approach is readily implementable via multi-shot ASP systems and benefits from an extension of ASP's full-fledged input language with temporal operators. This includes future as well as past operators whose combination offers a rich temporal modeling language. For computation, we identify the class of temporal logic programs and prove that it constitutes a normal form for our approach. Finally, we outline two implementations, a generic one and an extension of the ASP system clingo.

Under consideration for publication in Theory and Practice of Logic Programming (TPLP)
Y1  - 2018
U6  - https://doi.org/10.1017/S1471068418000297
SN  - 1471-0684
SN  - 1475-3081
VL  - 18
IS  - 3-4
SP  - 406
EP  - 420
PB  - Cambridge Univ. Press
CY  - New York
ER  - 
TY  - GEN
A1  - Shprits, Yuri
A1  - Zhelavskaya, Irina
A1  - Green, Janet C.
A1  - Pulkkinen, Antti A.
A1  - Horne, Richard B.
A1  - Pitchford, David
A1  - Glover, Alexi
T1  - Discussions on Stakeholder Requirements for Space Weather-Related Models
T2  - Space Weather: The International Journal of Research and Applications
N2  - Participants of the 2017 European Space Weather Week in Ostend, Belgium, discussed the stakeholder requirements for space weather-related models. It was emphasized that stakeholders show an increased interest in space weather-related models. Participants of the meeting discussed particular prediction indicators that can provide first-order estimates of the impact of space weather on engineering systems.
KW  - 7924
KW  - 7934
KW  - 7959
Y1  - 2018
U6  - https://doi.org/10.1002/2018SW001864
SN  - 1542-7390
VL  - 16
IS  - 4
SP  - 341
EP  - 342
PB  - American Geophysical Union
CY  - Washington
ER  - 
TY  - GEN
A1  - Schaub, Torsten
A1  - Woltran, Stefan
T1  - Special issue on answer set programming
T2  - Künstliche Intelligenz
Y1  - 2018
U6  - https://doi.org/10.1007/s13218-018-0554-8
SN  - 0933-1875
SN  - 1610-1987
VL  - 32
IS  - 2-3
SP  - 101
EP  - 103
PB  - Springer
CY  - Heidelberg
ER  - 
TY  - JOUR
A1  - Zhelayskaya, Irina S.
A1  - Vasile, Ruggero
A1  - Shprits, Yuri
A1  - Stolle, Claudia
A1  - Matzka, Jürgen
T1  - Systematic Analysis of Machine Learning and Feature Selection Techniques for Prediction of the Kp Index
JF  - Space Weather: The International Journal of Research and Applications
N2  - The Kp index is a measure of the midlatitude global geomagnetic activity and represents short-term magnetic variations driven by solar wind plasma and interplanetary magnetic field. The Kp index is one of the most widely used indicators for space weather alerts and serves as input to various models, such as for the thermosphere and the radiation belts. It is therefore crucial to predict the Kp index accurately. Previous work in this area has mostly employed artificial neural networks to nowcast Kp, based their inferences on the recent history of Kp and on solar wind measurements at L1. In this study, we systematically test how different machine learning techniques perform on the task of nowcasting and forecasting Kp for prediction horizons of up to 12 hr. Additionally, we investigate different methods of machine learning and information theory for selecting the optimal inputs to a predictive model. We illustrate how these methods can be applied to select the most important inputs to a predictive model of Kp and to significantly reduce input dimensionality. We compare our best performing models based on a reduced set of optimal inputs with the existing models of Kp, using different test intervals, and show how this selection can affect model performance.
KW  - Kp index
KW  - Predictive models
KW  - Feature selection
KW  - Machine learning
KW  - Validation
Y1  - 2019
U6  - https://doi.org/10.1029/2019SW002271
SN  - 1542-7390
VL  - 17
IS  - 10
SP  - 1461
EP  - 1486
PB  - American Geophysical Union
CY  - Washington
ER  - 
TY  - JOUR
A1  - Rabl, Tilmann
T1  - Reminiscences on influential papers
JF  - SIGMOD record
N2  - When I started my PhD, I wanted to do something related to systems but I wasn't sure exactly what. I didn't consider data management systems initially, because I was unaware of the richness of the systems work that data management systems were build on. I thought the field was mainly about SQL. Luckily, that view changed quickly.
Y1  - 2023
U6  - https://doi.org/10.1145/3582302.3582310
SN  - 0163-5808
SN  - 1943-5835
VL  - 51
IS  - 4
SP  - 42
EP  - 44
PB  - Association for Computing Machinery
CY  - New York
ER  - 
TY  - JOUR
A1  - Shenar, Tomer
A1  - Sablowski, D. P.
A1  - Hainich, Rainer
A1  - Todt, Helge Tobias
A1  - Moffat, Anthony F. J.
A1  - Oskinova, Lidia M.
A1  - Ramachandran, Varsha
A1  - Sana, Hugues
A1  - Sander, Andreas Alexander Christoph
A1  - Schnurr, O.
A1  - St-Louis, N.
A1  - Vanbeveren, D.
A1  - Gotberg, Y.
A1  - Hamann, Wolf-Rainer
T1  - The Wolf-Rayet binaries of the nitrogen sequence in the Large Magellanic Cloud Spectroscopy, orbital analysis, formation, and evolution
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Massive Wolf-Rayet (WR) stars dominate the radiative and mechanical energy budget of galaxies and probe a critical phase in the evolution of massive stars prior to core collapse. It is not known whether core He-burning WR stars (classical WR; cWR) form predominantly through wind stripping (w-WR) or binary stripping (b-WR). Whereas spectroscopy of WR binaries has so-far largely been avoided because of its complexity, our study focuses on the 44 WR binaries and binary candidates of the Large Magellanic Cloud (LMC; metallicity Z approximate to 0.5 Z(circle dot)), which were identified on the basis of radial velocity variations, composite spectra, or high X-ray luminosities. Aims. Relying on a diverse spectroscopic database, we aim to derive the physical and orbital parameters of our targets, confronting evolution models of evolved massive stars at subsolar metallicity and constraining the impact of binary interaction in forming these stars. Methods. Spectroscopy was performed using the Potsdam Wolf-Rayet (PoWR) code and cross-correlation techniques. Disentanglement was performed using the code Spectangular or the shift-and-add algorithm. Evolutionary status was interpreted using the Binary Population and Spectral Synthesis (BPASS) code, exploring binary interaction and chemically homogeneous evolution. Results. Among our sample, 28/44 objects show composite spectra and are analyzed as such. An additional five targets show periodically moving WR primaries but no detected companions (SB1); two (BAT99 99 and 112) are potential WR + compact-object candidates owing to their high X-ray luminosities. We cannot confirm the binary nature of the remaining 11 candidates. About two-thirds of the WN components in binaries are identified as cWR, and one-third as hydrogen-burning WR stars. We establish metallicity-dependent mass-loss recipes, which broadly agree with those recently derived for single WN stars, and in which so-called WN3/O3 stars are clear outliers. We estimate that 45 +/- 30% of the cWR stars in our sample have interacted with a companion via mass transfer. However, only approximate to 12 +/- 7% of the cWR stars in our sample naively appear to have formed purely owing to stripping via a companion (12% b-WR). Assuming that apparently single WR stars truly formed as single stars, this comprises approximate to 4% of the whole LMC WN population, which is about ten times less than expected. No obvious differences in the properties of single and binary WN stars, whose luminosities extend down to log L approximate to 5.2 [L-circle dot], are apparent. With the exception of a few systems (BAT99 19, 49, and 103), the equatorial rotational velocities of the OB-type companions are moderate (v(eq) less than or similar to 250 km s(-1)) and challenge standard formalisms of angular-momentum accretion. For most objects, chemically homogeneous evolution can be rejected for the secondary, but not for the WR progenitor. Conclusions. No obvious dichotomy in the locations of apparently single and binary WN stars on the Hertzsprung-Russell diagram is apparent. According to commonly used stellar evolution models (BPASS, Geneva), most apparently single WN stars could not have formed as single stars, implying that they were stripped by an undetected companion. Otherwise, it must follow that pre-WR mass-loss/mixing (e.g., during the red supergiant phase) are strongly underestimated in standard stellar evolution models.
KW  - stars: massive
KW  - stars: Wolf-Rayet
KW  - Magellanic Clouds
KW  - binaries: close
KW  - binaries: spectroscopic
KW  - stars: evolution
Y1  - 2019
U6  - https://doi.org/10.1051/0004-6361/201935684
SN  - 0004-6361
SN  - 1432-0746
VL  - 627
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Shenar, Tomer
A1  - Hainich, Rainer
A1  - Todt, Helge Tobias
A1  - Moffat, Anthony F. J.
A1  - Sander, Andreas Alexander Christoph
A1  - Oskinova, Lidia M.
A1  - Ramachandran, Varsha
A1  - Munoz, M.
A1  - Pablo, H.
A1  - Sana, Hugues
A1  - Hamann, Wolf-Rainer
T1  - The shortest-period Wolf-Rayet binary in the small magellanic cloud
BT  - Part of a high-order multiple system Spectral and orbital analysis of SMC AB 6
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. SMC AB6 is the shortest-period (P = 6.5 d) Wolf-Rayet (WR) binary in the Small Magellanic Cloud. This binary is therefore a key system in the study of binary interaction and formation of WR stars at low metallicity. The WR component in AB6 was previously found to be very luminous (log L = 6.3 [L-circle dot]) compared to its reported orbital mass (approximate to 8 M-circle dot), placing it significantly above the Eddington limit. Aims. Through spectroscopy and orbital analysis of newly acquired optical data taken with the Ultraviolet and Visual Echelle Spectrograph (UVES), we aim to understand the peculiar results reported for this system and explore its evolutionary history. Methods. We measured radial velocities via cross-correlation and performed a spectral analysis using the Potsdam Wolf-Rayet model atmosphere code. The evolution of the system was analyzed using the Binary Population and Spectral Synthesis evolution code. Results. AB6 contains at least four stars. The 6.5 d period WR binary comprises the WR primary (WN3:h, star A) and a rather rapidly rotating (v(eq) = 265 km s(-1)) early O-type companion (O5.5 V, star B). Static N III and N IV emission lines and absorption signatures in He lines suggest the presence of an early-type emission line star (O5.5 I(f), star C). Finally, narrow absorption lines portraying a long-term radial velocity variation show the existence of a fourth star (O7.5 V, star D). Star D appears to form a second 140 d period binary together with a fifth stellar member, which is a B-type dwarf or a black hole. It is not clear that these additional components are bound to the WR binary. We derive a mass ratio of M-O/M-WR = 2.2 +/- 0.1. The WR star is found to be less luminous than previously thought (log L = 5.9 [L-circle dot]) and, adopting M-O = 41 M-circle dot for star B, more massive (M-WR = 18 M-circle dot). Correspondingly, the WR star does not exceed the Eddington limit. We derive the initial masses of M-i,M-WR = 60 M-circle dot and M-i,M-O = 40 M-circle dot and an age of 3.9 Myr for the system. The WR binary likely experienced nonconservative mass transfer in the past supported by the relatively rapid rotation of star B. Conclusions. Our study shows that AB6 is a multiple - probably quintuple - system. This finding resolves the previously reported puzzle of the WR primary exceeding the Eddington limit and suggests that the WR star exchanged mass with its companion in the past.
KW  - stars: massive
KW  - binaries: spectroscopic
KW  - stars: Wolf-Rayet
KW  - Magellanic Clouds
KW  - stars: individual: SMC AB 6
KW  - stars: atmospheres
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201833006
SN  - 1432-0746
SN  - 0004-6361
VL  - 616
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Ramachandran, Varsha
A1  - Hamann, Wolf-Rainer
A1  - Hainich, Rainer
A1  - Oskinova, Lidia M.
A1  - Shenar, Tomer
A1  - Sander, Andreas Alexander Christoph
A1  - Todt, Helge Tobias
A1  - Gallagher, John S.
T1  - Stellar population of the superbubble N206 in the LMC II. Parameters of the OB and WR stars, and the total massive star feedback
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Clusters or associations of early-type stars are often associated with a "superbubble" of hot gas. The formation of such superbubbles is caused by the feedback from massive stars. The complex N206 in the Large Magellanic Cloud (LMC) exhibits a superbubble and a rich massive star population. Aims. Our goal is to perform quantitative spectral analyses of all massive stars associated with the N206 superbubble in order to determine their stellar and wind parameters. We compare the superbubble energy budget to the stellar energy input and discuss the star formation history of the region. Results. We present the stellar and wind parameters of the OB stars and the two Wolf-Rayet (WR) binaries in the N206 complex. Twelve percent of the sample show Oe/Be type emission lines, although most of them appear to rotate far below critical. We found eight runaway stars based on their radial velocity. The wind-momentum luminosity relation of our OB sample is consistent with the expectations. The Hertzsprung-Russell diagram (HRD) of the OB stars reveals a large age spread (1-30 Myr), suggesting different episodes of star formation in the complex. The youngest stars are concentrated in the inner part of the complex, while the older OB stars are scattered over outer regions. We derived the present day mass function for the entire N206 complex as well as for the cluster NGC2018. The total ionizing photon flux produced by all massive stars in the N206 complex is Q(0) approximate to 5 x 10(50) s(-1), and the mechanical luminosity of their stellar winds amounts to L-mec = 1.7 x 10(38) erg s(-1). Three very massive Of stars are found to dominate the feedback among 164 OB stars in the sample. The two WR winds alone release about as much mechanical luminosity as the whole OB star sample. The cumulative mechanical feedback from all massive stellar winds is comparable to the combined mechanical energy of the supernova explosions that likely occurred in the complex. Accounting also for the WR wind and supernovae, the mechanical input over the last five Myr is approximate to 2.3 x 10(52) erg. Conclusions. The N206 complex in the LMC has undergone star formation episodes since more than 30 Myr ago. From the spectral analyses of its massive star population, we derive a current star formation rate of 2.2 x 10(-3) M-circle dot yr(-1). From the combined input of mechanical energy from all stellar winds, only a minor fraction is emitted in the form of X-rays. The corresponding input accumulated over a long time also exceeds the current energy content of the complex by more than a factor of five. The morphology of the complex suggests a leakage of hot gas from the superbubble.
KW  - stars: massive
KW  - Magellanic Clouds
KW  - stars: winds, outflows
KW  - Hertzsprung-Russell and C-M diagrams
KW  - techniques: spectroscopic
KW  - ISM: bubbles
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201832816
SN  - 1432-0746
VL  - 615
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Ramachandran, Varsha
A1  - Hainich, Rainer
A1  - Hamann, Wolf-Rainer
A1  - Oskinova, Lidia M.
A1  - Shenar, T.
A1  - Sander, Andreas Alexander Christoph
A1  - Todt, Helge Tobias
A1  - Gallagher, John S.
T1  - Stellar population of the superbubble N206 in the LMC I. Analysis of the Of-type stars
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Massive stars severely influence their environment by their strong ionizing radiation and by the momentum and kinetic energy input provided by their stellar winds and supernovae. Quantitative analyses of massive stars are required to understand how their feedback creates and shapes large scale structures of the interstellar medium. The giant H II region N206 in the Large Magellanic Cloud contains an OB association that powers a superbubble filled with hot X-ray emitting gas, serving as an ideal laboratory in this context. Aims. We aim to estimate stellar and wind parameters of all OB stars in N206 by means of quantitative spectroscopic analyses. In this first paper, we focus on the nine Of-type stars located in this region. We determine their ionizing flux and wind mechanical energy. The analysis of nitrogen abundances in our sample probes rotational mixing. Methods. We obtained optical spectra with the multi-object spectrograph FLAMES at the ESO-VLT. When possible, the optical spectroscopy was complemented by UV spectra from the HST, IUE, and FUSE archives. Detailed spectral classifications are presented for our sample Of-type stars. For the quantitative spectroscopic analysis we used the Potsdam Wolf-Rayet model atmosphere code. We determined the physical parameters and nitrogen abundances of our sample stars by fitting synthetic spectra to the observations. Results. The stellar and wind parameters of nine Of-type stars, which are largely derived from spectral analysis are used to construct wind momentum luminosity relationship. We find that our sample follows a relation close to the theoretical prediction, assuming clumped winds. The most massive star in the N206 association is an Of supergiant that has a very high mass-loss rate. Two objects in our sample reveal composite spectra, showing that the Of primaries have companions of late O subtype. All stars in our sample have an evolutionary age of less than 4 million yr, with the O2-type star being the youngest. All these stars show a systematic discrepancy between evolutionary and spectroscopic masses. All stars in our sample are nitrogen enriched. Nitrogen enrichment shows a clear correlation with increasing projected rotational velocities. Conclusions. The mechanical energy input from the Of stars alone is comparable to the energy stored in the N206 superbubble as measured from the observed X-ray and H alpha emission.
KW  - stars: early-type
KW  - Magellanic Clouds
KW  - stars: atmospheres
KW  - stars: winds, outflows
KW  - stars: mass-loss
KW  - stars: massive
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201731093
SN  - 1432-0746
SN  - 0004-6361
VL  - 609
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Sander, Andreas Alexander Christoph
A1  - Fürst, F.
A1  - Kretschmar, P.
A1  - Oskinova, Lidia M.
A1  - Todt, Helge Tobias
A1  - Hainich, Rainer
A1  - Shenar, Tomer
A1  - Hamann, Wolf-Rainer
T1  - Coupling hydrodynamics with comoving frame radiative transfer
BT  - Stellar wind stratification in the high-mass X-ray binary Vela X-1
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Aims. To gain a realistic picture of the donor star in Vela X-1, we constructed a hydrodynamically consistent atmosphere model describing the wind stratification while properly reproducing the observed donor spectrum. To investigate how X-ray illumination affects the stellar wind, we calculated additional models for different X-ray luminosity regimes. Methods. We used the recently updated version of the Potsdam Wolf-Rayet code to consistently solve the hydrodynamic equation together with the statistical equations and the radiative transfer. Results. The wind flow in Vela X-1 is driven by ions from various elements, with Fe III and S III leading in the outer wind. The model-predicted mass-loss rate is in line with earlier empirical studies. The mass-loss rate is almost unaffected by the presence of the accreting NS in the wind. The terminal wind velocity is confirmed at u(infinity) approximate to 600 km s(-1). On the other hand, the wind velocity in the inner region where the NS is located is only approximate to 100 km s(-1), which is not expected on the basis of a standard beta-velocity law. In models with an enhanced level of X-rays, the velocity field in the outer wind can be altered. If the X-ray flux is too high, the acceleration breaks down because the ionization increases. Conclusions. Accounting for radiation hydrodynamics, our Vela X-1 donor atmosphere model reveals a low wind speed at the NS location, and it provides quantitative information on wind driving in this important HMXB.
KW  - stars: mass-loss
KW  - stars: winds, outflows
KW  - stars: early-type
KW  - stars: atmospheres
KW  - stars: massive
KW  - X-rays: binaries
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201731575
SN  - 1432-0746
VL  - 610
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Sander, Andreas Alexander Christoph
A1  - Hamann, Wolf-Rainer
A1  - Todt, Helge Tobias
A1  - Hainich, Rainer
A1  - Shenar, Tomer
A1  - Ramachandran, Varsha
A1  - Oskinova, Lidia M.
T1  - The Galactic WC and WO stars
BT  - The impact of revised distances from Gaia DR2 and their role as massive black hole progenitors
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Wolf-Rayet stars of the carbon sequence (WC stars) are an important cornerstone in the late evolution of massive stars before their core collapse. As core-helium burning, hydrogen-free objects with huge mass-loss, they are likely the last observable stage before collapse and thus promising progenitor candidates for type Ib/c supernovae. Their strong mass-loss furthermore provides challenges and constraints to the theory of radiatively driven winds. Thus, the determination of the WC star parameters is of major importance for several astrophysical fields. With Gaia DR2, for the first time parallaxes for a large sample of Galactic WC stars are available, removing major uncertainties inherent to earlier studies. In this work, we re-examine a previously studied sample of WC stars to derive key properties of the Galactic WC population. All quantities depending on the distance are updated, while the underlying spectral analyzes remain untouched. Contrasting earlier assumptions, our study yields that WC stars of the same subtype can significantly vary in absolute magnitude. With Gaia DR2, the picture of the Galactic WC population becomes more complex: We obtain luminosities ranging from log L/L-circle dot = 4.9-6.0 with one outlier (WR 119) having log L/L-circle dot = 4.7. This indicates that the WC stars are likely formed from a broader initial mass range than previously assumed. We obtain mass-loss rates ranging between log(M) over dot = -5.1 and -4.1, with (M) over dot proportional to L-0.68 and a linear scaling of the modified wind momentum with luminosity. We discuss the implications for stellar evolution, including unsolved issues regarding the need of envelope inflation to address the WR radius problem, and the open questions in regard to the connection of WR stars with Gamma-ray bursts. WC and WO stars are progenitors of massive black holes, collapsing either silently or in a supernova that most-likely has to be preceded by a WO stage.
KW  - stars: evolution
KW  - stars: mass-loss
KW  - stars: Wolf-Rayet
KW  - stars: massive
KW  - stars: distances
KW  - Galaxy: stellar content
Y1  - 2019
U6  - https://doi.org/10.1051/0004-6361/201833712
SN  - 1432-0746
VL  - 621
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Hainich, Rainer
A1  - Ramachandran, Varsha
A1  - Shenar, Tomer
A1  - Sander, Andreas Alexander Christoph
A1  - Todt, Helge Tobias
A1  - Gruner, David
A1  - Oskinova, Lidia M.
A1  - Hamann, Wolf-Rainer
T1  - PoWR grids of non-LTE model atmospheres for OB-type stars of various metallicities
JF  - Astronomy and astrophysics : an international weekly journal
N2  - The study of massive stars in different metallicity environments is a central topic of current stellar research. The spectral analysis of massive stars requires adequate model atmospheres. The computation of such models is difficult and time-consuming. Therefore, spectral analyses are greatly facilitated if they can refer to existing grids of models. Here we provide grids of model atmospheres for OB-type stars at metallicities corresponding to the Small and Large Magellanic Clouds, as well as to solar metallicity. In total, the grids comprise 785 individual models. The models were calculated using the state-of-the-art Potsdam Wolf-Rayet (PoWR) model atmosphere code. The parameter domain of the grids was set up using stellar evolution tracks. For all these models, we provide normalized and flux-calibrated spectra, spectral energy distributions, feedback parameters such as ionizing photons, Zanstra temperatures, and photometric magnitudes. The atmospheric structures (the density and temperature stratification) are available as well. All these data are publicly accessible through the PoWR website.
KW  - stars: massive
KW  - stars: early-type
KW  - stars: atmospheres
KW  - stars: winds
KW  - outflows
KW  - stars: mass-loss
KW  - radiative transfer
Y1  - 2019
U6  - https://doi.org/10.1051/0004-6361/201833787
SN  - 1432-0746
VL  - 621
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - RPRT
A1  - Siedler, Thomas
A1  - Anger, Silke
A1  - Christoph, Bernhard
A1  - Galkiewicz, Agata Danuta
A1  - Margaryan, Shushanik
A1  - Peter, Frauke
A1  - Sandner, Malte
T1  - War, international spillovers, and adolescents
BT  - evidence from Russia’s invasion of Ukraine in 2022
T2  - Discussion paper series
N2  - Using novel longitudinal data, this paper studies the short- and medium-term effects of Russia's invasion of Ukraine on February 24, 2022 on social trust of adolescents in Germany. Comparing adolescents who responded to our survey shortly before the start of the war with those who responded shortly after the conflict began and applying difference-in-differences (DiD) models over time, we find a significant decline in the outcome after the war started. These findings provide new evidence on how armed conflicts influence social trust and well-being among young people in a country not directly involved in the war.
KW  - war
KW  - trust
KW  - social capital
KW  - Russia’s invasion of Ukraine
Y1  - 2024
UR  - https://www.iza.org/publications/dp/16921/war-international-spillovers-and-adolescents-evidence-from-russias-invasion-of-ukraine-in-2022
SN  - 2365-9793
N1  - published in: Journal of Economic Behavior & Organization, 2024, 224, 181-193
VL  - No. 16921
PB  - IZA
CY  - Bonn
ER  - 
TY  - RPRT
A1  - Brodeur, Abel
A1  - Mikola, Derek
A1  - Cook, Nikolai
A1  - Brailey, Thomas
A1  - Briggs, Ryan
A1  - Gendre, Alexandra de
A1  - Dupraz, Yannick
A1  - Fiala, Lenka
A1  - Gabani, Jacopo
A1  - Gauriot, Romain
A1  - Haddad, Joanne
A1  - Lima, Goncalo
A1  - Ankel-Peters, Jörg
A1  - Dreber, Anna
A1  - Campbell, Douglas
A1  - Kattan, Lamis
A1  - Fages, Diego Marino
A1  - Mierisch, Fabian
A1  - Sun, Pu
A1  - Wright, Taylor
A1  - Connolly, Marie
A1  - Hoces de la Guardia, Fernando
A1  - Johannesson, Magnus
A1  - Miguel, Edward
A1  - Vilhuber, Lars
A1  - Abarca, Alejandro
A1  - Acharya, Mahesh
A1  - Adjisse, Sossou Simplice
A1  - Akhtar, Ahwaz
A1  - Lizardi, Eduardo Alberto Ramirez
A1  - Albrecht, Sabina
A1  - Andersen, Synve Nygaard
A1  - Andlib, Zubaria
A1  - Arrora, Falak
A1  - Ash, Thomas
A1  - Bacher, Etienne
A1  - Bachler, Sebastian
A1  - Bacon, Félix
A1  - Bagues, Manuel
A1  - Balogh, Timea
A1  - Batmanov, Alisher
A1  - Barschkett, Mara
A1  - Basdil, B. Kaan
A1  - Dower, Jaromneda
A1  - Castek, Ondrej
A1  - Caviglia-Harris, Jill
A1  - Strand, Gabriella Chauca
A1  - Chen, Shi
A1  - Chzhen, Asya
A1  - Chung, Jong
A1  - Collins, Jason
A1  - Coppock, Alexander
A1  - Cordeau, Hugo
A1  - Couillard, Ben
A1  - Crechet, Jonathan
A1  - Crippa, Lorenzo
A1  - Cui, Jeanne
A1  - Czymara, Christian
A1  - Daarstad, Haley
A1  - Dao, Danh Chi
A1  - Dao, Dong
A1  - Schmandt, Marco David
A1  - Linde, Astrid de
A1  - Melo, Lucas De
A1  - Deer, Lachlan
A1  - Vera, Micole De
A1  - Dimitrova, Velichka
A1  - Dollbaum, Jan Fabian
A1  - Dollbaum, Jan Matti
A1  - Donnelly, Michael
A1  - Huynh, Luu Duc Toan
A1  - Dumbalska, Tsvetomira
A1  - Duncan, Jamie
A1  - Duong, Kiet Tuan
A1  - Duprey, Thibaut
A1  - Dworschak, Christoph
A1  - Ellingsrud, Sigmund
A1  - Elminejad, Ali
A1  - Eissa, Yasmine
A1  - Erhart, Andrea
A1  - Etingin-Frati, Giulian
A1  - Fatemi-Pour, Elaheh
A1  - Federice, Alexa
A1  - Feld, Jan
A1  - Fenig, Guidon
A1  - Firouzjaeiangalougah, Mojtaba
A1  - Fleisje, Erlend
A1  - Fortier-Chouinard, Alexandre
A1  - Engel, Julia Francesca
A1  - Fries, Tilman
A1  - Fortier, Reid
A1  - Fréchet, Nadjim
A1  - Galipeau, Thomas
A1  - Gallegos, Sebastián
A1  - Gangji, Areez
A1  - Gao, Xiaoying
A1  - Garnache, Cloé
A1  - Gáspár, Attila
A1  - Gavrilova, Evelina
A1  - Ghosh, Arijit
A1  - Gibney, Garreth
A1  - Gibson, Grant
A1  - Godager, Geir
A1  - Goff, Leonard
A1  - Gong, Da
A1  - González, Javier
A1  - Gretton, Jeremy
A1  - Griffa, Cristina
A1  - Grigoryeva, Idaliya
A1  - Grtting, Maja
A1  - Guntermann, Eric
A1  - Guo, Jiaqi
A1  - Gugushvili, Alexi
A1  - Habibnia, Hooman
A1  - Häffner, Sonja
A1  - Hall, Jonathan D.
A1  - Hammar, Olle
A1  - Kordt, Amund Hanson
A1  - Hashimoto, Barry
A1  - Hartley, Jonathan S.
A1  - Hausladen, Carina I.
A1  - Havránek, Tomáš
A1  - Hazen, Jacob
A1  - He, Harry
A1  - Hepplewhite, Matthew
A1  - Herrera-Rodriguez, Mario
A1  - Heuer, Felix
A1  - Heyes, Anthony
A1  - Ho, Anson T. Y.
A1  - Holmes, Jonathan
A1  - Holzknecht, Armando
A1  - Hsu, Yu-Hsiang Dexter
A1  - Hu, Shiang-Hung
A1  - Huang, Yu-Shiuan
A1  - Huebener, Mathias
A1  - Huber, Christoph
A1  - Huynh, Kim P.
A1  - Irsova, Zuzana
A1  - Isler, Ozan
A1  - Jakobsson, Niklas
A1  - Frith, Michael James
A1  - Jananji, Raphaël
A1  - Jayalath, Tharaka A.
A1  - Jetter, Michael
A1  - John, Jenny
A1  - Forshaw, Rachel Joy
A1  - Juan, Felipe
A1  - Kadriu, Valon
A1  - Karim, Sunny
A1  - Kelly, Edmund
A1  - Dang, Duy Khanh Hoang
A1  - Khushboo, Tazia
A1  - Kim, Jin
A1  - Kjellsson, Gustav
A1  - Kjelsrud, Anders
A1  - Kotsadam, Andreas
A1  - Korpershoek, Jori
A1  - Krashinsky, Lewis
A1  - Kundu, Suranjana
A1  - Kustov, Alexander
A1  - Lalayev, Nurlan
A1  - Langlois, Audrée
A1  - Laufer, Jill
A1  - Lee-Whiting, Blake
A1  - Leibing, Andreas
A1  - Lenz, Gabriel
A1  - Levin, Joel
A1  - Li, Peng
A1  - Li, Tongzhe
A1  - Lin, Yuchen
A1  - Listo, Ariel
A1  - Liu, Dan
A1  - Lu, Xuewen
A1  - Lukmanova, Elvina
A1  - Luscombe, Alex
A1  - Lusher, Lester R.
A1  - Lyu, Ke
A1  - Ma, Hai
A1  - Mäder, Nicolas
A1  - Makate, Clifton
A1  - Malmberg, Alice
A1  - Maitra, Adit
A1  - Mandas, Marco
A1  - Marcus, Jan
A1  - Margaryan, Shushanik
A1  - Márk, Lili
A1  - Martignano, Andres
A1  - Marsh, Abigail
A1  - Masetto, Isabella
A1  - McCanny, Anthony
A1  - McManus, Emma
A1  - McWay, Ryan
A1  - Metson, Lennard
A1  - Kinge, Jonas Minet
A1  - Mishra, Sumit
A1  - Mohnen, Myra
A1  - Möller, Jakob
A1  - Montambeault, Rosalie
A1  - Montpetit, Sébastien
A1  - Morin, Louis-Philippe
A1  - Morris, Todd
A1  - Moser, Scott
A1  - Motoki, Fabio
A1  - Muehlenbachs, Lucija
A1  - Musulan, Andreea
A1  - Musumeci, Marco
A1  - Nabin, Munirul
A1  - Nchare, Karim
A1  - Neubauer, Florian
A1  - Nguyen, Quan M. P.
A1  - Nguyen, Tuan
A1  - Nguyen-Tien, Viet
A1  - Niazi, Ali
A1  - Nikolaishvili, Giorgi
A1  - Nordstrom, Ardyn
A1  - Nü, Patrick
A1  - Odermatt, Angela
A1  - Olson, Matt
A1  - ien, Henning
A1  - Ölkers, Tim
A1  - Vert, Miquel Oliver i.
A1  - Oral, Emre
A1  - Oswald, Christian
A1  - Ousman, Ali
A1  - Özak, Ömer
A1  - Pandey, Shubham
A1  - Pavlov, Alexandre
A1  - Pelli, Martino
A1  - Penheiro, Romeo
A1  - Park, RyuGyung
A1  - Martel, Eva Pérez
A1  - Petrovičová, Tereza
A1  - Phan, Linh
A1  - Prettyman, Alexa
A1  - Procházka, Jakub
A1  - Putri, Aqila
A1  - Quandt, Julian
A1  - Qiu, Kangyu
A1  - Nguyen, Loan Quynh Thi
A1  - Rahman, Andaleeb
A1  - Rea, Carson H.
A1  - Reiremo, Adam
A1  - Renée, Laëtitia
A1  - Richardson, Joseph
A1  - Rivers, Nicholas
A1  - Rodrigues, Bruno
A1  - Roelofs, William
A1  - Roemer, Tobias
A1  - Rogeberg, Ole
A1  - Rose, Julian
A1  - Roskos-Ewoldsen, Andrew
A1  - Rosmer, Paul
A1  - Sabada, Barbara
A1  - Saberian, Soodeh
A1  - Salamanca, Nicolas
A1  - Sator, Georg
A1  - Sawyer, Antoine
A1  - Scates, Daniel
A1  - Schlüter, Elmar
A1  - Sells, Cameron
A1  - Sen, Sharmi
A1  - Sethi, Ritika
A1  - Shcherbiak, Anna
A1  - Sogaolu, Moyosore
A1  - Soosalu, Matt
A1  - Srensen, Erik
A1  - Sovani, Manali
A1  - Spencer, Noah
A1  - Staubli, Stefan
A1  - Stans, Renske
A1  - Stewart, Anya
A1  - Stips, Felix
A1  - Stockley, Kieran
A1  - Strobel, Stephenson
A1  - Struby, Ethan
A1  - Tang, John
A1  - Tanrisever, Idil
A1  - Yang, Thomas Tao
A1  - Tastan, Ipek
A1  - Tatić, Dejan
A1  - Tatlow, Benjamin
A1  - Seuyong, Féraud Tchuisseu
A1  - Thériault, Rémi
A1  - Thivierge, Vincent
A1  - Tian, Wenjie
A1  - Toma, Filip-Mihai
A1  - Totarelli, Maddalena
A1  - Tran, Van-Anh
A1  - Truong, Hung
A1  - Tsoy, Nikita
A1  - Tuzcuoglu, Kerem
A1  - Ubfal, Diego
A1  - Villalobos, Laura
A1  - Walterskirchen, Julian
A1  - Wang, Joseph Taoyi
A1  - Wattal, Vasudha
A1  - Webb, Matthew D.
A1  - Weber, Bryan
A1  - Weisser, Reinhard
A1  - Weng, Wei-Chien
A1  - Westheide, Christian
A1  - White, Kimberly
A1  - Winter, Jacob
A1  - Wochner, Timo
A1  - Woerman, Matt
A1  - Wong, Jared
A1  - Woodard, Ritchie
A1  - Wroński, Marcin
A1  - Yazbeck, Myra
A1  - Yang, Gustav Chung
A1  - Yap, Luther
A1  - Yassin, Kareman
A1  - Ye, Hao
A1  - Yoon, Jin Young
A1  - Yurris, Chris
A1  - Zahra, Tahreen
A1  - Zaneva, Mirela
A1  - Zayat, Aline
A1  - Zhang, Jonathan
A1  - Zhao, Ziwei
A1  - Yaolang, Zhong
T1  - Mass reproducibility and replicability
BT  - a new hope
T2  - I4R discussion paper series
N2  - This study pushes our understanding of research reliability by reproducing and replicating claims from 110 papers in leading economic and political science journals. The analysis involves computational reproducibility checks and robustness assessments. It reveals several patterns. First, we uncover a high rate of fully computationally reproducible results (over 85%). Second, excluding minor issues like missing packages or broken pathways, we uncover coding errors for about 25% of studies, with some studies containing multiple errors. Third, we test the robustness of the results to 5,511 re-analyses. We find a robustness reproducibility of about 70%. Robustness reproducibility rates are relatively higher for re-analyses that introduce new data and lower for re-analyses that change the sample or the definition of the dependent variable. Fourth, 52% of re-analysis effect size estimates are smaller than the original published estimates and the average statistical significance of a re-analysis is 77% of the original. Lastly, we rely on six teams of researchers working independently to answer eight additional research questions on the determinants of robustness reproducibility. Most teams find a negative relationship between replicators' experience and reproducibility, while finding no relationship between reproducibility and the provision of intermediate or even raw data combined with the necessary cleaning codes.
KW  - conomics
KW  - open science
KW  - political science
KW  - replication
KW  - reproduction
KW  - research transparency
Y1  - 2024
SN  - 2752-1931
IS  - 107
PB  - Institute for Replication
CY  - Essen
ER  - 
TY  - JOUR
A1  - Kolmakova, Olesya V.
A1  - Gladyshev, Michail I.
A1  - Fonvielle, Jeremy Andre
A1  - Ganzert, Lars
A1  - Hornick, Thomas
A1  - Grossart, Hans-Peter
T1  - Effects of zooplankton carcasses degradation on freshwater bacterial community composition and implications for carbon cycling
JF  - Environmental microbiology
N2  - Non-predatory mortality of zooplankton provides an abundant, yet, little studied source of high quality labile organic matter (LOM) in aquatic ecosystems. Using laboratory microcosms, we followed the decomposition of organic carbon of fresh C-13-labelled Daphnia carcasses by natural bacterioplankton. The experimental setup comprised blank microcosms, that is, artificial lake water without any organic matter additions (B), and microcosms either amended with natural humic matter (H), fresh Daphnia carcasses (D) or both, that is, humic matter and Daphnia carcasses (HD). Most of the carcass carbon was consumed and respired by the bacterial community within 15 days of incubation. A shift in the bacterial community composition shaped by labile carcass carbon and by humic matter was observed. Nevertheless, we did not observe a quantitative change in humic matter degradation by heterotrophic bacteria in the presence of LOM derived from carcasses. However, carcasses were the main factor driving the bacterial community composition suggesting that the presence of large quantities of dead zooplankton might affect the carbon cycling in aquatic ecosystems. Our results imply that organic matter derived from zooplankton carcasses is efficiently remineralized by a highly specific bacterial community, but does not interfere with the bacterial turnover of more refractory humic matter.
Y1  - 2018
U6  - https://doi.org/10.1111/1462-2920.14418
SN  - 1462-2912
SN  - 1462-2920
VL  - 21
IS  - 1
SP  - 34
EP  - 49
PB  - Wiley
CY  - Hoboken
ER  - 
TY  - JOUR
A1  - Block, Benjamin D.
A1  - Denfeld, Blaize A.
A1  - Stockwell, Jason D.
A1  - Flaim, Giovanna
A1  - Grossart, Hans-Peter
A1  - Knoll, Lesley B.
A1  - Maier, Dominique B.
A1  - North, Rebecca L.
A1  - Rautio, Milla
A1  - Rusak, James A.
A1  - Sadro, Steve
A1  - Weyhenmeyer, Gesa A.
A1  - Bramburger, Andrew J.
A1  - Branstrator, Donn K.
A1  - Salonen, Kalevi
A1  - Hampton, Stephanie E.
T1  - The unique methodological challenges of winter limnology
JF  - Limnology and Oceanography: Methods
N2  - Winter is an important season for many limnological processes, which can range from biogeochemical transformations to ecological interactions. Interest in the structure and function of lake ecosystems under ice is on the rise. Although limnologists working at polar latitudes have a long history of winter work, the required knowledge to successfully sample under winter conditions is not widely available and relatively few limnologists receive formal training. In particular, the deployment and operation of equipment in below 0 degrees C temperatures pose considerable logistical and methodological challenges, as do the safety risks of sampling during the ice-covered period. Here, we consolidate information on winter lake sampling and describe effective methods to measure physical, chemical, and biological variables in and under ice. We describe variation in snow and ice conditions and discuss implications for sampling logistics and safety. We outline commonly encountered methodological challenges and make recommendations for best practices to maximize safety and efficiency when sampling through ice or deploying instruments in ice-covered lakes. Application of such practices over a broad range of ice-covered lakes will contribute to a better understanding of the factors that regulate lakes during winter and how winter conditions affect the subsequent ice-free period.
Y1  - 2018
U6  - https://doi.org/10.1002/lom3.10295
SN  - 1541-5856
VL  - 17
IS  - 1
SP  - 42
EP  - 57
PB  - Wiley
CY  - Hoboken
ER  - 
TY  - JOUR
A1  - Beisner, Beatrix E.
A1  - Grossart, Hans-Peter
A1  - Gasol, Josep M.
T1  - A guide to methods for estimating phago-mixotrophy in nanophytoplankton
JF  - Journal of plankton research
N2  - Growing attention to phytoplankton mixotrophy as a trophic strategy has led to significant revisions of traditional pelagic food web models and ecosystem functioning. Although some empirical estimates of mixotrophy do exist, a much broader set of in situ measurements are required to (i) identify which organisms are acting as mixotrophs in real time and to (ii) assess the contribution of their heterotrophy to biogeochemical cycling. Estimates are needed through time and across space to evaluate which environmental conditions or habitats favour mixotrophy: conditions still largely unknown. We review methodologies currently available to plankton ecologists to undertake estimates of plankton mixotrophy, in particular nanophytoplankton phago-mixotrophy. Methods are based largely on fluorescent or isotopic tracers, but also take advantage of genomics to identify phylotypes and function. We also suggest novel methods on the cusp of use for phago-mixotrophy assessment, including single-cell measurements improving our capacity to estimate mixotrophic activity and rates in wild plankton communities down to the single-cell level. Future methods will benefit from advances in nanotechnology, micromanipulation and microscopy combined with stable isotope and genomic methodologies. Improved estimates of mixotrophy will enable more reliable models to predict changes in food web structure and biogeochemical flows in a rapidly changing world.
KW  - flow cytometry
KW  - phagotrophy
KW  - phytoplankton
KW  - methods
KW  - fluorescence
KW  - microscopy
KW  - FISH
KW  - isotopic methods
KW  - phylotypes
KW  - carbon flows
KW  - gene sequencing
Y1  - 2019
U6  - https://doi.org/10.1093/plankt/fbz008
SN  - 0142-7873
SN  - 1464-3774
VL  - 41
IS  - 2
SP  - 77
EP  - 89
PB  - Oxford Univ. Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Arias-Andres, Maria
A1  - Rojas-Jimenez, Keilor
A1  - Grossart, Hans-Peter
T1  - Collateral effects of microplastic pollution on aquatic microorganisms
BT  - An ecological perspective
JF  - Trends in Analytical Chemistry
N2  - Microplastics (MP) provide a unique and extensive surface for microbial colonization in aquatic ecosystems. The formation of microorganism-microplastic complexes, such as biofilms, maximizes the degradation of organic matter and horizontal gene transfer. In this context, MP affect the structure and function of microbial communities, which in turn render the physical and chemical fate of MP. This new paradigm generates challenges for microbiology, ecology, and ecotoxicology. Dispersal of MP is concomitant with that of their associated microorganisms and their mobile genetic elements, including antibiotic resistance genes, islands of pathogenicity, and diverse metabolic pathways. Functional changes in aquatic microbiomes can alter carbon metabolism and food webs, with unknown consequences on higher organisms or human microbiomes and hence health. Here, we examine a variety of effects of MP pollution from the microbial ecology perspective, whose repercussions on aquatic ecosystems begin to be unraveled. (C) 2018 Elsevier B.V. All rights reserved.
KW  - Microplastics (MP)
KW  - Biofilms
KW  - HGT
KW  - Microbial ecology
KW  - Carbon cycling
KW  - Aquatic ecosystems
KW  - Health risk assessment
Y1  - 2018
U6  - https://doi.org/10.1016/j.trac.2018.11.041
SN  - 0165-9936
SN  - 1879-3142
VL  - 112
SP  - 234
EP  - 240
PB  - Elsevier
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Gebser, Martin
A1  - Obermeier, Philipp
A1  - Otto, Thomas
A1  - Schaub, Torsten
A1  - Sabuncu, Orkunt
A1  - Van Nguyen, 
A1  - Tran Cao Son, 
T1  - Experimenting with robotic intra-logistics domains
JF  - Theory and practice of logic programming
N2  - We introduce the asprilo1 framework to facilitate experimental studies of approaches addressing complex dynamic applications. For this purpose, we have chosen the domain of robotic intra-logistics. This domain is not only highly relevant in the context of today's fourth industrial revolution but it moreover combines a multitude of challenging issues within a single uniform framework. This includes multi-agent planning, reasoning about action, change, resources, strategies, etc. In return, asprilo allows users to study alternative solutions as regards effectiveness and scalability. Although asprilo relies on Answer Set Programming and Python, it is readily usable by any system complying with its fact-oriented interface format. This makes it attractive for benchmarking and teaching well beyond logic programming. More precisely, asprilo consists of a versatile benchmark generator, solution checker and visualizer as well as a bunch of reference encodings featuring various ASP techniques. Importantly, the visualizer's animation capabilities are indispensable for complex scenarios like intra-logistics in order to inspect valid as well as invalid solution candidates. Also, it allows for graphically editing benchmark layouts that can be used as a basis for generating benchmark suites.
Y1  - 2018
U6  - https://doi.org/10.1017/S1471068418000200
SN  - 1471-0684
SN  - 1475-3081
VL  - 18
IS  - 3-4
SP  - 502
EP  - 519
PB  - Cambridge Univ. Press
CY  - New York
ER  - 
TY  - JOUR
A1  - Liemohn, Michael W.
A1  - McCollough, James P.
A1  - Jordanova, Vania K.
A1  - Ngwira, Chigomezyo M.
A1  - Morley, Steven K.
A1  - Cid, Consuelo
A1  - Tobiska, W. Kent
A1  - Wintoft, Peter
A1  - Ganushkina, Natalia Yu
A1  - Welling, Daniel T.
A1  - Bingham, Suzy
A1  - Balikhin, Michael A.
A1  - Opgenoorth, Hermann J.
A1  - Engel, Miles A.
A1  - Weigel, Robert S.
A1  - Singer, Howard J.
A1  - Buresova, Dalia
A1  - Bruinsma, Sean
A1  - Zhelavskaya, Irina
A1  - Shprits, Yuri
A1  - Vasile, Ruggero
T1  - Model Evaluation Guidelines for Geomagnetic Index Predictions
JF  - Space Weather: The International Journal of Research and Applications
N2  - Geomagnetic indices are convenient quantities that distill the complicated physics of some region or aspect of near-Earth space into a single parameter. Most of the best-known indices are calculated from ground-based magnetometer data sets, such as Dst, SYM-H, Kp, AE, AL, and PC. Many models have been created that predict the values of these indices, often using solar wind measurements upstream from Earth as the input variables to the calculation. This document reviews the current state of models that predict geomagnetic indices and the methods used to assess their ability to reproduce the target index time series. These existing methods are synthesized into a baseline collection of metrics for benchmarking a new or updated geomagnetic index prediction model. These methods fall into two categories: (1) fit performance metrics such as root-mean-square error and mean absolute error that are applied to a time series comparison of model output and observations and (2) event detection performance metrics such as Heidke Skill Score and probability of detection that are derived from a contingency table that compares model and observation values exceeding (or not) a threshold value. A few examples of codes being used with this set of metrics are presented, and other aspects of metrics assessment best practices, limitations, and uncertainties are discussed, including several caveats to consider when using geomagnetic indices. Plain Language Summary One aspect of space weather is a magnetic signature across the surface of the Earth. The creation of this signal involves nonlinear interactions of electromagnetic forces on charged particles and can therefore be difficult to predict. The perturbations that space storms and other activity causes in some observation sets, however, are fairly regular in their pattern. Some of these measurements have been compiled together into a single value, a geomagnetic index. Several such indices exist, providing a global estimate of the activity in different parts of geospace. Models have been developed to predict the time series of these indices, and various statistical methods are used to assess their performance at reproducing the original index. Existing studies of geomagnetic indices, however, use different approaches to quantify the performance of the model. This document defines a standardized set of statistical analyses as a baseline set of comparison tools that are recommended to assess geomagnetic index prediction models. It also discusses best practices, limitations, uncertainties, and caveats to consider when conducting a model assessment.
Y1  - 2018
U6  - https://doi.org/10.1029/2018SW002067
SN  - 1542-7390
VL  - 16
IS  - 12
SP  - 2079
EP  - 2102
PB  - American Geophysical Union
CY  - Washington
ER  - 
TY  - JOUR
A1  - Zhu, Hui
A1  - Shprits, Yuri
A1  - Chen, Lunjin
A1  - Liu, Xu
A1  - Kellerman, Adam C.
T1  - An event on simultaneous amplification of exohiss and chorus waves associated with electron density enhancements
JF  - Journal of geophysical research : Space physics
N2  - Whistler mode exohiss are the structureless hiss waves observed outside the plasma pause with featured equatorward Poynting flux. An event of the amplification of exohiss as well as chorus waves was recorded by Van Allen Probes during the recovery phase of a weak geomagnetic storm. Amplitudes of both types of the waves showed a significant increase at the regions of electron density enhancements. It is found that the electrons resonant with exohiss and chorus showed moderate pitch angle anisotropies. The ratio of the number of electrons resonating with exohiss to total electron number presented in-phase correlation with density variations, which suggests that exohiss can be amplified due to electron density enhancement in terms of cyclotron instability. The calculation of linear growth rates further supports above conclusion. We suggest that exohiss waves have potential to become more significant due to the background plasma fluctuation.
Y1  - 2018
U6  - https://doi.org/10.1029/2017JA025023
SN  - 2169-9380
SN  - 2169-9402
VL  - 123
IS  - 11
SP  - 8958
EP  - 8968
PB  - American Geophysical Union
CY  - Washington
ER  - 
TY  - JOUR
A1  - Oskinova, Lidia M.
A1  - Feldmeier, Achim
A1  - Hamann, Wolf-Rainer
T1  - High-resolution X-ray spectroscopy of bright O-type stars
JF  - Monthly notices of the Royal Astronomical Society
N2  - Archival X-ray spectra of the four prominent single, non-magnetic O stars zeta Pup, zeta Ori, xi Per and zeta Oph, obtained in high resolution with Chandra HETGS/MEG have been studied. The resolved X-ray emission line profiles provide information about the shocked, hot gas which emits the X-radiation, and about the bulk of comparably cool stellar wind material which partly absorbs this radiation. In this paper, we synthesize X-ray line profiles with a model of a clumpy stellar wind. We find that the geometrical shape of the wind inhomogeneities is important: better agreement with the observations can be achieved with radially compressed clumps than with spherical clumps. The parameters of the model, i.e. chemical abundances, stellar radius, mass-loss rate and terminal wind velocity, are taken from existing analyses of UV and optical spectra of the programme stars. On this basis, we also calculate the continuum-absorption coefficient of the cool-wind material, using the Potsdam Wolf-Rayet (POWR) model atmosphere code. The radial location of X-ray emitting gas is restricted from analysing the FIR line ratios of helium-like ions. The only remaining free parameter of our model is the typical distance between the clumps; here, we assume that at any point in the wind there is one clump passing by per one dynamical time-scale of the wind. The total emission in a model line is scaled to the observation. There is a good agreement between synthetic and observed line profiles. We conclude that the X-ray emission line profiles in O stars can be explained by hot plasma embedded in a cool wind which is highly clumped in the form of radially compressed shell fragments.
KW  - stars : individual : zeta Pup
KW  - stars : individual : zeta Ori
KW  - stars : individual : xi Per
KW  - stars : individual : zeta Oph
KW  - X-rays : stars
Y1  - 2006
U6  - https://doi.org/10.1111/j.1365-2966.2006.10858.x
SN  - 0035-8711
VL  - 372
SP  - 313
EP  - 326
PB  - Oxford University Press
CY  - Oxford
ER  - 
TY  - JOUR
A1  - Robrade, Jan
A1  - Oskinova, Lidia M.
A1  - Schmitt, J. H. M. M.
A1  - Leto, Paolo
A1  - Trigilio, C.
T1  - Outstanding X-ray emission from the stellar radio pulsar CU Virginis
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Among the intermediate-mass magnetic chemically peculiar (MCP) stars, CU Vir is one of the most intriguing objects. Its 100% circularly polarized beams of radio emission sweep the Earth as the star rotates, thereby making this strongly magnetic star the prototype of a class of nondegenerate stellar radio pulsars. While CU Vir is well studied in radio, its high-energy properties are not known. Yet, X-ray emission is expected from stellar magnetospheres and confined stellar winds. Aims. Using X-ray data we aim to test CU Vir for intrinsic X-ray emission and investigate mechanisms responsible for its generation. Methods. We present X-ray observations performed with XMM-Newton and Chandra and study obtained X-ray images, light curves, and spectra. Basic X-ray properties are derived from spectral modelling and are compared with model predictions. In this context we investigate potential thermal and nonthermal X-ray emission scenarios. Results. We detect an X-ray source at the position of CU Vir. With LX approximate to 3 x 10(28) erg s(-1) it is moderately X-ray bright, but the spectrum is extremely hard compared to other Ap stars. Spectral modelling requires multi-component models with predominant hot plasma at temperatures of about T-X = 25MK or, alternatively, a nonthermal spectral component. Both types of model provide a virtually equivalent description of the X-ray spectra. The Chandra observation was performed six years later than those by XMM-Newton, yet the source has similar X-ray flux and spectrum, suggesting a steady and persistent X-ray emission. This is further confirmed by the X-ray light curves that show only mild X-ray variability. Conclusions. CU Vir is also an exceptional star at X-ray energies. To explain its full X-ray properties, a generating mechanism beyond standard explanations, like the presence of a low-mass companion or magnetically confined wind-shocks, is required. Magnetospheric activity might be present or, as proposed for fast-rotating strongly magnetic Bp stars, the X-ray emission of CU Vir is predominantly auroral in nature.
KW  - individual: CU Vir
KW  - stars: activity
KW  - stars: chemically peculiar
KW  - stars: magnetic field
KW  - X-rays: stars
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201833492
SN  - 1432-0746
VL  - 619
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Oskinova, Lidia M.
A1  - Bulik, Tomasz
A1  - Gomez-Moran, Ada Nebot
T1  - Infrared outbursts as potential tracers of common-envelope events in high-mass X-ray binary formation
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. Classic massive binary evolutionary scenarios predict that a transitional common-envelope (CE) phase could be preceded as well as succeeded by the evolutionary stage when a binary consists of a compact object and a massive star, that is, a high-mass X-ray binary (HMXB). The observational manifestations of common envelope are poorly constrained. We speculate that its ejection might be observed in some cases as a transient event at mid-infrared (IR) wavelengths. Aims. We estimate the expected numbers of CE ejection events and HMXBs per star formation unit rate, and compare these theoretical estimates with observations. Methods. We compiled a list of 85 mid-IR transients of uncertain nature detected by the Spitzer Infrared Intensive Transients Survey and searched for their associations with X-ray, optical, and UV sources. Results. Confirming our theoretical estimates, we find that only one potential HMXB may be plausibly associated with an IR-transient and tentatively propose that X-ray source NGC4490-X40 could be a precursor to the SPIRITS 16az event. Among other interesting sources, we suggest that the supernova remnant candidate [BWL2012] 063 might be associated with SPIRITS 16ajc. We also find that two SPIRITS events are likely associated with novae, and seven have potential optical counterparts. Conclusions. The massive binary evolutionary scenarios that involve CE events do not contradict currently available observations of IR transients and HMXBs in star-forming galaxies.
KW  - X-rays: binaries
KW  - stars: massive
KW  - infrared: general
KW  - infrared: galaxies
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201832925
SN  - 0004-6361
SN  - 1432-0746
VL  - 613
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Pillitteri, Ignazio
A1  - Fossati, Luca
A1  - Rodriguez, N. Castro
A1  - Oskinova, Lidia M.
A1  - Wolk, Scott J.
T1  - Detection of magnetic field in the B2 star rho Ophiuchi A with ESO FORS2
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Circumstantial evidence suggests that magnetism and enhanced X-ray emission are likely correlated in early B-type stars: similar fractions of them (similar to 10%) are strong and hard X-ray sources and possess strong magnetic fields. It is also known that some B-type stars have spots on their surface. Yet up to now no X-ray activity associated with spots on early-type stars was detected. In this Letter we report the detection of a magnetic field on the B2V star rho Oph A. Previously, we assessed that the X-ray activity of this star is associated with a surface spot, herewith we establish its magnetic origin. We analyze spectra of rho Oph A obtained with the FORS2 spectrograph at ESO Very Large Telescope (VLT) at two epochs, and detect a longitudinal component of the magnetic field of the order of similar to 500 G in one of the datasets. The detection of the magnetic field only at one epoch can be explained by stellar rotation which is also invoked to explain observed periodic X-ray activity. From archival HARPS ESO VLT high resolution spectra we derived the fundamental stellar parameters of rho Oph A and further constrained its age. We conclude that rho Oph A provides strong evidence for the presence of active X-ray emitting regions on young magnetized early type stars.
KW  - stars: activity
KW  - stars: early-type
KW  - stars: magnetic field
KW  - pulsars: individual: rho Ophiuchi A
Y1  - 2017
U6  - https://doi.org/10.1051/0004-6361/201732078
SN  - 1432-0746
VL  - 610
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Gruner, David
A1  - Hainich, Rainer
A1  - Sander, Andreas Alexander Christoph
A1  - Shenar, Tomer
A1  - Todt, Helge Tobias
A1  - Oskinova, Lidia M.
A1  - Ramachandran, Varsha
A1  - Ayres, T.
A1  - Hamann, Wolf-Rainer
T1  - The extreme O-type spectroscopic binary HD 93129A A quantitative, multiwavelength analysis
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. HD 93129A was classified as the earliest O-type star in the Galaxy (O2 If*) and is considered as the prototype of its spectral class. However, interferometry shows that this object is a binary system, while recent observations even suggest a triple configuration. None of the previous spectral analyses of this object accounted for its multiplicity. With new high-resolution UV and optical spectra, we have the possibility to reanalyze this key object, taking its binary nature into account for the first time. Aims. We aim to derive the fundamental parameters and the evolutionary status of HD 93129A, identifying the contributions of both components to the composite spectrum Results. Despite the similar spectral types of the two components, we are able to find signatures from each of the components in the combined spectrum, which allows us to estimate the parameters of both stars. We derive log(L/L-circle dot) = 6.15, T-eff = 52 kK, and log (M)over dot = -4.7[M-circle dot yr(-1)] for the primary Aa, and log(L/L-circle dot) = 5.58, T-eff = 45 kK, and log (M)over dot = -5.8 [M(circle dot)yr(-1)] for the secondary Ab. Conclusions. Even when accounting for the binary nature, the primary of HD 93129A is found to be one of the hottest and most luminous O stars in our Galaxy. Based on the theoretical decomposition of the spectra, we assign spectral types O2 If* and O3 III(f*) to components Aa and Ab, respectively. While we achieve a good fit for a wide spectral range, specific spectral features are not fully reproduced. The data are not sufficient to identify contributions from a hypothetical third component in the system.
KW  - stars: individual: HD 93129A
KW  - stars: atmospheres
KW  - stars: fundamental parameters
KW  - stars: early-typeP
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201833178
SN  - 1432-0746
VL  - 621
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Hainich, Rainer
A1  - Oskinova, Lidia M.
A1  - Shenar, Tomer
A1  - Marchant Campos, Pablo
A1  - Eldridge, J. J.
A1  - Sander, Andreas Alexander Christoph
A1  - Hamann, Wolf-Rainer
A1  - Langer, Norbert
A1  - Todt, Helge Tobias
T1  - Observational properties of massive black hole binary progenitors
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context:
The first directly detected gravitational waves (GW 150914) were emitted by two coalescing black holes (BHs) with masses of ≈ 36 M⊙ and ≈ 29 M⊙. Several scenarios have been proposed to put this detection into an astrophysical context. The evolution of an isolated massive binary system is among commonly considered models.
Aims:
Various groups have performed detailed binary-evolution calculations that lead to BH merger events. However, the question remains open as to whether binary systems with the predicted properties really exist. The aim of this paper is to help observers to close this gap by providing spectral characteristics of massive binary BH progenitors during a phase where at least one of the companions is still non-degenerate.
Methods:
Stellar evolution models predict fundamental stellar parameters. Using these as input for our stellar atmosphere code (Potsdam Wolf-Rayet), we compute a set of models for selected evolutionary stages of massive merging BH progenitors at different metallicities.
Results:
The synthetic spectra obtained from our atmosphere calculations reveal that progenitors of massive BH merger events start their lives as O2-3V stars that evolve to early-type blue supergiants before they undergo core-collapse during the Wolf-Rayet phase. When the primary has collapsed, the remaining system will appear as a wind-fed high-mass X-ray binary. Based on our atmosphere models, we provide feedback parameters, broad band magnitudes, and spectral templates that should help to identify such binaries in the future.
Conclusions:
While the predicted parameter space for massive BH binary progenitors is partly realized in nature, none of the known massive binaries match our synthetic spectra of massive BH binary progenitors exactly. Comparisons of empirically determined mass-loss rates with those assumed by evolution calculations reveal significant differences. The consideration of the empirical mass-loss rates in evolution calculations will possibly entail a shift of the maximum in the predicted binary-BH merger rate to higher metallicities, that is, more candidates should be expected in our cosmic neighborhood than previously assumed.
KW  - gravitational waves
KW  - binaries: close
KW  - stars: early-type
KW  - stars: atmospheres
KW  - stars: winds
KW  - outflows
KW  - stars: mass-loss
Y1  - 2018
U6  - https://doi.org/10.1051/0004-6361/201731449
SN  - 1432-0746
VL  - 609
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Fulmer, Leah M.
A1  - Gallagher, John S.
A1  - Hamann, Wolf-Rainer
A1  - Oskinova, Lidia M.
A1  - Ramachandran, Varsha
T1  - Testing massive star evolution, star-formation history, and feedback at low metallicity
BT  - photometric analysis of OB stars in the SMC Wing
JF  - Astronomy and astrophysics : an international weekly journal
N2  - Context. 
The supergiant ionized shell SMC-SGS 1 (DEM 167), which is located in the outer Wing of the Small Magellanic Cloud (SMC), resembles structures that originate from an energetic star-formation event and later stimulate star formation as they expand into the ambient medium. However, stellar populations within and surrounding SMC-SGS 1 tell a different story. Aims. We present a photometric study of the stellar population encompassed by SMC-SGS 1 in order to trace the history of such a large structure and its potential influence on star formation within the low-density, low-metallicity environment of the SMC. 

Methods. 
For a stellar population that is physically associated with SMC-SGS 1, we combined near-ultraviolet (NUV) photometry from the Galaxy Evolution Explorer with archival optical (V-band) photometry from the ESO Danish 1.54 m Telescope. Given their colors and luminosities, we estimated stellar ages and masses by matching observed photometry to theoretical stellar isochrone models. Results. We find that the investigated region supports an active, extended star-formation event spanning similar to 25-40 Myr ago, as well as continued star formation into the present. Using a standard initial mass function, we infer a lower bound on the stellar mass from this period of similar to 3 x 10(4) M-circle dot, corresponding to a star-formation intensity of similar to 6 x 10(-3) M-circle dot kpc(-2) yr(-1). 

Conclusions. 
The spatial and temporal distributions of young stars encompassed by SMC-SGS 1 imply a slow, consistent progression of star formation over millions of years. Ongoing star formation, both along the edge and interior to SMC-SGS 1, suggests a combined stimulated and stochastic mode of star formation within the SMC Wing. We note that a slow expansion of the shell within this low-density environment may preserve molecular clouds within the volume of the shell, leaving them to form stars even after nearby stellar feedback expels local gas and dust.
KW  - galaxies
KW  - stellar content
KW  - stars
KW  - formation
KW  - individual
KW  - Small
KW  - Magellanic Cloud
Y1  - 2020
U6  - https://doi.org/10.1051/0004-6361/201834314
SN  - 0004-6361
SN  - 1432-0746
VL  - 633
PB  - EDP Sciences
CY  - Les Ulis
ER  - 
TY  - JOUR
A1  - Geist, Emily
A1  - Gallagher, John S.
A1  - Kotulla, Ralf
A1  - Oskinova, Lidia M.
A1  - Hamann, Wolf-Rainer
A1  - Ramachandran, Varsha
A1  - Sabbi, Elena
A1  - Smith, Linda J.
A1  - Kniazev, Alexey
A1  - Nota, Antonella
A1  - Rickard, Matthew J.
T1  - Ionization and star formation in the giant H ii region SMC-N66
JF  - Publications of the Astronomical Society of the Pacific
N2  - The NGC 346 young stellar system and associated N66 giant H ii region in the Small Magellanic Cloud are the nearest example of a massive star-forming event in a low metallicity (Z approximate to 0.2Z (circle dot)) galaxy. With an age of less than or similar to 3 Myr this system provides a unique opportunity to study relationships between massive stars and their associated H ii region. Using archival data, we derive a total H alpha luminosity of L(H alpha) = 4.1 x 10(38) erg s(-1) corresponding to an H-photoionization rate of 3 x 10(50) s(-1). A comparison with a predicted stellar ionization rate derived from the more than 50 known O-stars in NGC 346, including massive stars recently classified from Hubble Space Telescope far-ultraviolet (FUV) spectra, indicates an approximate ionization balance. Spectra obtained with SALT suggest the ionization structure of N66 could be consistent with some leakage of ionizing photons. Due to the low metallicity, the FUV luminosity from NGC 346 is not confined to the interstellar cloud associated with N66. Ionization extends through much of the spatial extent of the N66 cloud complex, and most of the cloud mass is not ionized. The stellar mass estimated from nebular L(H alpha) appears to be lower than masses derived from the census of resolved stars which may indicate a disconnect between the formation of high and low mass stars in this region. We briefly discuss implications of the properties of N66 for studies of star formation and stellar feedback in low metallicity environments.
Y1  - 2022
U6  - https://doi.org/10.1088/1538-3873/ac697b
SN  - 0004-6280
SN  - 1538-3873
VL  - 134
IS  - 1036
PB  - IOP Publishing
CY  - Bristol
ER  -