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Peritoneal dialysis (PD) is a method of renal replacement therapy that offers both medical and economic advantages. To patients it offers a safe therapy option that can be administered autonomously at home. Nevertheless, its adoption has remained slow, and most health care systems are still dominated by in-centre haemodialysis. One factor that determines overall prescription of peritoneal dialysis is the attitude of nephrologists towards the method and their confidence in administering peritoneal dialysis, especially in cases where patients present various comorbidities. This study analyses data gathered in the Mau-PD project between 2018 and 2019. A questionnaire that was sent to all nephrologists in Germany working in the ambulatory sector was analysed to determine how they perceive peritoneal dialysis, how they view their training and if they would prefer peritoneal dialysis or haemodialysis in certain cases. As a factor that may influence this inclination to favour one over the other, the size of dialysis centres in terms of absolute patient numbers was proposed as an explanatory variable in a linear regression model. So far, centre size has been studied in its effect on mortality and technique failure; however, its effect on nephrologist attitude and ultimately prescription habits, has so far not been studied. The main findings of this study are that most German nephrologists view peritoneal dialysis as an equivalent method to haemodialysis in terms of medical outcome (90.88%). Only 23.33% of German nephrologists considered their training in peritoneal dialysis to be thorough. When presented with patients presenting various comorbidities nephrologists, on the whole, preferred haemodialysis over peritoneal dialysis (3.42884; St. Err.: 0.0173021; 95%CI: 3.394856– 3.462824; on a 5-point scale where 1 = total preference for peritoneal dialysis and 5 = total preference for haemodialysis). This general inclination was shifted towards a preference for peritoneal dialy

© ESO 2015. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The support of the German BMBF and MPG, the Italian INFN, the Swiss National Fund SNF, and the ERDF funds under the Spanish MINECO is gratefully acknowledged. This work was also supported by the CPAN CSD2007-00042 and MultiDark CSD2009-00064 projects of the Spanish Consolider-Ingenio 2010 programme, by grant 127740 of the Academy of Finland, by the Croatian Science Foundation (HrZZ) Project 09/176, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, and by the Polish MNiSzWgrant 745/N-HESS-MAGIC/2010/0. J.C. acknowledges support by the Spanish Ministerio de Economía y Competividad (MINECO) under grant AYA2010-18080. The authors thank the anonymous referee for a thorough review and a very constructive list of remarks that helped improving the quality and clarity of this manuscript., Context. MWC 656 has recently been established as the first observationally detected high-mass X-ray binary system containing a Be star and a black hole (BH). The system has been associated with a gamma-ray flaring event detected by the AGILE satellite in July 2010. Aims. Our aim is to evaluate if the MWC 656 gamma-ray emission extends to very high energy (VHE > 100 GeV) gamma rays. Methods. We have observed MWC 656 with the MAGIC telescopes for ∼23 hours during two observation periods: between May and June 2012 and June 2013. During the last period, observations were performed contemporaneously with X-ray (XMM-Newton) and optical (STELLA) instruments. Results. We have not detected the MWC 656 binary system at TeV energies with the MAGIC Telescopes in either of the two campaigns carried out. Upper limits (ULs) to the integral flux above 300 GeV have been set, as well as differential ULs at a level of ∼ 5% of the Crab Nebula flux. The results obtained from the MAGIC observations do not support persistent emission of very high energy gamma rays from this system at a level of 2.4% the Crab flux., German BMBF, German MPG, Italian INFN, Spanish MINECO, Academy of Finland, by the Croatian Science Foundation (HrZZ), DFG Collaborative Research Centers, Polish MNiSzWgrant, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

Diese Arbeit untersucht Möglichkeiten zur Einsparung von Treibhausgasen (THG) im Nichtwohngebäudebestand. Quantifiziert werden die Potentiale der Strategien „Temperaturabsenkung“ (TAS) und „Energieflexibilisierung“ (FLEX) unter Berücksichtigung von thermischen Komfortanforderungen. Dabei wird TAS über Deckenheizsysteme und FLEX über die aktive Nutzung der Gebäudespeichermasse erreicht. Vor dem Hintergrund der Notwendigkeit, zukünftig verstärkt erneuerbare Energien zu nutzen, sind die Strategien TAS und FLEX ein wichtiger Baustein zur Dekarbonisierung von Gebäudeenergiesystemen. Obwohl die Sanierung des Gebäudebestands als ein zentraler Schlüssel zur Erfüllung der Energie- und Klimaziele angesehen wird, konzentrieren sich bisherige Ansätze vorrangig auf Wohngebäude im Neubaubereich. Deshalb fokussiert diese Arbeit auf den Nichtwohngebäudebestand und sucht insbesondere alternative Sanierungskonzepte für Gebäude, für die die Umsetzung „herkömmlicher“ Strategien des energieeffizienten Bauens (z. B. außenliegender Wärmeschutz) problematisch ist. Bislang liegt kein Instrumentarium vor, das es Planern ermöglicht, den Einfluss verschiedener Sanierungsoptionen im Gebäudebestand zur Umsetzung der Strategien TAS und FLEX auf das THG-Einsparpotential abzuschätzen. Diese Lücke füllt diese Arbeit. FLEX und TAS tragen auf unterschiedlichen Wegen dazu bei, THG-intensive Energieträger in der Versorgung von Gebäuden zu ersetzen. Energieflexibilität ist in Energieversorgungssystemen, die zunehmend auf volatilen, d. h. wetterabhängigen, erneuerbaren Energien beruhen, eine wichtige Gebäudeeigenschaft. Sie ermöglicht es Gebäuden, im Stromnetz vorhandene Überschüsse an erneuerbaren Energien zu speichern und damit in Zeiträumen, in denen das erneuerbare Angebot nicht ausreicht, auf den Bezug fossiler Energien zu verzichten. Heizsysteme im unsanierten Gebäudebestand beruhen in der Regel auf hohen Systemtemperaturen. Um jedoch erneuerbare Wärme, die häufig auf einem deutlich niedrigeren Temp

© 2020. The American Astronomical Society. All rights reserved. Artículo firmado por 259 autores. This research is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation, the Smithsonian Institution, and NSERC in Canada. This research used resources provided by the Open Science Grid, which is supported by the National Science Foundation and the U.S. Department of Energy's Office of Science, and the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under contract No. DE-AC0205CH11231. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and the collaborating institutions in the construction and operation of the instrument.; The MAGIC collaboration would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP201571662-C2-2-P, FPA201790566REDC), the Indian Department of Atomic Energy, the Japanese JSPS and MEXT, and the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2016-0588 and SEV2015-0548 and Unidad de Excelencia "María de Maeztu" MDM-2014-0369, the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782, the University of Rijeka Project 13.12.1.3.02, the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382, and the Brazilian MCTIC, CNPq, and FAPERJ.; This publica, We report on variability and correlation studies using multiwavelength observations of the blazar Mrk 421 during the month of 2010 February, when an extraordinary flare reaching a level of similar to 27 Crab Units above 1 TeV was measured in very high energy (VHE) gamma-rays with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) observatory. This is the highest flux state for Mrk 421 ever observed in VHE gamma-rays. Data are analyzed from a coordinated campaign across multiple instruments, including VHE gamma-ray (VERITAS, Major Atmospheric Gamma-ray Imaging Cherenkov), high-energy gamma-ray (Fermi-LAT), X-ray (Swift, Rossi X-ray Timing Experiment, MAXI), optical (including the GASP-WEBT collaboration and polarization data), and radio (Metsahovi, Owens Valley Radio Observatory, University of Michigan Radio Astronomy Observatory). Light curves are produced spanning multiple days before and after the peak of the VHE flare, including over several flare "decline" epochs. The main flare statistics allow 2 minute time bins to be constructed in both the VHE and optical bands enabling a cross-correlation analysis that shows evidence for an optical lag of similar to 25-55 minutes, the first time-lagged correlation between these bands reported on such short timescales. Limits on the Doppler factor (delta greater than or similar to 33) and the size of the emission region (delta R--1(B) less than or similar to 3.8 x 10(13) cm) are obtained from the fast variability observed by VERITAS during the main flare. Analysis of 10 minute binned VHE and X-ray data over the decline epochs shows an extraordinary range of behavior in the flux-flux relationship, from linear to quadratic to lack of correlation to anticorrelation. Taken together, these detailed observations of an unprecedented flare seen in Mrk 421 are difficult to explain with the classic single-zone synchrotron self-Compton model., Ministerio de Economía y Competitividad (MINECO)/FEDER, Centro de Excelencia Severo Ochoa, Unidad de Excelencia María de Maeztu, U.S. Department of Energy Office of Science United States Department of Energy (DOE), U.S. National Science Foundation (NSF), Smithsonian Institution, NSERC in Canada Natural Sciences and Engineering Research Council of Canada, National Science Foundation (NSF), U.S. Department of Energy's Office of Science United States Department of Energy (DOE), National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility, German BMBF Federal Ministry of Education & Research (BMBF), MPG Max Planck Society, Italian INFN Istituto Nazionale di Fisica Nucleare, INAF, Swiss National Fund SNF Swiss National Science Foundation (SNSF), Indian Department of Atomic Energy, Japanese JSPS, Japanese MEXT, Bulgarian Ministry of Education and Science, National RI Roadmap Project, Croatian Science Foundation (HrZZ) Project, University of Rijeka Project, DFG Collaborative Research Centers German Research Foundation (DFG), Polish National Research Centre grant, Brazilian MCTIC, Brazilian CNPq National Council for Scientific and Technological Development (CNPq), Brazilian FAPERJ, NASA National Aeronautics & Space Administration, NSF National Science Foundation (NSF), NASA Fermi GI award, Russian RFBR foundation, Shota Rustaveli National Science Foundation, Fermi Guest Investigator Program, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© MAGIC Collaboration 2020. Artículo firmado por 307 autores. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), the Indian Department of Atomic Energy, the Japanese JSPS and MEXT, the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia "María de Maeztu" MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. This research has made use of the CTA instrument response functions provided by the CTA Consortium and Observatory, see http://www.cta-observatory.org/science/cta-performance/(version prod3b-v1) for more details., Aims. We measure the Crab Nebula gamma-ray spectral energy distribution in the 100 TeV energy domain and test the validity of existing leptonic emission models at these high energies.Methods. We used the novel very large zenith angle observations with the MAGIC telescope system to increase the collection area above 10 TeV. We also developed an auxiliary procedure of monitoring atmospheric transmission in order to assure proper calibration of the accumulated data. This employs recording optical images of the stellar field next to the source position, which provides a better than 10% accuracy for the transmission measurements.Results. We demonstrate that MAGIC very large zenith angle observations yield a collection area larger than a square kilometer. In only 56 h of observations, we detect the gamma-ray emission from the Crab Nebula up to 100 TeV, thus providing the highest energy measurement of this source to date with Imaging Atmospheric Cherenkov Telescopes. Comparing accumulated and archival MAGIC and Fermi/LAT data with some of the existing emission models, we find that none of them provides an accurate description of the 1 GeV to 100 TeV gamma-ray signal., ERDF under the Spanish MINECO, Centro de Excelencia Severo Ochoa, Unidad de Excelencia María de Maeztu, German BMBF Federal Ministry of Education & Research (BMBF), MPG Max Planck Society, Italian INFN Istituto Nazionale di Fisica Nucleare, Italian INAF, Swiss National Fund SNF Swiss National Science Foundation (SNSF), Indian Department of Atomic Energy, Japanese JSPS Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science, MEXT Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT), Bulgarian Ministry of Education and Science, National RI Roadmap Project, Academy of Finland, Croatian Science Foundation (HrZZ), University of Rijeka Project, DFG Collaborative Research Centers German Research Foundation (DFG), Polish National Research Centre, Brazilian MCTIC, CNPq National Council for Scientific and Technological Development (CNPq), FAPERJ Carlos Chagas Filho Foundation for Research Support of the State of Rio de Janeiro (FAPERJ), Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© 2020. The American Astronomical Society. All rights reserved. Artículo firmado por 177 autores. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA 2015-68378-P, FPA2017-82729-C6-2-R, FPA2015-69210-C64-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA201676012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-RE DC), the Indian Department of Atomic Energy, the Japanese JSPS and MEXT, the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018, and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia "María de Maeztu" MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382, and by the Brazilian MCTIC, CNPq and FAPERJ.; E.P. has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sklodowska-Curie grant agreement No. 664931.; M.C. has received financial support through the Postdoctoral Junior Leader Fellowship Programme from la Caixa Banking Foundation, grant No. LCF/BQ/LI18/11630012., Extreme high-frequency-peaked BL Lac objects (EHBLs) are blazars that exhibit extremely energetic synchrotron emission. They also feature nonthermal gamma-ray emission whose peak lies in the very high-energy (VHE, E > 100 GeV) range, and in some sources exceeds 1 TeV: this is the case for hard-TeV EHBLs such as 1ES 0229+200. With the aim of increasing the EHBL population, 10 targets were observed with the MAGIC telescopes from 2010 to 2017, for a total of 265 hr of good-quality data. The data were complemented by coordinated Swift observations. The X-ray data analysis confirms that all but two sources are EHBLs. The sources show only a modest variability and a harder-when-brighter behavior, typical for this class of objects. At VHE gamma-rays, three new sources were detected and a hint of a signal was found for another new source. In each case, the intrinsic spectrum is compatible with the hypothesis of a hard-TeV nature of these EHBLs. The broadband spectral energy distributions (SEDs) of all sources are built and modeled in the framework of a single-zone, purely leptonic model. The VHE gamma-ray-detected sources were also interpreted with a spine-layer model and a proton synchrotron model. The three models provide a good description of the SEDs. However, the resulting parameters differ substantially in the three scenarios, in particular the magnetization parameter. This work presents the first mini catalog of VHE gamma-ray and multiwavelength observations of EHBLs., Unión Europea. Horizonte 2020, Ministerio de Economía y Competitividad (MINECO)/FEDER, Centro de Excelencia Severo Ochoa, Unidad de Excelencia Maria de Maeztu, German BMBF Federal Ministry of Education & Research (BMBF), German MPG, Italian INFN Istituto Nazionale di Fisica Nucleare, Italian INAF Istituto Nazionale Astrofisica, Swiss National Fund SNF Swiss National Science Foundation (SNSF), Indian Department of Atomic Energy, Japanese JSPS Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT) Japan Society for the Promotion of Science, Japanese MEXTMinistry of Education, Culture, Sports, Science and Technology, Japan (MEXT), Bulgarian Ministry of Education and Science, National RI Roadmap Project, Academy of FinlandAcademy of Finland, Croatian Science Foundation (HrZZ), University of Rijeka, DFG Collaborative Research Centers, Polish National Research Centre, Brazilian MCTIC, Brazilian CNPq National Council for Scientific and Technological Development (CNPq), Brazilian FAPERJ, La Caixa Banking Foundation, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© 2020 Elsevier B.V. All rights reserved. Artículo escrito por 161 autores. We would also like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, Germany, the Italian INFN and INAF, Italy, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2017-87859-P, FPA2017-85668-P, FPA2017-82729C6-2-R, FPA2017-82729-C6-6-R, FPA2017-82729-C6-5-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2017-87055-C22-P, FPA2017-90566-REDC), the Indian Department of Atomic Energy, the Japanese JSPS, Japan and MEXT, Japan, the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia ``Severo Ochoa'' SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia ``María de Maeztu'' MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka, Croatia Project 13.12.1.3.02, by the DFG, Germany Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre, Polland grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq, Brazil and FAPERJ, Brazil., We present the first results from very-high-energy observations of the dwarf spheroidal satellite candidate Triangulum II with the MAGIC telescopes from 62.4 h of good-quality data taken between August 2016 and August 2017. We find no gamma-ray excess in the direction of Triangulum II, and upper limits on both the differential and integral gamma-ray flux are presented. Currently, the kinematics of Triangulum II are affected by large uncertainties leading to a bias in the determination of the properties of its dark matter halo. Using a scaling relation between the annihilation J-factor and heliocentric distance of well-known dwarf spheroidal galaxies, we estimate an annihilation J-factor for Triangulum II for WIMP dark matter of log[J(ann)(0.5 degrees)/GeV2 cm(-5)] = 19.35 +/- 0.37. We also derive a dark matter density profile for the object relying on results from resolved simulations of Milky Way sized dark matter halos. We obtain 95% confidence-level limits on the thermally averaged annihilation cross section for WIMP annihilation into various Standard Model channels. The most stringent limits are obtained in the tau(-)tau(+) final state, where a cross section for annihilation down to = 3.05 x 10(-24) cm(3) s(-1) is excluded. (C) 2020 Elsevier B.V. All rights reserved., Ministerio de Economía y Competitividad (MINECO)/FEDER, Centro de Excelencia "Severo Ochoa", Unidad de Excelencia "María de Maeztu'', German BMBF, Germany Federal Ministry of Education & Research (BMBF), German MPG, Germany, Italian INAF, Italy, Italian INFN, Italy, Swiss National Fund SNF, Swiss National Science Foundation (SNSF), Indian Department of Atomic Energy, Japanese JSPS, Japan, MEXT, Japan Ministry of Education, Culture, Sports, Science and Technology, Bulgarian Ministry of Education and Science, National RI Roadmap Project, Academy of Finland, Croatian Science Foundation (HrZZ), University of Rijeka, Croatia, DFG, Germany Collaborative Research Centers German Research Foundation (DFG), Polish National Research Centre, Polland, Brazilian MCTIC, Brazil, Brazilian CNPq, Brazil, Brazilian FAPERJ, Brazil, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2020. Artículo firmado por 185 autores. The authors thank the anonymous referee for providing a constructive list of remarks that allowed us to clarify and improve some of the results reported in the manuscript. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia "María de Maeztu" MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique/Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA, Context. Markarian 501 (Mrk 501) is a very high-energy (VHE) gamma-ray blazar located at z=0.034, which is regularly monitored by a wide range of multi-wavelength instruments, from radio to VHE gamma rays. During a period of almost two weeks in July 2014, the highest X-ray activity of Mrk 501 was observed in similar to 14 years of operation of the Neil Gehrels Swift Gamma-ray Burst Observatory.Aims. We characterize the broadband variability of Mrk 501 from radio to VHE gamma rays during the most extreme X-ray activity measured in the last 14 years, and evaluate whether it can be interpreted within theoretical scenarios widely used to explain the broadband emission from blazars.Methods. The emission of Mrk 501 was measured at radio with Metsahovi, at optical-UV with KVA and Swift/UVOT, at X-ray with Swift/XRT and Swift/BAT, at gamma ray with Fermi-LAT, and at VHE gamma rays with the FACT and MAGIC telescopes. The multi-band variability and correlations were quantified, and the broadband spectral energy distributions (SEDs) were compared with predictions from theoretical models.Results. The VHE emission of Mrk 501 was found to be elevated during the X-ray outburst, with a gamma-ray flux above 0.15 TeV varying from similar to 0.5 to similar to 2 times the Crab nebula flux. The X-ray and VHE emission both varied on timescales of 1 day and were found to be correlated. We measured a general increase in the fractional variability with energy, with the VHE variability being twice as large as the X-ray variability. The temporal evolution of the most prominent and variable segments of the SED, characterized on a day-by-day basis from 2014 July 16 to 2014 July 31, is described with a one-zone synchrotron self-Compton model with variations in the break energy of the electron energy distribution (EED), and with some adjustments in the magnetic field strength and spectral shape of the EED. These results suggest that the main flux variations during this extreme X-ray outburst are, Ministerio de Economía y Competitividad (MINECO)/FEDER, Centro de Excelencia "Severo Ochoa", Unidad de Excelencia "María de Maeztu", German BMBF Federal Ministry of Education & Research (BMBF), German MPG, Italian INFN Istituto Nazionale di Fisica Nucleare (INFN), Italian INAF Istituto Nazionale Astrofisica (INAF), Swiss National Fund SNF Swiss National Science Foundation (SNSF), Japanese JSPS, Japanese MEXT, Croatian Science Foundation (HrZZ), University of Rijeka Project, DFG Collaborative Research Centers German Research Foundation (DFG), Polish National Research Centre, Brazilian MCTIC, Brazilian CNPq National Council for Scientific and Technological Development, Brazilian FAPERJ, ETH Zurich, German BMBF (Verbundforschung Astro- und Astroteilchenphysik), German HAP (Helmoltz Alliance for Astroparticle Physics), Deutsche Forschungsgemeinschaft (DFG) within the Collaborative Research Center German Research Foundation (DFG), Viera y Clavijo program - ACIISI, ULL, Project "Promotion inklusive" of the Universitat zu Koln, German Bundesministerium fur Arbeit und Soziales, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© MAGIC Collaboration 2020. Artículo firmado por 175 autores. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. We also thank Dario Grasso for the valuable comments. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), the Indian Department of Atomic Energy, the Japanese JSPS and MEXT, the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 and the Academy of Finland grant nr. 320045 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia "María de Maeztu" MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Center grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ., Aims. In the presence of a sufficient amount of target material, gamma-rays can be used as a tracer in the search for sources of Galactic cosmic rays (CRs). Here we present deep observations of the Galactic center (GC) region with the MAGIC telescopes and use them to infer the underlying CR distribution and to study the alleged PeV proton accelerator at the center of our Galaxy.Methods. We used data from approximate to 100 h observations of the GC region conducted with the MAGIC telescopes over five years (from 2012 to 2017). Those were collected at high zenith angles (58-70 deg), leading to a larger energy threshold, but also an increased effective collection area compared to low zenith observations. Using recently developed software tools, we derived the instrument response and background models required for extracting the diffuse emission in the region. We used existing measurements of the gas distribution in the GC region to derive the underlying distribution of CRs. We present a discussion of the associated biases and limitations of such an approach.Results. We obtain a significant detection for all four model components used to fit our data (Sgr A*, "Arc", G0.9+0.1, and an extended component for the Galactic Ridge). We observe no significant difference between the gamma-ray spectra of the immediate GC surroundings, which we model as a point source (Sgr A*) and the Galactic Ridge. The latter can be described as a power-law with index 2 and an exponential cut-off at around 20 TeV with the significance of the cut-off being only 2 sigma. The derived cosmic-ray profile hints to a peak at the GC position and with a measured profile index of 1.2 +/- 0.3 is consistent with the 1/r radial distance scaling law, which supports the hypothesis of a CR accelerator at the GC. We argue that the measurements of this profile are presently limited by our knowledge of the gas distribution in the GC vicinity., Ministerio de Economía y Competitividad (MINECO), German BMBF Federal Ministry of Education & Research (BMBF), Centro de Excelencia Severo Ochoa, Centro de Excelencia María de Maeztu, MPG Max Planck Society, Italian INFN Istituto Nazionale di Fisica Nucleare (INFN), Italian INAF Istituto Nazionale Astrofisica (INAF), Swiss National Fund SNF Swiss National Science Foundation (SNSF), Indian Department of Atomic Energy, Japanese JSPS Ministry of Education, Culture, Sports, Science and Technology, Japanese MEXT Ministry of Education, Culture, Sports, Science and Technology, Bulgarian Ministry of Education and Science, National RI Roadmap Project, Academy of Finland, Croatian Science Foundation (HrZZ) Project, University of Rijeka, DFG Collaborative Research Centers German Research Foundation (DFG), Polish National Research Center, Brazilian MCTIC, Brazilian CNPq National Council for Scientific and Technological Development (CNPq), Brazilian FAPERJ, Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub

© ESO 2020. Artículo firmado por 164 autores. We would like to thank the Instituto de Astrofísica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, FPA2017-90566-REDC), the Indian Department of Atomic Energy, the Japanese JSPS and MEXT and the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018 is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2016-0588 and SEV-2015-0548, and Unidad de Excelencia "María de Maeztu" MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. The Fermi-LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat a l'Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucleaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenbe, 1ES 1959+650 is a bright TeV high-frequency-peaked BL Lac object exhibiting interesting features like "orphan" TeV flares and broad emission in the high-energy regime that are difficult to interpret using conventional one-zone Synchrotron Self-Compton (SSC) scenarios. We report the results from the Major Atmospheric Gamma Imaging Cherenkov (MAGIC) observations in 2016 along with the multi-wavelength data from the Fermi Large Area Telescope (LAT) and Swift instruments. MAGIC observed 1ES 1959+650 with different emission levels in the very-high-energy (VHE, E> 100 GeV) gamma -ray band during 2016. In the long-term data, the X-ray spectrum becomes harder with increasing flux and a hint of a similar trend is also visible in the VHE band. An exceptionally high VHE flux reaching similar to 3 times the Crab Nebula flux was measured by MAGIC on the 13 and 14 of June, and 1 July 2016 (the highest flux observed since 2002). During these flares, the high-energy peak of the spectral energy distribution (SED) lies in the VHE domain and extends up to several TeV. The spectrum in the gamma -ray (both Fermi-LAT and VHE bands) and the X-ray bands are quite hard. On 13 June and 1 July 2016, the source showed rapid variations in the VHE flux within timescales of less than an hour. A simple one-zone SSC model can describe the data during the flares requiring moderate to large values of the Doppler factors (delta >= 30-60). Alternatively, the high-energy peak of the SED can be explained by a purely hadronic model attributed to proton-synchrotron radiation with jet power L-jet similar to 10(46) erg s(-1) and under high values of the magnetic field strength (similar to 100 G) and maximum proton energy (similar to few EeV). Mixed lepto-hadronic models require super-Eddington values of the jet power. We conclude that it is difficult to get detectable neutrino emission from the source during the extreme VHE flaring period of 2016., Ministerio de Economía y Competitividad (MINECO)/FEDER, Centro de Excelencia "Severo Ochoa", Unidad de Excelencia "María de Maeztu", German BMBF Federal Ministry of Education & Research (BMBF), German MPG, Italian INFN Istituto Nazionale di Fisica Nucleare (INFN), Italian INAF Istituto Nazionale Astrofisica (INAF), Swiss National Fund SNF Swiss National Science Foundation (SNSF), Indian Department of Atomic Energy, Japanese JSPS Ministry of Education, Culture, Sports, Science and Technology, Japanese MEXT Ministry of Education, Culture, Sports, Science and Technology, Bulgarian Ministry of Education and Science, National RI Roadmap Project, Croatian Science Foundation (HrZZ) Project, University of Rijeka, DFG Collaborative Research Centers German Research Foundation, Polish National Research Centre, Brazilian MCTIC, Brazilian CNPq National Council for Scientific and Technological Development, Brazilian FAPERJ, DOE United States Department of Energy (DOE), Depto. de Estructura de la Materia, Física Térmica y Electrónica, Fac. de Ciencias Físicas, TRUE, pub