13 research outputs found
The Relationship Between Body Morphology and Narcissism at Zero Acquaintance
No full textNarcissistic people are exceedingly successful in conveying positive first impressions to their social surrounding, yet, they appear to be the driving force behind unfavorable long-term social and romantic relationships. Hence, a quick identification of narcissistic people may be of adaptive value for their social partners. Narcissism perception research, however, is lacking evidence on human body morphology. In this study, N = 110 raters evaluated natural 3D body scans of unacquainted N = 307 target participants (152 men and 155 women) regarding narcissistic admiration and rivalry. Based on the Brunswikian lens model, multiple regression models revealed that bodily attractiveness (β = .54, 95% CI = [0.41; 0.66]), BMI (β = .32, 95% CI = [0.13; 0.51]), shoulder-to-hip ratio (β = .33, 95% CI = [0.20; 0.47]) and physical strength (β = .23, 95% CI = [0.07; 0.39]) were utilized in judging narcissistic admiration and rivalry. Shoulder-hip ratio showed small relationships with self-reported narcissistic admiration (β = .21, 95% CI = [0.03; 0.38]) and rivalry (β = .23, 95% CI = [0.07; 0.39]) that were not robust across all analyses. Correlations between self-reported and judged narcissism showed a significant positive association for narcissistic admiration (r = .17, 95% CI = [0.06; 0.28]). Results indicate a perceptual bias when judging narcissism, as perceivers used body cues to draw inferences about target’s levels of narcissism that were not significantly related to self-reported narcissistic admiration and rivalry (and can thus be seen as invalid). However, perceivers were able to somewhat accurately judge target’s levels of narcissistic admiration and rivalry, based on body morphology alone. Thus, people’s bodies might disclose social information at zero acquaintance, but different stimuli material with more information on the targets may lead to more accurate judgments
Prototyping a car seat with variable-stiffness soft robotic modules
No full textThis report concerned the development of a soft robotic module for a seat pan, its optimization and application. The soft robotic module has an LED and photosensors for determining the distance of indentation and the passive force created by compressing the foam spring inside. An air pressure sensor is used to determine the active force created when an air pump inflates the bellow with air. The system is trained by machine learning to calculate predictions of these distance and forces in real-time. In several iterations of the module the reproducibility and accuracy were developed in such a way that it could be built into a seat. Two modules are built into a seat pan and interestingly participants on the seat were able to experience significant comfort differences, showing that the principle works. Further development is needed to make a seat pan with more modules, combined with a central computing system that monitors, records and regulates the modules. Exploration of simplification by using a linear regression instead of a neural network to calculate the active force is recommended, as well exploration of improved functionality by dividing the neural network that calculates the distance of indentation.Integrated Product Desig
The relationship between body morphology and narcissism at zero acquaintance
No full textNarcissistic people are exceedingly successful in conveying positive first impressions to their social surrounding, yet, they appear to be the driving force behind unfavorable long-term social and romantic relationships. Hence, a quick identification of narcissistic people may be of adaptive value for their social partners. Narcissism perception research, however, is lacking evidence on human body morphology. In this study, N = 110 raters evaluated natural 3D body scans of unacquainted N = 307 target participants (152 men and 155 women) regarding narcissistic admiration and rivalry. Based on the Brunswikian lens model, multiple regression models revealed that bodily attractiveness (β = .54, 95% CI = [0.41; 0.66]), BMI (β = .32, 95% CI = [0.13; 0.51]), shoulder-to-hip ratio (β = .33, 95% CI = [0.20; 0.47]) and physical strength (β = .23, 95% CI = [0.07; 0.39]) were utilized in judging narcissistic admiration and rivalry. Shoulder-hip ratio showed small relationships with self-reported narcissistic admiration (β = .21, 95% CI = [0.03; 0.38]) and rivalry (β = .23, 95% CI = [0.07; 0.39]) that were not robust across all analyses. Correlations between self-reported and judged narcissism showed a significant positive association for narcissistic admiration (r = .17, 95% CI = [0.06; 0.28]). Results indicate a perceptual bias when judging narcissism, as perceivers used body cues to draw inferences about target’s levels of narcissism that were not significantly related to self-reported narcissistic admiration and rivalry (and can thus be seen as invalid). However, perceivers were able to somewhat accurately judge target’s levels of narcissistic admiration and rivalry, based on body morphology alone. Thus, people’s bodies might disclose social information at zero acquaintance, but different stimuli material with more information on the targets may lead to more accurate judgments
Bad debt problems and enterprise restructuring in eastern Germany
No full textThe bad debt problem of enterprises in Central and Eastern Europe (CEE) has received much attention in the recent literature about the reform process in these countries. The study begins by looking at the restructuring process and the opening balance sheets of enterprises in East Germany. We then compare the debt level and the liability structure of West and East German firms. Next, we examine what happened with enterprise debt when the monetary union of East and West Germany was implemented in July 1990. After that we look at working capital loans and the restitution problem, loan business, foundation of new enterprises and the bankruptcy law in eastern Germany. Finally, we draw some conclusions and briefly consider their application to the restructuring process in Hungary, Poland and Czechoslovakia. -from Author</p
Local search performance guarantees for restricted related parallel machine scheduling
No full textWe consider the problem of minimizing the makespan on restricted related parallel machines. In restricted machine scheduling each job is only allowed to be scheduled on a subset of machines. We study the worst-case behavior of local search algorithms. In particular, we analyze the quality of local optima with respect to the jump, swap, push and lexicographical jump neighborhood.operations research and management science;
Development of a Soft Robotics Module for Active Control of Sitting Comfort
No full textSitting comfort is an important factor for passengers in selecting cars, airlines, etc. This paper proposes a soft robotic module that can be integrated into the seat cushion to provide better comfort experiences to passengers. Building on rapid manufacturing technologies and a data-driven approach, the module can be controlled to sense the applied force and the displacement of the top surface and actuate according to four designed modes. A total of 2 modules were prototyped and integrated into a seat cushion, and 16 subjects were invited to test the module’s effectiveness. Experiments proved the principle by showing significant differences regarding (dis)comfort. It was concluded that the proposed soft robotics module could provide passengers with better comfort experiences by adjusting the pressure distribution of the seat as well as introducing a variation of postures relevant for prolonged sitting.Technical SupportEmerging MaterialsMaterials and ManufacturingMechatronic Desig
To The Graduate School:
No full textce Foundation under Grant No. CCR-9985239. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author and do not necessarily reflect the views of the National Science Foundation. Among the online resources I used are Google TM , CiteSeer, and LEO. I would like to thank everyone there for making their services available freely. Thorsten Altenkirch willingly answered my questions about [GHA01]. Natarajan Shankar provided me with some of his PVS files developed for [Sha96]. The L T E X template this thesis is based on was written by Thomas B ohne. I also want to thank him for proof-reading my thesis. Any remaining errors are of course my fault. Last but not least I would like to thank my parents Klaus and Frauke Weber for their great support over many, many years. v vi Contents List of Figures ix 1 Introduction 1 1.1 Objectives . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . . 2 1.2 Organization . . . . . . .
First detection of VHE gamma-ray emission from TXS 1515-273, study of its X-ray variability and spectral energy distribution
No full textArtículo firmado por 197 autores. © 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society. We 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, MPG, and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish Ministerio de Ciencia e Innovacion (MICINN) (FPA201787859-P, FPA2017-85668-P, FPA2017-82729-C6-5-R, FPA201790566-REDC, PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-105510GB-C31, PID2019-107847RB-C41, PID2019107847RB-C42, PID2019-107847RB-C44, PID2019-107988GBC22); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1268/16.12.2019 and the Academy of Finland grant nr. 317637 and 320045 are gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia `Severo Ochoa' SEV-20160588, SEV-2017-0709 and CEX2019-000920-S, and `Maria de Maeztu' CEX2019-000918-M, the Unidad de Excelencia `Maria de Maeztu' MDM-2015-0509-18-2 and the `la Caixa' Foundation (fellowshipLCF/BQ/PI18/11630012), 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, theCommissariat `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. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase from the following agencies is also gratefully acknowledged: the Istituto Nazionale di Astrofisica in Italy and the Centre National d'Etudes Spatiales in France.; This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC. This research has made use of data from the MOJAVE data base that is maintained by the MOJAVE team (Lister et al. 2018).We report here on the first multiwavelength (MWL) campaign on the blazar TXS 1515-273, undertaken in 2019 and extending from radio to very-high-energy gamma-rays (VFW). Up until now, this blazar had not been the subject of any detailed MWL observations. It has a rather hard photon index at GeV energies and was considered a candidate extreme high-synchrotron-peaked source. MAGIC observations resulted in the first-time detection of the source in VHE with a statistical significance of 7.6 sigma. The average integral VHE flux of the source is 6 +/- 1 per cent of the Crab nebula flux above 400 GeV. X-ray coverage was provided by Swift-XRT, XMM-Newton, and NuSTAR. The long continuous X-ray observations were separated by similar to 9 h, both showing clear hour scale flares. In the XMM-Newton data, both the rise and decay time-scales are longer in the soft X-ray than in the hard X-ray band, indicating the presence of a particle cooling regime. The X-ray variability time-scales were used to constrain the size of the emission region and the strength of the magnetic field. The data allowed us to determine the synchrotron peak frequency and classify the source as a flaring high, but not extreme synchrotron-peaked object. Considering the constraints and variability patterns from the X-ray data, we model the broad-band spectral energy distribution. We applied a simple one-zone model, which could not reproduce the radio emission and the shape of the optical emission, and a two-component leptonic model with two interacting components, enabling us to reproduce the emission from radio to VHE band.Ministerio de Ciencia e Innovación (MICINN)Centro de Excelencia Severo OchoaCentro de Excelencia María de MaeztuGerman BMBF Federal Ministry of Education & ResearchGerman MPGItalian INFN Istituto Nazionale di Fisica NucleareItalian INAF Istituto Nazionale AstrofisicaSwiss National Fund SNF Swiss National Science Foundation (SNSF)ERDF under the Spanish Ministerio de Ciencia e Innovación (MICINN)Indian Department of Atomic EnergyJapanese ICRRJapanese University of TokyoJapanese JSPS Ministry of Education, Culture, Sports, Science and TechnologyJapanese MEXT Ministry of Education, Culture, Sports, Science and TechnologyBulgarian Ministry of Education and Science, National RI Roadmap ProjectAcademy of Finland European CommissionFoundation La Caixa FoundationCroatian Science Foundation (HrZZ) ProjectUniversity of RijekaDFG Collaborative Research Centers German Research Foundation (DFG)Polish National Research CentreBrazilian MCTICBrazilian CNPq Conselho Nacional de Desenvolvimento Cientifico e TecnologicoBrazilian FAPERJDepto. de Estructura de la Materia, Física Térmica y ElectrónicaFac. de Ciencias FísicasTRUEpu
An intermittent extreme BL Lac: MWL study of 1ES 2344+514 in an enhanced state
No full text© 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society. Artículo firmado por 214 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 (FPA2017-87859-P, FPA2017-85668-P, FPA2017-82729-C6-2-R, FPA2017-82729-C6-6-R, FPA2017-82729-C6-5R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2017-87055-C2-2-P, and 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 no. 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. The FACT collaboration acknowledges the important contributions from ETH Zurich grants ETH-10.08-2 and ETH-27.12-1 as well as the funding by the Swiss SNF and the German BMBF (Verbundforschung Astro-und Astroteilchenphysik) and HAP (Helmoltz Alliance for Astroparticle Physics) are gratefully acknowledged. Part of this work is supported by Deutsche Forschungsgemeinschaft (DFG) within the Collaborative Research Center SFB 876 'Providing Information by ResourceConstrained Analysis', project C3. We are thankful for the very valuable contributions from E. Lorenz, D. Renker and G. Viertel during the early phase of the project. We thank the Instituto de Astrof ' isica de Canarias for allowing us to operate the telescope at the Observatorio del Roque de los Muchachos in La Palma, the Max-Planck-Institut fur Physik for providing us with the mount of the former HEGRA CT3 telescope, and the MAGIC collaboration for their support. This article is based partly on observations made with the 1.5 TCS and IAC80 telescopes operated by the IAC in the Spanish Observatorio del Teide. This article is also based partly on data obtained with the STELLA robotic telescopes in Tenerife, an AIP facility jointly operated by AIP and IAC. We acknowledge support from Russian Scientific Foundation grant 17-12-01029. AVF and WZ are grateful for support from NASA grant NNX12AF12G, the Christopher R. Redlich Fund, the TABASGO Foundation, and the Miller Institute for Basic Research in Science (U.C. Berkeley). KAIT and its ongoing operation were made possible by donations from Sun Microsystems, Inc., the HewlettPackard Company, AutoScope Corporation, Lick Observatory, the US National Science Foundation, the University of California, the Sylvia and Jim Katzman Foundation, and the TABASGO Foundation. Research at Lick Observatory is partially supported by a generous gift from Google.; WM acknowledges support from CONICYT project Basal AFB-170002. The OVRO 40-m monitoring program is supported in part by NASA grants NNX08AW31G, NNX11A043G, and NNX14AQ89G, and NSF grants AST-0808050 and AST-1109911. This research has made use of data and/or software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. We acknowledge the use of public data from the Swift data archive. This research has made use the TeVCat online source catalog (http://tevcat.uchicago.edu).Part of this work is based on archival data, software or online services provided by the Space Science Data Center -ASI.Extreme high-frequency BL Lacs (EHBL) feature their synchrotron peak of the broad-band spectral energy distribution (SED) at nu(s) >= 10(17) Hz. The BL Lac object 1ES 2344+514 was included in the EHBL family because of its impressive shift of the synchrotron peak in 1996. During the following years, the source appeared to be in a low state without showing any extreme behaviours. In 2016 August, 1ES 2344+514 was detected with the groundbased gamma-ray telescope FACT during a high gamma-ray state, triggering multiwavelength (MWL) observations. We studied the MWL light curves of 1ES 2344+514 during the 2016 flaring state, using data from radio to very-high-energy (VHE) gamma-rays taken with OVRO, KAIT, KVA, NOT, some telescopes of the GASP-WEBT collaboration at the Teide, Crimean, and St. Petersburg observatories, Swift-UVOT, Swift-XRT, Fermi-LAT, FACT, and MAGIC. With simultaneous observations of the flare, we built the broad-band SED and studied it in the framework of a leptonic and a hadronic model. The VHE gamma-ray observations show a flux level of 55 per cent of the Crab Nebula flux above 300 GeV, similar to the historical maximum of 1995. The combination of MAGIC and Fermi-LAT spectra provides an unprecedented characterization of the inverse-Compton peak for this object during a flaring episode. The Gamma index of the intrinsic spectrum in the VHE gamma-ray band is 2.04 +/- 0.12(stat) +/- 0.15(sys). We find the source in an extreme state with a shift of the position of the synchrotron peak to frequencies above or equal to 1018 Hz.Ministerio de Economía y Competitividad (MINECO)/FEDERCentro de Excelencia Severo OchoaCentro de Excelencia María de MaeztuGerman BMBF Federal Ministry of Education & ResearchGerman MPGItalian INFN Istituto Nazionale di Fisica NucleareItalian INAF Istituto Nazionale AstrofisicaSwiss National Fund SNFIndian Department of Atomic EnergyJapanese JSPS Ministry of Education, Culture, Sports, Science and TechnologyMEXT Ministry of Education, Culture, Sports, Science and Technology, JapanBulgarian Ministry of Education and Science, National RI Roadmap ProjectAcademy of FinlandCroatian Science Foundation (HrZZ)University of RijekaDFG Collaborative Research Centers German Research FoundationPolish National Research CentreBrazilian MCTICBrazilian CNPq National Council for Scientific and Technological DevelopmentBrazilian FAPERJETH ZurichSwiss SNF Swiss National Science FoundationGerman BMBF (Verbundforschung Astro-und Astroteilchenphysik) Federal Ministry of Education & ResearchHAP (Helmoltz Alliance for Astroparticle Physics)Deutsche Forschungsgemeinschaft (DFG) within the Collaborative Research CenterRussian Scientific Foundation (RSF)NASA National Aeronautics & Space AdministrationChristopher R. Redlich FundTABASGO FoundationMiller Institute for Basic Research in Science (U.C. Berkeley)CONICYT project BasalNSF National Science FoundationDepto. de Estructura de la Materia, Física Térmica y ElectrónicaFac. de Ciencias FísicasTRUEpu
Observation of the Gamma-Ray Binary HESS J0632+057 with the HESS, MAGIC, and VERITAS Telescopes
No full text© 2021. The Author(s). Published by the American Astronomical Society. Artículo firmado por 412 autores. The support of the Namibian authorities and of the University of Namibia in facilitating the construction and operation of H.E.S.S. is gratefully acknowledged, as is the support by the German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG), the Helmholtz Association, the Alexander von Humboldt Foundation, the French Ministry of Higher Education, Research and Innovation, the Centre National de la Recherche Scientifique (CNRS/IN2P3 and CNRS/INSU), the Commissariat a l'energie atomique et aux energies alternatives (CEA), the U.K. Science and Technology Facilities Council (STFC), the Knut and Alice Wallenberg Foundation, the National Science Centre, Poland grant no. 2016/22/M/ST9/00382, the South African Department of Science and Technology and National Research Foundation, the University of Namibia, the National Commission on Research, Science & Technology of Namibia (NCRST), the Austrian Federal Ministry of Education, Science and Research and the Austrian Science Fund (FWF), the Australian Research Council (ARC), the Japan Society for the Promotion of Science, and the University of Amsterdam. We appreciate the excellent work of the technical support staff in Berlin, Zeuthen, Heidelberg, Palaiseau, Paris, Saclay, Tubingen, and Namibia in the construction and operation of the equipment. This work benefited from services provided by the H.E.S.S. Virtual Organisation, supported by the national resource providers of the EGI Federation.; The MAGIC collaboration 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, MPG and HGF; the Italian INFN and INAF; the Swiss National Fund SNF; the ERDF under the Spanish Ministerio de Ciencia e Innovación (MICINN) (PID2019-104114RB-C31, PID2019-104114RB-C32, PID2019-104114RB-C33, PID2019-105510GB-C31,PID2019-107847RB-C41, PID2019-107847RB-C42, PID2019-107988GB-C22); the Indian Department of Atomic Energy; the Japanese ICRR, the University of Tokyo, JSPS, and MEXT; the Bulgarian Ministry of Education and Science, National RI Roadmap Project DO1-268/16.12.2019 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, CEX2019-000920-S), the Unidad de Excelencia "María de Maeztu" (CEX2019-000918-M, MDM-2015-0509-18-2), and the CERCA program of the Generalitat de Catalunya; 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.; VERITAS is supported by grants from the U.S. Department of Energy Office of Science, the U.S. National Science Foundation and the Smithsonian Institution, by NSERC in Canada, and by the Helmholtz Association in Germany. We acknowledge the excellent work of the technical support staff at the Fred Lawrence Whipple Observatory and at the collaborating institutions in the construction and operation of the instrument. 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 resources of the National Energy Research Scientific Computing Center (NERSC), a U.S. Department of Energy Office of Science User Facility operated under Contract No. DE-AC02-05CH11231.; D.F.T. acknowledges support by grants PGC2018-095512-B-I00, SGR2017-1383, and AYA2017-92402-EXP.; This research has made use of data obtained from the Chandra Data Archive and the Chandra Source Catalog; it has made use of data obtained from the Suzaku satellite, a collaborative mission between the space agencies of Japan (JAXA) and the USA (NASA); it is based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA; it made use of data from the NuSTAR mission, a project led by the California Institute of Technology, managed by the Jet Propulsion Laboratory, and funded by the NASA.The results of gamma-ray observations of the binary system HESS J0632 + 057 collected during 450 hr over 15 yr, between 2004 and 2019, are presented. Data taken with the atmospheric Cherenkov telescopes H.E.S.S., MAGIC, and VERITAS at energies above 350 GeV were used together with observations at X-ray energies obtained with Swift-XRT, Chandra, XMM-Newton, NuSTAR, and Suzaku. Some of these observations were accompanied by measurements of the H alpha emission line. A significant detection of the modulation of the very high-energy gamma-ray fluxes with a period of 316.7 +/- 4.4 days is reported, consistent with the period of 317.3 +/- 0.7 days obtained with a refined analysis of X-ray data. The analysis of data from four orbital cycles with dense observational coverage reveals short-timescale variability, with flux-decay timescales of less than 20 days at very high energies. Flux variations observed over a timescale of several years indicate orbit-to-orbit variability. The analysis confirms the previously reported correlation of X-ray and gamma-ray emission from the system at very high significance, but cannot find any correlation of optical H alpha parameters with fluxes at X-ray or gamma-ray energies in simultaneous observations. The key finding is that the emission of HESS J0632 + 057 in the X-ray and gamma-ray energy bands is highly variable on different timescales. The ratio of gamma-ray to X-ray flux shows the equality or even dominance of the gamma-ray energy range. This wealth of new data is interpreted taking into account the insufficient knowledge of the ephemeris of the system, and discussed in the context of results reported on other gamma-ray binary systems.Ministerio de Ciencia e Innovación (MICINN)/FEDERMinisterio de Ciencia e Innovación (MICINN)Centro de Excelencia Severo OchoaUnidad de Excelencia María de MaeztuGerman Ministry for Education and Research (BMBF) Federal Ministry of Education & Research (BMBF)Max Planck Society Foundation CELLEXGerman Research Foundation (DFG)Helmholtz AssociationAlexander von Humboldt FoundationFrench Ministry of Higher Education, Research and InnovationCentre National de la Recherche Scientifique (CNRS/IN2P3)Centre National de la Recherche Scientifique (CNRS/INSU)Commissariat a l'energie atomique et aux energies alternatives (CEA) French Atomic Energy CommissionU.K. Science and Technology Facilities Council (STFC)Knut and Alice Wallenberg FoundationNational Science Centre, PolandSouth African Department of Science and TechnologyNational Research FoundationNational Commission on Research, Science & Technology of Namibia (NCRST)Austrian Federal Ministry of Education, Science and ResearchAustrian Science Fund (FWF)Australian Research Council (ARC)Australian Research Council (ARC)Japan Society for the Promotion of Science Ministry of Education, Culture, Sports, Science and Technology, Japan (MEXT)University of AmsterdamGerman BMBF Federal Ministry of Education & ResearchGerman HGFItalian 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 EnergyJapanese ICRRJapanese University of TokyoJapanese JSPS Ministry of Education, Culture, Sports, Science and TechnologyJapanese MEXT Ministry of Education, Culture, Sports, Science and TechnologyBulgarian Ministry of Education and Science, National RI Roadmap ProjectAcademy of Finland European CommissionCERCA program of the Generalitat de CatalunyaCroatian Science Foundation (HrZZ) ProjectUniversity of Rijeka ProjectDFG Collaborative Research Centers German Research Foundation (DFG)Polish National Research Centre grantBrazilian MCTICBrazilian CNPq Conselho Nacional de Desenvolvimento Cientifico e TecnologicoBrazilian FAPERJU.S. Department of Energy Office of Science United States Department of Energy (DOE)U.S. National Science FoundationSmithsonian InstitutionNSERC in Canada Natural Sciences and Engineering Research Council of Canada (NSERC)Helmholtz Association in GermanyNational Science FoundationU.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 FacilityESA Member States European Space AgencyNASA National Aeronautics & Space AdministrationDepto. de Estructura de la Materia, Física Térmica y ElectrónicaFac. de Ciencias FísicasTRUEpu
