Astroparticle Physics最新文献

{"title":"A novel energy reconstruction method for the MAGIC stereoscopic observation","authors":"Kazuma Ishio ,&nbsp;David Paneque","doi":"10.1016/j.astropartphys.2024.102937","DOIUrl":"https://doi.org/10.1016/j.astropartphys.2024.102937","url":null,"abstract":"<div><p>We report the successful development of a novel methodology of energy reconstruction for very high energy gamma rays detected with Imaging Atmospheric Cherenkov Telescopes (IACTs). This methodology, based on the machine learning algorithm Random Forest, and named RF-Erec, has been adjusted for being used with data from the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) stereo telescope system, which is a worldwide leading instrument for gamma-ray astronomy in the energy range from about 20<!--> <!-->GeV to beyond 100<!--> <!-->TeV.</p><p>The RF-Erec has been evaluated using different realistic scenarios with Monte Carlo simulated data and real observations from the Crab Nebula (the standard candle for the VHE gamma-ray community). This new methodology has been validated by the MAGIC software board, and it is implemented and ready-to-use in the MAGIC Analysis and Reconstruction Software (MARS). This new methodology, validated by the MAGIC software board, has been implemented and is ready for use in the MAGIC Analysis and Reconstruction Software (MARS). We demonstrate that, in comparison to the previous energy reconstruction methodology for MAGIC data, which relied on Look-Up-Tables (LUTs- Erec) and has been utilized in over 100 scientific publications over the last decade, RF-Erec significantly enhances the energy reconstruction of gamma rays. This improvement extends the capabilities of the MAGIC telescopes.</p><p>Specifically, when quantifying the energy resolution with the width of a Gaussian fitted to the error distribution (<em>resolution-</em><span><math><mi>σ</mi></math></span>), the RF-Erec energy resolution-<span><math><mi>σ</mi></math></span> is 20% at 100 GeV and 11% above 1 TeV for Zenith distances (Zd) below 35 degrees, while it is 20% at 1<!--> <!-->TeV and 13% above 10<!--> <!-->TeV for Zd above 55 degrees. For a wide range of the observable energies, the improvement of energy resolution-<span><math><mi>σ</mi></math></span>, compared to LUTs-Erec, reaches roughly a factor of two, and the improvement is even larger for high Zd observations. Differently to many other works in the literature, our evaluation also considers the energy dispersion and the actual energy migration of events, where RF-Erec improves the performance of LUTs-Erec by factors of a few. The manuscript also demonstrates the importance of energy reconstruction methods with a small energy migration in order to prevent the appearance of artificial spectral features. These artifacts are particularly important at the high end of the gamma-ray spectra, where a few extra high-energy photons could have dramatic consequences for studies related to the EBL attenuation, Lorentz invariance violation, or searches for Axion-like-particles.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102937"},"PeriodicalIF":3.5,"publicationDate":"2024-02-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139907967","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"The expected potential of hadronic PeVatron searches with spectral γ-ray data from the Southern Wide-field Gamma-ray Observatory","authors":"Ekrem Oğuzhan Angüner ,&nbsp;Tülün Ergin","doi":"10.1016/j.astropartphys.2024.102936","DOIUrl":"10.1016/j.astropartphys.2024.102936","url":null,"abstract":"<div><p>The presence of a spectral softening, occurring at <span><math><mo>∼</mo></math></span>3 PeV energies, seen in the local cosmic-ray energy spectrum provides an evidence that our Galaxy hosts astrophysical objects, known as ’hadronic PeVatrons’, that are capable of accelerating hadrons to PeV energies and above. Recent results from ground-based particle detector array experiments have provided conclusive evidence that these facilities are essential to explore the ultra-high-energy (UHE, E<span><math><mrow><mo>&gt;</mo><mn>100</mn></mrow></math></span> TeV) <span><math><mi>γ</mi></math></span>-ray domain and pinpoint the location of PeVatrons in the Galaxy. The Southern Wide-field Gamma-ray Observatory (SWGO) is proposed next-generation ground-based extensive air shower observatory planned for construction in the Southern Hemisphere, which holds great scientific potential for UHE observations. In this study, we investigate the expected potential of SWGO to search for hadronic PeVatrons, based on the publicly available preliminary SWGO straw-man instrument response functions (IRFs). By using these straw-man IRFs, it can be shown that the SWGO detection of <span><math><mi>γ</mi></math></span>-ray spectral cutoffs between 30 TeV and 100 TeV, at a 95% confidence level, is possible for faint <span><math><mi>γ</mi></math></span>-ray sources of <span><math><mo>∼</mo></math></span>5 mCrab given that the spectral index is hard (<span><math><mrow><mi>Γ</mi><mo>≲</mo></mrow></math></span> 2.0), while spectral cutoffs from softer sources with <span><math><mrow><mi>Γ</mi><mo>≅</mo></mrow></math></span>2.3 can be detected for sources brighter than <span><math><mrow><mo>∼</mo><mn>11</mn><mo>−</mo></mrow></math></span>12 mCrab. The reconstructed SWGO PeVatron detection maps demonstrate that the future SWGO experiment can probe large parts of the investigated PeVatron parameter space, providing a robust detection and/or rejection of presence of spectral signatures associated with hadronic PeVatrons. A dedicated study on the promising Southern-sky PeVatron candidates, the Galactic Center region, Westerlund 1, HESS J1702<span><math><mo>−</mo></math></span>420 and HESS J1641<span><math><mo>−</mo></math></span>463, shows that the SWGO will have a great potential to confirm or exclude PeVatron nature of these candidate sources at a robust significance level after 5-years of observation. In addition, it is shown that controlling systematic errors will be necessary to reach full potential of the SWGO experiment for PeVatron searches.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102936"},"PeriodicalIF":3.5,"publicationDate":"2024-02-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139678316","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Neutron-star measurements in the multi-messenger Era","authors":"Stefano Ascenzi ,&nbsp;Vanessa Graber ,&nbsp;Nanda Rea","doi":"10.1016/j.astropartphys.2024.102935","DOIUrl":"10.1016/j.astropartphys.2024.102935","url":null,"abstract":"<div><p>Neutron stars are compact and dense celestial objects that offer the unique opportunity to explore matter and its interactions under conditions that cannot be reproduced elsewhere in the Universe. Their extreme gravitational, rotational and magnetic energy reservoirs fuel the large variety of their emission, which encompasses all available multi-messenger tracers: electromagnetic and gravitational waves, neutrinos, and cosmic rays. However, accurately measuring global neutron-star properties such as mass, radius, and moment of inertia poses significant challenges. Probing internal characteristics such as the crustal composition or superfluid physics is even more complex. This article provides a comprehensive review of the different methods employed to measure neutron-star characteristics and the level of reliance on theoretical models. Understanding these measurement techniques is crucial for advancing our knowledge of neutron-star physics. We also highlight the importance of employing independent methods and adopting a multi-messenger approach to gather complementary data from various observable phenomena as exemplified by the recent breakthroughs in gravitational-wave astronomy and the landmark detection of a binary neutron-star merger. Consolidating the current state of knowledge on neutron-star measurements will enable an accurate interpretation of the current data and errors, and better planning for future observations and experiments.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102935"},"PeriodicalIF":3.5,"publicationDate":"2024-02-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139662763","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Adaptive kernel density estimation for improved sky map computation in gamma-ray astronomy","authors":"M. Holler,&nbsp;T. Mitterdorfer,&nbsp;S. Panny","doi":"10.1016/j.astropartphys.2024.102934","DOIUrl":"10.1016/j.astropartphys.2024.102934","url":null,"abstract":"<div><p>We introduce an alternative method for the calculation of sky maps from data taken with gamma-ray telescopes. In contrast to the established method of smoothing the 2D histogram of reconstructed event directions with a static kernel, we apply a Kernel Density Estimation (KDE) where the kernel size of each gamma-ray candidate is related to its estimated direction uncertainty. Exploiting this additional information implies a gain in resulting image quality, which is validated using both simulations and data. For the tested simulation and analysis configuration, the achieved improvement can only be matched with the classical approach by removing events with lower reconstruction quality, reducing the data set by a considerable amount.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102934"},"PeriodicalIF":3.5,"publicationDate":"2024-02-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0927650524000112/pdfft?md5=a177a043ba4e7016e034a0aa302bd60a&pid=1-s2.0-S0927650524000112-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139662761","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Exploring one giga electronvolt cosmic gamma rays with a Cherenkov plenoscope capable of recording atmospheric light fields, Part 1: Optics","authors":"Sebastian Achim Mueller ,&nbsp;Spyridon Daglas ,&nbsp;Axel Arbet Engels ,&nbsp;Max Ludwig Ahnen ,&nbsp;Dominik Neise ,&nbsp;Adrian Egger ,&nbsp;Eleni Chatzi ,&nbsp;Adrian Biland ,&nbsp;Werner Hofmann","doi":"10.1016/j.astropartphys.2024.102933","DOIUrl":"10.1016/j.astropartphys.2024.102933","url":null,"abstract":"<div><p>Detecting cosmic gamma rays at high rates is the key to time-resolve the acceleration of particles within some of the most powerful events in the universe. Time-resolving the emission of gamma rays from merging celestial bodies, apparently random bursts of gamma rays, recurring novas in binary systems, flaring jets from active galactic nuclei, clocking pulsars, and many more became a critical contribution to astronomy. For good timing on account of high rates, we would ideally collect the naturally more abundant, low energetic gamma rays in the domain of one giga electronvolt in large areas. Satellites detect low energetic gamma rays but only in small collecting areas. Cherenkov telescopes have large collecting areas but can only detect the rare, high energetic gamma rays. To detect gamma rays with lower energies, Cherenkov-telescopes need to increase in precision and size. But when we push the concept of the –far/tele– seeing Cherenkov telescope accordingly, the telescope’s physical limits show more clearly. The narrower depth-of-field of larger mirrors, the aberrations of mirrors, and the deformations of mirrors and mechanics all blur the telescope’s image. To overcome these limits, we propose to record the –full/plenum– Cherenkov-light field of an atmospheric shower, i.e. recording the directions and impacts of each individual Cherenkov photon simultaneously, with a novel class of instrument. This novel Cherenkov plenoscope can turn a narrow depth-of-field into the perception of depth, can compensate aberrations, and can tolerate deformations. We design a Cherenkov plenoscope to explore timing by detecting low energetic gamma rays in large areas.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"158 ","pages":"Article 102933"},"PeriodicalIF":3.5,"publicationDate":"2024-01-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0927650524000100/pdfft?md5=ec6ab2fc414cb49a2e28c4074cfd3544&pid=1-s2.0-S0927650524000100-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139645215","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Inflection point of coupled quintessence","authors":"Jaskirat Kaur ,&nbsp;S.D. Pathak ,&nbsp;Vikash Kumar Ojha ,&nbsp;Maxim Yu Khlopov","doi":"10.1016/j.astropartphys.2024.102926","DOIUrl":"10.1016/j.astropartphys.2024.102926","url":null,"abstract":"<div><p>In this paper, we investigate the behavior of coupled quintessence at inflection point in the accelerated expansion of the universe. We consider spatially homogeneous quintessence coupled with the matter with two coupling parameters as <span><math><mrow><mi>Q</mi><mo>=</mo><mn>3</mn><mi>α</mi><mi>H</mi><msub><mrow><mi>ρ</mi></mrow><mrow><mi>m</mi></mrow></msub></mrow></math></span> and <span><math><mrow><mi>Q</mi><mo>=</mo><mn>3</mn><mi>β</mi><mover><mrow><msub><mrow><mi>ρ</mi></mrow><mrow><mi>m</mi></mrow></msub></mrow><mrow><mo>̇</mo></mrow></mover></mrow></math></span>. We obtain the inflection point for the power law form of potential <span><math><mrow><mi>V</mi><mrow><mo>(</mo><mi>ϕ</mi><mo>)</mo></mrow><mo>=</mo><msub><mrow><mi>V</mi></mrow><mrow><mn>3</mn></mrow></msub><msup><mrow><mrow><mo>(</mo><mi>ϕ</mi><mo>−</mo><msub><mrow><mi>ϕ</mi></mrow><mrow><mn>0</mn></mrow></msub><mo>)</mo></mrow></mrow><mrow><mn>3</mn></mrow></msup></mrow></math></span> and its generalized form in two coupled quintessence models.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"157 ","pages":"Article 102926"},"PeriodicalIF":3.5,"publicationDate":"2024-01-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139462589","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Non-oscillating early dark energy and quintessence from α-attractors","authors":"Lucy Brissenden,&nbsp;Konstantinos Dimopoulos,&nbsp;Samuel Sánchez López","doi":"10.1016/j.astropartphys.2024.102925","DOIUrl":"10.1016/j.astropartphys.2024.102925","url":null,"abstract":"<div><p>Early dark energy (EDE) is one of the most promising possibilities in order to resolve the Hubble tension: the discrepancy between the locally measured and cosmologically inferred values of the Hubble constant. In this paper we propose a toy model of unified EDE and late dark energy (DE), driven by a scalar field in the context of <span><math><mi>α</mi></math></span>-attractors. The field provides an injection of a subdominant dark energy component near matter-radiation equality, and redshifts away shortly after via free-fall, later refreezing to become late-time DE at the present day. Using reasonable estimates of the current constraints on EDE from the literature, we find that the parameter space is narrow but viable, making our model readily falsifiable. Since our model is non-oscillatory, the density of the field decays faster than the usual oscillatory EDE, thereby possibly achieving better agreement with observations.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"157 ","pages":"Article 102925"},"PeriodicalIF":3.5,"publicationDate":"2024-01-05","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://www.sciencedirect.com/science/article/pii/S0927650524000021/pdfft?md5=b58f8add097d0e5e61191c47f6ebd75a&pid=1-s2.0-S0927650524000021-main.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139103673","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"OA","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Energy spectra of the first TGE observed on Zugspitze by the SEVAN light detector compared with the energetic TGE observed on Aragats","authors":"A. Chilingarian ,&nbsp;T. Karapetyan ,&nbsp;B. Sargsyan ,&nbsp;J. Knapp ,&nbsp;M. Walter ,&nbsp;T. Rehm","doi":"10.1016/j.astropartphys.2024.102924","DOIUrl":"10.1016/j.astropartphys.2024.102924","url":null,"abstract":"<div><p><span>The energy spectra<span> of Thunderstorm ground enhancement (TGE) electrons and gamma rays are the key evidence for proving the origin of enhanced </span></span>particle fluxes<span> from thunderclouds. Till now, the electron energy spectrum was measured only by the Aragats large scintillation spectrometer ASNT. We changed the electronics board of the SEVAN detector installed at the Umwelt-Forschungs-Station (UFS, Schneefernerhaus, 2650 m asl) to allow these vital measurements near the top of the Zugspitze. The new electronics of the SEVAN detector, supplied with logarithmic ADC, for the energy release measurements up to 50 MeV (the thickness of the spectrometric scintillator is 25 cm). Thus, by measuring energy releases well above 3 MeV, we unambiguously separate Radon progeny gamma radiation from the electrons and gamma-ray relativistic runaway avalanches. Using the different energy release histograms allows for separating charged and neutral particles, enabling the disentangling of electron and gamma-ray energy spectra. On May 23, 2023, the first TGE was registered on Zugspitze by the SEVAN detector. The gamma-ray flux enhancement was 44%, corresponding to the observed count rate peak enhancement of 44σ. The gamma-ray energy spectrum was recovered, maximum energy is 60 MeV. On the same day, a large TGE was observed on Aragats. The TGE maximum flux overpasses the fair-weather flux by 207%, equivalent to a 1-minute peak significance of 400σ. Maximum energy of electrons is 50 MeV, gamma rays – 45 MeV. In this context, we will explore and explain the new capabilities of the SEVAN detector installed on Zugspitze and the rearranged similar detector on Aragats. We also present and compare electron and gamma-ray energy spectra from Aragats TGE and gamma-ray energy spectrum from Zugspitze.</span></p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"156 ","pages":"Article 102924"},"PeriodicalIF":3.5,"publicationDate":"2024-01-03","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139083150","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Proof of principle for template synthesis approach for the radio emission from vertical extensive air showers","authors":"Mitja Desmet ,&nbsp;Stijn Buitink ,&nbsp;Tim Huege ,&nbsp;David Butler ,&nbsp;Ralph Engel ,&nbsp;Olaf Scholten","doi":"10.1016/j.astropartphys.2023.102923","DOIUrl":"10.1016/j.astropartphys.2023.102923","url":null,"abstract":"<div><p><span>The radio detection technique of cosmic ray air showers has gained renewed interest in the last two decades. While the radio experiments are very cost-effective to deploy, the Monte-Carlo simulations required to analyse the data are computationally expensive. Here we present a proof of concept for a novel way to synthesise the radio emission from extensive air showers in simulations. It is a hybrid approach which uses a single microscopic Monte-Carlo simulation, called the origin shower, to generate the radio emission from a target shower with a different longitudinal evolution, primary particle type and energy. The method employs semi-analytical relations which only depend on the shower parameters to transform the radio signals in the simulated antennas. We apply this method to vertical air showers with energies ranging from </span><span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>17</mn></mrow></msup><mspace></mspace><mtext>eV</mtext></mrow></math></span> to <span><math><mrow><mn>1</mn><msup><mrow><mn>0</mn></mrow><mrow><mn>19</mn></mrow></msup><mspace></mspace><mtext>eV</mtext></mrow></math></span> and compare the results with CoREAS simulations in two frequency bands, namely the broad [20, 500] <span><math><mtext>MHz</mtext></math></span> band and a more narrow one at [30, 80] <span><math><mtext>MHz</mtext></math></span><span>. We gauge the synthesis quality using the maximal amplitude and energy fluence contained in the signal. We observe that the quality depends primarily on the difference in </span><span><math><msub><mrow><mi>X</mi></mrow><mrow><mtext>max</mtext></mrow></msub></math></span> between the origin and target shower. After applying a linear bias correction, we find that for a shift in <span><math><msub><mrow><mi>X</mi></mrow><mrow><mtext>max</mtext></mrow></msub></math></span> of less than 150 <span><math><mrow><mtext>g</mtext><mo>/</mo><msup><mrow><mtext>cm</mtext></mrow><mrow><mn>2</mn></mrow></msup></mrow></math></span>, template synthesis has a bias of less than 2% and a scatter up to 6%, both in amplitude, on the broad frequency range. On the restricted [30, 80] <span><math><mtext>MHz</mtext></math></span> range the bias is similar, but the spread on amplitude drops down to 3%. These fluctuations are on the same level as the intrinsic scatter we observe in Monte-Carlo ensembles. We therefore surmise the observed scatter in amplitude to originate from intrinsic shower fluctuations we do not explicitly account for in template synthesis.</p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"157 ","pages":"Article 102923"},"PeriodicalIF":3.5,"publicationDate":"2023-12-30","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139068039","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}

{"title":"Autonomous observation, control, data acquisition and monitoring of MACE telescope","authors":"Anushri Jain,&nbsp;Shikha Srivastava,&nbsp;Mahesh P․,&nbsp;J. Deshpande,&nbsp;Padmini S․","doi":"10.1016/j.astropartphys.2023.102922","DOIUrl":"10.1016/j.astropartphys.2023.102922","url":null,"abstract":"<div><p>Major Atmospheric Cherenkov Experiment (MACE) is a large telescope commissioned at Ladakh region of India. It consists of many subsystems operating in synchronization<span> to perform successful observations. The paper introduces a robust, concise and autonomous operator console to operate, control and monitor the entire experiment, providing workflow management, autonomous schedule-based observation, orchestration of data acquisition and monitoring of telemetry data, while maintaining safety of subsystems. Using a synchronised controller-observer pattern the highly-automated operator console carries out the entire observation on a single click from either local or from remote geographic locations. Remote operation of the telescope from BARC, Mumbai allowed pre-commissioning tests, troubleshooting and upgradation of the system from a more convenient environment.</span></p></div>","PeriodicalId":55439,"journal":{"name":"Astroparticle Physics","volume":"157 ","pages":"Article 102922"},"PeriodicalIF":3.5,"publicationDate":"2023-12-28","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"139067932","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":3,"RegionCategory":"物理与天体物理","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}