Experimental Astronomy最新文献

{"title":"Pulsar search acceleration using FPGAs and OpenCL templates","authors":"Julian Oppermann,&nbsp;Mitchell B. Mickaliger,&nbsp;Oliver Sinnen","doi":"10.1007/s10686-022-09888-z","DOIUrl":"10.1007/s10686-022-09888-z","url":null,"abstract":"<div><p>The Square Kilometre Array (SKA) is the world’s largest radio telescope currently under construction, and will employ elaborate signal processing to detect new pulsars, i.e. highly magnetised rotating neutron stars. This paper addresses the acceleration of demanding computations for this pulsar search on Field-Programmable Gate Arrays (FPGAs) using a new high-level design process based on OpenCL templates that is transferable to other scientific problems. The successful FPGA acceleration of large-scale scientific workloads requires custom architectures that fully exploit the parallel computing capabilities of modern reconfigurable hardware and are amenable to substantial design space exploration. OpenCL-based high-level synthesis toolchains, with their ability to express interconnected multi-kernel pipelines in a single source language, excel in this domain. However, the achievable performance strongly depends on how well the compiler can infer desirable hardware structures from the code. One key aspect to excellent performance is commonly the uninterrupted, high-bandwidth streaming of data into and through the design. This is difficult to achieve in complex designs when data order needs to be re-arranged, e.g. transposed. It is equally hard to pre-fetch and burst-load from DDR memory when reading occurs in non-trivial patterns. In this paper, we propose new approaches to these two problems that use OpenCL-based code templates.</p><p>We demonstrate the practical benefits of these approaches with the acceleration of a key component in the SKA’s pulsar search pipeline: the Fourier Domain Acceleration Search (FDAS) module. Using our proposed methodology, we are able to develop a more scalable FDAS accelerator architecture than previously possible. We explore its design space to eventually achieve a 10x throughput improvement over a prior, thoroughly optimised implementation in plain OpenCL.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"239 - 266"},"PeriodicalIF":3.0,"publicationDate":"2023-01-23","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09888-z.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4896279","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":"Hadronic interaction model dependence in cosmic Gamma-ray flux estimation using an extensive air shower array with a muon detector","authors":"S. Okukawa,&nbsp;M. Anzorena,&nbsp;S. Asano,&nbsp;C. A. H. Condori,&nbsp;E. de la Fuente,&nbsp;A. Gomi,&nbsp;K. Hibino,&nbsp;N. Hotta,&nbsp;A. Jimenez-Meza,&nbsp;Y. Katayose,&nbsp;C. Kato,&nbsp;S. Kato,&nbsp;T. Kawashima,&nbsp;K. Kawata,&nbsp;T. Koi,&nbsp;H. Kojima,&nbsp;D. Kurashige,&nbsp;J. Lozoya,&nbsp;R. Mayta,&nbsp;P. Miranda,&nbsp;K. Munakata,&nbsp;K. Nagaya,&nbsp;Y. Nakamura,&nbsp;Y. Nakazawa,&nbsp;C. Nina,&nbsp;M. Nishizawa,&nbsp;S. Ogio,&nbsp;M. Ohnishi,&nbsp;A. Oshima,&nbsp;M. Raljevic,&nbsp;H. Rivera,&nbsp;T. Saito,&nbsp;Y. Sakakibara,&nbsp;T. Sako,&nbsp;T. K. Sako,&nbsp;S. Shibata,&nbsp;A. Shiomi,&nbsp;M. Subieta,&nbsp;N. Tajima,&nbsp;W. Takano,&nbsp;M. Takita,&nbsp;Y. Tameda,&nbsp;K. Tanaka,&nbsp;R. Ticona,&nbsp;I. Toledano-Juarez,&nbsp;H. Tsuchiya,&nbsp;Y. Tsunesada,&nbsp;S. Udo,&nbsp;K. Yamazaki,&nbsp;Y. Yokoe","doi":"10.1007/s10686-022-09883-4","DOIUrl":"10.1007/s10686-022-09883-4","url":null,"abstract":"<div><p>Observation techniques of high-energy gamma rays using air showers have remarkably progressed via the Tibet AS<i>γ</i>, HAWC, and LHAASO experiments. These observations have significantly contributed to gamma-ray astronomy in the northern sky’s sub-PeV region. Moreover, in the southern sky, the ALPACA experiment is underway at 4,740 m altitude on the Chacaltaya plateau in Bolivia. This experiment estimates the gamma-ray flux from the difference between the number of on-source and off-source events by real data, utilizing the gamma-ray detection efficiency calculated through Monte Carlo simulations, which in turn depends on the hadronic interaction models. Even though the number of cosmic-ray background events can be experimentally estimated, this model dependence affects the estimation of gamma-ray detection efficiency. However, previous reports have assumed that the model dependence is negligible and have not included it in the error of gamma-ray flux estimation. Using ALPAQUITA, the prototype experiment of ALPACA, we quantitatively evaluated the model dependence on hadronic interaction models for the first time. We evaluate the model dependence on hadronic interactions as less than 3.6 % in the typical gamma-ray flux estimation performed by ALPAQUITA; this is negligible compared with other uncertainties such as energy scale uncertainty in the energy range from 6 to 300 TeV, which is dominated by the Monte Carlo statistics. This upper limit of 3.6 % model dependence is expected to apply to ALPACA.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"55 2","pages":"325 - 342"},"PeriodicalIF":3.0,"publicationDate":"2023-01-17","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4680569","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":"A simulation study for the expected performance of Sharjah-Sat-1 payload improved X-Ray Detector (iXRD) in the orbital background radiation","authors":"Ali M. Altıngün,&nbsp;Emrah Kalemci,&nbsp;Efe Öztaban","doi":"10.1007/s10686-022-09885-2","DOIUrl":"10.1007/s10686-022-09885-2","url":null,"abstract":"<div><p>Sharjah-Sat-1 is a 3U cubesat with a CdZnTe based hard X-ray detector, called iXRD (improved X-ray Detector) as a scientific payload with the primary objective of monitoring bright X-ray sources in the galaxy. We investigated the effects of the in-orbit background radiation on the iXRD based on Geant4 simulations. Several background components were included in the simulations such as the cosmic diffuse gamma-rays, galactic cosmic rays (protons and alpha particles), trapped protons and electrons, and albedo radiation arising from the upper layer of the atmosphere. The most dominant component is the albedo photon radiation which contributes at low and high energies alike in the instrument energy range of 20 keV - 200 keV. On the other hand, the cosmic diffuse gamma-ray contribution is the strongest between 20 keV and 60 keV in which most of the astrophysics source flux is expected. The third effective component is the galactic cosmic protons. The radiation due to the trapped particles, the albedo neutrons, and the cosmic alpha particles are negligible when the polar regions and the South Atlantic Anomaly region are excluded in the analysis. The total background count rates are <span>(sim )</span>0.36 and <span>(sim )</span>0.85 counts/s for the energy bands of 20 - 60 keV and 20 - 200 keV, respectively. We performed charge transportation simulations to determine the spectral response of the iXRD and used it in sensitivity calculations as well. The simulation framework was validated with experimental studies. The estimated sensitivity of 180 mCrab between the energy band of 20 keV - 100 keV indicates that the iXRD could achieve its scientific goals.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"117 - 140"},"PeriodicalIF":3.0,"publicationDate":"2023-01-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09885-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4302679","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":"CATCH: chasing all transients constellation hunters space mission","authors":"Panping Li,&nbsp;Qian-Qing Yin,&nbsp;Zhengwei Li,&nbsp;Lian Tao,&nbsp;Xiangyang Wen,&nbsp;Shuang-Nan Zhang,&nbsp;Liqiang Qi,&nbsp;Juan Zhang,&nbsp;Donghua Zhao,&nbsp;Dalin Li,&nbsp;Xizheng Yu,&nbsp;Qingcui Bu,&nbsp;Wen Chen,&nbsp;Yupeng Chen,&nbsp;Yiming Huang,&nbsp;Yue Huang,&nbsp;Ge Jin,&nbsp;Gang Li,&nbsp;Hongbang Liu,&nbsp;Xiaojing Liu,&nbsp;Ruican Ma,&nbsp;Wenxi Peng,&nbsp;Ruijing Tang,&nbsp;Yusa Wang,&nbsp;Jingyu Xiao,&nbsp;Shaolin Xiong,&nbsp;Sheng Yang,&nbsp;Yanji Yang,&nbsp;Chen Zhang,&nbsp;Tianchong Zhang,&nbsp;Liang Zhang,&nbsp;Xuan Zhang,&nbsp;Haisheng Zhao,&nbsp;Kang Zhao,&nbsp;Qingchang Zhao,&nbsp;Shujie Zhao,&nbsp;Xing Zhou","doi":"10.1007/s10686-022-09879-0","DOIUrl":"10.1007/s10686-022-09879-0","url":null,"abstract":"<div><p>In time-domain astronomy, a substantial number of transients will be discovered by multi-wavelength and multi-messenger observatories, posing a great challenge for follow-up capabilities. We have thus proposed an intelligent X-ray constellation, the Chasing All Transients Constellation Hunters (<i>CATCH</i>) space mission. Consisting of 126 micro-satellites in three types, <i>CATCH</i> will have the capability to perform follow-up observations for a large number of different types of transients simultaneously. Each satellite in the constellation will carry lightweight X-ray optics and use a deployable mast to increase the focal length. The combination of different optics and detector systems enables different types of satellites to have multiform observation capabilities, including timing, spectroscopy, imaging, and polarization. Controlled by the intelligent system, different satellites can cooperate to perform uninterrupted monitoring, all-sky follow-up observations, and scanning observations with a flexible field of view (FOV) and multi-dimensional observations. Therefore, <i>CATCH</i> will be a powerful mission to study the dynamic universe. Here, we present the current design of the spacecraft, optics, detector system, constellation configuration and observing modes, as well as the development plan.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"55 2","pages":"447 - 486"},"PeriodicalIF":3.0,"publicationDate":"2023-01-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09879-0.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4249463","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":"SULIS: A coronal magnetism explorer for ESA’s Voyage 2050","authors":"E. Scullion,&nbsp;H. Morgan,&nbsp;H. Lin,&nbsp;V. Fedun,&nbsp;R. Morton","doi":"10.1007/s10686-022-09877-2","DOIUrl":"10.1007/s10686-022-09877-2","url":null,"abstract":"<div><p>Magnetism dominates the structure and dynamics of the solar corona. To understand the true nature of the solar corona and the long-standing coronal heating problem requires measuring the vector magnetic field of the corona at a sufficiently high resolution (spatially and temporally) across a large Field-of-View (FOV). Despite the importance of the magnetic field in the physics of the corona and despite the tremendous progress made recently in the remote sensing of solar magnetic fields, reliable measurements of the coronal magnetic field strength and orientation do not exist. This is largely due to the weakness of coronal magnetic fields, previously estimated to be on the order of 1-10 G, and the difficulty associated with observing the extremely faint solar corona emission. With the Solar cUbesats for Linked Imaging Spectro-polarimetry (SULIS) mission, we plan to finally observe, in detail and over the long-term, uninterrupted measurements of the coronal magnetic vector field using a new and very affordable instrument design concept. This will be profoundly important in the study of local atmospheric coronal heating processes, as well as in measuring the nature of magnetic clouds, in particular, within geoeffective Earth-bound Coronal Mass Ejections (CMEs) for more accurate forecasting of severe space weather activity.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"54 2-3","pages":"317 - 334"},"PeriodicalIF":3.0,"publicationDate":"2022-12-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09877-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4814665","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":"Modelization of galactic cosmic-ray short-term variations for LISA","authors":"Mattia Villani,&nbsp;Federico Sabbatini,&nbsp;Catia Grimani,&nbsp;Michele Fabi,&nbsp;Andrea Cesarini","doi":"10.1007/s10686-022-09884-3","DOIUrl":"10.1007/s10686-022-09884-3","url":null,"abstract":"<div><p>The European Space Agency Laser Interferometer Space Antenna (LISA) will be the first mission dedicated to the detection of low-frequency gravitational waves in space. Particles of galactic and solar origin above tens of MeV will penetrate the spacecraft and charge the metal free-falling test masses (TMs) playing the role of mirrors of the interferometer. The poissonian fluctuations of the charging process and associated spurious Coulomb forces acting on the TMs limit the sensitivity of LISA mainly below 1 mHz. Moreover, galactic cosmic-ray (GCR) flux short-term variations will modulate differently the TM charging on the three satellites of the LISA constellation. Without a proper GCR flux monitoring, the LISA TM charging estimates will be carried out on the basis of the long-term solar modulation only. In this work we report about models of galactic cosmic-ray short-term variations to investigate to which extent the galactic cosmic-ray depressions can be also used as a proxy of the increase of interplanetary magnetic field and solar wind speed observed at the passage of high-speed solar wind streams and interplanetary coronal mass ejections. Our final aim is to study the optimum characteristics of particle detectors for both TM charging estimate and interplanetary medium monitoring for LISA.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"56 1","pages":"1 - 30"},"PeriodicalIF":3.0,"publicationDate":"2022-12-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4564994","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":"RAPOC: The Rosseland and Planck opacity converter","authors":"Lorenzo V. Mugnai,&nbsp;Darius Modirrousta-Galian","doi":"10.1007/s10686-022-09869-2","DOIUrl":"10.1007/s10686-022-09869-2","url":null,"abstract":"<div><p><span>RAPOC</span> (Rosseland and Planck Opacity Converter) is a Python 3 code that calculates Rosseland and Planck mean opacities (RPMs) from wavelength-dependent opacities for a given temperature, pressure, and wavelength range. In addition to being user-friendly and rapid, <span>RAPOC</span> can interpolate between discrete data points, making it flexible and widely applicable to the astrophysical and Earth-sciences fields, as well as in engineering. <span>RAPOC</span> uses <i>ExoMol</i>, <i>DACE</i>, or any user defined input data, provided that it is in a readable format. In this paper, we present the <span>RAPOC</span> code and compare its calculated Rosseland and Planck mean opacities with other values in the literature. <span>RAPOC</span> is open-source and available on Pypi and GitHub.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"55 2","pages":"521 - 539"},"PeriodicalIF":3.0,"publicationDate":"2022-10-29","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09869-2.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"5639633","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":"Proton irradiation of SiPM arrays for POLAR-2","authors":"Slawomir Mianowski,&nbsp;Nicolas De Angelis,&nbsp;Johannes Hulsman,&nbsp;Merlin Kole,&nbsp;Tomasz Kowalski,&nbsp;Sebastian Kusyk,&nbsp;Hancheng Li,&nbsp;Zuzanna Mianowska,&nbsp;Jerzy Mietelski,&nbsp;Agnieszka Pollo,&nbsp;Dominik Rybka,&nbsp;Jianchao Sun,&nbsp;Jan Swakon,&nbsp;Damian Wrobel,&nbsp;Xin Wu","doi":"10.1007/s10686-022-09873-6","DOIUrl":"10.1007/s10686-022-09873-6","url":null,"abstract":"<div><p>POLAR-2 is a space-borne polarimeter, built to investigate the polarization of Gamma-Ray Bursts and help elucidate their mechanisms. The instrument is targeted for launch in 2024 or 2025 aboard the China Space Station and is being developed by a collaboration between institutes from Switzerland, Germany, Poland and China. The instrument will orbit at altitudes between 340km and 450km with an inclination of <span>({42}{^{circ }})</span> and will be subjected to background radiation from cosmic rays and solar events. It is therefore pertinent to better understand the performance of sensitive devices under space-like conditions. In this paper we focus on the radiation damage of the silicon photomultiplier arrays S13361-6075NE-04 and S14161-6050HS-04 from Hamamatsu. The S13361 are irradiated with 58MeV protons at several doses up to 4.96Gy, whereas the newer series S14161 are irradiated at doses of 0.254Gy and 2.31Gy. Their respective performance degradation due to radiation damage are discussed. The equivalent exposure time in space for silicon photomultipliers inside POLAR-2 with a dose of 4.96Gy is 62.9years (or 1.78years when disregarding the shielding from the instrument). Primary characteristics of the I-V curves are an increase in the dark current and dark counts, mostly through cross-talk events. Annealing processes at <span>({25}{^{circ }C})</span> were observed but not studied in further detail. Biasing channels while being irradiated have not resulted in any significant impact. Activation analyses showed a dominant contribution of <span>(beta ^{+})</span> particles around 511 keV. These resulted primarily from copper and carbon, mostly with decay times shorter than the orbital period.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"55 2","pages":"343 - 371"},"PeriodicalIF":3.0,"publicationDate":"2022-10-25","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09873-6.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4990127","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":"The 100-m X-ray test facility at IHEP","authors":"Yusa Wang,&nbsp;Zijian Zhao,&nbsp;Dongjie Hou,&nbsp;Xiongtao Yang,&nbsp;Can Chen,&nbsp;Xinqiao Li,&nbsp;Yuxuan Zhu,&nbsp;Xiaofan Zhao,&nbsp;Jia Ma,&nbsp;He Xu,&nbsp;Yupeng Chen,&nbsp;Guofeng Wang,&nbsp;Fangjun Lu,&nbsp;Shuangnan Zhang,&nbsp;Shu Zhang,&nbsp;Yong Chen,&nbsp;Yupeng Xu","doi":"10.1007/s10686-022-09872-7","DOIUrl":"10.1007/s10686-022-09872-7","url":null,"abstract":"<div><p>The 100-m X-ray Test Facility of the Institute of High Energy Physics (IHEP) was initially proposed in 2012 for the test and calibration of the X-ray detectors of the Hard X-ray Modulation Telescope (HXMT) with the capability to support future X-ray missions. The large instrument chamber connected with a long vacuum tube can accommodate the X-ray mirror, focal plane detector and other instruments. The X-ray sources are installed at the other end of the vacuum tube with a distance of 105 m, which can provide an almost parallel X-ray beam covering 0.2<span>(sim)</span>60 keV energy band. The X-ray mirror modules of the Einstein Probe (EP) and the enhanced X-ray Timing and Polarimetry mission (eXTP) and payload of the Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) have been tested and calibrated with this facility. It has been also used to characterize the focal plane camera and aluminum filter used on the Einstein Probe. In this paper, we will introduce the overall configuration and capability of the facility, and give a brief introduction of some calibration results performed with this facility.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"55 2","pages":"427 - 445"},"PeriodicalIF":3.0,"publicationDate":"2022-10-22","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-022-09872-7.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4875265","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":"Classical novae with CUBES","authors":"Luca Izzo,&nbsp;Paolo Molaro,&nbsp;Piercarlo Bonifacio,&nbsp;Gabriele Cescutti,&nbsp;Massimo Della Valle,&nbsp;Pierluigi Selvelli","doi":"10.1007/s10686-022-09876-3","DOIUrl":"10.1007/s10686-022-09876-3","url":null,"abstract":"<div><p>Among the main science cases that have motivated the proposal of CUBES, a new high-resolution spectrograph for the Very Large Telescope at the European Southern Observatory, there is the study and the characterisation of the nucleosynthesis of beryllium. Classical novae have been proposed since the ’70s as one of the main factories of lithium in the Galaxy, but this hypothesis has been demonstrated on empirical basis only recently thanks to the direct identification of lithium in V1369 Cen and through the observations of the resonance transition of <span>(^{7})</span>Be II, the <span>(^{7})</span>Li parent, at 313.0 nm in the near-UV range. CUBES is then the ideal instrument to quantify the amount of <span>(^{7})</span>Be and therefore of <span>(^{7})</span>Li produced by the different novae types hosted in the different components of the Milky Way and also in its nearby satellite galaxies. As important by-product of high resolution spectroscopic observations obtained with CUBES, there are the study of the properties of nova ejecta abundances, the shocks evolution in novae and their connection with the high-energy emission observed in these transients, from satellites as Fermi and Swift.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"55 1","pages":"191 - 198"},"PeriodicalIF":3.0,"publicationDate":"2022-10-21","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"4843562","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}