Experimental Astronomy最新文献

{"title":"PLATO’s signal and noise budget","authors":"Anko Börner,&nbsp;Carsten Paproth,&nbsp;Juan Cabrera,&nbsp;Martin Pertenais,&nbsp;Heike Rauer,&nbsp;J. Miguel Mas-Hesse,&nbsp;Isabella Pagano,&nbsp;Jose Lorenzo Alvarez,&nbsp;Anders Erikson,&nbsp;Denis Grießbach,&nbsp;Yves Levillain,&nbsp;Demetrio Magrin,&nbsp;Valery Mogulsky,&nbsp;Sami-Matias Niemi,&nbsp;Thibaut Prod’homme,&nbsp;Sara Regibo,&nbsp;Joris De Ridder,&nbsp;Steve Rockstein,&nbsp;Reza Samadi,&nbsp;Dimitri Serrano-Velarde,&nbsp;Alan Smith,&nbsp;Peter Verhoeve,&nbsp;Dave Walton","doi":"10.1007/s10686-024-09948-6","DOIUrl":"10.1007/s10686-024-09948-6","url":null,"abstract":"<div><p>ESA’s PLATO mission aims the detection and characterization of terrestrial planets around solar-type stars as well as the study of host star properties. The noise-to-signal ratio (NSR) is the main performance parameter of the PLATO instrument, which consists of 24 Normal Cameras and 2 Fast Cameras. In order to justify, verify and breakdown NSR-relevant requirements the software simulator PINE was developed. PINE models the signal pathway from a target star to the digital output of a camera based on physical models and considers the major noise contributors. In this paper, the simulator’s coarse mode is introduced which allows fast performance analyses on instrument level. The added value of PINE is illustrated by exemplary applications.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"58 1","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-06-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09948-6.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141505213","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":"Characterization of the eXTP-LAD collimators","authors":"Zijian Zhao,&nbsp;Tao Luo,&nbsp;Francesco Ceraudo,&nbsp;Marco Feroci,&nbsp;Longhui Li,&nbsp;Jian Wang,&nbsp;Yupeng Xu,&nbsp;Hongwei Liu,&nbsp;Yuxuan Zhu,&nbsp;Yifan Zhang,&nbsp;Dongjie Hou,&nbsp;Xiongtao Yang,&nbsp;Huilin He,&nbsp;Shuang-Nan Zhang,&nbsp;Fangjun Lu,&nbsp;Yusa Wang","doi":"10.1007/s10686-024-09947-7","DOIUrl":"10.1007/s10686-024-09947-7","url":null,"abstract":"<div><p>The enhanced X-ray Timing and Polarimetry mission (eXTP) is a next-generation flagship X-ray astronomy satellite currently in phase-B study. The large Area Detector (LAD) on board eXTP contains 40 modules, each consisting of a set of 4<span>(times )</span>4 large area SDDs and 4<span>(times )</span>4 collimators, and has a designed effective area of 3.0 m<span>(^2)</span> at 8 keV and a Field of View (FoV) of 1<span>(^circ )</span>. To achieve such a large effective area, the collimator’s Open Area Ratio (OAR) should be greater than 70%. In this paper, we introduce the measurement methods used to determine the OAR and the rocking curve (angular response) of the LAD collimator at the 100-m X-ray Test Facility (100XF) of the Institute of High Energy Physics (IHEP) in Beijing, and report the results of the collimators manufactured under different conditions. The measured OARs of the collimators are usually smaller than the theoretical values by a few percent, which is due to the non-uniformity and irregularity of the pores. The measured rocking curves are usually broader than the theoretical triangular curves, and the lower the energy of the incident X-ray the broader the rocking curve. This broadening of the rocking curve is the result of reflection on the inner wall of the pores. Our results also show that increasing the etching time in the manufacturing of the collimators can increase the OARs but does not change significantly the shape of the rocking curves.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-06-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141394360","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":"Spectral and timing calibration of eXTP-SFA engineering model in 100XF","authors":"Yifan Zhang,&nbsp;Wei Li,&nbsp;Laidan Luo,&nbsp;Dongjie Hou,&nbsp;Yuxuan Zhu,&nbsp;Bin Meng,&nbsp;Zijian Zhao,&nbsp;Dong Xie,&nbsp;Xiongtao Yang,&nbsp;Yanji Yang,&nbsp;Yusa Wang,&nbsp;Yupeng Xu","doi":"10.1007/s10686-024-09945-9","DOIUrl":"10.1007/s10686-024-09945-9","url":null,"abstract":"<div><p>The spectroscopy focusing array is one of the four main scientific instruments of the enhanced X-ray Timing and Polarimetry mission, tasked with spectral and timing observation in the energy range 0.5-10 keV. An engineering model of the spectroscopy focusing array with a 4 mirror shells assembly and a focal plane detector using commercial detectors has now been developed. To evaluate the performance, the spectral and timing calibration of the engineering model has been held in the 100-m X-ray Test Facility. A multi-target X-ray source with multiple emission lines is used to calibrate the spectral performance. A timing X-ray source based on a grid controlled X-ray tube has been utilized for the timing calibration. The timing X-ray source can generate X-ray pulses to measure the response time distribution, and can also simulate the pulsar lightcurves to examine the detection ability for pulsars. The energy-channel relation and energy resolution are determined through spectral calibration. The energy resolution at 5.95 keV is 142 eV, now. According to the timing calibration, the mean response time of the engineering model is 1.55 <span>(upmu )</span>s, the full width at half maximum of the response time distribution is 0.45 <span>(upmu )</span>s, and the engineering model has sufficient ability to detect the profile of millisecond pulsars.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-06-14","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141412074","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":"SunbYte: an autonomous pointing framework for low-cost robotic solar telescopes on high altitude balloons","authors":"Yun-Hang Cho,&nbsp;Gianni Heung,&nbsp;Yakov Bobrov,&nbsp;Joseph Middleton,&nbsp;Josh Brownlow,&nbsp;Gary Verth,&nbsp;Viktor Fedun","doi":"10.1007/s10686-024-09944-w","DOIUrl":"10.1007/s10686-024-09944-w","url":null,"abstract":"<div><p>The design and usability of a fully autonomous robotic control system (SunbYte - Sheffield University Balloon “lYfted” TElescope) for solar tracking and observational applications onboard high-altitude balloons are addressed here. The design is based on a six-step development plan balancing scientific objectives and practical engineering requirements. The high-altitude solar observational system includes low-cost components such as a Cassegrain-type telescope, stepper motors, harmonic drives, USB cameras and microprocessors. OpenCV installed from ROS (Robotic Operating System), python and C facilitated the collection, compression, and processing of housekeeping and scientific data. This processed data was then transmitted to the ground station through the launch vehicle’s telecommunication link. The SunbYte system allows the brightest spot in the sky, the sun, to be identified, and a telescope pointed towards it with high enough accuracy that a scientific camera can capture images. This paper gathers and presents the results from primarily two missions with the High-Altitude Student Platform (HASP, NASA Balloon Program office and LaSpace). Additionally, a discussion will be made comparing these with an earlier iteration flown with the German-Swedish “REXUS/BEXUS” programme coordinated by the European Space Agency. By capturing and analysing a series of tracking images with the location of the Sun at the calibrated centre, the system demonstrated the tracking capabilities on an unstable balloon during ascent. Housekeeping sensor data was collected to further analyse the thermal and mechanical performance. The low temperature increased friction in the drive train and reduced the responsiveness of the harmonic drive actuation system. This caused some issues which require further work in future missions, for example, with SunbYte 4 and its work when flying with the HEMERA ZPB (Zero Pressure Balloon) program.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-06-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"https://link.springer.com/content/pdf/10.1007/s10686-024-09944-w.pdf","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141414444","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":"Simulation of the in-flight background and performance of DRO/GTM","authors":"Chenwei Wang,&nbsp;Juan Zhang,&nbsp;Shijie Zheng,&nbsp;Shaolin Xiong,&nbsp;Zhenghua An,&nbsp;Wenxi Peng,&nbsp;Haisheng Zhao,&nbsp;Xiaoyun Zhao,&nbsp;Chao Zheng,&nbsp;Peiyi Feng,&nbsp;Ke Gong,&nbsp;Dongya Guo,&nbsp;Xinqiao Li,&nbsp;Jiacong Liu,&nbsp;Yaqing Liu,&nbsp;Wenjun Tan,&nbsp;Yue Wang,&nbsp;Wangchen Xue,&nbsp;Sheng Yang,&nbsp;Dali Zhang,&nbsp;Fan Zhang,&nbsp;Yanqiu Zhang","doi":"10.1007/s10686-024-09946-8","DOIUrl":"10.1007/s10686-024-09946-8","url":null,"abstract":"<div><p>As a new member of the high energy astronomical transient monitoring network, Gamma-ray Transient Monitor (GTM) is an all-sky monitor onboard the Distant Retrograde Orbit (DRO) mission which has been launched in March 2024. In this work, we investigate the space radiation environment of DRO, and study the in-flight background of GTM using GEANT4. The background count rate on each of the 5 GTP detectors of GTM is estimated to be about 800<span>(sim )</span>1000 counts/s in the energy range from 20 keV to 1 MeV after one-year operation on orbit. We find that there are two distinct spectral lines clearly visible in the background spectrum, i.e. the 59 keV emission line from the embedded calibration source <span>(^{241})</span>Am and the 511 keV emission line induced by space radiations, which are suitable for the in-flight energy gain calibration. These results provide important reference for the development of payload, design of observation strategies, in-flight calibration of instrument and research of scientific objectives.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-06-13","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141401537","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 study of cosmic microwave background using non-extensive statistics","authors":"Somita Dhal,&nbsp;R. K. Paul","doi":"10.1007/s10686-024-09943-x","DOIUrl":"10.1007/s10686-024-09943-x","url":null,"abstract":"<div><p>The cosmic microwave background (CMB) radiation, the relic afterglow of the Big Bang, has become one of the most useful and precise tools in modern precision cosmology. In this article, we employ Tsallis non-extensive statistical framework to calculate the cosmic microwave background (CMB) temperature and its probability distribution by utilising a recently proposed blackbody radiation inversion (BRI) technique and the cosmic background explorer/ far infrared absolute spectrophotometer (COBE/FIRAS) dataset. Here, we have used the best-fit values of q = 0.99888 ± 0.00016 and q = 1.00012 ± 0.00001, obtained by fitting COBE/FIRAS data with two different versions of non-extensive models. We compare the results with the more conventional extensive statistical analysis i.e. for q = 1.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-06-12","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141402329","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":"Daksha: on alert for high energy transients","authors":"Varun Bhalerao,&nbsp;Santosh Vadawale,&nbsp;Shriharsh Tendulkar,&nbsp;Dipankar Bhattacharya,&nbsp;Vikram Rana,&nbsp;Hitesh Kumar L. Adalja,&nbsp;Hrishikesh Belatikar,&nbsp;Mahesh Bhaganagare,&nbsp;Gulab Dewangan,&nbsp;Abhijeet Ghodgaonkar,&nbsp;Shiv Kumar Goyal,&nbsp;Suresh Gunasekaran,&nbsp;Guruprasad P J,&nbsp;Jayprakash G. Koyande,&nbsp;Salil Kulkarni,&nbsp;APK Kutty,&nbsp;Tinkal Ladiya,&nbsp;Suddhasatta Mahapatra,&nbsp;Deepak Marla,&nbsp;Sujay Mate,&nbsp;N.P.S. Mithun,&nbsp;Rakesh Mote,&nbsp;Sanjoli Narang,&nbsp;Ayush Nema,&nbsp;Sudhanshu Nimbalkar,&nbsp;Archana Pai,&nbsp;Sourav Palit,&nbsp;Arpit Patel,&nbsp;Jinaykumar Patel,&nbsp;Priya Pradeep,&nbsp;Prabhu Ramachandran,&nbsp;B.S. Bharath Saiguhan,&nbsp;Divita Saraogi,&nbsp;Disha Sawant,&nbsp;M. Shanmugam,&nbsp;Piyush Sharma,&nbsp;Amit Shetye,&nbsp;Nishant Singh,&nbsp;Shreeya Singh,&nbsp;Akshat Singhal,&nbsp;S. Sreekumar,&nbsp;Srividhya Sridhar,&nbsp;Rahul Srinivasan,&nbsp;Siddharth Tallur,&nbsp;Neeraj K. Tiwari,&nbsp;Amrutha Lakshmi Vadladi,&nbsp;C. S. Vaishnava,&nbsp;Sandeep Vishwakarma,&nbsp;Gaurav Waratkar","doi":"10.1007/s10686-024-09926-y","DOIUrl":"10.1007/s10686-024-09926-y","url":null,"abstract":"<div><p>We present <i>Daksha</i>, a proposed high energy transients mission for the study of electromagnetic counterparts of gravitational wave sources, and gamma ray bursts. <i>Daksha</i> will comprise of two satellites in low earth equatorial orbits, on opposite sides of the Earth. Each satellite will carry three types of detectors to cover the entire sky in an energy range from 1 keV to <span>(&gt;1)</span> MeV. Any transients detected on-board will be announced publicly within minutes of discovery. All photon data will be downloaded in ground station passes to obtain source positions, spectra, and light curves. In addition, <i>Daksha</i> will address a wide range of science cases including monitoring X-ray pulsars, studies of magnetars, solar flares, searches for fast radio burst counterparts, routine monitoring of bright persistent high energy sources, terrestrial gamma-ray flashes, and probing primordial black hole abundances through lensing. In this paper, we discuss the technical capabilities of <i>Daksha</i>, while the detailed science case is discussed in a separate paper.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-06-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141529176","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":"Science with the Daksha high energy transients mission","authors":"Varun Bhalerao,&nbsp;Disha Sawant,&nbsp;Archana Pai,&nbsp;Shriharsh Tendulkar,&nbsp;Santosh Vadawale,&nbsp;Dipankar Bhattacharya,&nbsp;Vikram Rana,&nbsp;Hitesh Kumar L. Adalja,&nbsp;G C Anupama,&nbsp;Suman Bala,&nbsp;Smaranika Banerjee,&nbsp;Judhajeet Basu,&nbsp;Hrishikesh Belatikar,&nbsp;Paz Beniamini,&nbsp;Mahesh Bhaganagare,&nbsp;Ankush Bhaskar,&nbsp;Soumyadeep Bhattacharjee,&nbsp;Sukanta Bose,&nbsp;Brad Cenko,&nbsp;Mehul Vijay Chanda,&nbsp;Gulab Dewangan,&nbsp;Vishal Dixit,&nbsp;Anirban Dutta,&nbsp;Priyanka Gawade,&nbsp;Abhijeet Ghodgaonkar,&nbsp;Shiv Kumar Goyal,&nbsp;Suresh Gunasekaran,&nbsp;Manikantan Hemanth,&nbsp;Kenta Hotokezaka,&nbsp;Shabnam Iyyani,&nbsp;P. J. Guruprasad,&nbsp;Mansi Kasliwal,&nbsp;Jayprakash G. Koyande,&nbsp;Salil Kulkarni,&nbsp;APK Kutty,&nbsp;Tinkal Ladiya,&nbsp;Suddhasatta Mahapatra,&nbsp;Deepak Marla,&nbsp;Sujay Mate,&nbsp;Advait Mehla,&nbsp;N. P. S. Mithun,&nbsp;Surhud More,&nbsp;Rakesh Mote,&nbsp;Dipanjan Mukherjee,&nbsp;Sanjoli Narang,&nbsp;Shyama Narendranath,&nbsp;Ayush Nema,&nbsp;Sudhanshu Nimbalkar,&nbsp;Samaya Nissanke,&nbsp;Sourav Palit,&nbsp;Jinaykumar Patel,&nbsp;Arpit Patel,&nbsp;Biswajit Paul,&nbsp;Priya Pradeep,&nbsp;Prabhu Ramachandran,&nbsp;Kinjal Roy,&nbsp;B.S. Bharath Saiguhan,&nbsp;Joseph Saji,&nbsp;M. Saleem,&nbsp;Divita Saraogi,&nbsp;Parth Sastry,&nbsp;M. Shanmugam,&nbsp;Piyush Sharma,&nbsp;Amit Shetye,&nbsp;Nishant Singh,&nbsp;Shreeya Singh,&nbsp;Akshat Singhal,&nbsp;S. Sreekumar,&nbsp;Srividhya Sridhar,&nbsp;Rahul Srinivasan,&nbsp;Siddharth Tallur,&nbsp;Neeraj K. Tiwari,&nbsp;Amrutha Lakshmi Vadladi,&nbsp;C.S. Vaishnava,&nbsp;Sandeep Vishwakarma,&nbsp;Gaurav Waratkar","doi":"10.1007/s10686-024-09923-1","DOIUrl":"10.1007/s10686-024-09923-1","url":null,"abstract":"<div><p>We present the science case for the proposed <i>Daksha</i> high energy transients mission. <i>Daksha</i> will comprise of two satellites covering the entire sky from 1 keV to <span>(&gt;1)</span> MeV. The primary objectives of the mission are to discover and characterize electromagnetic counterparts to gravitational wave source; and to study Gamma Ray Bursts (GRBs). <i>Daksha</i> is a versatile all-sky monitor that can address a wide variety of science cases. With its broadband spectral response, high sensitivity, and continuous all-sky coverage, it will discover fainter and rarer sources than any other existing or proposed mission. <i>Daksha</i> can make key strides in GRB research with polarization studies, prompt soft spectroscopy, and fine time-resolved spectral studies. <i>Daksha</i> will provide continuous monitoring of X-ray pulsars. It will detect magnetar outbursts and high energy counterparts to Fast Radio Bursts. Using Earth occultation to measure source fluxes, the two satellites together will obtain daily flux measurements of bright hard X-ray sources including active galactic nuclei, X-ray binaries, and slow transients like Novae. Correlation studies between the two satellites can be used to probe primordial black holes through lensing. <i>Daksha</i> will have a set of detectors continuously pointing towards the Sun, providing excellent hard X-ray monitoring data. Closer to home, the high sensitivity and time resolution of <i>Daksha</i> can be leveraged for the characterization of Terrestrial Gamma-ray Flashes.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-06-10","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141505210","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 proposed plan of geodetic VLBI in India serving national and global objectives","authors":"Sujata Dhar,&nbsp;Nijat Mammadaliyev,&nbsp;Robert Heinkelmann,&nbsp;Susanne Glaser,&nbsp;Shrishail Raut,&nbsp;Arnab Laha,&nbsp;Ashutosh Tiwari,&nbsp;Harald Schuh,&nbsp;Onkar Dikshit,&nbsp;Nagarajan Balasubramanian","doi":"10.1007/s10686-024-09942-y","DOIUrl":"10.1007/s10686-024-09942-y","url":null,"abstract":"<div><p>Project “Saptarshi” was initiated by the National Centre for Geodesy, Indian Institute of Technology Kanpur to set up the modern space geodetic infrastructure in the country. This project primarily focuses on the establishment of an Indian Geodetic VLBI network. The purpose of this paper is to anticipate the potential impact of the geodetic VLBI network in India to the national and international scientific products. Saptarshi proposes to establish three VLBI stations along with a correlator at one facility. In this work, we investigate how adding proposed Indian VLBI antennas will affect terrestrial and celestial reference frames as well as Earth Orientation Parameters (EOP). Additionally, we shortly demonstrate scenario of VLBI observations of one of the Indian regional navigation satellite system called Navigation with Indian Constellation (NavIC) to determine its orbit. Two VLBI networks were simulated to observe the NAVIC satellite along with quasars to check how well the orbit of this satellite can be recovered from VLBI observations. To investigate the impact on the terrestrial reference frame, three types of 24-h sessions, IVS-R1 (legacy), IVS-VGOS (next generation VLBI), and IVS-AOV (Asia Oceania VLBI), were studied to examine the gain in precision of geodetic parameters when adding the proposed Indian VLBI antennas. IVS-type Intensive sessions were also investigated with the proposed Indian antennas to assess the improvement in the estimation of dUT1 as one important VLBI product. Furthermore, the u-v coverage of some radio sources of the southern hemisphere was compared utilizing observing networks with and without the proposed Indian antennas. Apart from that, we briefly discuss other benefits of the establishment of Indian geodetic VLBI in the scientific fields of atmosphere, metrology, and space missions.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-24","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"141102089","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":"Research and establishment of the X-ray monochromator at the 100XF","authors":"Dongjie Hou,&nbsp;Yifan Zhang,&nbsp;Yuxuan Zhu,&nbsp;Zijian Zhao,&nbsp;Ziliang Zhang,&nbsp;Xiongtao Yang,&nbsp;Jia Ma,&nbsp;He Xu,&nbsp;Yong Chen,&nbsp;Yupeng Xu,&nbsp;Yusa Wang,&nbsp;Congzhan Liu","doi":"10.1007/s10686-024-09941-z","DOIUrl":"10.1007/s10686-024-09941-z","url":null,"abstract":"<div><p>The 100-m X-ray Test Facility (100XF) was developed according to the calibration requirement of the first X-ray astronomical satellite <i>Insight</i>-HXMT in china. After that, the 100XF has provided calibration services for other X-ray astronomical satellites. In order to test the energy response matrices of space-borne detectors and to extend the capability of 100XF, a monochromator based on channel-cut crystals is developed. So far, 3.0-20.7 keV monochromatic X-rays have been realized successfully with Si(111) crystal. The monochromaticity (<span>(Delta )</span> <span>(mathrm E_textrm{FWHM})</span>/E) is better than 0.6% @5.9 keV, the flux stability can reach 2.6% in about one hour. The energy stability is particularly good, the variation is 0.05% in about one hour. Further more, the beam spot spreads in the plane orthogonal to the rocking direction after a propagation of 100-meter, which is sufficient and useful for testing detectors with large sensitive area. In this paper, we present the research and establishment of the X-ray monochromator at the 100XF.</p></div>","PeriodicalId":551,"journal":{"name":"Experimental Astronomy","volume":"57 3","pages":""},"PeriodicalIF":2.7,"publicationDate":"2024-05-11","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"140938548","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}