G. Ávila, G. Raskin, C. Schwab, J. Pember, B. Vandenbussche, H. Van Winckel, C. Guirao, Roman Guemperlein, J. Stürmer
MARVEL is a novel facility, consisting of an array of four robotic 80-cm telescopes and one highresolution Èchelle spectrograph. It targets extreme precision radial velocity observations for measuring the mass of exoplanets. The MARVEL spectrograph will be linked to the telescopes through a set of optical fibres. This fibre link consists of a combination of circular and octagonal fibres in an effort to maximize the photometric scrambling gain and hence, the illumination stability of the spectrograph. In this contribution, we present the design of the fibre link, as well as the results of a test campaign that evaluated the relevant characteristics of several circular and octagonal fibres. Based on this, we also report on the expected performances of the MARVEL fibre link.
{"title":"MARVEL: optical fiber link","authors":"G. Ávila, G. Raskin, C. Schwab, J. Pember, B. Vandenbussche, H. Van Winckel, C. Guirao, Roman Guemperlein, J. Stürmer","doi":"10.1117/12.2627382","DOIUrl":"https://doi.org/10.1117/12.2627382","url":null,"abstract":"MARVEL is a novel facility, consisting of an array of four robotic 80-cm telescopes and one highresolution Èchelle spectrograph. It targets extreme precision radial velocity observations for measuring the mass of exoplanets. The MARVEL spectrograph will be linked to the telescopes through a set of optical fibres. This fibre link consists of a combination of circular and octagonal fibres in an effort to maximize the photometric scrambling gain and hence, the illumination stability of the spectrograph. In this contribution, we present the design of the fibre link, as well as the results of a test campaign that evaluated the relevant characteristics of several circular and octagonal fibres. Based on this, we also report on the expected performances of the MARVEL fibre link.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"10 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-09-07","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"132805813","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
TNO, in close cooperation with Demcon, has designed the Laser Projection Subsystem (LPS) for ESO’s Extremely Large Telescope (ELT). The ELT LPS will consist of up to 8 laser projection subunits. The design is based on the Four Laser Guide Star Facility (4LGSF), built for the ESO Very Large Telescope (VLT) (5). The VLT AO system has been operational on the VLT UT4 in Paranal since early 2016. The system has demonstrated excellent performance and high reliability. The ELT LPS consist of a Baseplate with Beam Conditioning and Diagnostics System (BCDS), Optical Tube Assembly (OTA) and Cover Assembly. Control and driver electronics are mounted in a separate cabinet. TNO is responsible for the system design & verification and OTA. Demcon has designed the BCDS and Control Electronics. West End is building the Baseplate and Cover Assembly.
{"title":"Development of a laser projection system for the ELT","authors":"J. Nijenhuis, W. Jonker, F. Kamphues","doi":"10.1117/12.2630101","DOIUrl":"https://doi.org/10.1117/12.2630101","url":null,"abstract":"TNO, in close cooperation with Demcon, has designed the Laser Projection Subsystem (LPS) for ESO’s Extremely Large Telescope (ELT). The ELT LPS will consist of up to 8 laser projection subunits. The design is based on the Four Laser Guide Star Facility (4LGSF), built for the ESO Very Large Telescope (VLT) (5). The VLT AO system has been operational on the VLT UT4 in Paranal since early 2016. The system has demonstrated excellent performance and high reliability. The ELT LPS consist of a Baseplate with Beam Conditioning and Diagnostics System (BCDS), Optical Tube Assembly (OTA) and Cover Assembly. Control and driver electronics are mounted in a separate cabinet. TNO is responsible for the system design & verification and OTA. Demcon has designed the BCDS and Control Electronics. West End is building the Baseplate and Cover Assembly.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"30 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125181983","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
TMT will be a telescope with 492 segments making up the primary mirror. Each of these segments is supported with a highly sophisticated Segment Support Assembly (SSA) and each of them is to be tested for acceptance using a tool called SMATT. This tool will be mounted on top of each SSA and provides the load distribution applied to its 27 support points. These loads will vary slightly due to mechanical tolerances which is perfectly acceptable and can be predicted using FE-analysis. However manufacturing errors and parasitic stiffness contributions may cause unacceptable deviations. This should be avoided. The article will describe the functioning of SMATT. The tool is designed such that the segment support loads can be measured in any position. In the SSA, 21 Warping Harnesses (WH) are implemented to actively compensate for Surface Form Errors (SFE). These WH can also be verified for proper functioning when using SMATT.
{"title":"SMATT, a tool that measures the mechanical loads on the support points of the TMT primary mirror supports","authors":"J. Nijenhuis, N. van der Heiden, W. Jonker","doi":"10.1117/12.2630162","DOIUrl":"https://doi.org/10.1117/12.2630162","url":null,"abstract":"TMT will be a telescope with 492 segments making up the primary mirror. Each of these segments is supported with a highly sophisticated Segment Support Assembly (SSA) and each of them is to be tested for acceptance using a tool called SMATT. This tool will be mounted on top of each SSA and provides the load distribution applied to its 27 support points. These loads will vary slightly due to mechanical tolerances which is perfectly acceptable and can be predicted using FE-analysis. However manufacturing errors and parasitic stiffness contributions may cause unacceptable deviations. This should be avoided. The article will describe the functioning of SMATT. The tool is designed such that the segment support loads can be measured in any position. In the SSA, 21 Warping Harnesses (WH) are implemented to actively compensate for Surface Form Errors (SFE). These WH can also be verified for proper functioning when using SMATT.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"30 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125748475","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
A. Rakich, Hee-June Choi, C. Veillet, J. Hill, O. Kuhn, M. Bec, Yang Zhang, T. Brendel, B. Sitarski, W. Schoenell
LBTO, in partnership with GMTO, has been developing a laser-truss-based metrology system for the active alignment of telescope main optical components. Positive initial results convinced LBTO to commence to develop a "pathfinder" integrated operational active-optics system at prime focus, utilizing this technological approach. The prime-focus active-optics system benefits LBTO directly in improved system performance and is also very useful for GMTO in developing and gaining experience with a critical technical component of the GMT Telescope Metrology System. This paper describes the current system, which is now commissioned and operates in support of regular scientific observing. Technical aspects unique to direct laser truss metrology, such as system stability, the effects of correlated and uncorrelated noise, and the benefits of channel redundancy, will be discussed. Commissioning results and general system performance will also be reported. The paper will conclude with a section discussing some of the unexpected insights and improvements that the TMS has brought about at LBT by enabling the measurement of “clean” aberration data for aberrations arising from shape change on the borosilicate primary mirrors.
{"title":"Commissioning a laser metrology truss for active optics on the Large Binocular Telescope","authors":"A. Rakich, Hee-June Choi, C. Veillet, J. Hill, O. Kuhn, M. Bec, Yang Zhang, T. Brendel, B. Sitarski, W. Schoenell","doi":"10.1117/12.2629904","DOIUrl":"https://doi.org/10.1117/12.2629904","url":null,"abstract":"LBTO, in partnership with GMTO, has been developing a laser-truss-based metrology system for the active alignment of telescope main optical components. Positive initial results convinced LBTO to commence to develop a \"pathfinder\" integrated operational active-optics system at prime focus, utilizing this technological approach. The prime-focus active-optics system benefits LBTO directly in improved system performance and is also very useful for GMTO in developing and gaining experience with a critical technical component of the GMT Telescope Metrology System. This paper describes the current system, which is now commissioned and operates in support of regular scientific observing. Technical aspects unique to direct laser truss metrology, such as system stability, the effects of correlated and uncorrelated noise, and the benefits of channel redundancy, will be discussed. Commissioning results and general system performance will also be reported. The paper will conclude with a section discussing some of the unexpected insights and improvements that the TMS has brought about at LBT by enabling the measurement of “clean” aberration data for aberrations arising from shape change on the borosilicate primary mirrors.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"25 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-09-06","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"125194772","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Shuang Zhang, A. Santangelo, Yupeng Xu, M. Feroci, M. Hernanz, F. Lu, Yong Chen, H. Feng, K. Nandra, Weichun Jiang, J. Svoboda, S. Brandt, S. Schanne, J. I. in’t Zand, M. Michalska, E. Bozzo, E. Kalemci, I. Agudo, M. Ahangarianabhari, G. Aitink-Kroes, Z. An, Jiewei Cao, X. Cao, Tianxiang Chen, Can Chen, Yu-Peng Chen, Yaodong Cheng, Min Cong, W. Cui, T. Cui, Zhenyu Wu, Yichen Liu, Yongquan Su, James Ze Wang, Zhen Zhang, Ge Jin, Longhui Li, Xiangbiao Qiu, Yanjian Lin, Tao Li, Jiawei Zhang, Chao Wu, Wei Xu, Zexun Hu, Zhao Xu, Fangjian Qiao, K. Pan, S. Zhang, Liming Song, H. He, Fan Zhang, Hongwei Liu, Xiaojing Liu, Yanji Yang, Zeyu Song, Jiawei Zhang, Keyao Yu, Yusa Wang, Wei Li, Dawei Han, Juan Wang, Ziliang Zhang, Hao Wang, Dali Zhang, M. Gao, Jia‐jun Ma, J. Huo, Maoshun Li, D. Hou, Xiongtao Yang, Zijian Zhao, Xiaofa Zhao, Jingjing Xu, Laidan Luo, Yuxuan Zhu, Honglin Zhang, Xiaohua Liu, Yudong Gu, Yu Du, Sheng Yang, Liang Sun, Jiechen Jiang, Jia-wei Yang, Zefang Dong, Bo-ya Dai, Yang Jiao, X. Wen, B. Meng,
The enhanced x-ray timing and polarimetry mission (eXTP) is a flagship observatory for x-ray timing, spectroscopy and polarimetry developed by an international consortium. Thanks to its very large collecting area, good spectral resolution and unprecedented polarimetry capabilities, eXTP will explore the properties of matter and the propagation of light in the most extreme conditions found in the universe. eXTP will, in addition, be a powerful x-ray observatory. The mission will continuously monitor the x-ray sky, and will enable multi-wavelength and multi-messenger studies. The mission is currently in phase B, which will be completed in the middle of 2022.
{"title":"Enhanced X-ray Timing and Polarimetry mission: eXTP: an update on its scientific cases, mission profile and development status","authors":"Shuang Zhang, A. Santangelo, Yupeng Xu, M. Feroci, M. Hernanz, F. Lu, Yong Chen, H. Feng, K. Nandra, Weichun Jiang, J. Svoboda, S. Brandt, S. Schanne, J. I. in’t Zand, M. Michalska, E. Bozzo, E. Kalemci, I. Agudo, M. Ahangarianabhari, G. Aitink-Kroes, Z. An, Jiewei Cao, X. Cao, Tianxiang Chen, Can Chen, Yu-Peng Chen, Yaodong Cheng, Min Cong, W. Cui, T. Cui, Zhenyu Wu, Yichen Liu, Yongquan Su, James Ze Wang, Zhen Zhang, Ge Jin, Longhui Li, Xiangbiao Qiu, Yanjian Lin, Tao Li, Jiawei Zhang, Chao Wu, Wei Xu, Zexun Hu, Zhao Xu, Fangjian Qiao, K. Pan, S. Zhang, Liming Song, H. He, Fan Zhang, Hongwei Liu, Xiaojing Liu, Yanji Yang, Zeyu Song, Jiawei Zhang, Keyao Yu, Yusa Wang, Wei Li, Dawei Han, Juan Wang, Ziliang Zhang, Hao Wang, Dali Zhang, M. Gao, Jia‐jun Ma, J. Huo, Maoshun Li, D. Hou, Xiongtao Yang, Zijian Zhao, Xiaofa Zhao, Jingjing Xu, Laidan Luo, Yuxuan Zhu, Honglin Zhang, Xiaohua Liu, Yudong Gu, Yu Du, Sheng Yang, Liang Sun, Jiechen Jiang, Jia-wei Yang, Zefang Dong, Bo-ya Dai, Yang Jiao, X. Wen, B. Meng,","doi":"10.1117/12.2629340","DOIUrl":"https://doi.org/10.1117/12.2629340","url":null,"abstract":"The enhanced x-ray timing and polarimetry mission (eXTP) is a flagship observatory for x-ray timing, spectroscopy and polarimetry developed by an international consortium. Thanks to its very large collecting area, good spectral resolution and unprecedented polarimetry capabilities, eXTP will explore the properties of matter and the propagation of light in the most extreme conditions found in the universe. eXTP will, in addition, be a powerful x-ray observatory. The mission will continuously monitor the x-ray sky, and will enable multi-wavelength and multi-messenger studies. The mission is currently in phase B, which will be completed in the middle of 2022.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"235 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-09-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"114544900","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Yau-De Huang, Yuh-Jing Hwang, Chau-Ching Chiong, Hsi-Wei Yen, P. Koch, Chi-Den Huang, Bill Liu, Cheng Lin Chen, Jwu Jiunn Tsai, Wei-Ling Hsiung, Li-Pin Chi, Chin-Ting Ho, Chao Wang, Chen Chien, Y. Chu, P. Ho, F. Kemper, O. Morata, Álvaro González, S. Iguchi, Y. Uzawa, D. Iono, H. Nagai, J. Effland, K. Saini, M. Pospieszalski, D. Henke, K. Yeung, R. Finger, V. Tapia, N. Reyes, G. Siringo, G. Marconi, R. Cabezas
The Atacama large millimeter/submillimeter array (ALMA) band-1 receiver covers the frequency band between 35-50 GHz. An extension of up to 52 GHz is on a best-effort basis. Covering the longest wavelengths visible with ALMA, this receiver is enabling studies of dust grain evolution in proto-planetary systems probing dust grain sizes close to 1 cm, and with multiple red-shifted molecular lines it will open up a new window in the high-redshift universe. The band-1 project has recently achieved first light and with this passed a major project milestone. We present the challenges, from initial development to prototype, to establishing the infrastructure, integration, and evaluation of 73 production receiver units, and to the final tasks to complete the project. We conclude with the initial performance and characterization of the first band-1 receivers installed on ALMA.
{"title":"ALMA Band-1 (35-50GHz) receiver: first light, performance, and road to completion","authors":"Yau-De Huang, Yuh-Jing Hwang, Chau-Ching Chiong, Hsi-Wei Yen, P. Koch, Chi-Den Huang, Bill Liu, Cheng Lin Chen, Jwu Jiunn Tsai, Wei-Ling Hsiung, Li-Pin Chi, Chin-Ting Ho, Chao Wang, Chen Chien, Y. Chu, P. Ho, F. Kemper, O. Morata, Álvaro González, S. Iguchi, Y. Uzawa, D. Iono, H. Nagai, J. Effland, K. Saini, M. Pospieszalski, D. Henke, K. Yeung, R. Finger, V. Tapia, N. Reyes, G. Siringo, G. Marconi, R. Cabezas","doi":"10.1117/12.2629766","DOIUrl":"https://doi.org/10.1117/12.2629766","url":null,"abstract":"The Atacama large millimeter/submillimeter array (ALMA) band-1 receiver covers the frequency band between 35-50 GHz. An extension of up to 52 GHz is on a best-effort basis. Covering the longest wavelengths visible with ALMA, this receiver is enabling studies of dust grain evolution in proto-planetary systems probing dust grain sizes close to 1 cm, and with multiple red-shifted molecular lines it will open up a new window in the high-redshift universe. The band-1 project has recently achieved first light and with this passed a major project milestone. We present the challenges, from initial development to prototype, to establishing the infrastructure, integration, and evaluation of 73 production receiver units, and to the final tasks to complete the project. We conclude with the initial performance and characterization of the first band-1 receivers installed on ALMA.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"28 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-09-02","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115162336","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
G. Cataldo, P. Ade, C. Anderson, A. Barlis, E. Barrentine, N. Bellis, A. Bolatto, P. Breysse, B. Bulcha, J. Connors, P. Cursey, N. Ehsan, T. Essinger-Hileman, J. Glenn, J. Golec, J. Hays-Wehle, L. Hess, A. Jahromi, M. Kimball, A. Kogut, L. Lowe, P. Mauskopf, J. McMahon, Mona Mirzaei, S. Moseley, J. Mugge-Durum, O. Noroozian, Trevor M. Oxholm, U. Pen, A. Pullen, S. Rodriguez, P. Shirron, G. Siebert, A. Sinclair, R. Somerville, Ryan Stephenson, T. Stevenson, E. Switzer, P. Timbie, C. Tucker, E. Visbal, C. Volpert, Edward J. Wollack, Shengqi Yang
The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) will constrain star formation over cosmic time by carrying out a blind and complete census of redshifted carbon monoxide (CO) and ionized carbon ([CII]) emission in cross-correlation with galaxy survey data in redshift windows from the present to z=3.5 with a fully cryogenic, balloon-borne telescope. EXCLAIM will carry out extragalactic and Galactic surveys in a conventional balloon flight planned for 2023. EXCLAIM will be the first instrument to deploy µ-Spec silicon integrated spectrometers with a spectral resolving power R=512 covering 420-540 GHz. We summarize the design, science goals, and status of EXCLAIM.
{"title":"EXCLAIM: the EXperiment for Cryogenic Large-Aperture Intensity Mapping","authors":"G. Cataldo, P. Ade, C. Anderson, A. Barlis, E. Barrentine, N. Bellis, A. Bolatto, P. Breysse, B. Bulcha, J. Connors, P. Cursey, N. Ehsan, T. Essinger-Hileman, J. Glenn, J. Golec, J. Hays-Wehle, L. Hess, A. Jahromi, M. Kimball, A. Kogut, L. Lowe, P. Mauskopf, J. McMahon, Mona Mirzaei, S. Moseley, J. Mugge-Durum, O. Noroozian, Trevor M. Oxholm, U. Pen, A. Pullen, S. Rodriguez, P. Shirron, G. Siebert, A. Sinclair, R. Somerville, Ryan Stephenson, T. Stevenson, E. Switzer, P. Timbie, C. Tucker, E. Visbal, C. Volpert, Edward J. Wollack, Shengqi Yang","doi":"10.1117/12.2630054","DOIUrl":"https://doi.org/10.1117/12.2630054","url":null,"abstract":"The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) will constrain star formation over cosmic time by carrying out a blind and complete census of redshifted carbon monoxide (CO) and ionized carbon ([CII]) emission in cross-correlation with galaxy survey data in redshift windows from the present to z=3.5 with a fully cryogenic, balloon-borne telescope. EXCLAIM will carry out extragalactic and Galactic surveys in a conventional balloon flight planned for 2023. EXCLAIM will be the first instrument to deploy µ-Spec silicon integrated spectrometers with a spectral resolving power R=512 covering 420-540 GHz. We summarize the design, science goals, and status of EXCLAIM.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"552 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"123102031","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
Ultraviolet spectroscopy is a key element in the multi-wavelength approach to astronomy. Echelle spectroscopy provides high resolution and broad wavelength coverage and is a frequent choice for optical spectroscopy. However, it has limitations when applied to ultraviolet applications, particularly in the far ultraviolet, at wavelengths shortward of the MgF2 cutoff at ~ 1150 Å. I present an approach to provide echelle spectroscopy at these short wavelengths, enabling aberration control with only two optics post-telescope, by using gratings with curved and variable line-space grooves.
{"title":"Aberration corrected echelle spectrographs for the far ultraviolet","authors":"J. Green","doi":"10.1117/12.2623948","DOIUrl":"https://doi.org/10.1117/12.2623948","url":null,"abstract":"Ultraviolet spectroscopy is a key element in the multi-wavelength approach to astronomy. Echelle spectroscopy provides high resolution and broad wavelength coverage and is a frequent choice for optical spectroscopy. However, it has limitations when applied to ultraviolet applications, particularly in the far ultraviolet, at wavelengths shortward of the MgF2 cutoff at ~ 1150 Å. I present an approach to provide echelle spectroscopy at these short wavelengths, enabling aberration control with only two optics post-telescope, by using gratings with curved and variable line-space grooves.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"23 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127225779","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The Lyman-UV imaging spectrograph (LUVIS) is a NASA SMEX mission concept. Here, we describe the basic scientific requirements of LUVIS and instrumental requirements derived from the scientific requirements. Other papers in this conference by Woodruff et al. and Kendrick et al. describe the LUVIS instrument in detail.
莱曼-紫外成像光谱仪(LUVIS)是NASA SMEX任务的一个概念。在这里，我们描述了LUVIS的基本科学要求和由科学要求衍生出来的仪器要求。Woodruff et al.和Kendrick et al.在本次会议的其他论文中详细描述了LUVIS仪器。
{"title":"The Lyman-UV imaging spectrograph: a SMEX mission concept","authors":"S. Heap, T. Hull, S. Kendrick, R. Woodruff","doi":"10.1117/12.2630315","DOIUrl":"https://doi.org/10.1117/12.2630315","url":null,"abstract":"The Lyman-UV imaging spectrograph (LUVIS) is a NASA SMEX mission concept. Here, we describe the basic scientific requirements of LUVIS and instrumental requirements derived from the scientific requirements. Other papers in this conference by Woodruff et al. and Kendrick et al. describe the LUVIS instrument in detail.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"11 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"127308670","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
The source of galactic electron-positron annihilation 511 keV line has yet to be determined. Candidate sources include compact objects, radionuclides from stellar explosions, or the decay of dark matter particles. A major impediment to sensitive astrophysical gamma-ray spectroscopy is instrumental background. In the 200 keV–2 MeV energy range, cosmic-ray irradiation of spacecraft material results in contamination of secondary protons, neutrons, and gamma rays. This contamination is proportional to the spacecraft mass. A detector which maximizes the active detector mass fraction is the best way towards mapping the 511 keV sky and performing gamma-ray spectroscopy of astrophysical sources. We present progress in designing and building a compact, modular gamma-ray spectrometer that can be integrated into future spacecraft missions or as a small-satellite mission. A CubeSAT or SmallSAT-class mission based on such a design would improve sensitivity by an order-of-magnitude over current instruments like INTEGRAL-SPI by having a mass fraction of over 30% compared to INTEGRAL’s 0.6%.
{"title":"A compact gamma-ray spectrometer for nuclear astrophysics and planetary science","authors":"Z. Hughes, M. Errando, Tekeba Olbemo, William Ho","doi":"10.1117/12.2630475","DOIUrl":"https://doi.org/10.1117/12.2630475","url":null,"abstract":"The source of galactic electron-positron annihilation 511 keV line has yet to be determined. Candidate sources include compact objects, radionuclides from stellar explosions, or the decay of dark matter particles. A major impediment to sensitive astrophysical gamma-ray spectroscopy is instrumental background. In the 200 keV–2 MeV energy range, cosmic-ray irradiation of spacecraft material results in contamination of secondary protons, neutrons, and gamma rays. This contamination is proportional to the spacecraft mass. A detector which maximizes the active detector mass fraction is the best way towards mapping the 511 keV sky and performing gamma-ray spectroscopy of astrophysical sources. We present progress in designing and building a compact, modular gamma-ray spectrometer that can be integrated into future spacecraft missions or as a small-satellite mission. A CubeSAT or SmallSAT-class mission based on such a design would improve sensitivity by an order-of-magnitude over current instruments like INTEGRAL-SPI by having a mass fraction of over 30% compared to INTEGRAL’s 0.6%.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"34 1","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"115067050","PeriodicalName":null,"FirstCategoryId":null,"ListUrlMain":null,"RegionNum":0,"RegionCategory":"","ArticlePicture":[],"TitleCN":null,"AbstractTextCN":null,"PMCID":"","EPubDate":null,"PubModel":null,"JCR":null,"JCRName":null,"Score":null,"Total":0}
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