B. Salmaso, S. Basso, M. Ghigo, D. Spiga, Gabriele Vecchi, G. Sironi, V. Cotroneo, P. Conconi, E. Redaelli, Andrea Bianco, G. Pareschi, Gianpiero Tagliaferri, D. Sisana, C. Pelliciari, Mauro Fiorini, S. Incorvaia, M. Uslenghi, L. Paoletti, Claudio Ferrari, Andrea Zappettini, R. Lolli, M. Sanchez del Rio, G. Parodi, V. Burwitz, S. Rukdee, G. Hartner, T. Müller, T. Schmidt, A. Langmeier, D. Della Monica Ferreira, S. Massahi, N. Gellert, F. Christensen, M. Bavdaz, I. Ferreira, M. Collon, G. Vacanti, N. Barrière
The BEaTriX (Beam Expander Testing X-ray) facility is now operative at the INAF-Osservatorio Astronomico Brera (Merate, Italy). This facility has been specifically designed and built for the X-ray acceptance tests (PSF and Effective Area) of the ATHENA Silicon Pore Optics (SPO) Mirror Modules (MM). The unique setup creates a parallel, monochromatic, large X-ray beam, that fully illuminates the aperture of the MMs, generating an image at the ATHENA focal length of 12 m. This is made possible by a microfocus X-ray source followed by a chain of optical components (a paraboloidal mirror, 2 channel cut monochromators, and an asymmetric silicon crystal) able to expand the X-ray beam to a 6 cm × 17 cm size with a residual divergence of 1.5 arcsec (vertical) × 2.5 arcsec (horizontal). This paper reports the commissioning of the 4.5 keV beam line, and the first light obtained with a Mirror Module.
BEaTriX(波束扩展测试x射线)设备现在在意大利梅里特的国际天文研究所(inaf - observatorio Astronomico Brera)运行。该设施是专门为ATHENA硅孔光学(SPO)镜像模块(MM)的x射线验收测试(PSF和有效面积)而设计和建造的。独特的设置创造了一个平行的、单色的、大的x射线束，充分照亮mm的光圈，在雅典娜12米的焦距处产生图像。这可以通过微聚焦x射线源，然后是一系列光学元件(抛物面镜，2通道切割单色器和不对称硅晶体)，能够将x射线束扩展到6厘米× 17厘米的尺寸，剩余散度为1.5弧秒(垂直)× 2.5弧秒(水平)。本文报道了4.5 keV光束线的调试，以及用反射镜模块获得的第一束光。
{"title":"X-ray tests of the ATHENA mirror modules in BEaTriX: from design to reality","authors":"B. Salmaso, S. Basso, M. Ghigo, D. Spiga, Gabriele Vecchi, G. Sironi, V. Cotroneo, P. Conconi, E. Redaelli, Andrea Bianco, G. Pareschi, Gianpiero Tagliaferri, D. Sisana, C. Pelliciari, Mauro Fiorini, S. Incorvaia, M. Uslenghi, L. Paoletti, Claudio Ferrari, Andrea Zappettini, R. Lolli, M. Sanchez del Rio, G. Parodi, V. Burwitz, S. Rukdee, G. Hartner, T. Müller, T. Schmidt, A. Langmeier, D. Della Monica Ferreira, S. Massahi, N. Gellert, F. Christensen, M. Bavdaz, I. Ferreira, M. Collon, G. Vacanti, N. Barrière","doi":"10.1117/12.2628227","DOIUrl":"https://doi.org/10.1117/12.2628227","url":null,"abstract":"The BEaTriX (Beam Expander Testing X-ray) facility is now operative at the INAF-Osservatorio Astronomico Brera (Merate, Italy). This facility has been specifically designed and built for the X-ray acceptance tests (PSF and Effective Area) of the ATHENA Silicon Pore Optics (SPO) Mirror Modules (MM). The unique setup creates a parallel, monochromatic, large X-ray beam, that fully illuminates the aperture of the MMs, generating an image at the ATHENA focal length of 12 m. This is made possible by a microfocus X-ray source followed by a chain of optical components (a paraboloidal mirror, 2 channel cut monochromators, and an asymmetric silicon crystal) able to expand the X-ray beam to a 6 cm × 17 cm size with a residual divergence of 1.5 arcsec (vertical) × 2.5 arcsec (horizontal). This paper reports the commissioning of the 4.5 keV beam line, and the first light obtained with a Mirror Module.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"6 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":"125714130","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}
K. Mercier, F. Gonzalez, D. Götz, M. Boutelier, N. Boufracha, S. Clamagirand, Adrien Fort, A. Gomes, Emmanuel Guilhem, J. Le Duigou, Sophie Mazeau, J. Sanisidro, A. Meuris, C. Feldman, J. Pearson, R. Willingale, V. Burwitz, N. Meidinger, F. Robinet
SVOM (space-based multi-band astronomical variable objects monitor) is a mission developed within a Sino-French cooperation context and dedicated to the detection, localization and study of gamma ray bursts (GRBs) and other high-energy transient phenomena. Four instruments, operating in different wavelengths, are implemented on board in order to perform GRB detection and observations. The MXT instrument, developed by the National French Space Agency (CNES) in collaboration with CEA, MPE, IJCLab and the University of Leicester, is dedicated to the observation of GRB afterglows in the soft x-ray band and is one of the four instruments implemented on the Chinese satellite. First the design chosen of this instrument will be described and then the main results of the qualification campaign performed with the development models as EQM or STM and PFM models will be presented, as much at the instrument level as at the SVOM satellite QM level. Then, we will present how flight model design has been updated regarding the qualification campaign results. Furthermore, it will be presented how the performance of this kind of instrument is evaluated or measured through several models at sub system level or at instrument level. Finally, we will provide as a conclusion the main steps which have been achieved for this kind of development and give our main feedback.
{"title":"Results of the development of the MXT x-ray telescope for the SVOM mission","authors":"K. Mercier, F. Gonzalez, D. Götz, M. Boutelier, N. Boufracha, S. Clamagirand, Adrien Fort, A. Gomes, Emmanuel Guilhem, J. Le Duigou, Sophie Mazeau, J. Sanisidro, A. Meuris, C. Feldman, J. Pearson, R. Willingale, V. Burwitz, N. Meidinger, F. Robinet","doi":"10.1117/12.2630249","DOIUrl":"https://doi.org/10.1117/12.2630249","url":null,"abstract":"SVOM (space-based multi-band astronomical variable objects monitor) is a mission developed within a Sino-French cooperation context and dedicated to the detection, localization and study of gamma ray bursts (GRBs) and other high-energy transient phenomena. Four instruments, operating in different wavelengths, are implemented on board in order to perform GRB detection and observations. The MXT instrument, developed by the National French Space Agency (CNES) in collaboration with CEA, MPE, IJCLab and the University of Leicester, is dedicated to the observation of GRB afterglows in the soft x-ray band and is one of the four instruments implemented on the Chinese satellite. First the design chosen of this instrument will be described and then the main results of the qualification campaign performed with the development models as EQM or STM and PFM models will be presented, as much at the instrument level as at the SVOM satellite QM level. Then, we will present how flight model design has been updated regarding the qualification campaign results. Furthermore, it will be presented how the performance of this kind of instrument is evaluated or measured through several models at sub system level or at instrument level. Finally, we will provide as a conclusion the main steps which have been achieved for this kind of development and give our main feedback.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"27 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":"124095294","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}
D. Shy, C. Kierans, N. Cannady, R. Caputo, S. Griffin, E. Grove, E. Hays, E. Kong, N. Kirschner, I. Liceaga-Indart, J. Mcenery, J. Mitchell, A. Moiseev, L. Parker, J. Perkins, B. Phlips, M. Sasaki, Adam J. Schoenwald, C. Sleator, J. Smith, L. Smith, S. Wasti, R. Woolf, E. Wulf, A. Zajczyk
There is a growing interest in the science uniquely enabled by observations in the MeV range, particularly in light of multi-messenger astrophysics. The Compton Pair (ComPair) telescope, a prototype of the AMEGO Probe-class concept, consists of four subsystems that together detect and characterize gamma rays in the MeV regime. A double-sided strip silicon Tracker gives a precise measure of the first Compton scatter interaction and tracks pair-conversion products. A novel cadmium zinc telluride (CZT) detector with excellent position and energy resolution beneath the Tracker detects the Compton-scattered photons. A thick cesium iodide (CsI) calorimeter contains the high-energy Compton and pair events. The instrument is surrounded by a plastic anti-coincidence (ACD) detector to veto the cosmic-ray background. In this work, we will give an overview of the science motivation and a description of the prototype development and performance.
{"title":"Development of the ComPair gamma-ray telescope prototype","authors":"D. Shy, C. Kierans, N. Cannady, R. Caputo, S. Griffin, E. Grove, E. Hays, E. Kong, N. Kirschner, I. Liceaga-Indart, J. Mcenery, J. Mitchell, A. Moiseev, L. Parker, J. Perkins, B. Phlips, M. Sasaki, Adam J. Schoenwald, C. Sleator, J. Smith, L. Smith, S. Wasti, R. Woolf, E. Wulf, A. Zajczyk","doi":"10.1117/12.2628811","DOIUrl":"https://doi.org/10.1117/12.2628811","url":null,"abstract":"There is a growing interest in the science uniquely enabled by observations in the MeV range, particularly in light of multi-messenger astrophysics. The Compton Pair (ComPair) telescope, a prototype of the AMEGO Probe-class concept, consists of four subsystems that together detect and characterize gamma rays in the MeV regime. A double-sided strip silicon Tracker gives a precise measure of the first Compton scatter interaction and tracks pair-conversion products. A novel cadmium zinc telluride (CZT) detector with excellent position and energy resolution beneath the Tracker detects the Compton-scattered photons. A thick cesium iodide (CsI) calorimeter contains the high-energy Compton and pair events. The instrument is surrounded by a plastic anti-coincidence (ACD) detector to veto the cosmic-ray background. In this work, we will give an overview of the science motivation and a description of the prototype development and performance.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"32 16","pages":"0"},"PeriodicalIF":0.0,"publicationDate":"2022-08-31","publicationTypes":"Journal Article","fieldsOfStudy":null,"isOpenAccess":false,"openAccessPdf":"","citationCount":null,"resultStr":null,"platform":"Semanticscholar","paperid":"131501883","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}
Kosuke Sato, N. Yamasaki, S. Yamada, I. Mitsuishi, Y. Ichinohe, Hajime Omamiuda, Y. Uchida, K. Mitsuda, D. Nagai, K. Yoshikawa, K. Osato, K. Matsushita, Y. Fujita, Y. Ishisaki, Y. Ezoe, M. Ishida, Y. Maeda, N. Kawai, R. Fujimoto, T. Tsuru, N. Ota, Y. Nakashima
The super DIOS mission is a candidate of Japanese future satellite program after 2030’s and this scientific concept has been approved to establish an ISAS/JAXA research group. The main aim of the super DIOS is a x-ray survey to quantify of baryons, over several scales, from the circumgalactic medium around galaxies, cluster outskirts to the warm-hot intergalactic medium along the large cosmic structure by detections of the redshifted emission lines from OVII, OVIII and other ions, for investigating the dynamical state of baryons, including energy flow and metal cycles, in the universe. The super DIOS will have a resolution of 15 arcseconds and 3 kilo-pixels of transition edge sensor (TES) and its micro-wave SQUID multiplexer read-out system. This performance resolves most contaminating x-ray sources and reduces the level of diffuse x-ray background after subtracting point-like sources. The technical achievements of on-board cooling system reached by the Hitomi (ASTRO-H) and XRISM for microcalorimeter provide baseline technology for Super DIOS. We will also have a large scale collaborations with multi wave-length survey projects such as optical and radio survey observations.
{"title":"Super DIOS for exploring dark baryon","authors":"Kosuke Sato, N. Yamasaki, S. Yamada, I. Mitsuishi, Y. Ichinohe, Hajime Omamiuda, Y. Uchida, K. Mitsuda, D. Nagai, K. Yoshikawa, K. Osato, K. Matsushita, Y. Fujita, Y. Ishisaki, Y. Ezoe, M. Ishida, Y. Maeda, N. Kawai, R. Fujimoto, T. Tsuru, N. Ota, Y. Nakashima","doi":"10.1117/12.2629066","DOIUrl":"https://doi.org/10.1117/12.2629066","url":null,"abstract":"The super DIOS mission is a candidate of Japanese future satellite program after 2030’s and this scientific concept has been approved to establish an ISAS/JAXA research group. The main aim of the super DIOS is a x-ray survey to quantify of baryons, over several scales, from the circumgalactic medium around galaxies, cluster outskirts to the warm-hot intergalactic medium along the large cosmic structure by detections of the redshifted emission lines from OVII, OVIII and other ions, for investigating the dynamical state of baryons, including energy flow and metal cycles, in the universe. The super DIOS will have a resolution of 15 arcseconds and 3 kilo-pixels of transition edge sensor (TES) and its micro-wave SQUID multiplexer read-out system. This performance resolves most contaminating x-ray sources and reduces the level of diffuse x-ray background after subtracting point-like sources. The technical achievements of on-board cooling system reached by the Hitomi (ASTRO-H) and XRISM for microcalorimeter provide baseline technology for Super DIOS. We will also have a large scale collaborations with multi wave-length survey projects such as optical and radio survey observations.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"52 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":"130439128","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}
R. Boissay-Malaquin, T. Hayashi, K. Tamura, T. Okajima, Toshiki Sato, L. Olsen, R. Koenecke, Wilson Lara, Leor Bleier, M. Eckart, M. Leutenegger, T. Yaqoob, M. Chiao
We present a summary of the ground calibration of the x-ray mirror assemblies (XMAs) for the XRISM satellite, that has been performed at the x-ray beamline at NASA’s Goddard Space Flight Center. We used a scan method with a narrow x-ray pencil beam to calibrate both Resolve and Xtend XMAs, at eight different energies. In this paper, we give an overview of the measurement setup, and show the resulting on-axis and off-axis effective area response. Results of imaging performance, stray light, and performance variation across the aperture will be presented in separate publications.
{"title":"Ground calibration of the x-ray mirror assembly for the X-Ray Imaging and Spectroscopy Mission (XRISM) I-measurement setup and effective area","authors":"R. Boissay-Malaquin, T. Hayashi, K. Tamura, T. Okajima, Toshiki Sato, L. Olsen, R. Koenecke, Wilson Lara, Leor Bleier, M. Eckart, M. Leutenegger, T. Yaqoob, M. Chiao","doi":"10.1117/12.2627563","DOIUrl":"https://doi.org/10.1117/12.2627563","url":null,"abstract":"We present a summary of the ground calibration of the x-ray mirror assemblies (XMAs) for the XRISM satellite, that has been performed at the x-ray beamline at NASA’s Goddard Space Flight Center. We used a scan method with a narrow x-ray pencil beam to calibrate both Resolve and Xtend XMAs, at eight different energies. In this paper, we give an overview of the measurement setup, and show the resulting on-axis and off-axis effective area response. Results of imaging performance, stray light, and performance variation across the aperture will be presented in separate publications.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"12 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":"133851257","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}
Y. Ezoe, R. Funase, H. Nagata, Y. Miyoshi, H. Nakajima, I. Mitsuishi, K. Ishikawa, Yosuke Kawabata, Shintaro Nakajima, Landon Kamps, M. Numazawa, T. Yoneyama, K. Hagino, Y. Matsumoto, K. Hosokawa, S. Kasahara, J. Hiraga, K. Mitsuda, M. Fujimoto, M. Ueno, A. Yamazaki, H. Hasegawa, T. Mitani, Y. Kawakatsu, T. Iwata, H. Koizumi, H. Sahara, Y. Kanamori, K. Morishita
GEO-X (GEOspace X-ray imager) is a small satellite mission aiming at visualization of the Earth’s magnetosphere by X-rays and revealing dynamical couplings between solar wind and magnetosphere. In-situ spacecraft have revealed various phenomena in the magnetosphere. In recent years, X-ray astronomy satellite observations discovered soft X-ray emission originated from the magnetosphere. We therefore develop GEO-X by integrating innovative technologies of the wide FOV X-ray instrument and the microsatellite technology for deep space exploration. GEO-X is a 50 kg class microsatellite carrying a novel compact X-ray imaging spectrometer payload. The microsatellite having a large delta v (<700 m/s) to increase an altitude at 40-60 RE from relatively lowaltitude (e.g., Geo Transfer Orbit) piggyback launch is necessary. We thus combine a 18U Cubesat with the hybrid kick motor composed of liquid N2O and polyethylene. We also develop a wide FOV (5×5 deg) and a good spatial resolution (10 arcmin) X-ray (0.3-2 keV) imager. We utilize a micromachined X-ray telescope, and a CMOS detector system with an optical blocking filter. We aim to launch the satellite around the 25th solar maximum.
GEO-X(地球空间x射线成像仪)是一个小型卫星任务，旨在通过x射线可视化地球磁层并揭示太阳风和磁层之间的动力学耦合。原位航天器揭示了磁层中的各种现象。近年来，x射线天文卫星观测发现软x射线发射起源于磁层。因此，我们将大视场x射线仪器的创新技术与深空探测微卫星技术相结合，开发GEO-X。GEO-X是一颗50公斤级微型卫星，携带新型紧凑x射线成像光谱仪有效载荷。具有较大δ v (<700 m/s)的微型卫星从相对较低的高度(例如，地球转移轨道)在40-60 RE时增加高度是必要的。因此，我们将18U立方体卫星与液体N2O和聚乙烯组成的混合踢腿电机结合起来。我们还开发了宽视场(5×5度)和良好的空间分辨率(10角分)x射线(0.3-2 keV)成像仪。我们利用一个微机械x射线望远镜，和一个CMOS探测器系统与光学阻塞滤波器。我们的目标是在第25次太阳活动极大期前后发射卫星。
{"title":"GEO-X (GEOspace X-ray imager)","authors":"Y. Ezoe, R. Funase, H. Nagata, Y. Miyoshi, H. Nakajima, I. Mitsuishi, K. Ishikawa, Yosuke Kawabata, Shintaro Nakajima, Landon Kamps, M. Numazawa, T. Yoneyama, K. Hagino, Y. Matsumoto, K. Hosokawa, S. Kasahara, J. Hiraga, K. Mitsuda, M. Fujimoto, M. Ueno, A. Yamazaki, H. Hasegawa, T. Mitani, Y. Kawakatsu, T. Iwata, H. Koizumi, H. Sahara, Y. Kanamori, K. Morishita","doi":"10.1117/12.2629107","DOIUrl":"https://doi.org/10.1117/12.2629107","url":null,"abstract":"GEO-X (GEOspace X-ray imager) is a small satellite mission aiming at visualization of the Earth’s magnetosphere by X-rays and revealing dynamical couplings between solar wind and magnetosphere. In-situ spacecraft have revealed various phenomena in the magnetosphere. In recent years, X-ray astronomy satellite observations discovered soft X-ray emission originated from the magnetosphere. We therefore develop GEO-X by integrating innovative technologies of the wide FOV X-ray instrument and the microsatellite technology for deep space exploration. GEO-X is a 50 kg class microsatellite carrying a novel compact X-ray imaging spectrometer payload. The microsatellite having a large delta v (<700 m/s) to increase an altitude at 40-60 RE from relatively lowaltitude (e.g., Geo Transfer Orbit) piggyback launch is necessary. We thus combine a 18U Cubesat with the hybrid kick motor composed of liquid N2O and polyethylene. We also develop a wide FOV (5×5 deg) and a good spatial resolution (10 arcmin) X-ray (0.3-2 keV) imager. We utilize a micromachined X-ray telescope, and a CMOS detector system with an optical blocking filter. We aim to launch the satellite around the 25th solar maximum.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"13 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":"132455714","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. I. Gómez de Castro, Ana I De Isidro-Gómez, Diego de Leyva, Francesca Bachiotti, J. Leon, Pol Ribes, J. Casalta, C. Miravet, J. C. Vallejo, M. Sachkov, Ada Canet, B. Shustov, R. de la Fuente, K. France, Lucas Patty, S. Benetti, A. ud-Doula
The mission Ultraviolet Researcher to Investigate the Emergence of Life (URIEL) is designed to carry out low dispersion (600-1,000) UV spectropolarimetry in the 140-400 nm spectral range to investigate the formation of planetary systems, its interaction with stellar winds and search for signatures of prebiotic molecules by remote sensing of small bodies in the Solar System (comets and meteorites) in near Earth orbit. URIEL is conceived as a 50cm primary telescope with a RitcheyChrétien mounting. The telescope is equipped with a single instrument, the ultraviolet spectropolarimeter, whose low dispersion will enable resolving the main spectral features whilst guaranteeing enough flux per resolution element for the Stokes parameters to be measured to an accuracy of 500 ppm in the full range. According to recent calculations based on the chemical analysis of meteorites, this accuracy suffices for the remote detection of alanine by its optical activity at 180 nm in nearby minor bodies. In this sense, URIEL is a pathfinder mission to the technology that will enable remote sensing of amino acids and addressing the source of the chirality imbalance in Earth's bio-molecules.
{"title":"The ultraviolet researcher to investigate the emergence of life: a mission proposal to ESA's F-call","authors":"A. I. Gómez de Castro, Ana I De Isidro-Gómez, Diego de Leyva, Francesca Bachiotti, J. Leon, Pol Ribes, J. Casalta, C. Miravet, J. C. Vallejo, M. Sachkov, Ada Canet, B. Shustov, R. de la Fuente, K. France, Lucas Patty, S. Benetti, A. ud-Doula","doi":"10.1117/12.2630650","DOIUrl":"https://doi.org/10.1117/12.2630650","url":null,"abstract":"The mission Ultraviolet Researcher to Investigate the Emergence of Life (URIEL) is designed to carry out low dispersion (600-1,000) UV spectropolarimetry in the 140-400 nm spectral range to investigate the formation of planetary systems, its interaction with stellar winds and search for signatures of prebiotic molecules by remote sensing of small bodies in the Solar System (comets and meteorites) in near Earth orbit. URIEL is conceived as a 50cm primary telescope with a RitcheyChrétien mounting. The telescope is equipped with a single instrument, the ultraviolet spectropolarimeter, whose low dispersion will enable resolving the main spectral features whilst guaranteeing enough flux per resolution element for the Stokes parameters to be measured to an accuracy of 500 ppm in the full range. According to recent calculations based on the chemical analysis of meteorites, this accuracy suffices for the remote detection of alanine by its optical activity at 180 nm in nearby minor bodies. In this sense, URIEL is a pathfinder mission to the technology that will enable remote sensing of amino acids and addressing the source of the chirality imbalance in Earth's bio-molecules.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"68 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":"125001127","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}
D. Henke, F. Jiang, S. Salem Hesari, A. Seyfollahi, B. Veidt, L. Knee
In radio astronomy instrumentation, the benefit of increased spectral grasp must be evaluated against a decrease in overall system performance (e.g., system noise, stability, and optical efficiency) and considerable effort has gone into quantifying the best overall choice to define receiver bands for a particular telescope; present examples include the Square Kilometre Array (SKA) and the Next Generation Very Large Array (ngVLA) where the higher bands do not exceed a bandwidth of 1.7:1. During the last two years, NRC Herzberg has been researching wide bandwidth waveguide and active components in order to extend the bandwidth to a full 2:1 octave bandwidth. We report on recent innovation in front-end receiver components, including an octave bandwidth feed horn, OMT, and LNA, to enable wideband science
{"title":"Octave bandwidth receiver technology for radio and millimetre-wave telescopes","authors":"D. Henke, F. Jiang, S. Salem Hesari, A. Seyfollahi, B. Veidt, L. Knee","doi":"10.1117/12.2630537","DOIUrl":"https://doi.org/10.1117/12.2630537","url":null,"abstract":"In radio astronomy instrumentation, the benefit of increased spectral grasp must be evaluated against a decrease in overall system performance (e.g., system noise, stability, and optical efficiency) and considerable effort has gone into quantifying the best overall choice to define receiver bands for a particular telescope; present examples include the Square Kilometre Array (SKA) and the Next Generation Very Large Array (ngVLA) where the higher bands do not exceed a bandwidth of 1.7:1. During the last two years, NRC Herzberg has been researching wide bandwidth waveguide and active components in order to extend the bandwidth to a full 2:1 octave bandwidth. We report on recent innovation in front-end receiver components, including an octave bandwidth feed horn, OMT, and LNA, to enable wideband science","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"12 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":"115057206","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}
P. Nogara, G. Sottile, F. Russo, G. La Rosa, F. L. Lo Gerfo, M. Del Santo, Y. Evangelista, Riccardo Campana, F. Fuschino, F. Fiore
HERMES Pathfinder (High Energy Rapid Modular Ensemble of Satellites Pathfinder) is a space mission based on a constellation of nano-satellites in a low Earth Orbit, hosting new miniaturized detectors to probe the X-ray temporal emission of bright high-energy transients such as Gamma-Ray Bursts and the electromagnetic counterparts of Gravitational Waves. This ambitious goal will be achieved exploiting at most Commercial offthe-shelf components. For HERMES-SP, a custom Power Supply Unit board has been designed to supply the needed voltages to the payload and, at the same time, protecting it from Latch-Up events.
{"title":"The power supply unit onboard the HERMES nano-satellite constellation","authors":"P. Nogara, G. Sottile, F. Russo, G. La Rosa, F. L. Lo Gerfo, M. Del Santo, Y. Evangelista, Riccardo Campana, F. Fuschino, F. Fiore","doi":"10.1117/12.2628540","DOIUrl":"https://doi.org/10.1117/12.2628540","url":null,"abstract":"HERMES Pathfinder (High Energy Rapid Modular Ensemble of Satellites Pathfinder) is a space mission based on a constellation of nano-satellites in a low Earth Orbit, hosting new miniaturized detectors to probe the X-ray temporal emission of bright high-energy transients such as Gamma-Ray Bursts and the electromagnetic counterparts of Gravitational Waves. This ambitious goal will be achieved exploiting at most Commercial offthe-shelf components. For HERMES-SP, a custom Power Supply Unit board has been designed to supply the needed voltages to the payload and, at the same time, protecting it from Latch-Up events.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"62 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":"124924575","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}
Nianhua Jiang, L. Knee, D. Garcia, P. Niranjanan, I. Wevers
The next-generation Very Large Array (ngVLA) front end incorporates six dual-polarization receivers covering the frequency range from 1.2 to 116 GHz. The ngVLA Band-1 receiver covers a frequency range of 1.2 to 3.5 GHz. This wideband requirement presents a challenge for the extremely low noise design for the required cryogenic low noise amplifier (LNA). GaAs HEMT technology is very reliable at a gate length of 150 nm and that gate feature size is suitable for low noise amplifiers up to the microwave frequency range. Below 3 GHz, the transistor gate has a very large capacitive impedance, exhibiting like an open circuit, which requires large values of inductors for 50 Ω impedance and low noise matching. The hybrid circuit configuration allows the design to select high-Q discrete inductors and capacitors with large values to minimize loss/noise from passive components. A two-stage single-ended GaAs HEMT LNA was designed based on the hybrid configuration. A prototype ngVLA Band-1 LNA was assembled and fully tested at a physical temperature 12 K. This newly designed GaAs HEMT LNA achieved 1.6 K average noise temperature and 34 dB average high gain between 1.2 and 3.5 GHz, the total power consumption is about 10 mW, which can meet the current requirements of the ngVLA Band-1 receiver.
{"title":"Wideband cryogenic LNA design for the ngVLA Band-1 receiver","authors":"Nianhua Jiang, L. Knee, D. Garcia, P. Niranjanan, I. Wevers","doi":"10.1117/12.2629137","DOIUrl":"https://doi.org/10.1117/12.2629137","url":null,"abstract":"The next-generation Very Large Array (ngVLA) front end incorporates six dual-polarization receivers covering the frequency range from 1.2 to 116 GHz. The ngVLA Band-1 receiver covers a frequency range of 1.2 to 3.5 GHz. This wideband requirement presents a challenge for the extremely low noise design for the required cryogenic low noise amplifier (LNA). GaAs HEMT technology is very reliable at a gate length of 150 nm and that gate feature size is suitable for low noise amplifiers up to the microwave frequency range. Below 3 GHz, the transistor gate has a very large capacitive impedance, exhibiting like an open circuit, which requires large values of inductors for 50 Ω impedance and low noise matching. The hybrid circuit configuration allows the design to select high-Q discrete inductors and capacitors with large values to minimize loss/noise from passive components. A two-stage single-ended GaAs HEMT LNA was designed based on the hybrid configuration. A prototype ngVLA Band-1 LNA was assembled and fully tested at a physical temperature 12 K. This newly designed GaAs HEMT LNA achieved 1.6 K average noise temperature and 34 dB average high gain between 1.2 and 3.5 GHz, the total power consumption is about 10 mW, which can meet the current requirements of the ngVLA Band-1 receiver.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"12190 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":"129673444","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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