B. Westbrook, C. Raum, S. Beckman, Adrian T. Lee, Nicole Farias, Andrew Bogdan, A. Hornsby, A. Suzuki, K. Rotermund, T. Elleflot, Jason E. Austerman, J. Beall, S. Duff, J. Hubmayr, M. Vissers, M. Link, G. Jaehnig, N. Halverson, Tomasso Ghigna, S. Stever, Y. Minami, Keith L. Thompson, Megan B. Russell, K. Arnold, M. Silva-Feaver
LiteBIRD is a JAXA-led strategic large-class satellite mission designed to measure the polarization of the cosmic microwave background and Galactic foregrounds from 34 to 448 GHz across the entire sky from L2 in the late 2020s. The scientific payload includes three telescopes which are called the low-, mid-, and high-frequency telescopes each with their own receiver that covers a portion of the mission’s frequency range. The low frequency telescope will map synchrotron radiation from the Galactic foreground and the cosmic microwave background. We discuss the design, fabrication, and characterization of the low-frequency focal plane modules for low-frequency telescope, which has a total bandwidth ranging from 34 to 161 GHz. There will be a total of 4 different pixel types with 8 overlapping bands to cover the full frequency range. These modules are housed in a single low-frequency focal plane unit which provides thermal isolation, mechanical support, and radiative baffling for the detectors. The module design implements multi-chroic lenslet-coupled sinuous antenna arrays coupled to transition edge sensor bolometers read out with frequency-domain mulitplexing. While this technology has strong heritage in ground-based cosmic microwave background experiments, the broad frequency coverage, low optical loading conditions, and the high cosmic ray background of the space environment require further development of this technology to be suitable for LiteBIRD. In these proceedings, we discuss the optical and bolometeric characterization of a triplexing prototype pixel with bands centered on 78, 100, and 140 GHz.
{"title":"Development of the low frequency telescope focal plane detector modules for LiteBIRD","authors":"B. Westbrook, C. Raum, S. Beckman, Adrian T. Lee, Nicole Farias, Andrew Bogdan, A. Hornsby, A. Suzuki, K. Rotermund, T. Elleflot, Jason E. Austerman, J. Beall, S. Duff, J. Hubmayr, M. Vissers, M. Link, G. Jaehnig, N. Halverson, Tomasso Ghigna, S. Stever, Y. Minami, Keith L. Thompson, Megan B. Russell, K. Arnold, M. Silva-Feaver","doi":"10.1117/12.2630574","DOIUrl":"https://doi.org/10.1117/12.2630574","url":null,"abstract":"LiteBIRD is a JAXA-led strategic large-class satellite mission designed to measure the polarization of the cosmic microwave background and Galactic foregrounds from 34 to 448 GHz across the entire sky from L2 in the late 2020s. The scientific payload includes three telescopes which are called the low-, mid-, and high-frequency telescopes each with their own receiver that covers a portion of the mission’s frequency range. The low frequency telescope will map synchrotron radiation from the Galactic foreground and the cosmic microwave background. We discuss the design, fabrication, and characterization of the low-frequency focal plane modules for low-frequency telescope, which has a total bandwidth ranging from 34 to 161 GHz. There will be a total of 4 different pixel types with 8 overlapping bands to cover the full frequency range. These modules are housed in a single low-frequency focal plane unit which provides thermal isolation, mechanical support, and radiative baffling for the detectors. The module design implements multi-chroic lenslet-coupled sinuous antenna arrays coupled to transition edge sensor bolometers read out with frequency-domain mulitplexing. While this technology has strong heritage in ground-based cosmic microwave background experiments, the broad frequency coverage, low optical loading conditions, and the high cosmic ray background of the space environment require further development of this technology to be suitable for LiteBIRD. In these proceedings, we discuss the optical and bolometeric characterization of a triplexing prototype pixel with bands centered on 78, 100, and 140 GHz.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"20 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":"126011235","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}
L. Ferro, E. Virgilli, M. Moita, F. Frontera, P. Rosati, C. Guidorzi, C. Ferrari, R. Lolli, E. Caroli, N. Auricchio, J. Stephen, S. del Sordo, C. Gargano, S. Squerzanti, M. Pucci, O. Limousin, A. Meuris, P. Laurent, Hugo Allaire
Hard x-/soft gamma-ray astronomy (>100 keV) is a crucial field for the study of important astrophysical phenomena such as the 511 keV positron annihilation line in the galactic center region and its origin, gamma-ray bursts, soft gamma-ray repeaters, nuclear lines from SN explosions and more. However, several key questions in this field require sensitivity and angular resolution that are hardly achievable with present technology. A new generation of instruments suitable to focus hard x-/soft gamma-rays is necessary to overcome the technological limitations of current direct-viewing telescopes. One solution is using Laue lenses based on Bragg’s diffraction in a transmission configuration. To date, this technology is in an advanced stage of development and further efforts are being made in order to significantly increase its technology readiness level (TRL). To this end, massive production of suitable crystals is required, as well as an improvement of the capability of their alignment. Such a technological improvement could be exploited in stratospheric balloon experiments and, ultimately, in space missions with a telescope of about 20 m focal length, capable of focusing over a broad energy pass-band. We present the latest technological developments of the TRILL (technological readiness increase for Laue lenses) project, supported by ASI, devoted to the advancement of the technological readiness of Laue lenses. We show the method we developed for preparing suitable bent germanium and silicon crystals and the latest advancements in crystals alignment technology.
{"title":"The TRILL project: increasing the technological readiness of Laue lenses","authors":"L. Ferro, E. Virgilli, M. Moita, F. Frontera, P. Rosati, C. Guidorzi, C. Ferrari, R. Lolli, E. Caroli, N. Auricchio, J. Stephen, S. del Sordo, C. Gargano, S. Squerzanti, M. Pucci, O. Limousin, A. Meuris, P. Laurent, Hugo Allaire","doi":"10.1117/12.2629872","DOIUrl":"https://doi.org/10.1117/12.2629872","url":null,"abstract":"Hard x-/soft gamma-ray astronomy (>100 keV) is a crucial field for the study of important astrophysical phenomena such as the 511 keV positron annihilation line in the galactic center region and its origin, gamma-ray bursts, soft gamma-ray repeaters, nuclear lines from SN explosions and more. However, several key questions in this field require sensitivity and angular resolution that are hardly achievable with present technology. A new generation of instruments suitable to focus hard x-/soft gamma-rays is necessary to overcome the technological limitations of current direct-viewing telescopes. One solution is using Laue lenses based on Bragg’s diffraction in a transmission configuration. To date, this technology is in an advanced stage of development and further efforts are being made in order to significantly increase its technology readiness level (TRL). To this end, massive production of suitable crystals is required, as well as an improvement of the capability of their alignment. Such a technological improvement could be exploited in stratospheric balloon experiments and, ultimately, in space missions with a telescope of about 20 m focal length, capable of focusing over a broad energy pass-band. We present the latest technological developments of the TRILL (technological readiness increase for Laue lenses) project, supported by ASI, devoted to the advancement of the technological readiness of Laue lenses. We show the method we developed for preparing suitable bent germanium and silicon crystals and the latest advancements in crystals alignment technology.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"1 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":"126192650","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. Spiga, G. Sironi, D. Della Monica Ferreira, A. S. Jegers, E. Bergbäck Knudsen, M. Bavdaz, I. Ferreira
Silicon pore optics (SPO) are the technology selected for the assembly of the mirror module of the ATHENA x-ray telescope. An SPO mirror module consists of a quadruple stack of etched and wedged silicon wafers, in order to create a stiff and lightweight structure, able to reproduce in each pore the Wolter-I geometry required to image x-rays on the telescope focal plane. Due to the small pore size (a few mm2 ), aperture diffraction effects in x-rays are small, but not totally negligible to the angular resolutions at play. In contrast, diffraction effects are the dominant term in the UV light illumination that will be used to co-align the 600 mirror modules of ATHENA to a common focus. For this reason, diffractive effects need to be properly modeled, and this constitutes a specific task of the ESA-led SImPOSIUM (sIlicon pore optic simulation and modelling) project, involving INAF-Brera and DTU. In this context, a specific software tool (SWORDS: Software for diffraction of silicon pore optics) has been developed to the end of simulating diffraction effects in SPO mirror modules. This approach also allows the user to effectively predict the effects of various imperfections (figure errors, misalignments) in a self-consistent way, in different experimental configurations (x-ray source off-axis or at finite distance), as a fast and reliable alternative to ray-tracing, also at x-ray wavelengths.
硅孔光学(SPO)是雅典娜x射线望远镜反射镜模块选用的组装技术。SPO镜面模块由四层蚀刻和楔形硅晶片组成，以创建一个坚固而轻便的结构，能够在每个孔中复制Wolter-I几何形状，以便在望远镜焦平面上成像x射线。由于孔径较小(几mm2)， x射线中的孔径衍射效应很小，但对角分辨率的影响并非完全可以忽略不计。相比之下，衍射效应是紫外光照明的主要术语，它将用于将雅典娜的600个镜子模块对准一个共同的焦点。因此，衍射效应需要适当建模，这是esa领导的SImPOSIUM(硅孔光学模拟和建模)项目的一项具体任务，该项目涉及INAF-Brera和DTU。在此背景下，专门开发了一种软件工具(SWORDS: software for diffraction of silicon pore optics)来模拟SPO反射镜模块中的衍射效应。这种方法还允许用户以自一致的方式有效地预测各种缺陷(图形误差，不对准)的影响，在不同的实验配置(x射线源离轴或在有限距离)，作为射线追踪的快速可靠的替代方案，也在x射线波长。
{"title":"Modelling diffractive effects in silicon pore optics for the ATHENA X-ray Telescope","authors":"D. Spiga, G. Sironi, D. Della Monica Ferreira, A. S. Jegers, E. Bergbäck Knudsen, M. Bavdaz, I. Ferreira","doi":"10.1117/12.2628133","DOIUrl":"https://doi.org/10.1117/12.2628133","url":null,"abstract":"Silicon pore optics (SPO) are the technology selected for the assembly of the mirror module of the ATHENA x-ray telescope. An SPO mirror module consists of a quadruple stack of etched and wedged silicon wafers, in order to create a stiff and lightweight structure, able to reproduce in each pore the Wolter-I geometry required to image x-rays on the telescope focal plane. Due to the small pore size (a few mm2 ), aperture diffraction effects in x-rays are small, but not totally negligible to the angular resolutions at play. In contrast, diffraction effects are the dominant term in the UV light illumination that will be used to co-align the 600 mirror modules of ATHENA to a common focus. For this reason, diffractive effects need to be properly modeled, and this constitutes a specific task of the ESA-led SImPOSIUM (sIlicon pore optic simulation and modelling) project, involving INAF-Brera and DTU. In this context, a specific software tool (SWORDS: Software for diffraction of silicon pore optics) has been developed to the end of simulating diffraction effects in SPO mirror modules. This approach also allows the user to effectively predict the effects of various imperfections (figure errors, misalignments) in a self-consistent way, in different experimental configurations (x-ray source off-axis or at finite distance), as a fast and reliable alternative to ray-tracing, also at x-ray wavelengths.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"5 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":"126879661","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}
M. Collon, Luis Abalo, N. Barrière, A. Bayerle, Luigi Castiglione, Noë Eenkhoorn, D. Girou, R. Günther, Enrico Hauser, Roy van der Hoeven, Jasper den Hollander, Yvette Jenkins, B. Landgraf, L. Keek, Ben Okma, Paulo da Silva Ribeiro, Chris Rizzos, A. Thete, G. Vacanti, S. Verhoeckx, M. Vervest, R. Visser, L. Voruz, M. Bavdaz, E. Wille, I. Ferreira, M. Olde Riekerink, J. Haneveld, Arenda Koelewijn, Maurice Wijnperlé, J. Lankwarden, B. Schurink, R. Start, C. van Baren, J. D. den Herder, E. Handick, M. Krumrey, V. Burwitz, S. Massahi, D. Ferreira, S. Svendsen, F. Christensen, William Mundon, G. Phillips
Athena is the European Space Agency’s next flagship x-ray telescope, scheduled for launch in the 2030s. Its 2.5-m diameter mirror will be segmented and comprise more than 600 individual Silicon Pore Optics (SPO) grazing-incidence-angle imagers, called mirror modules. Arranged in concentric annuli and following a Wolter-Schwartzschild design, the mirror modules are made of several tens of primary-secondary mirror pairs, each mirror made of mono-crystalline silicon, coated to increase the collective area of the system, and shaped to bring the incoming photons to a common focus 12 m away. Aiming to deliver a half-energy width of 5”, and an effective area of about 1.4 m2 at 1 keV, the Athena mirror requires several hundred m2 of super-polished surfaces with a roughness of about 0.3 nm and a thickness of just 110 µm. SPO, using the highest-grade double-side polished 300 mm wafers commercially available, were invented for this purpose and have been consistently developed over the last several years to enable next-generation x-ray telescopes like Athena. SPO makes it possible to manufacture cost-effective, high-resolution, large-area x-ray optics by using all the advantages that mono-crystalline silicon and the mass production processes of the semiconductor industry provide. Ahead of important programmatic milestones for Athena, we present the status of the technology, and illustrate not only recent x-ray results but also the progress made on the environmental testing, manufacturing and assembly aspects of the technology.
{"title":"The development of the mirror for the Athena x-ray mission","authors":"M. Collon, Luis Abalo, N. Barrière, A. Bayerle, Luigi Castiglione, Noë Eenkhoorn, D. Girou, R. Günther, Enrico Hauser, Roy van der Hoeven, Jasper den Hollander, Yvette Jenkins, B. Landgraf, L. Keek, Ben Okma, Paulo da Silva Ribeiro, Chris Rizzos, A. Thete, G. Vacanti, S. Verhoeckx, M. Vervest, R. Visser, L. Voruz, M. Bavdaz, E. Wille, I. Ferreira, M. Olde Riekerink, J. Haneveld, Arenda Koelewijn, Maurice Wijnperlé, J. Lankwarden, B. Schurink, R. Start, C. van Baren, J. D. den Herder, E. Handick, M. Krumrey, V. Burwitz, S. Massahi, D. Ferreira, S. Svendsen, F. Christensen, William Mundon, G. Phillips","doi":"10.1117/12.2630775","DOIUrl":"https://doi.org/10.1117/12.2630775","url":null,"abstract":"Athena is the European Space Agency’s next flagship x-ray telescope, scheduled for launch in the 2030s. Its 2.5-m diameter mirror will be segmented and comprise more than 600 individual Silicon Pore Optics (SPO) grazing-incidence-angle imagers, called mirror modules. Arranged in concentric annuli and following a Wolter-Schwartzschild design, the mirror modules are made of several tens of primary-secondary mirror pairs, each mirror made of mono-crystalline silicon, coated to increase the collective area of the system, and shaped to bring the incoming photons to a common focus 12 m away. Aiming to deliver a half-energy width of 5”, and an effective area of about 1.4 m2 at 1 keV, the Athena mirror requires several hundred m2 of super-polished surfaces with a roughness of about 0.3 nm and a thickness of just 110 µm. SPO, using the highest-grade double-side polished 300 mm wafers commercially available, were invented for this purpose and have been consistently developed over the last several years to enable next-generation x-ray telescopes like Athena. SPO makes it possible to manufacture cost-effective, high-resolution, large-area x-ray optics by using all the advantages that mono-crystalline silicon and the mass production processes of the semiconductor industry provide. Ahead of important programmatic milestones for Athena, we present the status of the technology, and illustrate not only recent x-ray results but also the progress made on the environmental testing, manufacturing and assembly aspects of the technology.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"12181 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":"129148621","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}
M. Hernanz, S. Brandt, J. I. in’t Zand, Y. Evangelista, A. Meuris, C. Tenzer, G. Zampa, P. Orleanski, E. Kalemci, Müberra Sungur, S. Schanne, F. Zwart, R. de la Rie, P. Laubert, C. van Baren, G. Aitink-Kroes, L. Kuiper, J. Bayer, P. Hedderman, S. Pliego, Hao Xiong, R. Campana, E. Del Monte, M. Feroci, F. Ceraudo, O. Gevin, I. Kuvvetli, D. Tcherniak, K. Skup, M. Michalska, W. Nowosielski, A. Hormaetxe, J. Galvez, P. Ferrés, A. Patruno, W. Bonvicini, M. Antonelli, M. Boezio, D. Cirrincione, R. Munini, A. Rachevski, A. Vacchi, N. Zampa, I. Rashevskaya, A. Argan, O. Turhan, Ayhan Bozkurt, A. Onat, E. Bozzo, A. Santangelo, Shuang-Nan Zhang, F. Lu, Yupeng Xu
The eXTP (enhanced x-ray timing and polarimetry) mission is a major project of the Chinese Academy of Sciences (CAS), with a large involvement of Europe. The scientific payload of eXTP includes four instruments: the SFA (spectroscopy focusing array) and the PFA (polarimetry focusing array)—led by China —the LAD (large area detector) and the WFM (wide field monitor)—led by Europe (Italy and Spain). They offer a unique simultaneous wide-band x-ray timing and polarimetry sensitivity. The WFM is a wide field x-ray monitor instrument in the 2-50 keV energy range, consisting of an array of six coded mask cameras with a field of view of 180°x90° at an angular resolution of 5 arcmin and four silicon drift detectors in each camera. Its unprecedented combination of large field of view and imaging down to 2 keV will allow eXTP to make important discoveries of the variable and transient x-ray sky and is essential in detecting transient black holes, that are part of the primary science goals of eXTP, so that they can be promptly followed up with other instruments on eXTP and elsewhere.
{"title":"The wide field monitor onboard the Chinese-European x-ray mission eXTP","authors":"M. Hernanz, S. Brandt, J. I. in’t Zand, Y. Evangelista, A. Meuris, C. Tenzer, G. Zampa, P. Orleanski, E. Kalemci, Müberra Sungur, S. Schanne, F. Zwart, R. de la Rie, P. Laubert, C. van Baren, G. Aitink-Kroes, L. Kuiper, J. Bayer, P. Hedderman, S. Pliego, Hao Xiong, R. Campana, E. Del Monte, M. Feroci, F. Ceraudo, O. Gevin, I. Kuvvetli, D. Tcherniak, K. Skup, M. Michalska, W. Nowosielski, A. Hormaetxe, J. Galvez, P. Ferrés, A. Patruno, W. Bonvicini, M. Antonelli, M. Boezio, D. Cirrincione, R. Munini, A. Rachevski, A. Vacchi, N. Zampa, I. Rashevskaya, A. Argan, O. Turhan, Ayhan Bozkurt, A. Onat, E. Bozzo, A. Santangelo, Shuang-Nan Zhang, F. Lu, Yupeng Xu","doi":"10.1117/12.2628335","DOIUrl":"https://doi.org/10.1117/12.2628335","url":null,"abstract":"The eXTP (enhanced x-ray timing and polarimetry) mission is a major project of the Chinese Academy of Sciences (CAS), with a large involvement of Europe. The scientific payload of eXTP includes four instruments: the SFA (spectroscopy focusing array) and the PFA (polarimetry focusing array)—led by China —the LAD (large area detector) and the WFM (wide field monitor)—led by Europe (Italy and Spain). They offer a unique simultaneous wide-band x-ray timing and polarimetry sensitivity. The WFM is a wide field x-ray monitor instrument in the 2-50 keV energy range, consisting of an array of six coded mask cameras with a field of view of 180°x90° at an angular resolution of 5 arcmin and four silicon drift detectors in each camera. Its unprecedented combination of large field of view and imaging down to 2 keV will allow eXTP to make important discoveries of the variable and transient x-ray sky and is essential in detecting transient black holes, that are part of the primary science goals of eXTP, so that they can be promptly followed up with other instruments on eXTP and elsewhere.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"61 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":"128860735","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. Heilmann, A. Bruccoleri, V. Burwitz, P. Cheimets, C. DeRoo, A. Garner, E. Gullikson, H. M. Guenther, G. Hartner, E. Hertz, A. Langmeier, Thomas Mueller, S. Rukdee, T. Schmidt, Randall K. Smith, M. Schattenburg
High resolving power soft x-ray spectroscopy has been confirmed by the recent Astro2020 Decadal Survey as a high-priority strategic goal with R =λ/Δλ as high as 7500 for some science cases. Examples are the characterization of highly ionized gases in galaxy halos and within and around galaxy clusters, accretion onto supermassive black holes, coronal mass ejections and coronal heating. Below the level of an expensive strategic mission, but far exceeding current capabilities, falls the Arcus Grating Explorer mission concept, with a minimum R of 2500 (expected R = 3500) and effective area up to ∼ 300 cm2 in the 12-50 Å bandpass. Arcus relies on light-weight, high-efficiency, blazed and alignment-insensitive critical-angle transmission (CAT) gratings for dispersion. The mission calls for hundreds of ∼ 30×30 mm2 gratings with a hierarchy of integrated support structures. The most recent CAT gratings have been fabricated from 200 mm silicon-on-insulator wafers using commercial, volume production compatible tools from the semiconductor and MEMS industries. We report x-ray results from quasifully illuminated, co-aligned CAT gratings showing record-high R ∼ 1.3×104 in 18th order at Al-Kα wavelengths, and diffraction efficiency of blazed orders in agreement with pencil beam synchrotron measurements and model predictions at O-K. Tilt of the deep-etched, freestanding grating bars relative to the grating surface is measured and successfully compensated through angular alignment during bonding of the Si gratings to metal frames. We also report on updates to the Arcus resolving power error budget, and on post-fabrication thinning of grating bars, which could lead to increased diffraction efficiency.
{"title":"Flight-like critical-angle transmission grating x-ray performance for Arcus","authors":"R. Heilmann, A. Bruccoleri, V. Burwitz, P. Cheimets, C. DeRoo, A. Garner, E. Gullikson, H. M. Guenther, G. Hartner, E. Hertz, A. Langmeier, Thomas Mueller, S. Rukdee, T. Schmidt, Randall K. Smith, M. Schattenburg","doi":"10.1117/12.2628195","DOIUrl":"https://doi.org/10.1117/12.2628195","url":null,"abstract":"High resolving power soft x-ray spectroscopy has been confirmed by the recent Astro2020 Decadal Survey as a high-priority strategic goal with R =λ/Δλ as high as 7500 for some science cases. Examples are the characterization of highly ionized gases in galaxy halos and within and around galaxy clusters, accretion onto supermassive black holes, coronal mass ejections and coronal heating. Below the level of an expensive strategic mission, but far exceeding current capabilities, falls the Arcus Grating Explorer mission concept, with a minimum R of 2500 (expected R = 3500) and effective area up to ∼ 300 cm2 in the 12-50 Å bandpass. Arcus relies on light-weight, high-efficiency, blazed and alignment-insensitive critical-angle transmission (CAT) gratings for dispersion. The mission calls for hundreds of ∼ 30×30 mm2 gratings with a hierarchy of integrated support structures. The most recent CAT gratings have been fabricated from 200 mm silicon-on-insulator wafers using commercial, volume production compatible tools from the semiconductor and MEMS industries. We report x-ray results from quasifully illuminated, co-aligned CAT gratings showing record-high R ∼ 1.3×104 in 18th order at Al-Kα wavelengths, and diffraction efficiency of blazed orders in agreement with pencil beam synchrotron measurements and model predictions at O-K. Tilt of the deep-etched, freestanding grating bars relative to the grating surface is measured and successfully compensated through angular alignment during bonding of the Si gratings to metal frames. We also report on updates to the Arcus resolving power error budget, and on post-fabrication thinning of grating bars, which could lead to increased diffraction efficiency.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"12181 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":"130129363","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}
Five-hundred-meter Aperture Spherical radio Telescope (FAST) is the most sensitive single-dish telescope in the world. In the past few years since it was put into use, there have been some relatively important scientific research achievements in the fields of pulsars and Fast Radio Bursts (FRB). In the future, there may also be plans to build the FAST Array (FASTA) project, which will build 5 more telescopes similar to the aperture of the FAST in 5 different locations, and its ultra-high sensitivity will be benefited from the length of the baseline. With the upgrade of the project, the receiver system will be further upgraded. We plan to develop a digital backend of Phased Array Feed (PAF) with no less than 330 sampling units on the 1.2 diameter focal plane, the instantaneous bandwidth covers 0.6 to 1.8GHz, the system noise temperature is not higher than 25K, and simultaneous implement the real-time 90*2 digital beamforming.
{"title":"Development of key technologies of the radio astronomy phased array feed digital backend","authors":"Xinxin Zhang, R. Duan","doi":"10.1117/12.2629664","DOIUrl":"https://doi.org/10.1117/12.2629664","url":null,"abstract":"Five-hundred-meter Aperture Spherical radio Telescope (FAST) is the most sensitive single-dish telescope in the world. In the past few years since it was put into use, there have been some relatively important scientific research achievements in the fields of pulsars and Fast Radio Bursts (FRB). In the future, there may also be plans to build the FAST Array (FASTA) project, which will build 5 more telescopes similar to the aperture of the FAST in 5 different locations, and its ultra-high sensitivity will be benefited from the length of the baseline. With the upgrade of the project, the receiver system will be further upgraded. We plan to develop a digital backend of Phased Array Feed (PAF) with no less than 330 sampling units on the 1.2 diameter focal plane, the instantaneous bandwidth covers 0.6 to 1.8GHz, the system noise temperature is not higher than 25K, and simultaneous implement the real-time 90*2 digital beamforming.","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":"114324695","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}
L. Conti, J. Barnstedt, S. Diebold, Markus Höltzli, C. Kalkuhl, N. Kappelmann, T. Rauch, T. Schanz, B. Stelzer, Alexander Stock, K. Werner, H. Elsener, K. Meyer, D. Schaadt
We present the status of our imaging and photon counting UV-MCP detector versions, sensitive in the ultraviolet wavelength range. The detectors have a spatial resolution of 2k pixels per axis, are photon counting, have no readout noise and a very low dark rate, making it ideal for photometry and spectroscopy. The detector can be easily adapted to the requirements of different missions, e.g., only the mechanical interfaces and an electrical interface must be defined to integrate the detector, it is relatively lightweight (3 kg) and has a power consumption of only 15 W. For the sealed version of the detector, we are currently testing a sealed detector head with a cesium telluride photocathode in semitransparent mode. The open version of the detector uses a lightweight door mechanism and is currently optimized to use a KBr photocathode. Interesting advances have been made for AlGaN on MgF2 and MgO substrates. A complete h-GaN film could be grown on MgO (0 0 1), and a complete c-GaN film on MgO (1 1 0). Good crystal quality is crucial to obtain a high QE AlGaN photocathode. Finally, the challenges towards a sealed detector head with a diameter of about 8 cm are described. By rotating the detector window on the detector head during the sealing process, we were able to seal the detector. The photocathode in the sealed MCP detector is stable for at least weeks.
{"title":"A photon counting imaging detector for UV space missions","authors":"L. Conti, J. Barnstedt, S. Diebold, Markus Höltzli, C. Kalkuhl, N. Kappelmann, T. Rauch, T. Schanz, B. Stelzer, Alexander Stock, K. Werner, H. Elsener, K. Meyer, D. Schaadt","doi":"10.1117/12.2628735","DOIUrl":"https://doi.org/10.1117/12.2628735","url":null,"abstract":"We present the status of our imaging and photon counting UV-MCP detector versions, sensitive in the ultraviolet wavelength range. The detectors have a spatial resolution of 2k pixels per axis, are photon counting, have no readout noise and a very low dark rate, making it ideal for photometry and spectroscopy. The detector can be easily adapted to the requirements of different missions, e.g., only the mechanical interfaces and an electrical interface must be defined to integrate the detector, it is relatively lightweight (3 kg) and has a power consumption of only 15 W. For the sealed version of the detector, we are currently testing a sealed detector head with a cesium telluride photocathode in semitransparent mode. The open version of the detector uses a lightweight door mechanism and is currently optimized to use a KBr photocathode. Interesting advances have been made for AlGaN on MgF2 and MgO substrates. A complete h-GaN film could be grown on MgO (0 0 1), and a complete c-GaN film on MgO (1 1 0). Good crystal quality is crucial to obtain a high QE AlGaN photocathode. Finally, the challenges towards a sealed detector head with a diameter of about 8 cm are described. By rotating the detector window on the detector head during the sealing process, we were able to seal the detector. The photocathode in the sealed MCP detector is stable for at least weeks.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"14 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":"126755656","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. Steinhebel, H. Fleischhack, N. Striebig, Manoj Jadhav, Y. Suda, R. Luz, C. Kierans, R. Caputo, H. Tajima, R. Leys, I. Perić, J. Metcalfe, J. Perkins
Space-based γ-ray telescopes such as the Fermi Large Area Telescope have used single sided silicon strip detectors to track secondary charged particles produced by primary γ-rays with high resolution. At the lower energies targeted by keV-MeV telescopes, two dimensional position information within a single detector is required for event reconstruction—especially in the Compton regime. This work describes the development of monolithic CMOS active pixel silicon sensors—AstroPix—as a novel technology for use in future γ-ray telescopes. Based upon sensors (ATLASPix) designed for use in the ATLAS detector at the Large Hadron Collider, AstroPix has the potential to maintain high performance while reducing noise with low power consumption. This is achieved with the dual detection and readout capabilities in each CMOS pixel. The status of AstroPix development and testing, as well as outlook for future testing and application, will be presented.
{"title":"AstroPix: novel monolithic active pixel silicon sensors for future gamma-ray telescopes","authors":"A. Steinhebel, H. Fleischhack, N. Striebig, Manoj Jadhav, Y. Suda, R. Luz, C. Kierans, R. Caputo, H. Tajima, R. Leys, I. Perić, J. Metcalfe, J. Perkins","doi":"10.1117/12.2630405","DOIUrl":"https://doi.org/10.1117/12.2630405","url":null,"abstract":"Space-based γ-ray telescopes such as the Fermi Large Area Telescope have used single sided silicon strip detectors to track secondary charged particles produced by primary γ-rays with high resolution. At the lower energies targeted by keV-MeV telescopes, two dimensional position information within a single detector is required for event reconstruction—especially in the Compton regime. This work describes the development of monolithic CMOS active pixel silicon sensors—AstroPix—as a novel technology for use in future γ-ray telescopes. Based upon sensors (ATLASPix) designed for use in the ATLAS detector at the Large Hadron Collider, AstroPix has the potential to maintain high performance while reducing noise with low power consumption. This is achieved with the dual detection and readout capabilities in each CMOS pixel. The status of AstroPix development and testing, as well as outlook for future testing and application, will be presented.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"26 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":"115699100","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}
T. Nikola, Steve K. Choi, C. Duell, R. Freundt, Z. Huber, Yaqiong Li, Kshama Malavalli, M. Niemack, K. Rossi, G. Stacey, E. Vavagiakis, B. Zou, N. Cothard, J. Austermann, J. Wheeler, Jiansong Gao, M. Vissers, J. Hubmayr, J. Beall, J. Ullom
The Fred Young Submillimeter Telescope (FYST), which is the telescope of the CCAT-prime project, will be located at 5600 m near the summit of Cerro Chajnantor in northern Chile, and will host the modular instrument called Prime-Cam. Two of the instrument modules in Prime-Cam will be a spectrometer with a resolving power of R ∼ 100 and populated with a detector array of several thousand KIDs (Kinetic Inductance Detectors). The main science goal of this spectrometer module, called EoR-Spec, is to probe the Epoch of Reionization (EoR) in the early universe using the Line Intensity Mapping (LIM) technique with the redshifted [CII] fine-structure line. This presentation provides an overview of the optical, mechanical, and spectral design of EoR-Spec, as well as of the detector array that will be used. The optical design consists of four silicon lenses that have anti-reflection metamaterial layers. A scanning Fabry-Perot Interferometer (FPI) will be located at the pupil and provides the spectral resolution over the full spectral coverage of 210 GHz to 420 GHz in two orders, resulting in a redshift coverage of the [CII] line from z = 3.5 to z = 8. The detector array consists of three subarrays of KIDs, two of which are tuned for the frequency range between 210 GHz and 315 GHz, and one that is tuned for the 315 GHz to 420 GHz range. The angular resolution will be between about 30′′ to 50′′. This presentation also addresses the spectral and spatial scanning strategy of EoR-Spec on FYST. EoR-Spec is expected to be installed into Prime-Cam about 1 year after first light of FYST.
{"title":"CCAT-prime: the epoch reionization spectrometer for primce-cam on FYST","authors":"T. Nikola, Steve K. Choi, C. Duell, R. Freundt, Z. Huber, Yaqiong Li, Kshama Malavalli, M. Niemack, K. Rossi, G. Stacey, E. Vavagiakis, B. Zou, N. Cothard, J. Austermann, J. Wheeler, Jiansong Gao, M. Vissers, J. Hubmayr, J. Beall, J. Ullom","doi":"10.1117/12.2629338","DOIUrl":"https://doi.org/10.1117/12.2629338","url":null,"abstract":"The Fred Young Submillimeter Telescope (FYST), which is the telescope of the CCAT-prime project, will be located at 5600 m near the summit of Cerro Chajnantor in northern Chile, and will host the modular instrument called Prime-Cam. Two of the instrument modules in Prime-Cam will be a spectrometer with a resolving power of R ∼ 100 and populated with a detector array of several thousand KIDs (Kinetic Inductance Detectors). The main science goal of this spectrometer module, called EoR-Spec, is to probe the Epoch of Reionization (EoR) in the early universe using the Line Intensity Mapping (LIM) technique with the redshifted [CII] fine-structure line. This presentation provides an overview of the optical, mechanical, and spectral design of EoR-Spec, as well as of the detector array that will be used. The optical design consists of four silicon lenses that have anti-reflection metamaterial layers. A scanning Fabry-Perot Interferometer (FPI) will be located at the pupil and provides the spectral resolution over the full spectral coverage of 210 GHz to 420 GHz in two orders, resulting in a redshift coverage of the [CII] line from z = 3.5 to z = 8. The detector array consists of three subarrays of KIDs, two of which are tuned for the frequency range between 210 GHz and 315 GHz, and one that is tuned for the 315 GHz to 420 GHz range. The angular resolution will be between about 30′′ to 50′′. This presentation also addresses the spectral and spatial scanning strategy of EoR-Spec on FYST. EoR-Spec is expected to be installed into Prime-Cam about 1 year after first light of FYST.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"26 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":"125499835","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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