C. Rooney, Bo Peng, G. Stacey, T. Nikola, A. Vishwas, C. Ferkinhoff, C. Ball, C. Lamarche, J. Higdon, S. Higdon
We present recent developments on Cornell’s 2nd generation z (redshift) and Early Universe Spectrometer (ZEUS-2). ZEUS-2 is a long-slit echelle-grating spectrometer, originally implemented to deliver R∼1000 spectroscopy in the 350-, and 450-micron telluric windows using NIST Transition-Edge Sensed (TES) bolometer arrays. We have expanded its capabilities to also cover the 200-micron window, and present first-light data for the new array from our 2019 observing campaign on the Atacama Pathfinder EXperiment (APEX) telescope. We also discuss the various enhancements we have implemented to improve observing efficiency and noise performance, including identifying and mitigating vibrations in hardware and improving the stability and robustness of the control software for the detector temperature. Furthermore, we have implemented several software routines to interface with the telescope control systems. These improvements, demonstrated during our recent observing campaign in Nov-Dec 2021, resulted in enhanced reliability and ease of operation, as well as increased sensitivity. A data-driven software pipeline, leveraging data from all 300 detectors on the array to remove common-mode noise, was implemented, and noise performance was further improved by robustly detecting unstable detectors and disabling them during observations.
{"title":"Recent developments with Cornell’s ZEUS-2 spectrometer at APEX","authors":"C. Rooney, Bo Peng, G. Stacey, T. Nikola, A. Vishwas, C. Ferkinhoff, C. Ball, C. Lamarche, J. Higdon, S. Higdon","doi":"10.1117/12.2629453","DOIUrl":"https://doi.org/10.1117/12.2629453","url":null,"abstract":"We present recent developments on Cornell’s 2nd generation z (redshift) and Early Universe Spectrometer (ZEUS-2). ZEUS-2 is a long-slit echelle-grating spectrometer, originally implemented to deliver R∼1000 spectroscopy in the 350-, and 450-micron telluric windows using NIST Transition-Edge Sensed (TES) bolometer arrays. We have expanded its capabilities to also cover the 200-micron window, and present first-light data for the new array from our 2019 observing campaign on the Atacama Pathfinder EXperiment (APEX) telescope. We also discuss the various enhancements we have implemented to improve observing efficiency and noise performance, including identifying and mitigating vibrations in hardware and improving the stability and robustness of the control software for the detector temperature. Furthermore, we have implemented several software routines to interface with the telescope control systems. These improvements, demonstrated during our recent observing campaign in Nov-Dec 2021, resulted in enhanced reliability and ease of operation, as well as increased sensitivity. A data-driven software pipeline, leveraging data from all 300 detectors on the array to remove common-mode noise, was implemented, and noise performance was further improved by robustly detecting unstable detectors and disabling them during observations.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"54 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":"116527702","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. Mori, H. Tomida, H. Nakajima, T. Okajima, H. Noda, Takaaki Tanaka, H. Uchida, K. Hagino, S. Kobayashi, Hiromasa Suzuki, Tessei Yoshida, H. Murakami, H. Uchiyama, M. Nobukawa, K. Nobukawa, T. Yoneyama, H. Matsumoto, T. Tsuru, M. Yamauchi, I. Hatsukade, M. Ishida, Y. Maeda, T. Hayashi, K. Tamura, R. Boissay-Malaquin, Toshiki Sato, J. Hiraga, T. Kohmura, K. Yamaoka, T. Dotani, M. Ozaki, H. Tsunemi, Y. Kanemaru, J. Sato, Toshiyuki Takaki, Yuta Terada, Keitaro Miyazaki, Kohei Kusunoki, Y. Otsuka, Haruhiko Yokosu, Wakana Yonemaru, Yoh Asahina, K. Asakura, M. Yoshimoto, Yuichi Ode, J. Sato, T. Hakamata, Mio Aoyagi, Yuma Aoki, Shun Tsunomachi, T. Doi, D. Aoki, Kaito Fujisawa, Masatoshi Kitajima, K. Hayashida
Xtend is a soft x-ray imaging telescope developed for the x-ray imaging and spectroscopy mission (XRISM). XRISM is scheduled to be launched in the Japanese fiscal year 2022. Xtend consists of the soft x-ray imager (SXI), an x-ray CCD camera, and the x-ray mirror assembly (XMA), a thin-foil-nested conically approximated Wolter-I optics. The SXI uses the P-channel, back-illuminated type CCD with an imaging area size of 31mm on a side. The four CCD chips are arranged in a 2×2 grid and can be cooled down to −120 °C with a single-stage Stirling cooler. The XMA nests thin aluminum foils coated with gold in a confocal way with an outer diameter of 45 cm. A pre-collimator is installed in front of the x-ray mirror for the reduction of the stray light. Combining the SXI and XMA with a focal length of 5.6m, a field of view of 38′ × 38′ over the energy range from 0.4 to 13 keV is realized. We have completed the fabrication of the flight model of both SXI and XMA. The performance verification has been successfully conducted in a series of sub-system level tests. We also carried out on-ground calibration measurements and the data analysis is ongoing.
{"title":"Xtend, the soft x-ray imaging telescope for the X-Ray Imaging and Spectroscopy Mission (XRISM)","authors":"K. Mori, H. Tomida, H. Nakajima, T. Okajima, H. Noda, Takaaki Tanaka, H. Uchida, K. Hagino, S. Kobayashi, Hiromasa Suzuki, Tessei Yoshida, H. Murakami, H. Uchiyama, M. Nobukawa, K. Nobukawa, T. Yoneyama, H. Matsumoto, T. Tsuru, M. Yamauchi, I. Hatsukade, M. Ishida, Y. Maeda, T. Hayashi, K. Tamura, R. Boissay-Malaquin, Toshiki Sato, J. Hiraga, T. Kohmura, K. Yamaoka, T. Dotani, M. Ozaki, H. Tsunemi, Y. Kanemaru, J. Sato, Toshiyuki Takaki, Yuta Terada, Keitaro Miyazaki, Kohei Kusunoki, Y. Otsuka, Haruhiko Yokosu, Wakana Yonemaru, Yoh Asahina, K. Asakura, M. Yoshimoto, Yuichi Ode, J. Sato, T. Hakamata, Mio Aoyagi, Yuma Aoki, Shun Tsunomachi, T. Doi, D. Aoki, Kaito Fujisawa, Masatoshi Kitajima, K. Hayashida","doi":"10.1117/12.2626894","DOIUrl":"https://doi.org/10.1117/12.2626894","url":null,"abstract":"Xtend is a soft x-ray imaging telescope developed for the x-ray imaging and spectroscopy mission (XRISM). XRISM is scheduled to be launched in the Japanese fiscal year 2022. Xtend consists of the soft x-ray imager (SXI), an x-ray CCD camera, and the x-ray mirror assembly (XMA), a thin-foil-nested conically approximated Wolter-I optics. The SXI uses the P-channel, back-illuminated type CCD with an imaging area size of 31mm on a side. The four CCD chips are arranged in a 2×2 grid and can be cooled down to −120 °C with a single-stage Stirling cooler. The XMA nests thin aluminum foils coated with gold in a confocal way with an outer diameter of 45 cm. A pre-collimator is installed in front of the x-ray mirror for the reduction of the stray light. Combining the SXI and XMA with a focal length of 5.6m, a field of view of 38′ × 38′ over the energy range from 0.4 to 13 keV is realized. We have completed the fabrication of the flight model of both SXI and XMA. The performance verification has been successfully conducted in a series of sub-system level tests. We also carried out on-ground calibration measurements and the data analysis is ongoing.","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":"122825356","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. Poulson, P. Bloser, K. Ogasawara, C. Lemire, J. A. Trevino, J. Legere, J. Ryan, M. McConnell
Observing cosmic sources in the medium-energy gamma-ray regime (~0.4 – 10 MeV) requires an efficient instrument with good angular resolution and background rejection. Artificial single-crystal diamond detectors (SCDDs) have comparable energy ranges, energy resolution, and threshold levels as traditional silicon solid-state detectors (SSDs), but with faster rise times (~1 ns), improved radiation hardness, and are generally insensitive to light and temperature. Here we present work preliminary to the pairing of artificial single-crystal diamond detectors (SCDDs) with CeBr3 calorimeters to produce a prototype Compton telescope.
{"title":"Using single-crystal diamond detectors as a scattering medium in Compton telescopes","authors":"D. Poulson, P. Bloser, K. Ogasawara, C. Lemire, J. A. Trevino, J. Legere, J. Ryan, M. McConnell","doi":"10.1117/12.2628997","DOIUrl":"https://doi.org/10.1117/12.2628997","url":null,"abstract":"Observing cosmic sources in the medium-energy gamma-ray regime (~0.4 – 10 MeV) requires an efficient instrument with good angular resolution and background rejection. Artificial single-crystal diamond detectors (SCDDs) have comparable energy ranges, energy resolution, and threshold levels as traditional silicon solid-state detectors (SSDs), but with faster rise times (~1 ns), improved radiation hardness, and are generally insensitive to light and temperature. Here we present work preliminary to the pairing of artificial single-crystal diamond detectors (SCDDs) with CeBr3 calorimeters to produce a prototype Compton telescope.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"43 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":"122870201","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}
J. Wheeler, J. Austermann, M. Vissers, J. Beall, Jiansong Gao, J. Imrek, E. Heilweil, D. Bennett, J. Gard, J. van Lanen, J. Hubmayr, J. Ullom
The development of direct absorbing kinetic inductance detectors (KIDs) for broadband far-infrared (FIR) observations designed to meet the needs of present and future telescopes is presented. This development was initiated to investigate the potential for upgrading the High-resolution Airborne Wideband Camera Plus (HAWC+) instrument on the Stratospheric Observatory for Infrared Astronomy (SOFIA) with KIDs; but also has applications generally for FIR detectors. These detectors consist of backside-illuminated KIDs on a silicon substrate where the hybrid TiN/Al inductor forms a resistive wire grid with broadband absorption. Detectors can be configured to absorb in either one or two polarizations with a pixel filling factor of around 80%. A novel two-layer meta material anti-reflection coating, and a sub-quarter-wavelength backshort allow for greater than 85% detection efficiency over the ultra-wide 1 to 6 THz bandwidth. These detectors require no focal plane focusing optics such as feedhorns or microlenses, do not require fragile membranes, and utilize proven and straightforward fabrication methods. The optical and microwave design of these detectors is presented. Additionally, the performance of test devices is quantified. This includes measurements of the AR coating effectiveness, detector noise equivalent powers, and detector internal quality factors under the relevant loading levels for the HAWC+ instrument. This information is used to assess the potential benefit of upgrading the HAWC+ instrument with these new detectors and to determine the applicability of this technology for other future FIR detectors.
{"title":"Broadband kinetic inductance detectors for far-IR observations","authors":"J. Wheeler, J. Austermann, M. Vissers, J. Beall, Jiansong Gao, J. Imrek, E. Heilweil, D. Bennett, J. Gard, J. van Lanen, J. Hubmayr, J. Ullom","doi":"10.1117/12.2630672","DOIUrl":"https://doi.org/10.1117/12.2630672","url":null,"abstract":"The development of direct absorbing kinetic inductance detectors (KIDs) for broadband far-infrared (FIR) observations designed to meet the needs of present and future telescopes is presented. This development was initiated to investigate the potential for upgrading the High-resolution Airborne Wideband Camera Plus (HAWC+) instrument on the Stratospheric Observatory for Infrared Astronomy (SOFIA) with KIDs; but also has applications generally for FIR detectors. These detectors consist of backside-illuminated KIDs on a silicon substrate where the hybrid TiN/Al inductor forms a resistive wire grid with broadband absorption. Detectors can be configured to absorb in either one or two polarizations with a pixel filling factor of around 80%. A novel two-layer meta material anti-reflection coating, and a sub-quarter-wavelength backshort allow for greater than 85% detection efficiency over the ultra-wide 1 to 6 THz bandwidth. These detectors require no focal plane focusing optics such as feedhorns or microlenses, do not require fragile membranes, and utilize proven and straightforward fabrication methods. The optical and microwave design of these detectors is presented. Additionally, the performance of test devices is quantified. This includes measurements of the AR coating effectiveness, detector noise equivalent powers, and detector internal quality factors under the relevant loading levels for the HAWC+ instrument. This information is used to assess the potential benefit of upgrading the HAWC+ instrument with these new detectors and to determine the applicability of this technology for other future FIR detectors.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"96 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":"128449828","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. Rodriguez, A. Adami, A. Aliane, X. de la Broïse, C. Delisle, A. Demonti, D. Desforge, S. Dubos, L. Dussopt, C. Gennet, V. Goudon, O. Gevin, H. Kaya, G. Lasfargues, J. Martignac, X. Navick, A. Poglitsch, V. Révéret, M. Sauvage, T. Tollet, F. Visticot
One of the main goals of the canceled Space Infrared Telescope for Cosmology and Astrophysics (SPICA), was to reveal the evidence of the influence of magnetic field in the structuration of different astrophysical objects, as for example the filamentary structure of star-forming regions. For this purpose, “instrument-in-pixel” detector arrays were developed under ESA, CNES and FOCUS contracts, to propose sensitive, compact and easy to integrate detection solutions for a Space Observatory. Magnetic field influences the light emission or absorption of small grains and molecules imprinting its characteristics in the received electromagnetic message in terms of polarization, degree, angle and intensity. Each pixel of the developed detectors absorb the radiation through two orthogonal dipole networks. The detector array is organized like a chessboard with every other pixel having absorbers rotated by 45° in order to unveil simultaneously the linear Stokes parameters without any optical loss. A very large absorption efficiency is obtained, as usual since PACS detectors, by a backshort-under-grid scheme. To obtain the goal sensitivity of 1 attoW/√Hz, detectors are cooled to 50 mK and linked to an Above IC CMOS readout circuit. For each pixel, four interleaved spiral silicon sensors gather the absorber power. They are organized in a Wheatstone bridge configuration that allows fully differential outputs: total power and polarization unbalanced intensity.
{"title":"Highly sensitive and wide dynamic range polarimetric detectors arrays in the submillimeter domain","authors":"L. Rodriguez, A. Adami, A. Aliane, X. de la Broïse, C. Delisle, A. Demonti, D. Desforge, S. Dubos, L. Dussopt, C. Gennet, V. Goudon, O. Gevin, H. Kaya, G. Lasfargues, J. Martignac, X. Navick, A. Poglitsch, V. Révéret, M. Sauvage, T. Tollet, F. Visticot","doi":"10.1117/12.2630223","DOIUrl":"https://doi.org/10.1117/12.2630223","url":null,"abstract":"One of the main goals of the canceled Space Infrared Telescope for Cosmology and Astrophysics (SPICA), was to reveal the evidence of the influence of magnetic field in the structuration of different astrophysical objects, as for example the filamentary structure of star-forming regions. For this purpose, “instrument-in-pixel” detector arrays were developed under ESA, CNES and FOCUS contracts, to propose sensitive, compact and easy to integrate detection solutions for a Space Observatory. Magnetic field influences the light emission or absorption of small grains and molecules imprinting its characteristics in the received electromagnetic message in terms of polarization, degree, angle and intensity. Each pixel of the developed detectors absorb the radiation through two orthogonal dipole networks. The detector array is organized like a chessboard with every other pixel having absorbers rotated by 45° in order to unveil simultaneously the linear Stokes parameters without any optical loss. A very large absorption efficiency is obtained, as usual since PACS detectors, by a backshort-under-grid scheme. To obtain the goal sensitivity of 1 attoW/√Hz, detectors are cooled to 50 mK and linked to an Above IC CMOS readout circuit. For each pixel, four interleaved spiral silicon sensors gather the absorber power. They are organized in a Wheatstone bridge configuration that allows fully differential outputs: total power and polarization unbalanced intensity.","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":"130338518","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. Herrmann, R. Andritschke, M. Bonholzer, G. Hauser, Mie S. Magelund, J. Müller-Seidlitz, J. Reiffers
The wide field imager (WFI) for the ATHENA mission will enable the spectroscopic investigation of solid angles up to 40’ in the x-ray regime between 0.2 keV to 15 keV. The required sensors are planed as DEPFET (DEpleted P-channel field-effect transistor) active pixel matrices. These are readout by custom-designed ASICs called VERITAS in a rolling shutter mode. After column parallel processing of the analog signals row-by-row, the resulting pulse heights are multiplexed onto a differential analog line pair. Thus a transmission undisturbed from external influences is achieved. But successive signals can be affected by the limited rise-time of the VERITAS output stage, depending on the signal height, the multiplexing time and the cable length. In order to investigate the impact on the measurements a dedicated cable harness is used during the characterization of a prototype device. The characterizations are performed using either test pulses applied to the VERITAS or with a 55Fe calibration source illuminating the whole sensor. Different cable lengths and multiplexing times are tested to determine the influences. In order to deal with this effect a crosstalk correction algorithm is implemented for the analysis of the photon data. The determined crosstalk factors range up to 2.8% for the longest measured cablings of 2 m with the shortest multiplexing time. Using shorter cables and longer multiplexing times these factors can be reduced to below 1%. In all cases the accompanying effects in the data analysis can be corrected using the developed algorithm.
{"title":"Mitigation of bandwidth limitation induced crosstalk on Athena's WFI","authors":"M. Herrmann, R. Andritschke, M. Bonholzer, G. Hauser, Mie S. Magelund, J. Müller-Seidlitz, J. Reiffers","doi":"10.1117/12.2629620","DOIUrl":"https://doi.org/10.1117/12.2629620","url":null,"abstract":"The wide field imager (WFI) for the ATHENA mission will enable the spectroscopic investigation of solid angles up to 40’ in the x-ray regime between 0.2 keV to 15 keV. The required sensors are planed as DEPFET (DEpleted P-channel field-effect transistor) active pixel matrices. These are readout by custom-designed ASICs called VERITAS in a rolling shutter mode. After column parallel processing of the analog signals row-by-row, the resulting pulse heights are multiplexed onto a differential analog line pair. Thus a transmission undisturbed from external influences is achieved. But successive signals can be affected by the limited rise-time of the VERITAS output stage, depending on the signal height, the multiplexing time and the cable length. In order to investigate the impact on the measurements a dedicated cable harness is used during the characterization of a prototype device. The characterizations are performed using either test pulses applied to the VERITAS or with a 55Fe calibration source illuminating the whole sensor. Different cable lengths and multiplexing times are tested to determine the influences. In order to deal with this effect a crosstalk correction algorithm is implemented for the analysis of the photon data. The determined crosstalk factors range up to 2.8% for the longest measured cablings of 2 m with the shortest multiplexing time. Using shorter cables and longer multiplexing times these factors can be reduced to below 1%. In all cases the accompanying effects in the data analysis can be corrected using the developed algorithm.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"4 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":"114561307","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. Coutinho, M. Ramos-Ceja, K. Dennerl, F. Haberl, N. Meidinger, A. Merloni, P. Predehl, I. Stewart, M. Freyberg, W. Bornemann, H. Brunner, V. Burwitz, S. Czesla, J. Eder, S. Friedrich, R. Gaida, A. Gueguen, G. Hartner, W. Kink, I. Kreykenbohm, G. Lamer, C. Maitra, T. Mernik, S. Mueller, P. Nandra, E. Pfeffermann, J. Robrade
eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the soft X-ray scientific payload on board the SRG (Spektrum-Roentgen-Gamma) mission. It was successfully launched from Baikonur in July 2019. Following a 101 days cruise phase, SRG reached its final orbit around the Sun-Earth Lagrangian point L2, from where it has carried out already four full-sky surveys. eROSITA is a complex instrument composed of seven identical co-aligned X-ray telescopes with a focal length of 1600mm and an aperture of 350mm. Each telescope is equipped with an independent CCD camera. The cold redundant ITC (Interface and Thermal Controller) manages all seven cameras as well as the thermal control of the telescope and the interface to the spacecraft. The cruise phase of SRG was used to verify that all systems had survived launch and no degradation in the functionality was present. Following that, the main science mission, comprised of an early Calibration and Performance Verification Phase, followed by the all-sky survey. This paper presents the performance of the eROSITA telescope during the first four complete all-sky surveys. It presents the challenges encountered during the telescope operations as well as the operations and mitigation strategies put in place to understand or minimize the effects of the space environment in L2, such as micrometeoroid hits and radiation damage of the detectors.
{"title":"SRG/eROSITA status and operations during the first four all-sky surveys","authors":"D. Coutinho, M. Ramos-Ceja, K. Dennerl, F. Haberl, N. Meidinger, A. Merloni, P. Predehl, I. Stewart, M. Freyberg, W. Bornemann, H. Brunner, V. Burwitz, S. Czesla, J. Eder, S. Friedrich, R. Gaida, A. Gueguen, G. Hartner, W. Kink, I. Kreykenbohm, G. Lamer, C. Maitra, T. Mernik, S. Mueller, P. Nandra, E. Pfeffermann, J. Robrade","doi":"10.1117/12.2628946","DOIUrl":"https://doi.org/10.1117/12.2628946","url":null,"abstract":"eROSITA (extended ROentgen Survey with an Imaging Telescope Array) is the soft X-ray scientific payload on board the SRG (Spektrum-Roentgen-Gamma) mission. It was successfully launched from Baikonur in July 2019. Following a 101 days cruise phase, SRG reached its final orbit around the Sun-Earth Lagrangian point L2, from where it has carried out already four full-sky surveys. eROSITA is a complex instrument composed of seven identical co-aligned X-ray telescopes with a focal length of 1600mm and an aperture of 350mm. Each telescope is equipped with an independent CCD camera. The cold redundant ITC (Interface and Thermal Controller) manages all seven cameras as well as the thermal control of the telescope and the interface to the spacecraft. The cruise phase of SRG was used to verify that all systems had survived launch and no degradation in the functionality was present. Following that, the main science mission, comprised of an early Calibration and Performance Verification Phase, followed by the all-sky survey. This paper presents the performance of the eROSITA telescope during the first four complete all-sky surveys. It presents the challenges encountered during the telescope operations as well as the operations and mitigation strategies put in place to understand or minimize the effects of the space environment in L2, such as micrometeoroid hits and radiation damage of the detectors.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"43 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":"132517152","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}
Kinetic inductance detectors (KID) have great potential in astronomical observation, such as searching for exoplanets, because of their low noise, fast response and photon counting characteristics. In this paper, we present the design process and simulation results of a microstrip line coupled KIDs array for near-infrared astronomical observation. Compared with coplanar waveguide (CPW) feedlines, microstrip feedlines do not require air bridges, which simplify fabrication process. In the design part, we mainly focus on the impedance transforming networks, the KID structure, and the frequency crosstalk simulations. The test array has a total of 104 resonators with 8 rows and 13 columns, which ranges from 4.899 GHz to 6.194 GHz. The pitch size is about 200 µm and the frequency crosstalk is less than 50 kHz in simulation.
{"title":"Design of microstrip-line coupled kinetic inductance detectors for near infrared astronomy","authors":"Shilin Yu, S. Shu, R. Duan, Lihui Yang, Di Li","doi":"10.1117/12.2629154","DOIUrl":"https://doi.org/10.1117/12.2629154","url":null,"abstract":"Kinetic inductance detectors (KID) have great potential in astronomical observation, such as searching for exoplanets, because of their low noise, fast response and photon counting characteristics. In this paper, we present the design process and simulation results of a microstrip line coupled KIDs array for near-infrared astronomical observation. Compared with coplanar waveguide (CPW) feedlines, microstrip feedlines do not require air bridges, which simplify fabrication process. In the design part, we mainly focus on the impedance transforming networks, the KID structure, and the frequency crosstalk simulations. The test array has a total of 104 resonators with 8 rows and 13 columns, which ranges from 4.899 GHz to 6.194 GHz. The pitch size is about 200 µm and the frequency crosstalk is less than 50 kHz in simulation.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"17 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":"129999936","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. Asakura, K. Hayashida, S. Sakuma, A. Ishikura, K. Sawagami, W. Kamogawa, T. Yoneyama, H. Noda, K. Okazaki, M. Hanaoka, K. Hattori, Yusuke Matsushita, T. Mineta, M. Yoshimoto, Yuichi Ode, T. Hakamata, H. Matsumoto, H. Tsunemi
We have developed a novel x-ray interferometer, multi-image x-ray interferometer module (MIXIM), comprised of a fine aperture mask and an x-ray detector. The angular resolution of this system can be improved with an increase of the distance between two components or a decrease of the aperture size. Although MIXIM has already achieved an angular resolution of less than 0.1” by applying the Talbot effect with a periodic multi-pinhole mask, there remains the issue that its low opening fraction of 1.3% decreases the effective area of the imaging system. Therefore, we newly introduced periodic coded aperture masks which have opening fractions of about 50% instead of the multi-pinhole mask. Conducting an experiment with a 12.4 keV parallel x-ray beam, we successfully demonstrated that the periodic coded aperture could form the self-image, and obtained the x-ray source profile with sub-arcsecond angular resolution by deciphering the coded pattern. The effective area increases about 25 times compared with the multi-pinhole mask by the introduction of the periodic coded aperture masks, which indicates that this novel method can be effective for addressing the problem.
{"title":"Sub-arcsecond x-ray imaging with Multi-Image X-ray Interferometer Module (MIXIM): introduction of a periodic coded-aperture mask","authors":"K. Asakura, K. Hayashida, S. Sakuma, A. Ishikura, K. Sawagami, W. Kamogawa, T. Yoneyama, H. Noda, K. Okazaki, M. Hanaoka, K. Hattori, Yusuke Matsushita, T. Mineta, M. Yoshimoto, Yuichi Ode, T. Hakamata, H. Matsumoto, H. Tsunemi","doi":"10.1117/12.2629656","DOIUrl":"https://doi.org/10.1117/12.2629656","url":null,"abstract":"We have developed a novel x-ray interferometer, multi-image x-ray interferometer module (MIXIM), comprised of a fine aperture mask and an x-ray detector. The angular resolution of this system can be improved with an increase of the distance between two components or a decrease of the aperture size. Although MIXIM has already achieved an angular resolution of less than 0.1” by applying the Talbot effect with a periodic multi-pinhole mask, there remains the issue that its low opening fraction of 1.3% decreases the effective area of the imaging system. Therefore, we newly introduced periodic coded aperture masks which have opening fractions of about 50% instead of the multi-pinhole mask. Conducting an experiment with a 12.4 keV parallel x-ray beam, we successfully demonstrated that the periodic coded aperture could form the self-image, and obtained the x-ray source profile with sub-arcsecond angular resolution by deciphering the coded pattern. The effective area increases about 25 times compared with the multi-pinhole mask by the introduction of the periodic coded aperture masks, which indicates that this novel method can be effective for addressing the problem.","PeriodicalId":137463,"journal":{"name":"Astronomical Telescopes + Instrumentation","volume":"48 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":"134277288","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. Woolf, A. Moiseev, A. Bolotnikov, N. Cannady, G. Carini, J. Krizmanic, J. Mitchell, B. Phlips, M. Sasaki, D. Shy, L. Smith, D. Thompson, E. Yates, K. Ziock, A. Zoglauer
In this paper we describe ProtoGECCO–a prototype instrument for the Galactic Explorer with a Coded aperture mask and Compton Telescope (GECCO). ProtoGECCO is comprised of two main imaging calorimeters. The top calorimeter is an array of cadmium zinc telluride (CZT); the bottom calorimeter is an array of high-light yield Gd3Al2Ga3O12:Ce (GAGG) fingers with silicon photomultiplier (SiPM) readout. The calorimeters are surrounded by a thallium-doped cesium iodide (CsI:Tl) active shield. ProtoGECCO employs the techniques of both coded aperture imaging and a Compton telescope. The main goals of the prototype are to further develop the instrument technology, thereby raising the technical readiness level (TRL), and to fly on a high-altitude balloon from Fort Sumner, NM. The results of this work are directly applicable to future space instruments that require detectors with large area; excellent spatial, energy, and angular resolution; and high detection efficiency. Such future missions will address problems in the MeV domain of gamma-ray astronomy—one of the most underexplored windows on the universe.
{"title":"Development of the balloon-borne Galactic Explorer Coded Aperture Mask and Compton Telescope (GECCO) prototype","authors":"R. Woolf, A. Moiseev, A. Bolotnikov, N. Cannady, G. Carini, J. Krizmanic, J. Mitchell, B. Phlips, M. Sasaki, D. Shy, L. Smith, D. Thompson, E. Yates, K. Ziock, A. Zoglauer","doi":"10.1117/12.2630681","DOIUrl":"https://doi.org/10.1117/12.2630681","url":null,"abstract":"In this paper we describe ProtoGECCO–a prototype instrument for the Galactic Explorer with a Coded aperture mask and Compton Telescope (GECCO). ProtoGECCO is comprised of two main imaging calorimeters. The top calorimeter is an array of cadmium zinc telluride (CZT); the bottom calorimeter is an array of high-light yield Gd3Al2Ga3O12:Ce (GAGG) fingers with silicon photomultiplier (SiPM) readout. The calorimeters are surrounded by a thallium-doped cesium iodide (CsI:Tl) active shield. ProtoGECCO employs the techniques of both coded aperture imaging and a Compton telescope. The main goals of the prototype are to further develop the instrument technology, thereby raising the technical readiness level (TRL), and to fly on a high-altitude balloon from Fort Sumner, NM. The results of this work are directly applicable to future space instruments that require detectors with large area; excellent spatial, energy, and angular resolution; and high detection efficiency. Such future missions will address problems in the MeV domain of gamma-ray astronomy—one of the most underexplored windows on the universe.","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":"131192723","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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