The Experts below are selected from a list of 327 Experts worldwide ranked by ideXlab platform
Shoji Tsunematsu - One of the best experts on this subject based on the ideXlab platform.
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porous plug phase separator and superfluid film flow Suppression System for the soft x ray spectrometer onboard astro h
Proceedings of SPIE, 2016Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Ikuyuki Mitsuishi, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Shoji TsunematsuAbstract:Suppression of super fluid helium flow is critical for the Soft X-ray Spectrometer onboard ASTRO-H (Hitomi). In nominal operation, a small helium gas flow of ~30 μg/s must be safely vented and a super fluid film flow must be sufficiently small <2 μg/s. To achieve a life time of the liquid helium, a porous plug phase separator and a film flow Suppression System composed of an orifice, a heat exchanger, and knife edge devices are employed. In this paper, design, on-ground testing results and in-orbit performance of the porous plug and the film flow Suppression System are described.
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flight model measurements of the porous plug and film flow Suppression System for the astro h soft x ray spectrometer dewar
Cryogenics, 2016Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Ikuyuki Mitsuishi, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Shoji TsunematsuAbstract:Abstract Flight model measurements of a porous plug phase separator and a film flow Suppression System for the ASTRO-H Soft X-ray Spectrometer dewar are described. ASTRO-H is the sixth Japanese astronomy satellite and will be launched in 2016. It carries the Soft X-ray Spectrometer consisting of an X-ray optic and an X-ray microcalorimeter System operated at 50 mK. Superfluid liquid He is employed as a part of the cooling System. A wide range of He flows from 28 μ g/s to 3.2 mg/s in various operation cases must be safely vented under zero gravity. At the same time, superfluid He film flow through the vent line must be suppressed to μ g/s in a nominal case to avoid extra loss of the liquid He. For this purpose, a porous plug phase separator together with a film flow Suppression System is installed. To verify its performance, the mass flow rates and the film flow rate of the flight model System were measured at component level. The mass flow rates at various He tank temperatures (1.15, 1.30, 1.50, and 2.00 K) were obtained and also the film flow rate was measured at 1.15 K. Then, the mass flow rates were measured after installing the whole System into a flight model dewar at the He tank temperature of 1.16, 1.30, 1.50, and 2.00 K. The dewar was tilted so that the porous plug located at the top of the dewar is immersed in the liquid He and the porous plug separates the liquid and vapor He by the thermomechanical effect as in orbit. The obtained mass flow rates and the film flow rate in these tests were confirmed to meet the requirements and to be consistent with each other. No abnormal event such as large mass flow rates was observed. All these experimental results strongly suggest that this flight model of the porous plug and the film flow Suppression System will work properly in space.
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development of porous plug phase separator and superfluid film flow Suppression System for the soft x ray spectrometer onboard astro h
Cryogenics, 2012Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Hiroya Yamaguchi, Shoji TsunematsuAbstract:Abstract ASTRO-H is the sixth Japanese astronomy satellite scheduled for launch in 2014. The Soft X-ray Spectrometer instrument is onboard ASTRO-H. This is a 6 × 6 array of X-ray microcalorimeters with an energy resolution of
Yuichiro Ezoe - One of the best experts on this subject based on the ideXlab platform.
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porous plug phase separator and superfluid film flow Suppression System for the soft x ray spectrometer onboard hitomi
Journal of Astronomical Telescopes Instruments and Systems, 2017Co-Authors: Yuichiro Ezoe, Kumi Ishikawa, Ikuyuki Mitsuishi, Kenichi Kanao, Ryuichi Fujimoto, Kazuhisa Mitsuda, Michael Dipirro, Yoshitaka Ishisaki, Mark O Kimball, Masahide MurakamiAbstract:When using superfluid helium in low-gravity environments, porous plug phase separators are commonly used to vent boil-off gas while confining the bulk liquid to the tank. Invariably, there is a flow of superfluid film from the perimeter of the porous plug down the vent line. For the soft x-ray spectrometer onboard ASTRO-H (Hitomi), its approximately 30-liter helium supply has a lifetime requirement of more than 3 years. A nominal vent rate is estimated as ∼30 μg/s, equivalent to ∼0.7 mW heat load. It is, therefore, critical to suppress any film flow whose evaporation would not provide direct cooling of the remaining liquid helium. That is, the porous plug vent System must be designed to both minimize film flow and to ensure maximum extraction of latent heat from the film. The design goal for Hitomi is to reduce the film flow losses to <2 μg/s, corresponding to a loss of cooling capacity of <40 μW. The design adopts the same general design as implemented for Astro-E and E2, using a vent System composed of a porous plug, combined with an orifice, a heat exchanger, and knife-edge devices. Design, on-ground testing results, and in-orbit performance are described.
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porous plug phase separator and superfluid film flow Suppression System for the soft x ray spectrometer onboard astro h
Proceedings of SPIE, 2016Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Ikuyuki Mitsuishi, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Shoji TsunematsuAbstract:Suppression of super fluid helium flow is critical for the Soft X-ray Spectrometer onboard ASTRO-H (Hitomi). In nominal operation, a small helium gas flow of ~30 μg/s must be safely vented and a super fluid film flow must be sufficiently small <2 μg/s. To achieve a life time of the liquid helium, a porous plug phase separator and a film flow Suppression System composed of an orifice, a heat exchanger, and knife edge devices are employed. In this paper, design, on-ground testing results and in-orbit performance of the porous plug and the film flow Suppression System are described.
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flight model measurements of the porous plug and film flow Suppression System for the astro h soft x ray spectrometer dewar
Cryogenics, 2016Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Ikuyuki Mitsuishi, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Shoji TsunematsuAbstract:Abstract Flight model measurements of a porous plug phase separator and a film flow Suppression System for the ASTRO-H Soft X-ray Spectrometer dewar are described. ASTRO-H is the sixth Japanese astronomy satellite and will be launched in 2016. It carries the Soft X-ray Spectrometer consisting of an X-ray optic and an X-ray microcalorimeter System operated at 50 mK. Superfluid liquid He is employed as a part of the cooling System. A wide range of He flows from 28 μ g/s to 3.2 mg/s in various operation cases must be safely vented under zero gravity. At the same time, superfluid He film flow through the vent line must be suppressed to μ g/s in a nominal case to avoid extra loss of the liquid He. For this purpose, a porous plug phase separator together with a film flow Suppression System is installed. To verify its performance, the mass flow rates and the film flow rate of the flight model System were measured at component level. The mass flow rates at various He tank temperatures (1.15, 1.30, 1.50, and 2.00 K) were obtained and also the film flow rate was measured at 1.15 K. Then, the mass flow rates were measured after installing the whole System into a flight model dewar at the He tank temperature of 1.16, 1.30, 1.50, and 2.00 K. The dewar was tilted so that the porous plug located at the top of the dewar is immersed in the liquid He and the porous plug separates the liquid and vapor He by the thermomechanical effect as in orbit. The obtained mass flow rates and the film flow rate in these tests were confirmed to meet the requirements and to be consistent with each other. No abnormal event such as large mass flow rates was observed. All these experimental results strongly suggest that this flight model of the porous plug and the film flow Suppression System will work properly in space.
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development of porous plug phase separator and superfluid film flow Suppression System for the soft x ray spectrometer onboard astro h
Cryogenics, 2012Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Hiroya Yamaguchi, Shoji TsunematsuAbstract:Abstract ASTRO-H is the sixth Japanese astronomy satellite scheduled for launch in 2014. The Soft X-ray Spectrometer instrument is onboard ASTRO-H. This is a 6 × 6 array of X-ray microcalorimeters with an energy resolution of
Laurent Pueyo - One of the best experts on this subject based on the ideXlab platform.
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apodized pupil lyot coronagraphs designs for future segmented space telescopes
Space Telescopes and Instrumentation 2018: Optical Infrared and Millimeter Wave, 2018Co-Authors: Kathryn St Laurent, N Zimmerman, Anand Sivaramakrishnan, Christopher C Stark, Kevin Fogarty, Mamadou Ndiaye, Johan Mazoyer, Laurent PueyoAbstract:A coronagraphic starlight Suppression System situated on a future flagship space observatory offers a promising avenue to image Earth-like exoplanets and search for biomarkers in their atmospheric spectra. One NASA mission concept that could serve as the platform to realize this scientific breakthrough is the Large UV/Optical/IR Surveyor (LUVOIR). Such a mission would also address a broad range of topics in astrophysics with a multiwavelength suite of instruments. The apodized pupil Lyot coronagraph (APLC) is one of several coronagraph design families that the community is assessing as part of NASAs Exoplanet Exploration Program Segmented aperture coronagraph design and analysis (SCDA) team. The APLC is a Lyot-style coronagraph that suppresses starlight through a series of amplitude operations on the on-axis field. Given a suite of seven plausible segmented telescope apertures, we have developed an object-oriented software toolkit to automate the exploration of thousands of APLC design parameter combinations. This has enabled us to empirically establish relationships between planet throughput and telescope aperture geometry, inner working angle, bandwidth, and contrast level. In parallel with the parameter space exploration, we have investigated several strategies to improve the robustness of APLC designs to fabrication and alignment errors. We also investigate the combination of APLC with wavefront control or complex focal plane masks to improve inner working angle and throughput. Preliminary scientific yield evaluations based on design reference mission simulations indicate the APLC is a very competitive concept for surveying the local exoEarth population with a mission like LUVOIR.
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apodized pupil lyot coronagraphs for arbitrary apertures iv reduced inner working angle and increased robustness to low order aberrations
The Astrophysical Journal, 2015Co-Authors: Mamadou Ndiaye, Laurent Pueyo, Remi SoummerAbstract:The Apodized Pupil Lyot Coronagraph (APLC) is a diffraction Suppression System installed in the recently deployed instruments Palomar/P1640, Gemini/GPI, and VLT/SPHERE to allow direct imaging and spectroscopy of circumstellar environments. Using a prolate apodization, the current implementations offer raw contrasts down to 10–7 at 0.2 arcsec from a star over a wide bandpass (20%), in the presence of central obstruction and struts, enabling the study of young or massive gaseous planets. Observations of older or lighter companions at smaller separations would require improvements in terms of the inner working angle (IWA) and contrast, but the methods originally used for these designs were not able to fully explore the parameter space. We propose a novel approach to improve the APLC performance. Our method relies on the linear properties of the coronagraphic electric field with the apodization at any wavelength to develop numerical solutions producing coronagraphic star images with high-contrast region in broadband light. We explore the parameter space by considering different aperture geometries, contrast levels, dark-zone sizes, bandpasses, and focal plane mask sizes. We present an application of these solutions to the case of Gemini/GPI with a design delivering a 10–8 raw contrast at 0.19 arcsec and offering a significantly reduced sensitivity to low-order aberrations compared to the current implementation. Optimal solutions have also been found to reach 10–10 contrast in broadband light regardless of the aperture shape, with effective IWA in the 2-3.5 λ/D range, therefore making the APLC a suitable option for the future exoplanet direct imagers on the ground or in space.
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apodized pupil lyot coronagraphs for arbitrary apertures iv reduced inner working angle and increased robustness to low order aberrations
arXiv: Instrumentation and Methods for Astrophysics, 2014Co-Authors: Mamadou Ndiaye, Laurent Pueyo, Remi SoummerAbstract:The Apodized Pupil Lyot Coronagraph (APLC) is a diffraction Suppression System installed in the recently deployed instruments Palomar/P1640, Gemini/GPI, and VLT/SPHERE to allow direct imaging and spectroscopy of circumstellar environments. Using a prolate apodization, the current implementations offer raw contrasts down to $10^{-7}$ at 0.2 arcsec from a star over a wide bandpass (20\%), in the presence of central obstruction and struts, enabling the study of young or massive gaseous planets. Observations of older or lighter companions at smaller separations would require improvements in terms of inner working angle (IWA) and contrast, but the methods originally used for these designs were not able to fully explore the parameter space. We here propose a novel approach to improve the APLC performance. Our method relies on the linear properties of the coronagraphic electric field with the apodization at any wavelength to develop numerical solutions producing coronagraphic star images with high-contrast region in broadband light. We explore the parameter space by considering different aperture geometries, contrast levels, dark-zone sizes, bandpasses, and focal plane mask sizes. We present an application of these solutions to the case of Gemini/GPI with a design delivering a $10^{-8}$ raw contrast at 0.19 arcsec and offering a significantly reduced sensitivity to low-order aberrations compared to the current implementation. Optimal solutions have also been found to reach $10^{-10}$ contrast in broadband light regardless of the telescope aperture shape (in particular the central obstruction size), with effective IWA in the $2-3.5\lambda/D$ range, therefore making the APLC a suitable option for the future exoplanet direct imagers on the ground or in space.
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apodized pupil lyot coronagraphs development of designs with reduced iwa and robustness to low order aberrations
Proceedings of SPIE, 2014Co-Authors: Mamadou Ndiaye, Laurent Pueyo, Remi Soummer, Alexis CarlottiAbstract:The Apodized Pupil Lyot Coronagraph (APLC) is a di_raction Suppression System adopted in the baseline of several new and recent high-contrast imaging instruments (Palomar P1640, Gemini Planet Imager, VLT/SPHERE) to enable direct imaging of exoplanets at small angular separations (> 0.2 arcsec) from their host star. This coronagraph combines an entrance pupil apodizer, a hard-edge focal plane mask (FPM) and a Lyot stop in a relayed pupil plane to form the coronagraphic image of an observed star onto a camera located in the image plane. The APLC designs underlying these instruments take advantage of the eigen-properties between entrance pupil and Lyot stop, and rely on prolate apodization to reach a contrast performance of 10 7 over a 20% spectral bandwidth and with a moderate inner working angle (IWA, ~ 5 λ/=D) in the presence of central obstruction and support structures. In this communication we propose novel designs relying on the linearity between the coronagraphic electric field at the science camera and the apodization function. We use this relationship to devise a numerical optimization scheme that extends the APLC performance (contrast, IWA, apodizer through- put, chromaticity) beyond the intrinsic properties of prolate apodizations. We explore the parameter space by considering different aperture geometries, contrast levels, dark-zone size, spectral bandwidth and FPM size. We present the application of these new solutions to the case of the High-Contrast Imager for Complex Aperture Telescopes (HiCAT).
Remi Soummer - One of the best experts on this subject based on the ideXlab platform.
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apodized pupil lyot coronagraphs for arbitrary apertures iv reduced inner working angle and increased robustness to low order aberrations
The Astrophysical Journal, 2015Co-Authors: Mamadou Ndiaye, Laurent Pueyo, Remi SoummerAbstract:The Apodized Pupil Lyot Coronagraph (APLC) is a diffraction Suppression System installed in the recently deployed instruments Palomar/P1640, Gemini/GPI, and VLT/SPHERE to allow direct imaging and spectroscopy of circumstellar environments. Using a prolate apodization, the current implementations offer raw contrasts down to 10–7 at 0.2 arcsec from a star over a wide bandpass (20%), in the presence of central obstruction and struts, enabling the study of young or massive gaseous planets. Observations of older or lighter companions at smaller separations would require improvements in terms of the inner working angle (IWA) and contrast, but the methods originally used for these designs were not able to fully explore the parameter space. We propose a novel approach to improve the APLC performance. Our method relies on the linear properties of the coronagraphic electric field with the apodization at any wavelength to develop numerical solutions producing coronagraphic star images with high-contrast region in broadband light. We explore the parameter space by considering different aperture geometries, contrast levels, dark-zone sizes, bandpasses, and focal plane mask sizes. We present an application of these solutions to the case of Gemini/GPI with a design delivering a 10–8 raw contrast at 0.19 arcsec and offering a significantly reduced sensitivity to low-order aberrations compared to the current implementation. Optimal solutions have also been found to reach 10–10 contrast in broadband light regardless of the aperture shape, with effective IWA in the 2-3.5 λ/D range, therefore making the APLC a suitable option for the future exoplanet direct imagers on the ground or in space.
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apodized pupil lyot coronagraphs for arbitrary apertures iv reduced inner working angle and increased robustness to low order aberrations
arXiv: Instrumentation and Methods for Astrophysics, 2014Co-Authors: Mamadou Ndiaye, Laurent Pueyo, Remi SoummerAbstract:The Apodized Pupil Lyot Coronagraph (APLC) is a diffraction Suppression System installed in the recently deployed instruments Palomar/P1640, Gemini/GPI, and VLT/SPHERE to allow direct imaging and spectroscopy of circumstellar environments. Using a prolate apodization, the current implementations offer raw contrasts down to $10^{-7}$ at 0.2 arcsec from a star over a wide bandpass (20\%), in the presence of central obstruction and struts, enabling the study of young or massive gaseous planets. Observations of older or lighter companions at smaller separations would require improvements in terms of inner working angle (IWA) and contrast, but the methods originally used for these designs were not able to fully explore the parameter space. We here propose a novel approach to improve the APLC performance. Our method relies on the linear properties of the coronagraphic electric field with the apodization at any wavelength to develop numerical solutions producing coronagraphic star images with high-contrast region in broadband light. We explore the parameter space by considering different aperture geometries, contrast levels, dark-zone sizes, bandpasses, and focal plane mask sizes. We present an application of these solutions to the case of Gemini/GPI with a design delivering a $10^{-8}$ raw contrast at 0.19 arcsec and offering a significantly reduced sensitivity to low-order aberrations compared to the current implementation. Optimal solutions have also been found to reach $10^{-10}$ contrast in broadband light regardless of the telescope aperture shape (in particular the central obstruction size), with effective IWA in the $2-3.5\lambda/D$ range, therefore making the APLC a suitable option for the future exoplanet direct imagers on the ground or in space.
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apodized pupil lyot coronagraphs development of designs with reduced iwa and robustness to low order aberrations
Proceedings of SPIE, 2014Co-Authors: Mamadou Ndiaye, Laurent Pueyo, Remi Soummer, Alexis CarlottiAbstract:The Apodized Pupil Lyot Coronagraph (APLC) is a di_raction Suppression System adopted in the baseline of several new and recent high-contrast imaging instruments (Palomar P1640, Gemini Planet Imager, VLT/SPHERE) to enable direct imaging of exoplanets at small angular separations (> 0.2 arcsec) from their host star. This coronagraph combines an entrance pupil apodizer, a hard-edge focal plane mask (FPM) and a Lyot stop in a relayed pupil plane to form the coronagraphic image of an observed star onto a camera located in the image plane. The APLC designs underlying these instruments take advantage of the eigen-properties between entrance pupil and Lyot stop, and rely on prolate apodization to reach a contrast performance of 10 7 over a 20% spectral bandwidth and with a moderate inner working angle (IWA, ~ 5 λ/=D) in the presence of central obstruction and support structures. In this communication we propose novel designs relying on the linearity between the coronagraphic electric field at the science camera and the apodization function. We use this relationship to devise a numerical optimization scheme that extends the APLC performance (contrast, IWA, apodizer through- put, chromaticity) beyond the intrinsic properties of prolate apodizations. We explore the parameter space by considering different aperture geometries, contrast levels, dark-zone size, spectral bandwidth and FPM size. We present the application of these new solutions to the case of the High-Contrast Imager for Complex Aperture Telescopes (HiCAT).
Masahide Murakami - One of the best experts on this subject based on the ideXlab platform.
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porous plug phase separator and superfluid film flow Suppression System for the soft x ray spectrometer onboard hitomi
Journal of Astronomical Telescopes Instruments and Systems, 2017Co-Authors: Yuichiro Ezoe, Kumi Ishikawa, Ikuyuki Mitsuishi, Kenichi Kanao, Ryuichi Fujimoto, Kazuhisa Mitsuda, Michael Dipirro, Yoshitaka Ishisaki, Mark O Kimball, Masahide MurakamiAbstract:When using superfluid helium in low-gravity environments, porous plug phase separators are commonly used to vent boil-off gas while confining the bulk liquid to the tank. Invariably, there is a flow of superfluid film from the perimeter of the porous plug down the vent line. For the soft x-ray spectrometer onboard ASTRO-H (Hitomi), its approximately 30-liter helium supply has a lifetime requirement of more than 3 years. A nominal vent rate is estimated as ∼30 μg/s, equivalent to ∼0.7 mW heat load. It is, therefore, critical to suppress any film flow whose evaporation would not provide direct cooling of the remaining liquid helium. That is, the porous plug vent System must be designed to both minimize film flow and to ensure maximum extraction of latent heat from the film. The design goal for Hitomi is to reduce the film flow losses to <2 μg/s, corresponding to a loss of cooling capacity of <40 μW. The design adopts the same general design as implemented for Astro-E and E2, using a vent System composed of a porous plug, combined with an orifice, a heat exchanger, and knife-edge devices. Design, on-ground testing results, and in-orbit performance are described.
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porous plug phase separator and superfluid film flow Suppression System for the soft x ray spectrometer onboard astro h
Proceedings of SPIE, 2016Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Ikuyuki Mitsuishi, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Shoji TsunematsuAbstract:Suppression of super fluid helium flow is critical for the Soft X-ray Spectrometer onboard ASTRO-H (Hitomi). In nominal operation, a small helium gas flow of ~30 μg/s must be safely vented and a super fluid film flow must be sufficiently small <2 μg/s. To achieve a life time of the liquid helium, a porous plug phase separator and a film flow Suppression System composed of an orifice, a heat exchanger, and knife edge devices are employed. In this paper, design, on-ground testing results and in-orbit performance of the porous plug and the film flow Suppression System are described.
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flight model measurements of the porous plug and film flow Suppression System for the astro h soft x ray spectrometer dewar
Cryogenics, 2016Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Ikuyuki Mitsuishi, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Shoji TsunematsuAbstract:Abstract Flight model measurements of a porous plug phase separator and a film flow Suppression System for the ASTRO-H Soft X-ray Spectrometer dewar are described. ASTRO-H is the sixth Japanese astronomy satellite and will be launched in 2016. It carries the Soft X-ray Spectrometer consisting of an X-ray optic and an X-ray microcalorimeter System operated at 50 mK. Superfluid liquid He is employed as a part of the cooling System. A wide range of He flows from 28 μ g/s to 3.2 mg/s in various operation cases must be safely vented under zero gravity. At the same time, superfluid He film flow through the vent line must be suppressed to μ g/s in a nominal case to avoid extra loss of the liquid He. For this purpose, a porous plug phase separator together with a film flow Suppression System is installed. To verify its performance, the mass flow rates and the film flow rate of the flight model System were measured at component level. The mass flow rates at various He tank temperatures (1.15, 1.30, 1.50, and 2.00 K) were obtained and also the film flow rate was measured at 1.15 K. Then, the mass flow rates were measured after installing the whole System into a flight model dewar at the He tank temperature of 1.16, 1.30, 1.50, and 2.00 K. The dewar was tilted so that the porous plug located at the top of the dewar is immersed in the liquid He and the porous plug separates the liquid and vapor He by the thermomechanical effect as in orbit. The obtained mass flow rates and the film flow rate in these tests were confirmed to meet the requirements and to be consistent with each other. No abnormal event such as large mass flow rates was observed. All these experimental results strongly suggest that this flight model of the porous plug and the film flow Suppression System will work properly in space.
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development of porous plug phase separator and superfluid film flow Suppression System for the soft x ray spectrometer onboard astro h
Cryogenics, 2012Co-Authors: Yuichiro Ezoe, Masahide Murakami, Kumi Ishikawa, Kenichi Kanao, Takaya Ohashi, Ryuichi Fujimoto, Seiji Yoshida, Kazuhisa Mitsuda, Hiroya Yamaguchi, Shoji TsunematsuAbstract:Abstract ASTRO-H is the sixth Japanese astronomy satellite scheduled for launch in 2014. The Soft X-ray Spectrometer instrument is onboard ASTRO-H. This is a 6 × 6 array of X-ray microcalorimeters with an energy resolution of
