The National Astronomical Observatory of Japan (NAOJ) has been responsible for the telescope structure subsystem (STR) of the Thirty Meter Telescope since 2012 and has engaged Mitsubishi Electric Corporation (MELCO) for preliminary and final design and pre-production work. There are various subsystems on the telescope, such as instruments and moving optics. Power and fluids and other services are required to operate these subsystems and the telescope drives. TMT provides the following services: Electrical Power and Bonding/Grounding, Fire Alarm, Communication and Information System (CIS) Networks, Fixed Temperature Chilled Water (FTCW) and Variable Temperature Chilled Water (VTCW), Hydrostatic Bearing System (HBS) Oil, Facility Compressed Air (FCA), Cryogenic System (CRYO), Refrigerant System (REFR), and Lighting (Operational and Emergency). The TMT defines the Telescope Utility Services (TUS) as the infrastructure which includes the cables and pipes used to deliver these utilities, the structures that support and route them, and the other components (electrical or piping components such as electrical cabinets or manifolds, lighting fixtures, fire alarms, etc.) necessary to provide these services. The design work to attach the TUS components to the STR was complicated due to the wide variety of TUS components and the multitude of mounting configurations and locations throughout the telescope structure. In order to efficiently integrate the various types of TUS components onto the STR, several practices were established and refined in the development of the TUS and STR design: 1. Definition of SOW between TUS and STR to enable concurrent TUS and STR design development 2. Simultaneous development of TUS and STR using CAD model 3. Piping and Cabling allocation within the Azimuth/Elevation Wrap 4. Route planning for cabling and piping 5. Seismic evaluation of TUS components In this paper we present the approach and the design implementation of the TUS components onto the STR.
National Astronomical Observatory of Japan (NAOJ) is responsible for procuring the Telescope Structure System (STR) of the Thirty Meter Telescope (TMT) and engaged Mitsubishi Electric Corporation (MELCO) to perform the preliminary/final design and production readiness work since 2012. The final design of the TMT STR was deemed completed through a series of external design reviews covering structural and mechanical, controls, and auxiliary systems such as the Segment Handling System (SHS), Aerial Service Platform (ASP), Elevator (ELV), safety, and the seismic isolation system. TMT STR is currently in the production readiness phase and has already passed the Production Readiness Reviews (PRRs) for major rotating mechanical structures. In this paper we present an overview of the design progress of the TMT STR, matured through extensive studies, performance assessments, and design budgets derived from bottoms-up analyses. Additionally, we discuss prototype activities to mitigate risks to performance and manufacturability of complex designs, along with the current programmatic status of the project.
Hazard and Risk Assessment (HARA) is a critical Systems Engineering and safety activity used to ensure a safe environment for personnel and hardware. This paper discusses how TMT has tailored the Atlassian Jira tool and third-party embedded app, SoftComply Risk Manager, to provide a collaborative environment with subsystem teams in order to a develop a comprehensive HARA, starting with hazard identification and assessment and continuing through reassessment after mitigation. The paper shows how the tool was initially created for the Telescope Structure (STR) to facilitate collaboration with the National Astronomical Observatory of Japan (NAOJ) and Mitsubishi Electric Corporation (MELCO), and has since expanded to other subsystems as well as to the system-level, capturing intersystem hazards. From the system and subsystem HARAs, risk reduction actions are identified and if safety functions are used as a mitigation, they are described in terms of functional safety actions and associated SIL ratings. These safety functions are then traced to safety requirements imposed on the Observatory Safety System or on subsystems. This overall HARA process provides TMT with a comprehensive overview of all Observatory hazards and the status of the development and implementation of their mitigations thanks to the Jira and Risk Manager dashboards, risk matrix, and risk table views.
KEYWORDS: Antennas, Near field, Holography, Telescopes, Phase measurement, Holograms, Polarization, Detector arrays, Near field optics, Signal detection
Wide field-of-view millimeter-wave telescopes with a bolometric detector array have been developed for cosmic microwave background radiation observations. For the purpose of laboratory verification of these telescopes, several studies have demonstrated near-field antenna measurements using a phase-sensitive detector that replaces a few representative pixels of the focal-plane detector array. We present a holographic phase-retrieval method that enables near-field measurements with the bolometric detector array as it is. We place a reference emitter at a fixed position and scan a signal emitter at the telescope aperture. These two emitters are phase-locked and generate interference patterns (holograms) on the focal plane, from which the amplitude and phase of the aperture field can be retrieved. We experimentally demonstrated this method with a crossed-Dragone telescope with a field-of-view that is 18 deg × 9 deg. In the demonstration, we placed a phase-sensitive detector at three detector positions on the focal plane. The antenna patterns calculated from the hologram, neglecting the directly measured phase information, were consistent with those calculated from both intensity and phase measurements at the −60-dB level at 180 GHz. Applying this method, the antenna patterns for all of the bolometric detectors on the focal plane can theoretically be measured simultaneously.
LiteBIRD is a space mission intended for the late 2020s that aims to observe the large-angular-scale polarization pattern of the cosmic microwave background. The low-frequency telescope (LFT) aboard LiteBIRD has a crossed-Dragone design and observes at 34 to 161 GHz with a field of view (FoV) of 18 deg × 9 deg. The LFT antenna optics is predicted to induce polarization angle rotation by up to around 1.5 deg in its FoV, while polarization angles among the detectors should be corrected to a few arcminutes level to distinguish E- and B-mode polarizations. To characterize the polarization angle rotation by the antenna optics and to develop a ground calibration method, we performed polarization angle measurements with a small compact-antenna-test-range setup. We measured the polarization angles of a 1/4-scaled LFT antenna across the FoV at correspondingly scaled frequencies of 140 to 220 GHz (35 to 55 GHz for the full-scale LFT). We placed a collimated-wave source near the scaled-LFT aperture and rotated the scaled-LFT feed polarization. The measured polarization angles agree with those measured by rotating the collimated-wave polarization at the 15″ level for the on-axis case. The measurements are consistent with simulation and determined the polarization angles with an uncertainty of less than 1.9′.
We verified a method of near-field antenna pattern measurement for a wide-field telescope with a bolometric detector array, based on a holographic phase-retrieval technique. A signal emitter scans the telescope aperture and a reference emitter, which is phase-locked to the signal, is located at a fixed position to allow a bolometric detector to receive the both. It generates a hologram on the focal plane as a function of the signal emitter location. Since the hologram is obtained in a receiving mode, we can use the telescope-equipped detector as it is. It is beneficial for the case where such detector is integrated with a feed antenna, which characterizes the telescope performance. The new method also has an advantage that we do not need the phase calibration of the reference emitter since it is constant. We experimentally demonstrated this method with a crossed-Dragone antenna whose field of view is 18◦ × 9 ◦ at 180 GHz for three representative detector positions in the focal plane. The antenna patterns were consistent with those measured by a vector near-field measurement at the level of −60 dB, which directly acquires both the phase and the amplitude of the electric field.
National Astronomical Observatory of Japan (NAOJ) has had the responsibility for the Telescope Structure System (STR) of Thirty Meter Telescope (TMT) and engaged Mitsubishi Electric Corporation (MELCO) to take over the preliminary/final design and pre-production work since 2012. TMT defines that STR shall be designed to withstand earthquakes up to the levels of the 1000-years annual return period as keeping accelerations at the mirror/instrumental interface points below the specified thresholds. In this paper, we present the Seismic Isolation System (SIS) of TMT STR, as focusing on (1) the design to achieve compatibility of two conflicting performances that are the rigid connection to the ground during normal observations and flexible movement during seismic to suppress the seismic energy, (2) prototype results of the seismic isolation system, and (3) compliance status of the seismic requirements which is evaluated by time history analysis using the Finite Element Method (FEM) model of TMT STR.
Suppression of straylight is one of the challenges in the optical design of a wide-field-of-view telescope. It contaminates the weak target signal with radiation from strong sources at angles far from the observing direction. We evaluated the optical design of a crossed-Dragone telescope, the LiteBIRD Low-Frequency Telescope (LFT), which has 18° ×9° field of view. We measured a 1/4-scaled antenna of the LFT at accordingly scaled frequencies of 160–200 GHz (corresponding to 40–50 GHz for the full-scale LFT), for the feed at the center and the edges of the focal plane. To separate straylight components, we computed the time profiles of the aperture fields with ∼ 0.1 ns resolution by inverse Fourier transformation of the measured frequency spectra and applied time gating to them. We identified far-sidelobe components in the time-gated antenna beam patterns whose arrival time and angular direction are consistent with straylight predicted by a ray-tracing simulation. The identified far-sidelobe components include straylight reduced but reflected inside the front hood and straylight with multiple reflections without intercepted by the front hood. Their intensities are less than the −56 dB level, which is the far-sidelobe knowledge requirement for the LFT.
LiteBIRD is JAXA Strategic Large Mission for the late 2020s that aims to observe the large-scale B-mode polarization pattern of the cosmic microwave background. One of its telescopes, the Low Frequency Telescope (LFT), has a crossed-Dragone design and observes at 34-161 GHz with a field of view of 18° x 9°. Because a miscalibration of the polarization angles mixes E- and B-mode polarization, we have measured the variation of the polarization angles in the field of view of a 1/4-scaled LFT antenna at 140-220 GHz, which corresponds to 35-55 GHz for the full-scale LFT, considering a scaling of the wavelength. We placed a collimated-wave source near the scaled-LFT aperture and rotated the polarization angle of the LFT feed. The measurements were explained well with a simple Jones matrix calculation, and the fitting errors of the polarization angles were less than 0.1’. We also measured the polarization angles by rotating the polarization direction in the scaled-LFT aperture, and the results were consistent with the angles measured by rotating the feed polarization at the ±10” level, except at the lowest frequencies. The polarization angle at the edges of the focal plane varied from that at the center by up to around a degree, with larger variation at lower frequencies. We evaluated the polarization angles for both Pol-X and Pol-Y feeds, and the results with Pol-Y showed a trend consistent with ray-tracing simulations. The results for Pol-X showed the opposite trend of the polarization rotation direction and larger angle variations.
We propose the Allan Variance method to identify spurious signals with sensitive detectability. With this method, detection level of -56 dB with respect to the system noise can be achieved within the integration time less than 10 min. Detected spurious signals can be mitigated by masking these channels before spectral bunching to required spectral resolution. We will present the principle of the method and the performance taken through the ALMA system verification activity. This method can be applied for universal single-dish spectroscopy.
A holography receiver has been developed for both ALMA antennas (12m and 7m). ALMA had no holography receivers for the 7m antenna. It required high-accuracy, despite small size and light weight for easy installation with a limited working area. The ALMA antennas are also used for daytime observations. The antenna deformation strongly depends on ambient temperature and sun exposure. It is essential to know the daytime antenna deformation for success of the ALMA observation. The purpose of the project is to provide a holography receiver that can measure the diurnal and the seasonal antenna deformation.
The Atacama Large Millimeter/submillimeter Array (ALMA) will be composed of 66 high precision antennae located at
5000 meters altitude in northern Chile. This paper will present the methodology, tools and processes adopted to system
engineer a project of high technical complexity, by system engineering teams that are remotely located and from
different cultures, and in accordance with a demanding schedule and within tight financial constraints. The technical and
organizational complexity of ALMA requires a disciplined approach to the definition, implementation and verification of
the ALMA requirements. During the development phase, System Engineering chairs all technical reviews and facilitates
the resolution of technical conflicts. We have developed analysis tools to analyze the system performance, incorporating
key parameters that contribute to the ultimate performance, and are modeled using best estimates and/or measured values
obtained during test campaigns. Strict tracking and control of the technical budgets ensures that the different parts of the
system can operate together as a whole within ALMA boundary conditions. System Engineering is responsible for
acceptances of the thousands of hardware items delivered to Chile, and also supports the software acceptance process. In
addition, System Engineering leads the troubleshooting efforts during testing phases of the construction project. Finally,
the team is conducting System level verification and diagnostics activities to assess the overall performance of the
observatory. This paper will also share lessons learned from these system engineering and verification approaches.
The ALMA aperture synthesis radio telescope is under construction in northern Chile. This paper presents the
organization and process of ALMA System Verification. The purpose of System Verification is to measure the
performance of the integrated instrument with respect to the ALMA System Technical Requirements. The System
Technical Requirements flow down from the Science Requirements of the telescope and are intended to guide the design
of the array and set the standards for technical performance. The process of System Verification will help determine
how well the ALMA telescope meets its science goals. Some verification results are discussed.
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