The Subaru laser guide star system has been upgraded by implementing the TOPTICA/MPBC guide-star laser and a new mirror-based laser relay system. The upgrade is to replace the aged laser and its transfer system and provide the improved performance for stable science operation. The increased laser return photon can also bring a new capability of generating multiple laser guide stars (LGSs) by splitting the laser beam. The new laser guide star system was installed on the Subaru telescope in December 2021 and commissioning observations were conducted in 2022. The LGSAO mode with the new laser guide star system has been offered for science open use program since 2023. The new laser guide star system provides more stable LGS than the previous system with respect to the laser power and pointing. The LGS spot size is ∼1.0 arcsec in FWHM under median seeing condition. The LGS photon return is more than 10 times brighter than the previous system. By utilizing the increased brightness, further upgrade of the Laser Launching Telescope (LLT) is being implemented to generate the asterism of four LGSs with the diameter variable between 10 and 40 arcsec for the new Laser Tomography Adaptive Optics (LTAO) system.
The instrumentation of the Prime Focus Spectrograph (PFS), a next generation facility instrument on the Subaru telescope, is now in the final phase of its commissioning process and its general, open-use operations for sciences will provisionally start in 2025. The instrument enables simultaneous spectroscopy with 2386 individual fibers distributed over a very wide (∼1.3 degrees in diameter) field of view on the Subaru’s prime focus. The spectra cover a wide range of wavelengths from 380nm to 1260nm in one exposure in the Low-Resolution (LR) mode (while the visible red channel has the Medium-Resolution (MR) mode as well that covers 710−885nm). The system integration activities at the observatory on Maunakea in Hawaii have been continuing since the arrival of the Metrology Camera System in 2018. On-sky engineering tests and observations have also been carried out continually since September 2021 and, despite various difficulties in interlacing commissioning processes with development activities on the schedule and addressing some major issues on hardware and software, the team successfully observed many targeted stars as intended over the entire field of view (Engineering First Light) in September 2022. Then in parallel to the arrival, integration and commissioning of more hardware components, validations and optimizations of the performance and operation of the instrument are ongoing. The accuracy of the fiber positioning process and the speed of the fiber reconfiguration process have been recently confirmed to be ∼ 20−30μm for 95% of allocated fibers, and ∼130 seconds, respectively. While precise quantitative analyses are still in progress, the measured throughput has been confirmed to be consistent with the model where the information from various sub-components and sub-assemblies is integrated. Long integration of relatively faint objects are being taken to validate an expected increase of signal-to-noise ratio as more exposures are taken and co-added without any serious systematic errors from, e.g., sky subtraction process. The PFS science operation will be carried out in a queue mode by default and various developments, implementations and validations have been underway accordingly in parallel to the instrument commissioning activities. Meetings and sessions are arranged continually with the communities of potential PFS users on multiple scales, and discussions are iterated for mutual understanding and possible optimization of the rules and procedures over a wide range of processes such as proposal submission, observation planning, data acquisition and data delivery. The end-to-end processes of queue observations including successive exposures with updated plans based on assessed qualities of the data from past observations are being tested during engineering observations, and further optimizations are being undertaken. In this contribution, a top-level summary of these achievements and ongoing progresses and future perspectives will be provided.
We present the results of optical performance verification for the Prime Focus Spectrograph (PFS) fiber optics module, so-called “CableBs”, at Subaru Telescope. PFS is the next generation ultra-wide field multi object spectrograph. It employs 2386 fibers of which the fiber tips are placed precisely on the primary focal plane over a field of view of 1.3 degrees in diameter. CableB transfers light from the fiber positioning module, or Prime Focus Instrument, to the spectrographs. PFS utilizes four CableBs and each of them carries just over 600 science grade fibers. We completed installation of all CableBs at the telescope in June 2023 after two-years of intermittent work. The optical performance of each CableB was subsequently assessed, focusing on four areas; continuity, uniformity, throughput, and focal ratio degradation (FRD). For examining continuity, we illuminated one termination of CableB with flat LED panel and observed the transmitted light. We found only one fiber newly broken during shipment from the integration site. We also checked uniformity of the relative intensity of light propagating in each fiber. The whole variations around the average intensities fit in 20% range among fibers in each CableB, which was consistent with the measurement before shipping. Throughput of sampled fibers were measured in a wavelength range from 400 to 1400 nm with commercial spectrometers. The measurement at the telescope and the integration site each showed a throughput of approximately 70%, so both sets of measurements are consistent. Finally, we measured FRD employing the collimated beam method to ensure that CableBs were free from any significant physical stress after the installation. Our FRD measurements were comparable before and after the installation. In addition, a long-term monitoring of over a few months showed FRD remained sufficiently stable for science operations. According to these results, we conclude that the installation of CableBs at Subaru Telescope was successful.
PFS (Prime Focus Spectrograph) is an ultra-wide-field, multi-object spectrograph currently being commissioned at Subaru telescope. The focal plane is made of ∼2400 science fibers and fiber positioners at the telescope prime focus, covering a field of view of 1.3 deg in diameter. The science fibers will be connected to 4 identical spectrograph modules, each receiving ∼600 fibers. Every spectrograph module will host 3 cameras, covering the blue (380–650 nm), red (630–970 nm) and near-infrared (940–1260 nm) wavelengths. This presentation will focus on the completion of the PFS spectrograph modules at the Subaru telescope. We will present their integration and test processes and measured performance, as well as the technical challenges encountered along the way, and the solutions used to correct them.
PFS (Prime Focus Spectrograph), a next generation facility instrument on the Subaru telescope, is now being tested on the telescope. The instrument is equipped with very wide (1.3 degrees in diameter) field of view on the Subaru’s prime focus, high multiplexity by 2394 reconfigurable fibers, and wide waveband spectrograph that covers from 380nm to 1260nm simultaneously in one exposure. Currently engineering observations are ongoing with Prime Focus Instrument (PFI), Metrology Camera System (MCS), the first spectrpgraph module (SM1) with visible cameras and the first fiber cable providing optical link between PFI and SM1. Among the rest of the hardware, the second fiber cable has been already installed on the telescope and in the dome building since April 2022, and the two others were also delivered in June 2022. The integration and test of next SMs including near-infrared cameras are ongoing for timely deliveries. The progress in the software development is also worth noting. The instrument control software delivered with the subsystems is being well integrated with its system-level layer, the telescope system, observation planning software and associated databases. The data reduction pipelines are also rapidly progressing especially since sky spectra started being taken in early 2021 using Subaru Nigh Sky Spectrograph (SuNSS), and more recently using PFI during the engineering observations. In parallel to these instrumentation activities, the PFS science team in the collaboration is timely formulating a plan of large-sky survey observation to be proposed and conducted as a Subaru Strategic Program (SSP) from 2024. In this article, we report these recent progresses, ongoing developments and future perspectives of the PFS instrumentation.
PFS (Prime Focus Spectrograph), a next generation facility instrument on the Subaru telescope, is a very wide- field, massively multiplexed, and optical and near-infrared spectrograph. Exploiting the Subaru prime focus, 2394 reconfigurable fibers will be distributed in the 1.3 degree-diameter field of view. The spectrograph system has been designed with 3 arms of blue, red, and near-infrared cameras to simultaneously deliver spectra from 380nm to 1260nm in one exposure. The instrumentation has been conducted by the international collaboration managed by the project office hosted by Kavli IPMU. The team is actively integrating and testing the hardware and software of the subsystems some of which such as Metrology Camera System, the first Spectrograph Module, and the first on-telescope fiber cable have been delivered to the Subaru telescope observatory at the summit of Maunakea since 2018. The development is progressing in order to start on-sky engineering observation in 2021, and science operation in 2023. In parallel, the collaboration is trying to timely develop a plan of large-sky survey observation to be proposed and conducted in the framework of Subaru Strategic Program (SSP). This article gives an overview of the recent progress, current status and future perspectives of the instrumentation and scientific operation.
We report the current status of the laser guide star upgrade at Subaru Telescope with a new, more powerful TOPTICA/MPBC laser. While we recycle many of our existing components, such as laser launch telescope, we need to design a new mirror-based laser relay system to replace the current fiber-based relay to accommodate the high power beam. The laser unit has been delivered to Subaru office in March 2018 and installed in a testing lab in June 2018. We describe the preliminary design and its requirements and report future plans. This upgrade will not only improve our current adaptive optics system but also be the first step toward the future laser tomography and ground layer adaptive optics system at Subaru Telescope.
In 2014 and 2015 the Multi-Object InfraRed Camera and Spectrograph (MOIRCS) instrument at the Subaru Telescope on Maunakea is underwent a significant modernization and upgrade project. We upgraded the two Hawaii2 detectors to Hawaii2-RG models, modernized the cryogenic temperature control system, and rewrote much of the instrument control software. The detector upgrade replaced the Hawaii2 detectors which use the Tohoku University Focal Plane Array Controller (TUFPAC) electronics with Hawaii2-RG detectors using SIDECAR ASIC (a fully integrated FPA controller system-on-a-chip) and a SAM interface card. We achieved an improvement in read noise by a factor of about 2 with this detector and electronics upgrade. The cryogenic temperature control upgrade focused on modernizing the components and making the procedures for warm up and cool down of the instrument safer. We have moved PID control loops out of the instrument control software and into Lakeshore model 336 cryogenic temperature controllers and have added interlocks on the warming systems to prevent overheating of the instrument. Much of the instrument control software has also been re-written. This was necessitated by the different interface to the detector electronics (ASIC and SAM vs. TUFPAC) and by the desire to modernize the interface to the telescope control software which has been updated to Subaru's "Gen2" system since the time of MOIRCS construction and first light. The new software is also designed to increase reliability of operation of the instrument, decrease overheads, and be easier for night time operators and support astronomers to use.
During the past year, the Multi-Object InfraRed Camera and Spectrograph at Subaru has undergone an upgrade of its science detectors, the housekeeping electronics and the instrument control software. This overhaul aims at increasing MOIRCS' sensitivity, observing efficiency and stability. Here we present the installation and the alignment procedure of the two Hawaii 2RG detectors and the design of a cryogenic focus mechanism. The new detectors show significantly lower read noise, increased quantum efficiency, and lower the readout time.
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