Multi-object spectroscopy (MOS) is a technique in astronomy that allows for the simultaneous acquisition of multiple celestial objects spectra within a single field of view; this is an enabling capability for the next generation of NASA’s missions, including the Habitable Worlds Observatory and beyond. As part of previous NASA-funded technology maturation efforts, we have demonstrated that multi-object spectroscopy in space could be performed with a digital micromirror device (DMD) - a commercial micromirror array designed for display applications. Building on those efforts, we began a NASA APRA program to build the Spectroscopic Ultraviolet Multi-Object Observatory (SUMO) Prototype (a DMD-based spectrograph) with the intention to deploy it in the space environment as a secondary payload on the University of Colorado Boulder sounding rocket INFUSE. This will be the first time a DMD-based instrument is operated in space. The SUMO Prototype consists of: a DMD manufactured by Texas Instruments, an off-the-shelf camera for the imaging channel, a custom NUV CCD camera developed in-house at the Laboratory for Atmospheric and Space Physics (LASP) for the spectral channel, a Raspberry Pi for the on board computer, a custom controller for the DMD, and an electrical power system (EPS) powering the entirety of the SUMO prototype. This system has the requirement of being controlled autonomously, as the system is a secondary payload on the sounding rocket without downlinking capability. The research involved on this mission includes efforts to understand the processes of star formation and galaxy evolution. The SUMO Prototype is nominally scheduled for flight in the Spring of 2025.
SPRITE (Supernova Remnants and Proxies for Reionization Testbed Experiment) is a 12U CubeSat mission funded by NASA and led by the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado, Boulder. The payload will house the first sub-arcminute resolution Far-Ultraviolet (FUV) long-slit spectrograph with access to the Lyman UV (912 − 1216 Å), enabled by new enhanced lithium fluoride coatings and an ultra-low-noise photon-counting microchannel plate (MCP) detector. The scientific mission has two main components: constraining the escape fraction of ionizing Lyman-Continuum (LyC) radiation from low-redshift galaxies (0.14 ≤ z ≤ 0.4) and measuring feedback from nearby star forming regions and supernova remnants. Enabling the scientific mission are two distinct observing modes. For the faintest sources, we will operate the MCP detector in photon-counting mode. For brighter sources, we will operate the MCP in an accumulation / integration mode. For extended sources we will collate multiple pointings of the long slit, stepping across the field of view in a ‘push broom’ mapping to create 3D spectroscopic cubes. SPRITE will also take weekly calibration data to characterize the degradation of the coatings and detector. We present these observing modes along with the data acquisition and processing pipeline required to enable scientific analysis on the ground.
We present the optical design and testing of SPRITE, a 12U CubeSat being developed by the Laboratory of Atmospheric and Space Physics (LASP). SPRITE is designed to observe supernova remnants and low redshift galaxies in the far ultraviolet range (1000-1750 Å). SPRITE consists of an 18 x 16 cm parabolic primary mirror, a hyperbolic secondary mirror, an aberration-correcting concave holographic grating, a cylindrical fold mirror, and an advanced borosilicate glass Microchannel Plate (MCP) detector. The grating, secondary mirror (M2) and cylindrical fold mirror (M3) are coated with enhanced reflectivity lithium fluoride (LiF) protected aluminum, or “eLif”, capped with a thin overcoat of MgF2 for protection of the hygroscopic LiF from water vapor. SPRITE is serving as an orbital testbed for protected eLiF and boroscilicate glass MCP detectors ahead of potential adoption on a future NASA flagship mission, like the Habitable Worlds Observatory (HWO). This paper details the actions taken to protect the optics, as well as the MCP, as they are sensitive to molecular contamination and water vapor. We also detail the experimental setup for monitoring the reflectance of witness samples throughout the SPRITE integration and testing phase. Due to the unique nature of SPRITE, custom hardware for storage and optical testing was required to provide sufficient protection for the sensitive optics and detector. These facilities are essential for proving these new technologies for future flight programs, as well as ensuring SPRITE meets the science requirements. The coatings used on SPRITE’s optics are critical for the development of future large astronomy missions with high throughput down to 1000 angstroms.
The SPRITE (The Supernova remnants, Proxies for Re-Ionization Testbed Experiment) 12U CubeSat mission, funded by NASA and led by the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado Boulder, will house the first Far-UV (100-175 nm) long-slit spectrograph with access to the Lyman UV (λ ⪅ 115 nm) and sub-arcminute imaging resolution. SPRITE will map the high energy emission from diffuse gas allowing for the study of star formation feedback in a critical, but rarely studied, Far-UV regime on both stellar and galactic scales. This novel capability is enabled by new UV technologies incorporated into SPRITE’s design. These technologies include more robust, high broadband reflectivity mirror coatings and an ultra-low background photon counting microchannel plate detector. The SPRITE science mission includes weekly calibration observations to characterize the performance of these key UV technologies over time, increasing their technology readiness level (TRL) to 7+ and providing flight heritage essential for future UV flagship space missions such as the Habitable Worlds Observatory (HWO). Currently, SPRITE is in the beginning stages of integration and testing of its flight assembly with a planned delivery date of fall of 2024. This proceeding will overview the current mission status, the schedule for testing and integration prior to launch, and the planned mission operations for SPRITE.
SPRITE is a NASA far-UV telescope and spectrograph being designed and assembled at the Laboratory for Atmospheric and Space Physics (LASP). SPRITE’s mission is UV astrophysics in the 1000 - 1750 Angstroms spectral regime. SPRITE will observe low-redshift galaxies, as well as supernova remnants in the Milky Way. SPRITE’s complex science payload is extremely constrained by the volume allocation of the 12U CubeSat form factor. Our solution to deal with SPRITE's volume constraints, is to fabricate solar panels with a high fill factor. With only three deployable single-hinge panels and one body-mounted panel, SPRITE is able to generate 8.5 to 9.7 Watts of power when fully illuminated, using 45 Azur Space AG30A solar cell assemblies. SPRITE is currently finishing the integration and testing phase of its program, with a launch manifested for August 2024.
We present the design of the Spectroscopic Ultraviolet Multi-object Observatory (SUMO) prototype and our plan to deploy this instrument on the INFUSE sounding rocket as an independent fly-along instrument. The SUMO prototype is part of the technology maturation program of SUMO - a mission concept designed for a future small satellite platform. SUMO is designed for astrophysics research in the Far-Ultraviolet (FUV) and Near-Ultraviolet (NUV) regimes encapsulating a wide range of programs, including efforts to understand the processes of star formation and galaxy evolution. Since the last major UV NASA missions, FUSE and GALEX, NASA has invested significantly into technology development for the UV bandpass. As a result, high reflectance mirror coatings and state-of-the-art detectors are now available. These technologies, along with the developed optical design, allow SUMO to achieve effective areas that are comparable to those achieved by FUSE and GALEX, at a fraction of the size and cost. The SUMO prototype consists of an 8 cm Cassegrain telescope and a Digital Micromirror Device (DMD)-based Multi-Object Spectrometer (MOS), with parallel imaging and spectroscopic channels. As part of this work, we are also developing a custom DMD controller, which is suitable for operation in the space environment. Given that current DMD-based spectrographs have been solely ground-based, this will be the first time a DMD-based instrument is deployed in space. Because the SUMO prototype will be deployed as a secondary payload, the spectrograph is also designed for completely autonomous operation. The SUMO prototype is tentatively scheduled for flight in 2025.
The INtegral Field Ultraviolet Spectroscopic Experiment (INFUSE), a sounding rocket payload under development by the Colorado Ultraviolet Spectroscopy Program (CUSP), will be the first far ultraviolet (100 nm to 200 nm) Integral Field Spectrograph (IFS) in space. With access to part of the Lyman ultraviolet (100.0 nm to 121.6 nm), INFUSE will be able to study spectral emission lines such as O VI in extended objects at greater spatial resolution and coverage than has previously been possible. An F/16, 0.49 m Cassegrain telescope feeds the instrument. A 26-element image slicer provided by Canon, Inc. forms the basis for the IFS. Each reflective slice acts as a long-slit, creating 26 different channels. Each channel is re-focused and dispersed by one of 26 identical holographic gratings supplied by Horiba JY onto the same 94 x 94 mm cross-strip (XS) microchannel plate detector (MCP). This MCP, provided by Sensor Sciences, will be the largest MCP of its type ever flown in space and will be advancing high event rate photon-counting detector technology for future NASA missions. We discuss the process and results of aligning the telescope and instrument, with a focus on the method by which the 26 gratings are aligned with the image slicer. Additionally, we examine the challenges the large primary mirror presented when being mounted and coated for flight. The first flight of INFUSE is schedule for October 2023 when it will spectroscopically image the XA region of the Cygnus Loop at the interface between the supernova and the ambient ISM, studying shock fronts in the supernova remnant.
The development of high reflectivity, protective mirror coatings for the Lyman UV (λ < 120 nm) is essential for enabling both CubeSats and large UVOIR missions to tap this rich bandpass. Aluminum mirrors with fluoride-based protective layers are the baseline UV coating technology; these mirrors have been proven to be stable, reliable, and with long flight heritage. However, despite their overall acceptable optical performance, the efficiency of current state-of-theart Al coatings is still insufficient in the 100-120 nm wavelength range for optical systems in which several reflections are required. Optimizing the efficiency down to 100 nm is essential for the viability and scientific return of the next generation of future FUV-sensitive space telescopes, as was called out in the 2020 astrophysics decadal survey. In this proceeding, we will present recent advances in the development of environmentally stable Al+eLiF+MgF2 mirrors deposited on substrates with increasing thicknesses, developed for the SPRITE CubeSat. SPRITE is projected to be the most sensitive instrument to date in the 100 - 120 nm range and the first orbital imaging spectrograph for this bandpass with sub-arcminute resolution.
The thermal analysis of the SPRITE astrophysics CubeSat will be presented. As a far-UV instrument with a precision telescope, thermal control is essential to maintain instrument focus as well as to limit molecular contamination on the optics. A thermal model was created in Thermal Desktop to simulate the conductive and radiative heat transfer effects the components will experience during the mission. Mission specific orbital and attitude parameters were also incorporated to increase model fidelity. Several model parameters were created to simulate the most extreme temperature variations SPRITE would experience. A 'cold' case and a 'hot' case were created for charging and science attitudes, utilizing the bounds of recorded Earth albedo, solar flux, and IR Planetshine values. The results of these models are presented and outline the passive and active thermal control steps that will be employed by the SPRITE team to meet requirements.
The INtegral Field Ultraviolet Spectroscopic Experiment (INFUSE), a sounding rocket payload under development at the University of Colorado Laboratory for Atmospheric and Space Physics, will be the first far ultraviolet (1000 - 2000 A° ) integral field spectrograph (IFS) in space. With access to part of the Lyman ultraviolet (1000 - 1216 A° ), INFUSE will study spectral emission lines such as O VI in extended objects at greater spatial resolution and grasp than has previously been possible. An F/16, 0.49 m Cassegrain telescope feeds the instrument. A 26-element image slicer provided by Canon Inc. forms the basis for the IFS. Each reflective slice acts as a long-slit, creating 26 different channels. Each channel is re-focused and dispersed by one of 26 identical holographic gratings supplied by Horiba JY onto the same 94 x 94 mm cross-strip (XS) microchannel plate detector (MCP). This MCP, provided by Sensor Sciences, will be the largest MCP of its type ever flown in space and will be advancing high event rate photon-counting detector technology for future NASA missions. We discuss the process of aligning the instrument, with a focus on the method by which the 26 gratings are aligned with the image slicer. Additionally, we examine the challenges presented by mounting and coating the large primary mirror and the steps taken to ensure that the mirror remains stable in flight. The first flight of INFUSE is projected for Spring 2023 when it will spectroscopically image the XA region of the Cygnus Loop at the interface between the supernova and the ambient ISM, studying shock fronts in the supernova remnant.
We present the design of the Spectroscopic Ultraviolet Multi-object Observatory (SUMO), a small satellite mission concept for astrophysics research. SUMO's science instrument is a multi-object spectrograph based on a customized digital micromirror device (DMD). Like other DMD-based spectrographs, SUMO employs parallel imaging and spectroscopic channels. The imaging channel operates in the NUV range and covers a field of view of 2.5 square degrees, with a spatial resolution of 5 arcseconds. The spectrograph channel is designed to achieve a resolving power of R~2500, operating in the range of 140 - 200 nm. The imaging and spectroscopic channels employ a CCD detector and a microchannel plate detector, respectively. Recent advances in satellite bus technology and a wave of successful NASA-funded technology development programs allow SUMO to achieve an effective area comparable to much larger missions of the past.
SPRITE, the first NASA-funded 12U CubeSat for astrophysics science, will use an ultraviolet light spectrograph with a photon-counting microchannel plate detector to provide spatial and spectral data on the light observed from low-redshift galaxies, active galactic nuclei, and shocked emission features of supernova remnants in the 1000Å − 1750Å bandpass. This proceedings describes recent progress on the design, implementation, and experimental evaluation of SPRITE’s electrical subsystems, particularly the high voltage power supply required to drive the microchannel plate detector. Measured experimental results for the commercial high voltage power supply module and the electronics board designed and built to control it are presented and discussed. The average voltage and voltage ripple of the high voltage power supply output when driving a resistive load that simulates the load anticipated on orbit due to the detector and a parallel voltage divider are presented. Planned revisions to the SPRITE electronics design are discussed, including modifications to be made to the high voltage power supply control board and the addition of an electronics board to handle all the interfaces between the command and data handling subsystem and the instrument electrical subsystems. SPRITE is planned to launch in early 2023 and will provide on-orbit data for the microchannel plate detector and other technologies onboard that are candidates for use on future large missions.
Slated to launch in early 2023, Supernova Remnants and Proxies for Re-Ionization Testbed Experiment (SPRITE) is the first NASA funded 12U astrophysics CubeSat payload and the first orbital astrophysics instrument to operate in the windowless Far-ultraviolet (1000 - 1750 Å) since the deployment of HST-COS. SPRITE is an imaging spectrograph with 10 arcsecond angular resolution, breaking new ground with scientific observations enabled by a compact microchannel plate detector system and advanced protected eLiF mirror coatings baselined for the LUVOIR Surveyor. To provide flexibility and customizability the spacecraft bus and spectrograph are all being designed in house at the Laboratory for Atmospheric and Space Physics. SPRITE features several unique mechanical subsystems such as the pump/purge system for the hermetically sealed detector housing, the release mechanism for the detector door, the release mechanism for the solar array, the solar panel design, and compact rectangular telescope. SPRITE's mechanical design meets all science requirements, the CubeSat specific requirements of commercial 12U dispenser systems, and NASA orbital debris limits. We present an overview of the design and development of the mechanical systems and mechanisms for SPRITE prior to the comprehensive design review (CDR).
Improving the spectral multiplexing efficiency of ultraviolet (UV) instruments is one of the essential technology developments for future large missions. This is particularly hard in the far UV (FUV), where high reflectivity coatings and high material transmission are difficult to achieve. We present here the concept and design of the Ultraviolet Micromirror Imaging Spectrograph (UMIS), which utilizes Analog Micromirror Arrays (AMAs) as the spectral multiplexing element. These Micro-Opto-Electro-Mechanical-Systems (MOEMS)-based mirrors can be dynamically programmed to probe multiple points of interest across a wide field of view without spectral confusion limitations. We have assembled a benchtop version of UMIS, to characterize the individual arrays and to evaluate the performance of the overall system in optical and FUV wavelengths. The instrument consists of a 75 cm off-axis telescope, with two AMAs placed on either side of the focal plane, and an optical spectrograph with a resolution of about R=1000. The individual mirror orientations can be adjusted by varying their bias voltages, which are controlled using custom electronic boards designed and fabricated by Ball Aerospace and LASP. The same testbed will be reconfigured with an FUV grating and detector, to calibrate the instrument in a vacuum environment and qualify the AMAs for future flight missions.
Digital micromirror devices (DMDs) can be used as versatile, rapidly reconfigurable object selectors in spacebased multi-object spectrographs (MOS). DMDs are inexpensive, compact, reliable, high-throughput devices, that enable extremely flexible and efficient multi-object spectrographs; several DMD-based MOSs are currently being built for 4 m class ground-based telescopes. Previously, we have shown that DMDs are suitable for deployment and operation in space, in the near-UV and optical regimes (200 - 1000 nm). Using aluminum coatings protected with LiF and LiF/AlF3 films, we aim to extend the operational range of DMDs into the 100 - 200 nm FUV regime. Our initial coating runs produced DMDs with reflectivity > 40% in the range of 110 - 180 nm. Critically, the DMDs remain operational after the coating process. We will discuss potential for further improvement and introduce several mission concepts based on a FUV/NUV DMD MOS, that can be deployed on CubeSat and ESPA-class missions.
The INtegral Field Ultraviolet Spectroscopic Experiment (INFUSE) is a sounding rocket under sounding rocket under development by the Colorado Ultraviolet Spectroscopy Program (CUSP) at the University of Colorado. INFUSE will be the first far-ultraviolet (1000 - 2000 Å) integral field spectrograph in space and will have ˚ access to a portion of the Lyman ultraviolet (912 Å– 1216Å). This instrument leverages the development of ˚ enhanced lithium fluoride (eLiF) mirror coatings, which are roughly 30% more reflective than the conventional LiF+Al coatings used on previous missions. The integral field spectrograph is enabled by an 26-element image slicer precision machined by Canon Inc., with each element acting as a reflective long-slit. Each channel is re-focused and dispersed by one of 26 identical holographic gratings onto the same 94 x 94 mm XS MCP. This will be the largest cross-strip (XS) borosilicate microchannel plate detector yet deployed in space. INFUSE will spectroscopically image the XA region of the Cygnus Loop at the interface between the supernova and the ambient ISM. The first flight of INFUSE is projected for early 2023.
Planned to launch in 2022, SPRITE is the first NASA-funded 12U cubesat for astrophysics science. SPRITE is equipped with unique hardware for a cubesat that enables it to simultaneously perform underexplored astrophysical observations and serve as a testbed to evaluate the in-space performance of experimental technologies that are candidates for implementation on future large missions. SPRITE will observe ultraviolet light from low-redshift galaxies and other targets of interest to provide data on emissions from these targets in a bandpass that has not been investigated exhaustively to date. An ultraviolet light photon-counting borosilicate glass microchannel plate detector is one of the experimental components that is unique to SPRITE among cubesats, and it motivates the uncommon requirement for a high voltage power supply on the particularly volume-limited spacecraft platform. This proceedings describes SPRITE’s electrical subsystems with a focus on the payload electronics that directly enable its science objectives with particular attention given to the design and planned laboratory experimental validation of the high voltage power supply needed to drive the detector. The planned Time-Tag and Accumulate data acquisition modes and the data products of these routines are also discussed.
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