The Suborbital Imaging Spectrograph for Transition region Irradiance from Nearby Exoplanet host stars (SISTINE) is a rocket-borne ultraviolet (UV) imaging spectrograph designed to probe the radiation environment of nearby stars. SISTINE operates over a bandpass of 98 to 127 and 130 to 158 nm, capturing a broad suite of emission lines tracing the full 104−105 K formation temperature range critical for reconstructing the full UV radiation field incident on planets orbiting solar-type stars. SISTINE serves as a platform for key technology developments for future ultraviolet observatories. SISTINE operates at moderate resolving power (R∼1500), while providing spectral imaging over an angular extent of ∼6′, with ∼2″ resolution at the slit center. The instrument is composed of an f/14 Cassegrain telescope that feeds a 2.1× magnifying spectrograph, utilizing a blazed holographically ruled diffraction grating and a powered fold mirror. Spectra are captured on a large format microchannel plate (MCP) detector consisting of two 113×42 mm segments each read out by a cross-delay line anode. Several novel technologies are employed in SISTINE to advance their technical maturity in support of future NASA UV/optical astronomy missions. These include enhanced aluminum lithium fluoride coatings (eLiF), atomic layer deposition (ALD) protective optical coatings, and ALD-processed large-format MCPs. SISTINE was launched a total of three times with two of the three launches successfully observing targets Procyon A and α Centauri A and B.
The MANTIS (Monitoring Activity of Nearby sTars with uv Imaging and Spectroscopy) 16U CubeSat mission, led by the Laboratory for Atmospheric and Space Physics (LASP) at the University of Colorado Boulder, plans to characterize the high-energy stellar radiation that drives atmospheric photochemistry and escape on extrasolar planets by conducting simultaneous observations of exoplanet host stars at extreme-ultraviolet (100–1200A; EUV), far-ultraviolet (1300–2200A; FUV), near-ultraviolet (2200–3500A; NUV), and visible (3500–10000A; VIS) wavelengths. The science payload's two-telescope design enables simultaneous coverage over the entire UV passband and the first EUV astrophysics capability in over 20 years. An 8.5cm diameter grazing incidence telescope feeds a low-resolution EUV spectrograph while a 14x9cm rectangular Cassegrain telescope feeds a dichroic beamsplitter to divide the light into both an NUV/VIS and FUV channel. The MANTIS design, detector systems, spacecraft bus and mission operations build off of the heritage of the CUTE and SPRITE CubeSats developed by the MANTIS team. This proceeding overviews the design of the MANTIS instrument and general mission concept.
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.
The Far- and Lyman-ultraviolet imaging demonstrator (FLUID) is a rocket-borne arcsecond-level ultraviolet (UV) imaging instrument covering four bands between 92 and 193 nm. FLUID will observe nearby galaxies to find and characterize the most massive stars that are the primary drivers of the chemical and dynamical evolution of galaxies and the co-evolution of the surrounding galactic environment. The FLUID short wave channel is designed to suppress efficiency at Lyman-α (121.6 nm) while enhancing the reflectivity of shorter wavelengths. Utilizing this technology, FLUID will take the first ever images of local galaxies isolated in the Lyman UV (90–120 nm). As a pathfinder instrument, FLUID will employ and increase the technology readiness level of band-selecting UV coatings and solar-blind UV detector technologies, including microchannel plate and solid-state detectors; technologies that are prioritized in the 2022 NASA Astrophysical Biennial Technology Report. These technologies enable high throughput and high sensitivity observations in the four co-aligned UV imaging bands that make up the FLUID instrument. We present the design of FLUID, status on the technology development, and results from initial assembly and calibration of the FLUID instrument.
We present laboratory reflectivity results of two novel optical filters designed for the Lyman ultraviolet bandpass (LUV; 90-120 nm) and the far ultraviolet bandpass (FUV; 120-150 nm). These filters were developed in coordination with the Grupo de Óptica de Láminas Delgadas (GOLD) at the Instituto de Óptica-Consejo Superior de Investigaciones Cientìficas for the Far- and Lyman-Ultraviolet Imaging Demonstrator (FLUID) sounding rocket payload. In addition to maturing high priority band-selecting UV filter technology, FLUID will measure the LUV and far ultraviolet (FUV; 120-200 nm) morphologies of nearby galaxies in four imaging bands to provide local analogs for JWST observations of high redshift galaxies. Images in the LUV will be used to make the first ever morphological classifications of local galaxies in this bandpass. FLUID comprises four f /28.7 Cassegrain telescopes with ⪅3 arcsecond angular resolution over a 20 arcminute wide field-of-view. Each telescope receives a unique band-defining filter covering the LUV through FUV (approximately 15 nm FWHM band centered on 105 nm, and 20 nm FWHM bands centered on 140 nm, 160 nm, or 180 nm). These filters are multilayer reflectance filters, and were developed by GOLD in collaboration with CU Boulder. Evaluation of the F140M filter and the Lyman alpha (Ly-α; 121.6 nm) suppressing F110M filter witness samples, as well as the secondary and primary mirrors, were completed with optical testing facilities at both GOLD and CU. We present the measured efficiencies of the F110M optics, which all demonstrate reflectivites ⪅3% at Ly-α while maintaining ⪆40% reflectivity at 105 nm, and the F140M optics, which show show peak reflectivities for 140 nm greater than 87%. These values are used to estimate the performance of the FLUID instrument in this band. Additionally we will conduct further testing of all four filters, as well as testing age and environmental stability of the filters over the course of the project.
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.
The Far-and Lyman-Ultraviolet Imaging Demonstrator (FLUID) is a rocket-borne multi-band arcsecond-level Ultraviolet (UV) imaging instrument covering four bands between 92 – 193 nm. FLUID will observe nearby galaxies to find and characterize the most massive stars, the primary drivers of the chemical and dynamical evolution of galaxies, and the co-evolution of the surrounding galactic environment. The FLUID short wave channel is designed to suppress efficiency at Lyman alpha wavelengths, while enhancing the reflectivity of shorter wavelengths. Utilizing this technology, FLUID will take the first ever images of local galaxies isolated in the Lyman ultraviolet. As a pathfinder instrument, FLUID will employ and increase TRL of band-selecting UV coatings, and solar-blind UV detector technologies including microchannel plate and solid-state detectors; technologies prioritized in the 2022 NASA Astrophysical Biennial Technology Report. These technologies enable high throughput and high sensitivity observations in four co-aligned UV imaging bands that make up the FLUID instrument. We present the design of FLUID, status on the technology development, and results from initial assembly and calibration of the FLUID instrument.
The Suborbital Imaging Spectrograph for Transition-region Irradiance from Nearby Exoplanet host stars (SISTINE) is a rocket-borne imaging spectrograph designed to probe a broad region of the far-ultraviolet (FUV; 976-1272, 1300-1565 Å) emission of nearby stars. The instrument is composed of an f /14 Cassegrain telescope feeding a 2.1x magnifying spectrograph with a blazed, holographically ruled diffraction grating and a powered fold mirror. The telescope optics employ enhanced-lithium fluoride overcoated Al, with the secondary mirror providing the first flight test of hot-deoposition LiF coatings employing an ALD deposited aluminum trifluoride (Al + LiF + AlF3) capping layer. Spectra are captured on a large-format microchannel plate detector consisting of two 110 x 40 mm segments. The third flight of SISTINE was successfully executed on July 6th, 2022, from Arnhem Space Center (ASC), Northern Territory, Australia. SISTINE-3 successfully obtained FUV spectra of α Centauri A and B, fully resolving the binary pair with a 7” separation on sky. The spectra contain a suite of FUV emission lines crucial for reconstructing the high-energy stellar radiation incident onto planets orbiting solar-mass stars. We present the pre-flight calibration at the University of Colorado Boulder, including predicted performance, effective area, and resolving power; the integration and assembly performed at NASA Wallops Flight Facility (WFF) and ASC; and preliminary science results from the in-flight data.
The Colorado Ultraviolet Transit Experiment (CUTE) is a 6U cubesat housing a Cassegrain telescope and a nea rultraviolet (NUV) spectrograph designed to study the composition and mass-loss rates of exoplanet atmospheres. This instrument covers a bandpass of 250 - 330 nm with a peak effective area of ~28 cm2 and a resolving power of ~2000. The instrument focal plane consists of a back illuminated CCD driven by clocking and readout electronics developed at the Laboratory for Atmospheric and Space Physics (LASP). Special consideration is given to achieving low noise readout due to typical observation signal levels and time constraints of exoplanet transit observations. Additionally, the electronics driving the CCD are space constrained and designed to fit in a cubesat 1/2U volume. Prior to installation in the flight instrument the detector system parameters are optimized and characterized at LASP in a custom ultraviolet detector test chamber. Engineering and technical details including system gain, quantum efficiency, and read noise are discussed. We present the development, optimization, and characterization results of the CCD and associated readout electronics developed for the CUTE instrument.
The Colorado Ultraviolet Transit Experiment (CUTE) is a 6U CubeSat designed to explore the upper atmospheres of short-period exoplanets via near-ultraviolet (2500 – 3300 Å) transmission spectroscopy, with an anticipated launch date of September 2021. The 4U science instrument comprises a Cassegrain telescope with a 20 × 8 cm primary mirror, a spectrograph, and a thermal-electrically cooled CCD detector. The spacecraft structure and a 1.5U XB1 avionics module are provided by Blue Canyon Technologies. CUTE’s novel and compact instrument design presents unique challenges to conducting component-level testing, alignment, instrument and spacecraft integration, calibration, and end-to-end performance testing. We provide a description of several custom test setups and procedures designed to characterize the spectrograph performance and its expected science return. We also outline the remainder of our integration and testing plan.
The SPRITE cubesat is a recently selected NASA astrophysics mission designed to measure ionizing radiation escape from star-forming galaxies, and to map far-ultraviolet (1000 - 1750 Å) emission from shocked regions in supernova remnants. The instrument leverages a number of new technologies identified for future large mission concepts, including the LUVOIR surveyor, to achieve the required performance. These include high broadband reflectivity mirror coatings and an ultra-low background photon counting microchannel plate detector with an anti-coincidence particle rejection system. SPRITE will serve as a flight testbed for these technologies, employing a robust calibration program as part of the principal science mission to advance the technology readiness level (TRL) to 7+ and provide heritage for future Explorer-class and larger missions. SPRITE is a 6U class cubesat funded through NASA ROSES with an anticipated launch date in 2022. The science data products will be archived on the Mikulski Archive for Space Telescopes (MAST). This proceedings describes the instrument science program, optical design, preliminary performance projections, and project timeline.
The Colorado Ultraviolet Transit Experiment (CUTE) is a near-UV (NUV), 6U CubeSat designed to characterize the interaction between exoplanetary atmospheres and their host stars. CUTE is dedicated to observing multiple transits of short period planets with a range of masses to measure the transit depths of atomic and molecular nearUV features. These observations will enable us to quantify as a function of wavelength the transit ingress, egress, and depth of exoplanet light curves in order to determine the presence of bow shocks and strong atmospheric mass loss. The CUTE optical system combines a novel rectangular Cassegrain telescope and a holographically-ruled, aberration-correcting diffraction grating. The high-throughput optical system is projected to obtain an average effective area of ≈24 cm2 , comparable to previous Explorer class missions (GALEX) in a CubeSat package. This proceeding provides an overview of the science motivation, the final telescope and spacecraft design, and an outline of the mission operation.
In this proceeding, we describe the scientific motivation and technical development of the Colorado Highresolution Echelle Stellar Spectrograph (CHESS), focusing on the hardware advancements and testing of components for the fourth and final launch of the payload (CHESS-4). CHESS is a far ultraviolet rocket-borne instrument designed to study the atomic-to-molecular transitions within translucent cloud regions in the interstellar medium. CHESS is an objective echelle spectrograph, which uses a mechanically-ruled echelle and a powered (f/12.4) cross-dispersing grating; it is designed to achieve a resolving power R > 100,000 over the band pass λλ 1000–1600 Å. CHESS-4 utilizes a 40 mm-diameter cross-strip anode readout microchannel plate detector, fabricated by Sensor Sciences LLC, to achieve high spatial resolution with high global count rate capabilities (∼ MHz). An error in the fabrication of the cross disperser limited the achievable resolution on previous launches of the payload to R ∼ 4000. To remedy this for CHESS-4, we physically stress the echelle grating, introducing a shallow toroidal curvature to the surface of the optic. Preliminary laboratory measurements of the resulting spectrum show a factor of 4–5 improvement to the resolving power. Results from final efficiency and reflectivity measurements for the optical components of CHESS-4 are presented, along with the pre-flight laboratory spectra and calibration results. CHESS-4 launched on 17 April 2018 aboard NASA/University of Colorado Boulder sounding rocket mission 36.333 UG. We present flight results for the observation of the γ Ara sightline.
In this proceeding, we describe the scientific motivation and technical development of the Colorado HighResolution Echelle Stellar Spectrograph (CHESS), focusing on the hardware advancements and testing of components for the third launch of the payload (CHESS-3). CHESS is a far ultraviolet rocket-borne instrument designed to study the atomic-to-molecular transitions within translucent cloud regions in the interstellar medium. CHESS is an objective echelle spectrograph, which uses a mechanically-ruled echelle and a powered (f/12.4) crossdispersing grating, and is designed to achieve a resolving power R > 100,000 over the bandpass λλ 1000−1600 Å. Results from final efficiency and reflectivity measurements for the optical components of CHESS-3 are presented. An important role of sounding rocket experiments is the testing and verification of the space flight capabilities of experimental technologies. CHESS-3 utilizes a 40mm-diameter cross-strip anode microchannel plate detector fabricated by Sensor Sciences LLC, capable of achieving high spatial resolution and a high global count rate (∼1 MHz). We present pre-flight laboratory spectra and calibration results, including wavelength solution and resolving power of the instrument. The fourth launch of CHESS (CHESS-4) will demonstrate a δ-doped CCD, assembled in collaboration with the Microdevices Laboratory at JPL and Arizona State University. In support of CHESS-4, the CHESS-3 payload included a photomultiplier tube, used as a secondary confirmation of the optical alignment of the payload during flight. CHESS-3 launched on 26 June 2017 aboard NASA/CU sounding rocket mission 36.323 UG. We present initial flight results for the CHESS-3 observation of the β1 Scorpii sightline.
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