Astronomy at far-infrared (far-IR) wavelengths is essential to our understanding of the evolution of the cosmos, from the star formation history of galaxies to how the ice distribution affects the formation of extrasolar planetary systems. The Hubble Space Telescope, James Webb Space Telescope, and the Atacama Large Millimeter Array have already produced ground-breaking astronomical observations with high angular resolution spanning the visible to sub-millimetre wavelength regimes. However, this presents a gap in the far-IR, from roughly 30−400μm, where ground-based observations are largely intractable due to the opacity of Earth’s atmosphere. Indeed, no telescope, observatory, or interferometry array has ever achieved sub-arcsecond angular resolution over this wavelength range. A space-based solution is needed. However, a space-based far-IR telescope capable of subarcsecond angular resolution and high sensitivity, at a cost comparable to the largest space missions to date, presents unique physical, practical, and engineering challenges. In this paper, we envisage what a far-IR Great Observatory class mission might look like in the context of the already-studied Origins Space Telescope (OST) and the Space Infrared Interferometric Telescope (SPIRIT). We begin with a historical reflection of far-IR missions, including OST and the recommendations by the Astro2020 Decadal Survey for a de-scoped mission. We use this to motivate the recommendation of a space-based interferometer as a reasonable path towards sub-arcsecond angular resolution at far-IR wavelengths. Using the SPIRIT mission concept as inspiration, we consider multiple point designs for a two element, structurally connected spatial-spectral space-based far-IR interferometer to understand the implications on achieved angular resolution and estimate total mission cost in context of the Decadal Survey recommended far-IR Great Observatory cost cap. This paper illustrates the unique capabilities only possible through a space-based far-IR double Fourier interferometry mission capable of sub-arcsecond resolution.
The Far-Infrared (FIR; 25−350μm) band remains relatively unexplored in astronomy despite its importance for studying the formation and evolution of planets, stars, and galaxies. One factor which limits FIR observing capabilities is the impractically large single aperture telescopes that would be required to achieve the sub-arcsecond angular resolution that has been obtained in the optical and radio bands. A Double-Fourier Interferometer (DFI) has been proposed, which combines both a spatial interferometer and a Fourier Transform Spectrometer (FTS). Such an instrument, however, is lacking in experimental validation. This work contributes to DFI development by demonstrating the technique for a simple, spectrally uniform source.
The Large Interferometer For Exoplanets (LIFE) is a proposed space mission that enables the spectral characterization of the thermal emission of exoplanets in the solar neighborhood. The mission is designed to search for global atmospheric biosignatures on dozens of temperate terrestrial exoplanets and it will naturally investigate the diversity of other worlds. Here, we review the status of the mission concept, discuss the key mission parameters, and outline the trade-offs related to the mission’s architecture. In preparation for an upcoming concept study, we define a mission baseline based on a free-formation flying constellation of a double Bracewell nulling interferometer that consists of 4 collectors and a central beam-combiner spacecraft. The interferometric baselines are between 10–600m, and the estimated diameters of the collectors are at least 2m (but will depend on the total achievable instrument throughput). The spectral required wavelength range is 6–16μm (with a goal of 4–18.5μm), hence cryogenic temperatures are needed both for the collectors and the beam combiners. One of the key challenges is the required deep, stable, and broad-band nulling performance while maintaining a high system throughput for the planet signal. Among many ongoing or needed technology development activities, the demonstration of the measurement principle under cryogenic conditions is fundamentally important for LIFE.
Far-infrared (far-IR) astronomical observations with sub-arcsecond angular resolution and high spectral resolution require a space-based interferometer observatory with baselines of at least tens of meters in length. The European-funded Far Infrared Space Interferometer Critical Assessment (FISICA) studied Far Infrared Interferometer (FIRI) in detail, and developed software simulation tools (FIInS and PyFIInS) for modeling a FIRI-like interferometer and simulating the hyperspectral output datacubes. Here we present on-going work expanding upon the foundations of FIInS and pyFIInS towards an end-to-end simulation software suite. The software tools presented in this work provide a framework with which to study double Fourier interferometry in the far-IR and allow the astronomical community further exploration of the unique capabilities of such instrumentation.
Double-Fourier interferometry (DFI) from a space-based platform provides a path to achieve broadband imaging spectroscopy in the far-infrared with sub-arcsecond angular resolution. To provide further study of the technique and improve its technology readiness, we have constructed a laboratory-based DFI testbed. This instrument is coupled to a custom array of 25 feedback-controlled transition-edge sensor (TES) bolometers. We present the results of characterisation experiments to optimise the detector system as an integrated component of the DFI assembly. We demonstrate that tuning the proportional-integral-derivative (PID) feedback control loops of the detectors and the timing of the multiplexed measurement process can modify the detector array’s noise performance and speed of response to optical modulation for this purpose. From these, we have determined a set of optimised detector settings that reduce spectral noise in the spatial-spectral interferometer by 37–79%. In addition, we present further thermal characterisation of the detector array.
A space-based far-infrared interferometer could work synergistically with the James Webb Space Telescope (JWST) and the Atacama Large Millimeter Array (ALMA) to revolutionize our understanding of the astrophysical processes leading to the formation of habitable planets and the co-evolution of galaxies and their central supermassive black holes. Key to these advances are measurements of water in its frozen and gaseous states, observations of astronomical objects in the spectral range where most of their light is emitted, and access to critical diagnostic spectral lines, all of which point to the need for a far-infrared observatory in space. The objects of interest – circumstellar disks and distant galaxies – typically appear in the sky at sub-arcsecond scales, which rendered all but a few of them unresolvable with the successful and now-defunct 3.5-m Herschel Space Observatory, the largest far-infrared telescope flown to date. A far-infrared interferometer with maximum baseline length in the tens of meters would match the angular resolution of JWST at 10x longer wavelengths and observe water ice and water-vapor emission, which ALMA can barely do through the Earth’s atmosphere. Such a facility was conceived and studied two decades ago. Here we revisit the science case for a space-based far-infrared interferometer in the era of JWST and ALMA and summarize the measurement capabilities that will enable the interferometer to achieve a set of compelling scientific objectives. Common to all the science themes we consider is a need for sub-arcsecond image resolution.
Prime-Cam is a first-generation instrument for the Cerro Chajnantor Atacama Telescope-prime (CCAT-prime) Facility. The 850 GHz module for Prime-Cam will probe the highest frequency of all the instrument modules. We describe the parameter space of the 850 GHz optical system between the Fλ spacing, beam size, pixel sensitivity, and detector count. We present the optimization of an optical design for the 850 GHz instrument module for CCAT-prime. We further describe the development of the cryogenic RF chain design to accommodate 30 readout lines to read 41,400 kinetic inductance detectors (KIDs) within the cryogenic testbed.
KEYWORDS: Sensors, Multiplexing, Signal to noise ratio, Modulation, Signal detection, Detector arrays, Field programmable gate arrays, Space operations, Time division multiplexing, Cryogenics
We describe the commissioning and operation of a 25 element Transition-Edge Sensor (TES) cryogenic detector array system for use in the far-infrared band of the electromagnetic spectrum. This detector system, supplied by QMC Instruments Limited, is an integral component to the development of a spatial/spectral double Fourier laboratory-based interferometer testbed instrument within the Astronomical Instrumentation Group laboratories at the University of Lethbridge, Canada. The 5x5 rectangular grid of TES elements is feedhorn-coupled and operates at ∼6K within a dedicated cryostat providing both optical and thermal shielding. Cryogenic cooling of ∼0.5W is provided by a CryoMech PT405RM/CP2850 pulse-tube cooler/compressor suite. The detector readout system uses time-division multiplexing controlled by a dedicated National Instruments field-programmable gate array board and computer interface. This paper describes the characterization and optimization of this detector system, including the evaluation and validation of the readout electronics, hardware, software, detector noise properties, the multiplexing parameter space, optical sensitivity, and the integration of this system within a laboratory testbed interferometer instrument.
Over half of the light incident on the Earth from the Universe falls within the Far-Infrared (FIR) region of the spectrum. Due to the deleterious effects of the Earth's atmosphere and instrument self-emission, astronomical measurements in the FIR require space-borne instrumentation operating at cryogenic temperatures. These instruments place stringent constraints on the mechanical and thermal properties of the support structures at low temperatures. With high stiffness, tensile strength, strength-to-mass ratio, and extremely low thermal conductivity, carbon fibre reinforced polymers (CFRPs) are an important material for aerospace and FIR astronomical applications, however, little is known about their properties at cryogenic temperatures. We have developed a test facility for exploring CFRP properties down to 4 K. We present results from our ongoing study in which we compare and contrast the performance of CFRP samples using different materials, and multiple layup configurations. Current results include an evaluation of a cryostat dedicated for materials testing and a custom cryogenic metrology system, and preliminary cryogenic thermal expansion measurements. The goal of this research is to explore the feasibility of making CFRP-based, lightweight, cryogenic astronomical instruments.
For over two decades, astronomers have considered the possibilities for interferometry in space. The first of these missions was the Space Interferometry Mission (SIM), but that was followed by missions for studying exoplanets (e.g Terrestrial Planet Finder, Darwin), and then far-infrared interferometers (e.g. the Space Infrared Interferometric Telescope, the Far-Infrared Interferometer). Unfortunately, following the cancellation of SIM, the future for space-based interferometry has been in doubt, and the interferometric community needs to reevaluate the path forward. While interferometers have strong potential for scientific discovery, there are technological developments still needed, and continued maturation of techniques is important for advocacy to the broader astronomical community. We review the status of several concepts for space-based interferometry, and look for possible synergies between missions oriented towards different science goals.
We describe the current status, including preliminary design, characterization efforts, and recent progress, in the development of a spatial/spectral double Fourier laboratory-based interferometer testbed instrument within the Astronomical Instrumentation Group (AIG) laboratories at the University of Lethbridge, Canada (UL). Supported by CRC, CFI, and NSERC grants, this instrument development will provide laboratory demonstration of spatial-spectral interferometry with a concentration of furthering progress in areas including the development of spatial/spectral interferometry observation, data processing, characterization, and analysis techniques in the Far-Infrared (FIR) region of the electromagnetic spectrum.
Many important astrophysical processes occur at wavelengths that fall within the far-infrared band of the EM spectrum, and over distance scales that require sub-arc second spatial resolution. It is clear that in order to achieve sub-arc second resolution at these relatively long wavelengths (compared to optical/near-IR), which are strongly absorbed by the atmosphere, a space-based far-IR interferometer will be required. We present analysis of the optical system for a proposed spatial-spectral interferometer, discussing the challenges that arise when designing such a system and the simulation techniques employed that aim to resolve these issues. Many of these specific challenges relate to combining the beams from multiple telescopes where the wavelengths involved are relatively short (compared to radio interferometry), meaning that care must be taken with mirror surface quality, where surface form errors not only present potential degradation of the single system beams, but also serve to reduce fringe visibility when multiple telescope beams are combined. Also, the long baselines required for sub-arc second resolution present challenges when considering propagation of the relatively long wavelengths of the signal beam, where beam divergence becomes significant if the beam demagnification of the telescopes is not carefully considered. Furthermore, detection of the extremely weak far-IR signals demands ultra-sensitive detectors and instruments capable of operating at maximum efficiency. Thus, as will be shown, care must be taken when designing each component of such a complex quasioptical system.
David Naylor, Jean-Paul Baluteau, George Bendo, Dominique Benielli, Trevor Fulton, Brad Gom, Matthew Griffin, Rosalind Hopwood, Peter Imhof, Tanya Lim, Nanyao Lu, Gibion Makiwa, Nicola Marchili, Glenn Orton, Andreas Papageorgiou, Chris Pearson, Edward Polehampton, Bernhard Schulz, Locke Spencer, Bruce Swinyard, Ivan Valtchanov, Matthijs H. van der Wiel, Ian Veenendaal, Ronin Wu
The Spectral and Photometric Imaging Receiver (SPIRE) is one of three scientific instruments on board the European Space Agency's Herschel Space Observatory which ended its operational phase on 29 April 2013. The low to medium resolution spectroscopic capability of SPIRE is provided by an imaging Fourier transform spectrometer (iFTS) of the Mach-Zehnder configuration. With their high throughput, broad spectral coverage, and variable resolution, coupled with their well-defined instrumental line shape and intrinsic wavelength and intensity calibration, iFTS are becoming increasingly common in far-infrared space astronomy missions. The performance of the SPIRE imaging spectrometer will be reviewed and example results presented. The lessons learned from the measured performance of the spectrometer as they apply to future missions will be discussed.
We describe recent progress in the development of a lab-based spatial/spectral double Fourier interferometer within the Astronomical Instrumentation Group (AIG) laboratories at the University of Lethbridge, Canada (UL). This testbed interferometer is used in the development of spatial/spectral interferometry observation, data processing, characterization, and analysis techniques in the Far-Infrared (FIR) region of the electromagnetic spectrum. Several interferometry technological development milestones on the FIR astrophysics roadmap are addressed by this ongoing research program of the UL AIG, all of which are needed as precursors to an eventual space-based FIR interferometry mission. This research program is supported by recent CRC, CFI, and NSERC grants.
FIRI (Far Infrared Interferometer) is a concept for a spatial and spectral interferometer with an operating
wavelength range 25-300 μm and sub-arcsecond angular resolution, and is based in the combination of two well-known
techniques, Stellar Interferometry and Fourier Transform Spectroscopy to achieve high spectral and spatial
resolution in the Far Infrared. The resulting technique is called Double Fourier Spatio-Spectral Interferometry
(Mariotti and Ridgway 1988). With increased spatial and spectral resolution a number of interesting science cases
such as the formation and evolution of AGN and the characterization of gas, ice and dust in disks undergoing
planetary formation, among others, can be investigated. Here the current status of the design of the FIRI system
via an instrument simulator is presented, as well as the results of a test-bed implementation.
The Spectral and Photometric Imaging Receiver (SPIRE) is one of three scientific instruments onboard the European
Space Agency's Herschel Space Observatory launched on 14 May 2009. The low to medium resolution spectroscopic
capability of SPIRE is provided by an imaging Fourier transform spectrometer of the Mach-Zehnder configuration.
Results from the in flight performance verification phase of the SPIRE spectrometer are presented and conformance with
the instrument design specifications is reviewed.
SPIRE, the Spectral and Photometric Imaging Receiver, is a submillimetre camera and spectrometer for Herschel. It
comprises a three-band camera operating at 250, 350 and 500 µm, and an imaging Fourier Transform Spectrometer
covering 194-672 μm. The photometer field of view is 4x8 arcmin., viewed simultaneously in the three bands. The FTS
has an approximately circular field of view of 2.6 arcmin. diameter and spectral resolution adjustable between 0.04 and 2
cm-1 ( λ/▵λ=20-1000 at 250 μm). Following successful testing in a dedicated facility designed to simulate the in-flight
operational conditions, SPIRE has been integrated in the Herschel spacecraft and is now undergoing system-level testing
prior to launch. The main design features of SPIRE are reviewed, the key results of instrument testing are outlined, and
a summary of the predicted in-flight performance is given.
The Spectral and Photometric Imaging Receiver (SPIRE) is one of three scientific instruments onboard the
European Space Agency (ESA)'s Herschel Space Observatory. The low to medium resolution spectroscopic
capability of SPIRE is provided by an imaging Fourier transformspectrometer of the Mach-Zehnder configuration.
Instrument performance of the SPIRE flight model was evaluated during a series of test campaigns. The SPIRE
instrument performance verification was completed with instrument delivery to ESA in early 2007. In this paper
we present the resulting performance characteristics of the SPIRE spectrometer flight model as determined from
these test campaigns. We verify the instrument's conformance with fundamental design specifications such as
spectral coverage and resolution. Variations across the imaging array of such properties as spectral resolution,
vignetting, and instrumental line shape are explored. Additionally, instrumental artefacts observed during final
verification testing are identified and quantified; with explanations provided for potential causes, and proposed
methods to minimize their impact on scientific observations described.
The Spectral and Photometric Imaging REceiver (SPIRE) is one of the three scientific instruments to fly on the
European Space Agency's Herschel Space Observatory, and contains a three-band imaging submillimetre photometer
and an imaging Fourier transform spectrometer. The flight model of the SPIRE cold focal plane unit has been built up
in stages with a cold test campaign associated with each stage. The first campaign focusing on the spectrometer took
place in early 2005 and the second campaign focusing on the photometer was in Autumn 2005. SPIRE is currently
undergoing its third cold test campaign following cryogenic vibration testing. Test results to date show that the
instrument is performing very well and in general meets not only its requirements but also most of its performance
goals. We present an overview of the instrument tests performed to date, and the preliminary results.
The Spectral and Photometric Imaging Receiver (SPIRE) is one of three scientific instruments on ESA's Herschel Space Observatory. An imaging Fourier transform spectrometer (IFTS) provides the medium resolution spectroscopic capabilities of SPIRE. This paper compares the measured performance of the SPIRE IFTS, as determined from flight model instrument verification tests, with theoretical expectations. This analysis includes a discussion of the instrument line shape, signal-to-noise, resolution, field of view and spectrometer sensitivity.
Imaging Fourier transform spectrometers (IFTS) are becoming the preferred systems for remote sensing spectral imaging applications because of their ability to provide, simultaneously, both high spatial and spectral resolution images of a scene. IFTS can be operated in either step-and-integrate or rapid-scan modes, where it is common practice to sample interferograms at equal optical path difference intervals. The step-and-integrate mode requires a translation stage with fast and precise point-to-point motion and additional external trigger circuitry for the detector focal plane array (FPA), and produces uniformly position-sampled interferograms which can be analyzed using standard FFT routines. In the rapid-scan mode, the translation stage is continuously moving and interferograms are often acquired at the frame-rate of the FPA. Since all translation stages have associated velocity errors, the resulting interferograms are sampled at non-uniform intervals of optical path difference, which requires more sophisticated analysis. This paper discusses the processing pipeline which is being developed for the analysis of the non-uniform rapid-scan data produced by the Herschel/SPIRE IFTS.
The Spectral and Photometric Imaging Receiver (SPIRE) is one of three instruments on the European Space Agency's Herschel mission. A detailed understanding of the SPIRE instrument is essential for a successful mission. In particular, it is important to characterize both the in-band spectral profile, and any out-of-band spectral leaks, which would severely degrade performance. A test Fourier Transform Spectrometer (TFTS), with its braod spectral coverage and intermediate spectral resolution, was selected for the spectral characterization of SPIRE. The integration of the TFTS with the existing Ground Support Equipment of the Hershel/SPIRE test facility at the Rutherford Appleton Laboratory imposed several mechanical, optical, electrical, and software constraints. In this paper we describe the design and implementation of the TFTS, and present preliminary results from its use in the SPIRE verification and performance tests.
The Spectral and Photometric Imaging REceiver (SPIRE) is one of the three scientific instruments on the European Space Agency's Herschel mission. At the start of 2004 the Cryogenic Qualification Model (CQM) of SPIRE was tested with the aim of verifying the instrument system design and evaluating key performance parameters. We present a description of the test facility, an overview of the instrument tests carried out on the CQM, and the first results from the analysis of the test data. Instrument optical efficiency and detector noise levels are close to the values expected from unit-level tests, and the SPIRE instrument system works well, with no degradation in performance from stray light, electromagnetic interference or microphonically induced noise. Some anomalies and imperfections in the instrument performance, test set-up, and test procedures have been identified and will be addressed in the next test campaign.
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