The Exoplanet Characterisation Observatory (EChO) mission was one of the proposed candidates for the European Space Agency’s third medium mission within the Cosmic Vision Framework. EChO was designed to observe the spectra from transiting exoplanets in the 0.55-11 micron band with a goal of covering from 0.4 to 16 microns. The mission and its associated scientific instrument has now undergone a rigorous technical evaluation phase and we report here on the outcome of that study phase, update the design status and review the expected performance of the integrated payload and satellite.
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.
KEYWORDS: Stars, Electronics, Data processing, Sensors, Space operations, Data acquisition, Planets, Control systems, Exoplanets, Short wave infrared radiation
The Exoplanet Characterization Observatory (EChO) is conceived for the spectrophotometric study from space of the atmospheres of a selected target sample of transiting extra-solar planets. It has been designed to run as a candidate for the M3 launch opportunity of the ESA Cosmic Vision program and can be considered as the next step towards the fully characterization of a representative sample of the already discovered transiting exoplanets. The EChO payload is based on a single highly thermo-mechanical stabilized remote-sensing instrument hosting a dispersive spectrograph. It is able to perform time-resolved spectroscopy exploiting the temporal and spectral variations of the measured signal due to the primary and secondary occultations occurring between the exoplanet and its parent star. The adopted technique allows the extraction of the planet spectral signature and to probe the physical and chemical properties of its atmosphere. EChO is composed by four scientific modules, all suited on a common Instrument Optical Bench (IOB). Each module is operated by a unique control and processing electronics, the Instrument Control Unit (ICU), acting as interface between the payload and the spacecraft (S/C) Data Management Subsystem (DMS) and Power Control and Distribution Unit (PCDU). The main ICU tasks concern the instrument commanding, based on the received and interpreted TC and TM; instrument monitoring and control by means of the housekeeping (HK) data acquired from the focal plane units; synchronization of all the scientific payload activities; detectors readout and data acquisition, pre-processing, lossless compression and formatting before downloading the TM science data and HK to the spacecraft mass memory. As far as the software is concerned, these activities can be basically grouped and managed by the Instrument Control software and Data Processing software; both will constitute the On Board Software of the overall payload designed to address all the processing requirements as driven by the EChO science case [1, 2]. This paper is conceived as a memory for an EChO-like payload electrical architecture with processing capabilities mainly driven by the scientific requirements as defined and frozen at the end of both the Payload Assessment Phase and the M3 mission selection process, held by ESA at the beginning of February 2014.
KEYWORDS: Sensors, Spectroscopy, Space telescopes, Telescopes, Planets, Stars, Space operations, Mid-IR, Long wavelength infrared, Short wave infrared radiation
The Exoplanet Characterisation Observatory (EChO) is a space mission dedicated to undertaking spectroscopy of
transiting exoplanets over the widest wavelength range possible. It is based around a highly stable space platform with a
1.2 m class telescope. The mission is currently being studied by ESA in the context of a medium class mission within
the Cosmic Vision programme for launch post 2020. The payload suite is required to provide simultaneous coverage
from the visible to the mid-infrared and must be highly stable and effectively operate as a single instrument. In this
paper we describe the integrated spectrometer payload design for EChO which will cover the 0.4 to 16 micron
wavelength band. The instrumentation is subdivided into 5 channels (Visible/Near Infrared, Short Wave InfraRed, 2 x Mid Wave InfraRed; Long Wave InfraRed) with a common set of optics spectrally dividing the input beam via dichroics.
We discuss the significant design issues for the payload and the detailed technical trade-offs that we are undertaking to
produce a payload for EChO that can be built within the mission and programme constraints and yet which will meet the
exacting scientific performance required to undertake transit spectroscopy.
C. Darren Dowell, Michael Pohlen, Chris Pearson, Matt Griffin, Tanya Lim, George Bendo, Dominique Benielli, James Bock, Pierre Chanial, Dave Clements, Luca Conversi, Marc Ferlet, Trevor Fulton, Rene Gastaud, Jason Glenn, Tim Grundy, Steve Guest, Ken King, Sarah Leeks, Louis Levenson, Nanyao Lu, Huw Morris, Hien Nguyen, Brian O'Halloran, Seb Oliver, Pasquale Panuzzo, Andreas Papageorgiou, Edward Polehampton, Dimitra Rigopoulou, Helene Roussel, Nicola Schneider, Bernhard Schulz, Arnold Schwartz, David Shupe, Bruce Sibthorpe, Sunil Sidher, Anthony Smith, Bruce Swinyard, Markos Trichas, Ivan Valtchanov, Adam Woodcraft, C. Kevin Xu, Lijun Zhang
We describe the current state of the ground segment of Herschel-SPIRE photometer data processing, approximately
one year into the mission. The SPIRE photometer operates in two modes: scan mapping and chopped
point source photometry. For each mode, the basic analysis pipeline - which follows in reverse the effects from
the incidence of light on the telescope to the storage of samples from the detector electronics - is essentially
the same as described pre-launch. However, the calibration parameters and detailed numerical algorithms have
advanced due to the availability of commissioning and early science observations, resulting in reliable pipelines
which produce accurate and sensitive photometry and maps at 250, 350, and 500 μm with minimal residual
artifacts. We discuss some detailed aspects of the pipelines on the topics of: detection of cosmic ray glitches,
linearization of detector response, correction for focal plane temperature drift, subtraction of detector baselines
(offsets), absolute calibration, and basic map making. Several of these topics are still under study with the
promise of future enhancements to the pipelines.
Trevor Fulton, Jean-Paul Baluteau, George Bendo, Dominique Benielli, Rene Gastaud, Matt Griffin, Steve Guest, Peter Imhof, Tanya Lim, Nanyao Lu, David Naylor, Pasquale Panuzzo, Edward Polehampton, Arnold Schwartz, Christian Surace, Bruce Swinyard, Kevin Xu
We present an update to the data processing pipelines that generate calibrated spectral data products from the Spectral
and Photometric Imaging Receiver (SPIRE), one of three scientific instruments onboard the European Space Agency's
Herschel Space Observatory launched on 14 May 2009. The pipelines process telemetry from SPIRE's imaging Fourier
Transform Spectrometer (FTS) taken in point source, jiggle- and raster-map observing modes, producing calibrated
spectra in low-, medium-, high-, and mixed low- and high-spectral resolution. While the order and algorithms of the data
processing modules in the spectrometer pipelines remain for the most part unchanged compared to their pre-launch
status, some improvements and optimizations have been realized through the analysis of data from the performance
verification and science demonstration phases of the mission. The data processing pipelines for the SPIRE FTS as of the
beginning of the routine phase of the Herschel mission are presented in their entirety, with more detailed descriptions
reserved for those elements that have changed since launch, in particular the first- and second-level correction steps for
glitches, the step that corrects for clipped samples, and the process by which Level-1 spectral data are converted to
Level-2 products. In addition, we discuss some of the challenging aspects still faced by the automated processing
pipelines, such as the removal of the contributions from the Herschel telescope and SPIRE instrument, and the relative
spectral response correction and flux conversion steps.
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.
KEYWORDS: Bolometers, Photometry, Spectroscopy, Sensors, Temperature metrology, Field effect transistors, Data modeling, Signal detection, Interference (communication), Smoothing
The flight model of the SPIRE instrument underwent several test campaigns in a test facility at the Rutherford Appleton
Laboratory (RAL) in the UK. A final dark campaign, completed in March 2007, provided an environment virtually free
from optical radiation. This allowed re-determining the fundamental model parameters of the NTD spider web bolometer
detector arrays in the new environment. The tests reported in this paper produced a fairly homogeneous dataset to
investigate white noise and 1/f noise at different bias voltages, bias frequencies, and bath temperatures. We find that the
white noise performance is in excellent agreement with the model predictions, once we correct the low frequency signal
variations that are due to temperature fluctuations of the thermal bath at about 300 mK. The temperature of the thermal
bath (detector array base plate) is measured by thermistor pixels that are part of the bolometer arrays. A residual 1/f
component beyond those variations is hardly detected. This unexpected stability is very welcome and will positively
impact photometer scan maps, the most popular observing mode of SPIRE.
Trevor Fulton, David Naylor, Jean-Paul Baluteau, Matt Griffin, Peter Davis-Imhof, Bruce Swinyard, Tanya Lim, Christian Surace, Dave Clements, Pasquale Panuzzo, Rene Gastaud, Edward Polehampton, Steve Guest, Nanyao Lu, Arnold Schwartz, Kevin Xu
We present the data processing pipeline to generate calibrated data products from the Spectral and Photometric Imaging
Receiver (SPIRE) imaging Fourier Transform Spectrometer. The pipeline processes telemetry from SPIRE point source,
jiggle- and raster-map observations, producing calibrated spectra in low-, medium-, high-, and mixed low- and highresolution
modes. The spectrometer pipeline shares some elements with the SPIRE photometer pipeline, including the
conversion of telemetry packets into data timelines and the calculation of bolometer voltages from the raw telemetry. We
present the following fundamental processing steps unique to the spectrometer: temporal and spatial interpolation of the
stage mechanism and detector data to create interferograms; apodization; Fourier transform, and creation of a
hyperspectral data cube. We also describe the corrections for various instrumental effects including first- and secondlevel
glitch identification and removal, correction of the effects due to the Herschel primary mirror and the spectrometer
calibrator, interferogram baseline correction, channel fringe correction, temporal and spatial phase correction, non-linear
response of the bolometers, variation of instrument performance across the focal plane arrays, and variation of spectral
efficiency. Astronomical calibration is based on combinations of observations of standard astronomical sources and
regions of space known to contain minimal emission.
The Mid-Infrared Instrument (MIRI) is one of the three scientific instruments to fly on the James Webb Space
Telescope (JWST), which is due for launch in 2013. MIRI contains two sub-instruments, an imager, which has low
resolution spectroscopy and coronagraphic capabilities in addition to imaging, and a medium resolution IFU
spectrometer. A verification model of MIRI was assembled in 2007 and a cold test campaign was conducted between
November 2007 and February 2008. This model was the first scientifically representative model, allowing a first
assessment to be made of the performance. This paper describes the test facility and testing done. It also reports on the
first results from this test campaign.
We describe the on-board electronics chain and the on-ground data processing pipeline that will operate on data from the
Herschel-SPIRE photometer to produce calibrated astronomical products. Data from the three photometer arrays will be
conditioned and digitised by on-board electronics and sent to the ground with no further on-board data processing. On
the ground, the data pipeline will process the data from point source, jiggle-map, and scan-map observations in a fully
automatic manner, producing measured flux densities (for point source observations) or maps. It includes calculation of
the bolometer voltages from the raw telemetry, glitch removal, and corrections for various effects including time
constants associated with the detectors and electronics, electrical and optical crosstalk, detector temperature drifts, flatfielding,
and non-linear response of the bolometers to strong sources. Flux density calibration will be with respect to
standard astronomical sources with the planets Uranus and Neptune being adopted as the baseline primary standards.
The pipeline will compute estimated values of in-beam flux density for a standard flat νS(ν) source spectrum.
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 SPIRE instrument for the Herschel Space Observatory has two on-board calibration sources. The photometer calibrator, PCAL, is an electrically-heated thermal source which can be seen by all detectors, including the spectrometer. It is not an absolute calibrator, but a repeatable source of sub-millimetre radiation which may be used in the overall calibration scheme. The purpose of the spectrometer calibrator is to null the background emission from the Herschel telescope, thereby improving the dynamic range of the spectrometer detectors. This paper details the final flight design of the calibration units, and presents results from SPIRE flight model ground testing.
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.
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.
Tanya Lim, Gerard Hutchinson, Sunil Sidher, Sergio Molinari, Josephine Chan, Christopher Lloyd, Sarah Leeks, Edward Polehampton, A. Harwood, Bruce Swinyard
The Long Wavelength Spectrometer was one of two complementary spectrometers on the Infrared Space Observatory (ISO). The LWS operated between 44 and 197 microns either in medium resolution mode, using a diffraction grating, or in high resolution mode where a Fabry Perot was also placed in the beam. All LWS data is processed through a standard 'pipeline' and this standard processing is adequate for the majority of the data. However, as the understanding of instrument behaviour increased during operations, it became apparent that various modes, in particular the Fabry Perot scanning mode, could be better processed in an interactive manner. A complementary LWS Interactive Analysis (LIA) system was then developed for the scientific part of the data processing. The LIA system allows users to access the processing steps, in terms of visualisation of intermediate products and for interactive manipulation of the data at each stage. This paper describes the LIA system and details in terms of instrument behaviour those data sets that require interactive processing. Following the release of the ISO Legacy Archive in 2001, LIA 10 was released in November 2001. A further update, LIA 10.1, will be released later this year and we outline the new features along with some of the most commonly used LIA routines.
The Infrared Space Observatory (ISO) had a scientific payload of four complementary instruments, a camera, a photometer, and two spectrometers. Two instruments, the Long Wavelength Spectrometer (LWS) and the Camera were able to operate in parallel mode i.e. taking scientific data while another instrument was active. The LWS had ten detectors which allowed simultaneous coverage of the entire 43-197 micron range. In parallel mode the diffraction grating remained in a fixed position allowing the spectrometer to act like a 10 channel photometer with bandwidths of 0.3 microns (one resolution element in second order) for the five short wavelength detectors and 0.6 microns (one resolution element in first order) for the five long wavelength detectors. This paper describes the LWS parallel mode and gives details on the data was obtained. The paper will also describe the automated processing developed for the parallel mode data and the calibration strategy employed. The parallel data has very good sparse coverage in the Rho Oph region and a temperature map derived from the parallel mode data are presented.
The long wavelength spectrometer on board the ESA IR Space Observatory employs doped geranium photoconductors to perform spectroscopy in the 43 to 197 micrometers waveband. The instrument has been in continuous on orbit operation for over two years - longer than any other experiment in this waveband. Invaluable data have been gathered on the long term performance of a beryllium doped germanium detector and both stressed and unstressed gallium doped germanium detectors in the presence of ionizing radiation in the form of cosmic rays and charged particles trapped in the Earth's magnetic fields. In this paper we report on the in-orbit performance of the detectors and in particular on the long term behavior of the dark current and responsivity.
The long wavelength spectrometer on-board the European Space Agency IR Space Observatory (ISO) uses a grating and one of two Fabry-Perot interferometers to make medium and high resolution spectroscopic observations in the 43-196.9 micrometers wavelength range. The instrument has been in continuous use since the launch of ISO in November 1995. In this paper we describe the calibration of the instrument and its performance, both spectroscopic and photometric, over the two years of instrument operations.
The high level of automation in the operation of the ESA Infrared Space Observatory, together with high observing efficiency, leads to a requirement for a commensurate level of automation in the subsequent processing of the astronomical data. This inevitably means that all data for a given instrument mode have the same calibration applied, regardless of the exact details of the object being observed. Questions then arise about these 'pipeline processed' data in terms of the calibration accuracy achieved; how to control the quality of data received by the observer and how much further processing is required - or desirable - by the observer.In this paper we outline the experience of two years of operation of the long wavelength spectrometer on board ISO, detailing the improvements made in the pipeline processing during this time and the difficulties encountered in the automated processing of some instrument modes.
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