KEYWORDS: Equipment, Spectroscopy, Calibration, Sun, Design and modelling, Tunable filters, Optical filters, Glasses, Spectral calibration, Signal to noise ratio
CHIME, the Copernicus Hyperspectral Imaging Mission for the Environment, is one of six new missions that the EU and ESA are developing to expand the current suite of Copernicus Sentinels. The CHIME mission will provide systematic hyperspectral images to map changes in land cover and help sustainable agricultural practices. The contract for the development of two CHIME Satellites has been awarded in November 2020 to Thales Alenia Space France as Industrial Prime together with OHB Germany as Instrument Prime responsible for the novel Hyperspectral Imager (HSI). Compared to the two hyperspectral precursor missions, EnMAP (DLR) and PRISMA (ASI), CHIME will provide an enhancement allowing continuous and fully operational hyperspectral mapping of the Earth’s surface. The Hyperspectral Imager (HSI) on both satellites is a high-performance pushbroom imaging spectrometer type of instrument. Each instrument records ~130km of swath at 30m x 30m ground sampling. The spectral sampling interval is 10nm, covering a continuous spectral range from 400 nm to 2500 nm. A high performance Three Mirror Anastigmat (TMA) type telescope with wide-band coated optics collects the light reflected from ground and images it to three highly linear radiometric responsive and almost distortion-free spectrometers attaining very good spectral stability. All optical units are mounted to a torus-like carbon fiber (CFRP) optical bench structure providing the necessary line of sight stability. The electro-optical back end is based on passively cooled Teledyne CHROMA-D digital readout detectors creating robust margin in the predicted Signal-to-Noise performance. In flight, the HSI can be calibrated via on-board devices and using reference targets outside the spacecraft. We present the design of the instrument payload at the stage of the Preliminary Design Review (PDR) mid 2022. We show the predicted instrument performance and discuss several design aspect highlights, like the carbon-fiber torus optical bench and the novel spectral calibration unit based on a combination of diffused sun illumination and absorption glass filters.
4MOST (4-meter Multi-Object Spectroscopic Telescope) is a wide-field, fiber-fed, high-multiplex spectroscopic survey facility to be installed on the 4-meter ESO telescope VISTA in Chile. The back-end consists of one high-resolution spectrograph (HRS) and two identical low-resolution spectrographs. 4MOST will afford with the HRS simultaneous observations of up to 812 targets on a hexagonal 4.4 square degrees field of view at a spectral resolution R<18,000 covering 392.6 to 679 nm in three channels. It is expected to be fully operational early 2024. In this paper, we present the integration and alignment applied for the HRS optics. The results of the tests of the fully integrated sub-system in our integration facility are discussed. The instrument schedule is outlined and the actual timeline of the previous procurement and manufacturing phase is given
CHIME, the Copernicus Hyperspectral Imaging Mission for the Environment, is one of the six High Priority Candidate Missions (HPCM) of the evolution in the Copernicus Space Component (CSC) foreseen in the mid-2020s that is proposed for further analysis. In this paper we summarize the results as retrieved by OHB (D) as part of the Phase A/B1. The contract was kicked off in 2018 and concluded in 2020 after finalisation of the Pre-development activities. The proposed instrument is a hyperspectral imager instrument with reflective telescope and grating-based spectrometer. The selected orbit is in the range of 625 ± 30 km, LTDN 10:45 – 11:15 am with a repeat cycle of 20 to 25 days for a single satellite and 10-12.5 days revisit for 2 satellites. The payload of each satellite records at a Spatial Sampling Distance (SSD) of 30m the full spectral range from 400 to 2500nm at a Spectral Sampling interval < 10nm with Low Keystone/Smile. On the front end a high performance TMA with wide-band coated optics collects the light from ground and feeds it to a highly linear almost distortion free spectrometer assembly attaining very good spectral stability. All units are integrated in an optical bench structure that offers excellent AIT access and provides a highly stable LOS. The electro-optical backend contains low-noise cold MCT detectors creating margin in the predicted NEDL performance. The instrument can be calibrated via on-board devices or using reference targets outside the spacecraft. We present the functional decomposition and the physical instrument architecture: the optical design and opto-mechanical layout, the electro-optical imaging chain ant thermal control system.
KEYWORDS: Calibration, Mirrors, Telescopes, Sensors, Infrared telescopes, Modulation transfer functions, Signal to noise ratio, Near infrared, Manufacturing, Imaging systems
A Hosted Arctic Imager (HAI) concept is currently being investigated as part of ESA’s Polaris program. HAI intends to fulfil the needs for providing weather and atmospheric services in the polar regions enabling e.g. near-real-time observations of Atmospheric Motion Vectors of the Arctic and Nordic regions, similar to the measurements offered by its Meteosat counterparts in GEO, such as SEVIRI on MSG and FCI on MTG. The compact hosted-payload multispectral imager operates from a High Elliptical Orbit in 12 spectral bands from 0.4μm to 13.3μm at a Ground Sampling Distance of 1-3km. The optical concepts employs a split design into a wavelength-optimized VIS and a (N)IR telescope, built as all-metal free-form optics, where a hole in the first mirror of the (N)IR telescope presents the entrance aperture of the VIS telescope. Our instrument design maximizes the re-use of heritage technology, e.g. for detectors, scanner, and calibration elements, in order to enable a low-risk fast-track development program.
4MOST is a fibre-fed, multi-object spectroscopic survey facility to be installed on the VISTA telescope at ESO's Paranal observatory. This paper presents the final mechanical design of the optical fibre route from the fibre positioner at the focal plane of VISTA to the fibre-slits within the high- and low-resolution spectrographs below the azimuth platform. The technical challenges are to provide a safe, durable and efficient fibre route for over 2400 fibres. To accommodate the movements of the telescope, a Cassegrain Cable Wrap and a novel elevation chain concept has been prototyped and extensively tested to validate the design solutions.
4MOST (4-meter Multi-Object Spectroscopic Telescope) is a wide-field, fiber-feed, high-multiplex spectroscopic survey facility to be installed on the 4-meter ESO telescope VISTA in Chile. Its backend consists of one high resolution spectrograph and two identical low resolution spectrographs. The instrument is presently in the final design phase (review in May 2018) and is expected to enter full operations at the beginning of 2023 ([1] and [2]). The high resolution spectrograph (HRS) will afford simultaneous observations of up to 812 targets – over a hexagonal field of view of ~ 4.1 square degrees on sky – with a spectral resolution R>18,000 covering wavelength ranges between 393 and 679 nm in three channels. The optical design of the instrument is described in detail in [5]. In February 2017 the final design review for the optics was held and passed successfully. The final design review for the mechanics and all other parts of the instrument was held in May 2018. A summary and update of the optical and mechanical design of the HRS are presented in this paper. The detailed status of the manufacturing of the optics is given. The procedures and tools used during the AIT phase for the optical alignment of the HRS system, as well as the performance tests and characterizations are described.
4MOST (4-meter Multi-Object Spectroscopic Telescope) is a wide-field, fiber-feed, high-multiplex spectroscopic survey facility to be installed on the 4-meter ESO telescope VISTA in Chile. It consists of two identical low resolution spectrographs and one high resolution spectrograph. The instrument is presently in the preliminary design phase and expected to get operational end of 2022. The high resolution spectrograph will afford simultaneous observations of up to 812 targets - over a hexagonal field of view of ~ 4.1 sq.degrees on sky - with a spectral resolution R>18,000 covering a wavelength range from 393 to 679nm in three channels. In this paper we present the optical and mechanical design of the high resolution spectrograph (HRS) as prepared for the review at ESO, Garching. The expected performance including the highly multiplexed fiber slit concept is simulated and its impact on the optical performance given. We show the thermal and finite element analyses and the resulting stability of the spectrograph under operational conditions.
ARGOS is the Laser Guide Star and Wavefront sensing facility for the Large Binocular Telescope. With first laser light on sky in 2013, the system is currently undergoing commissioning at the telescope. We present the overall status and design, as well as first results on sky. Aiming for a wide field ground layer correction, ARGOS is designed as a multi- Rayleigh beacon adaptive optics system. A total of six powerful pulsed lasers are creating the laser guide stars in constellations above each of the LBTs primary mirrors. With a range gated detection in the wavefront sensors, and the adaptive correction by the deformable secondary’s, we expect ARGOS to enhance the image quality over a large range of seeing conditions. With the two wide field imaging and spectroscopic instruments LUCI1 and LUCI2 as receivers, a wide range of scientific programs will benefit from ARGOS. With an increased resolution, higher encircled energy, both imaging and MOS spectroscopy will be boosted in signal to noise by a large amount. Apart from the wide field correction ARGOS delivers in its ground layer mode, we already foresee the implementation of a hybrid Sodium with Rayleigh beacon combination for a diffraction limited AO performance.
LUCI (former LUCIFER) is the full cryogenic near-infrared multi-object spectrograph and imager at the LBT. It presently allows for seeing limited imaging and multi-object spectroscopy at R~2000-4000 in a 4x4arcmin2 FOV from 0.9 to 2.5 micron. We report on the instrument performance and the lessons learned during the first two years on sky from a technical and operational point of view. We present the upcoming detector upgrade to Hawaii-2 RG arrays and the operating modes to utilize the binocular mode, the LBT facility AO system for diffraction limited imaging as well as to use the wide-field AO correction afforded by the multi-laser GLAO System ARGOS in multi-object spectroscopy.
ARGOS the Advanced Rayleigh guided Ground layer adaptive Optics System for the LBT (Large Binocular Telescope)
is built by a German-Italian-American consortium. It will be a seeing reducer correcting the turbulence in the lower
atmosphere over a field of 2' radius. In such way we expect to improve the spatial resolution over the seeing of about a
factor of two and more and to increase the throughput for spectroscopy accordingly. In its initial implementation,
ARGOS will feed the two near-infrared spectrograph and imager - LUCI I and LUCI II.
The system consist of six Rayleigh lasers - three per eye of the LBT. The lasers are launched from the back of the
adaptive secondary mirror of the LBT. ARGOS has one wavefront sensor unit per primary mirror of the LBT, each of the
units with three Shack-Hartmann sensors, which are imaged on one detector.
In 2010 and 2011, we already mounted parts of the instrument at the telescope to provide an environment for the main
sub-systems. The commissioning of the instrument will start in 2012 in a staged approach. We will give an overview of
ARGOS and its goals and report about the status and new challenges we encountered during the building phase. Finally
we will give an outlook of the upcoming work, how we will operate it and further possibilities the system enables by
design.
Walter Seifert, Nancy Ageorges, Michael Lehmitz, Peter Buschkamp, Volker Knierim, Kai Polsterer, Andre Germeroth, Anna Pasquali, Vianak Naranjo, Marcus Jütte, Carmen Feiz, Hans Gemperlein, Reiner Hofmann, Werner Laun, Reinhard Lederer, Rainer Lenzen, Ulrich Mall, Holger Mandel, Peter Müller, Andreas Quirrenbach, Ludwig Schäffner, Clemens Storz, Peter Weiser
LUCIFER1 is a NIR camera and spectrograph installed at the Large Binocular Telescope (LBT). Working in
the wavelength range of 0.9-2.5micron, the instrument is designed for direct imaging and spectroscopy with 3
different cameras. A set of longslit masks as well as up to 23 user defined (MOS) masks are available. The set
of user defined masks can be exchanged while the instrument is at operating temperature.
Extensive tests have been done on the electro-mechanical functions, image motion due to flexure, optical
quality, instrument software, calibration and especially on the multi-object spectroscopy. Also a detailed characterization
of the instrument's properties in the different observing modes has been carried out. Results are
presented and compared to the specifications.
The LUCIFER-MOS unit is the full cryogenic mask-exchange unit for the near-infrared multi-object spectrograph
LUCIFER at the Large Binocular Telescope. We present the design and functionality of this unique device. In LUCIFER
the masks are stored, handled, and placed in the focal plane under cryogenic conditions at all times, resulting in very low
thermal background emission from the masks during observations. All mask manipulations are done by a novel
cryogenic mask handling robot that can individually address up to 33 fixed and user-provided masks and place them in
the focal plane with high accuracy. A complete mask exchange cycle is done in less than five minutes and can be run in
every instrument position and state reducing instrument setup time during science observations to a minimum. Exchange
of old and new MOS masks is likewise done under cryogenic conditions using a unique exchange drive mechanism and
two auxiliary cryostats that attach to the main instrument cryostat.
LUCIFER 1 is the rst of two identical camera-spectrograph units installed at the LBT (Large Binocular Telescope)
on Mount Graham in Arizona. Its commissioning took place between September 2008 and November
2009 and has immediately been followed by science operations since December 2009.
LUCIFER has a 4x4 arcminute eld of view. It is equipped with a 2048x2048 pixel HAWAII-2 array, suitable
lters (broad-band z, J, H, K & Ks plus 12 medium and narrow band near-infrared lters) and three gratings for
spectroscopy for a resolution of up to 15000. LUCIFER has 3 cameras: two specic for seeing limited imaging
(the N3.75 camera, with 0.12"/pixel) and spectroscopy (the N1.8 camera, with 0.25"/pixel) and one for diraction
limited observations (the N30 camera). We report here about the completed seeing-limited commissioning, thus
using only two of the cameras.
LUCIFER is a NIR spectrograph and imager (wavelength range 0.9 to 2.5 micron) for the Large Binocular
Telescope (LBT) on Mt. Graham, Arizona, working at cryogenic temperatures of less than 70K. Two instruments
are built by a consortium of five German institutes and will be mounted at the bent Gregorian foci of the two
individual telescope mirrors. Three exchangable cameras are available for imaging and spectroscopy: two of
them are optimized for seeing-limited conditions, a third camera for the diffraction limited case will be used with
the LBT adaptive secondary mirror working. Up to 33 exchangeable masks are available for longslit or multi-object
spectroscopy (MOS) over the full field of view (FOV). Both MOS-units (LUCIFER 1 and LUCIFER
2) and the auxiliary cryostats together with the control electronics have been completed. The observational
software-package is in its final stage of preparation.
After the total integration of LUCIFER 1 extensive tests were done for all electro-mechanical functions and
the verification of the instrument started. The results of the tests are presented in detail and are compared with
the specifications.
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