The PRobe far-Infrared Mission for Astrophysics (PRIMA) is an actively cooled, infrared observatory for the community for the next decade.
On board, an infrared camera, PRIMAger, will provide observers with coverage of mid-infrared to far-infrared wavelengths from about 25 to 264 microns. PRIMAger will offer two imaging modes: the Hyperspectral mode will cover the 25-80 microns wavelength range with a resolution R~10 while the Polarimetric mode will have four broad-band filters, sensitive to polarization, from 80 to 264 microns. These capabilities have been specifically tailored to answer fundamental astrophysical questions such as black hole and star-formation coevolution in galaxies, the evolution of small dust grains over a wide range of redshifts, and the effects of interstellar magnetic fields in various environments, as well as opening a vast discovery space with versatile photometric and polarimetric capabilities.
PRIMA is a cryogenically-cooled, far-infrared observatory for the community for the beginning of the next decade (∼2031). It features two instruments, PRIMAger and FIRESS. The PRIMAger instrument will cover the mid-IR to far-IR wavelengths, from about 25 to 260 µm. Hyperspectral imaging can be obtained in 12 medium-resolution bands (R ∼ 10, more precisely a linear variable filter) covering the wavelength range from 25 to 80 micrometers, and broad-band (R ∼ 4) photometric and polarimetric imaging can be carried out in four bands between 80 and 260 µm. PRIMAger’s unique and unprecedented scientific capabilities will enable study, both in PI and GO programs, of black hole and star-formation coevolution in galaxies, the evolution of small dust grains over a wide range of redshift, and the effects of interstellar magnetic fields in various environments, as well as opening up a vast discovery space with its versatile imaging and polarimetric capabilities. One of the most ambitious possibilities is to carry out an all-sky far-IR survey with PRIMAger, creating a rich data set for many investigations. The design of PRIMAger is presented is an accompanying paper (Ciesla et al., SPIE Astronomical Telescopes + Instrumentation 2024).
MOSAIC is the Multi-Object Spectrograph (MOS) for the 39m Extremely Large Telescope (ELT) of the European Southern Observatory (ESO), with unique capabilities in terms of multiplex, wavelength coverage and spectral resolution. It is a versatile multi-object spectrograph working in both the Visible and NIR domains, designed to cover the largest possible area (∼40 arcmin2) on the focal plane, and optimized to achieve the best possible signal-to-noise ratio on the faintest sources, from stars in our Galaxy to galaxies at the epoch of the reionization. In this paper we describe the main characteristics of the instrument, including its expected performance in the different observing modes. The status of the project will be briefly presented, together with the positioning of the instrument in the landscape of the ELT instrumentation. We also review the main expected scientific contributions of MOSAIC, focusing on the synergies between this instrument and other major ground-based and space facilities.
MOSAIC is the multi-object spectrograph (MOS) for the ESO 39m European Extremely Large Telescope (ELT) approved to enter phase B beginning 2023. MOSAIC combines visible and near-infrared channels, from resolved stars up to the most distant galaxies, with multi-object and multi-integral field spectroscopy capabilities. The NIRspectrograph (130K-90K) is one sub-system of the NIR-channel, led by the Universidad Complutense de Madrid (UCM, Spain). It includes four camera modules delivered by the Laboratoire d’Astrophysique de Marseille (LAM, France) and equipped with Teledyne H4RG science detectors (4kx4k, 15 μm pixels). The four modules distribute two identical cryogenic benches ensuring, on each, the spectral coverage of the two observing bands J (0.95 – 1.34 μm) and H (1.43 – 1.80 μm in LR mode and 1.52 – 1.63 μm in HR mode). This paper presents the design of a cryogenic NIR camera prototype based on an athermal concept and details the ongoing AIT development for verification in the 0.95 – 1.34 μm domain in relevant environment (ESO TRL5).
MOSAIC* is the multi-object spectrograph (MOS) for the ESO 39m European Extremely Large Telescope (ELT) approved to enter phase B at the of beginning 2023. MOSAIC combines visible and near-infrared channels, from resolved stars up to the most distant galaxies, with multi-object and multi-integral field spectroscopy capabilities. The NIR-spectrograph (130K-90K) is one sub-system of the NIR-channel, led by the Universidad Complutense de Madrid (UCM, Spain). The NIR Spectrograph (NIRSPEC) comprises 2 identical spectrographs, each one equipped with Teledyne H4RG science detectors (4kx4k, 15 μm pixels). Each spectrograph operates at 130K (with detectors at 90K) and covers the 2 observing bands J (1 – 1.38 μm) and H (1.43 – 1.85 μm in low-resolution mode and 1.52 – 1.65 μm in high-resolution mode). This paper presents the optical design of the NIRSPEC.
THESEUS mission aims to detect and observe transient sources in the X-ray and Gamma-Ray bands, with a follow-up in the infrared band. The primary objectives are to provide real time trigger and accurate location of GRBs and to discover new high-energy transients. THESEUS InfraRed Telescope (IRT) is, with the Soft X-ray Imager (SXI) and the X-Gamma ray Imaging Spectrometer (XGIS), one on the 3 instruments onboard THESEUS satellite. The IRT (0.7-1.8 μm) is a 0.7 m class IR telescope with 15x15 arcmin FOV, for fast response, with both imaging and spectroscopy capabilities. The most critical component for the spectroscopic mode is the grism. This grism is a complex component with multi - function properties: (i) fixing the line of sight towards the detector; (ii) selecting the correct spectral band with interferential filter; (iii) compensating for aberrations (both geometrical and chromatic) to reach near diffraction-limit image quality; (iiii) dispersing the wavelengths with a resolving power around 400. Such grisms have been developed by our laboratory for the NISP instrument of the EUCLID mission, with industry partnership from Silios Technologies. These grisms, with curved lines, are manufactured by photolithography. In the context of THESEUS IRT grisms, new R&D activities are mandatory to validate the manufacturability of the gratings since they have a groove density 3 times higher than NISP grisms. In this article, we will present the results we obtained on grating prototypes developed during the phase A of the project. Profilometric measurements of the groove profile and diffraction efficiency measurement are analyzed.
MOSAIC is a multi-object spectrograph planned to be installed on the ESO-Extremely Large Telescope. The project is approved to start its phase B in September/October 2022. The main science cases addressed by MOSAIC go from the study of faint stars in the Milky Way and in the local group, to the study of dark matter, galaxy evolution and first-light objects at the epoch of reionisation. The MOSAIC instrument offers Multi-Object Spectroscopy and Integral Field Units capabilities from the visible (VIS) to the near-infrared (NIR). The Laboratoire d’Astrophysique de Marseille is responsible for the development of the near infrared spectrograph. More precisely, it is in charge of the global architecture and design of the NIR spectrograph (optical, mechanical, thermal) and the assembly, integration, tests and verification (AIT/V) activities in cryogenic environment. In this article, the main tradeoffs in terms of optical and mechanical architectures are analyzed; the main technical choices are justified according to the science requirements (from which technical requirement specifications are derived) and the level of maturity of key critical technologies. The NIR spectrograph will be described in terms of system engineering approach. The requirement flow-down strategy, from high-level requirements at the system level toward technical specifications at the module and component levels will be presented. The main interfaces and the development philosophy (with an emphasis on the AIT/V plan) will also be included.
MOSAIC, the multi-object spectrograph (MOS) for the ESO 39m European Extremely Large Telescope (ELT), will combine visible and near-infrared observations with multi-object and multi-integral field spectroscopy capabilities. It will cover a wide panel of topics, from resolved stars up to the most distant galaxies. In the frame of the NIR spectrograph unit realization led by the Laboratoire d’Astrophysique de Marseille (LAM), this paper presents the ongoing development of a cryogenic (90-130 K) NIR camera prototype tested in the 0.77-1.063 µm wavelengths (I band) detailing the opto-mechanical design and the integration and verification strategies in accordance with validation in relevant environment (ESO TRL5).
MOSAIC is the Muti-Object Spectrograph for the ESO Extremely Large Telescope. The Laboratoire d’Astrophysique de Marseille (LAM) is in charge of the instrument “Assembly, Integration, Test and Verification (AIT/V)” phases. AITV for AO instruments, in laboratory as in the telescope, always represent numerous technical challenges. We already started the preparation and planning for the instrument level AIT activities, from identification of needs, challenges, risks, to defining the optimal AIT strategy. In this paper, we present the state of this study and describe several AIT/V scenarios and a planning for AIT phases in Europe and in Chile. We also show our capacity, experience and expertise to lead the instrument MOSAIC AIT/V activities.
The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments (see ref [1]). It operates in the near-IR spectral region (950-2020nm) as a photometer and spectrometer. The instrument is composed of: - a cold (135K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly, a filter wheel mechanism, a grism wheel mechanism, a calibration unit and a thermal control system - a detection system based on a mosaic of 16 H2RG with their front-end readout electronic. - a warm electronic system (290K) composed of a data processing / detector control unit and of an instrument control unit that interfaces with the spacecraft via a 1553 bus for command and control and via Spacewire links for science data This paper presents: - the final architecture of the flight model instrument and subsystems - the performances and the ground calibration measurement done at NISP level and at Euclid Payload Module level at operational cold temperature.
Today, the combination of high angular resolution and high revisit rate is not readily available from space, at least not at a reasonable cost. Many applications in the science, civil or defense domains would benefit from having access to detailed images of the ground as often as possible, in order to study temporal evolutions of specific events. The high angular resolution requires large optics hence large platforms, whereas the revisit rate requires constellations of multiple satellites and therefore small and affordable platforms. We proposed the concept of a deployable telescope onboard a CubeSat, called AZIMOV [1, 3, 5], to address this specific gap. Reaching a diameter of 30 cm once deployed, this concept gives access to a meter resolution on the ground from a Low Earth Orbit, or to a 70 cm resolution on Mars surface from a 400 km polar orbit. We study in this paper the performance of such a telescope in the aggressive thermal environment of space, with respect to the tight optical requirements of the system.
The Infra-Red Telescope (IRT) is part of the payload of the THESEUS mission, which is one of the two ESA M5 candidates within the Cosmic Vision program, planned for launch in 2032. The THESEUS payload, composed by two high energy wide field monitors (SXI and XGIS) and a near infra-red telescope (IRT), is optimized to detect, localize and characterize Gamma-Ray Bursts and other high-energy transients. The main goal of the IRT is to identify and precisely localize the NIR counterparts of the high-energy sources and to measure their distance. Here we present the design of the IRT and its expected performance.
A well-adapted visible and infrared spectrograph has been developed for the SNAP (SuperNova/Acceleration Probe) experiment proposed for JDEM. The primary goal of this instrument is to ensure the control of Type Ia supernovae. The spectrograph is also a key element for calibration and is able to measure redshift of some thousands of galaxy spectra both in visible and IR.
An instrument based on an integral field method with the powerful concept of imager slicing has been designed and is presented. We present the current design and expected performances. We show that with the current optimization and the proposed technology, we expect the most sensitive instrument proposed on this kind of mission. We recall the readiness of the concept and of the slicer technology thanks to large prototyping efforts performed in France which validate the proposition. This work is supported in France by CNRS/INSU, CNRS/IN2P3 and by the French spatial agency (CNES).
Euclid is a part of the European Space Agency Cosmic Vision program. Euclid mission’s goal is to understand the origin of the accelerating expansion of the Universe. This space mission will embark a 1.2 m Korsch telescope, a visible imager (VIS) and a near-infrared spectrometer and photometer (NISP).
The Euclid mission objective is to understand why the expansion of the Universe is accelerating through by mapping the geometry of the dark Universe
by investigating the distance-redshift relationship and tracing the evolution of cosmic structures. The Euclid project is part of ESA's Cosmic Vision
program with its launch planned for 2020 (ref [1]).
The NISP (Near Infrared Spectrometer and Photometer) is one of the two Euclid instruments and is operating in the near-IR spectral region (900-
2000nm) as a photometer and spectrometer. The instrument is composed of:
- a cold (135K) optomechanical subsystem consisting of a Silicon carbide structure, an optical assembly (corrector and camera lens), a filter wheel
mechanism, a grism wheel mechanism, a calibration unit and a thermal control system
- a detection subsystem based on a mosaic of 16 HAWAII2RG cooled to 95K with their front-end readout electronic cooled to 140K, integrated on a
mechanical focal plane structure made with molybdenum and aluminum. The detection subsystem is mounted on the optomechanical subsystem
structure
- a warm electronic subsystem (280K) composed of a data processing / detector control unit and of an instrument control unit that interfaces with the
spacecraft via a 1553 bus for command and control and via Spacewire links for science data
This presentation describes the architecture of the instrument at the end of the phase C (Detailed Design Review), the expected performance, the
technological key challenges and preliminary test results obtained for different NISP subsystem breadboards and for the NISP Structural and Thermal
model (STM).
In the scope of EUCLID spatial mission, NISP instrument requires high positioning accuracy and high dimensional stability to achieve the required optical performances. LAM is in charge of the development of the instrument main structure which is based on silicon carbide material technology and allows the accurate positioning and maintain of the optomechanical concept sub-systems. This article presents the main steps of this development. It describes the challenging design of this mechanical concept. The associated finite element model, demonstrating the thermomechanical strength of the structure, is presented. Spatial environment vibrations tests performed on the hardware are explained and detailed: requirements, instrumentation and test methodology with the introduction of notching. Finally, the correlation study between finite element analyses and tests is exposed.
The Euclid mission objective is to understand why the expansion of the Universe is accelerating by mapping the geometry of the dark Universe by
investigating the distance-redshift relationship and tracing the evolution of cosmic structures. The Euclid project is part of ESA's Cosmic Vision
program with its launch planned for 2020.
The NISP (Near Infrared Spectro-Photometer) is one of the two Euclid instruments and is operating in the near-IR spectral region (0.9-2μm) as a
photometer and spectrometer. The instrument is composed of:
- a cold (135K) optomechanical subsystem consisting of a SiC structure, an optical assembly (corrector and camera lens), a filter wheel mechanism, a
grism wheel mechanism, a calibration unit and a thermal control system
- a detection subsystem based on a mosaic of 16 Teledyne HAWAII2RG cooled to 95K with their front-end readout electronic cooled to 140K,
integrated on a mechanical focal plane structure made with Molybdenum and Aluminum. The detection subsystem is mounted on the optomechanical
subsystem structure
- a warm electronic subsystem (280K) composed of a data processing / detector control unit and of an instrument control unit that interfaces with the
spacecraft via a 1553 bus for command and control and via Spacewire links for science data
This presentation describes the architecture of the instrument at the end of the phase B (Preliminary Design Review), the expected performance, the
technological key challenges and preliminary test results obtained on a detection system demonstration model.
The Euclid mission objective is to map the geometry of the dark Universe by investigating the distance-redshift
relationship and the evolution of cosmic structures. The NISP (Near Infrared Spectro-Photometer) is one of the two
Euclid instruments operating in the near-IR spectral region (0.9-2μm). The instrument is composed of:
- a cold (140K) optomechanical subsystem constituted by a SiC structure, an optical assembly, a filter wheel
mechanism, a grism wheel mechanism, a calibration unit and a thermal control
- a detection subsystem based on a mosaic of 16 Teledyne HAWAII2RG 2.4μm. The detection subsystem is
mounted on the optomechanical subsystem structure
- a warm electronic subsystem (280K) composed of a data processing / detector control unit and of an
instrument control unit.
This presentation will describe the architecture of the instrument, the expected performance and the technological key
challenges. This paper is presented on behalf of the Euclid Consortium.
The Euclid mission proposed in the context of the ESA Cosmic Vision program is aimed to study the challenging
problem of the Dark Energy, responsible of the acceleration of the Universe. One of the three probes of Euclid is
dedicated to study the Baryonic Acoustic Oscillations by means of spectroscopic observations of millions of galaxies in
the Near Infrared. One option for the Euclid Near Infrared Spectrograph (ENIS) is a multi-slit approach based on Digital
Micromirror Device (DMD) used as reconfigurable slit mask. The Texas Instrument 2048*1080 DMD with 13.68
micrometers pitch has been chosen. ENIS optical design is composed of four arms each using one DMD to cover a total
FOV of 0.48 square degree. The fore-optic design has to cope with the difficult task of having simultaneously a fast
beam (F/2.7) and a quasi-diffraction limited image on a 24 deg tilted plane. The compact three mirrors spectrograph is
using a grism in convergent beam for simplicity and compactness purposes. From the optical design, the mechanical
structure is based on a common carbon honeycomb bench to reach the challenging requirements of volume and mass.
For integral field spectroscopy R&D activities in progress at LAM, and particularly in relation with SNAP - SuperNova/Acceleration Probe - spectrograph, LAM has an on-going program to qualify Image Slicers for space
instrumentation. In this context, an optomechanical concept of an image slicer supported by three bipods has been
designed, realized and tested at the laboratory. This paper presents the mechanical design of the invar mount equipped
with three bipods and supporting an assembly of 60 thin zerodur slices tied together thanks to optical contact. We
document the design improvement made from last blades flexures prototype and we describe all the tests conducted on
this new prototype: optical contact tests, vibration tests and thermal cycles. Thanks to a detailed FEM analysis on this
three bipods concept, we correlate simulations with tests.
A well-adapted visible and infrared spectrograph has been developed for the SNAP (SuperNova/Acceleration Probe)
experiment proposed for JDEM. The primary goal of this instrument is to ensure the control of Type Ia supernovae. The
spectrograph is also a key element for calibration and is able to measure redshift of some thousands of galaxy spectra
both in visible and IR.
An instrument based on an integral field method with the powerful concept of imager slicing has been designed and is
presented. We present the current design and expected performances. We show that with the current optimization and
the proposed technology, we expect the most sensitive instrument proposed on this kind of mission. We recall the
readiness of the concept and of the slicer technology thanks to large prototyping efforts performed in France which
validate the proposition. This work is supported in France by CNRS/INSU, CNRS/IN2P3 and by the French spatial
agency (CNES).
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