LiteBIRD, the next-generation cosmic microwave background (CMB) experiment, aims for a launch in Japan’s fiscal year 2032, marking a major advancement in the exploration of primordial cosmology and fundamental physics. Orbiting the Sun-Earth Lagrangian point L2, this JAXA-led strategic L-class mission will conduct a comprehensive mapping of the CMB polarization across the entire sky. During its 3-year mission, LiteBIRD will employ three telescopes within 15 unique frequency bands (ranging from 34 through 448 GHz), targeting a sensitivity of 2.2 μK-arcmin and a resolution of 0.5° at 100 GHz. Its primary goal is to measure the tensor-toscalar ratio r with an uncertainty δr = 0.001, including systematic errors and margin. If r ≥ 0.01, LiteBIRD expects to achieve a > 5σ detection in the ℓ = 2–10 and ℓ = 11–200 ranges separately, providing crucial insight into the early Universe. We describe LiteBIRD’s scientific objectives, the application of systems engineering to mission requirements, the anticipated scientific impact, and the operations and scanning strategies vital to minimizing systematic effects. We will also highlight LiteBIRD’s synergies with concurrent CMB projects.
Large-format infrared detectors are at the heart of major ground and space-based astronomical instruments, and the HgCdTe HxRG is the most widely used. The Near Infrared Spectrometer and Photometer (NISP) of the ESA’s Euclid mission launched in July 2023 hosts 16 H2RG detectors in the focal plane. Their performance relies heavily on the effect of image persistence, which results in residual images that can remain in the detector for a long time contaminating any subsequent observations. Deriving a precise model of image persistence is challenging due to the sensitivity of this effect to observation history going back hours or even days. Nevertheless, persistence removal is a critical part of image processing because it limits the accuracy of the derived cosmological parameters. We will present the empirical model of image persistence derived from ground characterization data, adapted to the Euclid observation sequence and compared with the data obtained during the in-orbit calibrations of the satellite.
KEYWORDS: Electronic design automation, Sensors, Digital signal processing, Signal detection, Microwave radiation, Inductance, Field programmable gate arrays, Signal processing, Design, Tunable filters
The IAC Electronics Department has developed a high-performance embedded Data Acquisition System (eDAS) to perform the readout of an array of microwave kinetic inductance detectors (MKIDs) and to carry out hardware-based digital signal processing in real time. The eDAS has been developed using the Zynq UltraScale+ RFSoC ZCU111 Evaluation Kit and PYNQ software framework. The ultimate goal is to be able to detect changes in the amplitude and phase of the MKID’s signal when a photon arrives at the detector, in order to observe a single photon signature. We have been able to identify the resonant frequency of individual pixels in total darkness.
FRIDA is a diffraction-limited imager and integral-field spectrograph for the adaptive-optics focus of the Gran Telescopio Canarias. In imaging mode FRIDA provides scales of 10, 20 and 40 mas/pixel and in IFS mode spectral resolutions of about 1200, 4000 and 30,000. Coronographic masks are available in both modes for highcontrast images. FRIDA is undergoing systems integration and is scheduled to complete system testing at the laboratory in December 2024 and to be delivered to the telescope shortly thereafter. In this contribution we present a summary of its design, fabrication, current status and potential scientific applications.
FRIDA is a diffraction-limited imager and integral-field spectrograph for the adaptive-optics focus of the Gran Telescopio Canarias. In imaging mode FRIDA provides scales of 10, 20 and 40 mas/pixel and in IFS mode spectral resolutions of about 1200, 4000 and 30,000. Coronographic masks are available in both modes for high-contrast images. FRIDA is starting systems integration and is scheduled to complete system testing at the laboratory by the end of 2023 and to be delivered to the telescope shortly thereafter. In this contribution we present a summary of its design, fabrication, current status and potential scientific applications.
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.
FRIDA is a diffraction-limited imager and integral-field spectrometer that is being built for the adaptive-optics focus of the Gran Telescopio Canarias. In imaging mode FRIDA will provide scales of 0.010, 0.020 and 0.040 arcsec/pixel and in IFS mode spectral resolutions of 1500, 4000 and 30,000. FRIDA is starting systems integration and is scheduled to complete fully integrated system tests at the laboratory by the end of 2017 and to be delivered to GTC shortly thereafter. In this contribution we present a summary of its design, fabrication, current status and potential scientific applications.
KEYWORDS: Control systems, Control systems, Cryogenics, Computer programming, Prototyping, Interfaces, Calibration, Current controlled current source, Electronics, Human-machine interfaces
FRIDA will be a near infrared imager and integral field spectrograph covering the wavelength range from 0.9 to 2.5 microns. FRIDA will work in two observing modes: direct imaging and integral field spectroscopy. This paper presents the main structure of the FRIDA mechanisms control system. In order to comply with a high level of re-configurability FRIDA will comprise eight cryogenic mechanisms and one room temperature mechanism. Most of these mechanisms require high positioning repeatability to ensure FRIDA fulfills with high astronomical specifications. In order to set up the mechanisms positioning control parameters a set of programs have been developed to perform several tests of mechanisms in both room and cryogenic environments. The embedded control software for most of the FRIDA mechanisms has been developed. A description of some mechanisms tests and the software used for this purpose are presented.
Rafael Toledo-Moreo, Carlos Colodro-Conde, Jaime Gómez-Sáenz-de-Tejada, David Pérez-Lizán, José Javier Díaz-García, Óscar Tubío-Araujo, Cayetano Raichs, Jordi Catalán, Rafael Rebolo-López
KEYWORDS: Control systems, Electronics, Calibration, Sensors, Near infrared, Power supplies, Clocks, Light emitting diodes, Interfaces, Field programmable gate arrays
The Near Infrared Spectrograph and Photometer (NISP) is one of the instruments on board the ESA EUCLID mission. The Universidad Polit´ecnica de Cartagena and Instituto de Astrof´ısica de Canarias are responsible of the Instrument Control Unit of the NISP (NI-ICU) in the Euclid Consortium. The NI-ICU hardware is developed by CRISA (Airbus Defence and Space), and its main functions are: communication with the S/C and the Data Processing Unit, control of the Filter and Grism Wheels, control of the Calibration Unit and thermal control of the instrument. This paper presents the NI-ICU status of definition and design at the end of the detailed design phase.
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).
Rafael Toledo-Moreo, Carlos Colodro-Conde, José Javier Díaz-García, Óscar Manuel Tubío-Araujo, Jaime Gómez-Sáenz, Antonio Peña-Godino, Tirso Velasco-Fernández, Sebastián Sánchez-Prieto, Isidro Villó-Pérez, Rafael Rebolo-López
KEYWORDS: Sensors, Field programmable gate arrays, Calibration, Light emitting diodes, Power supplies, Control systems, Electronics, Near infrared, Spectrographs, Position sensors
The Near Infrared Spectrograph and Photometer (NISP) is one of the instruments on board the ESA EUCLID mission. The Universidad Politecnica de Cartagena and Instituto de Astrofisica de Canarias are responsible of the Instrument Control Unit of the NISP (NI-ICU) in the Euclid Consortium. The NI-ICU main functions are: communication with the S/C and the Data Processing Unit, control of the Filter and Grism Wheels, control of the Calibration Unit and thermal control of the instrument. This paper presents the NI-ICU status of definition and design at the end of the preliminary design phase.
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.
KEYWORDS: Control systems, Cryogenics, Electronics, Photonic integrated circuits, Prototyping, Control systems design, Sensors, Electronic components, 3D modeling, Connectors
FRIDA will be a near infrared imager and integral field spectrograph covering the wavelength range from 0.9 to 2.5 microns. Primary observing modes are: direct imaging and integral field spectroscopy. This paper describes the main advances in the development of the electronics and control system for both the mechanisms and house-keeping of FRIDA. In order to perform several tests of mechanisms in both room and cryogenic environments, a set of programs had been developed. All variables of the vacuum control system were determined and the main control structure based on one Programmable Logic Controller (PLC) had been established. A key function of the FRIDA’s control system is keeping the integrity of cryostat during all processes, so we have designed a redundant heating control system which will be in charge of avoiding cryostat inner overheating. In addition, some improvements of cryogenic and room temperature cabling structure are described.
KEYWORDS: Electronics, Control systems, Sensors, Data acquisition, Inspection, Adaptive optics, Human-machine interfaces, Infrared telescopes, Imaging systems, Process control
FRIDA (inFRared Imager and Dissector for the Adaptive optics system of the Gran Telescopio Canarias) is a diffraction
limited instrument that will offer broad and narrow band imaging and integral field spectroscopy with low, intermediate
and high spectral resolutions in the 0.9 - 2.5 μm wavelength range. FRIDA will be installed at a Nasmyth focus of GTC,
behind the AO system. The characteristics and development status of the Control and Housekeeping Electronics are
described in this contribution.
FRIDA is a collaborative project between the IAC (Spain), UNAM (México), UCM (Spain) and the UF (Florida), lead
by UNAM.
FRIDA is a diffraction limited imager and integral field spectrometer that is being built for the Gran Telescopio
Canarias. FRIDA has been designed and is being built as a collaborative project between institutions from México, Spain
and the USA. In imaging mode FRIDA will provide scales of 0.010, 0.020 and 0.040 arcsec/pixel and in IFS mode
spectral resolutions R ~ 1000, 4,500 and 30,000. FRIDA is starting systems integration and is scheduled to complete
fully integrated system tests at the laboratory by the end of 2015 and be delivered to GTC shortly after. In this
contribution we present a summary of its design, fabrication, current status and potential scientific applications.
KEYWORDS: Sensors, High dynamic range imaging, Astronomical imaging, Calibration, Imaging spectroscopy, Linear filtering, Near infrared, Cadmium sulfide, Black bodies, Spectroscopy
EMIR is the NIR imager and multiobject spectrograph being built as a common user instrument for the GTC and it is
currently entering in the integration and verification phase at system level. EMIR is being built by a Consortium of
Spanish and French institutes led by the IAC.
In this paper we describe the readout modes of EMIR detector, a Hawaii2 FPA, after two full calibrations campaigns.
Besides the standard set of modes (reset-read, CDS, Fowler, Follow-up the ramp), the modified SDSU-III hardware and
home made software will also offer high dynamic range readout modes, which will improve the ability of the instrument
to sound densely populated areas which often are made of objects with large differences in brightness. These new high
dynamic range modes are: single readout with very short integration time, window mode and combination of both. The
results show that the new modes behave linearly with different exposition times, improve the maximum frame rate and
increase the saturation limit in image mode for EMIR instrument.
FRIDA (inFRared Imager and Dissector for the Adaptive optics system of the Gran Telescopio Canarias) is designed as
a diffraction limited instrument that will offer broad and narrow band imaging and integral field spectroscopy capabilities
with low (R ~ 1,500), intermediate (R ~ 4,500) and high (R ~ 30,000) spectral resolutions to operate in the wavelength
range 0.9 - 2.5 μm. The integral field unit is based on a monolithic image slicer. The imaging and IFS observing modes
will use the same Teledyne 2K x 2K detector. FRIDA will be based at the Nasmyth B platform of GTC, behind the AO
system. The key scientific objectives of the instrument include studies of solar system bodies, low mass objects,
circumstellar outflow phenomena in advanced stages of stellar evolution, active galactic nuclei, high redshift galaxies,
resolved stellar populations, semi-detached binary systems, young stellar objects and star forming environments. FRIDA
is a collaborative project between the main GTC partners, namely, Spain, México and Florida. In this paper, we present
the status of the instrument design as it is currently being prepared for its manufacture, after an intensive prototypes'
phase and design optimization. The CDR was held in September 2011.
KEYWORDS: Control systems, Electronics, Control systems design, Sensors, Prototyping, Temperature sensors, Photonic integrated circuits, Human-machine interfaces, Optical benches, Infrared radiation
FRIDA will be a common-user near infrared imager and integral field spectrograph covering the wavelength range from
0.9 to 2.5 microns. Primary observing modes driven the instrument design are two: direct imaging and integral field
spectroscopy. FRIDA will be installed at the Nasmyth-B platform of the Gran Telescopio Canarias (GTC) behind the
GTC Adaptive Optics (GTCAO) system. Instrument will use diffraction-limited optics to avoid degrading the high Strehl
ratios derived by the GTCAO system in the near infrared.
High-performance astronomical instruments with a high reconfiguration degree as FRIDA, not only depends on optical
and mechanical efficient designs but also on the good quality of its electronics and control systems design. In fact,
astronomical instruments operating performance on telescope greatly relies on electronics and control system. This paper
describes the main design topics for the FRIDA electronics and mechanisms control system, pointing on the
development that these areas have reached on the project status. FRIDA Critical Design Review (CDR) was held on
September 2011.
For the first time, sub-electron read noise has been achieved with a camera suitable for astronomical wavefront-sensing
(WFS) applications. The OCam system has demonstrated this performance at 1300 Hz frame rate and with
240×240-pixel frame rate.
ESO and JRA2 OPTICON2 have jointly funded e2v technologies to develop a custom CCD for Adaptive Optics (AO)
wavefront sensing applications. The device, called CCD220, is a compact Peltier-cooled 240×240 pixel frame-transfer
8-output back-illuminated sensor using the EMCCD technology. This paper demonstrates sub-electron read noise at
frame rates from 25 Hz to 1300 Hz and dark current lower than 0.01
e-/pixel/frame. It reports on the comprehensive,
quantitative performance characterization of OCam and the CCD220 such as readout noise, dark current, multiplication
gain, quantum efficiency, charge transfer efficiency... OCam includes a low noise preamplifier stage, a digital board to
generate the clocks and a microcontroller. The data acquisition system includes a user friendly timer file editor to
generate any type of clocking scheme. A second version of OCam, called OCam2, was designed offering enhanced
performances, a completely sealed camera package and an additional Peltier stage to facilitate operation on a telescope or
environmentally rugged applications. OCam2 offers two types of
built-in data link to the Real Time Computer: the
CameraLink industry standard interface and various fiber link options like the sFPDP interface. OCam2 includes also a
modified mechanical design to ease the integration of microlens arrays for use of this camera in all types of wavefront
sensing AO system. The front cover of OCam2 can be customized to include a microlens exchange mechanism.
The plenoptic wavefront sensor combines measurements at pupil and image planes in order to obtain wavefront
information from different points of view simultaneously, being capable to sample the volume above the telescope to
extract the tomographic information of the atmospheric turbulence. After describing the working principle, a laboratory
setup has been used for the verification of the capability of measuring the pupil plane wavefront. A comparative
discussion with respect to other wavefront sensors is also included.
The use of AO in Extremely Large Telescopes, used to improve performances in smaller telescopes, becomes now
mandatory to achieve diffraction limited images according to the large apertures. On the other hand, the new dimensions
push the specifications of the AO systems to new frontiers where the order of magnitude in terms of computation power,
time response and the required numbers of actuators impose new challenges to the technology. In some aspects
implementation methods used in the past result no longer applicable. This paper examines the real dimension of the
problem imposed by ELTs and shows the results obtained in the laboratory for a real modal wavefront recovery
algorithm (Hudgin) implemented in FPGAs. Some approximations are studied and the performances in terms of
configuration parameters are compared. Also a preferred configuration will be justified.
ESO and JRA2 OPTICON have jointly funded e2v technologies to develop a custom CCD for Adaptive Optic Wave
Front Sensor (AO WFS) applications. The device, called CCD220, is a compact Peltier-cooled 240×240 pixel frametransfer
8-output back-illuminated sensor. Using the electron-multiplying technology of L3Vision detectors, the device
is designed to achieve sub-electron read noise at frame rates from 25 Hz to 1,500 Hz and dark current lower than 0.01
e-/pixel/frame. The development has many unique features. To obtain high frame rates, multiple EMCCD gain registers
and metal buttressing of row clock lines are used. The baseline device is built in standard silicon. In addition, two
speculative variants have been built; deep depletion silicon devices to improve red response and devices with an
electronic shutter to extend use to Rayleigh and Pulsed Laser Guide Star applications. These are all firsts for L3Vision
CCDs.
These CCD220 detectors have now been fabricated by e2v technologies. This paper describes the design of the device,
technology trade-offs, and progress to date. A Test Camera, called "OCam", has been specially designed and built for
these sensors. Main features of the OCam camera are extensively described in this paper, together with first light images
obtained with the CCD220.
ELTs laser guide stars wavefront sensors are planned to have specifically developed sensor chips, which will probably
include readout logic and D/A conversion, followed by a powerful FPGA slope computer located very close to it, but not
inside for flexibility and simplicity reasons. This paper presents the architecture of an FPGA-based wavefront slope
computer, capable of handling the sensor output stream in a massively parallel approach. It will feature the ability of
performing dark and flat field correction, the flexibility needed for allocating complex processing schemes, the capability
of undertaking all computations expected to be performed at maximum speed, even though they were not strictly related
to the calculation of the slopes, and the necessary housekeeping controls to properly command it and evaluate its
behaviour. Feasibility using today's technology is evaluated, clearly showing its viability, together with an analysis of
the amount of external memory, power consumption and printed circuit board space needed.
This communication shows the design, layout, mounting and start-up of a high-resolution grating spectrograph for VIS-NIR
at GREGOR 1.5m Solar Telescope (Observatorio del Teide, Tenerife, Canary Islands). The instrument will be used
together with the Tenerife Infrared Polarimeter (TIP-II). As special characteristics of the design, the following can be
mentioned: The first folding mirror of the spectrograph can be placed in two positions to take into account the change of the
optical axis introduced by the polarizing beamsplitter of TIP-II. This way the instrument is optimally aligned when used
in situations with and without polarimeter. The second and third mirrors rotate the image of the entrance slit, making it parallel to the grating grooves. A system of prisms are used to adequately fit onto the detector the two orthogonal polarized beams generated by the
polarimeter. Two output beams are possible, to make feasible simultaneous visible and near-infrared observations.
The Configurable Slit Unit (CSU) for EMIR shall enable the possibility to generate a multi-slit configuration, a long slit, or an imaging aperture at the entrance focal plane of the GTC-EMIR instrument. The CSU is therefore a cryogenic reconfigurable slit mechanism. It contains 100 sliding bars which can be positioned within the 307x307mm wide aperture of EMIR's instrument field of view. The development of the CSU has been a challenging task for several reasons: the high number of elements to control to configure a single observing pattern; the nominal working temperature of 77 K at which all the functionalities have to be accomplished, the stringent requirements in both accuracy and repeatability for most of the functionalities and the rotating nature of the EMIR instrument. The combination of these requirements urged the need to develop new pioneering concepts for actuation and position measurement. An actuation mechanism has been developed based on a piezo drive concept. A dedicated incremental, endless capacitive measurement system has been developed to measure the position of each separate bar. Both technologies are successfully realized in the demonstration programme that has been launched to prove the feasibility of the CSU concept. Besides actuation and position control of the bars, also thermal behavior of the CSU concept have been evaluated within the demonstration programme.
EMIR, currently entering into its fabrication and AIV phase, will be one of the first common user instruments for the GTC, the 10 meter telescope under construction by GRANTECAN at the Roque de los Muchachos Observatory (Canary Islands, Spain). EMIR is being built by a Consortium of Spanish and French institutes led by the Instituto de Astrofisica de Canarias (IAC). EMIR is designed to realize one of the central goals of 10m class telescopes, allowing observers to obtain spectra for large numbers of faint sources in an time-efficient manner. EMIR is primarily designed to be operated as a MOS in the K band, but offers a wide range of observing modes, including imaging and spectroscopy, both long slit and multiobject, in the wavelength range 0.9 to 2.5 μm. It is equipped with two innovative subsystems: a robotic reconfigurable multislit mask and disperssive elements formed by the combination of high quality diffraction grating and conventional prisms, both at the heart of the instrument. The present status of development, expected performances, schedule and plans for scientific exploitation are described and discussed. The development and fabrication of EMIR is funded by GRANTECAN and the Plan Nacional de Astronomia y Astrofisica (National Plan for Astronomy and Astrophysics, Spain).
In the past decade, new thermal modelling tools have been offered to system designers. These modelling tools have rarely been used for the cooled instruments in ground-based astronomy. In addition to an overwhelming increase of PC computer capabilities, these tools are now mature enough to drive the design of complex astronomical instruments that are cooled. This is the case for WIRCam, the new wide-field infrared camera installed on the CFHT in Hawaii on the
Mauna Kea summit. This camera uses four 2K×2K Rockwell Hawaii-2RG infrared detectors and includes 2 optical barrels and 2 filter wheels. This camera is mounted at the prime focus of the 3.6m CFHT telescope. The mass to be cooled is close to 100 kg. The camera uses a Gifford Mac-Mahon closed-cycle cryo-cooler. The capabilities of the I-deas thermal module (TMG) is demonstrated for our particular application: predicted performances are presented and compared to real measurements after integration on the telescope in December 2004. In addition, we present thermal modelling of small Peltier cooled CCD packages, including the thermal model of the CCD220 Peltier package (fabricated by e2v technologies) and cold head. ESO and the OPTICON European network have funded e2v technologies to develop a compact packaged Peltier-cooled 8-output back illuminated L3Vision CCD. The device will achieve sub-electron read-noise at frame rates up to 1.5 kHz. The development, fully dedicated to the latest generation of adaptive optics wavefront sensors, has many unique features. Among them, the ultra-compactness offered by a Peltier package integrated in a small cold head including the detector drive electronics, is a way to achieve amazing performances for adaptive optics systems. All these models were carried out using a normal PC laptop.
ESO and JRA2 OPTICON have funded e2v technologies to develop a compact packaged Peltier cooled 24 μm square
240x240 pixels split frame transfer 8-output back-illuminated L3Vision CCD3, L3Vision CCD for Adaptive Optic Wave
Front Sensor (AO WFS) applications. The device is designed to achieve sub-electron read noise at frame rates from 25
Hz to 1,500 Hz and dark current lower than 0.01 e-/pixel/frame. The development has many unique features. To obtain
high frame rates, multi-output EMCCD gain registers and metal buttressing of row clock lines are used. The baseline
device is built in standard silicon. In addition, a split wafer run has enabled two speculative variants to be built; deep
depletion silicon devices to improve red response and devices with an electronic shutter to extend use to Rayleigh and
Pulsed Laser Guide Star applications. These are all firsts for L3Vision CCDs. The designs of the CCD and Peltier
package have passed their reviews and fabrication has begun. This paper will describe the progress to date, the
requirements and the design of the CCD and compact Peltier package, technology trade-offs, schedule and proposed test
plan. High readout speed, low noise and compactness (requirement to fit in confined spaces) provide special challenges
to ESO's AO variant of its NGC, New General detector Controller to drive this CCD. This paper will describe progress
made on the design of the controller to meet these special needs.
EMIR is a multiobject intermediate resolution near infrared (1.0-2.5 microns) spectrograph with image capabilities to be mounted on the 10m Gran Telescopio de Canarias (GTC), located on the Spanish island of La Palma. This paper shows an overview of the EMIR electronics and mechanism control.
First, a description of the detector (a Hawaii-2 array) electronics is given, which involves the use of commercial components (resistors, capacitors and operational amplifiers) working under cryogenic conditions (around 77K). This paper describes the particularities of the cold electronics, showing the problems found and the way to solve them. Preliminary results of the detector characterization are also presented in this paper.
Secondly, an overview of the different mechanisms of the instrument is presented. They are cryogenic mechanisms with pretty stringent positioning requirements. The technological solutions used to meet the tight control requirements will be described.
We present the final global design and performances of EMIR, the NIR multi-object spectrograph of the GTC, as well as the plan for its early scientific exploitation. EMIR, currently in the middle of its final phase, will be one of the first common user instruments for the GTC, the 10 meter telescope under construction by GRANTECAN at the Roque de los Muchachos Observatory (Canary Islands, Spain). EMIR is being built by a Consortium of Spanish and French institutes led by the IAC. EMIR is designed to realize one of the central goals of 10m class telescopes, allowing observers to obtain spectra for large numbers of faint sources in an time-efficient manner. EMIR is primarily designed to be operated as a MOS in the K band, but offers a wide range of observing modes, which include imaging and spectroscopy, both long slit and multi-object, in the wavelength range 0.9 to 2.5 mm. It is equipped with two innovative subsystems: a robotic reconfigurable multi-slit mask and dispersive elements formed by the combination of high quality diffraction grating and conventional prisms, both at the heart of the instrument. The present status of development, expected performances, schedule and plans for scientific exploitation are described and discussed. This project is mostly funded by GRANTECAN and the Plan Nacional de Astronomia y Astrofisica (National Plan for Astronomy and Astrophysics, Spain).
KEYWORDS: Data acquisition, Sensors, Telecommunications, Computer architecture, Infrared spectroscopy, Data communications, Operating systems, Telescopes, Control systems, Data modeling
OSIRIS (Optical System for Imaging and low/intermediate-Resolution Integrated Spectroscopy) and EMIR (InfraRed MultiObject Spectrograph) are instruments designed to obtain images and low resolution spectra of astronomical objects in the optical and infrared domains. They will be installed on Day One and Day Two, respectively, in the Nasmyth focus of the 10-meter Spanish GTC Telescope. This paper describes the architecture of the Data Acquisition System (DAS), emphasizing the functional and quality attributes. The DAS is a component oriented, concurrent, distributed and real time system which coordinates several activities: acquisition of images coming from the detectors controller, tagging, and data communication with the required telescope system resources. This architecture will minimize efforts in the development of future DAS. Common aspects, such as the data process flow, concurrency, asynchronous/synchronous communication, memory management, and exception handling, among others, are managed by the proposed architecture. This system also allows a straightforward inclusion of variable parts, such as dedicated hardware and different acquisition modes. The DAS has been developed using an object oriented approach and uses the Adaptive Communication Environment (ACE) to be operating system independent.
In this contribution we review the overall features of EMIR, the NIR multiobject spectrograph of the GTC. EMIR is at present in the middle of the PD phase and will be one of the first common user instruments for the GTC, the 10 meter telescope under construction by GRANTECAN at the Roque de los Muchachos Observatory (Canary Islands, Spain). EMIR is being built by a Consortium of Spanish, French and British institutes led by the IAC. EMIR is designed to realize one of the central goals of 10m class telescopes, allowing observers to obtain spectra for large numbers of faint sources in an time-efficient manner. EMIR is primarily designed to be operated as a MOS in the K band, but offers a wide range of observing modes, including imaging and spectroscopy, both long slit and multiobject, in the wavelength range 0.9 to 2.5 μm. The present status of development, expected performances and schedule are described and discussed. This project is funded by GRANTECAN and the Plan Nacional de Astronomía y Astrofísica (National Plan for Astronomy and Astrophysics, Spain).
EMIR (Espectrógrafo Multiobjeto Infrarrojo) is a wide-field, near-infrared, multi-object spectrograph, with image capabilities, which will be located at the Nasmyth focus of GTC (Gran Telescopio Canarias). It will allow observers to obtain many intermediate resolution spectra simultaneously, in the nIR bands Z, J, H, K. A multi-slit mask unit will be used for target acquisition.
This paper shows an overview of the EMIR software. Its architecture is distributed with real time features, having in mind to build a reusable, maintainable and inexpensive system. In this paper, we outline the main performances of the current design and some examples already implemented are given.
EMIR is a multiobject intermediate resolution near infrared (1.0 - 2.5 microns) spectrograph with image capabilities to be mounted on the Gran Telescopio Canarias (Observatorio del Roque de los Muchachos, La Palma, Spain). EMIR is under design by a consortium of Spanish, French and British institutions, led by the Instituto de Astrofisica de Canarias. This work has been partially funded by the GTC Project Office. The instrument will deliver images and spectra in a large FOV (6 X 6 arcmin), and because of the telescope image scale (1 arcmin equals 52 mm) and the spectral resolution required, around 4000, one of the major challenges of the instrument is the optics and optomechanics. Different approaches have been studied since the initial proposal, trying to control the risks of the instrument, while fitting the initial scientific requirements. Issues on optical concepts, material availability, temperature as well as optomechanical mounting of the instrument will be presented.
EMIR is a near-IR, multi-slit camera-spectrograph under development for the 10m GTC on La Palma. It will deliver up to 45 independent R equals 3500-4000 spectra of sources over a field of view of 6 feet by 3 feet, and allow NIR imaging over a 6 foot by 6 foot FOV, with spatial sampling of 0.175 inch/pixel. The prime science goal of the instrument is to open K-band, wide field multi-object spectroscopy on 10m class telescopes. Science applications range from the study of star-forming galaxies beyond z equals 2, to observations of substellar objects and dust-enshrouded star formation regions. Main technological challenges include the large optics, the mechanical and thermal stability and the need to implement a mask exchange mechanism that does not require warming up the spectrograph. EMIR is begin developed by the Instituto de Astrofisica de Canarias, the Instituto Nacional de Tecnica Aeroespacial, the Universidad Complutense de Madrid, the Observatoire Midi-Pyrennees, and the University of Durham. Currently in its Preliminary Design phase, EMIR is expected to start science operation in 2004.
KEYWORDS: Cameras, Data acquisition, Clocks, Infrared cameras, Human-machine interfaces, Electrons, Infrared radiation, Sensors, Camera shutters, Control systems
We report here the main characteristics of a near IR camera devoted to astrophysical solar research, which has been developed by the Instituto de Astrofisica de Canarias (IAC). The system is now being used for photometric and spectroscopic applications, and it will also be used for spectropolarimetry in the near future. The first application is described below in detail. The IACs IR camera is based on a Rockwell 256 X 256 HgCdTe NICMOS3 array, sensitive from 1 to 2.5 microns. The necessary cooling system is a LN2- cryostat, designed and built by IR labs under out requirements. The main electronics are the standard VME- based, FPGA programmable MCE-3 system, also developed by IR labs. We have implemented different readout schemes to improve sped, reduce noise and avoid seeing effects, taking into account each specific application. Data are transferred via fiber optics to a control unit, which re-send them to the main data acquisition system. Several acquisition modes to select the best images have been implemented, and a real- time data processing is available, the entire camera has been characterized and calibrated, and the main radiometric parameters given. Preliminary test in spectroscopic observations have been made in the German Towers at the Observatorio del Teide in Tenerife, Spain, and a series of photometric measurements performed in the Swedish Solar Telescope, at the Observatorio del Roque de los Muchachos in La Palma, Spain. As examples, some scientific results are also presented.
We have just finished the first tests at the telescope of an infrared camera designed and developed at the Instituto de Astrofisica de Canarias (IAC). This camera, based on a 256 X 256 focal plane array, has been built to operate at the 1.5 m Carlos Sanchez IR telescope (CST) in the Observatorio del Teide (Canary Islands, Spain). In this paper we describe the final configuration and performance of the camera. Some images taken during two telescope commissioning periods are shown.
The technology division of the Instituto de Astrofisica de Canarias (IAC) is developing a data acquisition system (DAS) for an IR camera to be used at the 1.5m Carlos Sanchez Telescope (TCS) in the Observatorio del Teide (Canary Islands, Spain). This camera will work between a wavelength of 1 and 5 microns and will employ an InSb focal plane array (FPA). The DAS and the user interface are based on a UNIX workstation with a modular transputer based controller. The IGA-256 (Cincinnati Electronics) has been evaluated as a candidate for the focal plane array. The main features related to the potential astronomical performance, such as well depth and dark current are reported. The testing procedures and present status of the camera are discussed.
The Instituto de Astrofisica de Canarias (IAC) is undertaking the construction of an IR camera for astronomical use at the 1.5 meter (f/13,8) Carlos Sanchez IR Telescope (CST), sited at the Observatorio del Teide (Tenerife). The camera will employ a 256 X 256 InSb focal plane array, and will be used in the 1 - 5 micron atmospheric windows. The Camera uses an optical reimaging system which maps 0.5 square arcseconds of sky per pixel. The optical system will be diamond turned in aluminum and mounted in such a way that the optical alignment is facilitated. Two filter wheels will accommodate 14 broad and narrow band filters. A SUN SPARCstation will control the camera and allow data handling and displaying of the images. With this configuration we expect to achieve sensitivities of 17 and 12.5 magnitude (3 (sigma) in 10 sec) at the K and L band respectively.
The Department of Detectors of the Instituto de Astrofisica de Canarias, Spain is developing a data acquisition system (DAS) for an infrared camera based in a 256 X 256 InSb detector. The camera is going to work from 1 to 5 microns wavelength, with a scale on the sky of 0.5 arcsec per pixel, and will be installed as a common user instrument at the Carlos Sanchez Telescope in the Observatorio del Teide (Canary Island, Spain). A multiprocessor architecture has been chosen for the DAS, due to the very tight requirements on real time processing, and high speed storage capability (20 images per second readout rate, 2 images per second storage rate). The complete system is split into two main parts, the front end electronics and the user workstation. They are interconnected through an ETHERNET link.
Hardware design based on 20 MHz transputers, 120 ns first-in, first-out (FIFO) memory, and a 20 MHz counter is discussed. The two transputers are used to generate the states and to write them into the FIFO memory. The data generated by the transputers is written in the FIFO memory in parallel. The system design is characterized by a minimal state of 100 ns, a resolution of 33.3 ns, and fast data rate generation.
The reliable knowledge of a detector is very important in astrophysical research The aim of IAC (Instituto de Asirofisica de Canarias Spain) is to dispose of a versatile system to test evaluate and calibrate a big vanety of imaging detectors which viill be opc ned in the future to the scientific community The main features of this detector test bench are as follows (a) Wide spectral range (JR and visible) and (b) Wide radiation response range For this purpose a compact and c omplete arrangement has been designed Optical, mechanic ,cryogenic and electronic devices are flexible enough to allow the acquisition of data necessary to characterize the detector in a direct way (linearity, dark noise, spectral and time response,...). The high speed of the readout, the data acquisition system and other parameters are designed in such a way, that will make the facility virtually independent of the detector itself. This will allow reliable comparison between different detectors, and also with approved standards. Several procedures and practical examples are extensively discussed in the paper
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