One of the challenges of astronomical instrumentation is overcoming the intermediate stages between instrument design and acceptance testing. Manufacturing, integration tasks, and especially testing to validate these instruments require specialized infrastructure. At the Instituto de Astronomía de la Universidad Nacional Autónoma de México (IA-UNAM), we have recognized the importance of investing in this infrastructure to ensure quality, cost efficiency, and timely completion. In this paper, we present the capabilities of IA-UNAM in the design, manufacturing, and metrology of optical and mechanical components that meet astronomical and aerospace quality requirements and standards. We also discuss the adaptation of spaces necessary to perform these tasks, as well as the development of methodologies and instrumentation that we have implemented for the integration and validation stages of these instruments.
FRIDA (inFRared Imager and Dissector for Adaptive optics of GTC) is 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 describes the main achievements and current status in the development of the electronics and control systems for FRIDA´s cryogenic mechanisms, cabling, and keeping (HK). A description of the main hardware and software tests is presented.
FRIDA is an infrared (0.9 microns- 2.5 microns ) imager and integral field spectrograph that will work in concert with the Gran Telescopio Canarias Adaptive Optics system (GTCAO). We describe the assembly, integration and validation of the FRIDA optics: the manufacture of the optical components at our UNAM workshops; the opto-mechanical assembly including the alignment and interferometric validation tests; the assembly and testing of all of the optics and mechanisms on a the cold bench at room temperature. Finally, the cryogenic subsystems validation, prior to the final assembly and integration of the instrument inside the FRIDA cryostat.
We present the design concept and validation of a cryogenic lens mount for a noncemented doublet for the near-infrared diffraction limited instrument FRIDA. The design uses an autocentering mount that maintains the relative alignment of the lenses, acting against any displacement that may be induced by external forces by automatically returning the lenses to their nominal positions. Autocentering techniques have been used for instruments at room temperature with relatively relaxed image quality requirements. We present in detail its application to a mount for a cryogenic instrument working at the diffraction limit. The design has been tested on the collimator of FRIDA, a noncemented doublet of CaF2 and S-FTM16. We describe the alignment requirements of the system, and we show the calculations that ensure that the lenses will suffer both appropriate stresses and temperature differences. We present the experimental validation of a prototype, demonstrating that the design delivers an excellent performance without inducing unnecessary stresses on the optical components, provided that the lenses are previously aligned with very high precision.
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.
KEYWORDS: Cameras, Collimators, Mirrors, Current controlled current source, Diffraction, Near infrared, Iterated function systems, Cryogenics, Spectrographs, Prototyping
FRIDA (inFRared Imager and Dissector for the Adaptive optics system of the Gran Telescopio Canarias
(GTC)) is designed as a diffraction limited instrument that will offer broad and narrow band imaging and
integral field spectroscopy capabilities with low, intermediate 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 and
the imaging and IFS observing modes will use the same Teledyne 2Kx2K detector. FRIDA will be based on a
Nasmyth B of GTC, behind the adaptive optics (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, including resolved stellar populations, semidetached
binary systems, young stellar objects and star forming environments. FRIDA subsystems are
presently being manufactured and tested. In this paper we present the challenges to perform the verification of
some critical specifications of a cryogenic and diffraction limited NIR instrument as FRIDA. FRIDA is a
collaborative project between the main GTC partners, namely, Spain, México and Florida.
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.
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: 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.
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.
We describe diamond-turned material tests for the integral field unit (IFU) for the FRIDA instrument (inFRared Imager
and Dissector for the Adaptive optics system of the Gran Telescopio Canarias). FRIDA is closely based on the design of
the successful FISICA cryogenic infrared image slicing device, which used "monolithic" mirror arrays, diamond turned
into single pieces of metal. FRIDA, however, will require better roughness characteristics than the 15nm RMS of
FISICA to avoid light scatter in FRIDA's shorter wavelength limit (900nm). Al 6061 seems to be limited to this
roughness level by its silicate inclusions so some new combination of materials that are compatible with FRIDA's Al
6061 structure must be found. To this end, we have tested six diamond-turned mirrors with different materials and
different platings. We used the Zygo interferometer facility at IA-UNAM to do warm and cold profile measurements of
the mirrors to investigate possible bimetallic deformation effects. We present a detailed comparison of the various
performance characteristics of the test mirrors.
FRIDA (inFRared Imager and Dissector for the Adaptive optics system of the Gran Telescopio Canarias) has been
designed as a diffraction limited instrument that will offer broad and narrow band imaging and integral field
spectroscopy (IFS) capabilities with low, intermediate and high spectral resolutions to operate in the wavelength range
0.9 - 2.5 μm. The integral field unit is based on a monolithic image slicer based on the University of Florida FISICA.
Both, the imaging mode and IFS observing modes will use the same Rockwell 2K×2K detector. FRIDA will be based at
a Nasmyth focus of GTC, behind the GTCAO system. The FRIDA optical design, stray light analysis, tolerance analysis
and manufacturing feasibility are described in this contribution.
Access to the requested content is limited to institutions that have purchased or subscribe to SPIE eBooks.
You are receiving this notice because your organization may not have SPIE eBooks access.*
*Shibboleth/Open Athens users─please
sign in
to access your institution's subscriptions.
To obtain this item, you may purchase the complete book in print or electronic format on
SPIE.org.
INSTITUTIONAL Select your institution to access the SPIE Digital Library.
PERSONAL Sign in with your SPIE account to access your personal subscriptions or to use specific features such as save to my library, sign up for alerts, save searches, etc.