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.
ÉBANO will be a new instrument for the 84-cm telescope in the Observatorio Astronómico Nacional in Sierra de San Pedro Mártir (Baja California Norte, Mexico) that will do integral field spectroscopy over two spectral ranges of 30 nm in wavelength in an unusually large field of view of 6.5×6.5 arcsec. The technique used by ÉBANO allows a wavelength scan over a wide spectral range by tilting a narrow-band filter thus changing the central wavelength of the transmission curve. We plan to begin observations with a complete cartography of the Andromeda galaxy (M31) with a mosaic of over 250 images, a region never fully explored with spatially resolved spectroscopy. Using two different filters we will sample the spectral range that covers the lines of NII, Hα, HeI and SII, and the range that covers OIII and Hβ, which gives ÉBANO a huge scientific potential.
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 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.
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.
A variety of electromagnetic interference (EMI) issues can emerge during the development of an astronomical instrument impacting project scope, budget and schedule. Furthermore, if the problem is detected at the observatory it would lead to delay the commissioning of the instrument or can degrade the instrument operation performance. To reduce the interference at levels that no longer represent a problem, namely, to achieve the instrument’s electromagnetic compatibility (EMC) its developers need to tackle the problem in an integrated approach along the entire project cycle development, starting at the early stages. In this paper we dig into some reported EMI issues related to astronomical instrumentation and the proactive measures taken in some observatories to preserve EMC. We present the main practices to achieve EMC, from the electrical engineering perspective, and we identify the key aspects that the project team needs to take into account from the systems engineering and project management perspectives.
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.
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.