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Grupo de Instrumentación Criogénica y Astronómica
Coordinación de línea
Estudio de la biodiversidad, ecología, evolución y mecanismos moleculares de adaptación de microorganismos y poblaciones microbianas de ambientes de interés astrobiólogico.
Two research lines are developed within the group:
Superconducting technologies are fundamental for a wide variety of applications, ranging from state-of-the-art astronomical instrumentation for astronomical facilities to devices for quantum computation or biological sensing.
In recent years, we have developed the required skills and resources for the development of microwave superconducting technologies, covering the design, nanofabrication and low temperature (mK) electrical and optical characterization of large-format resonator arrays with more than 1000 elements.
Left: Large format array of Ti-Al based Kinetic Inductance Detectors mounted on dilution cryostat for its characterization. Center: Cryogenic frequency sweep for superconducting resonators characterization. Each dip corresponds to each resonator coupled to the tested transmission line. Right: NbTiN Low Impedance Lumped Element Resonator for its coupling to nuclear transitions of Yb-Trensal microcrystals (shown in a SEM image as instet).
The main lines of research and development are:
– SUPERCONDUCTING KINETIC INDUCTANCE DETECTORS:
Within the field of microwave superconducting technologies, Kinetic Inductance Detectors (KIDs) represent state-of-the-art radiation detectors for millimeter, submillimeter, and far-infrared astronomical instrumentation. In this context, we have participated in the European project SPACEKIDS, funded under FP7, aimed at developing advanced KID arrays for space missions. We were also involved in the CORE mission proposal, submitted to the ESA M5 call in 2017, and we are currently contributing to the PRIMA NASA probe mission. In addition, we are members of the NIKA2, KISS, and CONCERTO collaborations, led by the Institut Néel–CNRS, which focus on the development of large-format KID-based cameras operating in the millimeter range, designed to map dust emission polarization and the Cosmic Microwave Background. At the national level, we lead the Spanish network KIDsNET, which coordinates KID development efforts across Spain. CAB also leads the CADEx experiment, which develops KID arrays for dark matter axion detection within the W-band (75–110 GHz), hosted at the Laboratorio Subterráneo de Canfranc (LSC). Furthermore, we participate in the AtLAST observatory project, the next-generation 50-meter class single-dish telescope planned for ESO, where we are studying KIDs as the baseline technology for its detectors.
– SUPERCONDUCTING LUMPED RESONATORS for quantum computation:
High-quality superconducting circuits are an essential component of state-of-the-art quantum computers. Our group is optimizing the development of high quality resonators, performing simulations, nanofabrication and cryogenic characterization of an hybrid quantum processor unit based on molecular qubits. These high quality resonators have the potential to be employed for the development of other key quantum technologies such as parametric amplifiers or quantum sensors of organic materials.
– CRYOGENIC SYSTEMS FOR ASTROPHYSICS APPLICATIONS
We are also developing associated key technologies, including microwave circuits, cryogenics, electrical components or nanofabrication protocols, among others. The expertise of the group also covers the development of cryogenic systems for both space telescopes such SPICA and Athena and ground-based instruments such as MOSAIC.
This research line is dedicated to the development of optical instrumentation for ground-based observatories like ELT, VLT, GTC and/or CAHA. The group has expertise in almost all the phases of the instrument development: from the conceptual design to the integration, test and verification phases. Currently, the group is formed by engineers from several disciplines (e.g. mechanical, optics, electronics, AIV and software) that could cover different aspects of the technical development phases, and scientists to support and assess the scientific performance of the instruments, and guarantee its future exploitation.
The activities include:
– ELT-HARMONI:
HARMONI is the first-light integral field spectrograph (IFS) for the Extremely Large Telecope (ELT). With its visible and near-IR IFS capabilities, HARMONI is an ambitious technical development that will address a broad range of scientific goals, from the direct imaging and spectroscopy of exoplanets to the study of the properties of distant galaxies. HARMONI is expected to be available as soon as the ELT begins its operations in ~2030.
Left: 3D CAD render of the Low-order Wavefront Sensing Subsystem, designed at CAB. Right: Positioning stage prototype under development for the Calibration Module of HARMONI.
The instrument is being developed by an international consortium conformed by Oxford University, UK-ATC, CRAL, LAM, IAC, CAB & Michigan University, The group is responsible of three of the technical Work Packages, Calibration Module (CARS-CM), LOWFS Pick Off Unit (LOWFS-LPOU) and Instrument Calibration and Alignment System (IFS-ICAS) of HARMONI, and also in charge of developing its Calibration Plan, and HSIM, the observation simulator for the instrument.
Left: 3D CAD render of one single LPOA, designed at CAB. Right: Preliminary design for CM.
– ELT:
MOSAIC is the first Multi-Object Spectrograph (MOS) for the ELT, and part of its second generation of instruments. It is conceived as a multi-purpose MOS, covering the visible and near-IR, with the capability of observe simultaneously ~200 objects across the widest possible field of view provided by the ELT (~40 arcmin^2). The characteristics of MOSAIC make it a unique instrument among the planned instruments for the ELT and fully complementary in this landscape in terms of wavelength coverage, spectral resolution and field of view. The MOSAIC Consortium includes more than 14 institutions located across Europe, Brazil and USA.
– ELT-ANDES:
ANDES is the high-resolution spectrograph for the ELT, and also part of its second generation of instruments. With its visible and near-IR capabilities, ANDES will enable astronomers to research an unprecedented range of topics spanning most areas of astrophysics and even breaking into the domain of fundamental physics. The ANDES project is developed by an international Consortium composed by Research Institutes of 14 Countries. CAB is responsible of the development and manufacture of several mirror mounts for the visible channel spectrograph.
– TARSIS (CAHA 3.5m):
TARSIS is a wide-FoV, blue-optimized IFS for the Calar Alto Observatory 3.5m. Expected to be available by the end of 2028, TARSIS and its scientific survey CATARSIS is being developed by the Universidad Complutense de Madrid (UCM), Instituto de Astrofísica de Andalucía (IAA CSIC), INAOE, Universidad de Sevilla (US), Universidad de Granada (UGR), Universidad de Almería (UAL), CAB, and FRACTAL company. CAB is currently responsible of the Exposure and Observations Simulator of the instrument, together with the data storage and archive of the CATARSIS survey.
Screenshot of the TARSIS Exposure Time Calculator prototype developed by the group
Miembros | Investigadores
Departamento de Instrumentación avanzada
Teléfono: +34 915206404