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| QUIJOTE CMB Experiment | |
|---|---|
| Name | QUIJOTE CMB Experiment |
| Abbreviation | QUIJOTE |
| Established | 2009 |
| Location | Teide Observatory, Tenerife, Canary Islands, Spain |
| Coordinates | 28.3006°N 16.5106°W |
QUIJOTE CMB Experiment QUIJOTE CMB Experiment is a ground-based microwave observatory focused on polarization measurements of the cosmic microwave background. It operates at the Teide Observatory near Tenerife and involves a consortium of Spanish and international institutions. The project aims to characterize Galactic foregrounds and constrain cosmological parameters by complementing missions like Planck and experiments such as WMAP, BICEP2, and POLARBEAR.
QUIJOTE was conceived to probe the polarized sky at low microwave frequencies and to disentangle Galactic emission components from primordial signals. The collaboration includes groups from Instituto de Astrofísica de Canarias, Instituto de Física de Cantabria, Universidad de Cantabria, Instituto de Astrofísica de Andalucía, and partners associated with European Space Agency and national agencies. The scientific motivation connects to research pursued by teams behind Max Planck Institute for Astrophysics, Harvard-Smithsonian Center for Astrophysics, Princeton University, California Institute of Technology, and experiments funded by Consejo Superior de Investigaciones Científicas and national science foundations akin to National Science Foundation.
The QUIJOTE facility comprises multiple telescopes and instrument modules designed to cover frequency bands between ~10 GHz and ~40 GHz. The first telescope and its instrumentation were developed with optics and cryogenics influenced by designs used at Atacama Cosmology Telescope and South Pole Telescope. Receiver technology includes polarimeters, orthomode transducers, and correlation receivers similar to hardware from NRAO projects and prototype designs from Jet Propulsion Laboratory. The feed horns and reflectors were manufactured in collaboration with engineering groups linked to Instituto Nacional de Técnica Aeroespacial and European industry partners experienced in microwave instrumentation for missions like Herschel and Planck. Calibration strategies reference methods used by COBE teams and modern implementations from ACTPol and SPTpol groups.
QUIJOTE implements wide-area surveys and targeted deep fields, employing scanning strategies comparable to those used by Planck and WMAP to map polarization Stokes parameters across the northern sky. Observing campaigns coordinate with complementary surveys, including follow-up from LOFAR, VLA, GBT, and radio catalogs from NVSS. The strategy includes monitoring of polarized point sources cataloged by ATCA and cross-correlation with infrared maps from IRAS and Herschel to separate thermal dust and synchrotron emission. Site selection at Teide Observatory leverages infrastructure shared with observatories such as IAC80 and Gran Telescopio Canarias.
Data reduction pipelines integrate time-ordered data processing, map-making, and component separation using algorithms developed in collaboration with groups familiar with HEALPix conventions and analysis packages used by Planck and WMAP teams. Map-making employs destriping and maximum-likelihood techniques akin to those implemented by Max Planck Institute for Radio Astronomy projects, while foreground separation adapts methods from Commander and independent component analysis approaches used by CMB-S4 preparatory studies. Statistical analyses of power spectra, null tests, and systematic error budgets reference methodologies from BICEP/Keck, POLARBEAR, and SPT collaborations. Cross-calibration uses celestial calibrators observed by Planck and radio source catalogs maintained by VLBA.
QUIJOTE has produced polarized maps of Galactic synchrotron and anomalous microwave emission, improving constraints on foreground spectral indices relevant for primordial B-mode searches conducted by experiments like BICEP2 and Keck Array. Results have implications for models developed by researchers at University of Cambridge and Stanford University on magnetic field structure and interstellar medium physics. QUIJOTE measurements have been used in joint analyses with data from Planck, WMAP, and WMAP-era legacy products to refine component models and to inform forecasts for future missions such as LiteBIRD and ground arrays planned by the Simons Observatory and CMB-S4 collaborations. Publications have appeared in journals frequented by collaborators from European Southern Observatory-associated institutes and university departments at University of Madrid and University of Cantabria.
The QUIJOTE collaboration is multidisciplinary, bringing together astronomers, engineers, and data scientists from Spanish institutions and international partners, with project governance modeled after consortia like Planck Collaboration and LSST Corporation. Funding sources include national science agencies comparable to Ministerio de Ciencia e Innovación and European funding mechanisms akin to European Research Council grants; technical contributions and in-kind support involve industrial contractors and observatory infrastructure managed by Instituto de Astrofísica de Canarias.
Planned upgrades aim to extend frequency coverage, sensitivity, and angular resolution to support deeper foreground characterization and tighter constraints on tensor-to-scalar ratio parameters pursued by teams at Princeton and Caltech. Prospective developments consider integration with multi-wavelength campaigns involving ALMA, SKA pathfinders, and coordination with satellite missions like LiteBIRD and analyses within the Simons Observatory framework. Technology upgrades draw on advances demonstrated by SPT-3G, ACTPol, and instrumentation roadmaps from JPL and European instrument consortia.