Start year
1986
Organizational Unit
Organizing institutions
Grants related:
General
Description
The general goal of this project is to determine and characterize the spatial and spectral variations in the temperature and polarisation of the Cosmic Microwave Background in angular scales from several arcminutes to several degrees. The primordial matter density fluctuations which originated the structure in the matter distribution of the present Universe, left imprinted inhomogeneities in the CMB temperature distribution, that are mathematically encoded in the so-called angular power spectrum. Initially, pioneering experiments like the COBE satellite (whose results deserved the Nobel Prize on Physics 2006) or the Tenerife CMB experiment demonstrated in the 90s that the level of anisotropy was about one part in a hundred thousands at angular scales of several degrees. Obtaining CMB maps at various frequencies with sufficient sensitivity to detect structures at this level is of fundamental importance to extract information on the power spectrum of primordial density fluctuations, to prove the existence of an inflationary period in the Early Universe and to establish the ultimate nature of the dark matter and dark energy. Recently, the WMAP satellite obtained CMB maps with unprecedented sensitivity that allowed to set restrictions on a large number of cosmological parameters.
The focus of this project is to undertake measurements at gradually higher angular resolutions and sensitivities, by using different experiments that have been operative from the Teide Observatory, like the Tenerife experiment, the IAC-Bartol experiment or the JBO-IAC interferometer. More recently, the Very Small Array interferometer performed observations between 1999 and 2008. At that time the COSMOSOMAS experiment was also operative, its goal having been not only the characterization of the primary CMB anisotropies but also the study and characterization of the Galactic foreground contamination. In more recent years the activity in this project has focused in the scientific exploitation of data from the Planck satellite, and in the development, operation and exploitation of the QUIJOTE experiment. Now that the Planck mission has been completed and finished, the activity is focused in the scientific exploitation of QUIJOTE, in the development of new instrumentation for QUIJOTE, and in in the development of new experiments that are being deployed or that will be deployed at the Teide Observatory: GroundBRID, STRIP, KISS and TMS.
Members
Principal investigator
Prof.
Rafael
Rebolo López
Project staff
Ricardo Tanausú
Genova Santos
Carlos Manuel
Gutiérrez de La Cruz
José Alberto
Rubiño Martín
Frédéric Nicolas David
Poidevin
Collaborators
Prof.
Anthony Lasenby
Dr.
Fernando Atrio Barandela
Dr.
Enrique Martínez González
Dr.
Carlos Hernández Monteagudo
Results
- 6-7 june: XV QUIJOTE Scientific Meeting (IFCA, Santander)
- July: publication of the final results (12 articles) and data from the Planck satellite.
- 15-19 october: "CMB foregrounds for B-mode studies" conference, organised within the Radioforegrounds proyect, IV AME workshop, and XVI QUIJOTE Scientific Meeting (all these eventes were celebrated at the IAC)
- October: installation of the dome of the GroundBIRD experiment, at the Teide Observatory.
- December: aceptation of the third QUIJOTE scientific article (Poidevin et al. 2019)
Scientific activity
Related publications
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JCMT BISTRO Observations: Magnetic Field Morphology of Bubbles Associated with NGC 6334We study the HII regions associated with the NGC 6334 molecular cloud observed in the submillimeter and taken as part of the B-fields In STar-forming Region Observations Survey. In particular, we investigate the polarization patterns and magnetic field morphologies associated with these HII regions. Through polarization pattern and pressureLi, Di et al.
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22023 -
QUIJOTE scientific results - VII. Galactic AME sources in the QUIJOTE-MFI northern hemisphere wide surveyThe QUIJOTE-MFI Northern Hemisphere Wide Survey has provided maps of the sky above declinations -30° at 11, 13, 17, and 19 GHz. These data are combined with ancillary data to produce Spectral Energy Distributions in intensity in the frequency range 0.4-3 000 GHz on a sample of 52 candidate compact sources harbouring anomalous microwave emissionPoidevin, F. et al.
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32023 -
QUIJOTE scientific results - IX. Radio sources in the QUIJOTE-MFI wide survey mapsWe present the catalogue of Q-U-I JOint TEnerife (QUIJOTE) Wide Survey radio sources extracted from the maps of the Multi-Frequency Instrument compiled between 2012 and 2018. The catalogue contains 786 sources observed in intensity and polarization, and is divided into two separate sub-catalogues: one containing 47 bright sources previously studiedHerranz, D. et al.
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32023 -
QUIJOTE scientific results - VIII. Diffuse polarized foregrounds from component separation with QUIJOTE-MFIWe derive linearly polarized astrophysical component maps in the Northern Sky from the QUIJOTE-MFI data at 11 and 13 GHz in combination with the Wilkinson Microwave Anisotropy Probe K and Ka bands (23 and 33 GHz) and all Planck polarized channels (30-353 GHz), using the parametric component separation method B-SeCRET. The addition of QUIJOTE-MFIde la Hoz, E. et al.
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32023 -
QUIJOTE scientific results - V. The microwave intensity and polarization spectra of the Galactic regions W49, W51 and IC443We present new intensity and polarization maps obtained with the QUIJOTE experiment towards the Galactic regions W49, W51 and IC443, covering the frequency range from 10 to 20 GHz at $\sim 1\, \text{deg}$ angular resolution, with a sensitivity in the range 35-79 $\mu \text{K}\, \text{beam}^{-1}$ for total intensity and 13-23 $\mu \text{K}\, \textTramonte, D. et al.
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32023 -
QUIJOTE scientific results - VI. The Haze as seen by QUIJOTEThe Haze is an excess of microwave intensity emission surrounding the Galactic Centre. It is spatially correlated with the γ-ray Fermi bubbles, and with the S-PASS radio polarization plumes, suggesting a possible common provenance. The models proposed to explain the origin of the Haze, including energetic events at the Galactic Centre and darkGuidi, F. et al.
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32023 -
QUIJOTE scientific results - IV. A northern sky survey in intensity and polarization at 10-20 GHz with the multifrequency instrumentWe present QUIJOTE intensity and polarization maps in four frequency bands centred around 11, 13, 17, and 19 GHz, and covering approximately 29 000 deg 2, including most of the northern sky region. These maps result from 9000 h of observations taken between May 2013 and June 2018 with the first QUIJOTE multifrequency instrument (MFI), and haveRubiño-Martín, J. A. et al.
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32023 -
Constraining the baryonic feedback with cosmic shear using the DES Year-3 small-scale measurementsWe use the small scales of the Dark Energy Survey (DES) Year-3 cosmic shear measurements, which are excluded from the DES Year-3 cosmological analysis, to constrain the baryonic feedback. To model the baryonic feedback, we adopt a baryonic correction model and use the numerical package BACCOEMU to accelerate the evaluation of the baryonic nonChen, A. et al.
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22023 -
Constraints on primordial magnetic fields from their impact on the ionization history with Planck 2018We update and extend our previous cosmic microwave background anisotropy constraints on primordial magnetic fields through their dissipation by ambipolar diffusion and magnetohydrodynamic decaying turbulence effects on the post-recombination ionization history. We derive the constraints using the latest Planck 2018 data release which improves onPaoletti, D. et al.
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122022 -
The BINGO Project. III. Optical design and optimization of the focal planeContext. The Baryon Acoustic Oscillations from Integrated Neutral Gas Observations (BINGO) telescope was designed to measure the fluctuations of the 21 cm radiation arising from the hyperfine transition of neutral hydrogen. It is also aimed at measuring the baryon acoustic oscillations (BAO) from such fluctuations, thereby serving as a pathfinderAbdalla, Filipe B. et al.
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82022 -
The BINGO project. IV. Simulations for mission performance assessment and preliminary component separation stepsAims: The large-scale distribution of neutral hydrogen (H I) in the Universe is luminous through its 21 cm emission. The goal of the Baryon Acoustic Oscillations from Integrated Neutral Gas Observations (BINGO) radio telescope is to detect baryon acoustic oscillations at radio frequencies through 21 cm intensity mapping (IM). The telescope willLiccardo, Vincenzo et al.
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82022 -
The BINGO project. II. Instrument descriptionContext. The measurement of diffuse 21-cm radiation from the hyperfine transition of neutral hydrogen (H I signal) in different redshifts is an important tool for modern cosmology. However, detecting this faint signal with non-cryogenic receivers in single-dish telescopes is a challenging task. The BINGO (Baryon Acoustic Oscillations fromWuensche, Carlos A. et al.
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82022 -
The BINGO project. V. Further steps in component separation and bispectrum analysisContext. Observing the neutral hydrogen distribution across the Universe via redshifted 21 cm line intensity mapping constitutes a powerful probe for cosmology. However, the redshifted 21 cm signal is obscured by the foreground emission from our Galaxy and other extragalactic foregrounds. This paper addresses the capabilities of the BINGO survey toFornazier, Karin S. F. et al.
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82022 -
The BINGO project. I. Baryon acoustic oscillations from integrated neutral gas observationsContext. Observations of the redshifted 21-cm line of neutral hydrogen (H I) are a new and powerful window of observation that offers us the possibility to map the spatial distribution of cosmic H I and learn about cosmology. Baryon Acoustic Oscillations from Integrated Neutral Gas Observations (BINGO) is a new unique radio telescope designed to beAbdalla, Elcio et al.
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82022 -
Fundamental physics with ESPRESSO: Constraints on Bekenstein and dark energy models from astrophysical and local probes<SUP>*</SUP>Dynamical scalar fields in an effective four-dimensional field theory are naturally expected to couple to the rest of the theory's degrees of freedom, unless some new symmetry is postulated to suppress these couplings. In particular, a coupling to the electromagnetic sector will lead to spacetime variations of the fine-structure constant, αMartins, C. J. A. P. et al.
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62022 -
Searching for dark-matter waves with PPTA and QUIJOTE pulsar polarimetryThe polarization of photons emitted by astrophysical sources might be altered as they travel through a dark matter medium composed of ultra light axion-like particles (ALPs). In particular, the coherent oscillations of the ALP background in the galactic halo induce a periodic change on the polarization of the electromagnetic radiation emitted byCastillo, Andrés et al.
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62022 -
The C-Band All-Sky Survey (C-BASS): template fitting of diffuse galactic microwave emission in the northern skyThe C-Band All-Sky Survey (C-BASS) has observed the Galaxy at 4.76 GHz with an angular resolution of 0${_{.}^{\circ}}$73 full-width half-maximum, and detected Galactic synchrotron emission with high signal-to-noise ratio over the entire northern sky (δ > -15 ○). We present the results of a spatial correlation analysis of Galactic foregrounds at midHarper, S. E. et al.
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72022 -
Polarization angle requirements for CMB B-mode experiments. Application to the LiteBIRD satelliteA methodology to provide the polarization angle requirements for different sets of detectors, at a given frequency of a CMB polarization experiment, is presented. The uncertainties in the polarization angle of each detector set are related to a given bias on the tensor-to-scalar ratio r parameter. The approach is grounded in using a linearVielva, P. et al.
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42022 -
Velocity dispersion and dynamical masses for 388 galaxy clusters and groups. Calibrating the M<SUB>SZ</SUB> − M<SUB>dyn</SUB> scaling relation for the PSZ2 sampleThe second catalogue of Planck Sunyaev-Zeldovich (SZ) sources, hereafter PSZ2, represents the largest galaxy cluster sample selected by means of their SZ signature in a full-sky survey. Using telescopes at the Canary Island observatories, we conducted the long-term observational program 128- MULTIPLE-16/15B (hereafter LP15), a large and completeAguado-Barahona, A. et al.
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32022 -
Fundamental physics with ESPRESSO: Precise limit on variations in the fine-structure constant towards the bright quasar HE 0515−4414The strong intervening absorption system at redshift 1.15 towards the very bright quasar HE 0515−4414 is the most studied absorber for measuring possible cosmological variations in the fine-structure constant, α. We observed HE 0515−4414 for 16.1 h with the Very Large Telescope and present here the first constraint on relative variations in α withMurphy, Michael T. et al.
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22022
Related talks
No related talks were found.Related conferences
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XIX Canary Islands Winter School of Astrophysics "The Cosmic Microwave | Background: from quantum fluctuations to the present Universe"Tenerife, Canary IslandsSpainDate-Past
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