quijote sur science case

7/25/2019 QUIJOTE Sur Science Case

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A joint European /South African CMB Polarizationexperiment combining imaging and interferometry in

the frequency range 10-40 GHz

S. Colafrancesco1, R. Rebolo

2, L. Piccirillo

3, J.A. Rubio Martin

2,R.T. Genova Santos

2, E.

Martinez-Gonzalez4, P. Alexander

5

1University of the Witwatersrand, Johannesburg (South Africa)

2IAC, Tenerife (Spain)

3University of Manchester, Manchester (UK)

4Inst de Fsica de Cantabria, Santander (Spain)

5Mullard Radio Astronomy Observatory, Cavendish Laboratory, Cambridge (UK)

Executive Summary

The measurement of the CMB polarization with high sensitivity may lead to the detection of B-

modes in the polarization of the Big Bang radiation and to set constraints on the generation of

primordial gravitational waves and on the energy of Inflation.

We propose here to develop a set of experiments in South Africa that will explore the polarization

of the CMB and of the relevant foregrounds in the frequency range 10 to 40 GHz via mapping of

the full sky at 6 different frequencies. These will be done in combination with observations from

the Canary Islands in order to cover both hemispheres, and to provide the first all-sky survey of

radio-microwave polarization in the still not fully explored frequency range 10-40 GHz.

The Northern Hemisphere observations for this programme have already started with the

QUIJOTE experiment: two telescopes located at the Teide Observatory (Tenerife, Canary

Islands) with a set of imaging instruments providing observations at 11, 13, 17, 19, 30 and 40

GHz with a spatial resolution better than 54 arcmin. This program is undertaken by a Consortium

of European Universities and Research Centres which include Instituto de Astrofisica de Canarias

(PI-institution, Spain), Instituto de Fisica de Cantabria (Spain) and the Universities of Cantabria

(Spain), Manchester (UK) and Cambridge (UK).

We propose to extend the present collaboration including the University of the Witwatersrand

(Johannesburg, South Africa), leading to a much more extended and powerful full sky CMB

polarization experiment. The extension of the project will bring the great advantages of i) full sky

coverage and ii) the increase in sensitivity by duplicating the number of detection elements.

The extension of the project to South Africa would consist of three phases:

Phase I: Replicating one QUIJOTE telescope at a South African Observatory (located in

Klerefontein, Karoo region) to conduct full sky mapping in the frequency range 10-20 GHz. In

this phase we will take advantage, and hence minimize the relative costs, of the already existing

infrastructures at the Klerefontein station in the Karoo where the C-BASS experiment is already

installed and operating. The combined Tenerife /South African experiments will provide the

most sensitive mapping of the Polarization of the Galactic Synchrotron emission in this frequency

range. Tracing the polarization of the synchrotron emission with high sensitivity is key to correct


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1. Introduction

Cosmology has experienced a striking advance in the last years as a consequence of the

development of new experiments to observe the Cosmic Microwave Background (CMB), the

large scale distribution of galaxies, distant supernovae, etc.The high-quality data produced have provided us with a consistent picture of our universe, the so-

called concordance model. The data also indicate that the primordial seeds of small-scale

inhomogeneities (including our own galaxy) are predominantly adiabatic and close to Gaussian

distributed with a nearly scale-invariant power spectrum. It is now generally believed that the

theoretical framework within which we can accommodate all these observational results is

inflation, a period of accelerated expansion in the early instants after the Big-Bang. Inflation not

only drives the universe towards the present large-scale homogeneity and flatness but also

predicts the generation of the primordial seeds from quantum fluctuations. However, we lack a

unique scenario of inflation and, what is even worse, we do not understand the physics at such

high energies. New physics beyond the standard model of particle physics are needed to

understand the physical processes that gave rise to the inflationary period in the early universe.

During the last two decades the study of the anisotropies in the Cosmic Microwave Background

(CMB) radiation has played a crucial role in our understanding of the form and composition of

the universe. This radiation is a relic of the Big Bang which propagates freely after the decoupling

of matter and radiation when the universe was some 380,000 years old. It is the farthest and oldest

light that can be observed in the universe, reflecting the dense and hot period of its early history

and representing therefore a unique proof of the Big Bang model of the universe. Since its first

detection in 1965 [Pen65], a large effort was dedicated to find the small fluctuations expected in

its temperature in different directions in the sky. These anisotropies would represent the

unambiguous sign of the presence of density fluctuations at early times which gave rise to the

formation of galaxies and to the large scale structure of the universe via gravitational instability.

The anisotropies were finally detected in 1992 with the NASA COBE satellite [Smo92] and,

together with the confirmation of the black-body radiation spectrum [Mat90] and the detection ofthe CMB radiation itself, it has made possible to award the Nobel Prize already twice within the

CMB field.

The anisotropies of the CMB carry a wealth of information about the properties of our universe

and of its constituents. However, the anisotropies detected by COBE correspond to large angular

scales (low multipoles) above 10 degrees, and are produced by the gravitational redshift suffered

by the microwave photons falling to the gravitational wells formed by the matter

inhomogeneities. The theory also predicts the existence of acoustic oscillations in the power

spectrum of the anisotropies at angular scales of about 1 degree and below, produced by the

acoustic waves formed in the primordial plasma of baryons and photons.

Later ground-based and balloon-borne experiments like BOOMERANG, MAXIMA, CBI,

Archeops and VSA, and specially the NASA WMAP satellite were able to not only detect those

oscillations but also to measure the power spectrum down to about 10-arcmin scales, implying an

accuracy in the cosmological parameters of a few percent [see e.g. Hin12, Reb04].

Planck, launched in May 14th 2009, has improved the accuracy on the determination of the

cosmological parameters at a level of precision of ! 1% [Pla05]. Planck has two instruments

onboard, the Low Frequency and High Frequency Instruments (LFI and HFI) covering together a

frequency range 30-900 GHz, and shall provide in 2014 the best measurements of intensity and

polarization anisotropy of the CMB in the whole sky with unprecedented sensitivity, resolution

and frequency coverage. The scientific exploitation of the data is a unique opportunity to extend


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the frontiers of our knowledge of the Universe. This satellite is aimed to study many

cosmological and astrophysical topics [Pla05].

The standard cosmological model also predicts that the CMB radiation is linearly polarized. The

polarization signal and its cross-correlation with the temperature anisotropies constitute an

important consistency check and help in breaking the degeneracies among some cosmological

parameters. A net value of the Stokes parameters Q and U is expected from Thomson scatteringduring decoupling of photons and baryons. Since Q and U are not invariant quantities on the

sphere it is convenient to transform them in a gradient field called E-mode and a rotational field

called B-mode. The most important property of the E and B-mode decomposition is that from

their measurement we can distinguish between primordial scalar perturbations (density) and

primordial tensor perturbations (gravitational waves).

More specifically, both types of perturbations can generate E-mode polarization, however only

gravitational waves can produce B-mode polarization. It is this property that makes polarization a

key tool for the detection of the primordial gravitational wave background (GWB) which is

expected to be generated during the inflationary period of the universe. Moreover, a detection of

the B-mode would directly provide the energy scale of inflation (as measured by the ratio r of

tensor to scalar perturbations, see Fig.0).


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Figure 0. Top: The cosmic mean density as a function of the Universe relative size. Detecting inflationary

gravitational waves with the CMB polarization would directly measure the shape of the cosmic density curvein the upper left corner of the plot, while experiments trying to characterise the dark energy would measure

the same curve in the lower right corner [Boc06]. Bottom: The GW energy density as a function of thefrequency. Theoretical predictions and observational constraints on primordial GW from inflation are shownin this plot. It is also shown the maximum expected signal for the case of r=0.01 and r=0.001. The blue

shaded region represents the range predicted for simple inflation models with the minimal number ofparameters and tunings [Boc06].


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2. Cosmic inflation and the early universe

Inflation is a period of accelerated expansion in the very early universe, leading to a substantial

flattening and smoothing of the universe, which explains why it appears to us so regular at very

large scales. Inflation, in addition to smoothing and wiping out previous inhomogeneities through

expansion, also stretches short distance quantum fluctuations to large scales. Thus, the seeds of

structure formation come mainly from short distance quantum fluctuations created at thebeginning of inflation. The simplest models of inflation generate adiabatic density perturbations

that are very nearly Gaussian and with a nearly scale-invariant spectrum [Dod03].

From Friedmann equations accelerated expansion follows if the pressure is negative enough

(verifiesp< -r / 3 in natural units with rbeing the energy density). But, then how can the cosmic

fluid parametrized in terms of p and r display such peculiar equation of state? If one considers a

scalar field model it can be shown that when its energy density is dominated by its potential

energy contribution it has an equation of state close to p= -r. These ideas indicate that if we have

one such field, usually called the inflaton, in a potential energy dominated regime, the universe

will follow an accelerated expansion.

The possibility explained above is just but one of the inflationary settings in the literature so far,

the single-field models (which are the simplest ones). There are many other scenarios for

inflation, which involve more fields or more complicated concepts. Among all the proposals of

inflationary models a huge amount of them remain compatible with the observational data

currently available.

Since inflation is thought to be a key ingredient in the generation of the seeds of inhomogeneities

in our present universe (primordial density fluctuations and gravitational waves), the

characteristics of the temperature and polarization anisotropies of the CMB are determined

(among other parameters) by the characteristics of the primordial spectra of fluctuations resulting

from inflation (scalar and tensor). The main parameters that characterize the primordial spectra

are the amplitude and the tilt, ns, (also known as spectral index) for the scalar primordial

spectrum, and the tensor-to-scalar ratio of amplitudes, r, for the tensor primordial spectrum. The

measurement of these parameters to be performed in this project will provide relevant insights

and constraints in the physics of inflation.In addition, the inflationary period can lead to other effects, such as the generation of primordial

magnetic fields. The investigation of the mechanisms of generation and the observational

implications of these primordial magnetic fields could also provide insights into the physics of

inflation [Bat09].

Understanding the physics of inflation is one of the main goals in Cosmology, and the

measurements of the B-mode polarization signal of the CMB is currently probably the most

promising method to attain considerable progress in the study of the physics of inflation. This has

been also pointed out by the ESA-ESO Working Group on Fundamental Cosmology [Pea06],

together with a strong recommendation to support these measurements and the required

technological developments.

As stated above, there is at present a wide set of inflationary models and for each model a wideset of inflaton potentials that satisfy the present observational constraints. Therefore, it is neither

clear which is the most compelling inflationary model nor the fittest inflaton potential for each

model. However, the new data are starting to constrain more restrictively the inflationary models

and the inflaton potentials. For example, recent upper bounds on the tensor to scalar ratio rby

WMAP/Planck combined with their bounds to the spectral index nshave led to the exclusion of

chaotic single-field inflation with a monomial f4 potential that gives 60 e-folds of inflation. In

other words, this inflationary model with this inflaton potential is excluded because it will lead to


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larger amplitudes in the B-mode spectrum than those observed (see Fig. 1). In this respect it is

worth mentioning that Dirac-Born-Infeld single-field inflation models can be better suited to the

observational constraints on r and ns than their conventional counterparts [Spa07], and so

potentials which would be in principle ruled out might actually be admissible. This possibility is

associated with the presence of an additional degree of freedom (linked to the proper velocity of

the DBI scenario brane in the multidimensional spacetime it lives in). In particular, an

ultrarelativistic regime would lead to a really low value of r, so if sucha result were obtained, onewould have a theoretical framework to try and provide an explanation.

Another significant feature of this inflationary setup is the generic presence of non-gaussianity,

commonly expressed in terms of the non-linear coupling parameter, fNL,which is another of the

observational goals of this project. A large departure from gaussianity can also be interpreted as

observational support for inflation models inspired by extradimensions, like the mentioned DBI

framework. Yet, a convincing signal of non-gaussianity in the perturbation spectrum can be also

nicely accommodated in the warm inflation scenario [Ber05], which is characterized by allowing

couplings of the inflaton to other fields in the theory, which result in a dissipative dynamics.

Thus, summarizing constraints in r and nslead to constraints in the inflationary models and their

inflaton potentials, and therefore contribute to defining the physical characteristics and dynamics

of the inflationary period. Even though inflation was originally associated with the grandunification of the strong and electroweak interactions it is now clear that its energy scale, or

epoch, is quite uncertain and can be above or below that of the grand unification. However, it is

worth mentioning that from the value of ns obtained by WMAP and qualitative arguments on the

shape of the inflaton potential in the simplest models of inflation, a value r > 0.01 has been

suggested [Boy06] which is within the reach of the present project. In any case, this project will

contribute largely to progress in the current understanding of the physics of inflation by

increasing the sensitivity in the determination of the tensor to scalar ratio r and deriving

consequences for inflationary models and inflaton potentials.

Figure 1. Contours show the 68% and 95% CL derived from Planck and other cosmological datasetscompared with the theoretical predictions for different inflation models. (This figure corresponds to the upperpanel of Fig. 1 in [Pla13])


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In addition, there is another topic on which this project can make a considerable impact:

primordial magnetic fields. If such fields were generated before photon decoupling they could

have left imprints in the CMB, as they could be responsible for non-Gaussianity, Planck spectrum

distortions, anisotropy spectrum modifications, generation of waves, Faraday Rotation and others.

Even though no clear signs of magnetic fields in CMB experiments have been found so far, the

situation may get reversed with new experiments QUIJOTE and Planck, due to their improvedsensitivity, frequency coverage and angular resolution, as well as with the improved capacity to

measure polarization.

This topic fits perfectly in the framework of this project, both from the experimental and

theoretical dimensions as the most attractive magnetogenesis mechanism is provided by inflation.

It can give fields at any scale in the same way that super-horizon energy density structures are

created and observed in the CMB (including the Sachs-Wolfe region of the power spectrum) and

in the large scale structure. This scenario was early assumed by [Tur88] and was developed by

several authors thereafter (i.e. [Gio07]; see [Bat00] and [Bat09] for a review of the different

mechanisms). But the mechanism lacks an as complete as desirable understanding and its

investigation is a goal of this project.

As for the observational hints, for a frequency of 30 GHz magnetic fields would provide a

rotation angle of between 1 and 20 degrees, which is measurable by QUIJOTE and Planck.

However the main difficulty is the weakness of the signal as compared to the noise, and the

expected contamination with the galactic contribution, which will require further developments in

the modelling.

3. Roadmap for CMB polarization research.

The goal of the field is to measure the CMB polarization with increasing precision and accuracy

in order to constrain the physics of the earliest moments of the Universe.

The executives of ESO (European Southern Observatory) and ESA and representatives of their

science advisory structures decided to establish a number of working groups that were tasked to

explore the possible synergies in areas of mutual interest and to make recommendations to both

organizations. One of those Working Groups was focused on Fundamental Cosmology, and their

report is publicly available [Pea06]. The Physics of inflation was identified by this group as one

of the five key questions in fundamental cosmology, for which CMB observations, especially in

polarization, provide a unique probe. These recommendations are also discussed in [Boc06]

(Task Force on CMB Research, a USA report prepared as a demand of NASA, National Science

Foundation, NSF, and the Department of Energy, DoE). In both reports, the main

recommendation under the heading of (large scale) CMB research is a future space mission (2020

or later) aimed to detect B-modesat levels between r=0.001 and r=0.01. In the mean time, they

have two basic recommendations:

1) As the highest priority, they recommend a phased program to measure the large-scale

polarization of the CMB expected from inflation. This program should start with ground-

based experiments which should be able to reach limits around r=0.01 in the next 7 years.

2) Foreground signals, and in particular emission from our Galaxy, will be the major

limiting factor of the possible constraints on the existence of B-modes. Thus, they

recommend a systematic program to study polarized astrophysical foregrounds,

especially from our Galaxy. Moreover, the [Pea06] document states that, in particular, it


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is desirable to obtain improved low-frequency maps around 10 GHz, which can

constrain not only the synchrotron foreground but also the so-called anomalous

foreground, which is sometimes hypothesized to arise from spinning dust grains.

The present project provides an answer to these two recommendations, and constitutes a unique

opportunity to play a leading role in the field during the next years.

3. Present status of CMB polarization observations

As discussed in the introduction, in the last decade there has been an explosion of CMB data that

has allowed a strong progress in the characterization of the temperature fluctuations. In addition,

a number of experiments (e.g. QUIET [Qui12], WMAP [Hin12], QUAD [Bro09]) have measured

the E-mode polarization of the CMB as well as the TE cross power spectrum. These observations,

in conjunction with other cosmological data sets, are allowing to place strong constraints on the

cosmological parameters and to provide a consistent picture of the universe, the so-called

concordance model. However, a detailed understanding of the processes that took place during

the early universe is still lacking. For this reason, the study of the B-mode polarization of the

CMB is one of the most important topics of current cosmology, since its detection wouldconstitute a major breakthrough in our understanding of the early universe.

Figure 2: Current constraints on the CMB B-mode of polarization from different experiments. The dashedgray line corresponds to a theoretical LambdaCDM spectrum with r=0.1, while the dotted line depicts the

contribution from the lensed E-mode signal. This figure has been taken from [QUI12].

A large effort is being put within the CMB community in order to achieve this goal. Severalexperiments are already setting constraints on the B-mode polarization, while others are in

preparation. In particular, the BICEP [Chi10] and QUAD [Bro09] experiments have imposed the

strongest constraints up to date in the B-mode power spectrum at scales below and above ~1,

respectively (see Figure 2). Constraints on the tensor-to-scalar ratio r have been obtained by

combining the WMAP data with Large Scale Structure and Supernovae data [Hin12] and is

r


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temperature power spectrum which, at large scales, is ultimately limited by the cosmic variance,

and can also suffer from degeneracies with other cosmological parameters. Conversely, the

primordial B-mode of polarization constitutes a more direct probe of the tensor modes since it

depends primarily on r. The best constraint on r obtained directly from the B-mode polarization

has been recently provided by BICEP [Chi10] and is r


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Microwave Integrated Circuits) technology, which allows for cross-checking of results with other

experiments based on bolometers

QUIJOTE (North) consists of two telescopes and three instruments instruments, which can be

exchanged in the focal plane of the two telescopes. The first instrument (hereafter Multi-

Frequency Instrument or MFI) is a multi-channel instrument with four separate polarimeters, two

operating at 10-14 GHz, and two at 16-20 GHz. Each horn feeds a novel cryogenic on-axisrotating polar modulator that can rotate. The Quijote telescope and some compoments of the MFI

can be seen in figures 5 to 7. The science driver for MFI is the characterization of the galactic

foregrounds, using the four frequency maps at 11, 13, 17 and 19 GHz that will be produced. At

present, MFI is in operation. Some preliminary results are shown in figures 8 to 10.

The second and third QUIJOTE instruments will consist of 30 and 40 polarimeters operating at 30

GHz and 40 GHz respectively, and will be devoted to primordial B-modes science. The detailed

design of the second instrument is concluded, manufacturing is very advanced, and its

integration is expected at the end of 2013. More instrumental details can also be found in the

QUIJOTE web page. The QUIJOTE instruments will be located in the focal plane of a telescope

(see figure 5) that follows a crossed-Dragonian design with an effective aperture of 2.3 meters.

Figure 3 Enclosure of the QUIJOTE telescope (already finished) at the Teide Observatory (July 2009).

Figure 4. Left. QUIJOTE scientific goal for the angular power spectrum of the CMB E and B mode signals. Itis shown the case for 3 years operation time, and a sky coverage of ~5, 000 square degrees. The red line

corresponds to the primordial B-mode contribution in the case of r = 0.1. Right: Expected foreground

contamination in the 30 GHz QUIJOTE frequency band. It is shown the contribution of polarized synchrotronemission and radio-sources for the case of subtracting sources down to 1 Jy in total intensity (upper dashed

line for radio-sources) and 300 mJy (lower dashed-line)


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Figure 5. Left: A section of the first QUIJOTE telescope, showing the optical configuration and the first

instrument assembled in the focal plane. Right: The first QUIJOTE telescope, at the Teide Observatory

(picture taken in March 2013).

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2 horns providing 8 channe ls a t 11 and 13 GHz

2 horns providing 8 channe ls a t 17 and 19 GHz

Horns

LNA

OMT and motor

Spinning polar modu lators

Polar Modulators

OMT10-14 GHz

26-34 GHz

16-20 GHz

Figure 6. View of various components (LNAs, Horns, OMT, Polarizers) of the Multifrequency Instrument of

QUIJOTE.


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Figure 7. MFI instrument fully assembled, before its integration in the first QUIJOTE telescope

Cygnuscomplex

W51SN remnantcomplex

QUIJOTENorthern

HemisphereSurvey

(20000 sq deg)

On-going

Cass ASN remnant

Fig. 8. Northern Hemisphere Survey performed by QUIJOTE at 11 GHz (four days of observations).


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WMAP 22 GHz

QUIJOTE 11 GHz

Cass A

SN remnant

W51

SN remnant

Fig. 9. Detail of the Galactic plane emission centred at the Cygnus complex. Observations by QUIJOTE and

WMAP at 11 and 22 GHz.

Fig.10. The Perseus molecular complex as seen by QUIJOTE MFI at 11 GHz (left panel) and PLANCK at30GHz (middle panel). The derived spectral energy distribution of the Perseus molecular cloud is shown in

the right panel (QUIJOTE points in red, and PLANCK points in green).

5. A European South-African CMB Polarization experiment

The present proposal aims to extend the current QUIJOTE Experiment to a South African site in

order to carry out a full sky mapping of the CMB Polarization in the frequency range 10-40 GHz.

We propose a three-phase project with a time sequential implementation of these phases:


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1) Phase I: to replicate one of the QUIJOTE telescopes and build a new MFI (10-20 GHz)

instrument. The QUIJOTE telescope is designed to provide polarization free sensitive

observations up to 200 GHz. Deploy this new telescope and instrument in a South

African observing site with the goal to obtain a full Southern Hemisphere survey of

20000 sq. deg with a sensitivity of 10 microK per beam. In combination with the data of

QUIJOTE from the Northern site, it will provide a Q, U and I high-sensitivity full sky

coverage at four frequencies 11, 13, 17 and 19 GHz. These full sky maps will be the mostsensitive ever obtained at these frequencies and will be used to investigate the

polarization properties of the synchrotron emission and other possible foreground

emissions. The construction of the telescope and instrument will take 2 years. One year of

data will be sufficient to obtain maps at the four frequencies with a sensitivity and

resolution equivalent to that of WMAP at 22 GHz.

2) Phase II: to produce two interferometers of 100-elements each operating in the frequency

range 30-40 GHz. One will be located in the South-African site and the other in the

Canarian site. These interferometers would be deployed two years after the start of

operations of the QUIJOTE telescope in the South African site. Both interferometers are

aimed to carry out very sensitive measurements of 1 microK / beam in selected low

galactic emission regions covering a total of 5000 sq deg in each Hemisphere. This set of

two interferometers in both hemispheres can provide a detection of B-modes if r=0.01

one year after the beginning of the observations (see figure 11), Improving by at least a

factor 5 the sensitivity of the current QUIJOTE imaging facility at the North Hemisphere.

Solving the problems associated with the correlation of hundreds of baselines would give a

large improvement in sensitivity with respect to direct imaging experiments for which the

maximum number of detectors that can be accommodated is constrained by the limited area

available at the focal plane.

The proposed optics consists of a closed-packed array of corrugated feed-horns co-pointed on

a flat platform. An OMT separates the two polarization into two waveguides where cryogenic

LNAs provide the necessary amplification. A mixer follows to provide a proper shift of the

bandwidth where the passive correlator is sensitive. The correlator consists of a front-to-front

array of corrugated feed horns. The signal coming from all the horns is added in amplitude at

each horn of the final array and then squared by a square-wave detector. The square of all the

added amplitudes provide all the N(N-1)/2 correlations.

This novel method, pioneered by one of us [Ali03], is capable of optically combining a large

number of baselines.

The whole receiving set of arrays is positioned on a commercial mechanical mount that

provides alt-az motion.

An example of Ku-band (10 GHz) system with co-ax input is shown in the figure below.


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Fig. 11. Predictions on E-mode and B-mode detection for 1 year of observations with two 100-elementinterferometers (30-40 GHz) covering a total of 20000 sq deg of high Galactic latitude regions (50% of

each hemisphere). We assume the foreground correction has been performed using high sensitivity

maps of the QUIJOTE imagers (10-20 GHz) at both the South African and the Canarian site.


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3) Phase III: Beyond 2018- Construction and development of two arrays of interferometers

consisting each of 10 units of 100 elements to be located at both the South African and

Canarian sites. These powerful arrays would have sufficient sensitivity to provide a

detection of B-modes if r=0.001. (see figure 12)

Fig. 12. Predictions on E-mode and B-mode detection for 1 year of observations with two arrays ofinterferometers (one in South Africa and one in Canary Islands). Each array containing ten 100-element

interferometers (30-40 GHz). The arrays covering a total of 20000 sq deg of high Galactic latituderegions (50% of each hemisphere). We assume the foreground correction has been performed using

high sensitivity maps of the QUIJOTE imagers (10-20 GHz) at both the South African and the Canariansites.

Objectives

- The major objective is the detection or the setting of strong constraints on the amplitude of theprimordial GWB, r!0.01.

- Improving the accuracy in the determination of nsby breaking the ns-! degeneracy combining

QUIJOTE and Planck. This will strongly constrain the possible models of inflation.

- Construction of the temperature (T) and polarization (Q, U) frequency maps. The full sky maps

at 10-20GHz will constitute a unique legacy product of this project.

- Construction of catalogues of extragalactic sources.


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- Construction of T, Q, U maps for CMB and Galactic foregrounds.

- Determination of the temperature and polarization power spectra: TT, TE, EE, BB.

- Implications of the temperature and polarization data on the physics of inflation.

- Implications of the temperature and polarization data on the Primordial Magnetic Fields.

- Characterization of the Galactic Magnetic field.

- Constraints on the physical models for the anomalous component.

- Statistical properties of the extragalactic sources.

- Non-Gaussianity studies of the CMB maps (non-linear coupling parameter fNL, Cold Spot

[Vie04], Corona Borealis anomaly [Gen08], North-South asymmetries [Hof09]

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