José Alberto Rubiño-Martín

The QUIJOTE CMB Experiment

(The millimeter and submillimeter sky in the Planck mission era,

Paris, 10-14 January 2011)

Outline

• Introduction

• The QUIJOTE CMB Experiment (10-40GHz).

• QUIJOTE Phase I.

– Multi-Frequency Instrument (10-30GHz)

– Second Instrument (30GHz)

• QUIJOTE Phase II.– Third Instrument (42GHz)

• EPI Consolider Project: Exploring the physics of inflation

• Schedule for 2011-2012

Primordial gravitational waves and B-modes

TT

Gravitational waves are the “smoking gun” of inflation. A detection of primordial

B-modes gives inmediately information about the energy scale of inflation

r=0.1 corresponds to an energy scale of inflation around 2x1016 GeV.

(from http://cosmology.berkeley.edu/~yuki/CMBpol/CMBpol.htm)

CMB polarization: foregrounds

Left) Without any Galactic removal, only the CMB E-mode can dominate at 100GHz and for l 2000.

Right) With a Galactic subtraction of a factor 10 the CMB B-mode (r=0.1) can dominate at 100GHz and for l 100. The major limitation comes in this case from extragalactic sources (S<1Jy) and lensing.

(Tucci et al. 2004)

E B

CMB polarization: observational status• Several E-mode

detections: DASI, CBI,

CAPMAP, Boomerang,

WMAP, QUAD, BICEP,

QUIET, etc.

• WMAP7 gives r<0.93 at

95% using TE/EE/BB, and

r<2.1 at 95% with BB

alone.

•WMAP7+BAO+SN

gives r<0.2 (Komatsu et

al. 2010).

• BICEP: r<0.72 at 95%

with BB only (Chiang et

al. 2010).

• QUIET: r=0.35+1.06-0.87

with BB only (Bischoff et

al. 2010)Chiang et al. 2010

QUIJOTE CMB experiment

(Q-U-I JOint TEnerife Cosmic Microwave Background Experiment)

The QUIJOTE CMB consortium

Instituto de Astrofísica de Canarias

R. Rebolo (PI), J.A. Rubiño-Martín (PS), R. Génova-Santos, R. Hoyland (InstS),

J.M. Herreros (PM), F. Gómez-Reñasco, M. Aguiar, C. López-Caraballo.

Instituto de Física de Cantabria

E. Martínez-González, P. Vielva, D. Herranz, F.J. Casas, B. Barreiro, R.

Fernández-Cobos, M. López-Caniego

Departamento Ingeniería de Comunicaciones

E. Artal, B. Aja, J.L. Cano, L. de la Fuente, A. Mediavilla, J.P. Pascual, E. Villa

IDOM

G. Murga, C. Gómez, A.Gómez, J. Ariño, R. Sanquirce, J.Pan, A. Vizcargüenaga

Jodrell Bank Observatory

L. Piccirillo, B. Maffei, G. Pisano, R.A. Watson, R. Davis, R. Davies, C. Dickinson

University of Cambridge

M. Hobson, M. Brown, A. Challinor, K. Grainge, A. Lasenby, R. Saunders, P. Scott

( http://www.iac.es/project/cmb/quijote )

• Main science driver: to constrain (or to detect)

gravitational B-modes if they have an amplitude

of r=0.05.

• Complement Planck at low frequencies. In

combination with Planck data, push the upper

limits below that value.

• Measure polarized foregrounds (synchrotron)

with high sensitivity to correct them in future

space missions aiming to reach r=0.001.

The QUIJOTE-CMB Experiment: Goals

QUIJOTE: Project baseline Site: Teide Observatory

Frequencies: 11, 13, 17, 19, 30 and 42 GHz.

Angular resolution: ~1 degree

Telescopes and instruments: two phases (funded!)

Phase I. First telescope, a Multi-Frequency Instrument providing 11-30 GHz, and Second Instrument with 15 polarimeters @ 30 GHz and a polarised source subtractor facility at 30GHz.

Phase II. Second telescope and third instrument at 42 GHz (~50 polarimeters).

Technology: Coherent detectors.

Polarization detection: modulation.

Observing strategy: Deep observations in selected areas using raster scans, plus large scale map using “nominal mode” (=each antenna mounted on a fast spinning system (0.25-0.1 Hz), and earth rotation provides daily sky coverage of several thousand sq degrees).

Time baseline: Main science goal (r=0.1) by 2013, and r=0.05 by 2015-2016. Possible extension of the observations for additional 4 years.

QUIJOTE CMB Experiment

PHASE I.

• Enclosure and First QUIJOTE telescope

• Multi-Frequency:10-30GHz

• 30GHz instrument

• Source subtractor facility @30GHz

PHASE II.

• Second QUIJOTE telescope

• Third instrument (42GHz).

QUIJOTE CMB Experiment

PHASE I.

• Enclosure and First QUIJOTE telescope

• Multi-Frequency:10-30GHz

• 30GHz instrument

• Source subtractor facility @30GHz

PHASE II.

• Second QUIJOTE telescope

• Third instrument (42GHz).

QUIJOTE.

Platform and

enclosure

QUIJOTE First Telescope

• Alto-azimutal mount

• Maximum rotation speed around AZ axis: 0.25 Hz

• Maximum zenith angle: 60º

• Cross-Dragonian design:

• Aperture: 3 m (primary) and 2.6 m

(secondary)

• Maximum frequency: 90 GHz

(rms≤20μm and max deviation =100

μm)

A dedicated instrument at 30 GHz to measure radiosources (an

upgraded version of the VSA subtractor converted to a polarimeter).

We estimate around 300 sources with I>300 mJy (at 30GHz).

A Source-Subtractor facility at 30GHz

VSA

source subtractor

Tenerife.

3.7 m dishes

Multi-Frequency Instrument 30GHz

Instr.

• Temperature sensitivity per beam, given by

• Our definition of Q is given by Q = Tx – Ty.

Nt

T

chan

sysUQ

int

2

QUIJOTE CMB Experiment - Phase I. Basic facts

QUIJOTE-Phase I. First instrument

11-13GHz

16-18GHz

30GHz

QUIJOTE-Phase I. First instrument

• 2 horns providing 8 channels at 11 and 13 GHz

• 2 horns providing 8 channels at 17 and 19 GHz

• 1 horn providing 2 channels at 30 GHz

• Commissioning phase: June 2011.

Horns

LNA

OMT and motor

Spinning polar modulators

Polar Modulators

OMT10-14 GHz

26-34 GHz

16-20 GHz

QUIJOTE first instrument: Multi-Frequency Instrument

QUIJOTE MFI: FEMs and BEMs

Band / polarimeter Avg, Noise temp,

K

10-14GHz / 1 7K

10-14GHz / 1 10K

10-14GHz / 2 9K

10-14GHz / 2 10K

16-20GHz / 1 10K

16-20GHz / 1 12K

16-20GHz / 2 17K

16-20GHz / 2 21K

25-35GHz 18K

* FEMs: in AIV phase.

* BEMs: in AIV phase.

QUIJOTE 1st Instrument & CMB polarized foregrounds

After one year of operation, QUIJOTE will produce five frequency maps

(11, 13, 17, 19 and 30 GHz) in Stokes Q, U and I, each one with a sensitivity

around 2-3μK per one degree beam, and covering a sky area between 5000 to

10000 square degrees.

These maps will provide valuable information about the polarization

properties of:

Synchrotron emission: it should dominate the emission at our frequencies

Anomalous microwave emission (spinning dust? little known about its

polarization).

Radio-sources: low contribution at degree scales, but relevant for B-

modes science

Maps used to clean the 30 GHz maps of the 2nd QUIJOTE instrument.

Excellent complement to Planck at low frequencies.

Synchrotron model: based on WMAP K-band map and observed polarization

degree and angles. Intensity is extrapolated using the model described in de

Oliveira-Costa et al. (2008).

Radio-sources model: Extrapolation based on NVSS and GB6 catalogues, plus

source counts at 15GHz from 9C survey using the method described in Tucci et al.

(2004) to assign the polarization degree.

Sky area: 10,000 square degrees.

Expected polarized emission at QUIJOTE frequencies

EE

EE

B, r=0.1

P16. Anomalous microwave emission: polarization of the Perseus molecular complex

COSMOSOMAS at 11GHz (Battistelli et al. 2006); WMAP7 at 23-41GHz (López-Caraballo et al. 2010).

11GHz

23GHz

QUIJOTE Second Instrument: the 30GHz Instrument

26-36 GHz

Feedhorn

Connectors for 26-

36GHz Receivers

Displacer

Vacuum Valve

Pressure Sensor

Connector for

Temperature sensors and

heaters

Motor

mount Telescope Mounting

Interface Flange

• 15 horns providing 30 channels at 30GHz.

• First conceptual design based on a re-scaled version of the first instrument. Several improvements have been applied to the opto-mechanical design and thermal interfaces.

• Prototype for one complete horn is under construction and will be tested in few months.

• Instrument ready for AIV in March 2012.

Hermetic

Feedthroughs for

encoders signals

Second instrument:

• Instantaneous sensitivity: 0.057 mK s1/2

• Effective observation time: 3 years

• Sky coverage: 5000 deg2

• Effective integration time per

1-degree beam: 5.96 h• Final map sensitivity: 0.38

μK/beam

Predicted performanceSimple estimate

gives r=0.1 (95%

CL) with 5,000 deg2

sky coverage and 3

years effective

observing time

QUIJOTE second instrument: B-mode science

Realistic

simulations and a

full pixel-based ML

approach shows

that r=0.1 is

detected at 3σ after

1year, and at 7σ

after 3 years.

QUIJOTE CMB Experiment

PHASE I.

• Enclosure and First QUIJOTE telescope

• Multi-Frequency:10-30GHz

• 30GHz instrument

• Source subtractor facility @30GHz

PHASE II.

• Second QUIJOTE telescope

• Third instrument (42GHz).

QUIJOTE Second Telescope

• A copy of the fist telescope. Optical specifications to work up to 100GHz.

• Manufacturing time: 6 months.

• Ready for operation by March 2012.

• To be installed at the Teide Observatory together with the second QUIJOTE instrument (30GHz).

QUIJOTE Third Instrument: the 42GHz Instrument

• 2 instruments, 25 horns each. Every horn provides 2 channels at 42 GHz.

• Time schedule: first instrument for AIV in 2013.

Consolider-Ingenio Program 2010:

“Exploring the physics of inflation

(EPI)”

Five-year grant (2011-2016).

PI: Enrique Martínez-González.

Nodes: IFCA, IAC, DICOM, UGR, UPV, Univ. of Manchester,

Univ. of Cambridge, Chalmers.

Technical contributions: Second QUIJOTE telescope.

QUIJOTE 42GHz experiment.

Development of technology to build 42GHz FEMs.

Pathfinder for a large-format interferometer. Digital correlator (FPGAs)

vs Analog correlator (Rotman lenses).

QUIJOTE: schedule for 2011-2013

First QUIJOTE instrument @11,13,17,19,30GHz (2011-2013).

o Assembly, integration and verification phase of the first QUIJOTE

instrument. March 2011.

o Installation of the telescope and first instrument at the Teide

Observatory. April-May 2011.

o Commissioning phase. June-July 2011.

Second QUIJOTE instrument @30GHz (2012-2014).

o AIV phase in March 2012.

Second QUIJOTE telescope.

o Installation at the Observatory together with 2nd instrument in March-

April 2012.

Third QUIJOTE instrument @42GHz (2013-)

o AIV phase within 2013.

Dalí 1945

We are close to begin to ride...

Thank you!