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!