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The QUIJOTE CMB Experiment

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The QUIJOTE CMB Experiment (The millimeter and submillimeter sky in the Planck mission era, Paris, 10-14 January 2011) The QUIJOTE CMB Experiment José Alberto Rubiño-Martín 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 (from http://cosmology.berkeley.edu/~yuki/CMBpol/CMBpol.htm) 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. CMB polarization: foregrounds E B (Tucci et al. 2004) 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. 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). +1.06 • QUIET: r=0.35 -0.87 with BB only (Bischoff et Chiang et al. 2010 al. 2010) QUIJOTE CMB experiment (Q-U-I JOint TEnerife Cosmic Microwave Background Experiment) The QUIJOTE CMB consortium ( http://www.iac.es/project/cmb/quijote ) 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 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 IDOM G. Murga, C. Gómez, A.Gómez, J. Ariño, R. Sanquirce, J.Pan, A. Vizcargüenaga The QUIJOTE-CMB Experiment: Goals • 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. 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 II. • Second QUIJOTE telescope PHASE I. • Third instrument (42GHz). • Enclosure and First QUIJOTE telescope • Multi-Frequency:10-30GHz • 30GHz instrument • Source subtractor facility @30GHz QUIJOTE CMB Experiment PHASE II. • Second QUIJOTE telescope PHASE I. • Third instrument (42GHz). • Enclosure and First QUIJOTE telescope • Multi-Frequency:10-30GHz • 30GHz instrument • Source subtractor facility @30GHz 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 Source-Subtractor facility at 30GHz 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). VSA source subtractor Tenerife. 3.7 m dishes QUIJOTE CMB Experiment - Phase I. Basic facts 30GHz Multi-Frequency Instrument Instr. • Temperature sensitivity per beam, given by QU2 Tsys tintNchan • Our definition of Q is given by Q = Tx – Ty. QUIJOTE-Phase I. First instrument 11-13GHz 16-18GHz 30GHz QUIJOTE-Phase I. First instrument QUIJOTE first instrument: Multi-Frequency Instrument Spinning polar modulators • 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. Polar Modulators 16-20 GHz LNA 26-34 GHz OMT 10-14 GHz OMT and motor Horns QUIJOTE MFI: FEMs and BEMs * FEMs: in AIV phase. 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 * 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. Expected polarized emission at QUIJOTE 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. 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 • 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. Connectors for 26- 36GHz Receivers Displacer Pressure Sensor Hermetic Feedthroughs for encoders signals 26-36 GHz Motor Connector for Vacuum Valve Feedhorn mount Telescope Mounting Temperature sensors and Interface Flange heaters QUIJOTE second instrument: B-mode science Second instrument: • Instantaneous sensitivity: 0.057 mK s1/2 • Effective integration time per • Effective observation time: 3 years 1-degree beam: 5.96 h • Sky coverage: 5000 deg2 • Final map sensitivity: 0.38 μK/beam Predicted performance Simple estimate gives r=0.1 (95% CL) with 5,000 deg2 sky coverage and 3 years effective observing time 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 II. • Second QUIJOTE telescope PHASE I. • Third instrument (42GHz). • Enclosure and First QUIJOTE telescope • Multi-Frequency:10-30GHz • 30GHz instrument • Source subtractor facility @30GHz 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. We are close to begin to ride... Thank you! Dalí 1945.
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