Constraints on the polarization of the Anomalous Microwave

emission with the QUIJOTE-CMB experiment

Ricardo Génova Santosfor the QUIJOTE collaboration

rgs@iac.es

47th ESLAB Symposium: The Universe as seen by PlanckESA-ESTEC, Noordwijk, 2-5 April 2013

❖ Instituto de Astrofísica de Canarias (IAC)R. Rebolo (PI), J.A. Rubiño-Martín (PS), M. Aguiar, R. Génova-Santos, F. Gómez-Reñasco, A. Pérez (PM), R. Hoyland (InstS), C.H. López-Caraballo, A. Peláez,V. Sánchez, A. Vega, T. Viera, R. Vignaga

❖ Instituto de Física de CantabriaE. Martínez-González, B. Barreiro, F.J. Casas, J.M. Diego, R.

Fernández-Cobos, D. Herranz, M. López-Caniego, D. Ortiz, P. Vielva

❖ DICOM - Universidad de CantabriaE. Artal, B. Aja, J. Cagigas, J.L. Cano, L. de la Fuente, A. Mediavilla, J.P. Pascual,

J.V. Terán, E. Villa

❖ JBO - University of ManchesterL. Piccirillo, R. Battye, E. Blackhurst, M. Brown, R.D. Davies, R.J. Davis,

C. Dickinson, K. Grainge, S. Harper, B. Maffei, M. McCulloch, S. Melhuish, G. Pisano, R.A. Watson

❖ University of CambridgeM.P. Hobson, A. Challinor, A.N. Lasenby, N. Razhavi, R.D.E. Saunders,

P.F. Scott, D. Titterington

❖ IDOMJ. Ariño, B. Etxeita, A. Gómez, C. Gómez, G. Murga, J. Pan, R. Sanquirce, A. Vizcargüenaga

The QUIJOTE collaboration

❖ Project baseline: • Site: Teide Observatory (altitude: 2400 m, latitude: 28º), Spain• Angular resolution: 1 degree• Sky coverage: 10,000 deg2

• Telescope and instruments:- Phase I: First Telescope (QT1), equipped with the Multifrequency Instrument (MFI) with 4 polarimeters @ 10-20 GHz (undergoing commissioning). Second Instrument (TGI) with 31 polarimeters @ 30 GHz (funded, starts operations in 2013). Polarized Source Subtractor (undergoing commissioning)- Phase II: Second Telescope (QT2), and FGI with 40 polarimeters @ 40 GHz (funded)- Phase III: instrument with 100 polarimeters @ 90 GHz (not funded)

❖ Time baseline: • Main science goal (r=0.1) by 2015, and r=0.05 by 2017• Possible extension of the observations for additional 4 years

❖ Science driver• To constrain (or to detect) primordial B-modes down to r=0.05• To measure and characterize polarized foregrounds (synchrotron and anomalous emissions) with high sensitivity at 10-20 GHz, allowing correction in future space missions aiming at r~0.001

The QUIJOTE-CMB project

The QUIJOTE-CMB project

Frequency (GHz) 11 13 17 19 30 40

Bandwidth (GHz) 2 2 2 2 8 10

Number of horns 2 2 31 40

Channels per horn 2 2 2 2 4 4

Beam FWHM (deg) 0.92 0.92 0.60 0.60 0.37 0.28

Tsys (K) 25 25 25 25 35 45

NEP per channel (µK s1/2) 456 370 663 1019 557 632

Sensitivity per channel (Jy s1/2) 0.49 0.55 0.73 1.40 0.66 0.76

MFI TGI FGI

• QT1 installed at the Teide observatory in May 3rd, 2012

QT1

• 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 ≤20 µm and max deviation =100 µm)

• QT2 is a replica of QT1, and will be built during 2013

MFI

• 5 conical corrugated feedhorns• 2 horns providing channels at 11 and 13 GHz• 2 horns providing channels at 17 and 19 GHz• 1 horn providing one channel at 30 GHz (removed)• First light November 2012

Polar Modulators

OMT

10-14 GHz

16-20 GHz

Science with the MFI

• Contamination introduced by synchrotron and AME at 30 GHz:

• Maps of the MFI will allow to characterize the polarization of the synchtrotron and AME

• Shallow surveywithasensitivityof20μK/(1degbeam)over10,000deg2after4months•Deep surveywithasensitivityof7μK/(1degbeam)over3,000deg2after10months

AME in polarization

★ Probing the electric and magnetic dipole emission models:

• Electric and dipole emissions present different polarization spectra

• Magnetic dipole emission, in the case of single-domain grains (no Fe inclusions) is expected to be strongly polarized (up to ~30% for ν> 40 GHz; Draine & Lazarian 1999). However, magnetic inclusions produce lower polarizations (<10% at ν ~ 30 GHz; Draine & Hensley 2012)

• Electric dipole emission (spinning dust) is weakly polarized (under ~2% above 20 GHz; Lazarian & Draine 2000)

★ Forecasts of the level of contamination for B-mode experiments

Draine & Hensley 2012

AME polarization constraints 2

TABLE I: Summary of the current constraints on the fractional polarization (Π) of the AME both for individual Galacticobjects and for large-scale (diffuse) measurements. Columns 1 to 3 indicate the region, the experiment used for this particular

constraint and the angular resolution, respectively. The following four columns indicate the constraints on the fractionalpolarization, Π, separated according to the frequency band for an easier comparison. When quoting upper limits, the 2-σ

range is given. Last column provides the reference(s).

Name Experiment Resolution Π [%] Reference

9-11 GHz 22 GHz 30-33 GHz 44 GHz

Galactic AME regions

Perseus COSMOSOMAS 1◦ 3.4+1.5−1.9 Battistelli et al. (2006)

” WMAP7 1◦ < 1.01 < 1.79 < 2.69 Lopez-Caraballo et al. (2011)

” WMAP7 1◦ < 1.4 < 1.9 < 4.7 Dickinson et al. (2011)

ρ-Ophiuchi CBI ∼ 9′ < 3.2 Casassus et al. (2008)

” WMAP7 1◦ < 1.7 < 1.6 < 2.6 Dickinson et al. (2011)

LDN1622 GBT ∼ 6′ < 2.7 Mason et al. (2009)

” WMAP7 1◦ < 2.6 < 4.8 < 8.3 Rubino-Martın et al. (2012)

Pleiades WMAP7 1◦ < 12.2 < 32.0 < 95.8 Rubino-Martın et al. (2012)

LPH96 CBI ∼ 9′ < 10 Dickinson et al. (2006)

” WMAP7 1◦ < 1.3 < 2.5 < 7.4 Rubino-Martın et al. (2012)

Helix CBI ∼ 9′ < 8 Casassus et al. (2007)

Diffuse Galactic AME

Full-Sky WMAP3 1◦ < 1 < 1 < 1 Kogut et al. (2003)

Full-Sky WMAP5 1◦ < 5 Macellari et al. (2011)

ν (GHz) I (Jy) Iame (Jy) Q (Jy) U (Jy) P (Jy) Pdb (Jy) (Πame)db (%)

DX8 corrected

30 46.076 ± 2.049 39.246 ± 2.100 −0.119 ± 0.200 0.243 ± 0.196 0.270 ± 0.197 < 0.306 < 0.778 (< 1.414)

44 36.272 ± 4.784 26.092 ± 4.804 −0.081 ± 0.617 −0.895 ± 0.469 0.899 ± 0.470 0.611+0.373−0.611 < 3.845 (< 6.601)

70 42.581 ± 11.261 14.331 ± 11.272 −0.339 ± 1.060 −0.087 ± 1.017 0.350 ± 1.057 < 1.072 < 8.322 (< 16.522)

DX9 corrected

30 46.186 ± 2.049 39.356 ± 2.100 −0.328 ± 0.180 0.132 ± 0.175 0.353 ± 0.179 0.292+0.162−0.205 < 0.973 (< 1.552)

44 36.142 ± 4.781 25.962 ± 4.801 −0.173 ± 0.549 −0.531 ± 0.420 0.558 ± 0.434 < 0.666 < 2.686 (< 5.024)

70 41.909 ± 11.256 13.659 ± 11.267 −0.412 ± 0.946 0.344 ± 0.901 0.537 ± 0.928 < 1.008 < 8.969 (< 17.477)

WMAP7

23 46.899 ± 1.322 40.449 ± 1.403 −0.038 ± 0.148 −0.007 ± 0.196 0.039 ± 0.150 < 0.173 < 0.434 (< 0.874)

33 42.839 ± 2.728 35.419 ± 2.765 0.035 ± 0.277 0.305 ± 0.369 0.307 ± 0.368 < 0.402 < 1.152 (< 2.216)

41 37.093 ± 4.087 27.983 ± 4.111 −0.020 ± 0.392 −0.510 ± 0.510 0.510 ± 0.510 < 0.613 < 2.245 (< 4.236)

61 35.418 ± 8.666 16.088 ± 8.678 0.263 ± 0.946 0.431 ± 1.244 0.505 ± 1.171 < 1.149 < 7.786 (< 15.450)

94 69.255 ± 18.086 4.815 ± 18.099 0.742 ± 2.328 −2.127 ± 3.072 2.253 ± 3.000 < 3.196 < 304.075 (< 506.563)

TABLE II: Perseus

QUIJOTE observations

★ Large observation programme (~100 hours, from december 2012, still ongoing), on an area covering ~200 deg2 around the Perseus molecular complex. One of the brightest AME regions on the sky (Watson et al. 2005, Planck collaboration 2011)

★ Final integration time of ~ 2500 s/beam, yielding a sensitivity of ~ 40 mJy/beam in Q and U

★ Daily calibration on Crab (flux and polarization angle calibrator) and Cas A (low-polarization source to calibrate the gains of pairs of correlated channels)

Quijote 11 GHz Planck 30 GHz

★ Also covering the California nebula (HII region - null polarization control region)

Perseus intensity maps

Horn 1 - 11 GHz Horn 3 - 11 GHz Horn 1 - 13 GHz Horn 3 - 13 GHz

Horn 2 - 17 GHz Horn 2 - 19 GHz LFI 30 GHz LFI 44 GHz

Perseus and California intensity SED

11 GHz 13 GHz 17 GHz 19 GHz

Perseus and California intensity SED

11 GHz 13 GHz 17 GHz 19 GHz

Polarization maps

11 GHz 13 GHz 17 GHz 19 GHz WMAP 23 GHz

11 GHz 13 GHz 17 GHz 19 GHz WMAP 23 GHz

U maps

Q maps

★ Aperture photometry:

• Signal integrated by averaging pixels belonging to region 1• Background subtracted by averaging pixels belonging to region 2

Upper limits estimation

• Rice bias corrected in P using the posterior distribution derived from the Rice distribution (Vaillancourt 2006):

1

f(P0|P ) = σ−1

√

2

πexp

[

−P 2

0

2σ2

]

exp[

−P 2

4σ2

]I0

(

PP0

σ2

)

I0

(

P 2

4σ2

)

• Bias in Π=P/I corrected through Monte-Carlo simulations

1

σ(Sν) =kBT 2

cmb

2h2c2

x4

sinh2(x/2)

[

σ2i

nb1

+σ2

j

nb2

]1/2

2

ν (GHz) I (Jy) Q (Jy) U (Jy) P (Jy) Pdb (Jy) Π (%) Πdb (%)

11 11.4 ± 1.1 0.07 ± 0.35 0.30 ± 0.27 0.30 ± 0.27 < 0.39 2.66 ± 2.39 < 3.385

13 14.4 ± 1.1 0.12 ± 0.29 0.22 ± 0.33 0.26 ± 0.32 < 0.37 1.78 ± 2.24 < 2.557

17 18.7 ± 1.6 −0.25 ± 0.40 0.28 ± 0.39 0.38 ± 0.40 < 0.50 2.02 ± 2.12 < 2.664

19 22.9 ± 2.4 −0.30 ± 0.70 0.35 ± 0.61 0.46 ± 0.65 < 0.74 2.00 ± 2.83 < 3.260

TABLE I: Perseus

Quijote upper limits

Comparison with other constraints