Joint 3D modelling of the polarized Galactic synchrotron and thermal dust foreground diffuse emission

Fauvet, L.; Macías-Pérez, J. F.; Aumont, J.; Désert, F.‐X.; Jaffe, T. R.; Banday, A. J.; Tristram, M.; Waelkens, A.; Santos, D.

doi:10.1051/0004-6361/201014492

Cited by 45 publications

(98 citation statements)

References 61 publications

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“…The magnetic field orientation depends on the spiral structure of the large-scale Galactic magnetic field and on local perturbation of the field due to turbulent motions or shell expansions. The former can be estimated using a model of the spiral structure of the field (Han et al 2006;Sun et al 2008;Sun & Reich 2010;Jansson et al 2009;Jaffe et al 2010Jaffe et al , 2011Fauvet et al 2011), but the latter can only be estimated statistically (Miville-Deschênes et al 2008). Note that, since the synchrotron spectral index varies across the sky due to variations of the cosmic ray energy spectrum across the Galaxy, and since geometric depolarisation effects also depend on local effects in three dimensions, it is expected that the spectral index β s is different for I, Q and U.…”

Section: Synchrotron Polarisationmentioning

confidence: 99%

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

Delabrouille

Betoule

Melin

et al. 2013

A&A

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214

231

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We present the Planck Sky Model (PSM), a parametric model for generating all-sky, few arcminute resolution maps of sky emission at submillimetre to centimetre wavelengths, in both intensity and polarisation. Several options are implemented to model the cosmic microwave background, Galactic diffuse emission (synchrotron, free-free, thermal and spinning dust, CO lines), Galactic H ii regions, extragalactic radio sources, dusty galaxies, and thermal and kinetic Sunyaev-Zeldovich signals from clusters of galaxies. Each component is simulated by means of educated interpolations/extrapolations of data sets available at the time of the launch of the Planck mission, complemented by state-of-the-art models of the emission. Distinctive features of the simulations are spatially varying spectral properties of synchrotron and dust; different spectral parameters for each point source; modelling of the clustering properties of extragalactic sources and of the power spectrum of fluctuations in the cosmic infrared background. The PSM enables the production of random realisations of the sky emission, constrained to match observational data within their uncertainties. It is implemented in a software package that is regularly updated with incoming information from observations. The model is expected to serve as a useful tool for optimising planned microwave and sub-millimetre surveys and testing data processing and analysis pipelines. It is, in particular, used to develop and validate data analysis pipelines within the Planck collaboration. A version of the software that can be used for simulating the observations for a variety of experiments is made available on a dedicated website.

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Section: Synchrotron Polarisationmentioning

confidence: 99%

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

Delabrouille

Betoule

Melin

et al. 2013

A&A

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214

231

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“…The colour correction depends on the actual dust SED; it is the scaling factor used to transform from the specific intensity of the dust emission, at the reference frequency, to the Planck brightness in MJy sr −1 (see Eq. (19) signal in the high frequency Planck bands (Tucci et al 2005;Dunkley et al 2009b;Fraisse et al 2009;Fauvet et al 2011;Planck Collaboration Int. XXII 2015).…”

Section: Planck Datamentioning

confidence: 99%

“…Since its specific intensity scaling with frequency follows a power law with a spectral index close to −3 (Gold et al 2011;Macellari et al 2011;Fuskeland et al 2014), synchrotron polarized emission is expected to be subdominant in the Planck HFI channels in general and negligible at 353 GHz (Tucci et al 2005;Dunkley et al 2009a;Gold et al 2011;Fauvet et al 2011;Fuskeland et al 2014;Planck Collaboration Int. XXII 2015).…”

Section: Synchrotron Emissionmentioning

confidence: 99%

“…The observed polarization relates to the nature, size, and shape of dust grains and the mechanisms of alignment, discussed for example by Draine (2004) and Martin (2007). It also probes the structure of the Galactic magnetic field, which is an essential component of models of Galactic dust polarization (Baccigalupi 2003;Fauvet et al 2011Fauvet et al , 2012O'Dea et al 2012;Jaffe et al 2013;Delabrouille et al 2013).…”

Section: Introductionmentioning

confidence: 99%

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Planckintermediate results

Adam¹,

Ade²,

Aghanim³

et al. 2016

A&A

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188

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The polarized thermal emission from diffuse Galactic dust is the main foreground present in measurements of the polarization of the cosmic microwave background (CMB) at frequencies above 100 GHz. In this paper we exploit the uniqueness of the Planck HFI polarization data from 100 to 353 GHz to measure the polarized dust angular power spectra C EE and C BB over the multipole range 40 < < 600 well away from the Galactic plane. These measurements will bring new insights into interstellar dust physics and allow a precise determination of the level of contamination for CMB polarization experiments. Despite the non-Gaussian and anisotropic nature of Galactic dust, we show that general statistical properties of the emission can be characterized accurately over large fractions of the sky using angular power spectra. The polarization power spectra of the dust are well described by power laws in multipole, C ∝ α , with exponents α EE,BB = −2.42 ± 0.02. The amplitudes of the polarization power spectra vary with the average brightness in a way similar to the intensity power spectra. The frequency dependence of the dust polarization spectra is consistent with modified blackbody emission with β d = 1.59 and T d = 19.6 K down to the lowest Planck HFI frequencies. We find a systematic difference between the amplitudes of the Galactic B-and E-modes, C BB /C EE = 0.5. We verify that these general properties are preserved towards high Galactic latitudes with low dust column densities. We show that even in the faintest dust-emitting regions there are no "clean" windows in the sky where primordial CMB B-mode polarization measurements could be made without subtraction of foreground emission. Finally, we investigate the level of dust polarization in the specific field recently targeted by the BICEP2 experiment. Extrapolation of the Planck 353 GHz data to 150 GHz gives a dust power D BB ≡ ( + 1)C BB /(2π) of 1.32 × 10 −2 µK 2 CMB over the multipole range of the primordial recombination bump (40 < < 120); the statistical uncertainty is ±0.29 × 10 −2 µK 2 CMB and there is an additional uncertainty (+0.28, −0.24) × 10 −2 µK 2 CMB from the extrapolation. This level is the same magnitude as reported by BICEP2 over this range, which highlights the need for assessment of the polarized dust signal even in the cleanest windows of the sky.

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“…XXIX 2014;Fauvet et al 2012Fauvet et al , 2011. The Planck mission 2 was equipped with 11 HEMT (Low Frequency Instrument, LFI, Mennella et al 2011) and 52 high-impedance bolometers (High Frequency Instrument, HFI, Planck HFI Core Team 2011) observing from 30 GHz to 1 THz.…”

Section: Introductionmentioning

confidence: 99%

Bi-layer kinetic inductance detectors for space observations between 80–120 GHz

Catalano

Goupy

Sueur

et al. 2015

A&A

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We have developed lumped element kinetic inductance detectors (LEKIDs) that are sensitive in the frequency band from 80 to 120 GHz. In this work, we take advantage of the so-called proximity effect to reduce the superconducting gap of aluminium (Al), otherwise strongly suppressing the LEKID response for frequencies smaller than 100 GHz. We designed, produced, and optically tested various fully multiplexed arrays based on multi-layer combinations of Al and titanium (Ti). Their sensitivities were measured using a dedicated closed-circle 100 mK dilution cryostat and a sky simulator, which allowed us to reproduce realistic observation conditions. The spectral response was characterised with a Martin-Puplett interferometer up to THz frequencies and had a resolution of 3 GHz. We demonstrate that Ti-Al LEKID can reach an optical sensitivity of about 1.4 × 10 −17 W/Hz 0.5 (best pixel), or 2.2 × 10 −17 W/Hz 0.5 when averaged over the whole array. The optical background was set to roughly 0.4 pW per pixel, which is typical for future space observatories in this particular band. The performance is close to a sensitivity of twice the CMB photon noise limit at 100 GHz, which drove the design of the Planck HFI instrument. This figure remains the baseline for the next generation of millimetre-wave space satellites.

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Joint 3D modelling of the polarized Galactic synchrotron and thermal dust foreground diffuse emission

Cited by 45 publications

References 61 publications

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

The pre-launchPlanckSky Model: a model of sky emission at submillimetre to centimetre wavelengths

Planckintermediate results

Bi-layer kinetic inductance detectors for space observations between 80–120 GHz

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