Quantum Suppression of Alignment in Ultrasmall Grains: Microwave Emission From Spinning Dust Will Be Negligibly Polarized

Draine, B. T.; Hensley, Brandon

doi:10.3847/0004-637x/831/1/59

Cited by 48 publications

(30 citation statements)

References 47 publications

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“…Theory suggests that AME should only be very weakly polarized. Draine & Hensley (2016) predict a polarization fraction of 10 −6 and current measurements place upper limits of ∼ 1% on the polarization fraction of diffuse AME. See the review of theory and observations in Dickinson et al (2018).…”

Section: Amementioning

confidence: 73%

The C-Band All-Sky Survey (C-BASS): Simulated parametric fitting in single pixels in total intensity and polarization

Jew

Taylor

Jones

et al. 2019

Monthly Notices of the Royal Astronomical Society

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The cosmic microwave background B-mode signal is potentially weaker than the diffuse Galactic foregrounds over most of the sky at any frequency. A common method of separating the CMB from these foregrounds is via pixel-based parametric-model fitting. There are not currently enough all-sky maps to fit anything more than the most simple models of the sky. By simulating the emission in seven representative pixels, we demonstrate that the inclusion of a 5 GHz data point allows for more complex models of low-frequency foregrounds to be fitted than at present. It is shown that the inclusion of the CBASS data will significantly reduce the uncertainties in a number of key parameters in the modelling of both the galactic foregrounds and the CMB. The extra data allow estimates of the synchrotron spectral index to be constrained much more strongly than is presently possible, with corresponding improvements in the accuracy of the recovery of the CMB amplitude. However, we show that to place good limits on models of the synchrotron spectral curvature will require additional low-frequency data.

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Section: Amementioning

confidence: 73%

The C-Band All-Sky Survey (C-BASS): Simulated parametric fitting in single pixels in total intensity and polarization

Jew

Taylor

Jones

et al. 2019

Monthly Notices of the Royal Astronomical Society

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“…AME is strongly correlated with far-infrared thermal dust emission at 100 microns (Davies et al 2006), so the best explanation for AME so far is electric dipole radiation from spinning dust grains in our Galaxy (Draine & Lazarian 1998). Since spinning dust polarization has been shown to be negligibly small (Draine & Hensley 2016), we consider unpolarized AME in our simulations.…”

Section: Amementioning

confidence: 99%

Leverage on small-scale primordial non-Gaussianity through cross-correlations between CMB $E$-mode and $μ$-distortion anisotropies

Remazeilles,

Ravenni,

Chluba

2021

Preprint

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Multi-field inflation models and non-Bunch-Davies vacuum initial conditions both predict sizeable non-Gaussian primordial perturbations and consequently anisotropic 𝜇-type spectral distortions of the cosmic microwave background (CMB) blackbody. While CMB anisotropies allow us to probe primordial non-Gaussianity at wavenumbers 𝑘 0.05 Mpc −1 , 𝜇-distortion anisotropies are related to non-Gaussianity of primordial perturbation modes with much larger wavenumbers, 𝑘 740 Mpc −1 . Through cross-correlations between CMB anisotropies and 𝜇-distortion anisotropies, one can therefore shed light on the aforementioned inflation models. We investigate the ability of a future CMB satellite imager like LiteBIRD to measure 𝜇𝑇 and 𝜇𝐸 cross-power spectra between anisotropic 𝜇-distortions and CMB temperature and 𝐸-mode polarization anisotropies in the presence of foregrounds, and derive LiteBIRD forecasts on 𝑓 𝜇 NL (𝑘 740 Mpc −1 ). We show that 𝜇𝐸 cross-correlations with CMB polarization provide more constraining power on 𝑓 𝜇 NL than 𝜇𝑇 cross-correlations in the presence of foregrounds, and the joint combination of 𝜇𝑇 and 𝜇𝐸 observables add further leverage to the detection of small-scale primordial non-Gaussianity. For multi-field inflation, we find that LiteBIRD would allow to detect 𝑓 𝜇 NL = 4500 at 5𝜎 significance after foreground removal, and achieve a minimum error of about 𝜎( 𝑓 𝜇 NL = 0) 800 at 68% CL by combining CMB temperature and polarization. Due to the huge dynamic range of wavenumbers between CMB and 𝜇-distortion anisotropies, such large 𝑓 𝜇 NL values at 𝑘 740 Mpc −1 would still be consistent with CMB constraints 𝑓 NL 5 at 𝑘 0.05 Mpc −1 in the case of very mild scale-dependence of primordial non-Gaussianity. Anisotropic spectral distortions thus provide a new path, complementary to CMB 𝐵-modes, to probe inflation with LiteBIRD.

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“…Significant contributors to the extinction are small silicates (sSi) in the far-UV, small graphite (gr) and PAH in the 217.5 nm extinction bump region, large amorphous carbon (aC) with a nearly constant extinction at 2 ≤ x = 1/λ ≤ 7 µm −1 , and large silicates (Si) that show a linear increase of the extinction with x in that range. Draine & Hensley (2016) pointed out that the rapid fall-off of the polarisation of starlight in the far-UV suggests that small (r < 6 nm) grains are nearly spherical and do not contribute to the far-UV polarisation. On the other hand, interstellar polarisation cannot be explained by spherical particles made of optically isotropic material.…”

Section: Dust Modelmentioning

confidence: 99%

Large Interstellar Polarisation Survey

Siebenmorgen

Voshchinnikov

Bagnulo

et al. 2018

A&A

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It is well known that the dust properties of the diffuse interstellar medium exhibit variations towards different sight-lines on a large scale. We have investigated the variability of the dust characteristics on a small scale, and from cloud-to-cloud. We use low-resolution spectro-polarimetric data obtained in the context of the Large Interstellar Polarisation Survey (LIPS) towards 59 sight-lines in the Southern Hemisphere, and we fit these data using a dust model composed of silicate and carbon particles with sizes from the molecular to the sub-micrometre domain. Large (≥6 nm) silicates of prolate shape account for the observed polarisation. For 32 sight-lines we complement our data set with UVES archive high-resolution spectra, which enable us to establish the presence of single-cloud or multiple-clouds towards individual sight-lines. We find that the majority of these 35 sight-lines intersect two or more clouds, while eight of them are dominated by a single absorbing cloud. We confirm several correlations between extinction and parameters of the Serkowski law with dust parameters, but we also find previously undetected correlations between these parameters that are valid only in single-cloud sight-lines. We find that interstellar polarisation from multiple-clouds is smaller than from single-cloud sight-lines, showing that the presence of a second or more clouds depolarises the incoming radiation. We find large variations of the dust characteristics from cloud-to-cloud. However, when we average a sufficiently large number of clouds in single-cloud or multiple-cloud sight-lines, we always retrieve similar mean dust parameters. The typical dust abundances of the single-cloud cases are [C]/[H] = 92 ppm and [Si]/[H] = 20 ppm.

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Quantum Suppression of Alignment in Ultrasmall Grains: Microwave Emission From Spinning Dust Will Be Negligibly Polarized

Cited by 48 publications

References 47 publications

The C-Band All-Sky Survey (C-BASS): Simulated parametric fitting in single pixels in total intensity and polarization

The C-Band All-Sky Survey (C-BASS): Simulated parametric fitting in single pixels in total intensity and polarization

Leverage on small-scale primordial non-Gaussianity through cross-correlations between CMB $E$-mode and $μ$-distortion anisotropies

Large Interstellar Polarisation Survey

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