POLARIZED FAR-INFRARED AND SUBMILLIMETER EMISSION FROM INTERSTELLAR DUST

By B. Draine, A. Fraisse. 2008

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Polarized far-infrared (FIR) and submillimeter emission is calculated for models of nonspherical dust grains that are constrained to reproduce the observed wavelength-dependent extinction and polarization of starlight. For emission from regions where the magnetic field is perpendicular to the line of sight, the FIR emission is expected to have substantial linear polarization at wavelengths λ ≳ 100 μm, but the degree of linear polarization, and its variation with wavelength, is model dependent. Models in which the starlight polarization is produced by both amorphous silicate and graphite grains have linear polarizations between 6% and 10% at λ>100 μm, but for some models in which only silicate grains are spheroidal, the linear polarization increases from about 3% at 100 μm to about 15% at 1 mm. We briefly discuss the implications of these results for the removal of the polarized dust emission from maps of the cosmic microwave background, as well as the possibility of discriminating among interstellar dust models based on observations of FIR and submillimeter linear polarization.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics

View Paper: https://www.semanticscholar.org/paper/316335c9acc3c5c42567160915e99fc812c8c46b

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Citations in the corpus

The global dust SED: tracing the nature and evolution of dust with DustEM (2010, background): “…models aim to consistently reproduce the observed extinction and emission (Désert et al. 1990, hereafter DBP90) (Siebenmorgen & Kruegel 1992; Dwek et al. 1997; Li & Draine 2001a; Zubko et al. 2004; Draine & Li 2007, hereafter DL07) as well as the associated polarization (Draine & Fraisse 2009).”
The pre-launch Planck Sky Model: a model of sky emission at submillimetre to centimetre wavelengths (2012, background): “Draine & Fraisse (2009) have shown that for particular mixtures of dust grains, the intrinsic polarisation of the dust emission could vary significantly with frequency in the 100–800 GHz range.”
A BUDGET AND ACCOUNTING OF METALS AT z ∼ 0: RESULTS FROM THE COS-HALOS SURVEY (2013, methodology): “Using the Weingartner & Draine (2001), Zubko et al. (2004), and Draine & Fraisse (2009) dust models to constrain the oxygen fraction of dust (see also Draine 2011), we find Moxy,dust Mdust = µoxyN oxy dust ∑ X µXNXdust , (A2) where µ is the average atomic mass, X is one of the elements C, N, O, Mg,…”
Planck intermediate results. XIX. An overview of the polarized thermal emission from Galactic dust (2014, background): “Secondly, the grains are aligned by the interstellar magnetic field because they are rotating, probably with differing efficiencies depending on grain size and composition (Draine & Fraisse 2009).”
Planck intermediate results. XXII. Frequency dependence of thermal emission from Galactic dust in intensity and polarization (2014, methodology): “This is much higher than upper limits reported from the analysis of compact sources (Dickinson et al. 2011; López-Caraballo et al. 2011; Rubiño-Martín et al. 2012) and theoretical predictions (Lazarian & Draine 2000; Hoang et al. 2013).”
The Quest for B Modes from Inflationary Gravitational Waves (2015, background): “In addition, the frequency dependence of the dust polarization fraction as observed by Planck [see Figure 13 in Ade et al. (2014i)] has an opposite trend compared to the longstanding predictions from models of silicate or carbonaceous dust grains (see Figure 8 of Draine & Fraisse (2009)).”