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The full-sky Planck polarization data at 850um revealed unexpected propertiesof the E and B mode power spectra of dust emission in the interstellar medium(ISM). The positive cross-correlation between the total dust intensity, T, withthe B modes has raised new questions about the physical mechanisms that affectdust polarization, such as the Galactic magnetic-field structure. This is keyboth to better understanding ISM dynamics and to accurately describing Galacticforegrounds to the polarization of the Cosmic Microwave Background (CMB). Inthis theoretical paper we investigate the possibility that the observedcross-correlations in the dust polarization power spectra, and specificallybetween T and B, can be related to a parity-odd quantity in the ISM such as themagnetic helicity. We produce synthetic dust polarization data, derived from 3Danalytical toy models of density structures and helical magnetic fields, tocompare with the E and B modes of observations. Focusing on the observed T-Bcorrelation, we propose a new line of interpretation of the Planck observationsbased on a large-scale helical component of the Galactic magnetic field in thesolar neighborhood. Our analysis shows that: I) the sign of magnetic helicitydoes not affect E and B modes for isotropic magnetic-field configurations; II)helical magnetic fields threading interstellar filaments cannot reproduce thePlanck results; III) a weak helical left-handed magnetic field structure in thesolar neighborhood may explain the T-B correlation seen in the Planck data.This work suggests a new perspective for the interpretation of the dustpolarization power spectra, which strongly supports the imprint of alarge-scale structure of the Galactic magnetic field in the solar neighborhood.

astronomy and astrophysics

Is there a left-handed magnetic field in the solar neighborhood?  Exploring helical magnetic fields in the interstellar medium through dust  polarization power spectra