Evidence for cloud-to-cloud variations in the ratio of polarized thermal dust emission to starlight polarization

The correlation between optical starlight polarization and polarized thermal dust emission can be used to infer intrinsic dust properties. This correlation is quantified by the ratio RP/p, which has been measured to be 5.42 ± 0.05 MJy sr−1 at 353 GHz when averaged over large areas of the sky. We investigate this correlation using newly published stellar polarimetric data densely sampling a continuous sky region of about four square degrees at intermediate Galactic latitude. We combine RoboPol optical polarization measurements for 1,430 stars with submillimeter data from the Planck satellite at 353 GHz. We perform linear fits between the Planck (Qs, Us) and optical (qv, uv) Stokes parameters, taking into account the differences in resolution between the two datasets as well as the distribution of clouds along the line of sight. We find that in this region of the sky the RP/p value is 3.67 ± 0.05 MJy sr−1, indicating a significantly shallower slope than that found previously using different stellar samples.We also find significant differences in the fitted slopes when fitting the Qs–qv and Us–uv data separately. We explore two explanations using mock data: miscalibration of polarization angle and variations in RP/p along the line of sight due to multiple clouds. We show that the former can produce differences in the correlations of Qs–qv and Us–uv, but large miscalibration angles would be needed to reproduce the magnitude of the observed differences. Our simulations favor the interpretation that RP/p differs between the two clouds that overlap on the sky in this region. The difference in RP/p suggests that the two clouds may have distinct dust polarimetric properties.With knowledge from the tomographic decomposition of the stellar polarization, we find that one cloud appears to dominate the correlation of Us–uv, while both clouds contribute to the correlation of the Qs–qv data.