On the Galactic Halos Rotation by Planck Data

TL;DR

This paper investigates the rotation of galactic halos using Planck CMB data, analyzing asymmetries and proposing the existence of virial clouds to trace halo dynamics.

Contribution

It introduces a method to constrain the composition of virial clouds in galactic halos using Planck data and asymmetry analysis.

Findings

Evidence of asymmetries in CMB towards multiple galaxies

Constraints on dust and gas fractions in virial clouds

Support for stable gas and dust clouds in thermal equilibrium

Abstract

As galactic halos are not directly visible, there are many ambiguities regarding their composition and rotational velocity. Though most of the dark matter is non-baryonic, {\it some fraction is}, and it can be used to trace the halo rotation. Asymmetries in the CMB towards M31 had been seen in the Planck data and ascribed to the rotational Doppler shift of the M31 halo. Subsequently, the same methods were used in the direction of five other galaxies belonging to the Local Group, namely M33, M81, M82, NGC 5128, and NGC 4594. It had been proved that there could be stable clouds of gas and dust in thermal equilibrium with the CMB at 2.7 K, which had been called ``virial clouds''. In this paper, adopting this scenerio, an attempt is made to constrain the fraction of dust grains and gas molecules in the clouds.