On the Galactic Halos Rotation by Planck Data

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.

18 pages, 7 figrues, Journal: Symmetry, Special Issues:Recent Advances Studies Cosmic Microwave Background

References in corpus (8)

• The long bar as seen by the VVV survey: I. Colour-magnitude diagrams
• Planck's confirmation of the M31 disk and halo rotation
• The challenge of measuring and mapping the missing baryons
• Triangulum galaxy viewed by Planck
• Distant foreground and the Planck-derived Hubble constant
• Virial clouds explaining the observed rotational asymmetry in the galactic halos
• The rotational kinetic Sunyaev-Zeldovich contribution to the temperature asymmetry toward the M31 halo
• Evolution of virial clouds-I: from surface of last scattering up to the formation of population-III stars