On the Galactic Halos Rotation by Planck Data

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, 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...

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Bibliographic Details
Published inSymmetry (Basel) Vol. 15; no. 1; p. 160
Main Authors Tahir, Noraiz, De Paolis, Francesco, Qadir, Asghar, Nucita, Achille A.
Format Journal Article
LanguageEnglish
Published Basel MDPI AG 01.01.2023
Subjects
Asymmetry
baryons
Boundary conditions
Clouds
Cold
cosmic microwave background
Cosmic rays
Dark matter
Doppler effect
Dust
Galactic halos
Galactic rotation
Local group (astronomy)
molecular clouds
Radiation
Spiral galaxies
Stars & galaxies
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Summary: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, 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.
ISSN:2073-8994
2073-8994
DOI:10.3390/sym15010160