{"status":"ok","message-type":"work","message-version":"1.0.0","message":{"indexed":{"date-parts":[[2026,3,16]],"date-time":"2026-03-16T09:01:29Z","timestamp":1773651689950,"version":"3.50.1"},"reference-count":55,"publisher":"MDPI AG","issue":"1","license":[{"start":{"date-parts":[[2023,1,5]],"date-time":"2023-01-05T00:00:00Z","timestamp":1672876800000},"content-version":"vor","delay-in-days":0,"URL":"https:\/\/creativecommons.org\/licenses\/by\/4.0\/"}],"content-domain":{"domain":[],"crossmark-restriction":false},"short-container-title":["Symmetry"],"abstract":"<jats:p>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 \u201cvirial clouds\u201d. In this paper, adopting this scenerio, an attempt is made to constrain the fraction of dust grains and gas molecules in the clouds.<\/jats:p>","DOI":"10.3390\/sym15010160","type":"journal-article","created":{"date-parts":[[2023,1,6]],"date-time":"2023-01-06T01:48:19Z","timestamp":1672969699000},"page":"160","update-policy":"https:\/\/doi.org\/10.3390\/mdpi_crossmark_policy","source":"Crossref","is-referenced-by-count":4,"title":["On the Galactic Halos Rotation by Planck Data"],"prefix":"10.3390","volume":"15","author":[{"ORCID":"https:\/\/orcid.org\/0000-0003-0475-0784","authenticated-orcid":false,"given":"Noraiz","family":"Tahir","sequence":"first","affiliation":[{"name":"Department of Mathematics and Physics \u201cEnnio De Giorgi\u201d, University of Salento, Via per Arnesano, I-73100 Lecce, Italy"},{"name":"INFN, Sezione di Lecce, Via per Arnesano, I-73100 Lecce, Italy"}]},{"ORCID":"https:\/\/orcid.org\/0000-0001-6460-7563","authenticated-orcid":false,"given":"Francesco","family":"De Paolis","sequence":"additional","affiliation":[{"name":"Department of Mathematics and Physics \u201cEnnio De Giorgi\u201d, University of Salento, Via per Arnesano, I-73100 Lecce, Italy"},{"name":"INFN, Sezione di Lecce, Via per Arnesano, I-73100 Lecce, Italy"},{"name":"INAF, Sezione di Lecce, Via per Arnesano, I-73100 Lecce, Italy"}]},{"given":"Asghar","family":"Qadir","sequence":"additional","affiliation":[{"name":"Abdul Salam School of Mathematics, G. C. University, Lahore 54600, Pakistan"}]},{"given":"Achille A.","family":"Nucita","sequence":"additional","affiliation":[{"name":"Department of Mathematics and Physics \u201cEnnio De Giorgi\u201d, University of Salento, Via per Arnesano, I-73100 Lecce, Italy"},{"name":"INFN, Sezione di Lecce, Via per Arnesano, I-73100 Lecce, Italy"},{"name":"INAF, Sezione di Lecce, Via per Arnesano, I-73100 Lecce, Italy"}]}],"member":"1968","published-online":{"date-parts":[[2023,1,5]]},"reference":[{"key":"ref_1","doi-asserted-by":"crossref","unstructured":"Bertone, G. (2010). Particle Dark Matter: Observations, Models and Searches, Cambridge University Press.","DOI":"10.1017\/CBO9780511770739"},{"key":"ref_2","doi-asserted-by":"crossref","unstructured":"Burdyuzha, V.V. (2020). From the Early Universe to the Modern Universe. Symmetry, 12.","DOI":"10.3390\/sym12030382"},{"key":"ref_3","doi-asserted-by":"crossref","unstructured":"P\u00e9rez de los Heros, C. (2020). 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