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tokens: such as the peculiar motion of the halo clouds, the nonuniform spectrum of the clouds due to the radiation balance and radiative transfer details, and so on. However, obviously, at this stage, those are lower-order effects with respect the global halo rotation. Moreover, since we consider M 104 as being foreground to the CMB, we note that for the maps we study (with monopole and dipole extracted) the foregrounds could also be negative due to physical processes, for example, in the case of clouds, the particular molecular energy level transitions, metastable states, two-photon emission or absorption, and so on. 3. Conclusions Similar to the case of other galaxies of the Local Group considered previously (in particular the galaxies M 31, M 82, M 81, M 33, and Cen A have been analyzed using Planck data and a temperature asymmetry Δ T about 60−80 μ K of one side with respect to the other about the rotation axis of the galactic disks has been detected in all cases), we found a consistent north–south temperature asymmetry toward the M 104 galaxy, that reaches values up to about 65 μ K within 0.6° (about 100 kpc) in all considered Planck bands 3 , and then starts to decrease. We mention that Chandra observations in the X-ray band of the M 104 galaxy show the presence of a diffuse X-ray emission extending at least up to 30 kpc from its center ( Li et al. 2011 ), together with hundreds of point sources which are a mixture of objects in the M 104 halo (mainly X-ray binaries) as well as background Quasars ( Li et al. 2010 ). However, the presence of this X-ray-emitting hot gas cannot explain the temperature asymmetry detected in Planck data. It is straightforward to show that if the cold-gas cloud model is at the origin of the detected temperature asymmetry (however, as anticipated in the previous section, other emission mechanisms may play a role in the detected signal), a lower limit to the M 104 galaxy dynamical mass is given by where R is the considered galaxy halo radius in units of 100 kpc, Δ T is the measured temperature asymmetry (in μ k ), and τ eff is the effective cloud optical depth (which depends on both the cloud filling factor and the averaged optical depth within a given Planck band. Expected values for τ eff are about a few 10 −3 ( Tahir et al. 2019 ), meaning that the M 104 dynamical mass out to ∼100 kpc is seen to be M dyn ≃ 3 × 10 12 M ⊙ , in agreement with other measurements (see, e.g., Tempel Tenjes 2006 ). It is interesting to mention in this respect that this galactocentric distance appears close to the transonic point (at ≃126 kpc), determined recently by Igarashi et al. (2014) within the framework of the transonic outflow model in a dark matter halo applied to the Sombrero galaxy 4 . The detected temperature asymmetry is, as discussed in the previous section, almost frequency-independent and indicates that the M 104 galaxy halo is rotating with respect to the major symmetry axis of the galaxy disk (Variant 1). However, the