Revisiting perfect fluid dark matter: Observational constraints from our galaxy

Abstract

We revisit certain features of an assumed spherically symmetric perfect fluid dark matter halo in the light of the observed data of our galaxy, the Milky Way (MW). The idea is to apply the Faber-Visser approach of combined observations of rotation curves and lensing to a first post-Newtonian approximation to "measure" the equation of state ω(r) of the perfect fluid galactic halo. However, for the model considered here, no constraints from lensing are used as it will be sufficient to consider only the rotation curve observations. The lensing mass together with other masses will be just computed using recent data. Since the halo has attractive gravity, we shall impose the constraint that ω(r) ≥ 0 for r ≤ R MW , where R MW ∼ 200 kpc is the adopted halo radius of our galaxy. The observed circular velocity ℓ = 2v 2 c /c 2 0 from the flat rotation curve and a crucial adjustable parameter D appearing in the perfect fluid solution then yield different numerical ranges of ω(r). It is demonstrated that the computed observables such as the rotation curve mass, the lens mass, the post-Newtonian mass of our galaxy compare well with the recent mass data. We also calculate the Faber-Visser χ− factor, which is a measure of pressure content in the dark matter. Our analysis indicates that a range 0 ≤ ω(r) ≤ 2.8 × 10 −7 for the perfect fluid dark matter can reasonably describe the attractive galactic halo. This is a strong constraint indicating a dust-like CDM halo (ω ∼ 0) supported also by CMB constraints.1 The reason for the appearance of static FLRW background around the imbedded perfect fluid dark matter is already explained in Ref. [1]. The Einstein field equations are solved with perfect fluid stress tensor in both the cases but we sought a static solution from the start. While working on a local problem (flat rotation curve), the scale factor is usually fixed to R 0 = 1 today.

The possible equation of state of dark matter in low surface brightness galaxies *

“…). This phenomenon has already been reported [39]. The velocity dispersion at the galaxy center is significantly less than the speed of light in Table 1.…”

“…This is not consistent with the observations. The observations show that the mass of the central black hole is far less than that of the DM halo for many types of galaxies [37][38][39].…”

Constraining the Rastall parameters in static space–times with galaxy-scale strong gravitational lensing

“…which describes how mass evolves as a function of radius r on the basis of Rastall gravity. For galaxies and galaxy clusters, the evidences from theories and observations provide that ω is extremely close to 0 (e.g., Rahaman et al 2010;Sartoris et al 2014;Potapov, Garipova, & Nandi 2016). Therefore, we let ω = 0 in this work.…”