Revisiting perfect fluid dark matter: Observational constraints from our galaxy

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• 作者：Alexander A. Potapov^a ; ^{potapovaa@mail.ru" class="auth_mail" title="E-mail the corresponding author} ; Guzel M. Garipova^a ; ^{goldberg144@gmail.com" class="auth_mail" title="E-mail the corresponding author} ; Kamal K. Nandi^a ; ^b ; ^c ; ^{kamalnandi1952@yahoo.co.in" class="auth_mail" title="E-mail the corresponding author}
• 关键词：Dark matter ; Perfect fluid ; Equation of state ; Galactic masses
• 刊名：Physics Letters B
• 出版年：2016
• 出版时间：10 February 2016
• 年：2016
• 卷：753
• 期：Complete
• 页码：140-146
• 全文大小：519 K

文摘

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)$\omega (r)$ 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 5703a0a6eb576617534ae" title="Click to view the MathML source">ω(r)≥0$\omega (r)\ge 0$ for r≤R_MW$r\le R_{\text{MW}}$, where R_MW∼200 kpc$R_{\text{MW}}\sim 200\text{kpc}$ is the adopted halo radius of our galaxy. The observed circular velocity ℓ   (i5" class="mathmlsrc">i5.gif&_user=111111111&_pii=S0370269315009132&_rdoc=1&_issn=03702693&md5=ddc532defcb3d70c118e6158cf3af656">i5.gif">) 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)$\omega (r)$. 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$0\le \omega (r)\le 2.8\times {10}^{-7}$ for the perfect fluid dark matter can reasonably describe the attractive galactic halo. This is a strong constraint indicating a dust-like CDM halo (57957e8811fda5a138b152adcce" title="Click to view the MathML source">ω∼0$\omega \sim 0$) supported also by CMB constraints.