Analysis of dark matter profiles in the halos of spiral galaxies

Ye.  Kurmanov; Kuantay Boshkayev; T.  Konysbayev; M.  Muccino; A.  Urazalina; G.  Ikhsan; N.  Saiyp; G.  Rabigulova; M.  Karlinova; G.  Suliyeva; A.  Taukenova; N.  Beissen

doi:10.26577/phst.2023.v10.i2.01

Authors

Ye. Kurmanov National Nanotechnology Laboratory of Open Type, Al-Farabi Kazakh National University, Almaty, Kazakhstan https://orcid.org/0000-0003-3695-0166
Kuantay Boshkayev Al-Farabi Kazakh National University
T. Konysbayev 2 Al-Farabi Kazakh National University, Almaty, Kazakhstan https://orcid.org/0000-0001-9476-3700
M. Muccino Istituto Nazionale di Fisica Nucleare, Laboratori Nazionali di Frascati, Frascati, Italy https://orcid.org/0000-0002-2234-9225
A. Urazalina National Nanotechnology Laboratory of Open Type, Almaty, Kazakhstan https://orcid.org/0000-0002-4633-9558
G. Ikhsan National Nanotechnology Laboratory of Open Type, Almaty, Kazakhstan https://orcid.org/0000-0003-0556-166X
N. Saiyp Al-Farabi Kazakh National University, Almaty, Kazakhstan https://orcid.org/0009-0001-9128-0671
G. Rabigulova Al-Farabi Kazakh National University, Almaty, Kazakhstan https://orcid.org/0009-0003-8998-6282
M. Karlinova Al-Farabi Kazakh National University, Almaty, Kazakhstan https://orcid.org/0009-0000-0764-4851
G. Suliyeva National Nanotechnology Laboratory of Open Type, Almaty, Kazakhstan https://orcid.org/0000-0001-5072-7898
A. Taukenova https://orcid.org/0000-0002-5154-330X
N. Beissen Al-Farabi Kazakh National University, Almaty, Kazakhstan https://orcid.org/0000-0002-1957-2768

DOI:

https://doi.org/10.26577/phst.2023.v10.i2.01

Abstract

The distribution of dark matter in the low surface brightness spiral galaxies U5750, U11454, U11819, and U11648 is analyzed by utilizing well-established density profiles from existing literature. These profiles include the Beta, Brownstein, Burkert, exponential sphere, pseudo-isothermal, and Persic profiles. For simplicity, we assume spherically symmetric distribution of dark matter in the considered galaxies, without accounting for their intricate structural complexities. For each density profile, we fit the rotation curve data to the aforementioned galaxies. Employing Markov Chain Monte Carlo statistical analyses, we infer model-free parameters from the rotation curves, namely the characteristic (central) density and scale radius. This enables us to estimate the total dark matter mass within the galactic halos. To identify the best-fit profile, we employ the Bayesian Information Criterion. Additionally, we adopt the Levenberg-Marquardt nonlinear least squares approach for the purpose of comparison and completeness. Through our statistical analysis, we offer a physical interpretation behind the selection of specific profiles. This interpretation is based on the insights obtained from the analyses.

Analysis of dark matter profiles in the halos of spiral galaxies

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