Galaxy formation with wave/fuzzy dark matter: The core-halo structure and the solitonic imprint
Pozo A. Emami R. Mocz P. Broadhurst T. Hernquist L. Vogelsberger M. Smith R. Tremblay G. Narayan R. Steiner J. Grindlay J. Smoot G.
1 July 2025EDP Sciences
Astronomy and Astrophysics
2025#699
Dark matter-dominated cores have long been claimed for the well-studied local group dwarf galaxies. More recently, extended stellar halos have been uncovered around several of these dwarfs through deeper imaging and spectroscopy. Such core-halo structures (inner flat core and a characteristic r-3 asymptotic outer halo profile) are not a feature of conventional cold dark matter (CDM). In contrast, smooth and prominent dark matter cores are predicted for wave/fuzzy dark matter ( DM). The question arises as to what extent the visible stellar profiles should reflect this dark matter core structure. Here we compare cosmological hydrodynamical simulations of CDM, WDM(model used as a proxy for DM) & DM, aiming to predict the stellar profiles for these three DM scenarios. We show that cores surrounded by extended halos are distinguishable for DM, where the stellar density is enhanced in the core due to the presence of the relatively dense soliton. Our analysis demonstrates that, in our simulations, a distinctive core-halo structure does not appear in the case of CDM in the DM, gas, or stars. Whereas we do find a core-halo transition for DM, gas, and stars for DM, and the scale of this transition is in line with the predicted core radius set by the soliton scale anticipated for the adopted boson mass of 2:5 x 10-22eV. The presence of a core-halo structure in the stellar profile for Galaxy 1 for DM is visible for the most massive and the first galaxy to form in the simulation. Clearly, further simulations are needed to establish how strict this possible relationship is between the DM and stellar core-halo profile as a potential observational discriminator. Furthermore, we observe the anticipated asymmetry for DM due to the solitons motion (jumping and random walk), a distinctive characteristic not found in the symmetric distributions of stars in the warm and CDM models.
Dark matter
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University of the Basque Country UPV/EHU, Department of Theoretical Physics, Bilbao, E-48080, Spain
DIPC, Basque Country UPV/EHU, San Sebastian, E-48080, Spain
Center for Astrophysics
Department of Astrophysical Sciences, Princeton University, 4 Ivy Lane, Princeton, 08544, NJ, United States
Lawrence Livermore National Laboratory, 7000 East Ave, Livermore, 94550, CA, United States
Ikerbasque, Basque Foundation for Science, Bilbao, E-48011, Spain
Hong Kong University of Science and Technology, Institute for Advanced Study and Department of Physics, IAS TT & WF Chao Foundation Professor, Hong Kong
Energetic Cosmos Laboratory, Nazarbayev University, Nursultan, Kazakhstan
Paris Centre for Cosmological Physics, APC, AstroParticule et Cosmologie, Université de Paris, CNRS/IN2P3, CEA/lrfu, Université Sorbonne Paris Cité, 10, Rue Alice Domon et Leonie Duquet, Paris, 75205 Cedex 13, France
Physics Department & LBNL, University of California at Berkeley, Emeritus, Berkeley, 94720, CA, United States
Department of Physics, Kavli Institute for Astrophysics and Space Research, Massachusetts Institute of Technology, Cambridge, 02139, MA, United States
Black Hole Initiative, Harvard University, 20 Garden Street, Cambridge, 02138, MA, United States
University of the Basque Country UPV/EHU
DIPC
Center for Astrophysics
Department of Astrophysical Sciences
Lawrence Livermore National Laboratory
Ikerbasque
Hong Kong University of Science and Technology
Energetic Cosmos Laboratory
Paris Centre for Cosmological Physics
Physics Department & LBNL
Department of Physics
Black Hole Initiative
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