2019
DOI: 10.1103/physrevlett.123.141301
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First Star-Forming Structures in Fuzzy Cosmic Filaments

Abstract: In hierarchical models of structure formation, the first galaxies form in low-mass dark matter potential wells, probing the behavior of dark matter on kiloparsec (kpc) scales. Even though these objects are below the detection threshold of current telescopes, future missions will open an observational window into this emergent world. In this Letter we investigate how the first galaxies are assembled in a 'fuzzy' dark matter (FDM) cosmology where dark matter is an ultralight ∼ 10 −22 eV boson and the primordial … Show more

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Cited by 160 publications
(141 citation statements)
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“…Thus, the box size for a cosmological simulation is limited to a few comoving Mpc for a resolution of 1024 3 . This limits applications of spectral methods to systems with low values of maximal velocities, such as low-mass first galaxies (in haloes of mass < 10 11 M ), such as the work presented by Mocz et al (2019) and the one here. Due to the resolution requirements we stop our simulations at z = 5.5.…”
Section: Discussion Of Various Numerical Approaches For Becdm and Thementioning
confidence: 94%
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“…Thus, the box size for a cosmological simulation is limited to a few comoving Mpc for a resolution of 1024 3 . This limits applications of spectral methods to systems with low values of maximal velocities, such as low-mass first galaxies (in haloes of mass < 10 11 M ), such as the work presented by Mocz et al (2019) and the one here. Due to the resolution requirements we stop our simulations at z = 5.5.…”
Section: Discussion Of Various Numerical Approaches For Becdm and Thementioning
confidence: 94%
“…As a result, such dark matter is expected to form solitonic cores (rather than cusps) in galaxy centers and render fewer dwarf galaxies than what is predicted for ΛCDM (Hu, Barkana & Gruzinov 2000;Goodman 2000;Guzmán & Matos 2000;Matos & Arturo Ureña-López 2001;Hui et al 2017). Furthermore, filaments, and not necessarily haloes as in ΛCDM, are the sites of primordial star formation in BECDM (Hirano, Sullivan & Bromm 2017;Mocz et al 2019), in a similar way to how the same process occurs in WDM models (Yoshida et al 2003b;Gao & Theuns 2007). Finally, due to the quantum nature of BECDM, the cosmic web exhibits interference patterns Mocz et al 2019).…”
Section: Introductionmentioning
confidence: 92%
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