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Gotowa bibliografia na temat „Ultra Light Axion Dark Matter (ULADM)”

Autor: Grafiati

Data publikacji: 6 września 2023

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Artykuły w czasopismach na temat "Ultra Light Axion Dark Matter (ULADM)"

Chakrabarti, Sayan, Bihag Dave, Koushik Dutta, and Gaurav Goswami. "Constraints on the mass and self-coupling of ultra-light scalar field dark matter using observational limits on galactic central mass." Journal of Cosmology and Astroparticle Physics 2022, no. 09 (2022): 074. http://dx.doi.org/10.1088/1475-7516/2022/09/074.

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Abstract It is well known that Ultra-Light Dark Matter (ULDM), usually scalar fields of mass m ∼ 10-22 eV, can solve some of the outstanding problems of the Cold Dark Matter (CDM) paradigm. Such a scalar field could have non-negligible self-coupling λ. In this work, using the known observational upper limit on the amount of centrally concentrated dark matter in a galaxy, we arrive at the observational constraints in the λ-m (self coupling-mass) parameter space. It is found that the observational limit on the mass m of the ULDM depends upon the sign and strength of the self-interactions. We demonstrate that, for m ∼ 10-22 eV, self-coupling values of 𝒪(10-96) (corresponding to a scattering length of as ∼ 10-82 m) can be probed using limits on the dark matter mass within 10 pc of the centre of M87 galaxy. Our analysis suggests that if Ultra Light Axion particles (ULAs) form all of dark matter, dark matter particle mass must be less than ∼ 6 × 10-23 eV.

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Lee, Jae-Weon. "Brief History of Ultra-light Scalar Dark Matter Models." EPJ Web of Conferences 168 (2018): 06005. http://dx.doi.org/10.1051/epjconf/201816806005.

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This is a review on the brief history of the scalar field dark matter model also known as fuzzy dark matter, BEC dark matter, wave dark matter, or ultra-light axion. In this model ultra-light scalar dark matter particles with mass m = O(10-22)eV condense in a single Bose-Einstein condensate state and behave collectively like a classical wave. Galactic dark matter halos can be described as a self-gravitating coherent scalar field configuration called boson stars. At the scale larger than galaxies the dark matter acts like cold dark matter, while below the scale quantum pressure from the uncertainty principle suppresses the smaller structure formation so that it can resolve the small scale crisis of the conventional cold dark matter model.

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Sabiu, Cristiano G., Kenji Kadota, Jacobo Asorey, and Inkyu Park. "Probing ultra-light axion dark matter from 21 cm tomography using Convolutional Neural Networks." Journal of Cosmology and Astroparticle Physics 2022, no. 01 (2022): 020. http://dx.doi.org/10.1088/1475-7516/2022/01/020.

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Abstract We present forecasts on the detectability of Ultra-light axion-like particles (ULAP) from future 21 cm radio observations around the epoch of reionization (EoR). We show that the axion as the dominant dark matter component has a significant impact on the reionization history due to the suppression of small scale density perturbations in the early universe. This behavior depends strongly on the mass of the axion particle. Using numerical simulations of the brightness temperature field of neutral hydrogen over a large redshift range, we construct a suite of training data. This data is used to train a convolutional neural network that can build a connection between the spatial structures of the brightness temperature field and the input axion mass directly. We construct mock observations of the future Square Kilometer Array survey, SKA1-Low, and find that even in the presence of realistic noise and resolution constraints, the network is still able to predict the input axion mass. We find that the axion mass can be recovered over a wide mass range with a precision of approximately 20%, and as the whole DM contribution, the axion can be detected using SKA1-Low at 68% if the axion mass is M X < 1.86 × 10-20 eV although this can decrease to M X < 5.25 × 10-21 eV if we relax our assumptions on the astrophysical modeling by treating those astrophysical parameters as nuisance parameters.

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Berman, Gennady P., Vyacheslav N. Gorshkov, and Vladimir I. Tsifrinovich. "Axionic dark matter halos in the gravitational field of baryonic matter." Modern Physics Letters A 35, no. 26 (2020): 2050248. http://dx.doi.org/10.1142/s021773232050248x.

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We consider a dark matter halo (DMH) of a spherical galaxy as a Bose–Einstein condensate (BEC) of the ultra-light axions (ULA) interacting with the baryonic matter. In the mean-field (MF) limit, we have derived the integro-differential equation of the Hartree–Fock type for the spherically symmetrical wave function of the DMH component. This equation includes two independent dimensionless parameters: (i) [Formula: see text] is the ratio of baryon and axion total mases and (ii) [Formula: see text] is the ratio of characteristic baryon and axion spatial parameters. We extended our “dissipation algorithm” for studying numerically the ground state of the axion halo in the gravitational field produced by the baryonic component. We calculated the characteristic size, [Formula: see text] of DMH as a function of [Formula: see text] and [Formula: see text] and obtained an analytical approximation for [Formula: see text].

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Berman, Gennady P., Vyacheslav N. Gorshkov, Vladimir I. Tsifrinovich, Marco Merkli, and Xidi Wang. "Bose–Einstein condensate of ultra-light axions as a candidate for the dark matter galaxy halos." Modern Physics Letters A 34, no. 30 (2019): 1950361. http://dx.doi.org/10.1142/s0217732319503619.

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We suggest that the dark matter halo in some of the spiral galaxies can be described as the ground state of the Bose–Einstein condensate of ultra-light self-gravitating axions. We have also developed an effective “dissipative” algorithm for the solution of nonlinear integro-differential Schrödinger equation describing self-gravitating Bose–Einstein condensate. The mass of an ultra-light axion is estimated.

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POLLOCK, M. D. "IS NEUTRALINO DARK MATTER POSSIBLE IN THE SUPERSTRING THEORY?" International Journal of Modern Physics D 13, no. 05 (2004): 819–30. http://dx.doi.org/10.1142/s0218271804004797.

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In the heterotic superstring theory, the decay constant of the QCD axion lies within the range 3×1016≲fa GeV ≲1018, the lower limit referring to the model-independent axion, while the upper limit is due to dimension-five, non-renormalizable effects first calculated by Cvetič. Consequently, the neutralino χ0, assumed to be a nearly pure B-ino, decays into the axino ã on the time scale obtained by Covi et al., [Formula: see text], which is ≲10-3 times the age of the Universe t0≈4×1017 s , but can only be made less than the time t≈1 s of the onset of Big-Bang nucleosynthesis by revising mχ0 to an unnaturally high level, mχ0≳500 TeV . Therefore, it is necessary to set the coefficient Ca YY =0, which is possible for the Kim–Shifman–Vainshtein–Zakharov invisible-axion model if the electric charge q c of the heavy-quark colour representation C vanishes. The neutralino does not then decay and can constitute some fraction of the dark matter of the Universe, depending upon the value of mχ0 (for a gaugino-dominated state, [Formula: see text] where [Formula: see text] is the SU(2) singlet slepton). The consequences of an ultra-light axion with fa≈1018 GeV are also discussed.

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Castillo, Andrés, Jorge Martin-Camalich, Jorge Terol-Calvo, et al. "Searching for dark-matter waves with PPTA and QUIJOTE pulsar polarimetry." Journal of Cosmology and Astroparticle Physics 2022, no. 06 (2022): 014. http://dx.doi.org/10.1088/1475-7516/2022/06/014.

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Abstract The polarization of photons emitted by astrophysical sources might be altered as they travel through a dark matter medium composed of ultra light axion-like particles (ALPs). In particular, the coherent oscillations of the ALP background in the galactic halo induce a periodic change on the polarization of the electromagnetic radiation emitted by local sources such as pulsars. Building up on previous works, we develop a new, more robust, analysis based on the generalised Lomb-Scargle periodogram to search for this periodic signal in the emission of the Crab supernova remnant observed by the QUIJOTE MFI instrument and 20 Galactic pulsars from the Parkes Pulsar Timing Array (PPTA) project. We also carefully take into account the stochastic nature of the axion field, an effect often overlooked in previous works. This refined analysis leads to the strongest limits on the axion-photon coupling for a wide range of dark matter masses spanning 10-23 eV ≲ ma ≲ 10-19 eV. Finally, we survey possible optimal targets and the potential sensitivity to axionic dark-matter in this mass range that could be achieved using pulsar polarimetry in the future.

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Kawasaki, Masahiro, Kazuyoshi Miyazaki, Kai Murai, Hiromasa Nakatsuka, and Eisuke Sonomoto. "Anisotropies in cosmological 21 cm background by oscillons/I-balls of ultra-light axion-like particle." Journal of Cosmology and Astroparticle Physics 2022, no. 08 (2022): 066. http://dx.doi.org/10.1088/1475-7516/2022/08/066.

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Abstract Ultra-light axion-like particle (ULAP) with mass m ∼ 10-22 eV has recently been attracting attention as a possible solution to the small-scale crisis. ULAP forms quasi-stable objects called oscillons/I-balls, which can survive up to a redshift z ∼ 10 and affect the structure formation on a scale ∼ 𝒪(0.1) Mpc by amplifying the density fluctuations. We study the effect of oscillons on 21 cm anisotropies caused by neutral hydrogen in minihalos. It is found that this effect can be observed in a wide mass range by future observations such as Square Kilometer Array (SKA) if the fraction of ULAP to the total dark matter density is 𝒪(0.01 – 0.1).

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Rogers, Keir K., Renée Hložek, Alex Laguë, et al. "Ultra-light axions and the S ₈ tension: joint constraints from the cosmic microwave background and galaxy clustering." Journal of Cosmology and Astroparticle Physics 2023, no. 06 (2023): 023. http://dx.doi.org/10.1088/1475-7516/2023/06/023.

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Abstract We search for ultra-light axions as dark matter (DM) and dark energy particle candidates, for axion masses 10-32 eV ≤ m a ≤ 10-24 eV, by a joint analysis of cosmic microwave background (CMB) and galaxy clustering data — and consider if axions can resolve the tension in inferred values of the matter clustering parameter S 8. We give legacy constraints from Planck 2018 CMB data, improving 2015 limits on the axion density Ωa h 2 by up to a factor of three; CMB data from the Atacama Cosmology Telescope and the South Pole Telescope marginally weaken Planck bounds at m a = 10-25 eV, owing to lower (and theoretically-consistent) gravitational lensing signals. We jointly infer, from Planck CMB and full-shape galaxy power spectrum and bispectrum data from the Baryon Oscillation Spectroscopic Survey (BOSS), that axions are, today, < 10% of the DM for m a ≤ 10-26 eV and < 1% for 10-30 eV ≤ m a ≤ 10-28 eV. BOSS data strengthen limits, in particular at higher m a by probing high-wavenumber modes (k < 0.4h Mpc-1). BOSS alone finds a preference for axions at 2.7σ, for m a = 10-26 eV, but Planck disfavours this result. Nonetheless, axions in a window 10-28 eV ≤ m a ≤ 10-25 eV can improve consistency between CMB and galaxy clustering data, e.g., reducing the S 8 discrepancy from 2.7σ to 1.6σ, since these axions suppress structure growth at the 8h -1 Mpc scales to which S 8 is sensitive. We expect improved constraints with upcoming high-resolution CMB and galaxy lensing and future galaxy clustering data, where we will further assess if axions can restore cosmic concordance.

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Gong, Yan, Bin Yue, Ye Cao, and Xuelei Chen. "Fuzzy Dark Matter as a Solution to Reconcile the Stellar Mass Density of High-z Massive Galaxies and Reionization History." Astrophysical Journal 947, no. 1 (2023): 28. http://dx.doi.org/10.3847/1538-4357/acc109.

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Abstract The JWST early release data show unexpected high stellar mass densities of massive galaxies at 7 < z < 11. A high star formation efficiency is probably needed to explain this. However, such a high star formation efficiency would greatly increase the number of ionizing photons, which would be in serious conflict with current cosmic microwave background (CMB) and other measurements of cosmic reionization history. To solve this problem, we explore fuzzy dark matter (FDM), which is composed of ultra-light scalar particles, e.g., ultra-light axions, and calculate its halo mass function and stellar mass density for different axion masses. We find that a FDM model with m a ≃ 5 × 10−23 eV and a possible uncertainty range ∼3 × 10−23–10−22 eV can effectively suppress the formation of small halos and galaxies, so that with higher star formation efficiency both the JWST data at z ∼ 8 and the reionization history measurements from optical depth of CMB scattering and ionization fraction can be simultaneously matched. We also find that the JWST data at z ∼ 10 are still too high to fit in this scenario. We note that the estimated mean redshift of the sample may have large uncertainty, that it can be as low as z ∼ 9 depending on adopted spectral energy distribution templates and photometric-redshift code. In addition, warm dark matter with ∼keV mass can also be an alternative choice, since it should have similar effects on halo formation as FDM.

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