Artykuły w czasopismach: „Ultra Light Axion Dark Matter (ULADM)”

1

Chakrabarti, Sayan, Bihag Dave, Koushik Dutta i 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, nr 09 (1.09.2022): 074. http://dx.doi.org/10.1088/1475-7516/2022/09/074.

Pełny tekst źródła

Streszczenie:

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.

Style APA, Harvard, Vancouver, ISO itp.

2

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.

Pełny tekst źródła

Streszczenie:

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.

Style APA, Harvard, Vancouver, ISO itp.

3

Sabiu, Cristiano G., Kenji Kadota, Jacobo Asorey i Inkyu Park. "Probing ultra-light axion dark matter from 21 cm tomography using Convolutional Neural Networks". Journal of Cosmology and Astroparticle Physics 2022, nr 01 (1.01.2022): 020. http://dx.doi.org/10.1088/1475-7516/2022/01/020.

Pełny tekst źródła

Streszczenie:

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.

Style APA, Harvard, Vancouver, ISO itp.

4

Berman, Gennady P., Vyacheslav N. Gorshkov i Vladimir I. Tsifrinovich. "Axionic dark matter halos in the gravitational field of baryonic matter". Modern Physics Letters A 35, nr 26 (21.08.2020): 2050248. http://dx.doi.org/10.1142/s021773232050248x.

Pełny tekst źródła

Streszczenie:

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].

Style APA, Harvard, Vancouver, ISO itp.

5

Berman, Gennady P., Vyacheslav N. Gorshkov, Vladimir I. Tsifrinovich, Marco Merkli i Xidi Wang. "Bose–Einstein condensate of ultra-light axions as a candidate for the dark matter galaxy halos". Modern Physics Letters A 34, nr 30 (28.09.2019): 1950361. http://dx.doi.org/10.1142/s0217732319503619.

Pełny tekst źródła

Streszczenie:

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.

Style APA, Harvard, Vancouver, ISO itp.

6

POLLOCK, M. D. "IS NEUTRALINO DARK MATTER POSSIBLE IN THE SUPERSTRING THEORY?" International Journal of Modern Physics D 13, nr 05 (maj 2004): 819–30. http://dx.doi.org/10.1142/s0218271804004797.

Pełny tekst źródła

Streszczenie:

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.

Style APA, Harvard, Vancouver, ISO itp.

7

Castillo, Andrés, Jorge Martin-Camalich, Jorge Terol-Calvo, Diego Blas, Andrea Caputo, Ricardo Tanausú Génova Santos, Laura Sberna, Michael Peel i Jose Alberto Rubiño-Martín. "Searching for dark-matter waves with PPTA and QUIJOTE pulsar polarimetry". Journal of Cosmology and Astroparticle Physics 2022, nr 06 (1.06.2022): 014. http://dx.doi.org/10.1088/1475-7516/2022/06/014.

Pełny tekst źródła

Streszczenie:

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.

Style APA, Harvard, Vancouver, ISO itp.

8

Kawasaki, Masahiro, Kazuyoshi Miyazaki, Kai Murai, Hiromasa Nakatsuka i 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, nr 08 (1.08.2022): 066. http://dx.doi.org/10.1088/1475-7516/2022/08/066.

Pełny tekst źródła

Streszczenie:

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).

Style APA, Harvard, Vancouver, ISO itp.

9

Rogers, Keir K., Renée Hložek, Alex Laguë, Mikhail M. Ivanov, Oliver H. E. Philcox, Giovanni Cabass, Kazuyuki Akitsu i David J. E. Marsh. "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, nr 06 (1.06.2023): 023. http://dx.doi.org/10.1088/1475-7516/2023/06/023.

Pełny tekst źródła

Streszczenie:

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.

Style APA, Harvard, Vancouver, ISO itp.

10

Gong, Yan, Bin Yue, Ye Cao i 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, nr 1 (1.04.2023): 28. http://dx.doi.org/10.3847/1538-4357/acc109.

Pełny tekst źródła

Streszczenie:

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.

Style APA, Harvard, Vancouver, ISO itp.

11

Ivanov, M. M., Y. Y. Kovalev, M. L. Lister, A. G. Panin, A. B. Pushkarev, T. Savolainen i S. V. Troitsky. "Constraining the photon coupling of ultra-light dark-matter axion-like particles by polarization variations of parsec-scale jets in active galaxies". Journal of Cosmology and Astroparticle Physics 2019, nr 02 (28.02.2019): 059. http://dx.doi.org/10.1088/1475-7516/2019/02/059.

Pełny tekst źródła

Style APA, Harvard, Vancouver, ISO itp.

12

Ferreira, Elisa G. M. "Ultra-light dark matter". Astronomy and Astrophysics Review 29, nr 1 (9.09.2021). http://dx.doi.org/10.1007/s00159-021-00135-6.

Pełny tekst źródła

Streszczenie:

AbstractUltra-light dark matter is a class of dark matter models (DM), where DM is composed by bosons with masses ranging from $$10^{-24}\, \mathrm {eV}< m < \mathrm {eV}$$ 10 - 24 eV < m < eV . These models have been receiving a lot of attention in the past few years given their interesting property of forming a Bose–Einstein condensate (BEC) or a superfluid on galactic scales. BEC and superfluidity are some of the most striking quantum mechanical phenomena that manifest on macroscopic scales, and upon condensation, the particles behave as a single coherent state, described by the wavefunction of the condensate. The idea is that condensation takes place inside galaxies while outside, on large scales, it recovers the successes of $$\varLambda $$ Λ CDM. This wave nature of DM on galactic scales that arise upon condensation can address some of the curiosities of the behaviour of DM on small-scales. There are many models in the literature that describe a DM component that condenses in galaxies. In this review, we are going to describe those models, and classify them into three classes, according to the different non-linear evolution and structures they form in galaxies: the fuzzy dark matter (FDM), the self-interacting fuzzy dark matter (SIFDM), and the DM superfluid. Each of these classes comprises many models, each presenting a similar phenomenology in galaxies. They also include some microscopic models like the axions and axion-like particles. To understand and describe this phenomenology in galaxies, we are going to review the phenomena of BEC and superfluidity that arise in condensed matter physics, and apply this knowledge to DM. We describe how ULDM can potentially reconcile the cold DM picture with the small-scale behaviour. These models present a rich phenomenology that is manifest in different astrophysical consequences. We review here the astrophysical and cosmological tests used to constrain those models, together with new and future observations that promise to test these models in different regimes. For the case of the FDM class, the mass where this model has an interesting phenomenology on small-scales $$ \sim 10^{-22}\, \mathrm {eV}$$ ∼ 10 - 22 eV , is strongly challenged by current observations. The parameter space for the other two classes remains weakly constrained. We finalize by showing some predictions that are a consequence of the wave nature of this component, like the creation of vortices and interference patterns, that could represent a smoking gun in the search of these rich and interesting alternative class of DM models.

Style APA, Harvard, Vancouver, ISO itp.

13

Laroche, Alexander, Daniel Gilman, Xinyu Li, Jo Bovy i Xiaolong Du. "Quantum fluctuations masquerade as haloes: Bounds on ultra-light dark matter from quadruply-imaged quasars". Monthly Notices of the Royal Astronomical Society, 22.09.2022. http://dx.doi.org/10.1093/mnras/stac2677.

Pełny tekst źródła

Streszczenie:

Abstract Ultra-light dark matter (ULDM) refers to a class of theories, including ultra-light axions, in which particles with mass $m_{\psi } < 10^{-20}\, \rm {eV}$ comprise a significant fraction of the dark matter. A galactic scale de Broglie wavelength distinguishes these theories from cold dark matter (CDM), suppressing the overall abundance of structure on sub-galactic scales, and producing wave-like interference phenomena in the density profiles of haloes. With the aim of constraining the particle mass, we analyse the flux ratios in a sample of eleven quadruple-image strong gravitational lenses. We account for the suppression of the halo mass function and concentration-mass relation predicted by ULDM theories, and the wave-like fluctuations in the host halo density profile, calibrating the model for the wave interference against numerical simulations of galactic-scale haloes. We show that the granular structure of halo density profiles, in particular, the amplitude of the fluctuations, significantly impacts image flux ratios, and therefore inferences on the particle mass derived from these data. We infer relative likelihoods of CDM to ULDM of 8:1, 7:1, 6:1, and 4:1 for particle masses $\log _{10}(m_\psi /\rm {eV})\in [-22.5,-22.25], [-22.25,-22.0],[-22.0,-21.75], [-21.75,-21.5]$, respectively. Repeating the analysis and omitting fluctuations associated with the wave interference effects, we obtain relative likelihoods of CDM to ULDM with a particle mass in the same ranges of 98:1, 48:1, 26:1 and 18:1, highlighting the significant perturbation to image flux ratios associated with the fluctuations. Nevertheless, our results disfavor the lightest particle masses with $m_{\psi } < 10^{-21.5}\, \rm {eV}$, adding to mounting pressure on ultra-light axions as a viable dark matter candidate.

Style APA, Harvard, Vancouver, ISO itp.

14

Chakrabarti, Soumya. "Collapse of an axion scalar field". European Physical Journal C 81, nr 2 (luty 2021). http://dx.doi.org/10.1140/epjc/s10052-021-08930-2.

Pełny tekst źródła

Streszczenie:

AbstractThe manuscript deals with an interacting scalar field that mimics the evolution of the so-called axion scalar dark matter or axion like particles with ultra-light masses. It is discussed that such a scalar along with an ordinary fluid description can collapse under strong gravity. The end state of the collapse depends on how the axion interacts with geometry and ordinary matter. For a self-interacting axion and an axion interacting with geometry the collapse may lead to a zero proper volume singularity or a bounce and total dispersal of the axion. However, for an axion interacting with the ordinary fluid description, there is no formation of singularity and the axion field exhibits periodic behavior before radiating away to zero value. Usually this collapse and dispersal is accompanied by a violation of the null energy condition for the ordinary fluid description.

Style APA, Harvard, Vancouver, ISO itp.

15

Montero, Miguel, Julian B. Muñoz i Georges Obied. "Swampland bounds on dark sectors". Journal of High Energy Physics 2022, nr 11 (21.11.2022). http://dx.doi.org/10.1007/jhep11(2022)121.

Pełny tekst źródła

Streszczenie:

Abstract We use Swampland principles to theoretically disfavor regions of the parameter space of dark matter and other darkly charged particles that may exist. The Festina Lente bound, the analogue of the Weak-Gravity conjecture in de Sitter, places constraints on the mass and charge of dark particles, which here we show cover regions in parameter space that are currently allowed by observations. As a consequence, a broad set of new ultra-light particles are in the Swampland, independently of their cosmic abundance, showing the complementarity of Quantum Gravity limits with laboratory and astrophysical studies. In parallel, a Swampland bound on the UV cutoff associated to the axion giving a Stückelberg photon its longitudinal mode translates to a new constraint on the kinetic mixings and masses of dark photons. This covers part of the parameter space targeted by upcoming dark-photon direct-detection experiments. Moreover, it puts astrophysically interesting models in the Swampland, including freeze-in dark matter through an ultra-light dark photon, as well as radio models invoked to explain the 21-cm EDGES anomaly.

Style APA, Harvard, Vancouver, ISO itp.

16

Mocz, Philip, Anastasia Fialkov, Mark Vogelsberger, Michael Boylan-Kolchin, Pierre-Henri Chavanis, Mustafa A. Amin, Sownak Bose i in. "Cosmological structure formation and soliton phase transition in Fuzzy Dark Matter with axion self-interactions". Monthly Notices of the Royal Astronomical Society, 6.03.2023. http://dx.doi.org/10.1093/mnras/stad694.

Pełny tekst źródła

Streszczenie:

Abstract We investigate cosmological structure formation in Fuzzy Dark Matter (FDM) with an attractive self-interaction (SI) with numerical simulations. Such a SI would arise if the FDM boson were an ultra-light axion, which has a strong CP symmetry-breaking scale (decay constant). Although weak, the attractive SI may be strong enough to counteract the quantum ‘pressure’ and alter structure formation. We find in our simulations that the SI can enhance small-scale structure formation, and soliton cores above a critical mass undergo a phase transition, transforming from dilute to dense solitons.

Style APA, Harvard, Vancouver, ISO itp.

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

Utwórz poprawne odniesienie w stylach APA, MLA, Chicago, Harvard i wielu innych