Introduction to Dark Matter

We show that for parameters consistent with Standard Model measurements and Planck observation results lead to MPBH ∊ (10−16, 10−15) M⊙ primordial black holes with significant abundance, which may consist the majority of dark matter.

Alternatively, primordial black holes as dark matter could also form binaries in the late universe due to dynamical encounters and gravitational-wave braking.

The first bright objects to form in the Universe might not have been "ordinary" fusion-powered stars, but "Dark Stars" (DSs) powered by the annihilation of dark matter (DM) in the form of Weakly Interacting Massive Particles (WIMPs).

Although it is usually thought that a class of weakly interacting massive particle (WIMP) dark matters (DMs), which have the vector coupling with the Z boson, is denied by null results of the direct DM searches, such WIMP DMs are still viable if they are superheavy with the mass of mDM & 10 9 GeV.

We devise a novel mechanism and for the first time illustrate that the Higgs model in particle physics can drive the inflation to satisfy cosmic microwave background observations and simultaneously enhance the curvature perturbations at small scales to explain the abundance of dark matter in our universe created in the form of primordial black holes.

We perform the first test of Dark Matter (DM) stress-energy evolution through cosmic history, using Cosmic Microwave Background measurements supplemented with Baryon Acoustic Oscillation data and the Hubble Space Telescope key project data.

This, together with the intrinsic radiopurity of its constituting elements, offers advantages for noble gas and liquid based time projection chambers, used for dark matter searches and neutrino experiments.

The LZ collaboration aims to directly detect dark matter by using a liquid xenon Time Projection Chamber (TPC).

In astroparticle, nuclear and subnuclear physics, low-counting experiments play an increasingly important role in the investigation of rare processes such as dark matter, double beta decay, some neutrino processes and low-background spectrometry.

Examples include direct dark matter detection, neutrinoless double beta decay, and searches for permanent electric dipole moments of the neutron and atoms.

The implication of J/ψ → γ + invisible for the effective field theories of neutrino and dark matter Tong Li,1, ∗ Xiao-Dong Ma,2, † Michael A.

The Effective Field Theory of Large-Scale Structure (EFTofLSS) provides a consistent way to predict the clustering of dark matter and baryons on large scales, where their leading corrections in perturbation theory are given by a simple and calculable functional form even after the onset of baryonic processes.

We take interacting scenario of dark energy and dark matter with three cutoffs like Granda–Oliveros, higher order derivative of Hubble parameter and generalized holographic dark energy model.

In this scenario, the interaction Γ between the Barrow holographic dark energy model (whose infrared cutoff scale is set by Hubble and event horizons) and pressureless dark matter are considered.

We analyze neutrino mass matrix, lepton flavor violating processes, electron/muon g − 2 and dark matter annihilation cross section which are induced via interactions among Standard Model leptons and particles in U ( 1 ) X hidden sector, and their interactions can be sizable in our scenario.

The mission would have a broad impact on astroparticle physics, but the primary science drivers for the mission include: (1) probing WIMP dark matter across the entire natural mass range and annihilation cross section for a thermalWIMP, (2) providing a nearly all-sky instantaneous FoV, with prompt sub-degree localization and polarization measurements for gamma-ray transients such as neutron-star mergers and (3) making measurements of rare utraheavy cosmic ray nuclei to distinguish between n-star merger and SNae r-process synthesis of the heavy elements.

We present cross-section expectations for various processes and collider options, for benchmark scenarios of the Inert Doublet Model, a Two Higgs Doublet Model with a dark matter candidate.

The Inert Doublet Model is one of the simplest extensions of the Standard Model, providing a dark matter candidate.

In the latter, dark matter and dark energy, governing the large-scale structure and the cosmological evolution, seem to escape from any final fundamental theory and detection.

The Ly-α forest is the large-scale structure probe for which we appear to have modeling control to the highest wavenumbers, which makes it of great interest for constraining the warmness/fuzziness of the dark matter and the timing of reionization processes.

The framework successfully generates eV masses of the light neutrinos via seesaw mechanism, and accommodates a feebly interacting massive particle (FIMP) as dark matter candidate.

Feebly Interacting Massive Particles (FIMPs) are dark matter candidates that never thermalize in the early universe and whose production takes place via decays and/or scatterings of thermal bath particles.

Ultralight axion like particles (ALPs) of mass ma ∈ (10−21eV − 10−22eV) with axion decay constant fa ∼ 1017GeV can be candidates for fuzzy dark matter (FDM).

The SU(5) breaking also triggers the breaking of the PQ symmetry, resulting in axion dark matter (DM), with the axion decay constant fa of order MGUT or somewhat larger.

While LERGs dominate among most massive galaxies with the largest black holes and HERGs dominate at high specific star formation rates, they otherwise largely populate similar-sized dark matter halos and have similar host galaxy properties.

We further investigate the variation of the CCF using subsamples divided by dark matter halo mass (M DH), galaxy stellar mass (M ⋆), and star formation rate (SFR) and find that the CCF signal becomes stronger with increasing M DH, M ⋆, and SFR.

Many non-minimal dark matter scenarios lead to oscillatory features in the matter power spectrum induced by interactions either within the dark sector or with particles from the standard model.

At the level of Dark Matter (DM), we show that COLA accurately reproduces the matter power spectrum up to k ∼ 1 h Mpc-1, while it is less accurate in reproducing the velocity field.

Using a set of high-resolution simulations we study the statistical correlation of dark matter halo properties with the large-scale environment.

Both simulation and observational data have shown that the spin and shape of dark matter halos are correlated with their nearby large-scale environment.

Assuming no deviation from a source gamma-ray emission due to accelerated electron inverse-Compton scattering, higher event energies can extend constraints on the effects of new physics; we consider oscillation between gamma rays and axions, plus attenuation effects from gamma-ray absorption in the case of dark photon dark matter.

Gamma-ray emission is expected in galaxy clusters both from interactions of cosmic rays (CR) with the intra-cluster medium, or as a product of annihilation or decay of dark matter (DM) particles in case they are weakly interactive massive particles (WIMPs).

This standard model involves two dark components of the universe, dark energy and dark matter.

This standard model involves two dark components of the universe, dark energy and dark matter.

In the standard Lambda cold dark matter paradigm, pure dark matter simulations predict dwarf galaxies should inhabit dark matter haloes with a centrally diverging density `cusp'.

023)  × 10−10 we have calculated using this approach is about four times lower than that estimated using the standard lambda cold dark matter (ΛCDM) cosmological model, and is consistent with the most agreed observational value of 1.

We briefly review the status of keV-scale sterile neutrinos as dark matter and the possibility of explaining the matter-antimatter asymmetry of the Universe through leptogenesis driven by yet heavier sterile neutrinos.

These developments started the era of precision Cosmic Ray physics providing access to a rich program of high-energy astrophysics addressing fundamental questions like matter-antimatter asymmetry, indirect detection for Dark Matter and the detailed study of origin, acceleration and propagation of CRs and their interactions with the interstellar medium.

To this end, we use the framework of Rastall gravity (RG) and universe is assumed to be consists of interacting/ non-interacting dark energy (DE) and dark matter (DM).

In this work, we investigate the dynamics of the interacting dark energy and dark matter in viable models of f(R) gravity by using a standard framework of dynamical system analysis.

In this work, we investigate the beyond standard model (BSM) impact of leptophilic U(1) models, namely $U(1{)}_{{L}_{\ensuremath{\mu}}\ensuremath{-}{L}_{e}}$, $U(1{)}_{{L}_{e}\ensuremath{-}{L}_{\ensuremath{\tau}}}$ and $U(1{)}_{{L}_{\ensuremath{\mu}}\ensuremath{-}{L}_{\ensuremath{\tau}}}$ on coherent elastic neutrino-nucleus scattering ($\mathrm{CE}\ensuremath{\nu}\mathrm{NS}$) and hence its effect on dark matter (DM) direct detection experiments.

Particle detectors based on liquid argon are now recognised as an attractive technology for dark matter direct detection and coherent elastic neutrino-nucleus scattering measurement.

In light of these two recent appealing scenarios, we consider here an interacting dark matter-dark energy model with a non-zero spatial curvature component and a freely varying dark energy equation of state in both the quintessential and phantom regimes.

In this work we propose a new coupled generalized three-form dark energy model, in which dark energy are represented by a three-form field and dark matter are represented by point particles that can be regarded as dust.

The WIMP proposed here yields the observed abundance of dark matter, and is consistent with the current limits from direct detection, indirect detection, and collider experiments, if its mass is GeV/c 2.

GeV-scale dark matter is an increasingly attractive target for direct detection, indirect detection, and collider searches.

Neutrino mass and dark matter are the two leading questions in science, which require the new physics beyond the conventional standard model [1].

Dark matter is a milestone in the understanding of the Universe and a portal to the discovery of new physics beyond the Standard Model of particles.

The topological hypothesis has potential to explain dark matter, dark energy, and electromagnetic-gravitational union.

The topological hypothesis has potential to explain dark matter, dark energy, and electromagnetic-gravitational union.

A search for dark matter particles is performed using events with a Z boson candidate and large missing transverse momentum.

A search for dark matter particles is performed using events with a Z boson candidate and large missing transverse momentum.

The recent confirmation by the Fermilab-based Muon g-2 experiment of the (g − 2)μ anomaly has important implications for allowed particle spectra in softly broken supersymmetry (SUSY) models with neutralino dark matter (DM).

In light of the recent result of the muon g-2 experiment and the update on the test of lepton flavor universality R_{K} published by the LHCb Collaboration, we systematically study for the first time a set of models with minimal field content that can simultaneously give (i) a thermal dark matter candidate; (ii) large loop contributions to b→sℓℓ processes able to address R_{K} and the other B anomalies; (iii) a natural solution to the muon g-2 discrepancy through chirally enhanced contributions.

The predicted halo mass function, spherically averaged density, velocity dispersion, velocity anisotropy, ellipticity, prolateness, and potential profiles, as well as the abundance and number density profiles of accreted and stripped subhalos and diffuse dark matter, accurately recover the results of cosmological N-body simulations.

Several essentials that may influence the lifetime estimation have been explored, including the dark matter (DM) halo mass function (HMF), the width of the redshift bin, the growth of DM halos within each redshift bin, and the stellar mass.

R-parity conserving supersymmetric models with right-handed (RH) neutrinos are very appealing since they could naturally explain neutrino physics and also provide a good dark matter (DM) candidate such as the lightest supersymmetric particle (LSP).

The lightest neutralino, assumed to be the lightest supersymmetric particle, is proposed to be a dark matter (DM) candidate for the mass range around O(100) GeV.

Accessing enormous uncultivated microorganisms (known as microbial dark matter) in a variety of Earth environments requires accurate, nondestructive classification and molecular understanding of the microorganisms in situ and at the single-cell level, which are not feasible with the current genomics approaches.

Understanding the metabolic interactions between bacteria in natural habitat at the single-cell level and the contribution of individual cell to their functions is essential for exploring the dark matter of uncultured bacteria.

The primary objective of this model is to see if determining the observed rotation speed of galactic matter is possible, without using dark matter (halo) as a parameter.

The primary objective of this model is to see if determining the observed rotation speed of galactic matter is possible, without using dark matter (halo) as a parameter.

Over the whole range of scales considered, we expect our predictions to be accurate at the $2{{\ \rm per\ cent}}$ level for parameters in the minimal Lambda cold dark matter model and to $3{{\ \rm per\ cent}}$ when extended to dynamical dark energy and massive neutrinos.

We explore the phenomenology of scalar fields coupled to asymptotically safe quantum gravity, in light of their potential significance for dark matter, for the inflaton as well as dynamical dark energy, and in the Higgs sector in and beyond the Standard Model.

A search for dark matter is conducted in final states containing a photon and missing transverse momentum in proton-proton collisions at s $$ \sqrt{s} $$ = 13 TeV.

The results of a search for direct pair production of top squarks and for dark matter in events with two opposite-charge leptons (electrons or muons), jets and missing transverse momentum are reported, using 139 fb−1 of integrated luminosity from proton–proton collisions at √ s = 13 TeV, collected by the ATLAS detector at the Large Hadron Collider during Run 2 (2015–2018).

In recent years, the very high accuracy of telescopes and advanced facilities for computation have brought a high level of interest in cosmological problems such as the structure of galaxies (dark matter) and the apparently anomalous expansion of the universe (dark energy).

In this paper, we analyze the evolution of the universe in the TADE model and the new Tsallis agegraphic dark energy (NTADE) model by considering an interaction between dark matter and dark energy as $$Q=H(\alpha \rho _{m}+\beta \rho _{D})$$.

Moreover, combining this ${\theta}_{BAO}$ measurement at low redshift with other BAO angular scale data reported in the literature, we perform statistical analyses for the cosmological parameters of some Lambda cold dark matter (${\Lambda}$CDM) type models.

Our main findings are: (1) The splashback feature is detected at a consistent location in both the mass and galaxy profiles and its location is consistent with predictions of cold dark matter N-body simulations.

We review the current status of model building for light dark matter in theories of QCD-like gauge groups in the hidden sector.

Ultra-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.

The unculturable microbial communities are referred to as “microbial dark matter” which almost covers a high percentage of the planet’s biomass and biodiversity.

Culture-independent and meta-omics sequencing methods have shed considerable light on the so-called “microbial dark matter” of Earth’s environmental microbiome, improving our understanding of phylogeny, the tree of life, and the vast functional diversity of microorganisms.

We study the structure of galactic halos within a scalar dark matter model, endowed with a repulsive quartic self-interaction, capable of undergoing the superfluid phase transition in high-density regions.

Finally, we apply these results to present analytical vacuum stability conditions for vacuum stability for $\mathbb{Z}_3$ scalar dark matter.

The SU(5) breaking also triggers the breaking of the PQ symmetry, resulting in axion dark matter (DM), with the axion decay constant fa of order MGUT or somewhat larger.

Our computation retains the information of perturbed velocities for individual axion components, opening a new avenue for setting up initial conditions for future axion dark matter simulations.

We study the possibility that (nearly) totally dissipative self-interacting dark matter (tdSIDM)–in rare, high density dark matter fluctuations in the early Universe — produces SMBH seeds through catastrophic collapse.

Self-interacting dark matter is known to be one of the most appropriate candidates for dark matter.

We use a semi-analytic model with suppressed initial power spectra to obtain the UV Luminosity Function in thermal Warm Dark Matter and sterile neutrino cosmologies.

In the light of the recently observed XENON1T electronic recoil (ER) data, we investigate the possibility of constraining the parameter space of a generic fermionic warm dark matter (WDM), decaying into a standard model (SM) neutrino and a photon.

This novel detector will search for ultralight dark matter, test quantum mechanics in new regimes, and serve as a technology pathfinder for future gravitational wave detectors in a previously unexplored frequency band.

The next generation of ultralight dark matter (DM) direct detection experiments, which could confirm sub-eV bosons as the dominant source of DM, will feature multiple detectors operating at various terrestrial locations.

We model the 21 cm power spectrum across the Cosmic Dawn and the Epoch of Reionization (EoR) in fuzzy dark matter (FDM) cosmologies.

Ultralight axion like particles (ALPs) of mass ma ∈ (10−21eV − 10−22eV) with axion decay constant fa ∼ 1017GeV can be candidates for fuzzy dark matter (FDM).

Fourth and fifth assumptions are helpful in understanding current galactic dark matter and flat rotation speeds.

In this work, we study the potential of the Cherenkov Telescope Array (CTA) for the detection of Galactic dark matter (DM) subhalos.

We demonstrate that the perturbations of strongly lensed images by low-mass dark matter subhaloes are significantly impacted by the concentration of the perturbing subhalo.

DAMIC-M (Dark Matter in CCDs at Modane) is a near-future experiment aiming to search for low-mass dark matter particles through their interactions with silicon atoms in the bulk of chargecoupled devices (CCDs).

This paper aims to put constraints on the parameters of the Scalar Field Dark Matter (SFDM) model, when dark matter is described by a free real scalar field filling the whole universe, plus a cosmological constant term.

Scalar Field Dark Matter (SFDM) comprised of ultralight bosons has attracted great interest as an alternative to standard, collisionless Cold Dark Matter (CDM) because of its novel structure-formation dynamics, described by the coupled Schrödinger-Poisson equations.

Taking all the constraints into account, we identify parameter space where the dark baryon can be a viable dark matter candidate and discuss promising avenues for probing it.

25 GeV/n) are a compelling, mostly uncharted channel of many viable dark matter models and benefit from highly suppressed astrophysical background.

Water nanoclusters (section ‘Water nanoclusters’) offer a hypothetical scenario connecting major mysteries of our Universe: dark matter (section ‘Baryonic dark matter’), dark energy (section ‘Dark energy’), cosmology (section ‘Cosmology’), astrobiology (section ‘Astrobiology’) and the RNA world (section ‘The RNA world’) as the origin of life on Earth and habitable exoplanets.

Therefore, we need non-baryonic dark matter to comprise the universe.

A classically scale-invariant scalar singlet can be a MeV-scale dark matter, with a feeble Higgs portal coupling at O(10−10).

GeV-scale dark matter is an increasingly attractive target for direct detection, indirect detection, and collider searches.