claims depot shelf
Dark Matter
Formal claims (Lean)
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In the sub-EeV scenario, the hidden monopoles from the breaking $SU(2)_d\to U(1)_d$ have mass $m_M\sim 4\pi T_p\sim 10^{10}$ GeV, and their number density after bubble collisions is $n_M = p\,n_b$ with $p\sim 0.1$; this yields a relic density that can account for the observed dark matter. The interaction with the axion, the Witten effect, is controlled by the coupling $\mathcal{L}_\theta = -e'^2/(
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On the paper's own terms, the central discovery is that the field equations of phantom scalar-field cosmologies with dark-matter interactions allow a normalization $D = \sqrt{\tfrac12\dot{\phi}^2 + V + \rho_m}$ such that the dimensionless state variables $\chi$, $\zeta$, $\xi$ lie on the unit sphere and the first Friedmann constraint closes the system, giving a compact two-dimensional phase space
Stated claims
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The paper's central claim is that, even under deliberately optimistic assumptions, capture-driven accumulation of non-annihilating (asymmetric) fermionic dark matter in a cold, non-rotating neutron star cannot produce observable gravitational-wave signatures. Using a three-layer polytropic equation of state for baryons, a zero-temperature degenerate Fermi gas for the dark component, and the coupled two-fluid Tolman–Oppenheimer–Volkoff equations, the authors evolve the star through a sequence of hydrostatic equilibria connected by the capture rate. With a canonical Galactic halo ($\rho_{\mathrm{halo}}=0.3\,\mathrm{GeV}/\mathrm{cm}^3$) the tidal response barely changes over a Hubble time; in the maximized scenario—a dark-matter spike with $\rho_{\mathrm{halo}}=2.2\times10^9\,M_\odot/\mathrm{pc}^3$ and $v_{\mathrm{ns}}=30\,\mathrm{km/s}$—the total mass reaches at most $M_{\mathrm{tot,max}}\approx1.4484\,M_\odot$, the compactness rises by a few tens of percent, and the tidal observables shift by $|\Delta k_2|\sim10^{-2}$ and $|\Delta\Lambda|\sim10^1$. The stars remain on the stable TOV branch, so dark-matter accumulation does not trigger collapse. The conclusion is that asymmetric dark matter alone, via capture, is unlikely to be detectable in current or near-future gravitational-wave observations of neutron stars.
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The paper constructs static, spherically symmetric black holes dressed with anisotropic dark-matter halos modeled as Einstein clusters with generalized $(\alpha,\beta,\gamma)$ density profiles, and studies their axial gravitational perturbations. It shows that the entire ringdown spectrum is a uniformly redshifted Schwarzschild spectrum, $\omega_{\mathrm{DM}} = e^{-I/2} \omega_{\mathrm{Sch}}$, where $I$ is the halo redshift integral of Eq. (46) built from the enclosed halo mass outside the light ring. Because the same factor multiplies the real and imaginary parts, the fractional shifts of the oscillation frequency and the damping rate are equal and coincide with the shifts of the light-ring frequency and Lyapunov exponent. The paper also derives the static axial tidal Love number to leading order in halo compactness, finding $\kappa_l \propto \int m_h'(r) r^{2l}\,dr$; for $l=2$ this is $(4\pi/5)\int \bar\rho(r) r^6\,dr$, dominated by the outermost halo and the truncation radius. Since the ringdown shift is inner-weighted and the tidal response outer-weighted, the two observables break the compactness-shape degeneracy.
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The paper's central discovery is that the conditional probability $P^{\rm Lens}_{\rm GC}(\tau_{\rm GC}|\tau_{\rm halo})$ — the fraction of galaxy-scale strongly lensed gravitational-wave events that would also be distorted by an IMBH in a globular cluster — is suppressed to the range $10^{-4}$ to $10^{-2}$ depending on the magnification threshold, with the fiducial sub-second time-delay criterion yielding $\lesssim 10^{-3}$. The suppression is geometric and robust: most of the optical depth comes from clusters near the main halo's critical curves, where the external convergence and shear reshape the caustics, and the sub-second delay requirement cuts the rate by about an order of magnitude relative to a tens-of-minutes threshold. Applying this rate as an astrophysical prior to GW231123 gives a Bayes factor of $1/166$ and an odds ratio of $2.80\times10^{-12}$ against the IMBH+GC lensing hypothesis, even though GW231123 is the strongest lensing candidate seen so far. The authors therefore state that lensed GWs are unlikely to be confused with known astrophysical potentials and can serve as clean probes of sub-galactic dark-matter substructure and PBHs.
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On its own terms, the paper's central claim is that SKA-Mid AA4 will change HI rotation-curve studies from a small, heterogeneous enterprise into a statistical and cosmic-time machine. Three capabilities are forecast: targeted observations at about 1–2 arcsec resolution can resolve the inner rising parts of rotation curves and measure dark-matter core properties in dwarf galaxies; a wide or pointed survey can spatially resolve the HI kinematics of roughly twenty thousand galaxies across environments from clusters to voids; and a very deep, roughly 10,000-hour, Band-1 pencil-beam survey can place five or more independent resolution elements across the major axes of galaxies with HI mass near $10^{10}$ solar masses at $z\simeq1$. The paper connects these capabilities to the empirical dynamical laws of galaxies—the baryonic Tully-Fisher relation, the central density relation, and the radial acceleration relation—and notes that particle dark matter and modified gravity predict opposite behaviors for the intrinsic scatter, redshift evolution, and environmental residuals of these laws. It concludes that discriminating between those predictions is what would allow the dark matter problem to be closed.
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The central claim is that destructive interference is not a limitation but the operating point: with the two spin-wave paths balanced to cancel, the axion's tiny phase difference becomes a first-order amplitude change rather than a tiny perturbation on a large carrier. The axion field, acting through an effective magnetic field on the electron spin, shifts the spin-wave frequency and therefore the accumulated phase along each arm; the unequal arm lengths make the two phase shifts differ. The resulting magnetization oscillates at the sideband frequencies $\omega\pm\omega_a$, with amplitude proportional to the axion-electron coupling $g_{ae}$, and this oscillation can radiate electromagnetic power or induce a voltage in a pickup coil. The paper derives SNR formulas for linear-amplifier, single-photon, and inductive readouts and reports exclusion limits at SNR=3 spanning axion masses $10^{-8}$ to $10^{-6}$ eV, with an array of $10^9$ interferometers improving the projected reach.
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Within the Inert Doublet Model, the paper's central claim is that dark matter can be probed indirectly through charged Higgs pair production at future multi-TeV muon colliders, with statistical significance passing the 5σ discovery threshold for several benchmark points that survive all current constraints. The discovery channel is μ−μ+ → νμν̄μH±H∓, followed by H± → W±H, where H is the stable dark matter scalar and the W bosons decay hadronically, semileptonically, or leptonically. After applying a machine-learning classifier to kinematic distributions, the authors obtain significance as high as Z ≈ 74 at √s = 14 TeV with 20 ab−1 (BP7, semileptonic channel), and Z > 5 for BP6, BP7, BP8 across multiple channels and energies, while BP4 and BP5 generally remain below 5σ. The machine-learning analysis is the key lever: it reduces the Standard Model background so much that marginal cut-based significances become discovery-level.
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Working with spherically symmetric metrics that solve the Einstein equations for an SFDM soliton core and an NFW cusp, the paper finds that the halo pushes the photon sphere in opposite directions: SFDM moves it outward ($r_{\rm ph}/M = 3.0485$ for Sgr A*, $3.0613$ for M87*) while CDM moves it inward ($2.9397$ and $2.9637$), compared with $3$ for the vacuum case. The resulting shadow diameters are $49.81$-$53.16\,\mu$as for Sgr A* and $38.63$-$40.74\,\mu$as for M87*, all within $1.2\sigma$ of the measured values ($48.7\pm7.0$ and $42.0\pm3.0\,\mu$as). The best fits are CDM for Sgr A* ($+0.16\sigma$) and SFDM for M87* ($-0.42\sigma$), but the inter-model differences are only a few microarcseconds. In the caustic analysis, the dimensionless point-mass strength $\kappa_P$ for M87* ($2.0\times10^{-4}$ to $3.0\times10^{-4}$) sits near or above the critical threshold $\kappa_{\rm crit}$ ($2.71\times10^{-4}$ for CDM, $2.58\times10^{-4}$ for SFDM), while Sgr A* ($1.0\times10^{-4}$ to $1.5\times10^{-4}$) stays below it; hence the paper predicts tangential-only critical curves for M87* and both critical curve types for Sgr A*.
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The central claim is that unbound (hyperbolic) PBH-SMBH encounters produce signals too weak and too rare to be detected by LISA or µAres. The abstract states: 'Comparing these results to plausible central halo densities, we find that unbound PBHs are unlikely to yield detectable signals.' Section 6 states: 'This analysis yields a very pessimistic assessment of the ability of gravitational wave signals generated by their interactions with SMBHs to put useful bounds on a possible PBH population.' If correct, this channel cannot be used to detect or constrain PBH dark matter with these detectors.
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The authors' central claim is that the dark-matter parameter of the DMPF metric leaves an observable imprint on two-flavor neutrino oscillations only for non-radial, lensed trajectories. For pure radial motion the metric factors $A B = 1$ cancel, so the phase reduces to $\Phi_k \simeq m_k^2 (r_D-r_S)/(2E_0)$ and matches flat spacetime. For neutrinos deflected by the black hole, the weak-field phase integral gives Eq. (44), $\Phi_k \simeq \frac{m_k^2}{2E_0}(r_S+r_D)\left[1 - \frac{b^2}{2r_S r_D} + \frac{2M}{r_S+r_D} + \frac{a}{r_S+r_D}\ln\frac{r_S r_D}{M^2}\right]$, so $a$ enters both the coefficient of the mass-difference term and the total phase. Feeding this phase into the two-flavor transition probability produces oscillation curves that depend on $a/M$, and the numerical analysis shows a degeneracy between the lens mass $M$ and $a$: different pairs $(M,a)$ can give the same transition probability. The wave-packet treatment adds the claim that the absolute neutrino mass, not $a$, controls the decoherence length.
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The paper's central result, stated in the abstract, is that for scalar dark matter masses smaller than about 3e-8 eV down to the smallest allowed mass of about 1e-21 eV, only 9% to 54% of the total neutrino mass can arise from the coupling to the background scalar, so a purely scalar-induced neutrino mass is excluded. The supporting quantitative claim is the set of 3-sigma upper bounds on sin^2 eta in Table 2, with the strongest bound sin^2 eta < 0.09 (T2K plus RENO, regime 2) and the projected JUNO six-year sensitivity sin^2 eta < 0.014 in regime 2.
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On the paper's own terms, the discovery is that the coexistence of a neutron star with an Einasto dark-matter halo whose radial pressure satisfies $p_r^{(d)}=-\rho_d c^2$ produces, for a range of halo parameters, a static, spherically symmetric spacetime in which $g_{rr}^{-1}=1-2G m_{\rm all}/(c^2 r)$ changes sign outside the stellar surface while the neutron star solution continues to exist as a regular interior configuration. The region of negative $g_{rr}^{-1}$ is bounded by an inner and outer horizon, and the star is fully contained within it; the paper calls this a 'neutron star in a black hole.' It occurs for two different equations of state and is not tied to a specific EOS. The paper also maps the three solution regimes—ordinary dark-matter admixed neutron star, neutron star in a black hole, and no static solution—in slices of the Einasto parameter space and reports that at horizon-forming densities the dark matter mass is comparable to the neutron star mass.
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On its own terms, the paper's central discovery is that rotating a singular Schwarzschild-like seed immersed in a Dehnen (1,4,γ) dark matter halo produces a spacetime whose curvature invariants stay finite at r=0 whenever γ≤2, so rotation plus the halo removes the essential singularity present in the static seed. The same construction yields a complete scalar spectroscopy: a hydrogen-like quasibound spectrum with an imaginary correction proportional to [m ξ(rh) − a mℓ]/(2κ), a superradiant amplification factor that is positive only below ω = mℓΩH, and a thermal extraction spectrum W(ω) = Z(ω) $ω^{4}$/($T^{3}$($e^{{ω/T}}$−1)) up to normalization. Dark matter enters through the combination ρ0 $r0^{3}$ and the inner slope γ: larger values bind quasibound states more tightly, shorten their lifetimes, narrow the superradiant window, and suppress thermal energy extraction.
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The central claim is that thermal relaxation of an axion field is not a single number, an abundance, but a momentum-resolved partition. The optical depth $\tau_x = \int dN \, \gamma_x(N)$ sets simultaneously the survival of the coherent mode, $|A_x/A_{x,i}|^2 = e^{-\tau_x}$, and the growth of stochastic occupation, $n_x = (1-e^{-\tau_x}) n_B(x)$; hence $n_x/n_B(x) + |A_x/A_{x,i}|^2 = 1$. Because the thermal bath has finite spatial and temporal correlation scales, the optical depth decreases with momentum, so high-momentum modes are suppressed; the relic is therefore subthermal in every increasing kinematic moment, in particular mean momentum and free-streaming length. In the benchmark, the stochastic population gives the observed dark matter abundance with $m_a \approx 2.8 \times 10^{2}$ keV, a coherent fraction $f_{\rm coh} = 1.2 \times 10^{-5}$, and a free-streaming wavenumber $k_{\rm fs} \approx 3 \times 10^{4}$ Mpc$^{-1}$, so dark matter is predominantly stochastic rather than misaligned.
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The central claim is that the photo-3x2-pt data vector, built from the same photometric galaxy catalog that supplies the shear sample, constrains $S_8$ to $0.76 \le S_8 \le 0.81$ at 68% credibility. This interval overlaps the results of the HSC-Y3 cosmic shear studies but is about 25% narrower. The improvement is attributed to the added sensitivity to the two nuisance parameters that dominate shear-only errors: the intrinsic alignment amplitude, which the galaxy-shear spectra help pin down, and the shift parameters of the source redshift distributions, which the galaxy clustering auto-spectra effectively self-calibrate. The paper also reports that the measured B-mode power spectra are consistent with zero, and that mock-catalog inferences recover unbiased values of $S_8$, intrinsic alignment parameters, galaxy clustering bias, and redshift shift parameters.
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The central discovery is a new inference criterion: the true Galactic potential is the one that minimizes the trace or determinant of the position covariance matrix of an expanding young stellar association when its member orbits are integrated backward to birth. The same observed present-day positions and velocities are used in every trial potential; only the potential changes. In the true potential the members reconverge to the most compact configuration, and the time of that minimum is the dynamical traceback age. With near-future data the minimum-trace criterion can distinguish halo masses, concentrations, and disk masses, though with strong degeneracies; the determinant is sharper for true three-dimensional focusing but noisier. A second, complementary route infers the potential by requiring the dynamical traceback age to match an independently measured stellar age.
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The paper shows that an excited dark matter component $\chi_2$ that is stable, or nearly stable, in vacuum can decay at observable rates near ordinary matter. Ordinary nucleons source a classical scalar field that either shifts the dark-state masses or induces kinetic mixing between a heavy $Z'$ and the photon. With benchmark parameters $g_\chi = 10^{-22}$, $m_{Z'} = 200$ GeV, and a 300 GeV vacuum mass splitting, the mass-shift scenario gives $\tau(\chi_2 \to \chi_1 Z') \approx 1.5 \times 10^{18}$ s; with $\varepsilon \approx 10^{-20}$, $m_{Z'} = 1$ TeV, and the same splitting, the kinetic-mixing scenario gives $\tau(\chi_2 \to \chi_1 \mu^+\mu^-) \approx 8 \times 10^{19}$ s. These lifetimes correspond to event rates of roughly one to ten dimuon events per cubic kilometer per year at the local dark matter density, and the paper computes that the muon pairs emerge with broad opening angles and energies of order 100 GeV or more, making them reconstructable in large-volume neutrino telescopes and essentially free of Standard Model background.
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The central claim is Eq. (9): for $-1 \le n \le 1$, the dark-matter-electron scattering rate $R$ satisfies $$R \le \frac{\rho_\chi \bar\sigma_e}{\rho_T m_\chi}\frac{\$omega_p^{{n+1}}$}{4 $e^{2}$ \mu_{\chi e}^2}\int dq\, $q^{3}$ $F^{2}$ \$eta^{{\max}}$_n(q)\left[\frac{\varepsilon(q,0)-1}{\varepsilon(q,0)}\right]^{(1-n)/2}.$$ The derivation applies H\"older's inequality to the two sum rules for the electron energy-loss function, bounding $K_n(q)=\int_0^\infty d\omega\, \omega^n \mathrm{Im}[-1/\varepsilon(q,\omega)]$ by $\frac{\pi}{2}\omega_p^{n+1}[(\varepsilon(q,0)-1)/\varepsilon(q,0)]^{(1-n)/2}$. The paper further shows that at large momentum transfer the static dielectric response follows the universal scaling $\varepsilon(q,0)-1 \approx 4 m_e^2 \omega_p^2/q^4$, controlled only by the plasma frequency, so for most materials the bounds reduce to a function of $\omega_p$ and $\rho_T$. As a corollary, the bounds become lower bounds on the cross-section sensitivity of a direct detection experiment, and conventional targets such as silicon and aluminum are already within an order of magnitude of the improved bounds for light mediators across a wide mass range.
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The paper's central claim is that in any of these unified models the axion has a derivative coupling to neutrinos of the form $\mathcal{L}\supset -c_\nu \frac{\partial_\mu a}{4 v_s}\bar\nu\gamma^\mu\gamma^5\nu$, so its partial width into a neutrino pair is $\Gamma(a\to\nu_i\nu_i)=\frac{m_a}{16\pi}\left|\frac{c_\nu m_{\nu_i}}{N f_a}\right|^2\sqrt{1-4m_{\nu_i}^2/m_a^2}$. Because the coupling is proportional to the physical neutrino mass divided by the PQ scale, the decay rate grows once the axion mass exceeds twice a neutrino mass, and the dineutrino branching ratio can overtake the diphoton channel. The paper also shows that the anomaly ratio $E/N$, which fixes the axion–photon coupling, is unchanged for Type-I, Type-II, and Zee variants in DFSZ, but shifted by the new fermions in Type-III seesaw, and takes distinct values in the two colored-seesaw realizations, separating the models in the $g_{a\gamma\gamma}$–$m_a$ plane. Assuming the QCD axion is the dark matter, the resulting neutrino line at $E=m_a/2$ is large enough to lie above the Cosmic Neutrino Background and the solar thermal neutrino flux over a wide energy range.
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The central claim is that a two-axion dark sector with a light dark-energy axion and a heavy dark-matter axion can be recast exactly as coupled quintessence, provided the heavy axion stays on its WKB branch. The interaction endows the dark-matter mass with a phi dependence given by $m_\chi(\phi) = m_\chi \sqrt{1 + \beta \cos(\phi/f_\phi)}$, Eq. (11), so the dark-matter density follows $\rho_\chi/\rho_{\chi,0} = (m_\chi(\phi)/m_{\chi,0}) a^{-3}$, Eq. (18). Because the effective potential for $\phi$ shifts its minimum from $\phi = \pi$ at early times to $\phi = 0$ at late times, the field's derivative changes sign; the coupling $Q(\phi)$ consequently switches from negative to positive, injecting energy into the dark-matter component and producing a percent-level dip in $\rho_\chi$ relative to cold dark matter. When this is interpreted as a standard dark-energy component plus standard CDM, the resulting effective equation of state, Eq. (38), crosses below $w = -1$ at low redshift although the actual field equation of state stays above $-1$. This offers a string-motivated, non-phantom explanation of the DESI DR2 preference for an apparent phantom crossing.
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The central discovery is the covariance map of every damped Fourier mode: the final covariance splits into a propagated memory term $U_k C_{k,i} U_k^T$ and an injected controllability Gramian $W_k = \Sigma_k - U_k \Sigma_k U_k^T$, with $W_k \succeq (1-\varepsilon_{2,k}^2)\Sigma_k$. Consequently the released phase-space covariance always contains at least the fraction $1-\varepsilon_{2,k}^2$ of the stationary thermal covariance in every direction, and the determinant bound $\det C_{k,f} \ge (1-\varepsilon_{2,k}^2)^2 \det \Sigma_k$ protects the classical phase-space volume. In the overdamped spatial projection the injected spectrum is a completely monotone Laplace transform, yielding a white-noise infrared $k^3$ law, and the zero-mode susceptibility identity $P_0 k_\star^2 = rT/(a f_a^2)$ links the spectrum's amplitude to its turnover scale. This is why thermal alignment is claimed to be calculable: the late oscillator's initial condition is determined by the release map of the finite-temperature theory, not by a hand-picked angle.
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The paper's central claim is that MOND's acceleration scale becomes variable, $a_0' = a_0 + a_s + a_0 a_s / a_N$, where $a_N$ is the Newtonian acceleration of the mass enclosed inside radius $r$ and $a_s$ is the scalar sum of inverse-square gravitational mass contributions from the cluster mass exterior to $r$. Because $a_s$ grows inward and vanishes at the virial radius, the boost is strongest in cluster cores and fades outward, matching the observed radial shape of MOND's residual mass discrepancy. The same interpolating function as standard MOND then yields $a \sim \sqrt{a_N a_0'}$ rather than $a \sim \sqrt{a_N a_0}$, producing the needed factor-of-a-few acceleration boosts in toy models of Coma-, Virgo-, and Fornax-like clusters.
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The central discovery is a joint dark-sector degeneracy: late-time BAO and supernova distances prefer $w_{\mathrm{DE}}>-1$, while the CMB fixes the early-Universe matter density around last scattering; a positive $w_{\mathrm{DM}}$ changes how that early density maps to the present, lowering the dark-matter density at $z=2.33$ and increasing the matter-era distance interval by about 0.2%, which relieves a tension with the high-redshift acoustic scale. In the constant-$w$ extension this yields $w_{\mathrm{DM}}\sim0.001$ and $w_{\mathrm{DE}}\sim-0.94$, with both standard values outside the 95% contour, while releasing only one parameter at a time gives no comparable departure. With dynamical dark energy, allowing phantom crossing absorbs this geometric freedom and makes $w_{\mathrm{DM}}=0$ consistent; when phantom crossing is forbidden, the positive $w_{\mathrm{DM}}$ preference returns. A non-phantom Pad\'e-$w$+$w_{\mathrm{DM}}$ model is mildly preferred over the phantom-crossing $w_0w_a$ model by best-fit $\chi^2$ and DIC, leading the authors to conclude that the apparent phantom-crossing preference may instead reflect deviations in the dark-matter sector.
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In Section 1 the paper states that MOTION is 'a 70 kg LXe detector that provides a unique platform for systematic studies of the development of reliable HV components, dielectric breakdown and discharge phenomena in LXe.' If correct, the facility delivers controlled breakdown data at up to 200 kV, filling a gap that currently limits LXe TPC operation.
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The central load-bearing assertion, stated in the abstract, is that "strong gravity observables can serve as practical tools for distinguishing between competing dark matter models through their geometric imprints on black hole spacetimes." Concretely, the paper claims PFDM produces near-Schwarzschild geometry, constant-omega dark matter is restricted by causality to 0 <= omega <= 1, and BEC dark matter gives smooth deviations governed by K. If correct, horizon radius, photon sphere, shadow radius, ISCO, and circular velocity would carry model-dependent signatures.
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The load-bearing result is stated in Section 5 and Figure 10: 'a non-rotating core (j=0) embedded in a dense MCG envelope (A=0.05,n=1) achieves an efficiency of about 6.5%, effectively mimicking the radiative output of a vacuum Kerr black hole with a moderate spin of j about 0.3.' If true, continuum-fitting spin estimators would be biased when dense dark matter envelopes exist.
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On the paper's own terms, the central discovery is that Cloud-9's observed neutral-hydrogen column density profile, interpreted as a reionization-limited HI cloud (RELHIC) in hydrostatic equilibrium with its dark halo, cannot by itself distinguish cuspy from cored halos: equally good fits exist for a standard NFW profile and for SIDM halos at very different gravothermal stages. The distinction emerges only when the inferred halo parameters are compared with the cosmological concentration–mass relation. The CDM fit requires a concentration around 7σ below the cosmological median, while SIDM halos near the maximum core-expansion stage need only a 3σ low concentration, with the favored cross section peaking around 200 cm²/g. This moves the tension from "CDM must produce an exceptionally diffuse halo" to "SIDM naturally produces such halos via core formation." The paper also reports that about half of the formal hydrostatic solutions are dynamically unstable, imposing a lower bound on the host halo mass near 2.5×10⁹ M⊙.
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The central discovery is that a specific interacting dark-sector theory—a quintessence field coupled to dark matter by the conformal transformation g̃μν = e^{-2αφ}gμν, with a potential engineered so ρφ = Λ + ρDM - ρc—can simultaneously keep the ΛCDM background and lower late-time structure growth enough to reconcile early-universe CMB measurements with growth data. In the fit, the conformal coupling drains energy from dark matter into the field, reducing the matter density at low redshifts and suppressing clustering, yielding σ8,0 ≈ 0.762 ± 0.010 and Ωm,0 ≈ 0.311 ± 0.007. The same analysis shows that adding a disformal coupling D_m^4 e^{-2(α+β)φ}∂μφ∂νφ acts as friction that damps this exchan
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The central claim is that the same CNN architecture can solve three related characterization tasks on distributions reconstructed at detector level. On mono-jet data (transverse momentum, missing transverse energy, pseudorapidity) the classifier separates one-component from two-component dark matter signals with roughly 70% accuracy on the two-component class, and the regressors recover the masses: within about 50–80 GeV at 68% tolerance for single-component scalar/fermion signals and about 100 GeV for two-component signals. On mono-Z data, the same network also uses the angular separation Δφ between the two leptons to distinguish a single scalar from a single fermion, and mass estimates tig
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The central claim, stated in the abstract and conclusion, is: 'Our forecasts indicate that UGRB-galaxy cross-correlation measurements can probe previously unexplored regions of the ALP parameter space over a broad range of ALP masses.' If the paper is correct, a Fermi-LAT and 2MRS cross-correlation measurement can constrain the ALP-proton coupling g_ap for ALP dark matter masses near and above the values already excluded by SNO.
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The paper's central claim is that the shape of a relativistically broadened iron line does not by itself distinguish a Kerr black hole from a compact, non-rotating fermionic dark-matter core in the extended RAR model. In this spacetime, stable circular orbits extend far inside the core because there is no innermost stable circular orbit, and the radiative efficiency saturates at r_sat, roughly a tenth of the core radius. When the accretion disk reaches that inner edge, the most compact configurations (u/u_cr = 1) generate red wings and blue horns comparable to those of rapidly rotating prograde black holes; decreasing the compactness moves the red-wing onset to higher energies and tracks ret
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The central discovery is that the phase space of cosmic filaments is organized and hierarchical. Using Skeletor, the thesis reconstructs filament spines directly from discrete tracers with a Voronoi tessellation, uses dark-matter information to refine the spine and to define each filament's radius Rv as the location of maximum radial infall, and classifies nested sub-filaments within parent filaments. Stacked profiles then show coherent anisotropic inflow toward the spine, a velocity transition at the inferred boundary, multistreaming inside, and localized caustic-like features—signatures expected from anisotropic gravitational collapse. The thesis also shows that sub-filaments are statistic
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On the paper's own terms, the central discovery is that the minimal scale-invariant singlet model is not merely a viable dark-matter candidate but a predictive one: theory alone -- perturbativity, vacuum stability and $\lambda^{\mathrm{eff}}_S>0$ -- together with the cosmological relic density reduces the parameter space to a unique freeze-in solution. The light window is bounded by two nearby roots of $\lambda^{\mathrm{eff}}_S=0$; the relic-density contour crosses it at $m_S\simeq2.59$ MeV with $\lambda^{\mathrm{eff}}_{HS}\simeq2.48\times10^{-10}$ and at $m_S\simeq2.68$ MeV with $\lambda^{\mathrm{eff}}_{HS}\simeq2.43\times10^{-10}$. The heavier window, $436\ \mathrm{GeV}\lesssim m_S\lesssim632\ \mathrm{GeV}$, would require a tiny effective portal obtained from a large tree-level $\lambda_{HS}\simeq6.3\text{--}13.2$ through an extreme cancellation, and is excluded by the requirement $\lambda_S>0$ and by loss of perturbative control. The paper argues that the resulting light solution is stable under renormalisation-scale variation within the modified on-shell scheme, and that its direct-detection rate, $\bar\sigma_e\simeq5.5\times10^{-65}\,\mathrm{cm}^2$, is unobservably small for current and foreseeable experiments.
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The central assertion: a massive spin-0 field with a linear coupling to a spherical bubble source is copiously produced during the expansion epoch, even for walls expanding at constant radial velocity, until the local-rest-frame radius of curvature of the wall exceeds the particle Compton wavelength, i.e. R_lab approximately gamma/m (abstract; section 2.3, Eq. (2.21); section 2.4, Eq. (2.27)). If the paper is correct, expansion-epoch production parametrically dominates freeze-in for light feebly coupled particles (section 3.2), and hidden SU(Nc) confinement transitions with an imperfectly protected axion produce dark radiation and/or dark matter over large parameter regions (section 3.3, Figs. 7-8).
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The central claim is that including intra-cluster globular clusters in the dynamical model changes what the measurement means: together with the clusters bound to NGC 1399, they trace the combined gravitational potential of the galaxy and the Fornax cluster out to 150 kpc. Both an NFW and a Burkert halo fit the observed dispersion and kurtosis profiles, and for the full sample the two profiles give nearly the same enclosed mass. The best-fitting NFW model yields $\log M_{200} = 13.81 \pm 0.09\,M_\odot$, versus $13.49 \pm 0.06$ for Burkert; the inner sample alone gives lower and more profile-dependent values. The red clusters stay mildly radial or isotropic while the blue clusters switch from tangential orbits inside 40 kpc to radial orbits in the outskirts, a pattern the paper interprets as accretion of metal-poor clusters along radial infall paths. At $1\,R_e$ the dark-matter fraction already exceeds 50 percent, and at $5\,R_e$ it exceeds 90 percent.
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The paper establishes that a constant 'radioactive' decay rate Γ for dark energy, measured in units of the Hubble rate H0, is compatible with the full current data set. For distance data alone (DESI DR2 BAO plus supernovae), the posterior for Γ/H0 shifts positive by about 2σ, corresponding to a dark-energy density that decreases with time and an effective equation of state w > -1 at low redshift. Adding CMB data from Planck or Planck+ACT removes this preference, making Γ/H0 consistent with the ΛCDM value of zero. The DESI DR1 full-shape analysis, which is new for these models, breaks the degeneracy between decay channels: decaying into dark matter changes the matter abundance and perturbatio
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The central load-bearing assertion is in the abstract: 'For ξ_w=0.01, we find that shock heating increases Y_χ by factors of approximately 4.3, 5.8, and 32 for m_χ=1.78, 2.30, and 5.03 TeV, respectively,' together with the second claim that 'hydrodynamic reheating can enhance Y_χ even when dark matter has already frozen out before the phase transition.' If the paper is correct, the filtered dark matter relic abundance in this model is not set by wall filtering against the undisturbed bath but by the hydrodynamic state of the plasma in front of the wall, and heavy DM that chemically decoupled before nucleation can still receive an order 10 to 30 boost.
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Within the one-function radial-Δ family, the paper's central claim is a convexity theorem: for any C² positive nondecreasing m(r) with m + r m' → m0 > 0 at r → 0+, m → M_ADM finite and r m' → 0 at infinity, and pointwise 2m' + r m'' < 1, the function H(r) = r − m(r) − r m'(r) is strictly increasing from a negative value to +∞, hence vanishes exactly once; consequently Δ'' = 2H' > 0 and Δ is strictly convex with a unique positive minimum. For a ≠ 0, the sign of that minimum decides between two simple positive roots, one double root, or no root; for a = 0 there is exactly one simple positive root after excluding the origin. The FDM-inspired profile satisfies the hypotheses whenever f_sol/(r_c/
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For any smooth, positive coupling function f(χ)>0, the oscillation-averaged backreaction drives f upward: Eq. (17) gives d f/dt = C(a)/(6H) f^{-3/2} [f'(χ)]^2 ≥ 0, with equality only at stationary points of f. Consequently the modified Jeans wavenumber, which scales as k_J ∝ f^{-1/2} in the relevant regime, cannot be dynamically reduced; the condensate quantum pressure is strengthened, not suppressed, and kinetically coupled dark matter cannot self-generate enhanced collapse on sub-Jeans scales.
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In the paper's own terms, the discovery is that a massive spin-1 vector field cannot hide in the early universe: before it starts oscillating at H ≈ m_A a, its homogeneous component redshifts as radiation (ρ_A ∝ a^-4) rather than staying constant like a scalar field, so the amount of radiation-like energy present before recombination grows as m_A^{-1/2}. The observed CMB then imposes a 95% lower bound log10(mA/eV) > −24.07 for the pure VFDM case, with all standard cosmological parameters remaining consistent with ΛCDM; in the mixed VFDM+CDM case the constraint relaxes along a correlation that lets smaller fractions f sustain lighter masses. On the anisotropic side, the preferred direction of
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The paper claims that a Proca-field perturbation on Kerr, sourced by a constant-density dark matter bath, forms a stationary density spike around the black hole with averaged profile rho ~ (r/r_c)^-3/2, essentially unchanged from the Schwarzschild case except within ~10M of the horizon. The qualitatively new effect is superradiance: for any nonzero spin, modes with m > 0 and mu < m Omega_H have negative mass accretion rate, meaning the black hole loses mass and angular momentum to the field rather than accreting it. For the dominant superradiant mode, (s, l, m) = (-1,1,1), this extraction reaches roughly 10 solar masses per year for a 10^9-solar-mass black hole at rho_c = 10 solar masses per
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On the paper's own terms: the dynamical friction acting on a globular cluster in ultralight dark matter is controlled by the relative velocity between the cluster and the local dark-matter flow, not by the cluster's speed alone. In the vortex soliton the dark matter rotates around the halo center, so a co-rotating cluster has |v_GC - u(r)| near zero at certain radii. There the gravitational wake is suppressed and the characteristic time T = v_GC M / F_fr develops sharp peaks, exceeding ten gigayears and reaching far higher values for GC3. The vortex's toroidal density profile also removes dark matter from the innermost region, further weakening the drag. The paper concludes that the Fornax t
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The authors find that the dominant source of astrophysical uncertainty for dark matter direct detection is not the overall speed scale or density but the halo-to-halo spread in the median azimuthal velocity of local dark matter, vbar_phi. In the TNG50 sample, the median vbar_phi is +31 km/s with 91% of halos corotating, and the local dark matter's angular momentum aligns with the baryonic disk to within about 5 degrees. This corotation reduces the geocentric dark matter speeds and shifts the halo integral eta(v_min) down at high v_min, which suppresses recoil rates for dark matter below ~50 GeV and spreads the directional flux over a wider sky angle, reducing the daily modulation amplitude.
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The central claim is that the same stochastic misalignment process used for axions becomes a predictive production mechanism for dark photon dark matter once the dark Higgs's post-inflationary evolution and decay are treated carefully. The paper derives the probability distribution of the initial Higgs amplitude, follows the field through quartic, hybrid, or quadratic oscillation regimes, computes the dark photon relic density and its velocity at structure formation, and imposes the measured upper bound on inflationary isocurvature perturbations plus likelihood and self-consistency conditions. The result is a narrow allowed triangle in the dark photon mass-coupling plane, with the quartic re
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The central claim is that a non-minimal dark sector with SU(2) gauge symmetry, a real scalar triplet, and two Weyl doublet fermions can produce a thermal population of stable 't Hooft–Polyakov monopoles that freeze out as the dark matter, despite the generic expectation that stable dark gauge bosons would dominate the relic density. The mechanism works by splitting the fermion masses so that the heavy partner decays early and the light dark fermion annihilates away through dark-photon emission, while the monopoles survive. The authors compute monopole production from second-order, weakly first-order, and strongly first-order (supercooled) phase transitions, and find that in the allowed windo
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The central claim is that the observed acceleration in a baryonic system embedded in a dark-matter halo is the Newtonian baryonic acceleration plus a geometric, baryon-weighted dark-matter contribution, and that this sum, evaluated either as a global constant or as a local radial term, reproduces the RAR across many orders of magnitude in acceleration. The constant-interaction model writes gobs = gB + gint, with gint = G aM, and fits early-type galaxies, late-type galaxies, dwarf spheroidals, brightest cluster galaxies, and intracluster regions; the virial-motivated interaction model replaces gint with a local term that depends on the enclosed dark-matter mass and local dark-matter density,
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The central claim is that, within the framework considered, reproducing the observed dark-matter density fixes the dark-photon mass to 5.6 < m < 7.4 µeV. Because the Jordan-frame mass parameter m is assumed constant, the Einstein-frame effective mass becomes bm = m/Ω, where Ω ≈ exp(ϕ/√6 M_Pl) is the Weyl factor. The longitudinal mode's kinetic function varies during and after inflation, and its power spectrum acquires the factor Ω²(t_k). The resulting density parameter is approximately Ω_DM h² ≈ 0.15 (m/10 µeV)^{1/2} (Ω(t_k*)/10)² (H(t_k*)/10¹³ GeV)². Imposing the observed scalar amplitude, Ω_DM h² = 0.120 ± 0.001, and ΔN_eff < 0.30 yields m ∈ (5.6, 7.4) µeV, i.e., f ∈ (1.4, 1.8) GHz.
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The central claim is that one effective operator, a Bμν \tilde F_D^{μν}/(4Λ), produces both dark-sector particles by freeze-in, while the dark photon's kinetic-mixing decay γ_D → e+e− accounts for the 511 keV line. Solving the coupled Boltzmann equations, the authors find that Z-boson decay dominates production, the two components end with roughly equal relic fractions, and the observed abundance fixes Λ near 10^10–10^12 GeV for MeV-scale masses. The near-degeneracy mγD ≈ ma suppresses the otherwise fatal radiative decay γ_D → aγ, leaving e+e− lifetimes around 10^26–10^29 s. The resulting region also passes the Leo T Hα bound (for a conservative efficiency factor) and all other listed constr
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The central claim is that the vertical-cut split-cavity design gives wide, continuous frequency tuning without the quality-factor penalty of rod-based tuners. The authors demonstrate this in three copper prototypes, with measurements of the TM010 resonant mode showing a continuous tuning range of about 800 MHz centred near 8.5 GHz and quality factors that stay close to simulation across the sweep: about 17,000 at room temperature, 17,000–39,000 at 4 K, and about 48,000 for the two-port version at roughly 0.4 K in a 6 T field (66% of simulation). They also show that a movable antenna, driven by a second nanopositioner, recouples the cavity so the coupling parameter remains near β ≈ 2 over the
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The paper claims that the ionization rate of molecular clouds is a viable observable for dark matter models that inject low-energy electrons and positrons, and that it currently produces some of the strongest limits for two classes of candidates. For annihilating dark matter in the 1–100 MeV mass range, the constraint from the inner-Galaxy cloud G1.4-1.8+87 can match or beat CMB-anisotropy limits at the low-mass end; for primordial black holes above 10^16 g, the same cloud gives a limit on their dark-matter fraction that surpasses previous X-ray, 511-keV, cosmic-ray, and CMB bounds. Decaying dark matter constraints from the same cloud are also competitive with CMB and gamma-ray limits at low
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The core claim is that the boundary condition κ(Λ_UV)=0 for the Higgs–dark‑scalar portal is not imposed by hand but follows from five‑dimensional locality: the Higgs and the hidden scalar are localized on different branes, so the delta‑function overlap δ(y)δ(y−L) vanishes for separated branes. The same heavy‑neutrino sector that generates light neutrino masses through the seesaw mechanism then induces the portal at one loop, with a threshold contribution κ_loop = −Σ_I y_N,I² (Y_ν†Y_ν)_II/(4π²). In the aligned seesaw limit this is proportional to the light‑neutrino masses, making the mixing angle scale as M_N². The resulting phenomenology confines the heavy‑neutrino scale to roughly 10 TeV <
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On the paper's own terms, the central discovery is that the cosmological relic state can spontaneously break the exact Z_N symmetry of the Lagrangian, storing the initial axion value in the WIMP sector. Freeze-out with slow inter-sector conversion produces Boltzmann-suppressed relic fractions that retain a memory of the initial axion angle, generating an unsuppressed finite-density potential V_fd ≈ σ_fd n_χ [1 - cos(Θ - Θ_i)]. This potential traps the axion at Θ_i at early times; once n_χ drops below Λ_D/σ_fd, the vacuum potential releases it, and the relic-weighted WIMP mass increases, transferring energy from DE to DM. The result is an effective equation of state that crosses below -1, com
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The paper's central claim is that solar gravitational focusing makes a dark-matter wake an irreducible target: any unbound component of the Galactic dark-matter flow, particle or wave, is perturbed by the Sun's gravity and produces a calculable downstream density perturbation. A two-spacecraft heliocentric formation measuring inter-spacecraft range can read this perturbation as a projected tidal tensor, with the raw free-response displacement growing as T^2 while the formation remains inside a coherent region of the wake. For a 2.5×10^6 km baseline crossing a 0.1 AU coherent width at 30 km/s, a one-percent focused excess yields a 0.63 pm range scale over 5.77 days; an idealized one-year cohe
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The paper's central claim is that, once Pop III star formation is modeled self-consistently with Lyman-Werner feedback, the streaming motion between dark matter and baryons, and IMF-dependent line luminosities, the Pop III line-intensity signal is nearly two orders of magnitude weaker than earlier forecasts. As a result, the HeII 1640-A auto-power spectrum—the cleanest Pop III tracer—is undetectable with SPHEREx and even with the proposed CDIM; only the H-alpha x HeII cross-power, observed with an improved CDIM+ configuration, reaches S/N>=5, doing so at z~5 and out to z~16. The paper also shows that 'exotic' Pop III models, in which pristine star formation extends into more massive atomic-c
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Including an explicit Schrödinger–Poisson residual (or a first-order kick–drift–kick consistency) loss inside a generative U-Net substantially improves both the evolution and the super-resolution of fuzzy-dark-matter fields relative to data-only training, so that a 1 h⁻¹ Mpc box can be reproduced accurately from only ~20 percent of the temporal snapshots and, for the first time, generative super-resolution can be trained directly on full Schrödinger–Poisson simulations.
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Frontier observables that probe nonlinear structure below roughly one megaparsec already deliver competitive microphysical dark-matter limits (optimistic joint analyses reaching thermal-relic warm-dark-matter masses above about 10 keV), and the decisive next advance will be joint statistical combination of multiple probes rather than further isolated single-probe analyses.
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In a representative toy model of dark-sector Q-balls that constitute all dark matter, density-dependent merging converts a fraction of non-relativistic rest-mass energy into free-streaming relativistic particles and thereby transforms an initial NFW cusp into a cored inner density profile while leaving the outer halo essentially unchanged, for parameters satisfying 22.3 MeV ≲ v Q₀^{1/12} ≲ 81.2 MeV.
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The paper's central claim is that in a scalar-tensor modified-gravity framework whose point-mass metric is Schwarzschild–de Sitter-like with an added κr² term, the differential time delay between two lensed FRB images acquires an extra term proportional to (1/c√κ) tan⁻¹(...). This extra term changes the optical depth for lensing and, through Poisson statistics on zero confirmed lensed FRBs, yields an upper bound on fPBH that varies strongly with κ (Fig. 1). The same κ term produces a cutoff in the minimum detectable time delay that reproduces the behavior of a plasma scattering screen, meaning modified gravity can mimic plasma lensing in FRB observations.
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When the resonator stack is modeled exactly as described—twenty 1 mm plates of relative permittivity 30, fixed 6.21 mm spacing, lossless mirror and perfect antenna—the electromagnetic spectrum below 12 GHz contains no mode whose electric-field eigenfunction has appreciable longitudinal overlap with a uniform external magnetic field. All computed form factors are at most a few times 10^{-3} and typically far smaller, so the apparatus as specified cannot produce the axion sensitivity shown in the original work.
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The authors establish, using analytic arguments, that a mass-varying dark matter model with one bare potential V(φ) and one coupling scale M can generate an early dark-energy-like peak near matter-radiation equality and a late-time apparent phantom crossing near matter-dark-energy equality. The early peak's amplitude is set by the ratio m(φi)/m(φ0) − 1, its timing by the curvature of m(φ), and the late-time crossing is driven by the bare potential pushing the field at low redshift—exponential potentials doing this most naturally. Since both effects stem from the same mass function m(φ), the same range of M controls both, and the timing tracks the background evolution rather than separate ene
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The central discovery is that the full production-time dependence of the nonthermal RHN distribution cannot be replaced by a single average momentum: RHNs born at different times have different redshifted momenta, time-dilated decay rates, and equations of state. Retaining that distribution, the paper derives an integro-differential Boltzmann system and analytic solutions in four asymptotic regimes. The effective equation of state alternates as 0 -> 1/3 -> 0 -> 1/3, and the SM temperature follows T ∝ a^0, a^-1/4, a^-3/8, a^-1. In the hierarchical limit m_phi >> 2m_N, the final DM yield from inflaton decays is controlled by m_N and enhanced by m_phi/(2m_N); for UV freeze-in, the critical expo
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The central claim is that the dark matter annihilation limits derived from Fermi-LAT observations of dwarf galaxies are sensitive to how one assigns priors to the NFW halo parameters in a Jeans analysis. The paper builds a ladder of priors, from a wide log-uniform prior that lets kinematics dominate to an SHMR-weighted log-normal prior derived from a semi-analytic satellite population, and recomputes J-factors for 39 dwarfs. It finds that the inferred 95% confidence upper limit on the velocity-averaged annihilation cross section to b-bbar varies by roughly a factor of 2–4 across these priors. Adopting the cosmologically informed prior excludes the thermal-relic cross section only below about
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The central claim is that in a dark-dimension setup with one graviton tower and N closed-string axion KK towers, the late-time energy distribution among towers is controlled by a scale-invariant attractor solution of the coupled fragmentation equations. Because all towers equilibrate, most of the dark matter mass is transferred into the N 'dark' axion towers, and any visible decays (from the graviton or the one SM-coupled axion) carry only ~1/N of the total energy. The paper quantifies this with mass fractions M_a/M_tot ∝ 1/N and M_h/M_tot ∝ N^{-(s+2)/p}, and energy-injection weights ε_a ≈ 0.69/N, ε_h ≈ 0.46/N, which directly weaken the CMB energy-injection bound. It then combines these weig
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On the paper's own terms, the central result is that the nonlinear saturation of electrostatic streaming instabilities — not just their linear growth — converts the relative bulk motion of a subhalo and its host into turbulent heating that unbinds dark-matter particles. The authors model this by computing, from particle-in-cell simulations of counter-streaming dark plasmas, the 'bound fraction' f_bound, the share of particles remaining below the subhalo escape speed after saturation, and then converting that fraction into a density-loss rate for each radial shell of the subhalo using the re-virialization timescale of the halo. Applied along orbits in a Milky Way-like potential, the recipe yi
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The central claim, stated on the paper's own terms, is that the evolution of a weakly coupled wave onto a detector is a linear beam-splitter mixing with efficiency η = sin²(gt) ≪ 1, so the detector's final P-function is a convolution of the initial detector state with the wave's P-function compressed by √η. This compression forces any negativity in the wave's quasiprobability distribution into rapid sign oscillations that cancel against smooth measurement functions; the general calculation shows the probability of any single-detector outcome differs from that of a Gaussian-smeared, classical proxy state by (η/4)∫P_fc ∇²f_O + O(η²). As a result, nonclassicality measures obey Q_c = ηQ_a for nu
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The work uses a semi-analytic satellite generator that reproduces cold dark matter subhalo populations, then conditions that population on each observed dwarf to infer its halo. The central result is a mismatch: matching the mass enclosed within the observed half-light radius (from stellar velocity dispersions) gives more extreme central dark matter densities than matching stellar mass through the stellar-to-halo mass relation. Compact dwarfs appear overdense (Segue 1, Willman 1), diffuse ones underdense (Crater II, Hercules, Bootes I). For ultra-faints with r1/2 < 300 pc, the kinematic V_circ–r1/2 slope is β = 0.18 ± 0.12 instead of ~0.5, a ~2.4–2.5σ difference that persists across systemat
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The shear–kSZ estimator Ĉ^{T V_i}_ℓ ≡ ⟨T, (ṽ_i/c) κ⟩ has expectation value equal to a calibratable velocity kernel V_i times the lensing kernel and the projected matter–electron spectrum P_me(k_ℓ, z_i)/χ_i². Because κ traces total matter, P_me maps to the baryonic suppression S(k)=P_mm/P_DMO_mm via an exact cold-dark-matter plus baryon decomposition, up to a sub-percent dark-matter backreaction and a small bounded electron auto-spectrum term. The analytic model matches AbacusSummit measurements at ≲5% for ℓ≳500; CMB foregrounds cancel by velocity parity; and a realistic SO+DESI+LSST forecast yields SNR≈16 (f_sky=0.2), corresponding to roughly 1% on S(k).
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After gauge fixing, the homogeneous classical ULDM condensate has no influence on gravitational-wave propagation: its four-point self-energy cancels against corresponding local terms in the Einstein tensor by background symmetries. The residual effect is a time-dependent graviton effective mass generated by the quantum pressure of the squeezed state, which can drive parametric resonance. Under a power-law squeezing spectrum and non-relativistic conditions at equality, that resonant growth is negligible (relative enhancement ≲ 10^{-12}) for masses m ∼ 10^{-21}–10^{-24} eV.
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In mirror dark matter admixed neutron stars treated as two non-interacting fluids, the mass-scaled outer-fluid fundamental mode obeys the same compactness universal relation found earlier for self-interacting dark matter (though the relation weakens once metric perturbations are kept), while the mass-scaled inner-fluid fundamental mode follows its own compactness fit that is largely independent of the normal-matter equation of state once the dark-matter mass fraction is held fixed. Simultaneous measurement of the two modes could therefore constrain that mass fraction even when the nuclear equation of state remains uncertain.
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Under a quadratic expansion of the profile likelihood in the composite signal strength z = J x and the null best-fit assumption ẑ = 0, a published upper limit on the annihilation cross section updates as ⟨σv⟩_new = ⟨σv⟩_old × (J_old/J_new) × P(σ_new)/P(σ_old). The penalty P is 1/√(1−λ r²) for a Gaussian prior on J (with r = σ_J/J_0) and √ε e^ε / (√λ σ) for a log-normal prior on ln J, with ε fixed by the confidence-level threshold λ. The same curvature coefficients reconstructed from single-target limits allow multi-target combination by a one-dimensional numerical root find.
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The central claim is that the MOND-producing version of SFDM can be covariantly interpreted through RAQUAL, and that its interaction term, written in the Jordan frame, is equivalent to BECDM's non-minimal coupling G^μν ∂_μϕ ∂_νϕ up to a small correction of the form ϕ R. The equivalence is established by identifying the phonon-baryon coupling with the first-order expansion of a disformal metric shift h_μν = (A−1)g_μν + B ∂_μϕ ∂_νϕ. The same shift produces a non-analytic kinetic term X√|X| in the Einstein frame, whereas BECDM has a standard quadratic kinetic term; the authors argue that no perturbative disformal transformation can convert one into the other. Hence the two models share their in
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For a bubble-wall profile with n ripples of wavenumber κ, the h→φφ splitting amplitude factorizes into a single-ripple amplitude times a geometric interference sum. Constructive interference occurs whenever the momentum transfer Δp_z equals an integer multiple of κ; the new dominant channel sits at Δp_z=κ and gives the transition probability P≈(2n+1)V_h²/(512 E κ) √(1−2M_φ²/(Eκ)) for E>2M_φ²/κ (Eq. 2.29). The (2n+1) factor means that for n≳κM_φ/T_n² the resonant channel overtakes the smooth-wall contribution. The authors further show that such ripples arise naturally in a classically scale-invariant model, where the post-tunneling Higgs oscillations yield n_eff=O(10–100), and that the extra
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Within flat ΛCDM and linear tracer bias, the paper treats binary black-hole mergers and 21-cm brightness temperature as biased tracers of the same dark-matter field, and computes their tomographic angular auto- and cross-spectra exactly, beyond the Limber approximation, including density, velocity, lensing, and gravity terms. The central result is a forecast: combining the full auto-plus-cross matrix for the most powerful GW network considered (two Einstein Telescope sites plus one Cosmic Explorer) with a next-generation single-dish 21-cm survey recovers the injected cosmology with H0 to ~0.5%, Ωm to ~1.2-1.3%, and σ8 to ~1.6%, while the isolated GW-HI cross-spectrum alone gives ~2.9% on H0,
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Based on ultra-deep space-based imaging that reaches more than a magnitude below the turnover magnitude of the globular cluster luminosity function, the authors report a total of 78.3±3.7 globular clusters around Dragonfly-44, after background subtraction and completeness correction. The cluster system is more extended than the stellar body, with a Sérsic half-number radius of 1.41 R_e, and the faint clusters are less centrally concentrated than the bright ones. From the integrated, completeness-corrected luminosity function they derive a total cluster mass of about 1.6×10^7 solar masses, roughly 5% of the galaxy's stellar mass, and from the cluster count–halo mass relation a virial halo mas
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The central claim is that gauge invariance is not an exact structural requirement but the zero-speed limit of a stable, predictive theory of a slow longitudinal photon. Starting from the Hamiltonian with (c_L^2/2)(div A)^2, the longitudinal mode has dispersion omega = c_L k and is protected from acquiring a mass by a Galilean higher-form symmetry. Because its interactions are suppressed by c_L, the limit c_L -> 0 recovers QED observables; yet on-shell emission of the mode by a moving charge gives a rate Gamma = 4 alpha c_L (E_p - p^2/(3E_p)) with momentum transfer k of order p, so the recoil is nearly elastic in the preferred frame. Applied to bound states, the momentum transfer is capped by
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The central claim is that the Kaluza-Klein tower of a single five-dimensional axion interpolates between inflation and dark matter. In the mass-eigenstate basis the heaviest mode, a_299, carries the inflationary trajectory, with a nearly vanishing turning rate so that the dynamics are effectively single-field and standard slow-roll formulas apply. The predicted observables for the benchmark are n_s = 0.9662, r = 1.4e-8, A_s = 2.105e-9, and alpha_s = -0.0106, consistent with the latest CMB anisotropy data; a small phase shift can also accommodate the larger spectral index favored by newer ACT measurements. After inflation the inflaton decays to photons and reheats the Universe to T_RH about 5
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On its own terms, the central discovery is a separation of environmental controls. Ordinary, orientation-averaged secondary bias of haloes at fixed mass is substantially suppressed when the sample is matched in tidal anisotropy α, a scalar measure of the smoothed tidal field's anisotropy. Anisotropic secondary bias—the dependence of clustering on direction relative to the halo major axis—is largely insensitive to tidal anisotropy and to the anisotropy amplitude of the outer matter distribution, but is strongly reduced when haloes are matched by the alignment between their major axis and the surrounding density or tidal field. The spin (both bound-particle and all-particle definitions) and th
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The central claim is that the Hulse-Taylor binary's GR-consistent orbital decay excludes novel quadratic axion-fermion couplings a^2 psi-bar psi / Lambda_psi for neutrons, electrons, and muons. In an ambient axion dark-matter background this operator gives a long-range spin-independent force via a one-loop diagram; inside neutron stars it can trigger a tachyonic phase transition that sources a Yukawa force. The same operator also emits dipole and quadrupole axion radiation. Fitting periastron advance, Einstein delay, and period derivative with parameters beta and xi, profiling over masses, yields exclusions. The headline result: for m_a below 10^-12 eV, the Hulse-Taylor bound on the axion-mu
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At resonance, the spin out-of-plane angle and the relative precession phase obey equations that separate the two couplings: the build-up rate is proportional to the difference of the two resonance strengths, while the phase-walk rate is proportional to their sum. In a multi-bunch fixed-energy run, fitting the phase dependence of both observables yields the individual strengths up to a two-fold sign ambiguity. Independently, because the EDM resonance strength scales linearly with beam momentum while the axion-wind strength is momentum-independent at fixed ring radius and resonance frequency, the total resonance amplitude is linear in momentum; measuring it at two momentum settings separates t
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The paper claims that the observed redshift distribution of luminous gamma-ray bursts, when interpreted with a model where the GRB rate traces the cosmic star formation rate with a redshift-evolution factor (1+z)^alpha, excludes warm dark matter particle masses below 1.3 keV at 95% confidence. If the GRB rate is assumed to exactly trace the SFR (alpha=0), the limit strengthens to 3.4 keV. These constraints are derived from 118 bursts with z<10 and luminosity above 4×10^52 erg/s, selected to avoid instrumental selection effects, and they are robust to a free evolution index alpha.
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In an exactly solvable one-dimensional N-site lattice the full dynamic structure factor and the incoherent approximation differ only by the presence of a crystal-momentum-conserving delta function. That constraint becomes a weak restriction on the available phonon phase space once n greater than or equal to 2 phonons are produced, so the incoherent approximation (and a hybrid long-wavelength-plus-incoherent scheme) reproduces the exact scattering rates to within about 30 percent for both massive and massless mediators over most of the sub-GeV window.
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The central claim is a rate formula: a coherent graviton wave packet containing N gravitons, with central frequency ω_s and bandwidth σ_ω, decays in vacuum into photon pairs at dP/dt = 3 G^2 N^2 ω_s^3 σ_ω^2/(25π), so the photon count grows as N_γ(t) ≈ G^2 N_0^2 6ω_s^3 σ_ω^2 t/(25π). Two features matter here: a single plane-wave graviton field produces no photons at leading order, and the quadratic photon-gravity coupling vanishes classically in vacuum. The process appears because the coherent state is a many-graviton superposition and because the calculation is carried to second order in the metric; the paper shows the quantum result matches a semiclassical treatment whose photon source is t
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A novel three-loop scotogenic topology dynamically generates the inverse-seesaw lepton-number-violating mass matrix µ, while the same residual Z2⊗Z3 symmetry that enforces the radiative origin stabilizes the lightest particles of up to three independent dark sectors, allowing single-, two-, and three-component dark-matter scenarios that can reproduce Ωh²≃0.12 under existing experimental constraints and admit points consistent with the observed baryon asymmetry in simplified leptogenesis estimates.
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CLASSIER-DDM evaluates generic two-body decaying-dark-matter perturbations via iteratively solved integral equations, achieving sub-0.1% convergence in Pm(k) and the CMB lensing spectrum across the observationally relevant parameter space, O(0.1%) accuracy up to k ~ 3 Mpc^{-1} with ~100 momentum bins, and O(1 min) runtimes without a Boltzmann hierarchy or fluid approximation, thereby making DDM parameter estimation numerically tractable.
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A self-consistent PTA analysis that models ultralight scalar dark matter as a Gaussian random field with finite spatial correlations supplies a continuous amplitude prior between the fully correlated and fully uncorrelated limits; on mock data the limiting priors bias 95 percent upper limits by up to ~0.3 dex (linear) and nearly 1 dex (quadratic), while blinded injections recover the true mass and amplitudes inside the posterior support.
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At four thermal-relic benchmarks for complex scalar dark matter mediated by a dark photon, LDMX Phase II has projected 5σ discovery reach on the R=2.5 targets across N_BG=1 and 100, recovers both m_A' and ε within uncertainties there, and can statistically distinguish kinetic-mixing from higher electromagnetic-moment dark-photon models via Bayes factors, with the two-dimensional recoil analysis far stronger than energy-only.
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After U(1)Y1⊗U(1)Y2⊗U(1)Y3 breaks to SM U(1)Y and U(1)D breaks to a residual Z2, one common gauge structure can simultaneously generate hierarchical charged-fermion masses and small CKM mixing from hyperon-suppressed operators, produce tiny neutrino masses with large mixing via seesaw or scotoseesaw, and stabilize fermionic or scalar dark matter with viable TeV-scale relic and direct-detection windows.
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Using the same NaI(Tl) target and annual-modulation technique as DAMA/LIBRA, the combined six-year data sets of ANAIS-112 and COSINE-100 yield modulation amplitudes consistent with zero and incompatible with DAMA/LIBRA at 4.7 sigma (1-6 keV) and 3.5 sigma (2-6 keV), furnishing a strong model-independent case that the DAMA/LIBRA signal is not dark matter.
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Around a Schwarzschild-like black hole dressed by an exponential-sphere dark-matter halo, the halo mass M0 and scale radius r0 reshape bound geodesics and EMRI waveforms through non-degenerate channels. Radii and energies of the MBO and ISCO vary non-monotonically with r0 and can reverse trend with M0 depending on halo extent, while periodic-orbit spectra labeled by q = ωφ/ωr − 1 = w + v/z separate the two parameters. Numerical-kludge waveforms show that varying r0 produces a strong monotonic enlargement, longer radial periods, and clear dephasing, whereas comparable M0 variations leave the signal nearly unchanged unless M0 is a sizable fraction of the black-hole mass—so EMRI waveforms can i
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The central claim is the 'Dark Matter-Baryon Separability criterion,' Eq. (19): for a dark-matter-deficient galaxy to form in a high-speed collision, f_int(1−e^{−D_χb}) + (1−f_int)f_grav ≤ δ, where δ ≡ μ_crit/μ_i is the observationally chosen threshold divided by the progenitor's initial dark-matter-to-baryon ratio. This single inequality jointly limits the interacting fraction f_int, the dark-matter–baryon momentum-transfer cross section (embedded in the drag depth D_χb = ∫ Γ_χb dt ≈ Σ_b σ_MT/(m_χ+m_b)), and the gravitational recapture efficiency f_grav. The same logic yields bounds on dissipative dark matter—if a cooled component follows the baryonic disk, its abundance must be ≲δ—and on f
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Given present limits on stellar-mass PBH abundance, LISA and DECIGO together are expected to detect O(10^2) PBH binaries that still have orbital eccentricity e > 0.01 when their waves enter the detector band; if those observatories can exclude such eccentric systems, the upper limit on the PBH abundance can be strengthened by an order of magnitude. Isolated early binaries circularize completely except for residual O(10^{-2}) eccentricities in LISA, while binaries that experience binary-single interactions inside dense dark-matter halos retain higher eccentricity even at late inspiral.
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For spherically symmetric static black holes embedded in a constant-density baryonic halo within Weyl-incorporated gravity, there exist unique values of the coupling λ ≈ 3.5–3.9 that preserve a horizon near r = 2m; the associated photon-sphere impact parameters produce shadow radii that increase with black-hole mass, decrease under homogeneous plasma, and support test-field massive scalar modes that all decay while reaching quality factors of order 10^3–10^4.
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With combined exposures of 495.1 and 354.2 days in two MIMAC chambers, no statistically significant excess of nuclear recoils is found in the Anti-Cygnus ON cone relative to data-driven OFF regions. The resulting 90% CL Profile-Likelihood upper limit is σ_SD-p < 6.65×10^{-36} cm².
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Central claim: after a full-orbit fit of a spinning vacuum binary to the cNFW-corrected lens (parameters A, χ, d, q, γ, δΦ), the best model — equal mass, common spin, A = 0.0326, χ = 0.84, d = 0.340, γ = 25° — still leaves at the selected crossing near phase 0.08 an aligned timing shift of 1.5 × 10^-3 in orbital phase and a local window rms of 1.34 × 10^-2 (maximum residual 4.02 × 10^-2). A nearby resolution gives 1.8 × 10^-3 and 1.50 × 10^-2, so the quoted features do not disappear under a grid change — a disappearance check, not a formal convergence test. All three rising half-response crossings in one orbit were audited; the chosen event is not the strongest, with shifts ranging from −9.5
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The paper's central claim is that the light inflaton scenario survives the latest ACT DR6 cosmological constraints once the quartic inflaton potential receives a relative one-loop correction Δ_L ≡ β/λ_φ at the level of ≳0.01. At tree level (Δ_L = 0) the model's predictions lie just outside the ACT 2σ contour; with Δ_L = 0.01–0.05 they fall within the 1σ region. For m_φ ≲ 10 GeV, the same Higgs-mixing angle that governs inflationary reheating also controls the inflaton's production in kaon and B decays and its decay length, so existing bounds from NA62, KOTO, BaBar/Belle and LHCb—together with the lifetime-independent B0–B̄0 mixing bound sinθ ≲ 0.96 (m_φ/GeV) for m_φ ≲ 1 GeV—already exclude a
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In the muonic realisation of the fermionic portal to vector dark matter, Drell–Yan pair production of the heavy vector-like muon μ' is followed by cascade decays through the dark vector V' and the dark scalar H_D, producing final states with four, six, eight, or ten visible muons. The paper's central claim is that the six-muon channel is the best target: it combines a sizeable branching fraction over a broad region of the (m_V', m_H_D) plane, a very clean experimental signature, and enough internal resonance structure to reconstruct the intermediate states and the parent heavy lepton. Six muons arise from either the symmetric (3+3)μ topology, in which each μ' chain yields three muons, or the
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The central claim is that the pre-inflationary QCD axion is not just a one-line upper bound on the inflationary energy scale but a structural constraint on the architecture of inflation. On the paper's own terms: for a light, canonically normalized axion with a scale-invariant spectrum, the exact pivot-scale bound is H_I < 2π f_I / (γ_a |T_θ G(θ_i)|) √P^max_II, where γ_a is the axion dark-matter fraction, T_θ the superhorizon transfer, and G(θ_i) = ∂ln Ω_a/∂θ_i the logarithmic abundance response including anharmonic effects. In the minimal benchmark this gives 95% C.L. bounds H_I < 1.25×10^10 GeV (at the prior f_a ≤ M_Pl, with an extrapolated abundance law) and H_I < 2.2×10^7 GeV for θ_i = 1
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The central discovery is that the scaling global monopole network is a copious and soft source of NG bosons: the spectrum of each of the two massless modes peaks at momenta of order the Hubble scale, the comoving number density increases linearly with conformal time (n_NG = C v^2 H with C ≈ 0.7–0.9), and the radial mode is subdominant. This linear growth is tied to the scaling of the network: monopole separation ξ ∝ τ, so the energy lost to radiation is roughly 2Hρ_M. When a soft mass is added, the abundance of the resulting pNG bosons is given by Eq. (15), and the paper maps the viable region in the (m_NG, v) plane, including the black-hole superradiance constraint. The same spectral shape
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The central claim is that a pure momentum-transfer interaction between dark matter and baryons, with interaction rate Γm = γ a^{-2}, modifies only the Euler equations of the two fluids in linear perturbation theory. In the early universe the photon–baryon plasma's effective pressure is transmitted to dark matter, suppressing matter clustering on small scales and lowering σ8. The authors implement the model in CLASS, CAMB, and SymBoltz, confirm agreement among all three, and show that combining Planck CMB (including lensing), BAO, Pantheon+ supernovae, and the Planck SZ cluster S8 measurement yields log10γ = −6.73 (+0.26,+0.39 / −0.06,−0.50) at 68/95% C.L., a non-zero interaction at more than
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The central claim is that the entropic generalized Chaplygin gas — a unified dark fluid with equation of state p = -A/ρ^α, plus an entropy perturbation that drives the effective rest-frame sound speed to zero — is consistent at the background level with the full set of late-Universe distance and growth data, and that its only significant effect is a late-time bending of the distance-redshift relation. The paper argues this deformation moves the joint posterior in (H0, Ωm, S8) almost exclusively along directions controlled by the expansion history: with one supernova calibration it substantially shifts H0 and improves the fit over ΛCDM; with another calibration the two models nearly coincide.
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The core discovery is that in a conformally invariant theory of gravity plus matter with a dilaton, the conformal BRST cohomology is trivial: the only even trace anomalies are exact cocycles, i.e. coboundaries that can be canceled by local counterterms. The paper identifies all candidate anomaly densities built from the Weyl-invariant metric, curvature tensors, and dilaton derivatives, and shows that each one either vanishes by the consistency conditions or is the BRST variation of a counterterm. It further shows that when the dilaton is set to a constant value, the counterterms needed to cancel the coboundaries match the forms of the Weyl-squared and Ricci-scalar-squared actions, so tuning