Wed·Jul 24, 2024Wednesday·July 24, 2024

1. 01*

   The CSS Hamiltonian: high energy evolution of rapidity dependent observables

   Haowu Duan🇺🇸 · Alex Kovner🇺🇸 · Michael Lublinsky🇮🇱

   We consider evolution of observables which depend on a small but fixed value of longitudinal momentum fraction $x$, to high rapidity, such that $\eta >\ln 1/x$. We show that this evolution is not given by the JIMWLK (or BK) equation. We derive the evolution Hamiltonian - $H_{CSS-JIMWLK}$ which generates this evolution in the cases of dilute and dense projectile wave function. The two limits yield identical results for $H_{CSS-JIMWLK}$. We show that the resulting evolution for the gluon TMD is identical to the (double logarithmic) perturbative Collins-Soper-Sterman evolution equation in the longitudinal resolution parameter at a fixed and very large transverse resolution.

   hep-phhep-thnucl-thPRD(2025)·10 citations
2. 02*

   A framework for simultaneous fit of QCD and BSM parameters with xFitter

   XiaoMin Shen🇨🇳 · Simone Amoroso🇩🇪 · Jun Gao🇨🇳 · Katerina Lipka🇩🇪 · Oleksandr Zenaiev🇩🇪

   An extension of the xFitter open-source program for QCD analyses is presented, allowing for a polynomial parameterization of the dependence of physical observables on theoretical parameters. This extension enables simultaneous determination of parton distribution functions (PDFs) and new physics parameters within the framework of the Standard Model Effective Field Theory (SMEFT). The functionalities of the code are illustrated in a sensitivity study, where a simultaneous determination of the PDFs, top quark mass and the couplings of selected dimension-6 SMEFT operators is addressed using projections for measurements of top quark-antiquark pair production at the High-Luminosity LHC. The importance of considering all the correlations of the parton distributions, top quark mass and the EFT parameters in a simultaneous QCD+SMEFT analysis is demonstrated. This work serves as a new platform for simultaneous extraction of the PDFs and the SM/SMEFT parameters based on xFitter.

   hep-phEPJC(2024)·6 citations
3. 03*

   Unifying the landscape of nucleon structure: an infrared-safe evolution scheme

   Rong Wang🇨🇳 · Chengdong Han🇨🇳 · Xurong Chen🇨🇳

   A novel approach for describing the evolution of nucleon structure from the low-$Q^2$ regime to the high-$Q^2$ asymptotic region is proposed. This infrared-safe scheme modifies the parton distribution evolution equations to incorporate the corrections from emergent hadron mass mechanisms and parton-parton recombination at low $Q^2$. The effective parton mass, generated by dynamical chiral symmetry breaking, slows the evolution of parton distributions in the infrared region, causing the DGLAP evolution to freeze when $Q^2\ll M_{q/g}$. Notably, this scheme renders the high-$Q^2$ parton distributions insensitive to the choice of input hadronic scale. The parton-parton recombination effect is crucial in suppressing the rapid growth of parton distributions at small $x$, consistent with experimental data. When applied to three valence quark distributions derived from a quark model, our scheme yields parton distributions that agree well with deep-inelastic scattering data in both large-$x$ and small-$x$ regions, providing a unified description of nucleon structure across the entire $Q^2$ range.

   hep-phPRD(2024)·4 citations
4. 04*

   Low-mass constraints on WIMP effective models of inelastic scattering using the Migdal effect

   Sunghyun Kang🇰🇷 · Stefano Scopel🇰🇷 · Gaurav Tomar🇮🇳

   We use the Migdal effect to extend to low masses the bounds on each of the effective couplings of the non-relativistic effective field theory of a WIMP of mass $m_{\chi }$ and spin 1/2 that interacts inelastically with nuclei by either upscattering to a heavier state with mass splitting $\delta >0$ or by downscattering to a lighter state with $\delta <0$. In order to do so we perform a systematic analysis of the Migdal bounds in the $m_{\chi }-\delta$ parameter space comparing them to those from nuclear recoil searches. The Migdal effect allows to significantly extend to low WIMP masses the nuclear recoil bounds for $\delta <0$. In this case the bounds are driven by XENON1T, except when $\delta$ is vanishing or very small, when, depending on the WIMP-nucleus interaction, in the lower end of the $m_{\chi }$ range either DS50 or SuperCDMS are more constraining. On the other hand, when $\delta >0$ and the WIMP particle upscatters to a heavier state nuclear recoil bounds are stronger than those from the Migdal effect.

   hep-phhep-exJCAP(2025)·11 citations
5. 05*

   Revisiting the Minimal Nelson-Barr Model

   Kai Murai🇯🇵 · Kazunori Nakayama🇯🇵

   We revisit the minimal Nelson-Barr model for solving the strong CP problem through the idea of spontaneous CP breaking. The minimal model suffers from the quality problem, which means that the strong CP angle is generated by higher-dimensional operators and one-loop effects. Consequently, it has been considered that there is a cosmological domain wall problem and that leptogenesis does not work. We point out that just imposing an additional approximate global symmetry solves the quality problem. We also propose a simple solution to the domain wall problem and show that the thermal leptogenesis scenario works.

   hep-phastro-ph.COJHEP(2024)·14 citations
6. 06*

   Discovering an Unquenched Dynamics Mechanism for Charmonium Scattering

   Qi Huang🇨🇳 · Rui Chen🇨🇳 · Jun He🇨🇳 · Xiang Liu🇨🇳

   In this work, we propose an unquenched mechanism for charmonium scattering that utilizes the internal structure of charmonium. By capturing light flavor quarks and anti-quarks from the vacuum, charm and anti-charm quarks form virtual charmed mesons, which mediate an effective one-boson exchange process. This approach accurately reproduces the di-$J/\psi$ invariant mass spectrum observed by CMS and LHCb, demonstrating its validity. Our mechanism offers a comprehensive framework for understanding charmonium scattering and is applicable to the scattering problems involving all fully heavy hadrons, an area of increasing interest.

   hep-phPRD(2026)·12 citations
7. 07*

   Towards QCD at Five Loops

   Andreas Maier🇩🇪 · Peter Marquard🇩🇪 · York Schröder🇨🇱

   We report on recent progress on five-loop calculations in perturbative QCD. We discuss the computation of the perturbative quark condensate, decoupling in QCD, and the precision determination of charm and bottom quark masses. For the latter, we give some first results from a gauge-invariant subset of five-loop diagrams.

   hep-phPoS(2024)·4 citations
8. 08*

   Scalar and vector dark matter admixed neutron stars with linear and quadratic couplings

   Francesco Grippa🇮🇹 · Gaetano Lambiase🇮🇹 · Tanmay Kumar Poddar🇮🇹

   We investigate the effects of dark scalar- and vector-mediated interactions on dark matter admixed neutron stars, employing the two-fluid formalism. We adopt three different nuclear equations of state -- BSk22, MPA1 and APR4 -- to describe the baryonic sector, while the dark component consists of fermionic particles within a relativistic mean field framework. We consider both linear and quadratic scalar interactions with the dark fermion, including a quartic self-interaction in the latter case. The parameters of the dark matter models are inferred via a Bayesian analysis that incorporates data from NICER observations and binary neutron star merger detections. The neutron star configurations obtained from the selected model parameters develop dark matter cores, leading to more compact objects with smaller masses and radii. Our findings suggest that scalar interactions generally have a weaker impact on the stellar structure compared to vector-mediated ones, though quantitative differences arise. In particular, quadratic scalar couplings suppress the net attractive interaction, allowing for larger dark matter fractions to be accreted. We also compute the sound speed of DM, finding that the scalar and quadratic interactions modify the stiffness of the dark equation of state while respecting causality: vector repulsion enhances the sound speed, whereas scalar attraction tends to soften it. We compare our results with GW1708017, GW190425 and NICER data and constrain DM couplings and mass.

   hep-phastro-ph.COgr-qcPRD(2026)·10 citations
9. 09*

   Cascade (${\Xi }^0$) Baryon Spectroscopy in the Relativistic Framework of Independent Quark Model

   Rameshri V. Patel🇮🇳 · Manan N. Shah🇮🇳

   The spectroscopy of ${\Xi }^0$ is performed within the relativistic framework of independent quark model. The equal mixture of scalar and vector components in the potential having Martin-like form is considered for the confinement. With the suitable potential parameters for ${\Xi }^0$, mass spectra for high radial and orbital excitation is calculated. The experimentally observed values of ground state magnetic moment, branching ratios and asymmetry parameters for radiative weak decays, ${\Xi }^0\to {\Lambda }^0+{\gamma }^0$ \& ${\Xi }^0\to {\Sigma }^0+{\gamma }^0$ are obtained to validate the model. The spin parity of experimentally known resonances like $\Xi (1530)$, $\Xi (1820)$, \& $\Xi (2030)$ are confirmed through the Regge trajectories in $(J,M^2)$ plane. The spin pa+rity of $\Xi (1950)$, $\Xi (2130)$, \& $\Xi (2250)$ are predicted using those Regge trajectories. The radiative decay width and magnetic moment of first resonance is also predicted.

   hep-phPRD(2024)·7 citations
10. 10*

    Dark Photon Dark Matter and Low-Frequency Gravitational Wave Detection with Gaia-like Astrometry

    Haipeng An🇨🇳 · Tingyu Li🇨🇳 · Jing Shu🇨🇳 · Xin Wang🇬🇧 · Xiao Xue🇩🇪 · Yue Zhao🇺🇸

    Astrometric surveys offer us a method to search for elusive cosmic signatures, such as ultralight dark photon dark matter and gravitational waves, by observing the deflection to the apparent positions of the stars. The detection capabilities of such surveys rapidly decrease at low frequencies, because the signals become hardly distinguishable from the background motion of stars. In this work, we find that the background motion can be well described by a linear model over time, based on which we propose a linear background subtraction scheme. Compared to the conventional quadratic subtraction, the advantage of linear subtraction emerges within the frequency range below $6\times 10^{-9}\mathrm{Hz}$. Taking dark photons with purely gravitational interactions, dark photons with additional $U(1{)}_B$ or $U(1{)}_{B-L}$ gauge interactions, and low-frequency gravitational waves as examples, we illustrate that the linear subtraction scheme can result in an enhancement of more than one order of magnitude in the exclusion limits of Gaia-like experiments in the low-frequency range.

    hep-phastro-ph.COastro-ph.GAastro-ph.IM+1ApJ(2024)·8 citations
11. 11*

    ftint: Calculating gradient-flow integrals with pySecDec

    Robert V. Harlander🇩🇪 · Theodoros Nellopoulos🇩🇪 · Anton Olsson🇩🇪 · Marius Wesle🇩🇪

    The program ftint is introduced which numerically evaluates dimensionally regulated integrals as they occur in the perturbative approach to the gradient-flow formalism in quantum field theory. It relies on sector decomposition in order to determine the coefficients of the individual orders in $ϵ=(4-D)/2$, where $D$ is the space-time dimension. For that purpose, it implements an interface to the public library pySecDec. The current version works for massive and massless integrals up to three-loop level with vanishing external momenta, but the underlying method is extendable to more general cases.

    hep-phhep-latComput.Phys.Commun.(2025)·5 citations
12. 12*

    Quantum coherence in neutrino spin-flavor oscillations

    Ashutosh Kumar Alok🇮🇳 · Trambak Jyoti Chall🇮🇳 · Neetu Raj Singh Chundawat🇮🇳 · Shireen Gangal🇮🇳 · Gaetano Lambiase🇮🇹

    Coherence, which represents the superposition of orthogonal states, is a fundamental concept in quantum mechanics and can also be precisely defined within quantum resource theory. Thus exploring quantum coherence in neutrino oscillations can not only help in examining the intrinsic quantum nature but can also explore their potential applications in quantum information technologies. Previous studies on quantum coherence have focused on neutrino flavor oscillations (FO). However, FO imply that neutrinos have mass and this can lead to the generation of a tiny but finite magnetic dipole moment of neutrinos through quantum loop diagrams at higher orders of perturbative expansion of the interaction. This electromagnetic property of neutrinos can induce spin flavor oscillations (SFO) in the presence of an external magnetic field and hence is expected to enrich the study of coherence. In this work, we investigate quantum coherence in neutrino SFO with three flavor mixing within the interstellar as well as intergalactic magnetic fields, quantified by the $l_1$ norm and the relative entropy of coherence, and express these measures in terms of neutrino SFO probabilities. For FO, coherence measures can sustain higher values (say, within 50% of the maximum) over distances of several kilometers, which are relevant for terrestrial experiments like reactor and accelerator neutrinos. However, for SFO, we find that the coherence scale can extend to astrophysical distances, spanning from kiloparsecs to gigaparsecs.

    hep-phquant-phPRD(2025)·8 citations
13. 13*

    Leptogenesis via Bubble Collisions

    Martina Cataldi🇩🇪 · Bibhushan Shakya🇩🇪

    We present a novel realization of leptogenesis from the decays of sterile (right-handed) neutrinos (RHNs) produced from runaway bubble collisions at a first order phase transition. Such configurations can produce heavy RHNs with mass many orders of magnitude above the scale of symmetry breaking as well as the temperature of the plasma, thereby enabling high scale leptogenesis without the need for high reheat temperatures while also naturally suppressing washout effects. This mechanism also extends the window of viability to RHN masses $\gtrsim 10^{14}$ GeV, the natural scale for type-I seesaw with $\mathcal{O}(1)$ couplings, where standard thermal leptogenesis cannot produce the observed baryon asymmetry. The corresponding phase transitions are at scales $\gtrsim 10^9$ GeV and produce gravitational wave signals that could be detected by future experiments.

    hep-phastro-ph.COJCAP(2024)·43 citations
14. 14*

    Completing the one-loop $\nu$SMEFT Renormalization Group Evolution

    Marco Ardu🇪🇸 · Xabier Marcano🇪🇸

    In this work we consider the Standard Model Effective Field Theory extended with right-handed neutrinos, the $\nu$SMEFT, and calculate the full set of one-loop anomalous dimensions that are proportional to Yukawa couplings. These contributions are particularly relevant when symmetry-protected low scale seesaw models are embeded in the SMEFT, since large neutrino Yukawa couplings are expected. By combining our results with the already available gauge anomalous dimensions, we provide the complete set of one-loop renormalization group evolution equations for the dimension six $\nu$SMEFT. As a possible phenomenological implication of our results, we discuss the sensitivity of lepton flavor-violating observables to $\nu$SMEFT operators, focusing on the more sensitive $\mu \to e$ transitions.

    hep-phJHEP(2024)·11 citations
15. 15*

    On the sensitivity of nuclear clocks to new physics

    Andrea Caputo🇨🇭 · Doron Gazit🇮🇱 · Hans-Werner Hammer🇩🇪 · Joachim Kopp🇨🇭 · Gil Paz🇺🇸 · Gilad Perez🇮🇱 · Konstantin Springmann🇮🇱

    The recent demonstration of laser excitation of the $\approx 8$ eV isomeric state of Thorium-229 is a significant step towards a nuclear clock. The low excitation energy likely results from a cancellation between electromagnetic and strong contributions, which new physics can disrupt. In this Letter, we quantify the enhancement of a nuclear clock's sensitivity to new physics using a geometric model and a novel $d$-wave halo model of the nucleus that reproduces measured differences between Thorium-229 states. We find likely enhancements of order $10^4$ while a worst case scenario with enhancement $\ll 1$ is unlikely.

    hep-phnucl-exnucl-thPRC(2025)·35 citations
16. 16*

    Axion species scale and axion weak gravity conjecture-like bound

    Min-Seok Seo🇰🇷

    As a cutoff scale of quantum gravity, the species scale can be defined by the scale at which the perturbativity of the non-renormalizable gravitational interaction begins to break down. Since it is determined by the number of species in the effective field theory, we can find the close connection to the distance conjecture, which predicts the lowering of the cutoff at the asymptotic limit of the moduli space caused by the descent of a tower of states from UV. Meanwhile, the same kind of the cutoff scale can be obtained from any non-renormalizable interaction, in particular the interaction between the axion and the gauge field through the $\theta F\wedge F$ term. Demanding this `axion species scale' not to exceed the gravitational species scale, we obtain the bound $(8{\pi }^2/g^2)f\lesssim M_{\mathrm{Pl}}$. This is quite similar to the axion weak gravity conjecture bound, but can be applied to any gauge as well as the string interactions which are relevant to towers of states. We also investigate the implications of the (axion) species scale and the axion weak gravity conjecture-like bound by considering the Peccei-Quinn charge reduction of black hole through the interaction between black hole and the string or wormhole.

    ↳ hep-thgr-qchep-phJHEP(2024)·9 citations
17. 17*

    Recent IceCube Results: Diffuse Flux, Point Sources and Dark Matter

    Minjin Jeong (on behalf of the IceCube Collaboration)🇺🇸

    In 2013, the IceCube Collaboration reported the first observation of an astrophysical neutrino flux, with energies extending up to the PeV-scale. Over the last decade, this flux has been characterized by measurements in multiple detection channels that are complementary with respect to the sensitive energy range, flavor composition, sky coverage, and backgrounds. The origin of these neutrinos remains largely unknown. However, evidence has been found for neutrino emission from the directions of the blazar TXS 0506+056, Seyfert galaxy NGC 1068. and the Galactic Plane. IceCube also has an active program of indirect dark matter searches with competitive constraints on dark matter models. In this talk, we will present recent results of the IceCube experiment, highlighting the latest diffuse flux measurements, point source searches, and dark matter analyses.

    ↳ astro-ph.HEhep-ph1 citation
18. 18*

    Spinning waveforms of scalar radiation in quadratic modified gravity

    Adam Falkowski🇫🇷 · Panagiotis Marinellis🇫🇷

    We study scalar-tensor gravitational theories using on-shell amplitude methods. We focus on theories with gravity coupled to a massless scalar via the Gauss-Bonnet and Chern-Simons terms. In this framework, we calculate the waveforms for classical scalar radiation emitted in scattering of macroscopic objects, including spin effects. To this end, we use the Kosower-Maybee-O'Connell formalism, with the 5-particle amplitude for scalar emission in matter scattering calculated at tree level using the unitarity-factorization bootstrap techniques. We also discuss in detail the dependence of that amplitude on the contact terms of the intermediate 4-particle scalar-graviton-matter amplitude. Finally, we discuss the conditions for resolvability of classical scalar radiation.

    ↳ hep-thgr-qchep-phEPJC(2025)·20 citations
19. 19*

    An indirect search for dark matter with a combined analysis of dwarf spheroidal galaxies from VERITAS

    (VERITAS collaboration) A. Acharyya🇺🇸 · C. B. Adams🇺🇸 · P. Bangale🇺🇸 · J. T. Bartkoske🇺🇸 · P. Batista🇩🇪 · W. Benbow🇺🇸 · J. L. Christiansen🇺🇸 · A. J. Chromey🇺🇸 · A. Duerr🇺🇸 · M. Errando🇺🇸 · A. Falcone🇺🇸 · Q. Feng🇺🇸 and 50 other authors

    Understanding the nature and identity of dark matter is a key goal in the physics community. In the case that TeV-scale dark matter particles decay or annihilate into standard model particles, very-high-energy (VHE) gamma rays (greater than 100 GeV) will be present in the final state. The Very Energetic Radiation Imaging Telescope Array System (VERITAS) is an imaging atmospheric Cherenkov telescope array that can indirectly detect VHE gamma rays in an energy range of 100 GeV to > 30 TeV. Dwarf spheroidal galaxies (dSphs) are ideal candidates in the search for dark matter due to their high dark matter content, high mass-to-light ratios, and their low gamma-ray fluxes from astrophysical processes. This study uses a legacy data set of 638 hours collected on 17 dSphs, built over 11 years with an observing strategy optimized according to the dark matter content of the targets. The study addresses a broad dark matter particle mass range, extending from 200 GeV to 30 PeV. In the absence of a detection, we set the upper limits on the dark matter velocity-weighted annihilation cross section.

    ↳ astro-ph.HEastro-ph.COhep-exhep-phPRD(2024)·17 citations
20. 20*

    Application of the Eddington inversion method to constrain the dark matter halo of galaxies using only observed surface brightness profiles

    Jorge Sanchez Almeida (1 and 2)🇪🇸 · Angel R. Plastino (3) · Ignacio Trujillo (1 and 2) ((1) Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain, (2) Universidad de La Laguna, Spain, (3) CeBio y Departamento de Ciencias Basicas, UNNOBA, CONICET, Junin, Argentina)

    *** Context: The halos of low-mass galaxies may allow us to constrain the nature of dark matter (DM), but the kinematic measurements to diagnose the required properties are technically extremely challenging. However, the photometry of these systems is doable. Aims. Using only stellar photometry, constrain key properties of the DM haloes in low-mass galaxies. *** Methods: Unphysical pairs of DM gravitational potentials and starlight distributions can be identified if the pair requires a distribution function f that is negative somewhere in the phase space. We use the classical Eddington inversion method (EIM) to compute f for a battery of DM gravitational potentials and around 100 observed low-mass galaxies with Mstar between 10**6 and 10**8 Msun. The battery includes NFW potentials (expected from cold DM) and potentials stemming from cored mass distributions (expected in many alternatives to cold DM). The method assumes spherical symmetry and isotropic velocity distribution and requires fitting the observed profiles with analytic functions, for which we use polytropes (with zero inner slope, a.k.a. core) and profiles with variable inner and outer slopes. The validity of all these assumptions is analyzed. *** Results: In general, the polytropes fit well the observed starlight profiles. If they were the correct fits (which could be the case) then all galaxies are inconsistent with NFW-like potentials. Alternatively, when the inner slope is allowed to vary for fitting, between 40% and 70% of the galaxies are consistent with cores in the stellar mass distribution and thus inconsistent with NFW-like potentials. *** Conclusions: Even though the stellar mass of the observed galaxies is still not low enough to constrain the nature of DM, this work shows the practical feasibility of the EIM technique to infer DM properties only from photometry.

    ↳ astro-ph.GAastro-ph.COhep-phAstron.Astrophys.(2024)·7 citations
21. 21*

    Unitarization of the one-loop graviton-graviton scattering amplitudes and study of the graviball

    J. A. Oller🇪🇸 · Marcela Peláez🇺🇾

    From the graviton-graviton scattering amplitudes calculated perturbatively in quantum gravity to the one-loop order, we develop further a formalism that allows one to calculate infrared-finite partial-wave amplitudes fulfilling perturbative unitarity. As a result of this process a parameter dubbed $\ln a$ emerges that separate between infrared and typical external momenta. The resulting partial-wave amplitudes are next unitarized by employing the Inverse Amplitude Method and the algebraic-$N/D$ method. Then, the graviball resonance, with a similar pole position, is confirmed in the $S$-wave partial-wave amplitude for all unitarization methods, also with respect to the unitarization of only the leading-order amplitude. Although the spectrum of the theory is independent of the specific value of $\ln a$, the requirement for a well-behaved unitarized effective field theory of gravity identifies the optimal range of $\ln a$ for our next-to-leading-order calculations as $0.5\lesssim \ln a\lesssim 1.7$. Briefly, we discuss the $D$-wave scattering that is weaker than the $S-$wave scattering, repulsive and non-resonant for $\ln a\approx 1$.

    ↳ hep-thhep-phPLB(2025)·4 citations
22. 22*

    Constraining the impact of standard model phase transitions on primordial black holes

    Xavier Pritchard🇬🇧 · Christian T. Byrnes🇬🇧

    Phase transitions in the early universe lead to a reduction in the equation of state of the primordial plasma. This exponentially enhances the formation rate of primordial black holes. However, this sensitivity to the equation of state is the same that primordial black hole abundances show to the primordial curvature power spectrum amplitude. In this paper, we investigate peaked power spectra and show the challenges associated with motivating populations of primordial black holes with standard model enhancements. The parametrisation of different power spectra plays an important role in this discussion. The allowed parameter space consistent with a large QCD phase transition impact on the primordial black hole abundance differs greatly. This is particularly evident for broader spectra. We also show that, in our framework, the electroweak phase transition cannot significantly affect the overall abundance.

    ↳ astro-ph.COhep-phJCAP(2025)·16 citations
23. 23*

    $\omega$ meson from lattice QCD

    Haobo Yan🇨🇳 · Maxim Mai🇺🇸 · Marco Garofalo🇩🇪 · Ulf-G. Meißner🇩🇪 · Chuan Liu🇨🇳 · Liuming Liu🇨🇳 · Carsten Urbach🇩🇪

    Many excited states in the hadron spectrum have large branching ratios to three-hadron final states. Understanding such particles from first principles QCD requires input from lattice QCD with one-, two-, and three-meson interpolators as well as a reliable three-body formalism relating finite-volume spectra at unphysical pion mass values to the scattering amplitudes at the physical point. In this work, we provide the first-ever calculation of the resonance parameters of the $\omega$ meson from lattice QCD, including an update of the formalism through matching to effective field theories. The main result of this pioneering study, the pole position of the $\omega$ meson at $\sqrt{s_{\omega }}=(778.0(11.2)-i3.0(5))\mathrm{MeV}$, agrees reasonably well with experiment. In addition we provide an estimate of the $\omega -\rho$ mass difference as $29(15)\mathrm{MeV}$.

    ↳ hep-lathep-phnucl-thPRL(2024)·58 citations
24. 24*

    Robust Preference for Dynamical Dark Energy in DESI BAO and SN Measurements

    William Giarè🇬🇧 · Mahdi Najafi · Supriya Pan🇮🇳 · Eleonora Di Valentino🇬🇧 · Javad T. Firouzjaee🇮🇷

    Recent Baryon Acoustic Oscillation (BAO) measurements released by DESI, when combined with Cosmic Microwave Background (CMB) data from Planck and two different samples of Type Ia supernovae (Pantheon-Plus and DESY5) reveal a preference for Dynamical Dark Energy (DDE) characterized by a present-day quintessence-like equation of state that crossed into the phantom regime in the past. A core ansatz for this result is assuming a linear Chevallier-Polarski-Linder (CPL) parameterization $w(a)=w_0+w_a(1-a)$ to describe the evolution of the DE equation of state (EoS). In this paper, we test if and to what extent this assumption impacts the results. To prevent broadening uncertainties in cosmological parameter inference and facilitate direct comparison with the baseline CPL case, we focus on 4 alternative well-known models that, just like CPL, consist of only two free parameters: the present-day DE EoS ($w_0$) and a parameter quantifying its dynamical evolution ($w_a$). We demonstrate that the preference for DDE remains robust regardless of the parameterization: $w_0$ consistently remains in the quintessence regime, while $w_a$ consistently indicates a preference for a dynamical evolution towards the phantom regime. This tendency is significantly strengthened by DESY5 SN measurements. By comparing the best-fit ${\chi }^2$ obtained within each DDE model, we notice that the linear CPL parameterization is not the best-fitting case. Among the models considered, the EoS proposed by Barboza and Alcaniz consistently leads to the most significant improvement.

    ↳ astro-ph.COhep-phJCAP(2024)·231 citations
25. 25*

    The stellar distribution in ultra-faint dwarf galaxies suggests deviations from the collision-less cold dark matter paradigm

    Jorge Sanchez Almeida (1 and 2)🇪🇸 · Ignacio Trujillo (1 and 2) · Angel R. Plastino (3) ((1) Instituto de Astrofisica de Canarias, La Laguna, Tenerife, Spain, (2) Departamento de Astrofisica, Universidad de La Laguna, Spain, (3) CeBio y Departamento de Ciencias Basicas, UNNOBA, CONICET, Junin, Argentina)

    Unraveling the nature of dark matter (DM) stands as a primary objective in modern physics. Here we present evidence suggesting deviations from the collisionless Cold DM (CDM) paradigm. It arises from the radial distribution of stars in six Ultra Faint Dwarf (UFD) galaxies measured with the Hubble Space Telescope (HST). After a trivial renormalization in size and central density, the six UFDs show the same stellar distribution, which happens to have a central plateau or core. Assuming spherical symmetry and isotropic velocities, the Eddington inversion method proves the observed distribution to be inconsistent with potentials characteristic of CDM particles. Under such assumptions, the observed innermost slope of the stellar profile discards the UFDs to reside in a CDM potential at a > 97% confidence level. The extremely low stellar mass of these galaxies, 10**3-10**4 Msun , prevents stellar feedback from modifying the shape of a CDM potential. Other conceivable explanations for the observed cores, like deviations from spherical symmetry and isotropy, tidal forces, and the exact form of the used CDM potential, are disfavored by simulations and/or observations. Thus, the evidence suggests that collisions among DM particles or other alternatives to CDM are likely shaping these galaxies. Many of these alternatives produce cored gravitational potentials, shown here to be consistent with the observed stellar distribution.

    ↳ astro-ph.GAastro-ph.COhep-phApJL(2024)·23 citations

* Reconstructed cohort: no mailing for this day survives in the archive. Papers are grouped by their submission times and arXiv's announcement cut-off, assuming announcement without delay; positions follow identifier order. Validated at ~91% exact-day agreement against the archived era.