We present a complete calculation of the one-loop self-energies for all fields in the linear sigma model coupled to quarks at finite temperature and in the presence of a uniform magnetic field. The analysis consistently incorporates thermal and magnetic effects for both neutral and charged degrees of freedom, providing a unified framework valid for arbitrary values of the temperature and the field strength. The computation is performed using the Matsubara formalism to account for finite-temperature effects and the Schwinger proper-time representation for charged propagators in a magnetic background. Special attention is given to loop contributions involving particles with different electric charges, for which the associated Schwinger phases do not cancel. We show that these terms can be systematically evaluated in coordinate space using the Ritus formalism, which provides the appropriate framework for treating external charged states in the presence of a magnetic background, and consistently expressed in momentum space. The resulting expressions exhibit a nontrivial interplay between thermal fluctuations and magnetic effects and allow for a clear separation between vacuum and matter contributions, providing a well-defined structure for the identification of ultraviolet divergences. Our results establish a consistent and systematic framework for the computation of thermomagnetic one-loop corrections in effective models of QCD, capturing the full interplay between thermal and magnetic effects for all dynamical degrees of freedom.

Mexico

Adolfo Flores-Aguilar

Luis A. Hernández

J. Carlos Márquez

Chile

R. Zamora

Complete one-loop self-energies of the linear sigma model coupled to quarks at finite temperature and in a magnetic field

Gamma-ray bursts (GRBs) offer a powerful probe of the cosmic expansion history far beyond the redshift range accessible to Type Ia supernovae. However, the study of cosmological models using GRBs is hindered by the circularity problem, which arises from assuming a fiducial cosmological model during GRB luminosity distance calibration. In this work, we perform a model-independent calibration of GRB luminosity relations using observational measurements of the Hubble parameter from the A220 and J220 compilations, thereby avoiding explicit cosmological assumptions. We employ an artificial neural network to reconstruct the calibration relation directly from the data. In addition, we implement a Bayesian neural network framework as an alternative approach, enabling a data-driven treatment of both statistical and systematic uncertainties. We use calibrated GRB samples to constrain the Amati relation and systematically compare the outcomes obtained from different calibration techniques and datasets. We find that the Amati relation slopes derived from the two neural network approaches are consistent with each other and with previous low-redshift calibrations obtained using model-independent methods. The Bayesian Neural Network approach provides a more robust framework for propagating uncertainties in the calibration procedure.

India

Nilanjana Aurpa

Abha Habib

Nisha Rani

Reconstructing gamma-ray burst energy relations with observational $\textit{H}$($\textit{z}$) data in a neural network framework

We propose a radiative Dirac neutrino mass model stabilized by a noninvertible fusion rule originating from a <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>Z</mi><mn>3</mn></msub><mo>×</mo><msubsup><mi>Z</mi><mn>3</mn><mo>′</mo></msubsup></math> gauging. The imposed symmetry forbids tree-level Yukawa couplings and ensures that neutrino masses are generated only at the one-loop level through the exchange of exotic fermions and inert scalars. This minimal framework simultaneously accommodates neutrino masses and mixings consistent with current oscillation data, while providing a viable dark matter candidate. We analyze lepton flavor violating processes and lepton anomalous magnetic moments, finding that all contributions remain well below present experimental bounds. In the dark matter sector, the bosonic singlet emerges as a promising candidate with relic density compatible with cosmological observations, whereas the fermionic option is strongly disfavored due to suppressed annihilation cross sections. Our study demonstrates that noninvertible fusion rules can serve as a powerful organizing principle for constructing minimal and phenomenologically consistent extensions of the Standard Model, linking neutrino physics and dark matter within a unified radiative framework.

China

Hiroshi Okada

Labh Singh

Dirac one-loop seesaw mechanism with a noninvertible fusion rule

We phenomenologically calculate direct-detection constraints on inelastic dark matter (DM) for a scalar portal scenario with leptophilic couplings. The p-wave velocity suppression of the annihilation cross section of scalar-mediated inelastic Dirac DM implies the opening of viable regions of DM parameter space in the MeV-GeV mass range. Xenon-based experiments can provide a constraints on scalar-mediated inelastic fermion dark matter for sub-MeV mass splitting, via endothermic and exothermic spin-independent DM-electron scattering. To estimate the relevant constraints, we use public data from the XENON1T, PandaX-4T, and LUX-ZEPLIN liquid-xenon experiments that measure ionization electron signals.

Russia

I.V. Voronchikhin

D.V. Kirpichnikov

Direct-detection constraints on inelastic dark matter with a scalar mediator

We analyze the potential of the Universal SMEFT as a tool to study universal new physics in the neutral and charged Drell-Yan processes at the high-luminosity LHC. In order to do so, we generated pseudodata containing the contributions of beyond the standard model vector bosons to the dilepton production. Our results show that fits with the minimal theoretical bias can be used not only to unveil the existence of new physics but also to accurately extract its properties. Moreover, the results are rather stable with respect to the order of truncation of the effective field theory.

Austria

Tyler Corbett

United States

Jay Desai

Brazil

O.J.P. Éboli

Spain

M.C. Gonzalez-Garcia

Matheus Martines

Universal SMEFT as a tool for discovery of universal new physics at the high luminosity LHC

We investigate the charmonium-nucleon interaction, focusing on its connection with the internal structure of the nucleon encoded in the gravitational form factors. To describe this interaction, we employ an effective potential based on the QCD multipole expansion within the leading chromoelectric dipole approximation. In this framework, the potential is expressed in terms of the energy and pressure distributions inside the nucleon. We first construct these distributions from the gravitational form factors fitted to lattice-QCD data. The remaining model parameters are then fixed by requiring that the resulting ***<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi>J</mi><mo>/</mo><mi>ψ</mi><mtext>−</mtext><mi>N</mi></mrow></math> potential reproduce the Hadrons to Atomic nuclei from Lattice QCD (HAL QCD) potential outside the short-distance region, as well as the scattering phase shift estimated from the HAL QCD data. Based on this potential, we evaluate the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>J</mi><mo>/</mo><mi>ψ</mi><mtext>−</mtext><mi>N</mi></math> correlation function and further investigate the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>ψ</mi><mo stretchy="false">(</mo><mn>2</mn><mi>S</mi><mo stretchy="false">)</mo><mtext>−</mtext><mi>N</mi></math> system. We then examine the sensitivity of these correlation functions to the nucleon <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>D</mi></math>-form factor.

Japan

Ren Ejima

Daisuke Fujii

Mamiya Kawaguchi

Charmonium-nucleon femtoscopy as a possible probe of the nucleon gravitational form factor

We apply the soft photon approximation to QED processes in a strong plane-wave laser field. New compact expressions for the emission factors are presented, which simplify the generalization to multiple soft photon emission. The method is applied to nonlinear single, double, and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>N</mi></math>-photon Compton scattering. For single Compton scattering, we show that the soft photon approximation reproduces the exact spectrum with accuracy <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi mathvariant="script">O</mi><mo stretchy="false">(</mo><mi>ω</mi><mo>/</mo><mi>ϵ</mi><mo stretchy="false">)</mo></math>, significantly outperforming the classical radiation theory. For double Compton scattering, we derive analytical expressions for the differential probability in two kinematic regimes: when both photons are soft, and when one photon is soft while the other has arbitrary energy. We present a compact analytical expression for the amplitude of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>N</mi></math>-photon emission within the soft photon approximation. A numerical implementation in wolfram mathematica for single and double Compton scattering is provided.

Peter A. Krachkov

Simon V. Sorokin

Soft photon approximation in a laser field: Applications

The first observation of a new meson state decaying into <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>B</mi><mi>c</mi><mo>+</mo></msubsup></math> and a photon is presented using a dataset of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>p</mi><mi>p</mi></math> collisions at a center-of-mass energy <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msqrt><mrow><mi>s</mi></mrow></msqrt><mo>=</mo><mn>13</mn><mtext> </mtext><mtext> </mtext><mi>TeV</mi></mrow></math> collected by the ATLAS detector at the Large Hadron Collider, corresponding to an integrated luminosity of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>140</mn><mtext> </mtext><mtext> </mtext><msup><mi>fb</mi><mrow><mo>−</mo><mn>1</mn></mrow></msup></math>. The <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>B</mi><mi>c</mi><mo>+</mo></msubsup></math> mesons are reconstructed from a three-muon final state from <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>B</mi></mrow><mrow><mi>c</mi></mrow><mrow><mo>+</mo></mrow></msubsup><mo stretchy="false">→</mo><mi>J</mi><mo>/</mo><mi>ψ</mi><mo stretchy="false">(</mo><msup><mrow><mi>μ</mi></mrow><mrow><mo>+</mo></mrow></msup><msup><mrow><mi>μ</mi></mrow><mrow><mo>−</mo></mrow></msup><mo stretchy="false">)</mo><msup><mrow><mi>μ</mi></mrow><mrow><mo>+</mo></mrow></msup><msub><mrow><mi>ν</mi></mrow><mrow><mi>μ</mi></mrow></msub><mi>X</mi></mrow></math> decays, along with photons reconstructed via conversions to electron-positron pairs in the detector material. The new state is observed with a significance that exceeds 8 standard deviations. The mass difference between the new meson state and the ground-state <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>B</mi></mrow><mrow><mi>c</mi></mrow><mrow><mo>+</mo></mrow></msubsup></mrow></math> meson is measured to be <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>64.5</mn><mo>±</mo><mn>1.4</mn><mrow><mo stretchy="false">(</mo><mi>stat</mi><mo stretchy="false">)</mo></mrow><msubsup><mrow><mtext> </mtext></mrow><mrow><mo>−</mo><mn>1.4</mn></mrow><mrow><mo>+</mo><mn>1.0</mn></mrow></msubsup><mo stretchy="false">(</mo><mi>syst</mi><mo stretchy="false">)</mo><mtext> </mtext><mtext> </mtext><mi>MeV</mi></mrow></math>. This corresponds to a mass for the observed state of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>6339.0</mn><mo>±</mo><mn>1.4</mn><mrow><mo stretchy="false">(</mo><mi>stat</mi><mo stretchy="false">)</mo></mrow><msubsup><mrow><mtext> </mtext></mrow><mrow><mo>−</mo><mn>1.4</mn></mrow><mrow><mo>+</mo><mn>1.0</mn></mrow></msubsup><mrow><mo stretchy="false">(</mo><mi>syst</mi><mo stretchy="false">)</mo></mrow><mo>±</mo><mn>0.3</mn><mrow><mo stretchy="false">(</mo><msub><mrow><mi>m</mi></mrow><mrow><msubsup><mrow><mi>B</mi></mrow><mrow><mi>c</mi></mrow><mrow><mo>+</mo></mrow></msubsup></mrow></msub><mo stretchy="false">)</mo></mrow><mtext> </mtext><mtext> </mtext><mtext> </mtext><mi>MeV</mi></mrow></math>, where the last uncertainty is due to the precision of the best knowledge of the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>B</mi><mi>c</mi><mo>+</mo></msubsup></math> meson mass. The low mass difference value matches the theory expectations for the lowest vector state of the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mover accent="true"><mi>b</mi><mo stretchy="false">¯</mo></mover><mi>c</mi></math> system, the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>B</mi></mrow><mrow><mi>c</mi></mrow><mrow><mo>*</mo><mo>+</mo></mrow></msubsup></mrow></math> meson.

France

G. Aad

Norway

E. Aakvaag

B. Abbott

United Arab Emirates

S. Abdelhameed

Germany

K. Abeling

N.J. Abicht

S.H. Abidi

M. Aboelela

Morocco

A. Aboulhorma

Israel

H. Abramowicz

Italy

B.S. Acharya

A. Ackermann

Switzerland

J. Ackerschott

C. Adam Bourdarios

Poland

L. Adamczyk

S.V. Addepalli

United Kingdom

M.J. Addison

J. Adelman

Türkiye

A. Adiguzel

T. Adye

A.A. Affolder

Y. Afik

M.N. Agaras

A. Aggarwal

Romania

C. Agheorghiesei

A. Ahmad

F. Ahmadov

S. Ahuja

X. Ai

G. Aielli

A. Aikot

M. Ait Tamlihat

Sweden

T.P.A. Åkesson

D. Akiyama

N.N. Akolkar

S. Aktas

G.L. Alberghi

Canada

J. Albert

U. Alberti

P. Albicocco

S. Alderweireldt

Z.L. Alegria

CERN

M. Aleksa

I.N. Aleksandrov

C. Alexa

Greece

T. Alexopoulos

F. Alfonsi

M. Algren

M. Alhroob

Czechia

B. Ali

H.M.J. Ali

S. Ali

S.W. Alibocus

South Africa

M. Aliev

G. Alimonti

C. Allaire

B.M.M. Allbrooke

D.R. Allen

J.S. Allen

J.F. Allen

Australia

C.S. Alley

E.R. Almazan

A. Aloisio

Argentina

F. Alonso

C. Alpigiani

A. Alvarez Fernandez

M. Alves Cardoso

M.G. Alviggi

Y. Amaral Coutinho

C. Amelung

M. Amerl

T. Amezza

B. Amini

K. Amirie

A. Amirkhanov

D. Amperiadou

C. Anastopoulos

T. Andeen

J.K. Anders

A.C. Anderson

A. Andreazza

S. Angelidakis

A. Angerami

A.V. Anisenkov

A. Annovi

C. Antel

E. Antipov

M. Antonelli

F. Anulli

M. Aoki

T. Aoki

M.A. Aparo

L. Aperio Bella

M. Apicella

C. Appelt

A. Apyan

R. Arakida

M. Arampatzi

S.J. Arbiol Val

C. Arcangeletti

Observation of a <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>B</mi></mrow><mrow><mi>c</mi></mrow><mrow><mo>*</mo><mo>+</mo></mrow></msubsup></mrow></math> Meson with the ATLAS Detector

We report on measurements of axion spectra and their unequal time correlators in simulations on <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msup><mrow><mn>12</mn><mtext> </mtext><mn>288</mn></mrow><mrow><mn>3</mn></mrow></msup></mrow></math> fixed grids, the largest such measurements to date. We use a novel combination of the fields that allow us to better distinguish the contributions from propagating axions from the contributions from strings, showing that previous measurements of the axion energy spectrum are approximately 30% derived from the string fields. We conclude that axion emission from a scaling string network is close to scale invariant (<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>q</mi><mo>≳</mo><mn>1</mn></math> in the standard parametrization), and that the energy spectrum of subhorizon modes behaves as <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>p</mi></mrow><mrow><mi>ax</mi></mrow></msub><mi>ln</mi><mo stretchy="false">(</mo><mi>k</mi><mi>τ</mi><mo stretchy="false">)</mo></mrow></math>, where <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>k</mi></math> is the comoving wave number, <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>τ</mi></math> the conformal time, and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>p</mi><mi>ax</mi></msub><mo>≃</mo><mn>10</mn></math>. The number density spectrum evolves towards a single curve for <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>k</mi><mi>τ</mi><mo>≲</mo><msup><mn>10</mn><mn>2</mn></msup></math>, with higher wave number deviations arising from initial conditions and resonant axion production at the string width scale. Our results are consistent with scaling framework, in which the total number density of axions produced from strings is <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>n</mi></mrow><mrow><mi>ax</mi></mrow></msub><mo>=</mo><mn>1.66</mn><mo stretchy="false">(</mo><mn>17</mn><mo stretchy="false">)</mo><msubsup><mrow><mi>f</mi></mrow><mrow><mi mathvariant="normal">a</mi></mrow><mrow><mn>2</mn></mrow></msubsup><mi>H</mi></mrow></math>, where <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>f</mi><mi mathvariant="normal">a</mi></msub></math> is the axion decay constant and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>H</mi></math> the Hubble rate. To interpret these results, we develop a simple analytic model based on an ensemble of string segments. The model reproduces the main features of the measured spectra and unequal-time correlators, and predicts <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>q</mi><mo>≤</mo><mn>1</mn></math>, leaving <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>q</mi><mo>=</mo><mn>1</mn></math> as the only value consistent with theory and measurement. We report on axion production from the final collapse of the network in a future work.

Finland

José Correia

Mark Hindmarsh

Joanes Lizarraga

Asier Lopez-Eiguren

Kari Rummukainen

Jon Urrestilla

Spectrum of axions in a scaling string network

We update the analysis of minimal supersymmetric <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>S</mi><mi>O</mi><mo stretchy="false">(</mo><mn>10</mn><mo stretchy="false">)</mo></math> grand unification with a universal, constrained-minimal supersymmetric Standard Model (MSSM)-like soft-breaking spectrum. A pair of Yukawa matrices in the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn mathvariant="bold">10</mn><mo stretchy="false">⊕</mo><mover accent="true"><mn mathvariant="bold">126</mn><mo stretchy="true">¯</mo></mover></math> Higgs sector fixes the charged fermion masses and quark mixing, the baryon number-violating dimension-five operators that mediate proton decay, and the right-handed neutrino Majorana masses of the type-I seesaw. The simultaneously imposed constraints include: (i) gauge coupling unification and vacuum stability; (ii) dimension-five proton decay (the dimension-six gauge mode also computed and negligible), the 125-GeV Higgs mass, and the Large Electron-Positron chargino limit; and (iii) <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>μ</mi><mo stretchy="false">→</mo><mi>e</mi><mi>γ</mi></math>, the muon <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>g</mi><mo>−</mo><mn>2</mn></math>, and electric dipole moments. We perform a global scan over the soft-breaking parameters, complemented by a constrained-<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>μ</mi></math> cross-check that fixes the electroweakino sector from the grand unified theory (GUT)-scale boundary conditions through radiative electroweak symmetry breaking. Subject to a single effective colored Higgs scale <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><msub><mi>H</mi><mi>C</mi></msub></msub></math> for the proton decay normalization (common to unification and decay, though in a general color triplet mass matrix the two can differ) and to a constrained-<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>μ</mi></math> treatment, what survives is a narrow minisplit region: heavy, multitens-of-TeV scalars with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>m</mi><mn>0</mn></msub><mo>≳</mo><mn>11.0</mn><mtext> </mtext><mtext> </mtext><mi>TeV</mi></math> for a dressing electroweakino mass <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>m</mi><mi>χ</mi></msub><mo>=</mo><mn>1</mn><mtext> </mtext><mtext> </mtext><mi>TeV</mi></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>tan</mi><mi>β</mi><mo>≲</mo><msubsup><mn>8.0</mn><mrow><mo>−</mo><mn>2.0</mn></mrow><mrow><mo>+</mo><mn>5.5</mn></mrow></msubsup></math>, the uncertainty being the Higgs mass theory error. We also examine the fate of the lightest supersymmetric particle as a dark matter candidate, in both the universal model and its free-<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>μ</mi></math> nonuniversal-Higgs-mass extension. The surviving region is sharply bounded and testable in the coming decade, most directly by Hyper-Kamiokande proton decay and electroweakino searches, with dark matter direct detection and electric dipole moment experiments.

Cheng-Wei Chiang

Takeshi Fukuyama

Updated analysis of minimal supersymmetric <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>S</mi><mi>O</mi><mo stretchy="false">(</mo><mn>10</mn><mo stretchy="false">)</mo></math> with a universal soft spectrum