We study the new $Z'$ boson as a portal for the production of Higgs bosons $h_0$ and $H_0$ predicted by the Bestest Little Higgs Model through Higgs-strahlung processes $\mu^+\mu^- \to (Z, Z') \to Zh_0, ZH_0$ . We focus on the resonant and nonresonant effects of the $Zh_0, ZH_0$ signals. In our analysis, we consider the center-of-mass energies of $\sqrt{s}=3, 4, 6, 10, 30$ TeV and integrated luminosities of ${\cal{L}}=2, 4, 6, 10, 30$ ${ {\rm{ab}}^{-1}}$ projected for a future muon collider. The possibility of performing precision measurements for Higgs bosons $h_0$ and $H_0$ is very promising for the future muon collider. Furthermore, our results may be useful to the High Energy Physics community. Complementarily, we generate and provide the Feynman rules necessary for studying processes $\mu^+\mu^- \to (Z, Z') \to Zh_0, ZH_0$ .

J.M. Martínez-Martínez

A. Gutiérrez-Rodríguez

E. Cruz-Albaro

M.A. Hernández-Ruíz

New $\textit{Z}$' boson of the bestest little Higgs model as a portal to signatures of Higgs bosons $\textit{h}$ $_{0}$ and $\textit{H}$ $_{0}$ at the future muon collider

The <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>X</mi><mo stretchy="false">(</mo><mn>3872</mn><mo stretchy="false">)</mo></math>, as the first and the most crucial member in the exotic charmoniumlike <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>X</mi><mi>Y</mi><mi>Z</mi></math> family, has been studied for a long time. However, its dynamical origin, whether stemming from a <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>D</mi><msup><mover accent="true"><mi>D</mi><mo stretchy="false">¯</mo></mover><mo>*</mo></msup></math> hadronic molecule or the first excited <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>P</mi></math>-wave charmonium <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>χ</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub><mo stretchy="false">(</mo><mn>2</mn><mi>P</mi><mo stretchy="false">)</mo></math>, remains controversial. In this Letter, we demonstrate that the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>X</mi><mo stretchy="false">(</mo><mn>3872</mn><mo stretchy="false">)</mo></math> definitely does not result from the mass shift of the higher bare <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>χ</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub><mo stretchy="false">(</mo><mn>2</mn><mi>P</mi><mo stretchy="false">)</mo></math> resonance pole in the coupled-channel dynamics involving a short-distance <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>c</mi><mover accent="true"><mi>c</mi><mo stretchy="false">¯</mo></mover></math> core and the long-distance <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>D</mi><msup><mover accent="true"><mi>D</mi><mo stretchy="false">¯</mo></mover><mo>*</mo></msup></math> channels. Instead, it originates from either the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>D</mi><msup><mover accent="true"><mi>D</mi><mo stretchy="false">¯</mo></mover><mo>*</mo></msup></math> molecular pole or the shadow pole associated with the antiresonance of the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>P</mi></math>-wave charmonium, depending on the weak or strong coupling mode, respectively. To differentiate these origins and fully exploit the nature of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>X</mi><mo stretchy="false">(</mo><mn>3872</mn><mo stretchy="false">)</mo></math>, we conduct a comprehensive analysis in a couple-channel dynamics framework, including the isospin violation, the three-body <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>D</mi><mover accent="true"><mi>D</mi><mo stretchy="false">¯</mo></mover><mi>π</mi></math> effect, the dynamical width of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>D</mi><mo>*</mo></msup></math>, and nonopen-charm decays of the bare <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>χ</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub><mo stretchy="false">(</mo><mn>2</mn><mi>P</mi><mo stretchy="false">)</mo></math>. Our findings highlight the pivotal role of the coupled-channel dynamics in explaining the disparity between the pole widths of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>X</mi><mo stretchy="false">(</mo><mn>3872</mn><mo stretchy="false">)</mo></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>T</mi><mrow><mi>c</mi><mi>c</mi></mrow><mo>+</mo></msubsup></math>, while also predicting a new resonance with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>J</mi><mrow><mi>P</mi><mi>C</mi></mrow></msup><mo>=</mo><msup><mn>1</mn><mrow><mo>+</mo><mo>+</mo></mrow></msup></math> around 4.0 GeV. By matching the newly observed <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>χ</mi><mrow><mi>c</mi><mn>1</mn></mrow></msub><mo stretchy="false">(</mo><mn>4010</mn><mo stretchy="false">)</mo></math> by the LHCb Collaboration to our predicted resonance, we conclude that the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>X</mi><mo stretchy="false">(</mo><mn>3872</mn><mo stretchy="false">)</mo></math> most likely originates from the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>D</mi><msup><mover accent="true"><mi>D</mi><mo stretchy="false">¯</mo></mover><mo>*</mo></msup></math> pole with a confidence level exceeding 99.7%.

China

Jun-Zhang Wang

Zi-Yang Lin

Yan-Ke Chen

Germany

Lu Meng

Shi-Lin Zhu

Uncovering the mystery of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>X</mi><mo stretchy="false">(</mo><mn>3872</mn><mo stretchy="false">)</mo></math> with the coupled-channel dynamics

We present a novel way to probe inelastic dark matter using cosmic-ray (CR) cooling in active galactic nuclei (AGNs). Dark matter (DM) in the vicinity of supermassive black holes may scatter off CRs, resulting in the rapid cooling of CRs for sufficiently large cross sections. This in turn can alter the high-energy neutrino and gamma-ray fluxes detected from these sources. We show that AGN cooling bounds obtained through the multimessenger data of NGC 1068 and TXS <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>0506</mn><mo>+</mo><mn>056</mn></mrow></math> allows us to reach unprecedently large mass splittings for inelastic DM (<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mo>≳</mo><mi>TeV</mi></math>), orders of magnitude larger than those probed by direct detection experiments and DM capture in neutron stars. Furthermore, we demonstrate that cooling bounds from AGNs can probe thermal light DM with small mass splittings. This provides novel and complementary constraints in parts of a parameter space accessible solely by colliders and beam-dump experiments.

United States

Japan

R. Andrew Gustafson

Gonzalo Herrera

Mainak Mukhopadhyay

Kohta Murase

Ian M. Shoemaker

Cosmic-ray cooling in active galactic nuclei as a new probe of inelastic dark matter

CubeSat technology is an emerging alternative to large-scale space telescopes due to its short development time and cost effectiveness. MeVCube is a proposed CubeSat mission to study the least explored MeV gamma-ray sky, also known as the “MeV gap.” Besides being sensitive to a plethora of astrophysical phenomena, MeVCube can also be important in the hunt for dark matter. If dark matter is made up of evaporating primordial black holes, then it can produce photons in the sensitivity range of MeVCube. Besides, particle dark matter can also decay or annihilate to produce final state gamma-ray photons. We perform the first comprehensive study of dark matter discovery potential of a near-future MeVCube CubeSat mission. In all cases, we find that MeVCube will have much better discovery reach compared to existing limits in the parameter space. This may be an important step towards discovering dark matter through its nongravitational interactions.

India

Akash Kumar Saha

Searching for dark matter with MeVCube

We study the impact of the non-holomorphic (NH) soft supersymmetry-breaking terms <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msubsup><mrow><mi>T</mi></mrow><mrow><mn>33</mn></mrow><mrow><mo>′</mo><mi>D</mi></mrow></msubsup></mrow></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>μ</mi><mo>′</mo></msup></math>, which introduce additional supersymmetry-breaking effects beyond the holomorphic structure of the superpotential, on the Higgs boson mass spectrum in the NH Minimal Supersymmetric Standard Model. The term <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>T</mi><mn>33</mn><mrow><mo>′</mo><mi>D</mi></mrow></msubsup></math> modifies the scalar bottom-quark mass matrix and Higgs couplings, while <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>μ</mi><mo>′</mo></msup></math> affects the mass matrices of charginos and neutralinos. In our analysis, we incorporate constraints from charge- and color-breaking minima where we find that a portion of the parameter space is excluded by these constraints. Focusing on the allowed parameter space, the NH contributions to the light <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi mathvariant="script">C</mi><mi mathvariant="script">P</mi></mrow></math>-even Higgs boson mass <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><mi>h</mi></msub></math> from <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>μ</mi><mo>′</mo></msup></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>T</mi><mn>33</mn><mrow><mo>′</mo><mi>D</mi></mrow></msubsup></math> can reach up to 1.4 GeV and 90 MeV, respectively. For the heavy <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mi mathvariant="script">C</mi><mi mathvariant="script">P</mi></mrow></math>-even Higgs boson mass <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><mi>H</mi></msub></math> and the charged Higgs boson mass <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><msup><mi>H</mi><mo>±</mo></msup></msub></math>, these contributions can be substantially larger in certain regions of the parameter space, reaching up to 44 GeV for <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><mi>H</mi></msub></math> and 42 GeV for <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><msup><mi>H</mi><mo>±</mo></msup></msub></math> due to <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>μ</mi><mo>′</mo></msup></math> and up to 60 GeV due to <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>T</mi><mn>33</mn><mrow><mo>′</mo><mi>D</mi></mrow></msubsup></math> for both <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><mi>H</mi></msub></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>M</mi><msup><mi>H</mi><mo>±</mo></msup></msub></math>. These corrections are significantly larger than the expected future experimental precision for Higgs boson masses and should therefore be considered in precision analyses for future experiments.

Pakistan

M. Rehman

Spain

S. Heinemeyer

Toward a refined understanding of nonholomorphic soft SUSY-breaking effects on the Higgs boson mass spectra

Searching for exotic interactions beyond the standard model of particle physics may solve some of the current puzzles in physics. Here, the authors experimentally explore a spin- and velocity-dependent exotic interaction between the nucleons in a gold sphere and the electrons in a spin source in the micrometer range. The microfabricated spin source provides periodically varying spin density of electrons, resulting in a periodic exotic field. A cantilever glued with a gold sphere is used to measure the force acting on the gold sphere by the spin source. The spin source is driven to oscillate, and then, the imaginary component of the signal is extracted at the 10th harmonic of the oscillation frequency, which effectively separates the exotic interaction from the spurious forces commonly present in such short-range measurements. No signal of the exotic interaction is observed, then, new limits on the coupling constant are set in the interaction range below <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>10</mn><mtext> </mtext><mtext> </mtext><mi mathvariant="normal">μ</mi><mrow><mi mathvariant="normal">m</mi></mrow></mrow></math>, with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msub><mrow><mi>f</mi></mrow><mrow><mo>⊥</mo></mrow></msub><mo>≤</mo><mn>2.2</mn><mo>×</mo><msup><mrow><mn>10</mn></mrow><mrow><mo>−</mo><mn>9</mn></mrow></msup></mrow></math> at <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>2.1</mn><mtext> </mtext><mtext> </mtext><mi mathvariant="normal">μ</mi><mrow><mi mathvariant="normal">m</mi></mrow></mrow></math>.

Sumin Li

Wenbo Zhang

Rui Luo

Jinquan Liu

Pengshun Luo

Improved Limits on the Spin- and Velocity-Dependent Exotic Interaction in the Micrometer Range

Considering the Einstein-Hilbert truncation for the running action in (Euclidean) quantum gravity, we derive the renormalization group equations for the cosmological and Newton constant. We find that these equations admit only the Gaussian fixed point with a UV-attractive and a UV-repulsive eigendirection, and that there is no sign of the nontrivial UV-attractive fixed point of the asymptotic safety scenario. Crucial to our analysis is a careful treatment of the measure in the path integral that defines the running action and a proper introduction of the physical running scale <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>k</mi></math>. We also show why and how in usual implementations of the RG equations the aforementioned UV-attractive fixed point is generated.

Italy

Carlo Branchina

Vincenzo Branchina

Filippo Contino

Arcangelo Pernace

Path integral measure and RG equations for gravity

We propose the possibility of using the near detector at reactor neutrino experiments to probe the renormalization group (RG) running effect on the leptonic Dirac <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>C</mi><mi>P</mi></math> phase <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>δ</mi><mi>D</mi></msub></math>. Although the reactor neutrino oscillation cannot directly measure <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>δ</mi><mi>D</mi></msub></math>, it can probe the deviation <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi mathvariant="normal">Δ</mi><mi>δ</mi><mo>≡</mo><msub><mi>δ</mi><mi>D</mi></msub><mo stretchy="false">(</mo><msubsup><mi>Q</mi><mi>d</mi><mn>2</mn></msubsup><mo stretchy="false">)</mo><mo>−</mo><msub><mi>δ</mi><mi>D</mi></msub><mo stretchy="false">(</mo><msubsup><mi>Q</mi><mi>p</mi><mn>2</mn></msubsup><mo stretchy="false">)</mo></math> caused by the RG running. Being a key element, the mismatched momentum transfers at neutrino production (<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>Q</mi><mi>p</mi><mn>2</mn></msubsup></math>) and detection (<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>Q</mi><mi>d</mi><mn>2</mn></msubsup></math>) processes can differ by two orders. We illustrate this concept with the upcoming Taishan Antineutrino Observatory (TAO, also known as JUNO-TAO) experiment and obtain the projected sensitivity to the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>C</mi><mi>P</mi></math> RG running beta function <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>β</mi><mi>δ</mi></msub></math>.

Shao-Feng Ge

Chui-Fan Kong

Brazil

Pedro Pasquini

Testing the RG running of the leptonic Dirac <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>C</mi><mi>P</mi></math> phase with reactor neutrinos

Cosmological scalar fields coupled to the Standard Model drive temporal variations in the fundamental constants that grow with redshift, positioning the early Universe as a powerful tool to study such models. We investigate the dynamics and phenomenology of coupled scalars from the early Universe to the present to consistently leverage the myriad searches for time-varying constants and the cosmological signatures of scalars’ gravitational effects. We compute the in-medium contribution from Standard Model particles to the scalar’s dynamics and identify only a limited range of couplings for which the scalar has an observable impact on the fundamental constants without either evolving before recombination or gravitating non-negligibly. We then extend existing laboratory and astrophysical bounds to the hyperlight scalar regime. We present joint limits from the early and late Universe, specializing to hyperlight, quadratically coupled scalars that modulate the mass of the electron or the strength of electromagnetism and make up a subcomponent of the dark matter today. Our dedicated analysis of observations of the cosmic microwave background, baryon acoustic oscillations, and type Ia supernovae provides the most stringent constraints on quadratically coupled scalars with masses from <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mn>10</mn><mrow><mo>−</mo><mn>28.5</mn></mrow></msup></math> to <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mo>∼</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>31</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>, below which quasar absorption spectra yield stronger bounds. These results jointly limit hyperlight scalars that comprise a few percent of the current dark matter density to near- or subgravitational couplings to electrons or photons.

Masha Baryakhtar

Olivier Simon

Canada

Zachary J. Weiner

Searching for coupled, hyperlight scalars across cosmic history

We use the recently proposed supersymmetric expansion algorithm to obtain a complete analytical solution to the Schrödinger equation with the Cornell potential. We find that the energy levels <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>E</mi><mrow><mi>n</mi><mi>l</mi></mrow></msub><mo stretchy="false">(</mo><mi>λ</mi><mo stretchy="false">)</mo></math> depend on <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>n</mi><mn>2</mn></msup></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mi>L</mi><mn>2</mn></msup><mo>=</mo><mi>l</mi><mo stretchy="false">(</mo><mi>l</mi><mo>+</mo><mn>1</mn><mo stretchy="false">)</mo></math>. For a given <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>n</mi></math>, the energy decreases with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>l</mi></math> and the radial probabilities have the Coulomb shape but their peaks are shifted toward smaller radius. We study the heavy quarkonium structure on the light of these results, showing that the measured <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mover accent="true"><mi>b</mi><mo stretchy="false">¯</mo></mover><mi>b</mi></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mover accent="true"><mi>c</mi><mo stretchy="false">¯</mo></mover><mi>c</mi></math> meson masses follow the inverted spectrum pattern predicted by the Cornell potential. Details of the structure of heavy quarkonium like the mean inverse radius and mean squared velocity for the different quarkonium configurations can be obtained from our solution. These details point to significant relativistic corrections for all the configurations of real heavy quarkonium. We calculate relativistic corrections using perturbation theory finding an expansion in <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msubsup><mi>α</mi><mi>s</mi><mn>2</mn></msubsup></math> for the heavy quarkonium masses. The mass hierarchies in the fine splittings can be qualitatively understood from this expansion. The quantitative analysis of the Bohr-like levels and of the fine splittings in the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>l</mi><mo>=</mo><mn>0</mn></math> sector allow us to make well-defined predictions for the masses of some of the missing heavy quarkonium states, to identify the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>ψ</mi><mo stretchy="false">(</mo><mn>4040</mn><mo stretchy="false">)</mo></math> as the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mn>3</mn><mn>3</mn></msup><msub><mi>S</mi><mn>1</mn></msub></math> <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mover accent="true"><mi>c</mi><mo stretchy="false">¯</mo></mover><mi>c</mi></math> state and the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>ψ</mi><mo stretchy="false">(</mo><mn>3842</mn><mo stretchy="false">)</mo></math>, <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>ψ</mi><mo stretchy="false">(</mo><mn>3823</mn><mo stretchy="false">)</mo></math> and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>ψ</mi><mo stretchy="false">(</mo><mn>3770</mn><mo stretchy="false">)</mo></math> as the <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mn>3</mn><mn>3</mn></msup><msub><mi>D</mi><mn>3</mn></msub></math>, <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mn>3</mn><mn>3</mn></msup><msub><mi>D</mi><mn>2</mn></msub></math>, and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msup><mn>3</mn><mn>3</mn></msup><msub><mi>D</mi><mn>1</mn></msub></math> <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mover accent="true"><mi>c</mi><mo stretchy="false">¯</mo></mover><mi>c</mi></math> states, respectively.

Mexico

M. Napsuciale

S. Rodríguez

A.E. Villanueva-Gutiérrez

Complete analytical solution to the Cornell potential and heavy quarkonium structure