To give more credence to the M-theoretic Emergence Proposal it is important to show that also classical kinetic terms in a low energy effective action arise as a quantum effect from integrating out light towers of states. We show that for compactifications of type IIA on Calabi-Yau manifolds, the classical weak coupling Yukawa couplings, which are the triple intersection numbers of the Calabi-Yau threefold, can be obtained from the 1/2-BPS protected one-loop Schwinger integral over $\textit{D}$2-$\textit{D}$0 bound states, after employing a novel regularization for the final infinite sum of Gopakumar-Vafa invariants. Approaching the problem in a consecutive manner from 6D decompactification over emergent string to the ultimate M-theory limits, we arrive at a mathematically concrete regularization that involves finite distance degeneration limits of Calabi-Yau threefolds in an intriguing way. We test and challenge this proposal by the concrete determination of the periods around such degeneration points for threefolds with one Kähler modulus and the two examples $\textit{ℙ}$ [18] and $\textit{ℙ}$ [12].

Germany

Ralph Blumenhagen

Aleksandar Gligovic

Emergence of CY triple intersection numbers in M-theory

Axionlike particles (ALPs), hypothetical particles beyond the Standard Model (SM), are considered as promising dark matter candidates. ALPs can convert into photons and vice versa in a magnetic field via the Primakoff effect, potentially generating detectable oscillation in <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>γ</mi></math>-ray spectra. This study analyzes 16.5 years of data from the Fermi Large Area Telescope (Fermi-LAT) on NGC 1275, the brightest galaxy in the Perseus cluster, to constrain the ALP parameter space. Our results improve the previous 95% exclusion limits of the photon-ALP coupling <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi></mrow></msub></math> by a factor of 2 in the ALP mass range of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>4</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>10</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi><mo>≲</mo><msub><mi>m</mi><mi>a</mi></msub><mo>≲</mo><mn>5</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>9</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>. Moreover, we investigate the projected sensitivity of the future Very Large Area <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>γ</mi></math>-ray Space Telescope (VLAST) on searching for ALPs. We find that (i) the expected sensitivity on the photon-ALP coupling <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi></mrow></msub></math> can be stronger than that from the upcoming International Axion Observatory in the ALP mass range of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>2</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>11</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi><mo>≲</mo><msub><mi>m</mi><mi>a</mi></msub><mo>≲</mo><mn>1</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>7</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>, with the best sensitivity of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi></mrow></msub><mo>∼</mo><mn>7</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>13</mn></mrow></msup><mtext> </mtext><mtext> </mtext><msup><mrow><mi>GeV</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math> at <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>m</mi><mi>a</mi></msub><mo>∼</mo><mn>2</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>10</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>; (ii) VLAST can extend the sensitivity of the ALP masses below <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>5</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>12</mn></mrow></msup><mtext> </mtext><mtext> </mtext><mi>eV</mi></math>, where the photon-ALP coupling <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi></mrow></msub><mo>≳</mo><mn>1.5</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>11</mn></mrow></msup><mtext> </mtext><mtext> </mtext><msup><mrow><mi>GeV</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math> will be excluded; (iii) the entire parameter space of ALP accounting for TeV transparency can be fully tested. These results demonstrate that VLAST will offer an excellent opportunity for ALPs searches.

China

Zhi-Qi Guo

Yue-Lin Sming Tsai

Lei Wu

Zi-Qing Xia

Constraints on axionlike particles from 16.5 years of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mi>F</mi><mi>e</mi><mi>r</mi><mi>m</mi><mi>i</mi></math>-LAT data and prospects for VLAST

In this study, we construct a traversable wormhole solution within the framework of <math altimg='si16.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity by assuming conformal symmetry. The matter content is modeled using phantom energy, characterized by an equation of state parameter <math altimg='si17.svg'><mrow><mi>&#969;</mi><mo linebreak='goodbreak'>&lt;</mo><mo>&#8722;</mo><mn>1</mn></mrow></math>, which inherently violates the null energy condition. By employing conformal Killing vector symmetry, we derive exact analytical expressions for the shape function, energy density, and pressure components of the anisotropic fluid. Our analysis includes a detailed examination of the flare-out condition, proper radial distance, embedding diagrams, and the generalized Tolman-Oppenheimer-Volkoff equation. Notably, the model yields a positive active gravitational mass and positive total gravitational energy, despite the presence of exotic matter.

Türkiye

Doğukan Taşer

Existence of conformal symmetric wormhole with phantom energy in <math altimg='si16.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> theory

In this study, we investigate the viability of the <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity framework in explaining the accelerated expansion of the universe within the context of the locally rotationally symmetric (LRS) Bianchi-I space-time. Modified gravity theories have emerged as promising alternatives to General Relativity (GR) to account for cosmic acceleration and dark energy phenomena. We employ observational constraints from Type Ia Supernovae (SN Ia), Baryon Acoustic Oscillations (BAO), and Cosmic Chronometers (CC) to calibrate the free parameters of our model. The field equations are formulated based on a specific functional form of <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math>, and analytical solutions are obtained. The Hubble parameter, deceleration parameter ( <math altimg='si10.svg'><mi>q</mi></math>), statefinder diagnostics <math altimg='si74.svg'><mrow><mo>(</mo><mi>r</mi><mo>,</mo><mi>s</mi><mo>)</mo></mrow></math>, and the jerk parameter ( <math altimg='si12.svg'><mi>j</mi></math>) are utilized to analyze the evolutionary dynamics of the universe. Our results indicate a transition from a decelerating to an accelerating phase, with the transition redshift <math altimg='si75.svg'><mrow><msub><mi>z</mi><mi>t</mi></msub><mo linebreak='goodbreak'>=</mo><mn>0</mn><mo>.</mo><msubsup><mn>7293</mn><mrow><mo>&#8722;</mo><mn>0.06</mn></mrow><mrow><mo>+</mo><mn>0.07</mn></mrow></msubsup></mrow></math> and present deceleration parameter <math altimg='si76.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo linebreak='goodbreak'>=</mo><mo>&#8722;</mo><mn>0.56</mn></mrow></math>, consistent with observational data. The estimated age of the universe in this framework is <math altimg='si77.svg'><mrow><mn>13.27</mn><mo>&#177;</mo><mn>0.26</mn></mrow></math> Gyrs. The statefinder parameters suggest that the model closely mimics the standard <math altimg='si5.svg'><mstyle mathvariant='normal'><mi>&#923;</mi></mstyle></math>CDM scenario at present but exhibits deviations at earlier epochs, potentially indicating a dynamic nature of dark energy. The <math altimg='si78.svg'><msub><mi>O</mi><mi>m</mi></msub></math> diagnostic further confirms the compatibility of our model with a phantom-like behavior of dark energy. These findings support the viability of <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity as an alternative framework for explaining cosmic acceleration, providing new interplay between matter and curvature in gravitational dynamics.

India

Vinod Kumar Bhardwaj

Anil Kumar Yadav

S.H. Shekh

Constraining <math altimg='si4.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi mathvariant='script'>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> gravity with SN Ia and BAO observational data in Bianchi I space time

We construct superinvariants in M-theory via local supersymmetry, which include ($\textit{DF}$) terms and fermionic bilinear terms with mass dimension eight. The bases of the ($\textit{DF}$) and the fermionic bilinear terms are classified and the variations under the local supersymmetry are evaluated by using the Mathematica codes. By imposing the local supersymmetry, we find that 24 independent terms of ($\textit{DF}$) are governed by 10 parameters. The result is consistent with the effective action obtained by analyzing scattering amplitudes of superparticles or supermembranes.

Japan

Yoshifumi Hyakutake

Effective action in M-theory: ($\textit{DF}$)

The late-time acceleration of the universe remains one of the central challenges in modern cosmology, motivating both dynamical dark energy models and extensions of general relativity. In this work, we investigate the cosmology of the recently proposed <math altimg='si5.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity framework, which generalizes the <math altimg='si34.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> and <math altimg='si35.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>)</mo></mrow></math> models by incorporating the Ricci scalar <math altimg='si36.svg'><mi>R</mi></math>, the matter Lagrangian <math altimg='si37.svg'><msub><mi>L</mi><mi>m</mi></msub></math>, and the trace of the energy-momentum tensor <math altimg='si38.svg'><mi>T</mi></math> within a unified gravitational action. By adopting the simplest functional form <math altimg='si39.svg'><mrow><mi>f</mi><mrow><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow><mo linebreak='goodbreak'>=</mo><mi>R</mi><mo linebreak='goodbreak'>+</mo><mi>&#945;</mi><msub><mi>L</mi><mi>m</mi></msub><mo linebreak='goodbreak'>+</mo><mi>&#946;</mi><mi>T</mi><mo linebreak='goodbreak'>+</mo><mi>&#947;</mi></mrow></math>, we derive modified Friedmann equations in a dust-dominated FLRW background and constrain the parameters <math altimg='si40.svg'><mrow><mo>(</mo><msub><mi>H</mi><mn>0</mn></msub><mo>,</mo><mi>&#945;</mi><mo>,</mo><mi>&#946;</mi><mo>,</mo><mi>&#947;</mi><mo>)</mo></mrow></math> using cosmic chronometers (CC), Type Ia supernovae from the PantheonPlus (PP)+SH0ES compilation, and their joint dataset. The inferred Hubble constant values are <math altimg='si41.svg'><mrow><msub><mi>H</mi><mn>0</mn></msub><mo linebreak='goodbreak'>=</mo><mn>68.69</mn><mo>&#177;</mo><mn>0.52</mn></mrow></math> km/s/Mpc (CC), <math altimg='si23.svg'><mrow><mn>72.75</mn><mo>&#177;</mo><mn>0.15</mn></mrow></math> km/s/Mpc (PP+SH0ES), and <math altimg='si26.svg'><mrow><mn>72</mn><mo>.</mo><msubsup><mn>68</mn><mrow><mo>&#8722;</mo><mn>0.12</mn></mrow><mrow><mo>+</mo><mn>0.15</mn></mrow></msubsup></mrow></math> km/s/Mpc (Joint), while the corresponding deceleration parameters are <math altimg='si42.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>&#8764;</mo><mo>&#8722;</mo><mn>0.561</mn></mrow></math>, <math altimg='si43.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>&#8764;</mo><mo>&#8722;</mo><mn>0.451</mn></mrow></math>, and <math altimg='si44.svg'><mrow><msub><mi>q</mi><mn>0</mn></msub><mo>&#8764;</mo><mo>&#8722;</mo><mn>0.458</mn></mrow></math>, respectively. Notably, the obtained <math altimg='si1.svg'><msub><mi>H</mi><mn>0</mn></msub></math> values lie between early-universe and local measurements, indicating that the model can accommodate both low- and high-redshift datasets, partially easing the Hubble tension. The <math altimg='si13.svg'><mrow><mi>O</mi><mi>m</mi><mo>(</mo><mi>z</mi><mo>)</mo></mrow></math> diagnostic analyses reveal a quintessence-like evolution of the cosmic energy density, distinguishing this framework from the standard <math altimg='si9.svg'><mstyle mathvariant='normal'><mi>&#923;</mi></mstyle></math>CDM model while preserving late-time acceleration.

Morocco

M. Koussour

Saudi Arabia

M.K.M. Ali

Uzbekistan

S. Muminov

J. Rayimbaev

Observational constraints on cosmic expansion in <math altimg='si5.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity

In this paper, we present intriguing traversable and asymptotically flat wormhole solutions within <math altimg='si18.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity. We integrate our model with the gravitational analog of the Schwinger effect, describing the emergence of particle-antiparticle pairs from the vacuum. By introducing a fundamental minimal length via the generalized uncertainty principle, we establish critical constraints on matter distribution and spacetime structure. Our findings reveal how this fundamental length shapes the wormhole geometry, steepening the slope toward the throat and mitigating violations of the weak and null energy conditions. This adjustment allows the supporting matter to avoid phantom behavior at the Planck scale, suggesting a more stable configuration. We also explore the intriguing effects of gravitational lensing, showing that these exotic wormholes repel light rather than capture it. For <math altimg='si9.svg'><mi>&#946;</mi></math> values ranging from 0 to 45, the deflection angle remains negative for all corresponding <math altimg='si14.svg'><mrow><mi>&#945;</mi><mo>(</mo><msub><mi>r</mi><mrow><mi>t</mi><mi>p</mi></mrow></msub><mo>)</mo></mrow></math> values, indicating a repulsive gravitational force that pushes photons away from the throat. Moreover, the forces acting on the wormhole exhibit a delicate balance, demonstrating equal strength in opposing directions&#8211;an essential feature of stability. The complexity factor <math altimg='si17.svg'><msub><mi>Y</mi><mrow><mi>T</mi><mi>F</mi></mrow></msub></math> decreases with distance from the throat, indicating that corrections from the generalized uncertainty principle are most significant near the throat and diminish outward. Overall, our work highlights the allure of these wormhole geometries and the pivotal role of quantum effects in their formation, paving new avenues for understanding gravity and spacetime.

South Africa

Azerbaijan

A. Errehymy

B. Turimov

Kazakhstan

A. Syzdykova

K. Myrzakulov

N. Alessa

A.H. Abdel-Aty

Dymnikova-Schwinger GUP-corrected wormholes in <math altimg='si18.svg'><mrow><mi>f</mi><mo>(</mo><mi>R</mi><mo>,</mo><msub><mi>L</mi><mi>m</mi></msub><mo>,</mo><mi>T</mi><mo>)</mo></mrow></math> gravity

<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mtext>DMRadio-</mtext><msup><mrow><mi mathvariant="normal">m</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math> is an experimental search for dark matter axions. It uses a solenoidal dc magnetic field to convert an axion dark-matter signal to an ac electromagnetic response in a coaxial copper pickup. The current induced by this axion signal is measured by dc SQUIDs. <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mtext>DMRadio-</mtext><msup><mrow><mi mathvariant="normal">m</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math> is designed to be sensitive to Kim-Shifman-Vainshtein-Zakharov (KSVZ) and Dine-Fischler-Srednicki-Zhitnisky (DFSZ) QCD axion models in the 10–200 MHz (<math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>41</mn><mtext> </mtext><mtext> </mtext><mi>neV</mi><mo>/</mo><msup><mi>c</mi><mn>2</mn></msup><mi>–</mi><mrow><mn>0.83</mn><mtext> </mtext><mtext> </mtext><mi mathvariant="normal">μ</mi><mi>eV</mi><mo>/</mo><msup><mi>c</mi><mn>2</mn></msup></mrow></mrow></math>) range, and to axions with <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi><mi>γ</mi></mrow></msub><mo>=</mo><msub><mi>g</mi><mrow><mi>a</mi><mi>γ</mi><mi>γ</mi><mo>,</mo><mrow><mi>DFSZ</mi></mrow></mrow></msub><mo stretchy="false">(</mo><mn>30</mn><mtext> </mtext><mtext> </mtext><mi>MHz</mi><mo stretchy="false">)</mo><mo>=</mo><mn>1.87</mn><mo>×</mo><msup><mn>10</mn><mrow><mo>−</mo><mn>17</mn></mrow></msup><mtext> </mtext><mtext> </mtext><msup><mrow><mi>GeV</mi></mrow><mrow><mo>−</mo><mn>1</mn></mrow></msup></math> over 5–30 MHz as an extended goal. In this work, we present the electromagnetic modeling of the response of the experiment to an axion signal over the full frequency range of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mtext>DMRadio-</mtext><msup><mrow><mi mathvariant="normal">m</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math>, which extends from the low-frequency, lumped-element limit to a regime where the axion Compton wavelength is only a factor of 2 larger than the detector size. With these results, we determine the live time and sensitivity of the experiment. The primary science goal of sensitivity to DFSZ axions across 30–200 MHz can be achieved with a <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>3</mn><mi>σ</mi></math> live scan time of 2.9 years.

United States

A. AlShirawi

V. Ankel

C. Bartram

J. Begin

C. Bell

J.N. Benabou

L. Brouwer

S. Chaudhuri

H.M. Cho

J. Corbin

W. Craddock

S. Cuadra

A. Droster

J. Echevers

J.W. Foster

J.T. Fry

P.W. Graham

R. Henning

K.D. Irwin

F. Kadribasic

Y. Kahn

A. Keller

R. Kolevatov

S. Kuenstner

A. Kunder

N. Kurita

A.F. Leder

D. Li

N. Otto

J.L. Ouellet

K.M.W. Pappas

A. Phipps

N.M. Rapidis

B.R. Safdi

C.P. Salemi

M. Simanovskaia

J. Singh

P. Stark

E.C. van Assendelft

K. van Bibber

K. Wells

J. Wiedemann

L. Winslow

W.J. Wisniewski

D. Wright

A.K. Yi

B.A. Young

Electromagnetic modeling and science reach of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mtext>DMRadio-</mtext><msup><mrow><mi mathvariant="normal">m</mi></mrow><mrow><mn>3</mn></mrow></msup></mrow></math>

Combining toric geometry techniques and $$\mathcal {N}=2$$ supergravity formalisms, we study 5D black branes in the M-theory compactification on a four parameter Calabi–Yau threefold. First, we investigate 5D BPS and non-BPS black holes that are derived by wrapping M2-branes on non-holomorphic 2-cycles in such a toric Calabi–Yau manifold. Concretely, we provide the allowed electric charge regions of BPS and non-BPS black hole states that are obtained by surrounding M2-branes over appropriate 2-cycles. Then, we approach the black hole thermodynamic behavior by computing the entropy and the temperature. By evaluating the recombination factor, we examine the stability of such non-BPS black holes. Precisely, we find stable and unstable solutions depending on the allowed electric charge regions. After that, we study 5D black strings by wrapping M5-branes on non-holomorphic dual 4-cycles in the proposed toric Calabi–Yau manifold by focusing on the stability behaviors. In the allowed regions of the moduli space of the non-BPS stringy solutions, we find stable and unstable states depending on the magnetic charge values.

A. Belhaj

H. Belmahi

A. Bouhouch

S. Ennadifi

M. Sedra

Black holes and black strings in M-theory on Calabi–Yau threefolds with four Kähler parameters

We report on a search for sub-GeV dark matter (DM) particles interacting with electrons using the DAMIC-M prototype detector at the Modane Underground Laboratory. The data feature a significantly lower detector single <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup></mrow></math> rate (factor 50) compared to our previous search, while also accumulating a 10 times larger exposure of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mo>∼</mo><mn>1.3</mn><mtext> </mtext><mtext> </mtext><mi>kg</mi><mtext>−</mtext><mi>day</mi></mrow></math>. DM interactions in the skipper charge-coupled devices (CCDs) are searched for as groups of two or three adjacent pixels with a total charge between 2 and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mn>4</mn><mtext> </mtext><mtext> </mtext><msup><mi>e</mi><mo>−</mo></msup></math>. We find 144 candidates of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>2</mn><mtext> </mtext><mtext> </mtext><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup></mrow></math> and 1 candidate of <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>4</mn><mtext> </mtext><mtext> </mtext><msup><mrow><mi>e</mi></mrow><mrow><mo>−</mo></mrow></msup></mrow></math>, where 141.5 and 0.071, respectively, are expected from background. With no evidence of a DM signal, we place stringent constraints on DM particles with masses between 1 and <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>1000</mn><mtext> </mtext><mtext> </mtext><mi>MeV</mi><mo>/</mo><msup><mrow><mi>c</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math> interacting with electrons through an ultralight or heavy mediator. For large ranges of DM masses below <math xmlns="http://www.w3.org/1998/Math/MathML" display="inline"><mrow><mn>1</mn><mtext> </mtext><mi>GeV</mi><mo>/</mo><msup><mrow><mi>c</mi></mrow><mrow><mn>2</mn></mrow></msup></mrow></math>, we exclude theoretically motivated benchmark scenarios where hidden-sector particles are produced as a major component of DM in the Universe through the freeze-in or freeze-out mechanisms.