Mon·Feb 20, 2023Monday·February 20, 2023

1. 01*

   Can SUSY relax LNV constraints coming from loop corrections to light neutrino masses on the low-scale Seesaw?

   J. Jones-Pérez🇵🇪 · O. Suarez-Navarro🇵🇪

   Heavy neutrinos from the Type-I Seesaw model can have a large mixing with active states, motivating their search at collider experiments. However, loop corrections to light neutrino masses constrain the heavy neutrinos to appear in pseudo-Dirac pairs, leading to a potential suppression of lepton number violating parameters. In this work we perform a detailed review of a proposal to relax constraints on lepton number violation by adding supersymmetry. We define the conditions necessary to maximise the SUSY screening effect, with the objective of allowing a larger mass splitting between low-scale heavy neutrino masses. We find that the sole addition of SUSY does not guarantee a screening, and that favourable cases have some degree of fine-tuning.

   hep-phPRD(2023)·1 citation
2. 02*

   Evading the Landau pole in the minimal 3-3-1 model with leptoquarks

   A. Doff🇧🇷 · C. A. de S. Pires🇧🇷

   In its original version, the minimal 3-3-1 model possess a Landau-pole around 2-6 TeV scale. Current LHC bound on $Z^{\prime }$ implies that the $SU(3{)}_L\times U(1{)}_X$ symmetry must break spontaneously around 4 TeV which means that the model may lose its perturbative character even before symmetry breaking. This is a disaster for the model. Few attention has been devoted to this problem. Here we investigate the efficiency of scalar leptoquarks in evading or shifting the Landau pole to a harmless energy scale.

   hep-phNPB(2023)·8 citations
3. 03*

   Jet SIFT-ing: a new scale-invariant jet clustering algorithm for the substructure era

   Andrew J. Larkoski🇺🇸 · Denis Rathjens🇺🇸 · Jason Veatch🇺🇸 · Joel W. Walker🇺🇸

   We introduce a new jet clustering algorithm named SIFT (Scale-Invariant Filtered Tree) that maintains the resolution of substructure for collimated decay products at large boosts. The scale-invariant measure combines properties of kT and anti-kT by preferring early association of soft radiation with a resilient hard axis, while avoiding the specification of a fixed cone size. Integrated filtering and variable-radius isolation criteria block assimilation of soft wide-angle radiation and provide a halting condition. Mutually hard structures are preserved to the end of clustering, automatically generating a tree of subjet axis candidates. Excellent object identification and kinematic reconstruction for multi-pronged resonances are realized across more than an order of magnitude in transverse energy. The clustering measure history facilitates high-performance substructure tagging, which we quantify with the aid of supervised machine learning. These properties suggest that SIFT may prove to be a useful tool for the continuing study of jet substructure.

   hep-phPRD(2023)·5 citations
4. 04*

   Neutral and Doubly-Charged Scalars at Future Lepton Colliders

   Fang Xu🇺🇸

   Many new physics scenarios beyond the Standard Model (BSM) necessitate the existence of new neutral and/or charged scalar fields, which might couple to the SM charged leptons (but not hadrons), and thus, can give rise to BSM signals while evading strong constraints mostly coming from the hadronic sector. I show that future lepton colliders provide a clean environment to probe these leptophilic new scalars via multi-lepton final states, including some interesting lepton flavor violating (LFV) channels. I also study the kinematic distributions of the final state leptons to distinguish the BSM contributions from neutral and doubly-charged scalars giving rise to the same final state, as well as from the irreducible SM background.

   hep-phhep-exPRD(2023)·8 citations
5. 05*

   Effect of Ultralight Dark Matter on $g-2$ of the Electron

   Jason L. Evans🇨🇳

   If dark matter is ultralight, the number density of dark matter is very high and the techniques of zero-temperature field theory are no longer valid. The dark matter number density modifies the vacuum giving it a non-negligible particle occupation number. For fermionic dark matter, this occupation number can be no larger than one. However, in the case of bosons the occupation number is unbounded. If there is a large occupation number, the Bose enhancement needs to be taken into consideration for any process involving particles which interact with the dark matter. Because the occupation number scales inversely with the dark matter mass, this effect is most prominent for ultralight dark matter. In fact, the Bose enhancement effect from the background is so significant for ultralight dark matter that, if dark matter is a dark photon, the correction to the anomalous magnetic moment is larger than experimental uncertainties for a mixing parameter of order $10^{-16}$ and a dark photon mass of order $10^{-20}$ eV. Furthermore, the constraint on the mixing parameter scales linearly with the dark photon mass and so new significant constraints can be placed on the dark matter mass all the way up to $10^{-14}$ eV. Future experiments measuring $g-2$ will probe even smaller gauge mixing parameters.

   hep-phPRL(2024)·11 citations
6. 06*

   Probing Baryogenesis with Radiative Beauty Decay and Electron EDM

   Wei-Shu Hou🇹🇼 · Girish Kumar🇹🇼 · Tanmoy Modak🇩🇪

   With the Large Hadron Collider (LHC) running, we should probe electroweak baryogenesis (EWBG) while probing $CP$ violation (CPV) with electron electric dipole moment (eEDM). Rooted in the flavor structure of the Standard Model (SM), the general two Higgs doublet model (g2HDM) with a second set of Yukawa couplings can deliver EWBG while surviving eEDM. We point out a chiral-enhanced top-bottom interference effect that makes $b\to s\gamma$ decay an exquisite window on EWBG and eEDM, and illustrate the importance of the $\Delta A_{CP}$ observable at Belle II.

   hep-phhep-exPRD(2024)·4 citations
7. 07*

   Two body final states production in electron-positron annihilation and their contributions to $(g-2{)}_{\mu }$

   Shi-Jia Wang🇨🇳 · Zhen Fang🇨🇳 · Ling-Yun Dai🇨🇳

   In this paper, we study the processes of $e^{+}{e}^{-}$ annihilation into two body final states, either two pseudoscalar mesons or one meson with a photon. The hadronic vacuum polarization form factors are calculated within the framework of resonance chiral theory in the energy region of $E\lesssim 2$ GeV, with final state interactions taken into account. A joint analysis on the processes of $e^{+}{e}^{-}\to {\pi }^{+}{\pi }^{-}$, $K^{+}{K}^{-}$, $K_L^0{K}_S^0$, ${\pi }^0\gamma$, and $\eta \gamma$ has been performed, and the latest experimental data are included. Based on the vacuum polarization form factors of these processes, we estimate their contributions to the lowest order of anomalous magnetic moment of the muon, $(g-2{)}_{\mu }$. Combined with other contributions from hadronic vacuum polarization and other interactions from the standard model, the discrepancy between theoretical prediction and experimental measurement is $\Delta a_{\mu }=(24.1\pm 5.4)\times 10^{-10}$, i.e., 4.5$\sigma$.

   hep-phnucl-thJHEP(2023)·20 citations
8. 08*

   Shedding light on the $X(3930)$ and $X(3960)$ states with the $B^{-}\to K^{-}J/\psi \omega$ reaction

   L. M. Abreu🇧🇷 · M. Albaladejo🇪🇸 · A. Feijoo🇪🇸 · E. Oset🇪🇸 · J. Nieves🇪🇸

   We have studied the contribution of the state $X(3930)$, coming from the interaction of the $D\overline{D}$ and $D_s^{+}{D}_s^{-}$ channels, to the $B^{-}\to K^{-}J/\psi \omega$ decay. The purpose of this work is to offer a complementary tool to see if the $X(3930)$ state observed in the $D^{+}{D}^{-}$ channel is the same or not as the $X(3960)$ resonance claimed by the LHCb collaboration from a peak in the $D_s^{+}{D}_s^{-}$ mass distribution around threshold. We present results for what we expect in the $J/\psi \omega$ mass distribution in the $B^{-}\to K^{-}J/\psi \omega$ decay and conclude that a clear signal should be seen around $3930\mathrm{MeV}$. At the same time, finding no extra resonance signal at $3960\mathrm{MeV}$ would be a clear indication that there is not a new state at $3960\mathrm{MeV}$, supporting the hypothesis that the near-threshold peaking structure peak in the $D_s^{+}{D}_s^{-}$ mass distribution is only a manifestation of a resonance below threshold.

   hep-phEPJC(2023)·10 citations
9. 09*

   Coup de grace to the charged Higgs solution of $P_5^{\prime }$ and $R_{D^{(\ast )}}$ discrepancies

   Syuhei Iguro🇩🇪

   We consider a general two Higgs doublet model which can simultaneously solve discrepancies in neutral B meson decay ($b\to s\ell \overline{\ell }$ distribution) and charged B meson decay ($b\to c\tau \overline{\nu }$) with a charged Higgs. The model contains two additional neutral scalars at the same mass scale and predicts distinctive signals at the LHC. Based on the recent same-sign top search by the ATLAS collaboration, we found the constraint on the scalar mass spectrum. To probe the remaining mass window, we propose a novel $cg\to t\tau \overline{\tau }$ process at the LHC.

   hep-phhep-exPRD(2023)·24 citations
10. 10*

    Tropical Feynman integration in the Minkowski regime

    Michael Borinsky🇨🇭 · Henrik J. Munch🇮🇹 · Felix Tellander🇩🇪

    We present a new computer program, $\text{feyntrop}$, which uses the tropical geometric approach to evaluate Feynman integrals numerically. In order to apply this approach in the physical regime, we introduce a new parametric representation of Feynman integrals that implements the causal $i\epsilon$ prescription concretely while retaining projective invariance. $\text{feyntrop}$ can efficiently evaluate dimensionally regulated, quasi-finite Feynman integrals, with not too exceptional kinematics in the physical regime, with a relatively large number of propagators and with arbitrarily many kinematic scales. We give a systematic classification of all relevant kinematic regimes, review the necessary mathematical details of the tropical Monte Carlo approach, give fast algorithms to evaluate (deformed) Feynman integrands, describe the usage of $\text{feyntrop}$ and discuss many explicit examples of evaluated Feynman integrals.

    hep-phhep-thmath-phmath.MPComput.Phys.Commun.(2023)·73 citations
11. 11*

    Lorentz Violation in Neutrino Oscillations using IceCube Atmospheric Neutrino Interferometry

    Barbara Skrzypek🇺🇸 · Carlos A. Argüelles🇺🇸

    Lorentz invariance is a fundamental symmetry of spacetime underpinning the Standard Model (SM) and our understanding of high-energy phenomena in particle physics. However, beyond the quantum gravity scale, we expect the SM to be replaced with a more fundamental, covariant theory giving a quantum description of gravity. The effective theory arising from this theory can break Lorentz invariance and thus predicts observables that exhibit low-energy manifestations of Lorentz violation. In particular, these observables could be a subleading contribution to neutrino oscillations and could therefore explain anomalous flavor measurements. The Standard Model Extension (SME) formalism describing such an effective theory predicts terms whose characteristic oscillation length becomes significant at atmospheric neutrino energies accessible by the IceCube Neutrino Observatory. We descibe past measurements and efforts to extend these using ten years of data along with a new energy reconstruction to study ${\nu }_{\mu }$ disappearance.

    hep-phhep-ex2 citations
12. 12*

    Two-loop amplitudes in massless QCD for diphoton-plus-jet production via gluon fusion at hadron colliders

    Ryan Moodie🇮🇹

    The ability to calculate analytic full-colour two-to-three two-loop helicity amplitudes in massless QCD has been a recent triumph of the field, driving phenomenology towards one percent precision. In this contribution, we focus on the virtual correction of diphoton-plus-jet production via gluon fusion, $gg\to g\gamma \gamma$. We outline state-of-the-art strategies to optimise the reconstruction over finite fields of the rational coefficients of the amplitude. We also present an updated performance analysis of our publicly-available C++ implementation of the amplitude, demonstrating its typical speed and stability, and study its stability in infrared regions of phase space. These results are relevant for improving predictions in Higgs physics at hadron colliders.

    hep-phJ.Phys.Conf.Ser.(2026)·0 citations
13. 13*

    Gravitational form factors of a kink in $1+1$ dimensional ${\varphi }^4$ model

    Hiroaki Ito🇯🇵 · Masakiyo Kitazawa🇯🇵

    We calculate the one-loop correction to the distribution of energy-momentum tensor around a kink in $1+1$ dimensional ${\varphi }^4$ model. We employ the collective coordinate method to eliminate the zero mode that gives rise to infrared divergence. The ultraviolet divergences are removed by vacuum subtraction and mass renormalization. We obtain an analytic result that is finite and satisfies the momentum conservation. The total energy of the kink obtained from the spatial integral of energy density reproduces the known result. Our result obtained on a finite space has a spatially-uniform term that is inversely proportional to the spatial length.

    ↳ hep-thcond-mat.otherhep-phnlin.PSJHEP(2023)·10 citations
14. 14*

    Search for Ultraheavy Dark Matter from Observations of Dwarf Spheroidal Galaxies with VERITAS

    A. Acharyya🇺🇸 · A. Archer🇺🇸 · P. Bangale🇺🇸 · J. T. Bartkoske🇺🇸 · P. Batista🇩🇪 · M. Baumgart🇺🇸 · W. Benbow🇺🇸 · J. H. Buckley🇺🇸 · A. Falcone🇺🇸 · Q. Feng🇺🇸 · J. P. Finley🇺🇸 · G. M. Foote🇺🇸 and 42 other authors

    Dark matter is a key piece of the current cosmological scenario, with weakly interacting massive particles (WIMPs) a leading dark matter candidate. WIMPs have not been detected in their conventional parameter space (100 GeV $\lesssim M_{\chi }\lesssim$ 100 TeV), a mass range accessible with current Imaging Atmospheric Cherenkov Telescopes. As ultraheavy dark matter (UHDM; $M_{\chi }\gtrsim$ 100 TeV) has been suggested as an under-explored alternative to the WIMP paradigm, we search for an indirect dark matter annihilation signal in a higher mass range (up to 30 PeV) with the VERITAS gamma-ray observatory. With 216 hours of observations of four dwarf spheroidal galaxies, we perform an unbinned likelihood analysis. We find no evidence of a $\gamma$-ray signal from UHDM annihilation above the background fluctuation for any individual dwarf galaxy nor for a joint-fit analysis, and consequently constrain the velocity-weighted annihilation cross section of UHDM for dark matter particle masses between 1 TeV and 30 PeV. We additionally set constraints on the allowed radius of a composite UHDM particle.

    ↳ astro-ph.HEastro-ph.COhep-exhep-phApJ(2023)·28 citations
15. 15*

    Model-independent measurement of cosmic curvature with the latest $H(z)$ and SNe Ia data: A comprehensive investigation

    Jing-Zhao Qi🇨🇳 · Ping Meng · Jing-Fei Zhang🇺🇸 · Xin Zhang🇺🇸

    In the context of the discrepancies between the early and late universe, we emphasize the importance of independent measurements of the cosmic curvature in the late universe. We present an investigation of the model-independent measurement of the cosmic curvature parameter ${\Omega }_k$ in the late universe with the latest Hubble parameter $H(z)$ measurements and type Ia supernovae (SNe Ia) data. For that, we use two reconstruction methods, the Gaussian process (GP) and artificial neural network (ANN) methods, to achieve the distance construction from $H(z)$ data. Our analysis reveals that the GP method provides the most precise constraint on ${\Omega }_k$, with a constraint precision of $\xi ({\Omega }_k)=0.13$, surpassing recent estimations using similar methods. The GP method consistently indicates a preference for a flat universe at the 2$\sigma$ confidence level. Moreover, we find that the choice of reconstruction method influences the estimation of ${\Omega }_k$. The ANN reconstruction method exhibits higher sensitivity to the addition of BAO $H(z)$ data, resulting in comparable constraint precision to the GP method. A discrepancy exists between the best-fit values obtained by these two reconstruction methods, indicating their dependence on the reconstruction approach. However, we anticipate that with the improvement of sample size and precision of observational $H(z)$ data, the estimation of ${\Omega }_k$ using this approach will become more robust and reliable.

    ↳ astro-ph.COgr-qchep-phPRD(2023)·57 citations
16. 16*

    Primordial Black Holes Dark Matter and Secondary Gravitational Waves from Warm Higgs-G Inflation

    Richa Arya🇮🇳 · Rajeev Kumar Jain🇮🇳 · Arvind Kumar Mishra🇮🇳

    We explore the role of dissipative effects during warm inflation leading to the small-scale enhancement of the power spectrum of curvature perturbations. In this paper, we specifically focus on non-canonical warm inflationary scenarios and study a model of warm Higgs-G inflation, in which the Standard Model Higgs boson drives inflation, with a Galileon-like non-linear kinetic term. We show that in the Galileon-dominated regime, the primordial power spectrum is strongly enhanced, leading to the formation of primordial black holes (PBH) with a wide range of the mass spectrum. Interestingly, PBHs in the asteroid mass window $\sim (10^{17}$ -- $10^{23}$) g are generated in this model, which can explain the total abundance of the dark matter in the Universe. In our analysis, we also calculate the secondary gravitational waves (GW) sourced by these small-scale overdense fluctuations and find that the induced GW spectrum can be detected in the future GW detectors, such as LISA, BBO, DECIGO, etc. Our scenario thus provides a novel way of generating PBHs as dark matter and a detectable stochastic GW background from warm inflation. We also show that our scenario is consistent with the swampland and the trans-Planckian censorship conjectures and, thus, remains in the viable landscape of UV complete theories.

    ↳ astro-ph.COgr-qchep-phJCAP(2024)·19 citations
17. 17*

    The Ups and Downs of Early Dark Energy solutions to the Hubble tension: a review of models, hints and constraints circa 2023

    Vivian Poulin🇫🇷 · Tristan L. Smith🇺🇸 · Tanvi Karwal🇺🇸

    We review the current status of Early Dark Energy (EDE) models proposed to resolve the "Hubble tension", the discrepancy between "direct" measurements of the current expansion rate of the Universe and "indirect measurements" for which the values inferred rely on the $\Lambda$CDM cosmological model calibrated on early-universe data. EDE refers to a new form of dark energy active at early times (typically a scalar-field), that quickly dilutes away at a redshift close to matter-radiation equality. The role of EDE is to decrease the sound horizon by briefly contributing to the Hubble rate in the pre-recombination era. We summarize the results of several analyses of EDE models suggested thus far in light of recent cosmological data, including constraints from the canonical {\it Planck} data, baryonic acoustic oscillations and Type Ia supernovae, and the more recent hints driven by cosmic microwave background observations using the Atacama Cosmology Telescope. We also discuss potential challenges to EDE models, from theoretical ones (a second "cosmic coincidence" problem in particular) to observational ones, related to the amplitude of clustering on scales of $8h$/Mpc as measured by weak-lensing observables (the so-called $S_8$ tension) and the galaxy power spectrum from BOSS analyzed through the effective field theory of large-scale structure. We end by reviewing recent attempts at addressing these shortcomings of the EDE proposal. While current data remain inconclusive on the existence of an EDE phase, we stress that given the signatures of EDE models imprinted in the CMB and matter power spectra, next-generation experiments can firmly establish whether EDE is the mechanism responsible for the Hubble tension and distinguish between the various models suggested in the literature.

    ↳ astro-ph.COhep-phhep-thPhys.Dark Univ.(2023)·326 citations
18. 18*

    Possible Relation between the Cosmological Constant and Standard Model Parameters

    Mark P. Hertzberg🇺🇸 · Abraham Loeb🇺🇸

    We propose possible properties of quantum gravity in de Sitter space, and find that they relate the value of the cosmological constant to parameters of the Standard Model. In de Sitter space we suggest (i) that the most sharply defined observables are obtained by scattering objects from the horizon and back to the horizon and (ii) that black holes of discrete charge are well defined states in the theory. For a black hole of minimal discrete electric charge, we therefore demand that a scattering process involving the black hole and a probe can take place within a Hubble time before evaporating away, so that the state of a discretely charged black hole is well defined. By imposing that the black hole's charge is in principle detectable, which involves appreciably altering the state of a scattered electron, we derive a relation between the Hubble scale, or cosmological constant, and the electron's mass and charge and order one coefficients that describe our ignorance of the full microscopic theory. This gives the prediction $\Lambda \sim 10^{-123\pm 2}{M}_{Pl}^4$, which includes the observed value of dark energy. We suggest possible ways to test this proposal.

    ↳ hep-thastro-ph.COgr-qchep-phPRD(2023)·5 citations
19. 19*

    Neutrino-Assisted Early Dark Energy is a Natural Resolution of the Hubble Tension

    Mariana Carrillo González🇬🇧 · Qiuyue Liang🇺🇸 · Jeremy Sakstein🇺🇸 · Mark Trodden🇺🇸

    It has very recently been claimed that the neutrino-assisted early dark energy model -- a promising resolution of the Hubble tension that can ameliorate the theoretical fine-tuning and coincidence problems that plague other theories -- does not provide natural or cosmologically interesting results. In this short paper, we show that these conclusions are incorrect for three reasons. First, we identify errors in the calculations. Second, we dispute the definition in of what constitutes an 'interesting' and 'natural' model. Finally, we demonstrate that the conclusions of were arrived at without fully exploring the full parameter space of the model. Neutrino-assisted early dark energy remains a natural and interesting potential resolution of the Hubble tension that merits further study.

    ↳ astro-ph.COhep-ph22 citations
20. 20*

    Primordial Gravitational Waves From Black Hole Evaporation in Standard and Non-Standard Cosmologies

    Aurora Ireland🇺🇸 · Stefano Profumo🇺🇸 · Jordan Scharnhorst🇺🇸

    Gravitons radiated from light, evaporating black holes contribute to the stochastic background of gravitational waves. The spectrum of such emission depends on both the mass and the spin of the black holes, as well as on the redshifting that occurs between the black hole formation and today. This, in turn, depends on the expansion history of the universe, which is largely unknown and unconstrained at times prior to the synthesis of light elements. Here, we explore the features of the stochastic background of gravitational waves from black hole evaporation under a broad range of possible early cosmological histories. The resulting gravitational wave signals typically peak at very high frequencies, and offer opportunities for proposed ultra-high frequency gravitational wave detectors. Lower-frequency peaks are also possible, albeit with a suppressed intensity that is likely well below the threshold of detectability. We find that the largest intensity peaks correspond to cosmologies dominated by fluids with equations of state that have large pressure-to-density ratios. Such scenarios can be constrained on the basis of violation of $\Delta N_{\mathrm{eff}}$ bounds.

    ↳ gr-qcastro-ph.COastro-ph.HEhep-phPRD(2023)·66 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.