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class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.16596">arXiv:2501.16596</a> <span> [<a href="https://arxiv.org/pdf/2501.16596">pdf</a>, <a href="https://arxiv.org/format/2501.16596">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> </div> <p class="title is-5 mathjax"> Polarized Dissociation and Spin Alignment of Moving Quarkonium in Quark-Gluon Plasma </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhishun Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Lin%2C+S">Shu Lin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.16596v1-abstract-short" style="display: inline;"> Recent experiments have found spin alignment of $J/蠄$ with respect to event plane in heavy ion collisions, suggesting a medium effect that is spin dependent. We propose a possible mechanism with polarized dissociation from the motion of $J/蠄$ with respect to the medium. We calculate polarized dissociation rate for quarkonium spin triplet state from spin chromomagnetic coupling in the potential non… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16596v1-abstract-full').style.display = 'inline'; document.getElementById('2501.16596v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.16596v1-abstract-full" style="display: none;"> Recent experiments have found spin alignment of $J/蠄$ with respect to event plane in heavy ion collisions, suggesting a medium effect that is spin dependent. We propose a possible mechanism with polarized dissociation from the motion of $J/蠄$ with respect to the medium. We calculate polarized dissociation rate for quarkonium spin triplet state from spin chromomagnetic coupling in the potential non-relativistic QCD framework. This is done for the leading order gluo-dissociation process and next to leading order inelastic Coulomb scattering process. The polarized dissociation rate is expressed as a function of relative velocity between quarkonium and QGP and the quantization axis. Applying the polarized dissociation rate to quarkonium evolution with dissociation effect only in a Bjorken flow, we find the spin $0$ state to dissociate less than the other spin states, leading to positive $蟻_{00}-1/3$. Regeneration contribution is expected to give a contribution with the opposite sign. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16596v1-abstract-full').style.display = 'none'; document.getElementById('2501.16596v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.14092">arXiv:2412.14092</a> <span> [<a href="https://arxiv.org/pdf/2412.14092">pdf</a>, <a href="https://arxiv.org/format/2412.14092">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Machine Learning-Assisted Measurement of Lepton-Jet Azimuthal Angular Asymmetries in Deep-Inelastic Scattering at HERA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=The+H1+collaboration"> The H1 collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Andreev%2C+V">V. Andreev</a>, <a href="/search/hep-ph?searchtype=author&query=Arratia%2C+M">M. Arratia</a>, <a href="/search/hep-ph?searchtype=author&query=Baghdasaryan%2C+A">A. Baghdasaryan</a>, <a href="/search/hep-ph?searchtype=author&query=Baty%2C+A">A. Baty</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Bolz%2C+A">A. Bolz</a>, <a href="/search/hep-ph?searchtype=author&query=Boudry%2C+V">V. Boudry</a>, <a href="/search/hep-ph?searchtype=author&query=Brandt%2C+G">G. Brandt</a>, <a href="/search/hep-ph?searchtype=author&query=Britzger%2C+D">D. Britzger</a>, <a href="/search/hep-ph?searchtype=author&query=Buniatyan%2C+A">A. Buniatyan</a>, <a href="/search/hep-ph?searchtype=author&query=Bystritskaya%2C+L">L. Bystritskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Campbell%2C+A+J">A. J. Campbell</a>, <a href="/search/hep-ph?searchtype=author&query=Avila%2C+K+B+C">K. B. Cantun Avila</a>, <a href="/search/hep-ph?searchtype=author&query=Cerny%2C+K">K. Cerny</a>, <a href="/search/hep-ph?searchtype=author&query=Chekelian%2C+V">V. Chekelian</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Z. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Contreras%2C+J+G">J. G. Contreras</a>, <a href="/search/hep-ph?searchtype=author&query=Cvach%2C+J">J. Cvach</a>, <a href="/search/hep-ph?searchtype=author&query=Dainton%2C+J+B">J. B. Dainton</a>, <a href="/search/hep-ph?searchtype=author&query=Daum%2C+K">K. Daum</a>, <a href="/search/hep-ph?searchtype=author&query=Deshpande%2C+A">A. Deshpande</a>, <a href="/search/hep-ph?searchtype=author&query=Diaconu%2C+C">C. Diaconu</a>, <a href="/search/hep-ph?searchtype=author&query=Drees%2C+A">A. Drees</a>, <a href="/search/hep-ph?searchtype=author&query=Eckerlin%2C+G">G. Eckerlin</a> , et al. (119 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.14092v2-abstract-short" style="display: inline;"> In deep-inelastic positron-proton scattering, the lepton-jet azimuthal angular asymmetry is measured using data collected with the H1 detector at HERA. When the average transverse momentum of the lepton-jet system, $\lvert \vec{P}_\perp \rvert $, is much larger than the total transverse momentum of the system, $\lvert \vec{q}_\perp \rvert$, the asymmetry between parallel and antiparallel configura… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.14092v2-abstract-full').style.display = 'inline'; document.getElementById('2412.14092v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.14092v2-abstract-full" style="display: none;"> In deep-inelastic positron-proton scattering, the lepton-jet azimuthal angular asymmetry is measured using data collected with the H1 detector at HERA. When the average transverse momentum of the lepton-jet system, $\lvert \vec{P}_\perp \rvert $, is much larger than the total transverse momentum of the system, $\lvert \vec{q}_\perp \rvert$, the asymmetry between parallel and antiparallel configurations, $\vec{P}_\perp$ and $\vec{q}_\perp$, is expected to be generated by initial and final state soft gluon radiation and can be predicted using perturbation theory. Quantifying the angular properties of the asymmetry therefore provides an additional test of the strong force. Studying the asymmetry is important for future measurements of intrinsic asymmetries generated by the proton's constituents through Transverse Momentum Dependent (TMD) Parton Distribution Functions (PDFs), where this asymmetry constitutes a dominant background. Moments of the azimuthal asymmetries are measured using a machine learning method for unfolding that does not require binning. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.14092v2-abstract-full').style.display = 'none'; document.getElementById('2412.14092v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 4 figures, 2 tables, updated affiliations and acknowledgements</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DESY24-200 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.03163">arXiv:2412.03163</a> <span> [<a href="https://arxiv.org/pdf/2412.03163">pdf</a>, <a href="https://arxiv.org/format/2412.03163">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Constraints on dark matter annihilation in the Large Magellanic Cloud from multiple low-frequency radio observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhanfang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Huang%2C+F">Feng Huang</a>, <a href="/search/hep-ph?searchtype=author&query=Fang%2C+T">Taotao Fang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.03163v1-abstract-short" style="display: inline;"> Low-frequency radio emission from the Large Magellanic Cloud~(LMC) is assumed to be dominated by nonthermal synchrotron radiation from energy loss of energetic $e^+/e^-$ in magnetic field. Two different kinds of sources of $e^+/e^-$, dark matter~(DM) annihilation and cosmic rays~(CR) related to massive stars, are taken into account in this paper. We fit the multiple low-frequency radio observation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03163v1-abstract-full').style.display = 'inline'; document.getElementById('2412.03163v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.03163v1-abstract-full" style="display: none;"> Low-frequency radio emission from the Large Magellanic Cloud~(LMC) is assumed to be dominated by nonthermal synchrotron radiation from energy loss of energetic $e^+/e^-$ in magnetic field. Two different kinds of sources of $e^+/e^-$, dark matter~(DM) annihilation and cosmic rays~(CR) related to massive stars, are taken into account in this paper. We fit the multiple low-frequency radio observations, from 19.7 MHz to 1.4 GHz, with a double power-law model $S_{nth} =S_{DM}(\frac 谓{谓_{\star}})^{-伪_{DM}}+S_{CR}( \frac 谓{谓_{\star}})^{-伪_{CR}} $. $谓_{\star}$ is set to be $1.4$ GHz and $S_{CR}$ could be determined from the 24 $渭m$ luminosity based on the global radio-infrared correlation. Our best fit with a fixed $伪_{CR}$ changing from $0.80$ to $0.55$ yields $伪_{DM}$ ranging from $0.21$ to $0.66$. Given a fixed value of $伪_{CR}$, we derive the upper limits of synchrotron emission induced by dark matter annihilation at different radio frequencies. Larger value of $伪_{CR}$ represents for a harder $e^+/e^-$ spectrum from cosmic rays, which leads to a smaller value of $伪_{DM}$ and allow less synchrotron emission resulted from dark matter annihilation in lower frequency. Under the same assumption on the magnetic field, we find that the lower the frequency, the stronger the restriction on DM parameter space. Meanwhile, as the peak frequency of synchrotron radiation decrease with the energy of $e^+/e^-$, constraints on DM properties obtained from lower frequency are more severe in the case of DM with lower mass. Future low-frequency radio survey should be considered a promising and powerful way to constrain DM. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03163v1-abstract-full').style.display = 'none'; document.getElementById('2412.03163v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 7 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.02229">arXiv:2412.02229</a> <span> [<a href="https://arxiv.org/pdf/2412.02229">pdf</a>, <a href="https://arxiv.org/format/2412.02229">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> First Pulsar Polarization Array Limits on Ultralight Axion-like Dark Matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Xue%2C+X">Xiao Xue</a>, <a href="/search/hep-ph?searchtype=author&query=Dai%2C+S">Shi Dai</a>, <a href="/search/hep-ph?searchtype=author&query=Luu%2C+H+N">Hoang Nhan Luu</a>, <a href="/search/hep-ph?searchtype=author&query=Liu%2C+T">Tao Liu</a>, <a href="/search/hep-ph?searchtype=author&query=Ren%2C+J">Jing Ren</a>, <a href="/search/hep-ph?searchtype=author&query=Shu%2C+J">Jing Shu</a>, <a href="/search/hep-ph?searchtype=author&query=Zhao%2C+Y">Yue Zhao</a>, <a href="/search/hep-ph?searchtype=author&query=Zic%2C+A">Andrew Zic</a>, <a href="/search/hep-ph?searchtype=author&query=Bhat%2C+N+D+R">N. D. Ramesh Bhat</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Feng%2C+Y">Yi Feng</a>, <a href="/search/hep-ph?searchtype=author&query=Hobbs%2C+G">George Hobbs</a>, <a href="/search/hep-ph?searchtype=author&query=Kapur%2C+A">Agastya Kapur</a>, <a href="/search/hep-ph?searchtype=author&query=Manchester%2C+R+N">Richard N. Manchester</a>, <a href="/search/hep-ph?searchtype=author&query=Mandow%2C+R">Rami Mandow</a>, <a href="/search/hep-ph?searchtype=author&query=Mishra%2C+S">Saurav Mishra</a>, <a href="/search/hep-ph?searchtype=author&query=Reardon%2C+D+J">Daniel J. Reardon</a>, <a href="/search/hep-ph?searchtype=author&query=Russell%2C+C+J">Christopher J. Russell</a>, <a href="/search/hep-ph?searchtype=author&query=Shannon%2C+R+M">Ryan M. Shannon</a>, <a href="/search/hep-ph?searchtype=author&query=Wang%2C+S">Shuangqiang Wang</a>, <a href="/search/hep-ph?searchtype=author&query=Zhang%2C+L">Lei Zhang</a>, <a href="/search/hep-ph?searchtype=author&query=Zhang%2C+S">Songbo Zhang</a>, <a href="/search/hep-ph?searchtype=author&query=Zhu%2C+X">Xingjiang Zhu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.02229v1-abstract-short" style="display: inline;"> We conduct the first-ever Pulsar Polarization Array (PPA) analysis to detect the ultralight Axion-Like Dark Matter (ALDM) using the polarization data of 22 millisecond pulsars from the third data release of Parkes Pulsar Timing Array. As one of the major dark matter candidates, the ultralight ALDM exhibits a pronounced wave nature on astronomical scales and offers a promising solution to small-sca… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02229v1-abstract-full').style.display = 'inline'; document.getElementById('2412.02229v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.02229v1-abstract-full" style="display: none;"> We conduct the first-ever Pulsar Polarization Array (PPA) analysis to detect the ultralight Axion-Like Dark Matter (ALDM) using the polarization data of 22 millisecond pulsars from the third data release of Parkes Pulsar Timing Array. As one of the major dark matter candidates, the ultralight ALDM exhibits a pronounced wave nature on astronomical scales and offers a promising solution to small-scale structure issues within local galaxies. While the linearly polarized pulsar light travels through the ALDM galactic halo, its position angle (PA) can be subject to an oscillation induced by the ALDM Chern-Simons coupling with electromagnetic field. The PPA is thus especially suited for detecting the ultralight ALDM by correlating polarization data across the arrayed pulsars. To accomplish this task, we develop an advanced Bayesian analysis framework that allows us to construct pulsar PA residual time series, model noise contributions properly and search for pulsar cross-correlations. We find that for an ALDM density of $蟻_0=0.4\,\textrm{GeV}/\textrm{cm}^3$, the Parkes PPA offers the best global limits on the ALDM Chern-Simons coupling, namely $\lesssim 10^{-13.5}-10^{-12.2}~{\rm GeV}^{-1}$, for the mass range of $10^{-22} - 10^{-21}~{\rm eV}$. The crucial role of pulsar cross-correlation in recognizing the nature of the derived limits is also highlighted. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.02229v1-abstract-full').style.display = 'none'; document.getElementById('2412.02229v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">6+15 pages, 10 figures, 2 tables, submitted to the journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.00198">arXiv:2412.00198</a> <span> [<a href="https://arxiv.org/pdf/2412.00198">pdf</a>, <a href="https://arxiv.org/format/2412.00198">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Improving the performance of weak supervision searches using data augmentation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zong-En Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chiang%2C+C">Cheng-Wei Chiang</a>, <a href="/search/hep-ph?searchtype=author&query=Hsieh%2C+F">Feng-Yang Hsieh</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.00198v1-abstract-short" style="display: inline;"> Weak supervision combines the advantages of training on real data with the ability to exploit signal properties. However, training a neural network using weak supervision often requires an excessive amount of signal data, which severely limits its practical applicability. In this study, we propose addressing this limitation through data augmentation, increasing the training data's size and diversi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00198v1-abstract-full').style.display = 'inline'; document.getElementById('2412.00198v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.00198v1-abstract-full" style="display: none;"> Weak supervision combines the advantages of training on real data with the ability to exploit signal properties. However, training a neural network using weak supervision often requires an excessive amount of signal data, which severely limits its practical applicability. In this study, we propose addressing this limitation through data augmentation, increasing the training data's size and diversity. Specifically, we focus on physics-inspired data augmentation methods, such as $p_{\text{T}}$ smearing and jet rotation. Our results demonstrate that data augmentation can significantly enhance the performance of weak supervision, enabling neural networks to learn efficiently from substantially less data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.00198v1-abstract-full').style.display = 'none'; document.getElementById('2412.00198v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.11648">arXiv:2411.11648</a> <span> [<a href="https://arxiv.org/pdf/2411.11648">pdf</a>, <a href="https://arxiv.org/ps/2411.11648">ps</a>, <a href="https://arxiv.org/format/2411.11648">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Evidence for Two Excited $惟^{-}$ Hyperons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Afedulidis%2C+O">O. Afedulidis</a>, <a href="/search/hep-ph?searchtype=author&query=Ai%2C+X+C">X. C. Ai</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+H+-">H. -R. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a>, <a href="/search/hep-ph?searchtype=author&query=Brueggemann%2C+A">A. Brueggemann</a> , et al. (650 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.11648v1-abstract-short" style="display: inline;"> Using $e^+e^-$ collision data corresponding to an integrated luminosity of 19 fb$^{-1}$ collected by the BESIII detector at center-of-mass energies ranging from 4.13 to 4.70 GeV, we report the first evidence for a new excited $惟^{-}$ hyperon, the $惟^*(2109)^{-}$, through the process $e^+ e^- \to 惟^*(2109)^{-} \bar惟^{+} +c.c.$ with a significance of 3.7 $蟽$. The mass and width of $惟^*(2109)^{-}$ ar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11648v1-abstract-full').style.display = 'inline'; document.getElementById('2411.11648v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.11648v1-abstract-full" style="display: none;"> Using $e^+e^-$ collision data corresponding to an integrated luminosity of 19 fb$^{-1}$ collected by the BESIII detector at center-of-mass energies ranging from 4.13 to 4.70 GeV, we report the first evidence for a new excited $惟^{-}$ hyperon, the $惟^*(2109)^{-}$, through the process $e^+ e^- \to 惟^*(2109)^{-} \bar惟^{+} +c.c.$ with a significance of 3.7 $蟽$. The mass and width of $惟^*(2109)^{-}$ are measured to be $2108.8 \pm 5.5_{\rm stat} \pm 1.5_{\rm syst} {\rm MeV}/c^{2}$ and $21.6 \pm 17.7_{\rm stat} \pm 9.4_{\rm syst} {\rm MeV}$, respectively. We also present evidence for production of the $惟^*(2012)^{-}$ in the process $e^+ e^- \to 惟^*(2012)^{-} \bar惟^{+} +c.c.$ with a significance of 3.7 $蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.11648v1-abstract-full').style.display = 'none'; document.getElementById('2411.11648v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 2 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.17559">arXiv:2410.17559</a> <span> [<a href="https://arxiv.org/pdf/2410.17559">pdf</a>, <a href="https://arxiv.org/format/2410.17559">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Polarization study of the P-wave charmonium radiative decay into a light vector meson at $e^{+}e^{-}$ collider experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Y">Yong-Qing Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Hong%2C+P">Peng-Cheng Hong</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhuo Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Shan%2C+W">Wei Shan</a>, <a href="/search/hep-ph?searchtype=author&query=Song%2C+W">Wei-Min Song</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.17559v1-abstract-short" style="display: inline;"> In this work, a formalism is presented for the helicity amplitude analysis of the decays $蠄(2S) \to 纬_1 蠂_{cJ},~ 蠂_{cJ} \to 纬_2 V (V=蟻^0,~蠁,~蠅)$~(the subscript 1,2 is used to distinguish the two radiative photons), and the polarization expressions of the P-wave charmonia $蠂_{cJ}$ and the vector mesons $蟻^0, 蠁, 蠅$ for experimental measurements at Electron-Positron Collider. In addition, we derive t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17559v1-abstract-full').style.display = 'inline'; document.getElementById('2410.17559v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.17559v1-abstract-full" style="display: none;"> In this work, a formalism is presented for the helicity amplitude analysis of the decays $蠄(2S) \to 纬_1 蠂_{cJ},~ 蠂_{cJ} \to 纬_2 V (V=蟻^0,~蠁,~蠅)$~(the subscript 1,2 is used to distinguish the two radiative photons), and the polarization expressions of the P-wave charmonia $蠂_{cJ}$ and the vector mesons $蟻^0, 蠁, 蠅$ for experimental measurements at Electron-Positron Collider. In addition, we derive the formulae of the angular distributions of the $蠂_{c1,2} \to 纬V$ to extract the degree of transverse polarization $P_T$ of $e^+ e^-$ pairs with symmetric beam energy as well as the ratios of two helicity amplitudes $x$ (in $蠂_{c1}$ decays) and $x,~y$ (in $蠂_{c2}$ decays) representing the relative magnitudes of transverse to longitudinal polarization amplitude, and validate it by performing the Monte Carlo simulation. Finally, the statistical sensitivity of $P_T$, $x$ and $y$ are estimated based on the large $蠄(2S)$ data samples collected at the current and proposed future $e^+e^-$ collider experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.17559v1-abstract-full').style.display = 'none'; document.getElementById('2410.17559v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">26 pages, 13 figures. Submitted to CPC</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.13515">arXiv:2410.13515</a> <span> [<a href="https://arxiv.org/pdf/2410.13515">pdf</a>, <a href="https://arxiv.org/format/2410.13515">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Lattice">hep-lat</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41467-024-55042-y">10.1038/s41467-024-55042-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of a rare beta decay of the charmed baryon with a Graph Neural Network </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Afedulidis%2C+O">O. Afedulidis</a>, <a href="/search/hep-ph?searchtype=author&query=Ai%2C+X+C">X. C. Ai</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+H+-">H. -R. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a> , et al. (637 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.13515v2-abstract-short" style="display: inline;"> The beta decay of the lightest charmed baryon $螞_c^+$ provides unique insights into the fundamental mechanism of strong and electro-weak interactions, serving as a testbed for investigating non-perturbative quantum chromodynamics and constraining the Cabibbo-Kobayashi-Maskawa (CKM) matrix parameters. This article presents the first observation of the Cabibbo-suppressed decay… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13515v2-abstract-full').style.display = 'inline'; document.getElementById('2410.13515v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.13515v2-abstract-full" style="display: none;"> The beta decay of the lightest charmed baryon $螞_c^+$ provides unique insights into the fundamental mechanism of strong and electro-weak interactions, serving as a testbed for investigating non-perturbative quantum chromodynamics and constraining the Cabibbo-Kobayashi-Maskawa (CKM) matrix parameters. This article presents the first observation of the Cabibbo-suppressed decay $螞_c^+ \rightarrow n e^+ 谓_{e}$, utilizing $4.5~\mathrm{fb}^{-1}$ of electron-positron annihilation data collected with the BESIII detector. A novel Graph Neural Network based technique effectively separates signals from dominant backgrounds, notably $螞_c^+ \rightarrow 螞e^+ 谓_{e}$, achieving a statistical significance exceeding $10蟽$. The absolute branching fraction is measured to be $(3.57\pm0.34_{\mathrm{stat.}}\pm0.14_{\mathrm{syst.}})\times 10^{-3}$. For the first time, the CKM matrix element $\left|V_{cd}\right|$ is extracted via a charmed baryon decay as $0.208\pm0.011_{\rm exp.}\pm0.007_{\rm LQCD}\pm0.001_{蟿_{螞_c^+}}$. This work highlights a new approach to further understand fundamental interactions in the charmed baryon sector, and showcases the power of modern machine learning techniques in experimental high-energy physics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13515v2-abstract-full').style.display = 'none'; document.getElementById('2410.13515v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Commun. 16, 681 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.13368">arXiv:2410.13368</a> <span> [<a href="https://arxiv.org/pdf/2410.13368">pdf</a>, <a href="https://arxiv.org/format/2410.13368">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Observation of the Singly Cabibbo-Suppressed Decay $螞_c^{+}\to p蟺^0$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Afedulidis%2C+O">O. Afedulidis</a>, <a href="/search/hep-ph?searchtype=author&query=Ai%2C+X+C">X. C. Ai</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+H+-">H. -R. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a> , et al. (638 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.13368v1-abstract-short" style="display: inline;"> Utilizing 4.5${~\rm{fb}}^{-1}$ of $e^+e^-$ annihilation data collected with the BESIII detector at the BEPCII collider at center-of-mass energies between 4.600 and 4.699 GeV, the first observation of the singly Cabibbo-suppressed decay $螞_c^{+}\to p蟺^0$ is presented, with a statistical significance of $5.4蟽$. The ratio of the branching fractions of $螞_c^{+}\to p蟺^0$ and $螞_c^{+}\to p畏$ is measured… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13368v1-abstract-full').style.display = 'inline'; document.getElementById('2410.13368v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.13368v1-abstract-full" style="display: none;"> Utilizing 4.5${~\rm{fb}}^{-1}$ of $e^+e^-$ annihilation data collected with the BESIII detector at the BEPCII collider at center-of-mass energies between 4.600 and 4.699 GeV, the first observation of the singly Cabibbo-suppressed decay $螞_c^{+}\to p蟺^0$ is presented, with a statistical significance of $5.4蟽$. The ratio of the branching fractions of $螞_c^{+}\to p蟺^0$ and $螞_c^{+}\to p畏$ is measured as $\mathcal{B}(螞_c^{+}\to p蟺^0)/\mathcal{B}(螞_c^{+}\to p畏)=(0.120\pm0.026_{\rm stat.}\pm0.007_{\rm syst.})$. This result resolves the longstanding discrepancy between earlier experimental searches, providing both a decisive conclusion and valuable input for QCD-inspired theoretical models. A sophisticated deep learning approach using a Transformer-based architecture is employed to distinguish the signal from the prevalent hadronic backgrounds, complemented by thorough validation and systematic uncertainty quantification. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13368v1-abstract-full').style.display = 'none'; document.getElementById('2410.13368v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 4 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.09847">arXiv:2410.09847</a> <span> [<a href="https://arxiv.org/pdf/2410.09847">pdf</a>, <a href="https://arxiv.org/format/2410.09847">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> QCD sum rule analysis of $0^{+}$ four-quark states </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Li%2C+S">Shuang-Hong Li</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Ze-Sheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Y">Yi-Xin Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Jin%2C+H">Hong-Ying Jin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.09847v3-abstract-short" style="display: inline;"> We present a comprehensive QCD sum rules analysis at next-to-leading order for all types of $J^P=0^{+}$ four-quark states composed of $u$, $d$, and $s$ quarks. The eigenvectors of the renormalization matrix are chosen to be the renormalized four-quark operators, which can be equally interpreted as tetraquark or molecule operators. Meanwhile, the typical nonet masses given by bare tetraquark operat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09847v3-abstract-full').style.display = 'inline'; document.getElementById('2410.09847v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.09847v3-abstract-full" style="display: none;"> We present a comprehensive QCD sum rules analysis at next-to-leading order for all types of $J^P=0^{+}$ four-quark states composed of $u$, $d$, and $s$ quarks. The eigenvectors of the renormalization matrix are chosen to be the renormalized four-quark operators, which can be equally interpreted as tetraquark or molecule operators. Meanwhile, the typical nonet masses given by bare tetraquark operators are lower than those given by bare molecule operators. Most of the nonet masses are around $1-2\text{GeV}$, and they can be interpreted as the $0^+$ mesons observed in experiments. We find a category of four-quark nonets with masses $\lesssim1\text{GeV}$, potentially corresponding to the light $0^+$ mesons $f_0(500)$, $K^*_0(700)$, $f_0(980)$, and $a_0(980)$. On the other hand, the possible 27-fold states are heavier than most of the nonets, with masses $\gtrsim 2\text{GeV}$. The main uncertainty arises from the factorization of high-dimensional condensates, which usually underestimates their values. To address this, we introduce deviation factors for the dimension-6, -8, and -10 condensates, and vary them over a wide range to obtain conservative estimates of the $0^+$ four-quark state masses. Some general properties of the $0^+$ light four-quark states can be derived that do not rely on precise numerical values. We also find that the ambiguity in the factorization of the dimension-8 condensate can introduce a larger discrepancy than previously estimated. As a byproduct, we propose a simple trick for renormalizing multi-quark operators at the one-loop level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.09847v3-abstract-full').style.display = 'none'; document.getElementById('2410.09847v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">61 pages, 40 figures, 11 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.03172">arXiv:2409.03172</a> <span> [<a href="https://arxiv.org/pdf/2409.03172">pdf</a>, <a href="https://arxiv.org/format/2409.03172">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Further study of the maximally symmetry breaking patterns in an ${\rm SU}(8)$ theory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+N">Ning Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhiyuan Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Hou%2C+Z">Zhanpeng Hou</a>, <a href="/search/hep-ph?searchtype=author&query=Teng%2C+Z">Zhaolong Teng</a>, <a href="/search/hep-ph?searchtype=author&query=Wang%2C+B">Bin Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.03172v2-abstract-short" style="display: inline;"> The ${\rm SU}(8)$ was previously found to be the minimal simple gauge group where all three-generational Standard Model fermions can be non-trivially embedded, and it is maximally broken into ${\rm SU}(8)\to {\cal G}_{441}\equiv {\rm SU}(4)_s \otimes {\rm SU}(4)_W \otimes {\rm U}(1)_{X_0}$ at the GUT scale by the ${\rm SU}(8)$ adjoint Higgs field. Gauge symmetries in the strong and the weak sector… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03172v2-abstract-full').style.display = 'inline'; document.getElementById('2409.03172v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.03172v2-abstract-full" style="display: none;"> The ${\rm SU}(8)$ was previously found to be the minimal simple gauge group where all three-generational Standard Model fermions can be non-trivially embedded, and it is maximally broken into ${\rm SU}(8)\to {\cal G}_{441}\equiv {\rm SU}(4)_s \otimes {\rm SU}(4)_W \otimes {\rm U}(1)_{X_0}$ at the GUT scale by the ${\rm SU}(8)$ adjoint Higgs field. Gauge symmetries in the strong and the weak sectors are extended by one and two ranks, respectively. The sequential strong-weak-weak (SWW) symmetry breaking stages were found to generate the observed hierarchical SM quark/lepton masses as well as the Cabibbo-Kobayashi-Maskawa (CKM) mixing pattern with the precise flavor identifications [1, 2]. We further study the possible weak-strong-weak (WSW) and weak-weak-strong (WWS) symmetry breaking patterns, and compare with the results that we have obtained by following the SWW sequence. The two-loop RGEs following both patterns are derived, where we cannot achieve the gauge coupling unification in the field theory framework. Based on these analyses, we suggest the gauge coupling unification to be interpreted in the context of the Ka{膷}-Moody Lie algebra. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.03172v2-abstract-full').style.display = 'none'; document.getElementById('2409.03172v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">55 pages plus references, 3 figures, 21 tables. arXiv admin note: substantial text overlap with arXiv:2402.10471</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.06677">arXiv:2408.06677</a> <span> [<a href="https://arxiv.org/pdf/2408.06677">pdf</a>, <a href="https://arxiv.org/format/2408.06677">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Search for $畏_c(2S)\to蠅蠅$ and $蠅蠁$ decays and measurements of $蠂_{cJ}\to蠅蠅$ and $蠅蠁$ in $蠄(2S)$ radiative processes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Afedulidis%2C+O">O. Afedulidis</a>, <a href="/search/hep-ph?searchtype=author&query=Ai%2C+X+C">X. C. Ai</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+H+-">H. -R. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a> , et al. (643 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.06677v1-abstract-short" style="display: inline;"> Using $(2712\pm 14)$ $\times$ 10$^{6}$ $蠄(2S)$ events collected with the BESIII detector at the BEPCII collider, we search for the decays $畏_{c}(2S)\to蠅蠅$ and $畏_{c}(2S)\to蠅蠁$ via the process $蠄(2S)\to纬畏_{c}(2S)$. Evidence of $畏_{c}(2S)\to蠅蠅$ is found with a statistical significance of $3.2蟽$. The branching fraction is measured to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.06677v1-abstract-full').style.display = 'inline'; document.getElementById('2408.06677v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.06677v1-abstract-full" style="display: none;"> Using $(2712\pm 14)$ $\times$ 10$^{6}$ $蠄(2S)$ events collected with the BESIII detector at the BEPCII collider, we search for the decays $畏_{c}(2S)\to蠅蠅$ and $畏_{c}(2S)\to蠅蠁$ via the process $蠄(2S)\to纬畏_{c}(2S)$. Evidence of $畏_{c}(2S)\to蠅蠅$ is found with a statistical significance of $3.2蟽$. The branching fraction is measured to be $\mathcal{B}(畏_{c}(2S)\to蠅蠅)=(5.65\pm3.77(\rm stat.)\pm5.32(\rm syst.))\times10^{-4}$. No statistically significant signal is observed for the decay $畏_{c}(2S)\to蠅蠁$. The upper limit of the branching fraction at the 90\% confidence level is determined to be $\mathcal{B}(蠄(2S)\to纬畏_{c}(2S),畏_{c}(2S)\to蠅蠁)<2.24\times 10^{-7}$. We also update the branching fractions of $蠂_{cJ}\to 蠅蠅$ and $蠂_{cJ}\to蠅蠁$ decays via the $蠄(2S)\to纬蠂_{cJ}$ transition. The branching fractions are determined to be $\mathcal{B}(蠂_{c0}\to蠅蠅)=(10.63\pm0.11\pm0.46)\times 10^{-4}$, $\mathcal{B}(蠂_{c1}\to蠅蠅)=(6.39\pm0.07\pm0.29)\times 10^{-4}$, $\mathcal{B}(蠂_{c2}\to蠅蠅)=(8.50\pm0.08\pm0.38)\times 10^{-4}$, $\mathcal{B}(蠂_{c0}\to蠅蠁)=(1.18\pm0.03\pm0.05)\times 10^{-4}$, $\mathcal{B}(蠂_{c1}\to蠅蠁)=(2.03\pm0.15\pm0.12)\times 10^{-5}$, and $\mathcal{B}(蠂_{c2}\to蠅蠁)=(9.37\pm1.07\pm0.59)\times 10^{-6}$, where the first uncertainties are statistical and the second are systematic. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.06677v1-abstract-full').style.display = 'none'; document.getElementById('2408.06677v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.11727">arXiv:2407.11727</a> <span> [<a href="https://arxiv.org/pdf/2407.11727">pdf</a>, <a href="https://arxiv.org/ps/2407.11727">ps</a>, <a href="https://arxiv.org/format/2407.11727">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.110.052002">10.1103/PhysRevD.110.052002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the branching fraction of $D^+_s\to \ell^+谓_\ell$ via $e^+e^-\to D^{*+}_{s} D^{*-}_{s}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Afedulidis%2C+O">O. Afedulidis</a>, <a href="/search/hep-ph?searchtype=author&query=Ai%2C+X+C">X. C. Ai</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+H+-">H. -R. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a> , et al. (634 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.11727v3-abstract-short" style="display: inline;"> Based on $10.64~\mathrm{fb}^{-1}$ of $e^+e^-$ collision data taken at center-of-mass energies between 4.237 and 4.699 GeV with the BESIII detector, we study the leptonic $D^+_s$ decays using the $e^+e^-\to D^{*+}_{s} D^{*-}_{s}$ process. The branching fractions of $D_s^+\to\ell^+谓_{\ell}\,(\ell=渭,蟿)$ are measured to be $\mathcal{B}(D_s^+\to渭^+谓_渭)=(0.547\pm0.026_{\rm stat}\pm0.016_{\rm syst})\%$ a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.11727v3-abstract-full').style.display = 'inline'; document.getElementById('2407.11727v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.11727v3-abstract-full" style="display: none;"> Based on $10.64~\mathrm{fb}^{-1}$ of $e^+e^-$ collision data taken at center-of-mass energies between 4.237 and 4.699 GeV with the BESIII detector, we study the leptonic $D^+_s$ decays using the $e^+e^-\to D^{*+}_{s} D^{*-}_{s}$ process. The branching fractions of $D_s^+\to\ell^+谓_{\ell}\,(\ell=渭,蟿)$ are measured to be $\mathcal{B}(D_s^+\to渭^+谓_渭)=(0.547\pm0.026_{\rm stat}\pm0.016_{\rm syst})\%$ and $\mathcal{B}(D_s^+\to蟿^+谓_蟿)=(5.60\pm0.16_{\rm stat}\pm0.20_{\rm syst})\%$, respectively. The product of the decay constant and Cabibbo-Kobayashi-Maskawa matrix element $|V_{cs}|$ is determined to be $f_{D_s^+}|V_{cs}|=(246.5\pm5.9_{\rm stat}\pm3.6_{\rm syst}\pm0.5_{\rm input})_{渭谓}~\mathrm{MeV}$ and $f_{D_s^+}|V_{cs}|=(252.7\pm3.6_{\rm stat}\pm4.5_{\rm syst}\pm0.6_{\rm input}))_{蟿谓}~\mathrm{MeV}$, respectively. Taking the value of $|V_{cs}|$ from a global fit in the Standard Model, we obtain ${f_{D^+_s}}=(252.8\pm6.0_{\rm stat}\pm3.7_{\rm syst}\pm0.6_{\rm input})_{渭谓}$ MeV and ${f_{D^+_s}}=(259.2\pm3.6_{\rm stat}\pm4.5_{\rm syst}\pm0.6_{\rm input})_{蟿谓}$ MeV, respectively. Conversely, taking the value for $f_{D_s^+}$ from the latest lattice quantum chromodynamics calculation, we obtain $|V_{cs}| =(0.986\pm0.023_{\rm stat}\pm0.014_{\rm syst}\pm0.003_{\rm input})_{渭谓}$ and $|V_{cs}| = (1.011\pm0.014_{\rm stat}\pm0.018_{\rm syst}\pm0.003_{\rm input})_{蟿谓}$, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.11727v3-abstract-full').style.display = 'none'; document.getElementById('2407.11727v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 110, 052002 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.08698">arXiv:2406.08698</a> <span> [<a href="https://arxiv.org/pdf/2406.08698">pdf</a>, <a href="https://arxiv.org/format/2406.08698">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Constraints on Ultra Heavy Dark Matter Properties from Dwarf Spheroidal Galaxies with LHAASO Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/hep-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/hep-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/hep-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (255 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.08698v1-abstract-short" style="display: inline;"> In this work we try to search for signals generated by ultra-heavy dark matter at the Large High Altitude Air Shower Observatory (LHAASO) data. We look for possible gamma-ray by dark matter annihilation or decay from 16 dwarf spheroidal galaxies in the field of view of LHAASO. Dwarf spheroidal galaxies are among the most promising targets for indirect detection of dark matter which have low fluxes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.08698v1-abstract-full').style.display = 'inline'; document.getElementById('2406.08698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.08698v1-abstract-full" style="display: none;"> In this work we try to search for signals generated by ultra-heavy dark matter at the Large High Altitude Air Shower Observatory (LHAASO) data. We look for possible gamma-ray by dark matter annihilation or decay from 16 dwarf spheroidal galaxies in the field of view of LHAASO. Dwarf spheroidal galaxies are among the most promising targets for indirect detection of dark matter which have low fluxes of astrophysical $纬$-ray background while large amount of dark matter. By analyzing more than 700 days observational data at LHAASO, no significant dark matter signal from 1 TeV to 1 EeV is detected. Accordingly we derive the most stringent constraints on the ultra-heavy dark matter annihilation cross-section up to EeV. The constraints on the lifetime of dark matter in decay mode are also derived. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.08698v1-abstract-full').style.display = 'none'; document.getElementById('2406.08698v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 12 figures, accepted by PRL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.17792">arXiv:2405.17792</a> <span> [<a href="https://arxiv.org/pdf/2405.17792">pdf</a>, <a href="https://arxiv.org/format/2405.17792">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> JUNO Sensitivity to Invisible Decay Modes of Neutrons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ph?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ph?searchtype=author&query=Adamowicz%2C+K">Kai Adamowicz</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ph?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ph?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ph?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ph?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ph?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/hep-ph?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ph?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ph?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ph?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ph?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ph?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ph?searchtype=author&query=Beretta%2C+M">Marco Beretta</a>, <a href="/search/hep-ph?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a>, <a href="/search/hep-ph?searchtype=author&query=Bick%2C+D">Daniel Bick</a> , et al. (635 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.17792v1-abstract-short" style="display: inline;"> We explore the bound neutrons decay into invisible particles (e.g., $n\rightarrow 3 谓$ or $nn \rightarrow 2 谓$) in the JUNO liquid scintillator detector. The invisible decay includes two decay modes: $ n \rightarrow { inv} $ and $ nn \rightarrow { inv} $. The invisible decays of $s$-shell neutrons in $^{12}{\rm C}$ will leave a highly excited residual nucleus. Subsequently, some de-excitation mode… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17792v1-abstract-full').style.display = 'inline'; document.getElementById('2405.17792v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17792v1-abstract-full" style="display: none;"> We explore the bound neutrons decay into invisible particles (e.g., $n\rightarrow 3 谓$ or $nn \rightarrow 2 谓$) in the JUNO liquid scintillator detector. The invisible decay includes two decay modes: $ n \rightarrow { inv} $ and $ nn \rightarrow { inv} $. The invisible decays of $s$-shell neutrons in $^{12}{\rm C}$ will leave a highly excited residual nucleus. Subsequently, some de-excitation modes of the excited residual nuclei can produce a time- and space-correlated triple coincidence signal in the JUNO detector. Based on a full Monte Carlo simulation informed with the latest available data, we estimate all backgrounds, including inverse beta decay events of the reactor antineutrino $\bar谓_e$, natural radioactivity, cosmogenic isotopes and neutral current interactions of atmospheric neutrinos. Pulse shape discrimination and multivariate analysis techniques are employed to further suppress backgrounds. With two years of exposure, JUNO is expected to give an order of magnitude improvement compared to the current best limits. After 10 years of data taking, the JUNO expected sensitivities at a 90% confidence level are $蟿/B( n \rightarrow { inv} ) > 5.0 \times 10^{31} \, {\rm yr}$ and $蟿/B( nn \rightarrow { inv} ) > 1.4 \times 10^{32} \, {\rm yr}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17792v1-abstract-full').style.display = 'none'; document.getElementById('2405.17792v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 7 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.08077">arXiv:2405.08077</a> <span> [<a href="https://arxiv.org/pdf/2405.08077">pdf</a>, <a href="https://arxiv.org/format/2405.08077">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.110.092009">10.1103/PhysRevD.110.092009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Methods and stability tests associated with the sterile neutrino search using improved high-energy $谓_渭$ event reconstruction in IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=IceCube+Collaboration"> IceCube Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/hep-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/hep-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/hep-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/hep-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/hep-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/hep-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/hep-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/hep-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/hep-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/hep-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/hep-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/hep-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/hep-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/hep-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/hep-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/hep-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/hep-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/hep-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/hep-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/hep-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (398 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.08077v2-abstract-short" style="display: inline;"> We provide supporting details for the search for a 3+1 sterile neutrino using data collected over eleven years at the IceCube Neutrino Observatory. The analysis uses atmospheric muon-flavored neutrinos from 0.5 to 100\, TeV that traverse the Earth to reach the IceCube detector, and finds a best-fit point at $\sin^2(2胃_{24}) = 0.16$ and $螖m^{2}_{41} = 3.5$ eV$^2$ with a goodness-of-fit p-value of 1… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.08077v2-abstract-full').style.display = 'inline'; document.getElementById('2405.08077v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.08077v2-abstract-full" style="display: none;"> We provide supporting details for the search for a 3+1 sterile neutrino using data collected over eleven years at the IceCube Neutrino Observatory. The analysis uses atmospheric muon-flavored neutrinos from 0.5 to 100\, TeV that traverse the Earth to reach the IceCube detector, and finds a best-fit point at $\sin^2(2胃_{24}) = 0.16$ and $螖m^{2}_{41} = 3.5$ eV$^2$ with a goodness-of-fit p-value of 12\% and consistency with the null hypothesis of no oscillations to sterile neutrinos with a p-value of 3.1\%. Several improvements were made over past analyses, which are reviewed in this article, including upgrades to the reconstruction and the study of sources of systematic uncertainty. We provide details of the fit quality and discuss stability tests that split the data for separate samples, comparing results. We find that the fits are consistent between split data sets. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.08077v2-abstract-full').style.display = 'none'; document.getElementById('2405.08077v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 19 figures, 2 tables. This long-form paper is a companion to the letter "A search for an eV-scale sterile neutrino using improved high-energy 谓渭 event reconstruction in IceCube." Matches published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 110, 092009 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.08070">arXiv:2405.08070</a> <span> [<a href="https://arxiv.org/pdf/2405.08070">pdf</a>, <a href="https://arxiv.org/format/2405.08070">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.133.201804">10.1103/PhysRevLett.133.201804 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for an eV-scale sterile neutrino using improved high-energy $谓_渭$ event reconstruction in IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=IceCube+Collaboration"> IceCube Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/hep-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/hep-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/hep-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/hep-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/hep-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/hep-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/hep-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/hep-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/hep-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/hep-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/hep-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/hep-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/hep-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/hep-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/hep-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/hep-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/hep-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/hep-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/hep-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/hep-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (398 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.08070v2-abstract-short" style="display: inline;"> This Letter presents the result of a 3+1 sterile neutrino search using 10.7 years of IceCube data. We analyze atmospheric muon neutrinos that traverse the Earth with energies ranging from 0.5 to 100 TeV, incorporating significant improvements in modeling neutrino flux and detector response compared to earlier studies. Notably, for the first time, we categorize data into starting and through-going… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.08070v2-abstract-full').style.display = 'inline'; document.getElementById('2405.08070v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.08070v2-abstract-full" style="display: none;"> This Letter presents the result of a 3+1 sterile neutrino search using 10.7 years of IceCube data. We analyze atmospheric muon neutrinos that traverse the Earth with energies ranging from 0.5 to 100 TeV, incorporating significant improvements in modeling neutrino flux and detector response compared to earlier studies. Notably, for the first time, we categorize data into starting and through-going events, distinguishing neutrino interactions with vertices inside or outside the instrumented volume, to improve energy resolution. The best-fit point for a 3+1 model is found to be at $\sin^2(2胃_{24}) = 0.16$ and $螖m^{2}_{41} = 3.5$ eV$^2$, which agrees with previous iterations of this study. The result is consistent with the null hypothesis of no sterile neutrinos with a p-value of 3.1\%. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.08070v2-abstract-full').style.display = 'none'; document.getElementById('2405.08070v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 4 figures. This letter is supported by the long-form paper "Methods and stability tests associated with the sterile neutrino search using improved high-energy $谓_渭$ event reconstruction in IceCube," also appearing on arXiv. Matches published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 133, 201804 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.19202">arXiv:2404.19202</a> <span> [<a href="https://arxiv.org/pdf/2404.19202">pdf</a>, <a href="https://arxiv.org/format/2404.19202">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.110.056040">10.1103/PhysRevD.110.056040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dihadron helicity correlation in photon-nucleus collisions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhao-Xuan Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Dong%2C+H">Hui Dong</a>, <a href="/search/hep-ph?searchtype=author&query=Wei%2C+S">Shu-Yi Wei</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.19202v3-abstract-short" style="display: inline;"> The helicity correlation of two back-to-back hadrons is a powerful tool that makes it possible to probe the longitudinal spin transfer, $G_{1L}$, in unpolarized hadronic collisions. In this work, we investigate the helicity correlation of back-to-back dihadrons produced in photon-nucleus collisions with both space-like and quasireal photons and explore its potential in understanding the flavor dep… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.19202v3-abstract-full').style.display = 'inline'; document.getElementById('2404.19202v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.19202v3-abstract-full" style="display: none;"> The helicity correlation of two back-to-back hadrons is a powerful tool that makes it possible to probe the longitudinal spin transfer, $G_{1L}$, in unpolarized hadronic collisions. In this work, we investigate the helicity correlation of back-to-back dihadrons produced in photon-nucleus collisions with both space-like and quasireal photons and explore its potential in understanding the flavor dependence of spin-dependent fragmentation functions. We present helicity amplitudes of partonic scatterings with both virtual and real photons and make numerical predictions for the dihadron helicity correlations at the future Electron Ion Collider experiment and the current RHIC/LHC ultra-peripheral collision experiment. Future experimental measurements can also illuminate the fragmentation function of circularly polarized gluons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.19202v3-abstract-full').style.display = 'none'; document.getElementById('2404.19202v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D 110 (2024) 5, 056040 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.11441">arXiv:2404.11441</a> <span> [<a href="https://arxiv.org/pdf/2404.11441">pdf</a>, <a href="https://arxiv.org/format/2404.11441">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Two-loop electroweak corrections to the Higgs boson rare decay process $H\to Z纬$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zi-Qiang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+L">Long-Bin Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Qiao%2C+C">Cong-Feng Qiao</a>, <a href="/search/hep-ph?searchtype=author&query=Zhu%2C+R">Ruilin Zhu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.11441v2-abstract-short" style="display: inline;"> Recently, the ATLAS and CMS collaborations jointly announced the first evidence of the rare Higgs boson decay channel $H\to Z纬$, with a ratio of $2.2\pm 0.7$ times the leading order standard model (SM) prediction. In order to face this challenge, it is urgent to produce an even more accurate calculation within the SM. To this end, we calculate in this paper the next-to-leading order (NLO) electrow… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11441v2-abstract-full').style.display = 'inline'; document.getElementById('2404.11441v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.11441v2-abstract-full" style="display: none;"> Recently, the ATLAS and CMS collaborations jointly announced the first evidence of the rare Higgs boson decay channel $H\to Z纬$, with a ratio of $2.2\pm 0.7$ times the leading order standard model (SM) prediction. In order to face this challenge, it is urgent to produce an even more accurate calculation within the SM. To this end, we calculate in this paper the next-to-leading order (NLO) electroweak (EW) corrections to the $H\to Z纬$ process, in which the NLO quantum chromodynamics (QCD) corrections were found tiny. Our calculation finds that the inclusion of NLO EW corrections greatly enhances the prediction reliability. To tame the theoretical uncertainty, we adopt five different renormalization schemes. Combining our result with previous NLO QCD corrections and the signal-background interference, we conclude that the excess in $H\to Z纬$ cannot be explained within the SM. In fact, the incompatibility between the SM prediction and the LHC measurement of the concerned process is exacerbated upon considering the higher order EW corrections, which implies that something beyond the SM could be involved. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.11441v2-abstract-full').style.display = 'none'; document.getElementById('2404.11441v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication as a Letter in Physical Review D</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.02033">arXiv:2404.02033</a> <span> [<a href="https://arxiv.org/pdf/2404.02033">pdf</a>, <a href="https://arxiv.org/format/2404.02033">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Search for $C$-even states decaying to $D_{s}^{\pm}D_{s}^{*\mp}$ with masses between $4.08$ and $4.32~\mathrm{GeV}/c^{2}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Afedulidis%2C+O">O. Afedulidis</a>, <a href="/search/hep-ph?searchtype=author&query=Ai%2C+X+C">X. C. Ai</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+H+-">H. -R. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a> , et al. (638 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.02033v2-abstract-short" style="display: inline;"> Six $C$-even states, denoted as $X$, with quantum numbers $J^{PC}=0^{-+}$, $1^{\pm+}$, or $2^{\pm+}$, are searched for via the $e^+e^-\to纬D_{s}^{\pm}D_{s}^{*\mp}$ process using $(1667.39\pm8.84)~\mathrm{pb}^{-1}$ of $e^+e^-$ collision data collected with the BESIII detector operating at the BEPCII storage ring at center-of-mass energy of $\sqrt{s}=(4681.92\pm0.30)~\mathrm{MeV}$. No statistically s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02033v2-abstract-full').style.display = 'inline'; document.getElementById('2404.02033v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.02033v2-abstract-full" style="display: none;"> Six $C$-even states, denoted as $X$, with quantum numbers $J^{PC}=0^{-+}$, $1^{\pm+}$, or $2^{\pm+}$, are searched for via the $e^+e^-\to纬D_{s}^{\pm}D_{s}^{*\mp}$ process using $(1667.39\pm8.84)~\mathrm{pb}^{-1}$ of $e^+e^-$ collision data collected with the BESIII detector operating at the BEPCII storage ring at center-of-mass energy of $\sqrt{s}=(4681.92\pm0.30)~\mathrm{MeV}$. No statistically significant signal is observed in the mass range from $4.08$ to $4.32~\mathrm{GeV}/c^{2}$. The upper limits of $蟽[e^+e^- \to 纬X] \cdot \mathcal{B}[X \to D_{s}^{\pm} D_{s}^{*\mp}]$ at a $90\%$ confidence level are determined. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02033v2-abstract-full').style.display = 'none'; document.getElementById('2404.02033v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 110, 032017 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.10877">arXiv:2403.10877</a> <span> [<a href="https://arxiv.org/pdf/2403.10877">pdf</a>, <a href="https://arxiv.org/ps/2403.10877">ps</a>, <a href="https://arxiv.org/format/2403.10877">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.134.011803">10.1103/PhysRevLett.134.011803 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Test of lepton universality and measurement of the form factors of $D^0\to K^{*}(892)^-渭^+谓_渭$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Afedulidis%2C+O">O. Afedulidis</a>, <a href="/search/hep-ph?searchtype=author&query=Ai%2C+X+C">X. C. Ai</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+H+-">H. -R. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a> , et al. (637 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.10877v3-abstract-short" style="display: inline;"> We report a first study of the semileptonic decay $D^0\rightarrow K^-蟺^0渭^{+}谓_渭$ by analyzing an $e^+e^-$ annihilation data sample of $7.9~\mathrm{fb}^{-1}$ collected at the center-of-mass energy of 3.773 GeV with the BESIII detector. The absolute branching fraction of $D^0\to K^-蟺^0渭^{+}谓_渭$ is measured for the first time to be $(0.729 \pm 0.014_{\rm stat} \pm 0.011_{\rm syst})\%$. Based on an a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10877v3-abstract-full').style.display = 'inline'; document.getElementById('2403.10877v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10877v3-abstract-full" style="display: none;"> We report a first study of the semileptonic decay $D^0\rightarrow K^-蟺^0渭^{+}谓_渭$ by analyzing an $e^+e^-$ annihilation data sample of $7.9~\mathrm{fb}^{-1}$ collected at the center-of-mass energy of 3.773 GeV with the BESIII detector. The absolute branching fraction of $D^0\to K^-蟺^0渭^{+}谓_渭$ is measured for the first time to be $(0.729 \pm 0.014_{\rm stat} \pm 0.011_{\rm syst})\%$. Based on an amplitude analysis, the $S\text{-}{\rm wave}$ contribution is determined to be $(5.76 \pm 0.35_{\rm stat} \pm 0.29_{\rm syst})\%$ of the total decay rate in addition to the dominated $K^{*}(892)^-$ component. The branching fraction of $D^0\to K^{*}(892)^-渭^+谓_渭$ is given to be $(2.062 \pm 0.039_{\rm stat} \pm 0.032_{\rm syst})\%$, which improves the precision of the world average by a factor of 5. Combining with the world average of ${\mathcal B}(D^0\to K^{*}(892)^-e^+谓_e)$, the ratio of the branching fractions obtained is $\frac{{\mathcal B}(D^0\to K^{*}(892)^-渭^+谓_渭)}{{\mathcal B}(D^0\to K^{*}(892)^-e^+谓_e)} = 0.96\pm0.08$, in agreement with lepton flavor universality. Furthermore, assuming single-pole dominance parameterization, the most precise hadronic form factor ratios for $D^0\to K^{*}(892)^{-} 渭^+谓_渭$ are extracted to be $r_{V}=V(0)/A_1(0)=1.37 \pm 0.09_{\rm stat} \pm 0.03_{\rm syst}$ and $r_{2}=A_2(0)/A_1(0)=0.76 \pm 0.06_{\rm stat} \pm 0.02_{\rm syst}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10877v3-abstract-full').style.display = 'none'; document.getElementById('2403.10877v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 134, 011803 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.10134">arXiv:2403.10134</a> <span> [<a href="https://arxiv.org/pdf/2403.10134">pdf</a>, <a href="https://arxiv.org/format/2403.10134">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-024-12987-0">10.1140/epjc/s10052-024-12987-0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of groomed event shape observables in deep-inelastic electron-proton scattering at HERA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=The+H1+collaboration"> The H1 collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Andreev%2C+V">V. Andreev</a>, <a href="/search/hep-ph?searchtype=author&query=Arratia%2C+M">M. Arratia</a>, <a href="/search/hep-ph?searchtype=author&query=Baghdasaryan%2C+A">A. Baghdasaryan</a>, <a href="/search/hep-ph?searchtype=author&query=Baty%2C+A">A. Baty</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Bolz%2C+A">A. Bolz</a>, <a href="/search/hep-ph?searchtype=author&query=Boudry%2C+V">V. Boudry</a>, <a href="/search/hep-ph?searchtype=author&query=Brandt%2C+G">G. Brandt</a>, <a href="/search/hep-ph?searchtype=author&query=Britzger%2C+D">D. Britzger</a>, <a href="/search/hep-ph?searchtype=author&query=Buniatyan%2C+A">A. Buniatyan</a>, <a href="/search/hep-ph?searchtype=author&query=Bystritskaya%2C+L">L. Bystritskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Campbell%2C+A+J">A. J. Campbell</a>, <a href="/search/hep-ph?searchtype=author&query=Avila%2C+K+B+C">K. B. Cantun Avila</a>, <a href="/search/hep-ph?searchtype=author&query=Cerny%2C+K">K. Cerny</a>, <a href="/search/hep-ph?searchtype=author&query=Chekelian%2C+V">V. Chekelian</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Z. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Contreras%2C+J+G">J. G. Contreras</a>, <a href="/search/hep-ph?searchtype=author&query=Cvach%2C+J">J. Cvach</a>, <a href="/search/hep-ph?searchtype=author&query=Dainton%2C+J+B">J. B. Dainton</a>, <a href="/search/hep-ph?searchtype=author&query=Daum%2C+K">K. Daum</a>, <a href="/search/hep-ph?searchtype=author&query=Deshpande%2C+A">A. Deshpande</a>, <a href="/search/hep-ph?searchtype=author&query=Diaconu%2C+C">C. Diaconu</a>, <a href="/search/hep-ph?searchtype=author&query=Drees%2C+A">A. Drees</a>, <a href="/search/hep-ph?searchtype=author&query=Eckerlin%2C+G">G. Eckerlin</a> , et al. (123 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.10134v2-abstract-short" style="display: inline;"> The H1 Collaboration at HERA reports the first measurement of groomed event shape observables in deep inelastic electron-proton scattering (DIS) at $\sqrt{s}=319$ GeV, using data recorded between the years 2003 and 2007 with an integrated luminosity of $351$ pb$^{-1}$. Event shapes provide incisive probes of perturbative and non-perturbative QCD. Grooming techniques have been used for jet measurem… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10134v2-abstract-full').style.display = 'inline'; document.getElementById('2403.10134v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10134v2-abstract-full" style="display: none;"> The H1 Collaboration at HERA reports the first measurement of groomed event shape observables in deep inelastic electron-proton scattering (DIS) at $\sqrt{s}=319$ GeV, using data recorded between the years 2003 and 2007 with an integrated luminosity of $351$ pb$^{-1}$. Event shapes provide incisive probes of perturbative and non-perturbative QCD. Grooming techniques have been used for jet measurements in hadronic collisions; this paper presents the first application of grooming to DIS data. The analysis is carried out in the Breit frame, utilizing the novel Centauro jet clustering algorithm that is designed for DIS event topologies. Events are required to have squared momentum-transfer $Q^2 > 150$ GeV$^2$ and inelasticity $ 0.2 < y < 0.7$. We report measurements of the production cross section of groomed event 1-jettiness and groomed invariant mass for several choices of grooming parameter. Monte Carlo model calculations and analytic calculations based on Soft Collinear Effective Theory are compared to the measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10134v2-abstract-full').style.display = 'none'; document.getElementById('2403.10134v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 17 tables, 7 figures, version as accepted by EPJ C</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DESY-24-036 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> EPJC 84 (2024), 718 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.10109">arXiv:2403.10109</a> <span> [<a href="https://arxiv.org/pdf/2403.10109">pdf</a>, <a href="https://arxiv.org/format/2403.10109">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Measurement of the 1-jettiness event shape observable in deep-inelastic electron-proton scattering at HERA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=The+H1+collaboration"> The H1 collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Andreev%2C+V">V. Andreev</a>, <a href="/search/hep-ph?searchtype=author&query=Arratia%2C+M">M. Arratia</a>, <a href="/search/hep-ph?searchtype=author&query=Baghdasaryan%2C+A">A. Baghdasaryan</a>, <a href="/search/hep-ph?searchtype=author&query=Baty%2C+A">A. Baty</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Bolz%2C+A">A. Bolz</a>, <a href="/search/hep-ph?searchtype=author&query=Boudry%2C+V">V. Boudry</a>, <a href="/search/hep-ph?searchtype=author&query=Brandt%2C+G">G. Brandt</a>, <a href="/search/hep-ph?searchtype=author&query=Britzger%2C+D">D. Britzger</a>, <a href="/search/hep-ph?searchtype=author&query=Buniatyan%2C+A">A. Buniatyan</a>, <a href="/search/hep-ph?searchtype=author&query=Bystritskaya%2C+L">L. Bystritskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Campbell%2C+A+J">A. J. Campbell</a>, <a href="/search/hep-ph?searchtype=author&query=Avila%2C+K+B+C">K. B. Cantun Avila</a>, <a href="/search/hep-ph?searchtype=author&query=Cerny%2C+K">K. Cerny</a>, <a href="/search/hep-ph?searchtype=author&query=Chekelian%2C+V">V. Chekelian</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Z. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Contreras%2C+J+G">J. G. Contreras</a>, <a href="/search/hep-ph?searchtype=author&query=Cvach%2C+J">J. Cvach</a>, <a href="/search/hep-ph?searchtype=author&query=Dainton%2C+J+B">J. B. Dainton</a>, <a href="/search/hep-ph?searchtype=author&query=Daum%2C+K">K. Daum</a>, <a href="/search/hep-ph?searchtype=author&query=Deshpande%2C+A">A. Deshpande</a>, <a href="/search/hep-ph?searchtype=author&query=Diaconu%2C+C">C. Diaconu</a>, <a href="/search/hep-ph?searchtype=author&query=Drees%2C+A">A. Drees</a>, <a href="/search/hep-ph?searchtype=author&query=Eckerlin%2C+G">G. Eckerlin</a> , et al. (124 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.10109v1-abstract-short" style="display: inline;"> The H1 Collaboration reports the first measurement of the 1-jettiness event shape observable $蟿_1^b$ in neutral-current deep-inelastic electron-proton scattering (DIS). The observable $蟿_1^b$ is equivalent to a thrust observable defined in the Breit frame. The data sample was collected at the HERA $ep$ collider in the years 2003-2007 with center-of-mass energy of $\sqrt{s}=319\,\text{GeV}$, corres… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10109v1-abstract-full').style.display = 'inline'; document.getElementById('2403.10109v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.10109v1-abstract-full" style="display: none;"> The H1 Collaboration reports the first measurement of the 1-jettiness event shape observable $蟿_1^b$ in neutral-current deep-inelastic electron-proton scattering (DIS). The observable $蟿_1^b$ is equivalent to a thrust observable defined in the Breit frame. The data sample was collected at the HERA $ep$ collider in the years 2003-2007 with center-of-mass energy of $\sqrt{s}=319\,\text{GeV}$, corresponding to an integrated luminosity of $351.1\,\text{pb}^{-1}$. Triple differential cross sections are provided as a function of $蟿_1^b$, event virtuality $Q^2$, and inelasticity $y$, in the kinematic region $Q^2>150\,\text{GeV}^{2}$. Single differential cross section are provided as a function of $蟿_1^b$ in a limited kinematic range. Double differential cross sections are measured, in contrast, integrated over $蟿_1^b$ and represent the inclusive neutral-current DIS cross section measured as a function of $Q^2$ and $y$. The data are compared to a variety of predictions and include classical and modern Monte Carlo event generators, predictions in fixed-order perturbative QCD where calculations up to $\mathcal{O}(伪_s^3)$ are available for $蟿_1^b$ or inclusive DIS, and resummed predictions at next-to-leading logarithmic accuracy matched to fixed order predictions at $\mathcal{O}(伪_s^2)$. These comparisons reveal sensitivity of the 1-jettiness observable to QCD parton shower and resummation effects, as well as the modeling of hadronization and fragmentation. Within their range of validity, the fixed-order predictions provide a good description of the data. Monte Carlo event generators are predictive over the full measured range and hence their underlying models and parameters can be constrained by comparing to the presented data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.10109v1-abstract-full').style.display = 'none'; document.getElementById('2403.10109v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45 pages, 38 tables, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DESY-24-035 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.08982">arXiv:2403.08982</a> <span> [<a href="https://arxiv.org/pdf/2403.08982">pdf</a>, <a href="https://arxiv.org/format/2403.08982">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1140/epjc/s10052-024-13003-1">10.1140/epjc/s10052-024-13003-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation and differential cross section measurement of neutral current DIS events with an empty hemisphere in the Breit frame </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=The+H1+collaboration"> The H1 collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Andreev%2C+V">V. Andreev</a>, <a href="/search/hep-ph?searchtype=author&query=Arratia%2C+M">M. Arratia</a>, <a href="/search/hep-ph?searchtype=author&query=Baghdasaryan%2C+A">A. Baghdasaryan</a>, <a href="/search/hep-ph?searchtype=author&query=Baty%2C+A">A. Baty</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Bolz%2C+A">A. Bolz</a>, <a href="/search/hep-ph?searchtype=author&query=Boudry%2C+V">V. Boudry</a>, <a href="/search/hep-ph?searchtype=author&query=Brandt%2C+G">G. Brandt</a>, <a href="/search/hep-ph?searchtype=author&query=Britzger%2C+D">D. Britzger</a>, <a href="/search/hep-ph?searchtype=author&query=Buniatyan%2C+A">A. Buniatyan</a>, <a href="/search/hep-ph?searchtype=author&query=Bystritskaya%2C+L">L. Bystritskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Campbell%2C+A+J">A. J. Campbell</a>, <a href="/search/hep-ph?searchtype=author&query=Avila%2C+K+B+C">K. B. Cantun Avila</a>, <a href="/search/hep-ph?searchtype=author&query=Cerny%2C+K">K. Cerny</a>, <a href="/search/hep-ph?searchtype=author&query=Chekelian%2C+V">V. Chekelian</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Z. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Contreras%2C+J+G">J. G. Contreras</a>, <a href="/search/hep-ph?searchtype=author&query=Cvach%2C+J">J. Cvach</a>, <a href="/search/hep-ph?searchtype=author&query=Dainton%2C+J+B">J. B. Dainton</a>, <a href="/search/hep-ph?searchtype=author&query=Daum%2C+K">K. Daum</a>, <a href="/search/hep-ph?searchtype=author&query=Deshpande%2C+A">A. Deshpande</a>, <a href="/search/hep-ph?searchtype=author&query=Diaconu%2C+C">C. Diaconu</a>, <a href="/search/hep-ph?searchtype=author&query=Drees%2C+A">A. Drees</a>, <a href="/search/hep-ph?searchtype=author&query=Eckerlin%2C+G">G. Eckerlin</a> , et al. (124 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.08982v2-abstract-short" style="display: inline;"> The Breit frame provides a natural frame to analyze lepton-proton scattering events. In this reference frame, the parton model hard interactions between a quark and an exchanged boson defines the coordinate system such that the struck quark is back-scattered along the virtual photon momentum direction. In Quantum Chromodynamics (QCD), higher order perturbative or non-perturbative effects can chang… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.08982v2-abstract-full').style.display = 'inline'; document.getElementById('2403.08982v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.08982v2-abstract-full" style="display: none;"> The Breit frame provides a natural frame to analyze lepton-proton scattering events. In this reference frame, the parton model hard interactions between a quark and an exchanged boson defines the coordinate system such that the struck quark is back-scattered along the virtual photon momentum direction. In Quantum Chromodynamics (QCD), higher order perturbative or non-perturbative effects can change this picture drastically. As Bjorken-$x$ decreases below one half, a rather peculiar event signature is predicted with increasing probability, where no radiation is present in one of the two Breit-frame hemispheres and all emissions are to be found in the other hemisphere. At higher orders in $伪_s$ or in the presence of soft QCD effects, predictions of the rate of these events are far from trivial, and that motivates measurements with real data. We report on the first observation of the empty current hemisphere events in electron-proton collisions at the HERA collider using data recorded with the H1 detector at a center-of-mass energy of 319 GeV. The fraction of inclusive neutral-current DIS events with an empty hemisphere is found to be $0.0112 \pm 3.9\,\%_\text{stat} \pm 4.5\,\%_\text{syst} \pm 1.6\,\%_\text{mod}$ in the selected kinematic region of $150< Q^2<1500$ GeV$^2$ and inelasticity $0.14< y<0.7$. The data sample corresponds to an integrated luminosity of 351.1 pb$^{-1}$, sufficient to enable differential cross section measurements of these events. The results show an enhanced discriminating power at lower Bjorken-$x$ among different Monte Carlo event generator predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.08982v2-abstract-full').style.display = 'none'; document.getElementById('2403.08982v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 5 figures, 2 Tables. This version as accepted for publication</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DESY-24-034 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> EPJC 84 (2024), 720 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.05397">arXiv:2402.05397</a> <span> [<a href="https://arxiv.org/pdf/2402.05397">pdf</a>, <a href="https://arxiv.org/format/2402.05397">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> NLO QCD corrections to the $B_c$-pair hadroproduction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zi-Qiang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+L">Long-Bin Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Qiao%2C+C">Cong-Feng Qiao</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.05397v1-abstract-short" style="display: inline;"> The $B_c$ meson pair, including pairs of pseudoscalar states and vector states, productions in proton-proton collisions are investigated at the next-to-leading order (NLO) accuracy in the nonrelativistic quantum chromodynamics factorization formalism. The corresponding cross sections at the Large Hadron Collider (LHC) with $\sqrt{s}=14\; \text{TeV}$ are evaluated. Numerical results indicate that t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.05397v1-abstract-full').style.display = 'inline'; document.getElementById('2402.05397v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.05397v1-abstract-full" style="display: none;"> The $B_c$ meson pair, including pairs of pseudoscalar states and vector states, productions in proton-proton collisions are investigated at the next-to-leading order (NLO) accuracy in the nonrelativistic quantum chromodynamics factorization formalism. The corresponding cross sections at the Large Hadron Collider (LHC) with $\sqrt{s}=14\; \text{TeV}$ are evaluated. Numerical results indicate that the NLO corrections are substantial, and even dominate over the leading order contributions. Considering the predicted cross sections are sizable, the $B_c$-pair production is expected to be observable at the High-Luminosity LHC experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.05397v1-abstract-full').style.display = 'none'; document.getElementById('2402.05397v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.03117">arXiv:2402.03117</a> <span> [<a href="https://arxiv.org/pdf/2402.03117">pdf</a>, <a href="https://arxiv.org/format/2402.03117">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Lattice">hep-lat</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.094011">10.1103/PhysRevD.109.094011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> P-wave fully charm and fully bottom tetraquark states </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhi-Zhong Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+X">Xu-Liang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Yang%2C+P">Peng-Fei Yang</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+W">Wei Chen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.03117v2-abstract-short" style="display: inline;"> We have studied the mass spectra of the P-wave fully charm and fully bottom tetraquark states in the framework of QCD sum rules. We construct the interpolating currents by inserting the covariant derivative operator $\overset{ \leftrightarrow } { \mathcal D }_{ 渭}$ between the S-wave diquark and antidiquark fields. The excitation structures show that the pure $位$-mode excited P-wave fully heavy te… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.03117v2-abstract-full').style.display = 'inline'; document.getElementById('2402.03117v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.03117v2-abstract-full" style="display: none;"> We have studied the mass spectra of the P-wave fully charm and fully bottom tetraquark states in the framework of QCD sum rules. We construct the interpolating currents by inserting the covariant derivative operator $\overset{ \leftrightarrow } { \mathcal D }_{ 渭}$ between the S-wave diquark and antidiquark fields. The excitation structures show that the pure $位$-mode excited P-wave fully heavy tetraquarks exist for the quantum numbers $J^{PC}=1^{--}, 1^{-+}, 2^{--}, 2^{-+}$ and $3^{--}$, while it is difficult to separate the $位$-mode and $蟻$-mode excitations in the $0^{-+}$ channel. Within three Lorentz indices, there is no pure $位$-mode excited P-wave fully charm/bottom tetraquark operators with $J^{PC}=0^{--}$ and $3^{-+}$. Our results support that the recent observed $X(6900)$ and $X(7200)$ resonances could be interpreted as the P-wave fully charm $cc \bar c \bar c$ tetraquark states with $J^{PC}=1^{-+}$ and $2^{-+}$, respectively. Some P-wave fully bottom $bb\bar b\bar b$ tetraquark states are predicted to be lower than the di-$畏_b(1S)$ and di-$违(1S)$ mass thresholds. Hopefully our calculations will be useful for identifying the nature of new exotic tetraquark states. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.03117v2-abstract-full').style.display = 'none'; document.getElementById('2402.03117v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 11 figures. Accepted by Physical Review D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109, 094011 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.02901">arXiv:2401.02901</a> <span> [<a href="https://arxiv.org/pdf/2401.02901">pdf</a>, <a href="https://arxiv.org/format/2401.02901">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Charged-current non-standard neutrino interactions at Daya Bay </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Daya+Bay+collaboration"> Daya Bay collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+F+P">F. P. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+W+D">W. D. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Balantekin%2C+A+B">A. B. Balantekin</a>, <a href="/search/hep-ph?searchtype=author&query=Bishai%2C+M">M. Bishai</a>, <a href="/search/hep-ph?searchtype=author&query=Blyth%2C+S">S. Blyth</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+G+F">G. F. Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+J">J. Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+Y">Y. Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+H+S">H. S. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+H+Y">H. Y. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+S+M">S. M. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Y">Y. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Y+X">Y. X. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z+Y">Z. Y. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Cheng%2C+J">J. Cheng</a>, <a href="/search/hep-ph?searchtype=author&query=Cheng%2C+Y+C">Y. C. Cheng</a>, <a href="/search/hep-ph?searchtype=author&query=Cheng%2C+Z+K">Z. K. Cheng</a>, <a href="/search/hep-ph?searchtype=author&query=Cherwinka%2C+J+J">J. J. Cherwinka</a>, <a href="/search/hep-ph?searchtype=author&query=Chu%2C+M+C">M. C. Chu</a>, <a href="/search/hep-ph?searchtype=author&query=Cummings%2C+J+P">J. P. Cummings</a>, <a href="/search/hep-ph?searchtype=author&query=Dalager%2C+O">O. Dalager</a>, <a href="/search/hep-ph?searchtype=author&query=Deng%2C+F+S">F. S. Deng</a>, <a href="/search/hep-ph?searchtype=author&query=Ding%2C+X+Y">X. Y. Ding</a> , et al. (177 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.02901v6-abstract-short" style="display: inline;"> The full data set of the Daya Bay reactor neutrino experiment is used to probe the effect of the charged current non-standard interactions (CC-NSI) on neutrino oscillation experiments. Two different approaches are applied and constraints on the corresponding CC-NSI parameters are obtained with the neutrino flux taken from the Huber-Mueller model with a $5\%$ uncertainty. For the quantum mechanics-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02901v6-abstract-full').style.display = 'inline'; document.getElementById('2401.02901v6-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.02901v6-abstract-full" style="display: none;"> The full data set of the Daya Bay reactor neutrino experiment is used to probe the effect of the charged current non-standard interactions (CC-NSI) on neutrino oscillation experiments. Two different approaches are applied and constraints on the corresponding CC-NSI parameters are obtained with the neutrino flux taken from the Huber-Mueller model with a $5\%$ uncertainty. For the quantum mechanics-based approach (QM-NSI), the constraints on the CC-NSI parameters $蔚_{e伪}$ and $蔚_{e伪}^{s}$ are extracted with and without the assumption that the effects of the new physics are the same in the production and detection processes, respectively. The approach based on the weak effective field theory (WEFT-NSI) deals with four types of CC-NSI represented by the parameters $[\varepsilon_{X}]_{e伪}$. For both approaches, the results for the CC-NSI parameters are shown for cases with various fixed values of the CC-NSI and the Dirac CP-violating phases, and when they are allowed to vary freely. We find that constraints on the QM-NSI parameters $蔚_{e伪}$ and $蔚_{e伪}^{s}$ from the Daya Bay experiment alone can reach the order $\mathcal{O}(0.01)$ for the former and $\mathcal{O}(0.1)$ for the latter, while for WEFT-NSI parameters $[\varepsilon_{X}]_{e伪}$, we obtain $\mathcal{O}(0.1)$ for both cases. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02901v6-abstract-full').style.display = 'none'; document.getElementById('2401.02901v6-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 16 figures, 6 tables; 36 pages, format changed, references added</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.12114">arXiv:2312.12114</a> <span> [<a href="https://arxiv.org/pdf/2312.12114">pdf</a>, <a href="https://arxiv.org/format/2312.12114">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Neutron-antineutron oscillation accompanied by CP-violation in magnetic fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Hao%2C+Y">Yongliang Hao</a>, <a href="/search/hep-ph?searchtype=author&query=Nyirenda%2C+K+S">Kamphamba Sokalao Nyirenda</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhenwei Chen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.12114v5-abstract-short" style="display: inline;"> In this work, we explore the possibility of the $n$-$\bar{n}$ oscillation accompanied by CP-violation in the presence of magnetic fields. The $n$-$\bar{n}$ oscillation, which violates the baryon number ($\mathcal{B}$) by two units ($|螖\mathcal{B}| = 2$), can be originated from the mixing between the neutron ($n$) and the neutral elementary particle ($畏$) and may give rise to non-trivial effects th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12114v5-abstract-full').style.display = 'inline'; document.getElementById('2312.12114v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.12114v5-abstract-full" style="display: none;"> In this work, we explore the possibility of the $n$-$\bar{n}$ oscillation accompanied by CP-violation in the presence of magnetic fields. The $n$-$\bar{n}$ oscillation, which violates the baryon number ($\mathcal{B}$) by two units ($|螖\mathcal{B}| = 2$), can be originated from the mixing between the neutron ($n$) and the neutral elementary particle ($畏$) and may give rise to non-trivial effects that are different from previous theoretical predictions. We show that the probability of the $n$-$\bar{n}$ oscillation can be greatly enhanced by adjusting the magnetic field properly. In particular, the peak values of the oscillation probability in the presence of resonance magnetic fields can be $8$-$10$ orders of magnitude higher than that in the absence of magnetic fields. We point out that there might not be sizable CP-violating effects in the $n$-$\bar{n}$ oscillation unless the mass of $畏$ is close to the mass of the neutron. We also analyze the interplay between various parameters associated with both $\mathcal{B}$-violation and CP-violation and attempt to disentangle the effects of such parameters. The $n$-$\bar{n}$ oscillation process accompanied by CP-violation may open a promising avenue for exploring new physics beyond the Standard Model (SM). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.12114v5-abstract-full').style.display = 'none'; document.getElementById('2312.12114v5-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 (sub-)figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.11165">arXiv:2312.11165</a> <span> [<a href="https://arxiv.org/pdf/2312.11165">pdf</a>, <a href="https://arxiv.org/format/2312.11165">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Testing Leptogenesis and Seesaw using Long-lived Particle Searches in the $B-L$ Model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Liu%2C+W">Wei Liu</a>, <a href="/search/hep-ph?searchtype=author&query=Deppisch%2C+F+F">Frank F. Deppisch</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zixiang Chen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.11165v2-abstract-short" style="display: inline;"> We discuss the potential of using long-lived particle (LLP) searches for right-handed neutrinos (RHNs) to test resonant leptogenesis and the seesaw mechanism. This is challenging if only RHNs are added to the Standard Model (SM), as naturally the active-sterile mixing strengths $|V_{\ell N}|^2$ are small, for 1 GeV $\lesssim M_N \lesssim 1000$ GeV. Instead, we consider the minimal $B-L$ gauge mode… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11165v2-abstract-full').style.display = 'inline'; document.getElementById('2312.11165v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.11165v2-abstract-full" style="display: none;"> We discuss the potential of using long-lived particle (LLP) searches for right-handed neutrinos (RHNs) to test resonant leptogenesis and the seesaw mechanism. This is challenging if only RHNs are added to the Standard Model (SM), as naturally the active-sterile mixing strengths $|V_{\ell N}|^2$ are small, for 1 GeV $\lesssim M_N \lesssim 1000$ GeV. Instead, we consider the minimal $B-L$ gauge model, where a $Z^\prime$ gauge boson couples to fermions including the RHNs. During leptogenesis, this gauge coupling introduces scattering processes that washout the $B-L$ asymmetry. At colliders, it can lead to abundant production of RHNs which allows probing the associated seesaw mechanism using LLP searches. We find that LLP searches at the FCC-hh can test leptogenesis and the seesaw mechanism simultaneously, and probe the active-sterile mixing at or below the seesaw floor. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11165v2-abstract-full').style.display = 'none'; document.getElementById('2312.11165v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 10 figures, plus appendix and references, to be published in PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.10254">arXiv:2312.10254</a> <span> [<a href="https://arxiv.org/pdf/2312.10254">pdf</a>, <a href="https://arxiv.org/ps/2312.10254">ps</a>, <a href="https://arxiv.org/format/2312.10254">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Why are hydrodynamic theories applicable beyond the hydrodynamic regime? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Jaiswal%2C+S">Sunil Jaiswal</a>, <a href="/search/hep-ph?searchtype=author&query=Blaizot%2C+J">Jean-Paul Blaizot</a>, <a href="/search/hep-ph?searchtype=author&query=Bhalerao%2C+R+S">Rajeev S. Bhalerao</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zenan Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Jaiswal%2C+A">Amaresh Jaiswal</a>, <a href="/search/hep-ph?searchtype=author&query=Yan%2C+L">Li Yan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.10254v1-abstract-short" style="display: inline;"> We present an alternative approach to deriving second-order non-conformal hydrodynamics from the relativistic Boltzmann equation. We demonstrate how constitutive relations for shear and bulk stresses can be transformed into dynamical evolution equations, resulting in Israel-Stewart-like (ISL) hydrodynamics. To understand the far-from-equilibrium applicability of such ISL theories, we investigate t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10254v1-abstract-full').style.display = 'inline'; document.getElementById('2312.10254v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.10254v1-abstract-full" style="display: none;"> We present an alternative approach to deriving second-order non-conformal hydrodynamics from the relativistic Boltzmann equation. We demonstrate how constitutive relations for shear and bulk stresses can be transformed into dynamical evolution equations, resulting in Israel-Stewart-like (ISL) hydrodynamics. To understand the far-from-equilibrium applicability of such ISL theories, we investigate the one-dimensional boost-invariant Boltzmann equation using special moments of the distribution function for a system with finite particle mass. Our analysis reveals that the mathematical structure of the ISL equations is akin to that of moment equations, enabling them to approximately replicate even the collisionless dynamics. We conclude that this particular feature is important in extending the applicability of ISL theories beyond the hydrodynamic regime. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10254v1-abstract-full').style.display = 'none'; document.getElementById('2312.10254v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to Quark Matter 2023 (4 pages)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.06152">arXiv:2312.06152</a> <span> [<a href="https://arxiv.org/pdf/2312.06152">pdf</a>, <a href="https://arxiv.org/format/2312.06152">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Improving the performance of weak supervision searches using transfer and meta-learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Beauchesne%2C+H">Hugues Beauchesne</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zong-En Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chiang%2C+C">Cheng-Wei Chiang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.06152v2-abstract-short" style="display: inline;"> Weak supervision searches have in principle the advantages of both being able to train on experimental data and being able to learn distinctive signal properties. However, the practical applicability of such searches is limited by the fact that successfully training a neural network via weak supervision can require a large amount of signal. In this work, we seek to create neural networks that can… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06152v2-abstract-full').style.display = 'inline'; document.getElementById('2312.06152v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.06152v2-abstract-full" style="display: none;"> Weak supervision searches have in principle the advantages of both being able to train on experimental data and being able to learn distinctive signal properties. However, the practical applicability of such searches is limited by the fact that successfully training a neural network via weak supervision can require a large amount of signal. In this work, we seek to create neural networks that can learn from less experimental signal by using transfer and meta-learning. The general idea is to first train a neural network on simulations, thereby learning concepts that can be reused or becoming a more efficient learner. The neural network would then be trained on experimental data and should require less signal because of its previous training. We find that transfer and meta-learning can substantially improve the performance of weak supervision searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06152v2-abstract-full').style.display = 'none'; document.getElementById('2312.06152v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 7 figures, matches the published version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.01824">arXiv:2312.01824</a> <span> [<a href="https://arxiv.org/pdf/2312.01824">pdf</a>, <a href="https://arxiv.org/format/2312.01824">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> NANOGrav hints for first-order confinement-deconfinement phase transition in different QCD-matter scenarios </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Li%2C+S">Shou-Long Li</a>, <a href="/search/hep-ph?searchtype=author&query=Wu%2C+P">Puxun Wu</a>, <a href="/search/hep-ph?searchtype=author&query=Yu%2C+H">Hongwei Yu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.01824v2-abstract-short" style="display: inline;"> Recent observations from several pulsar timing array (PTA) collaborations have unveiled compelling evidence for a stochastic signal in the nanohertz band. This signal aligns remarkably with a gravitational wave (GW) background, potentially originating from the first-order color charge confinement phase transition. Distinct quantum chromodynamics (QCD) matters, such as quarks or gluons, and diverse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01824v2-abstract-full').style.display = 'inline'; document.getElementById('2312.01824v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.01824v2-abstract-full" style="display: none;"> Recent observations from several pulsar timing array (PTA) collaborations have unveiled compelling evidence for a stochastic signal in the nanohertz band. This signal aligns remarkably with a gravitational wave (GW) background, potentially originating from the first-order color charge confinement phase transition. Distinct quantum chromodynamics (QCD) matters, such as quarks or gluons, and diverse phase transition processes thereof can yield disparate GW energy density spectra. In this paper, employing the Bayesian analysis on the NANOGrav 15-year data set, we explore the compatibility with the observed PTA signal of the GW from phase transitions of various QCD matter scenarios in the framework of the holographic QCD. We find that the PTA signal can be effectively explained by the GW from the confinement-deconfinement phase transition of pure quark systems in a hard wall model of the holographic QCD where the bubble dynamics, one important source of the GWs, is of the Jouguet detonations. Notably, our analysis decisively rules out the plausibility of the pure gluon QCD-matter scenario and the non-runaway bubble dynamics model for the phase transition in explaining the observed PTA signal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.01824v2-abstract-full').style.display = 'none'; document.getElementById('2312.01824v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 2 figures; accepted by PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.00934">arXiv:2311.00934</a> <span> [<a href="https://arxiv.org/pdf/2311.00934">pdf</a>, <a href="https://arxiv.org/format/2311.00934">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2024.138966">10.1016/j.physletb.2024.138966 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurements of charged-particle multiplicity dependence of higher-order net-proton cumulants in $p$+$p$ collisions at $\sqrt{s} =$ 200 GeV from STAR at RHIC </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=STAR+Collaboration"> STAR Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Abdulhamid%2C+M+I">M. I. Abdulhamid</a>, <a href="/search/hep-ph?searchtype=author&query=Aboona%2C+B+E">B. E. Aboona</a>, <a href="/search/hep-ph?searchtype=author&query=Adam%2C+J">J. Adam</a>, <a href="/search/hep-ph?searchtype=author&query=Adamczyk%2C+L">L. Adamczyk</a>, <a href="/search/hep-ph?searchtype=author&query=Adams%2C+J+R">J. R. Adams</a>, <a href="/search/hep-ph?searchtype=author&query=Aggarwal%2C+I">I. Aggarwal</a>, <a href="/search/hep-ph?searchtype=author&query=Aggarwal%2C+M+M">M. M. Aggarwal</a>, <a href="/search/hep-ph?searchtype=author&query=Ahammed%2C+Z">Z. Ahammed</a>, <a href="/search/hep-ph?searchtype=author&query=Aschenauer%2C+E+C">E. C. Aschenauer</a>, <a href="/search/hep-ph?searchtype=author&query=Aslam%2C+S">S. Aslam</a>, <a href="/search/hep-ph?searchtype=author&query=Atchison%2C+J">J. Atchison</a>, <a href="/search/hep-ph?searchtype=author&query=Bairathi%2C+V">V. Bairathi</a>, <a href="/search/hep-ph?searchtype=author&query=Cap%2C+J+G+B">J. G. Ball Cap</a>, <a href="/search/hep-ph?searchtype=author&query=Barish%2C+K">K. Barish</a>, <a href="/search/hep-ph?searchtype=author&query=Bellwied%2C+R">R. Bellwied</a>, <a href="/search/hep-ph?searchtype=author&query=Bhagat%2C+P">P. Bhagat</a>, <a href="/search/hep-ph?searchtype=author&query=Bhasin%2C+A">A. Bhasin</a>, <a href="/search/hep-ph?searchtype=author&query=Bhatta%2C+S">S. Bhatta</a>, <a href="/search/hep-ph?searchtype=author&query=Bhosale%2C+S+R">S. R. Bhosale</a>, <a href="/search/hep-ph?searchtype=author&query=Bielcik%2C+J">J. Bielcik</a>, <a href="/search/hep-ph?searchtype=author&query=Bielcikova%2C+J">J. Bielcikova</a>, <a href="/search/hep-ph?searchtype=author&query=Brandenburg%2C+J+D">J. D. Brandenburg</a>, <a href="/search/hep-ph?searchtype=author&query=Broodo%2C+C">C. Broodo</a>, <a href="/search/hep-ph?searchtype=author&query=Cai%2C+X+Z">X. Z. Cai</a> , et al. (338 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.00934v2-abstract-short" style="display: inline;"> We report on the charged-particle multiplicity dependence of net-proton cumulant ratios up to sixth order from $\sqrt{s}=200$ GeV $p$+$p$ collisions at the Relativistic Heavy Ion Collider (RHIC). The measured ratios $C_{4}/C_{2}$, $C_{5}/C_{1}$, and $C_{6}/C_{2}$ decrease with increased charged-particle multiplicity and rapidity acceptance. Neither the Skellam baselines nor PYTHIA8 calculations ac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00934v2-abstract-full').style.display = 'inline'; document.getElementById('2311.00934v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.00934v2-abstract-full" style="display: none;"> We report on the charged-particle multiplicity dependence of net-proton cumulant ratios up to sixth order from $\sqrt{s}=200$ GeV $p$+$p$ collisions at the Relativistic Heavy Ion Collider (RHIC). The measured ratios $C_{4}/C_{2}$, $C_{5}/C_{1}$, and $C_{6}/C_{2}$ decrease with increased charged-particle multiplicity and rapidity acceptance. Neither the Skellam baselines nor PYTHIA8 calculations account for the observed multiplicity dependence. In addition, the ratios $C_{5}/C_{1}$ and $C_{6}/C_{2}$ approach negative values in the highest-multiplicity events, which implies that thermalized QCD matter may be formed in $p$+$p$ collisions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00934v2-abstract-full').style.display = 'none'; document.getElementById('2311.00934v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 6 figures, accepted version by PLB</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.11238">arXiv:2310.11238</a> <span> [<a href="https://arxiv.org/pdf/2310.11238">pdf</a>, <a href="https://arxiv.org/format/2310.11238">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.109.084045">10.1103/PhysRevD.109.084045 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Non-Tensorial Gravitational-Wave Backgrounds in the NANOGrav 15-Year Data Set </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Wu%2C+Y">Yu-Mei Wu</a>, <a href="/search/hep-ph?searchtype=author&query=Bi%2C+Y">Yan-Chen Bi</a>, <a href="/search/hep-ph?searchtype=author&query=Huang%2C+Q">Qing-Guo Huang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.11238v3-abstract-short" style="display: inline;"> The recent detection of a stochastic signal in the NANOGrav 15-year data set has aroused great interest in uncovering its origin. However, the evidence for the Hellings-Downs correlations, a key signature of the gravitational-wave background (GWB) predicted by general relativity, remains inconclusive. In this letter, we search for an isotropic non-tensorial GWB, allowed by general metric theories… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11238v3-abstract-full').style.display = 'inline'; document.getElementById('2310.11238v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.11238v3-abstract-full" style="display: none;"> The recent detection of a stochastic signal in the NANOGrav 15-year data set has aroused great interest in uncovering its origin. However, the evidence for the Hellings-Downs correlations, a key signature of the gravitational-wave background (GWB) predicted by general relativity, remains inconclusive. In this letter, we search for an isotropic non-tensorial GWB, allowed by general metric theories of gravity, in the NANOGrav 15-year data set. Our analysis reveals a Bayes factor of approximately 2.5, comparing the quadrupolar (tensor transverse, TT) correlations to the scalar transverse (ST) correlations, suggesting that the ST correlations provide a comparable explanation for the observed stochastic signal in the NANOGrav data. We obtain the median and the $90\%$ equal-tail amplitudes as $\mathcal{A}_\mathrm{ST} = 7.8^{+5.1}_{-3.5} \times 10^{-15}$ at the frequency of 1/year. Furthermore, we find that the vector longitudinal (VL) and scalar longitudinal (SL) correlations are weakly and strongly disfavoured by data, respectively, yielding upper limits on the amplitudes: $\mathcal{A}_\mathrm{VL}^{95\%} \lesssim 1.7 \times 10^{-15}$ and $\mathcal{A}_\mathrm{SL}^{95\%} \lesssim 7.4 \times 10^{-17}$. Lastly, we fit the NANOGrav data with the general transverse (GT) correlations parameterized by a free parameter $伪$. Our analysis yields $伪=1.74^{+1.18}_{-1.41}$, thus excluding both the TT ($伪=3$) and ST ($伪=0$) models at the $90\%$ confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.11238v3-abstract-full').style.display = 'none'; document.getElementById('2310.11238v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 4 figures, 3 tables; match the published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D 109 (2024) 8, 084045 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.09487">arXiv:2309.09487</a> <span> [<a href="https://arxiv.org/pdf/2309.09487">pdf</a>, <a href="https://arxiv.org/format/2309.09487">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> Correlations of dihadron polarization in central, peripheral and ultraperipheral heavy-ion collisions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Li%2C+X">Xiaowen Li</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhao-Xuan Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+S">Shanshan Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Wei%2C+S">Shu-Yi Wei</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.09487v2-abstract-short" style="display: inline;"> While jet quenching in relativistic heavy-ion collisions has been extensively studied over decades, the polarization of quenched hadrons has rarely been discussed. It has recently been proposed that the correlations of dihadron polarization in $e^+e^-$ and $pp$ collisions provide a novel probe of the longitudinal spin transfer from hard partons to hadrons without requiring the colliding beams to b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.09487v2-abstract-full').style.display = 'inline'; document.getElementById('2309.09487v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.09487v2-abstract-full" style="display: none;"> While jet quenching in relativistic heavy-ion collisions has been extensively studied over decades, the polarization of quenched hadrons has rarely been discussed. It has recently been proposed that the correlations of dihadron polarization in $e^+e^-$ and $pp$ collisions provide a novel probe of the longitudinal spin transfer from hard partons to hadrons without requiring the colliding beams to be polarized. To support realistic experimental measurement of dihadron polarization with sufficient luminosity, we extend the aforementioned study to relativistic heavy-ion collisions by convoluting the vacuum fragmentation of partons with their energy loss inside the quark-gluon plasma (QGP). We find that while the correlation functions of $螞$-$螞$ (or $螞$-$\bar螞$) polarization in peripheral collisions is consistent with those in $pp$ collisions, clear enhancement can be seen in central collisions. These correlation functions appear sensitive to different assumptions in the DSV parameterization of parton fragmentation functions, and therefore could place additional constraints on the spin-dependent fragmentation functions of quarks and gluons. The correlation of dihadron polarization has also been explored in ultraperipheral heavy-ion collisions, which provides a cleaner probe of fragmentation functions of quarks produced by energetic photon-photon and photon-pomeron interactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.09487v2-abstract-full').style.display = 'none'; document.getElementById('2309.09487v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Slightly revised. References added</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.07109">arXiv:2309.07109</a> <span> [<a href="https://arxiv.org/pdf/2309.07109">pdf</a>, <a href="https://arxiv.org/ps/2309.07109">ps</a>, <a href="https://arxiv.org/format/2309.07109">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Real-time Monitoring for the Next Core-Collapse Supernova in JUNO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ph?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ph?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ph?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ph?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ph?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ph?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ph?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ph?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ph?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/hep-ph?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ph?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ph?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ph?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ph?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ph?searchtype=author&query=Bellato%2C+M">Marco Bellato</a>, <a href="/search/hep-ph?searchtype=author&query=Beretta%2C+M">Marco Beretta</a>, <a href="/search/hep-ph?searchtype=author&query=Bergnoli%2C+A">Antonio Bergnoli</a> , et al. (606 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.07109v2-abstract-short" style="display: inline;"> The core-collapse supernova (CCSN) is considered one of the most energetic astrophysical events in the universe. The early and prompt detection of neutrinos before (pre-SN) and during the supernova (SN) burst presents a unique opportunity for multi-messenger observations of CCSN events. In this study, we describe the monitoring concept and present the sensitivity of the system to pre-SN and SN neu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07109v2-abstract-full').style.display = 'inline'; document.getElementById('2309.07109v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.07109v2-abstract-full" style="display: none;"> The core-collapse supernova (CCSN) is considered one of the most energetic astrophysical events in the universe. The early and prompt detection of neutrinos before (pre-SN) and during the supernova (SN) burst presents a unique opportunity for multi-messenger observations of CCSN events. In this study, we describe the monitoring concept and present the sensitivity of the system to pre-SN and SN neutrinos at the Jiangmen Underground Neutrino Observatory (JUNO), a 20 kton liquid scintillator detector currently under construction in South China. The real-time monitoring system is designed to ensure both prompt alert speed and comprehensive coverage of progenitor stars. It incorporates prompt monitors on the electronic board as well as online monitors at the data acquisition stage. Assuming a false alert rate of 1 per year, this monitoring system exhibits sensitivity to pre-SN neutrinos up to a distance of approximately 1.6 (0.9) kiloparsecs and SN neutrinos up to about 370 (360) kiloparsecs for a progenitor mass of 30 solar masses, considering both normal and inverted mass ordering scenarios. The pointing ability of the CCSN is evaluated by analyzing the accumulated event anisotropy of inverse beta decay interactions from pre-SN or SN neutrinos. This, along with the early alert, can play a crucial role in facilitating follow-up multi-messenger observations of the next galactic or nearby extragalactic CCSN. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07109v2-abstract-full').style.display = 'none'; document.getElementById('2309.07109v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 9 figures, accepted for the publication at JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.00105">arXiv:2308.00105</a> <span> [<a href="https://arxiv.org/pdf/2308.00105">pdf</a>, <a href="https://arxiv.org/format/2308.00105">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Theory">hep-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1038/s41567-024-02436-w">10.1038/s41567-024-02436-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searching for Decoherence from Quantum Gravity at the IceCube South Pole Neutrino Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/hep-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/hep-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/hep-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/hep-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/hep-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/hep-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/hep-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/hep-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/hep-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/hep-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/hep-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/hep-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/hep-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/hep-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/hep-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/hep-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/hep-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/hep-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/hep-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a>, <a href="/search/hep-ph?searchtype=author&query=Benning%2C+C">C. Benning</a> , et al. (380 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.00105v1-abstract-short" style="display: inline;"> Neutrino oscillations at the highest energies and longest baselines provide a natural quantum interferometer with which to study the structure of spacetime and test the fundamental principles of quantum mechanics. If the metric of spacetime has a quantum mechanical description, there is a generic expectation that its fluctuations at the Planck scale would introduce non-unitary effects that are inc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.00105v1-abstract-full').style.display = 'inline'; document.getElementById('2308.00105v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.00105v1-abstract-full" style="display: none;"> Neutrino oscillations at the highest energies and longest baselines provide a natural quantum interferometer with which to study the structure of spacetime and test the fundamental principles of quantum mechanics. If the metric of spacetime has a quantum mechanical description, there is a generic expectation that its fluctuations at the Planck scale would introduce non-unitary effects that are inconsistent with the standard unitary time evolution of quantum mechanics. Neutrinos interacting with such fluctuations would lose their quantum coherence, deviating from the expected oscillatory flavor composition at long distances and high energies. The IceCube South Pole Neutrino Observatory is a billion-ton neutrino telescope situated in the deep ice of the Antarctic glacier. Atmospheric neutrinos detected by IceCube in the energy range 0.5--10 TeV have been used to test for coherence loss in neutrino propagation. No evidence of anomalous neutrino decoherence was observed, leading to the strongest experimental limits on neutrino-quantum gravity interactions to date, significantly surpassing expectations from natural Planck-scale models. The resulting constraint on the effective decoherence strength parameter within an energy-independent decoherence model is $螕_0\leq 1.17\times10^{-15}$~eV, improving upon past limits by a factor of 30. For decoherence effects scaling as E$^2$, limits are advanced by more than six orders of magnitude beyond past measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.00105v1-abstract-full').style.display = 'none'; document.getElementById('2308.00105v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nature Phys. 20 (2024) 913-920 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.14911">arXiv:2307.14911</a> <span> [<a href="https://arxiv.org/pdf/2307.14911">pdf</a>, <a href="https://arxiv.org/format/2307.14911">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Probing the equation of state of the early Universe with pulsar timing arrays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Liu%2C+L">Lang Liu</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Huang%2C+Q">Qing-Guo Huang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.14911v2-abstract-short" style="display: inline;"> The recently released data by pulsar timing array (PTA) collaborations have amassed substantial evidence corroborating the existence of a stochastic signal consistent with a gravitational-wave background at frequencies around the nanohertz regime. We investigate the situation in which the PTA signal originates from scalar-induced gravitational waves~(SIGWs), which serves as a valuable tool to prob… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14911v2-abstract-full').style.display = 'inline'; document.getElementById('2307.14911v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.14911v2-abstract-full" style="display: none;"> The recently released data by pulsar timing array (PTA) collaborations have amassed substantial evidence corroborating the existence of a stochastic signal consistent with a gravitational-wave background at frequencies around the nanohertz regime. We investigate the situation in which the PTA signal originates from scalar-induced gravitational waves~(SIGWs), which serves as a valuable tool to probe the equation of state parameter $w$ during the Universe's early stages. The joint consideration of the PTA data from the NANOGrav 15-year data set, PPTA DR3, and EPTA DR2 yields that $w=0.60^{+0.32}_{-0.39}$ (median + $90\%$ credible interval), indicating a period of condensate domination at the production of SIGWs is allowed by the data. Moreover, the data also supports radiation domination ($w=1/3$) within the $90\%$ credible interval. We also impose an upper bound on the reheating temperature that $T_\mathrm{rh} \lesssim 0.2\,\mathrm{GeV}$ and the constraint on $w$ reveals valuable information on the inflationary potential and the dynamics at the end of inflation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14911v2-abstract-full').style.display = 'none'; document.getElementById('2307.14911v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 3 figures, 1 table; accepted by JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.14633">arXiv:2307.14633</a> <span> [<a href="https://arxiv.org/pdf/2307.14633">pdf</a>, <a href="https://arxiv.org/ps/2307.14633">ps</a>, <a href="https://arxiv.org/format/2307.14633">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Observation of the decay $J/蠄\to e^+ e^- 畏(1405)$ with $畏(1405) \to 蟺^0 f_0(980)$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Ai%2C+X+C">X. C. Ai</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+M+R">M. R. An</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a>, <a href="/search/hep-ph?searchtype=author&query=Brueggemann%2C+A">A. Brueggemann</a> , et al. (601 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.14633v1-abstract-short" style="display: inline;"> Using a data sample of $(10087\pm44)\times 10^6$ $J/蠄$ events collected by the BESIII detector in 2009, 2012, 2018 and 2019, the electromagnetic Dalitz process $J/蠄\to e^+ e^- 畏(1405)$ is observed via the decay $畏(1405) \to 蟺^0 f_0(980)$, $f_0(980) \to 蟺^+ 蟺^-$, with a significance of about $9.6蟽$. The branching fraction of this decay is measured to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14633v1-abstract-full').style.display = 'inline'; document.getElementById('2307.14633v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.14633v1-abstract-full" style="display: none;"> Using a data sample of $(10087\pm44)\times 10^6$ $J/蠄$ events collected by the BESIII detector in 2009, 2012, 2018 and 2019, the electromagnetic Dalitz process $J/蠄\to e^+ e^- 畏(1405)$ is observed via the decay $畏(1405) \to 蟺^0 f_0(980)$, $f_0(980) \to 蟺^+ 蟺^-$, with a significance of about $9.6蟽$. The branching fraction of this decay is measured to be ${\mathcal B}(J/蠄\to e^+ e^- 蟺^0 畏(1405) \to e^+ e^- 蟺^0 f_0(980) \to e^+ e^- 蟺^0 蟺^+ 蟺^-)=(2.02\pm0.24(\rm{stat.})\pm0.09(\rm{syst.}))\times 10^{-7}$. The branching-fraction ratio ${\mathcal B}(J/蠄\to e^+ e^- 畏(1405))$/${\mathcal B}(J/蠄\to 纬畏(1405))$ is determined to be $(1.35\pm0.19(\rm{stat.})\pm0.06(\rm{syst.}))\times10^{-2}$. Furthermore, an $e^+e^-$ invariant-mass dependent transition form factor of $J/蠄\to e^+ e^-畏(1405)$ is presented for the first time. The obtained result provides input for different theoretical models, and is valuable for the improved understanding the intrinsic structure of the $畏(1405)$ meson. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.14633v1-abstract-full').style.display = 'none'; document.getElementById('2307.14633v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.08687">arXiv:2307.08687</a> <span> [<a href="https://arxiv.org/pdf/2307.08687">pdf</a>, <a href="https://arxiv.org/format/2307.08687">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2023/09/016">10.1088/1475-7516/2023/09/016 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Confronting sound speed resonance with pulsar timing arrays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Jin%2C+J">Jia-Heng Jin</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Yi%2C+Z">Zhu Yi</a>, <a href="/search/hep-ph?searchtype=author&query=You%2C+Z">Zhi-Qiang You</a>, <a href="/search/hep-ph?searchtype=author&query=Liu%2C+L">Lang Liu</a>, <a href="/search/hep-ph?searchtype=author&query=Wu%2C+Y">You Wu</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.08687v2-abstract-short" style="display: inline;"> The stochastic signal detected by pulsar timing arrays (PTAs) has raised great interest in understanding its physical origin. Assuming the signal is a cosmological gravitational-wave background produced by overly large primordial curvature perturbations, we investigate the sound speed resonance effect with an oscillatory behavior using the combined PTA data from NANOGrav 15-yr data set, PPTA DR3,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08687v2-abstract-full').style.display = 'inline'; document.getElementById('2307.08687v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.08687v2-abstract-full" style="display: none;"> The stochastic signal detected by pulsar timing arrays (PTAs) has raised great interest in understanding its physical origin. Assuming the signal is a cosmological gravitational-wave background produced by overly large primordial curvature perturbations, we investigate the sound speed resonance effect with an oscillatory behavior using the combined PTA data from NANOGrav 15-yr data set, PPTA DR3, and EPTA DR2. We find that the stochastic signal can be explained by the induced gravitational waves sourced by the sound speed resonance mechanism, with the oscillation frequency $f_* \in [1.51, 4.90] \times 10^{-7}$Hz and the start time of oscillation $|蟿_0| \in [2.05, 106] \times 10^7$s <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.08687v2-abstract-full').style.display = 'none'; document.getElementById('2307.08687v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 3 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP09(2023)016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.03141">arXiv:2307.03141</a> <span> [<a href="https://arxiv.org/pdf/2307.03141">pdf</a>, <a href="https://arxiv.org/format/2307.03141">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Cosmological Interpretation for the Stochastic Signal in Pulsar Timing Arrays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Wu%2C+Y">Yu-Mei Wu</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Huang%2C+Q">Qing-Guo Huang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.03141v2-abstract-short" style="display: inline;"> The pulsar timing array (PTA) collaborations have recently reported compelling evidence for the presence of a stochastic signal consistent with a gravitational-wave background. In this letter, we combine the latest data sets from NANOGrav, PPTA and EPTA collaborations to explore the cosmological interpretations for the detected signal from first-order phase transitions, domain walls and cosmic str… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.03141v2-abstract-full').style.display = 'inline'; document.getElementById('2307.03141v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.03141v2-abstract-full" style="display: none;"> The pulsar timing array (PTA) collaborations have recently reported compelling evidence for the presence of a stochastic signal consistent with a gravitational-wave background. In this letter, we combine the latest data sets from NANOGrav, PPTA and EPTA collaborations to explore the cosmological interpretations for the detected signal from first-order phase transitions, domain walls and cosmic strings, separately. We find that the first-order phase transitions and cosmic strings can give comparable interpretations compared to supermassive black hole binaries (SMBHBs) characterized by a power-law spectrum, but the domain wall model is strongly disfavored with the Bayes factor compared to the SMBHB model being 0.009. Furthermore, the constraints on the parameter spaces indicate that: 1) a strong phase transition at temperatures below the electroweak scale is favored and the bubble collisions make the dominant contribution to the energy density spectrum; 2) the cosmic string tension is $G 渭\in [1.46, 15.3]\times 10^{-12}$ at $90\%$ confidence interval and a small reconnection probability $p<6.68\times 10^{-2}$ is preferred at $95\%$ confidence level, implying that the strings in (super)string theory are strongly favored over the classical field strings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.03141v2-abstract-full').style.display = 'none'; document.getElementById('2307.03141v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 5 figures, 2 tables; References updated</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.01102">arXiv:2307.01102</a> <span> [<a href="https://arxiv.org/pdf/2307.01102">pdf</a>, <a href="https://arxiv.org/format/2307.01102">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Implications for the non-Gaussianity of curvature perturbation from pulsar timing arrays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Liu%2C+L">Lang Liu</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Huang%2C+Q">Qing-Guo Huang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.01102v3-abstract-short" style="display: inline;"> The recently released data by pulsar timing array (PTA) collaborations present strong evidence for a stochastic signal consistent with a gravitational-wave background. Assuming this signal originates from scalar-induced gravitational waves, we jointly use the PTA data from the NANOGrav 15-yr data set, PPTA DR3, and EPTA DR2 to probe the small-scale non-Gaussianity. We put the first-ever constraint… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01102v3-abstract-full').style.display = 'inline'; document.getElementById('2307.01102v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.01102v3-abstract-full" style="display: none;"> The recently released data by pulsar timing array (PTA) collaborations present strong evidence for a stochastic signal consistent with a gravitational-wave background. Assuming this signal originates from scalar-induced gravitational waves, we jointly use the PTA data from the NANOGrav 15-yr data set, PPTA DR3, and EPTA DR2 to probe the small-scale non-Gaussianity. We put the first-ever constraint on the non-Gaussianity parameter, finding $|F_\mathrm{NL}|\lesssim 13.9$ for a lognormal power spectrum of the curvature perturbations. Furthermore, we obtain $-13.9 \lesssim F_\mathrm{NL}\lesssim -0.1$ to prevent excessive production of primordial black holes. Moreover, the multi-band observations with the space-borne gravitational-wave detectors, such as LISA/Taiji/TianQin, will provide a complementary investigation of primordial non-Gaussianity. Our findings pave the way to constrain inflation models with PTA data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01102v3-abstract-full').style.display = 'none'; document.getElementById('2307.01102v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 2 figures, 1 table; Refs added; Supplementary Material added; Accepted by PRD as a Letter</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.00722">arXiv:2307.00722</a> <span> [<a href="https://arxiv.org/pdf/2307.00722">pdf</a>, <a href="https://arxiv.org/format/2307.00722">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s11433-023-2252-4">10.1007/s11433-023-2252-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Implications for the Supermassive Black Hole Binaries from the NANOGrav 15-year Data Set </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Bi%2C+Y">Yan-Chen Bi</a>, <a href="/search/hep-ph?searchtype=author&query=Wu%2C+Y">Yu-Mei Wu</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Huang%2C+Q">Qing-Guo Huang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.00722v2-abstract-short" style="display: inline;"> NANOGrav, EPTA, PPTA, and CPTA have announced the evidence for a stochastic signal from their latest data sets. Supermassive black hole binaries (SMBHBs) are supposed to be the most promising gravitational-wave (GW) sources of pulsar timing arrays. Assuming an astro-informed formation model, we use the NANOGrav 15-year data set to constrain the gravitational wave background (GWB) from SMBHBs. Our… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.00722v2-abstract-full').style.display = 'inline'; document.getElementById('2307.00722v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.00722v2-abstract-full" style="display: none;"> NANOGrav, EPTA, PPTA, and CPTA have announced the evidence for a stochastic signal from their latest data sets. Supermassive black hole binaries (SMBHBs) are supposed to be the most promising gravitational-wave (GW) sources of pulsar timing arrays. Assuming an astro-informed formation model, we use the NANOGrav 15-year data set to constrain the gravitational wave background (GWB) from SMBHBs. Our results prefer a large turn-over eccentricity of the SMBHB orbit when GWs begin to dominate the SMBHBs evolution. Furthermore, the GWB spectrum is extrapolated to the space-borne GW detector frequency band by including inspiral-merge-cutoff phases of SMBHBs and should be detected by LISA, Taiji and TianQin in the near future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.00722v2-abstract-full').style.display = 'none'; document.getElementById('2307.00722v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 3 figures, 3 tables; version accepted for publication in SCPMA</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Sci. China-Phys. Mech. Astron. 66, 120402 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.09567">arXiv:2306.09567</a> <span> [<a href="https://arxiv.org/pdf/2306.09567">pdf</a>, <a href="https://arxiv.org/format/2306.09567">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2023/09/001">10.1088/1475-7516/2023/09/001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=JUNO+Collaboration"> JUNO Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Abusleme%2C+A">Angel Abusleme</a>, <a href="/search/hep-ph?searchtype=author&query=Adam%2C+T">Thomas Adam</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmad%2C+S">Shakeel Ahmad</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmed%2C+R">Rizwan Ahmed</a>, <a href="/search/hep-ph?searchtype=author&query=Aiello%2C+S">Sebastiano Aiello</a>, <a href="/search/hep-ph?searchtype=author&query=Akram%2C+M">Muhammad Akram</a>, <a href="/search/hep-ph?searchtype=author&query=Aleem%2C+A">Abid Aleem</a>, <a href="/search/hep-ph?searchtype=author&query=Alexandros%2C+T">Tsagkarakis Alexandros</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+F">Fengpeng An</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Qi An</a>, <a href="/search/hep-ph?searchtype=author&query=Andronico%2C+G">Giuseppe Andronico</a>, <a href="/search/hep-ph?searchtype=author&query=Anfimov%2C+N">Nikolay Anfimov</a>, <a href="/search/hep-ph?searchtype=author&query=Antonelli%2C+V">Vito Antonelli</a>, <a href="/search/hep-ph?searchtype=author&query=Antoshkina%2C+T">Tatiana Antoshkina</a>, <a href="/search/hep-ph?searchtype=author&query=Asavapibhop%2C+B">Burin Asavapibhop</a>, <a href="/search/hep-ph?searchtype=author&query=de+Andr%C3%A9%2C+J+P+A+M">Jo茫o Pedro Athayde Marcondes de Andr茅</a>, <a href="/search/hep-ph?searchtype=author&query=Auguste%2C+D">Didier Auguste</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+W">Weidong Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Balashov%2C+N">Nikita Balashov</a>, <a href="/search/hep-ph?searchtype=author&query=Baldini%2C+W">Wander Baldini</a>, <a href="/search/hep-ph?searchtype=author&query=Barresi%2C+A">Andrea Barresi</a>, <a href="/search/hep-ph?searchtype=author&query=Basilico%2C+D">Davide Basilico</a>, <a href="/search/hep-ph?searchtype=author&query=Baussan%2C+E">Eric Baussan</a>, <a href="/search/hep-ph?searchtype=author&query=Bellato%2C+M">Marco Bellato</a> , et al. (581 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.09567v3-abstract-short" style="display: inline;"> We discuss JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo via detecting inverse beta decay reactions of electron anti-neutrinos resulting from the annihilation. We study possible backgrounds to the signature, including the reactor neutrinos, diffuse supernova neutrino background, charged- and neutral-current interactions of atmospheric neutrinos, backgrounds from muon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09567v3-abstract-full').style.display = 'inline'; document.getElementById('2306.09567v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.09567v3-abstract-full" style="display: none;"> We discuss JUNO sensitivity to the annihilation of MeV dark matter in the galactic halo via detecting inverse beta decay reactions of electron anti-neutrinos resulting from the annihilation. We study possible backgrounds to the signature, including the reactor neutrinos, diffuse supernova neutrino background, charged- and neutral-current interactions of atmospheric neutrinos, backgrounds from muon-induced fast neutrons and cosmogenic isotopes. A fiducial volume cut, as well as the pulse shape discrimination and the muon veto are applied to suppress the above backgrounds. It is shown that JUNO sensitivity to the thermally averaged dark matter annihilation rate in 10 years of exposure would be significantly better than the present-day best limit set by Super-Kamiokande and would be comparable to that expected by Hyper-Kamiokande. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.09567v3-abstract-full').style.display = 'none'; document.getElementById('2306.09567v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 9 figures, matches the publised version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 09 (2023) 001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.17030">arXiv:2305.17030</a> <span> [<a href="https://arxiv.org/pdf/2305.17030">pdf</a>, <a href="https://arxiv.org/format/2305.17030">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/acfd29">10.3847/1538-4365/acfd29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The First LHAASO Catalog of Gamma-Ray Sources </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Cao%2C+Z">Zhen Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Axikegu"> Axikegu</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y+X">Y. X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bao%2C+Y+W">Y. W. Bao</a>, <a href="/search/hep-ph?searchtype=author&query=Bastieri%2C+D">D. Bastieri</a>, <a href="/search/hep-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/hep-ph?searchtype=author&query=Bi%2C+Y+J">Y. J. Bi</a>, <a href="/search/hep-ph?searchtype=author&query=Cai%2C+J+T">J. T. Cai</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+Q">Q. Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+W+Y">W. Y. Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Cao%2C+Z">Zhe Cao</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+J+F">J. F. Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+A+M">A. M. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+E+S">E. S. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+L">Liang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+L">Lin Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+L">Long Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+M+J">M. J. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+M+L">M. L. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Q+H">Q. H. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+S+H">S. H. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+S+Z">S. Z. Chen</a> , et al. (255 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.17030v2-abstract-short" style="display: inline;"> We present the first catalog of very-high energy and ultra-high energy gamma-ray sources detected by the Large High Altitude Air Shower Observatory (LHAASO). The catalog was compiled using 508 days of data collected by the Water Cherenkov Detector Array (WCDA) from March 2021 to September 2022 and 933 days of data recorded by the Kilometer Squared Array (KM2A) from January 2020 to September 2022.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.17030v2-abstract-full').style.display = 'inline'; document.getElementById('2305.17030v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.17030v2-abstract-full" style="display: none;"> We present the first catalog of very-high energy and ultra-high energy gamma-ray sources detected by the Large High Altitude Air Shower Observatory (LHAASO). The catalog was compiled using 508 days of data collected by the Water Cherenkov Detector Array (WCDA) from March 2021 to September 2022 and 933 days of data recorded by the Kilometer Squared Array (KM2A) from January 2020 to September 2022. This catalog represents the main result from the most sensitive large coverage gamma-ray survey of the sky above 1 TeV, covering declination from $-$20$^{\circ}$ to 80$^{\circ}$. In total, the catalog contains 90 sources with an extended size smaller than $2^\circ$ and a significance of detection at $> 5蟽$. Based on our source association criteria, 32 new TeV sources are proposed in this study. Among the 90 sources, 43 sources are detected with ultra-high energy ($E > 100$ TeV) emission at $> 4蟽$ significance level. We provide the position, extension, and spectral characteristics of all the sources in this catalog. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.17030v2-abstract-full').style.display = 'none'; document.getElementById('2305.17030v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">40 pages, 13 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Supplement Series, 271 (2024) 25 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.08091">arXiv:2305.08091</a> <span> [<a href="https://arxiv.org/pdf/2305.08091">pdf</a>, <a href="https://arxiv.org/format/2305.08091">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2023/09/021">10.1088/1475-7516/2023/09/021 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Pulsar timing residual induced by ultralight tensor dark matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Wu%2C+Y">Yu-Mei Wu</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zu-Cheng Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Huang%2C+Q">Qing-Guo Huang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.08091v2-abstract-short" style="display: inline;"> Ultralight boson fields, with a mass around $10^{-23}\text{eV}$, are promising candidates for the elusive cosmological dark matter. These fields induce a periodic oscillation of the spacetime metric in the nanohertz frequency band, which is detectable by pulsar timing arrays. In this paper, we investigate the gravitational effect of ultralight tensor dark matter on the arrival time of radio pulses… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.08091v2-abstract-full').style.display = 'inline'; document.getElementById('2305.08091v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.08091v2-abstract-full" style="display: none;"> Ultralight boson fields, with a mass around $10^{-23}\text{eV}$, are promising candidates for the elusive cosmological dark matter. These fields induce a periodic oscillation of the spacetime metric in the nanohertz frequency band, which is detectable by pulsar timing arrays. In this paper, we investigate the gravitational effect of ultralight tensor dark matter on the arrival time of radio pulses from pulsars. We find that the pulsar timing signal caused by tensor dark matter exhibits a different angular dependence than that by scalar and vector dark matter, making it possible to distinguish the ultralight dark matter signal with different spins. Combining the gravitational effect and the coupling effect of ultralight tensor dark matter with standard model matter provides a complementary way to constrain the coupling parameter $伪$. We estimate $伪\lesssim 10^{-6}\sim 10^{-5}$ in the mass range $m<5\times 10^{-23}\mathrm{eV}$ with current pulsar timing array. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.08091v2-abstract-full').style.display = 'none'; document.getElementById('2305.08091v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 3 figures; match the published version</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.13921">arXiv:2304.13921</a> <span> [<a href="https://arxiv.org/pdf/2304.13921">pdf</a>, <a href="https://arxiv.org/ps/2304.13921">ps</a>, <a href="https://arxiv.org/format/2304.13921">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Theory">nucl-th</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.130.251902">10.1103/PhysRevLett.130.251902 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First study of reaction $螢^{0}n\rightarrow螢^{-}p$ using $螢^0$-nucleus scattering at an electron-positron collider </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=BESIII+Collaboration"> BESIII Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Ablikim%2C+M">M. Ablikim</a>, <a href="/search/hep-ph?searchtype=author&query=Achasov%2C+M+N">M. N. Achasov</a>, <a href="/search/hep-ph?searchtype=author&query=Adlarson%2C+P">P. Adlarson</a>, <a href="/search/hep-ph?searchtype=author&query=Aliberti%2C+R">R. Aliberti</a>, <a href="/search/hep-ph?searchtype=author&query=Amoroso%2C+A">A. Amoroso</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+M+R">M. R. An</a>, <a href="/search/hep-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+Y">Y. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=Bakina%2C+O">O. Bakina</a>, <a href="/search/hep-ph?searchtype=author&query=Balossino%2C+I">I. Balossino</a>, <a href="/search/hep-ph?searchtype=author&query=Ban%2C+Y">Y. Ban</a>, <a href="/search/hep-ph?searchtype=author&query=Batozskaya%2C+V">V. Batozskaya</a>, <a href="/search/hep-ph?searchtype=author&query=Begzsuren%2C+K">K. Begzsuren</a>, <a href="/search/hep-ph?searchtype=author&query=Berger%2C+N">N. Berger</a>, <a href="/search/hep-ph?searchtype=author&query=Berlowski%2C+M">M. Berlowski</a>, <a href="/search/hep-ph?searchtype=author&query=Bertani%2C+M">M. Bertani</a>, <a href="/search/hep-ph?searchtype=author&query=Bettoni%2C+D">D. Bettoni</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchi%2C+F">F. Bianchi</a>, <a href="/search/hep-ph?searchtype=author&query=Bianco%2C+E">E. Bianco</a>, <a href="/search/hep-ph?searchtype=author&query=Bloms%2C+J">J. Bloms</a>, <a href="/search/hep-ph?searchtype=author&query=Bortone%2C+A">A. Bortone</a>, <a href="/search/hep-ph?searchtype=author&query=Boyko%2C+I">I. Boyko</a>, <a href="/search/hep-ph?searchtype=author&query=Briere%2C+R+A">R. A. Briere</a>, <a href="/search/hep-ph?searchtype=author&query=Brueggemann%2C+A">A. Brueggemann</a> , et al. (593 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.13921v3-abstract-short" style="display: inline;"> Using $(1.0087\pm0.0044)\times10^{10}$ $J/蠄$ events collected with the BESIII detector at the BEPCII storage ring, the process $螢^{0}n\rightarrow螢^{-}p$ is studied, where the $螢^0$ baryon is produced in the process $J/蠄\rightarrow螢^0\bar螢^0$ and the neutron is a component of the $^9\rm{Be}$, $^{12}\rm{C}$ and $^{197}\rm{Au}$ nuclei in the beam pipe. A clear signal is observed with a statistical si… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13921v3-abstract-full').style.display = 'inline'; document.getElementById('2304.13921v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.13921v3-abstract-full" style="display: none;"> Using $(1.0087\pm0.0044)\times10^{10}$ $J/蠄$ events collected with the BESIII detector at the BEPCII storage ring, the process $螢^{0}n\rightarrow螢^{-}p$ is studied, where the $螢^0$ baryon is produced in the process $J/蠄\rightarrow螢^0\bar螢^0$ and the neutron is a component of the $^9\rm{Be}$, $^{12}\rm{C}$ and $^{197}\rm{Au}$ nuclei in the beam pipe. A clear signal is observed with a statistical significance of $7.1蟽$. The cross section of the reaction $螢^0+{^9\rm{Be}}\rightarrow螢^-+p+{^8\rm{Be}}$ is determined to be $蟽(螢^0+{^9\rm{Be}}\rightarrow螢^-+p+{^8\rm{Be}})=(22.1\pm5.3_{\rm{stat}}\pm4.5_{\rm{sys}})$ mb at the $螢^0$ momentum of $0.818$ GeV/$c$, where the first uncertainty is statistical and the second is systematic. No significant $H$-dibaryon signal is observed in the $螢^-p$ final state. This is the first study of hyperon-nucleon interactions in electron-positron collisions and opens up a new direction for such research. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13921v3-abstract-full').style.display = 'none'; document.getElementById('2304.13921v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 figures, with Supplemental Material</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15920">arXiv:2303.15920</a> <span> [<a href="https://arxiv.org/pdf/2303.15920">pdf</a>, <a href="https://arxiv.org/format/2303.15920">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Probing Heavy Neutrinos at the LHC from Fat-jet using Machine Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Liu%2C+W">Wei Liu</a>, <a href="/search/hep-ph?searchtype=author&query=Li%2C+J">Jing Li</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zixiang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Sun%2C+H">Hao Sun</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.15920v1-abstract-short" style="display: inline;"> We explore the potential to use machine learning methods to search for heavy neutrinos, from their hadronic final states including a fat-jet signal, via the processes $pp \rightarrow W^{\pm *}\rightarrow 渭^{\pm} N \rightarrow 渭^{\pm} 渭^{\mp} W^{\pm} \rightarrow 渭^{\pm} 渭^{\mp} J$ at hadron colliders. We use either the Gradient Boosted Decision Tree or Multi-Layer Perceptron methods to analyse the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15920v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15920v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15920v1-abstract-full" style="display: none;"> We explore the potential to use machine learning methods to search for heavy neutrinos, from their hadronic final states including a fat-jet signal, via the processes $pp \rightarrow W^{\pm *}\rightarrow 渭^{\pm} N \rightarrow 渭^{\pm} 渭^{\mp} W^{\pm} \rightarrow 渭^{\pm} 渭^{\mp} J$ at hadron colliders. We use either the Gradient Boosted Decision Tree or Multi-Layer Perceptron methods to analyse the observables incorporating the jet substructure information, which is performed at hadron colliders with $\sqrt{s}=$ 13, 27, 100 TeV. It is found that, among the observables, the invariant masses of variable system and the observables from the leptons are the most powerful ones to distinguish the signal from the background. With the help of machine learning techniques, the limits on the active-sterile mixing have been improved by about one magnitude comparing to the cut-based analyses, with $V_{渭N}^2 \lesssim 10^{-4}$ for the heavy neutrinos with masses, 100 GeV$~<m_N<~$1 TeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15920v1-abstract-full').style.display = 'none'; document.getElementById('2303.15920v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 8 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.14117">arXiv:2303.14117</a> <span> [<a href="https://arxiv.org/pdf/2303.14117">pdf</a>, <a href="https://arxiv.org/format/2303.14117">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/05/129">10.1088/1475-7516/2024/05/129 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SKA sensitivity for possible radio emission from dark matter in Omega Centauri </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Wang%2C+G">Guan-Sen Wang</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+Z">Zhan-Fang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Zu%2C+L">Lei Zu</a>, <a href="/search/hep-ph?searchtype=author&query=Gong%2C+H">Hao Gong</a>, <a href="/search/hep-ph?searchtype=author&query=Feng%2C+L">Lei Feng</a>, <a href="/search/hep-ph?searchtype=author&query=Fan%2C+Y">Yi-Zhong Fan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.14117v4-abstract-short" style="display: inline;"> Omega Centauri, the largest known globular cluster in the Milky Way, is believed to be the remains of a dwarf galaxy's core. Giving its potential abundance of dark matter (DM), it is an attractive target for investigating the nature of this elusive substance in our local environment. Our study demonstrates that by observing Omega Centauri with the SKA for 1000 hours, we can detect synchrotron radi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14117v4-abstract-full').style.display = 'inline'; document.getElementById('2303.14117v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.14117v4-abstract-full" style="display: none;"> Omega Centauri, the largest known globular cluster in the Milky Way, is believed to be the remains of a dwarf galaxy's core. Giving its potential abundance of dark matter (DM), it is an attractive target for investigating the nature of this elusive substance in our local environment. Our study demonstrates that by observing Omega Centauri with the SKA for 1000 hours, we can detect synchrotron radio or Inverse Compton (IC) emissions from the DM annihilation products. It enables us to constrain the cross-section of DM annihilation down to $\sim {\rm 10^{-30}~cm^3~s^{-1}}$ for DM mass from several $\rm{GeV}$ to $\rm{100~GeV}$, which is much stronger compared with other observations. Additionally, we explore the axion, another well-motivated DM candidate, and provide stimulated decay calculations. It turns out that the sensitivity can reach $g_{\rm{a纬纬}} \sim 10^{-10} ~\rm{GeV^{-1}}$ for $2\times 10^{-7} ~\rm{eV} < m_a < 2\times 10^{-4} ~\rm{eV}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.14117v4-abstract-full').style.display = 'none'; document.getElementById('2303.14117v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP05(2024)129 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.13663">arXiv:2303.13663</a> <span> [<a href="https://arxiv.org/pdf/2303.13663">pdf</a>, <a href="https://arxiv.org/format/2303.13663">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Search for neutrino lines from dark matter annihilation and decay with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=The+IceCube+Collaboration"> The IceCube Collaboration</a>, <a href="/search/hep-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/hep-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/hep-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/hep-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/hep-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/hep-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/hep-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/hep-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/hep-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/hep-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/hep-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/hep-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/hep-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/hep-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/hep-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/hep-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/hep-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/hep-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/hep-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/hep-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/hep-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/hep-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/hep-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/hep-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (373 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.13663v1-abstract-short" style="display: inline;"> Dark Matter particles in the Galactic Center and halo can annihilate or decay into a pair of neutrinos producing a monochromatic flux of neutrinos. The spectral feature of this signal is unique and it is not expected from any astrophysical production mechanism. Its observation would constitute a dark matter smoking gun signal. We performed the first dedicated search with a neutrino telescope for s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13663v1-abstract-full').style.display = 'inline'; document.getElementById('2303.13663v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.13663v1-abstract-full" style="display: none;"> Dark Matter particles in the Galactic Center and halo can annihilate or decay into a pair of neutrinos producing a monochromatic flux of neutrinos. The spectral feature of this signal is unique and it is not expected from any astrophysical production mechanism. Its observation would constitute a dark matter smoking gun signal. We performed the first dedicated search with a neutrino telescope for such signal, by looking at both the angular and energy information of the neutrino events. To this end, a total of five years of IceCube's DeepCore data has been used to test dark matter masses ranging from 10~GeV to 40~TeV. No significant neutrino excess was found and upper limits on the annihilation cross section, as well as lower limits on the dark matter lifetime, were set. The limits reached are of the order of $10^{-24}$~cm$^3/s$ for an annihilation and up to $10^{27}$ seconds for decaying Dark Matter. Using the same data sample we also derive limits for dark matter annihilation or decay into a pair of Standard Model charged particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13663v1-abstract-full').style.display = 'none'; document.getElementById('2303.13663v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Chen%2C+Z&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Chen%2C+Z&start=0" class="pagination-link 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