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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.00090">arXiv:2410.00090</a> <span> [<a href="https://arxiv.org/pdf/2410.00090">pdf</a>, <a href="https://arxiv.org/format/2410.00090">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="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Massive neutrinos and cosmic composition </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Loverde%2C+M">Marilena Loverde</a>, <a href="/search/hep-ph?searchtype=author&query=Weiner%2C+Z+J">Zachary J. Weiner</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="2410.00090v2-abstract-short" style="display: inline;"> Cosmological data probe massive neutrinos via their effects on the geometry of the Universe and the growth of structure, both of which are degenerate with the late-time expansion history. We clarify the nature of these degeneracies and the individual roles of both probes in neutrino mass inference. Geometry is strongly sensitive to neutrino masses: within $螞$CDM, the primary cosmic microwave backg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00090v2-abstract-full').style.display = 'inline'; document.getElementById('2410.00090v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.00090v2-abstract-full" style="display: none;"> Cosmological data probe massive neutrinos via their effects on the geometry of the Universe and the growth of structure, both of which are degenerate with the late-time expansion history. We clarify the nature of these degeneracies and the individual roles of both probes in neutrino mass inference. Geometry is strongly sensitive to neutrino masses: within $螞$CDM, the primary cosmic microwave background anisotropies alone impose that the matter fraction $惟_m$ must increase fivefold with increasing neutrino mass. Moreover, large-scale structure observables, like weak lensing of the CMB, are dimensionless and thus depend not on the matter density (as often quoted) but in fact the matter fraction. We explore the consequential impact of this distinction on the interplay between probes of structure, low-redshift distances, and CMB anisotropies. We derive constraints on the neutrino's masses independently from their suppression of structure and impact on geometry, showing that the latter is at least as important as the former. While the Dark Energy Spectroscopic Instrument's recent baryon acoustic oscillation data place stringent bounds largely deriving from their geometric incompatibility with massive neutrinos, all recent type Ia supernova datasets drive marginal preferences for nonzero neutrino masses because they prefer substantially larger matter fractions. Recent CMB lensing data, however, neither exclude neutrinos' suppression of structure nor constrain it strongly enough to discriminate between mass hierarchies. Current data thus evince not a need for modified dynamics of neutrino perturbations or structure growth but rather an inconsistent compatibility with massive neutrinos' impact on the expansion history. We identify two of DESI's measurements that strongly influence its constraints, and we also discuss neutrino mass measurements in models that alter the sound horizon. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00090v2-abstract-full').style.display = 'none'; document.getElementById('2410.00090v2-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> 16 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 September, 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">38+16 pages, 20 figures; matches 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/2212.13264">arXiv:2212.13264</a> <span> [<a href="https://arxiv.org/pdf/2212.13264">pdf</a>, <a href="https://arxiv.org/format/2212.13264">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="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.107.123517">10.1103/PhysRevD.107.123517 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Confronting interacting dark radiation scenarios with cosmological data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Brinckmann%2C+T">Thejs Brinckmann</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+J+H">Jae Hyeok Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Du%2C+P">Peizhi Du</a>, <a href="/search/hep-ph?searchtype=author&query=LoVerde%2C+M">Marilena LoVerde</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="2212.13264v2-abstract-short" style="display: inline;"> Dark radiation (DR) is generally predicted in new physics scenarios that address fundamental puzzles of the Standard Model or tensions in the cosmological data. Cosmological data has the sensitivity to constrain not only the energy density of DR, but also whether it is interacting. In this paper, we present a systematic study of five types of interacting DR (free-streaming, fluid, decoupling, inst… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.13264v2-abstract-full').style.display = 'inline'; document.getElementById('2212.13264v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2212.13264v2-abstract-full" style="display: none;"> Dark radiation (DR) is generally predicted in new physics scenarios that address fundamental puzzles of the Standard Model or tensions in the cosmological data. Cosmological data has the sensitivity to constrain not only the energy density of DR, but also whether it is interacting. In this paper, we present a systematic study of five types of interacting DR (free-streaming, fluid, decoupling, instantaneous decoupling, and recoupling DR) and their impact on cosmological observables. We modify the Boltzmann hierarchy to describe all these types of interacting DR under the relaxation time approximation. We, for the first time, robustly calculate the collision terms for recoupling scalar DR and provide a better estimation of the recoupling transition redshift. We demonstrate the distinct features of each type of DR on the CMB and matter power spectra. We perform MCMC scans using the Planck 2018 data and BAO data. Assuming no new physics in the SM neutrino sector, we find no statistically significant constraints on the couplings of DR, although there is a slight preference for the fluid-like limit of all the cases. In the case of instantaneous decoupling DR, this limit corresponds to a late transition redshift around recombination. The $螖N_{\rm eff}$ constraint varies marginally depending on the type of DR. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2212.13264v2-abstract-full').style.display = 'none'; document.getElementById('2212.13264v2-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, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2022. </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 + references, 12 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/2209.06854">arXiv:2209.06854</a> <span> [<a href="https://arxiv.org/pdf/2209.06854">pdf</a>, <a href="https://arxiv.org/format/2209.06854">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 Physics - Theory">hep-th</span> </div> </div> <p class="title is-5 mathjax"> Snowmass Theory Frontier: Astrophysics and Cosmology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Green%2C+D">Daniel Green</a>, <a href="/search/hep-ph?searchtype=author&query=Ruderman%2C+J+T">Joshua T. Ruderman</a>, <a href="/search/hep-ph?searchtype=author&query=Safdi%2C+B+R">Benjamin R. Safdi</a>, <a href="/search/hep-ph?searchtype=author&query=Shelton%2C+J">Jessie Shelton</a>, <a href="/search/hep-ph?searchtype=author&query=Ach%C3%BAcarro%2C+A">Ana Ach煤carro</a>, <a href="/search/hep-ph?searchtype=author&query=Adshead%2C+P">Peter Adshead</a>, <a href="/search/hep-ph?searchtype=author&query=Akrami%2C+Y">Yashar Akrami</a>, <a href="/search/hep-ph?searchtype=author&query=Baryakhtar%2C+M">Masha Baryakhtar</a>, <a href="/search/hep-ph?searchtype=author&query=Baumann%2C+D">Daniel Baumann</a>, <a href="/search/hep-ph?searchtype=author&query=Berlin%2C+A">Asher Berlin</a>, <a href="/search/hep-ph?searchtype=author&query=Blinov%2C+N">Nikita Blinov</a>, <a href="/search/hep-ph?searchtype=author&query=Boddy%2C+K+K">Kimberly K. Boddy</a>, <a href="/search/hep-ph?searchtype=author&query=Buschmann%2C+M">Malte Buschmann</a>, <a href="/search/hep-ph?searchtype=author&query=Cabass%2C+G">Giovanni Cabass</a>, <a href="/search/hep-ph?searchtype=author&query=Caldwell%2C+R">Robert Caldwell</a>, <a href="/search/hep-ph?searchtype=author&query=Castorina%2C+E">Emanuele Castorina</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+T+Y">Thomas Y. Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+X">Xingang Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Coulton%2C+W">William Coulton</a>, <a href="/search/hep-ph?searchtype=author&query=Croon%2C+D">Djuna Croon</a>, <a href="/search/hep-ph?searchtype=author&query=Cui%2C+Y">Yanou Cui</a>, <a href="/search/hep-ph?searchtype=author&query=Curtin%2C+D">David Curtin</a>, <a href="/search/hep-ph?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/hep-ph?searchtype=author&query=Dessert%2C+C">Christopher Dessert</a>, <a href="/search/hep-ph?searchtype=author&query=Dienes%2C+K+R">Keith R. Dienes</a> , et al. (62 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="2209.06854v1-abstract-short" style="display: inline;"> We summarize progress made in theoretical astrophysics and cosmology over the past decade and areas of interest for the coming decade. This Report is prepared as the TF09 "Astrophysics and Cosmology" topical group summary for the Theory Frontier as part of the Snowmass 2021 process. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.06854v1-abstract-full" style="display: none;"> We summarize progress made in theoretical astrophysics and cosmology over the past decade and areas of interest for the coming decade. This Report is prepared as the TF09 "Astrophysics and Cosmology" topical group summary for the Theory Frontier as part of the Snowmass 2021 process. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.06854v1-abstract-full').style.display = 'none'; document.getElementById('2209.06854v1-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </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">57 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/2208.11714">arXiv:2208.11714</a> <span> [<a href="https://arxiv.org/pdf/2208.11714">pdf</a>, <a href="https://arxiv.org/format/2208.11714">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/10.1088/1475-7516/2023/02/064">10.1088/1475-7516/2023/02/064 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing neutrino interactions and dark radiation with gravitational waves </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Loverde%2C+M">Marilena Loverde</a>, <a href="/search/hep-ph?searchtype=author&query=Weiner%2C+Z+J">Zachary J. Weiner</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="2208.11714v2-abstract-short" style="display: inline;"> After their generation, cosmological backgrounds of gravitational waves propagate nearly freely but for the expansion of the Universe and the anisotropic stress of free-streaming particles. Primordial signals -- both that from inflation and the infrared spectrum associated to subhorizon production mechanisms -- would carry clean information about the cosmological history of these effects. We study… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.11714v2-abstract-full').style.display = 'inline'; document.getElementById('2208.11714v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.11714v2-abstract-full" style="display: none;"> After their generation, cosmological backgrounds of gravitational waves propagate nearly freely but for the expansion of the Universe and the anisotropic stress of free-streaming particles. Primordial signals -- both that from inflation and the infrared spectrum associated to subhorizon production mechanisms -- would carry clean information about the cosmological history of these effects. We study the modulation of the standard damping of gravitational waves by free-streaming radiation due to the decoupling (or recoupling) of interactions. We focus on nonstandard neutrino interactions in effect after the decoupling of weak interactions as well as more general scenarios in the early Universe involving other light relics. We develop semianalytic results in fully free-streaming scenarios to provide intuition for numerical results that incorporate interaction rates with a variety of temerpature dependencies. Finally, we compute the imprint of neutrino interactions on the $B$-mode polarization of the cosmic microwave background, and we comment on other means to infer the presence of such effects at higher frequencies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.11714v2-abstract-full').style.display = 'none'; document.getElementById('2208.11714v2-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </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">33 pages, 8 figures; matches 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/2203.08024">arXiv:2203.08024</a> <span> [<a href="https://arxiv.org/pdf/2203.08024">pdf</a>, <a href="https://arxiv.org/format/2203.08024">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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 - 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"> Snowmass 2021 CMB-S4 White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Abazajian%2C+K">Kevork Abazajian</a>, <a href="/search/hep-ph?searchtype=author&query=Abdulghafour%2C+A">Arwa Abdulghafour</a>, <a href="/search/hep-ph?searchtype=author&query=Addison%2C+G+E">Graeme E. Addison</a>, <a href="/search/hep-ph?searchtype=author&query=Adshead%2C+P">Peter Adshead</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmed%2C+Z">Zeeshan Ahmed</a>, <a href="/search/hep-ph?searchtype=author&query=Ajello%2C+M">Marco Ajello</a>, <a href="/search/hep-ph?searchtype=author&query=Akerib%2C+D">Daniel Akerib</a>, <a href="/search/hep-ph?searchtype=author&query=Allen%2C+S+W">Steven W. Allen</a>, <a href="/search/hep-ph?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/hep-ph?searchtype=author&query=Alvarez%2C+M">Marcelo Alvarez</a>, <a href="/search/hep-ph?searchtype=author&query=Amin%2C+M+A">Mustafa A. Amin</a>, <a href="/search/hep-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/hep-ph?searchtype=author&query=Anderson%2C+A">Adam Anderson</a>, <a href="/search/hep-ph?searchtype=author&query=Ansarinejad%2C+B">Behzad Ansarinejad</a>, <a href="/search/hep-ph?searchtype=author&query=Archipley%2C+M">Melanie Archipley</a>, <a href="/search/hep-ph?searchtype=author&query=Arnold%2C+K+S">Kam S. Arnold</a>, <a href="/search/hep-ph?searchtype=author&query=Ashby%2C+M">Matt Ashby</a>, <a href="/search/hep-ph?searchtype=author&query=Aung%2C+H">Han Aung</a>, <a href="/search/hep-ph?searchtype=author&query=Baccigalupi%2C+C">Carlo Baccigalupi</a>, <a href="/search/hep-ph?searchtype=author&query=Baker%2C+C">Carina Baker</a>, <a href="/search/hep-ph?searchtype=author&query=Bakshi%2C+A">Abhishek Bakshi</a>, <a href="/search/hep-ph?searchtype=author&query=Bard%2C+D">Debbie Bard</a>, <a href="/search/hep-ph?searchtype=author&query=Barkats%2C+D">Denis Barkats</a>, <a href="/search/hep-ph?searchtype=author&query=Barron%2C+D">Darcy Barron</a>, <a href="/search/hep-ph?searchtype=author&query=Barry%2C+P+S">Peter S. Barry</a> , et al. (331 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="2203.08024v1-abstract-short" style="display: inline;"> This Snowmass 2021 White Paper describes the Cosmic Microwave Background Stage 4 project CMB-S4, which is designed to cross critical thresholds in our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. We provide an overview of the science case, the technical design, and project plan. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.08024v1-abstract-full" style="display: none;"> This Snowmass 2021 White Paper describes the Cosmic Microwave Background Stage 4 project CMB-S4, which is designed to cross critical thresholds in our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. We provide an overview of the science case, the technical design, and project plan. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08024v1-abstract-full').style.display = 'none'; document.getElementById('2203.08024v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </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 Snowmass 2021. arXiv admin note: substantial text overlap with arXiv:1908.01062, arXiv:1907.04473</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07943">arXiv:2203.07943</a> <span> [<a href="https://arxiv.org/pdf/2203.07943">pdf</a>, <a href="https://arxiv.org/format/2203.07943">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> </div> </div> <p class="title is-5 mathjax"> The Physics of Light Relics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Dvorkin%2C+C">Cora Dvorkin</a>, <a href="/search/hep-ph?searchtype=author&query=Meyers%2C+J">Joel Meyers</a>, <a href="/search/hep-ph?searchtype=author&query=Adshead%2C+P">Peter Adshead</a>, <a href="/search/hep-ph?searchtype=author&query=Amin%2C+M">Mustafa Amin</a>, <a href="/search/hep-ph?searchtype=author&query=Arg%C3%BCelles%2C+C+A">Carlos A. Arg眉elles</a>, <a href="/search/hep-ph?searchtype=author&query=Brinckmann%2C+T">Thejs Brinckmann</a>, <a href="/search/hep-ph?searchtype=author&query=Castorina%2C+E">Emanuele Castorina</a>, <a href="/search/hep-ph?searchtype=author&query=Cohen%2C+T">Timothy Cohen</a>, <a href="/search/hep-ph?searchtype=author&query=Craig%2C+N">Nathaniel Craig</a>, <a href="/search/hep-ph?searchtype=author&query=Curtin%2C+D">David Curtin</a>, <a href="/search/hep-ph?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/hep-ph?searchtype=author&query=Du%2C+P">Peizhi Du</a>, <a href="/search/hep-ph?searchtype=author&query=Knox%2C+L">Lloyd Knox</a>, <a href="/search/hep-ph?searchtype=author&query=Li%2C+B">Bohua Li</a>, <a href="/search/hep-ph?searchtype=author&query=Loverde%2C+M">Marilena Loverde</a>, <a href="/search/hep-ph?searchtype=author&query=Lozanov%2C+K">Kaloian Lozanov</a>, <a href="/search/hep-ph?searchtype=author&query=Mu%C3%B1oz%2C+J+B">Julian B. Mu帽oz</a>, <a href="/search/hep-ph?searchtype=author&query=Schutz%2C+K">Katelin Schutz</a>, <a href="/search/hep-ph?searchtype=author&query=Shapiro%2C+P">Paul Shapiro</a>, <a href="/search/hep-ph?searchtype=author&query=Wallisch%2C+B">Benjamin Wallisch</a>, <a href="/search/hep-ph?searchtype=author&query=Weiner%2C+Z+J">Zachary J. Weiner</a>, <a href="/search/hep-ph?searchtype=author&query=Xu%2C+W+L">Weishuang Linda Xu</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="2203.07943v1-abstract-short" style="display: inline;"> Many well-motivated extensions of the Standard Model predict the existence of new light species that may have been produced in the early universe. Prominent examples include axions, sterile neutrinos, gravitinos, dark photons, and more. The gravitational influence of light relics leaves imprints in the cosmic microwave background fluctuations, the large-scale structure of the universe and the prim… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07943v1-abstract-full').style.display = 'inline'; document.getElementById('2203.07943v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07943v1-abstract-full" style="display: none;"> Many well-motivated extensions of the Standard Model predict the existence of new light species that may have been produced in the early universe. Prominent examples include axions, sterile neutrinos, gravitinos, dark photons, and more. The gravitational influence of light relics leaves imprints in the cosmic microwave background fluctuations, the large-scale structure of the universe and the primordial element abundances. In this paper, we detail the physics of cosmological light relics, and describe how measurements of their relic density and mass serve as probes of physics beyond the Standard Model. A measurement of the light relic density at the precision of upcoming cosmological surveys will point the way toward new physics or severely constrain the range of viable extensions to the Standard Model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07943v1-abstract-full').style.display = 'none'; document.getElementById('2203.07943v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </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 Snowmass 2021. 59 pages, 12 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/2203.07638">arXiv:2203.07638</a> <span> [<a href="https://arxiv.org/pdf/2203.07638">pdf</a>, <a href="https://arxiv.org/format/2203.07638">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</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 - 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"> Snowmass2021 Cosmic Frontier: Cosmic Microwave Background Measurements White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Chang%2C+C+L">Clarence L. Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Huffenberger%2C+K+M">Kevin M. Huffenberger</a>, <a href="/search/hep-ph?searchtype=author&query=Benson%2C+B+A">Bradford A. Benson</a>, <a href="/search/hep-ph?searchtype=author&query=Bianchini%2C+F">Federico Bianchini</a>, <a href="/search/hep-ph?searchtype=author&query=Chluba%2C+J">Jens Chluba</a>, <a href="/search/hep-ph?searchtype=author&query=Delabrouille%2C+J">Jacques Delabrouille</a>, <a href="/search/hep-ph?searchtype=author&query=Flauger%2C+R">Raphael Flauger</a>, <a href="/search/hep-ph?searchtype=author&query=Hanany%2C+S">Shaul Hanany</a>, <a href="/search/hep-ph?searchtype=author&query=Jones%2C+W+C">William C. Jones</a>, <a href="/search/hep-ph?searchtype=author&query=Kogut%2C+A+J">Alan J. Kogut</a>, <a href="/search/hep-ph?searchtype=author&query=McMahon%2C+J+J">Jeffrey J. McMahon</a>, <a href="/search/hep-ph?searchtype=author&query=Meyers%2C+J">Joel Meyers</a>, <a href="/search/hep-ph?searchtype=author&query=Sehgal%2C+N">Neelima Sehgal</a>, <a href="/search/hep-ph?searchtype=author&query=Simon%2C+S+M">Sara M. Simon</a>, <a href="/search/hep-ph?searchtype=author&query=Umilta%2C+C">Caterina Umilta</a>, <a href="/search/hep-ph?searchtype=author&query=Abazajian%2C+K+N">Kevork N. Abazajian</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmed%2C+Z">Zeeshan Ahmed</a>, <a href="/search/hep-ph?searchtype=author&query=Akrami%2C+Y">Yashar Akrami</a>, <a href="/search/hep-ph?searchtype=author&query=Anderson%2C+A+J">Adam J. Anderson</a>, <a href="/search/hep-ph?searchtype=author&query=Ansarinejad%2C+B">Behzad Ansarinejad</a>, <a href="/search/hep-ph?searchtype=author&query=Austermann%2C+J">Jason Austermann</a>, <a href="/search/hep-ph?searchtype=author&query=Baccigalupi%2C+C">Carlo Baccigalupi</a>, <a href="/search/hep-ph?searchtype=author&query=Barkats%2C+D">Denis Barkats</a>, <a href="/search/hep-ph?searchtype=author&query=Barron%2C+D">Darcy Barron</a>, <a href="/search/hep-ph?searchtype=author&query=Barry%2C+P+S">Peter S. Barry</a> , et al. (107 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="2203.07638v1-abstract-short" style="display: inline;"> This is a solicited whitepaper for the Snowmass 2021 community planning exercise. The paper focuses on measurements and science with the Cosmic Microwave Background (CMB). The CMB is foundational to our understanding of modern physics and continues to be a powerful tool driving our understanding of cosmology and particle physics. In this paper, we outline the broad and unique impact of CMB science… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07638v1-abstract-full').style.display = 'inline'; document.getElementById('2203.07638v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07638v1-abstract-full" style="display: none;"> This is a solicited whitepaper for the Snowmass 2021 community planning exercise. The paper focuses on measurements and science with the Cosmic Microwave Background (CMB). The CMB is foundational to our understanding of modern physics and continues to be a powerful tool driving our understanding of cosmology and particle physics. In this paper, we outline the broad and unique impact of CMB science for the High Energy Cosmic Frontier in the upcoming decade. We also describe the progression of ground-based CMB experiments, which shows that the community is prepared to develop the key capabilities and facilities needed to achieve these transformative CMB measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07638v1-abstract-full').style.display = 'none'; document.getElementById('2203.07638v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </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 Snowmass 2021</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.07377">arXiv:2203.07377</a> <span> [<a href="https://arxiv.org/pdf/2203.07377">pdf</a>, <a href="https://arxiv.org/format/2203.07377">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> </div> </div> <p class="title is-5 mathjax"> Synergy between cosmological and laboratory searches in neutrino physics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Gerbino%2C+M">Martina Gerbino</a>, <a href="/search/hep-ph?searchtype=author&query=Grohs%2C+E">Evan Grohs</a>, <a href="/search/hep-ph?searchtype=author&query=Lattanzi%2C+M">Massimiliano Lattanzi</a>, <a href="/search/hep-ph?searchtype=author&query=Abazajian%2C+K+N">Kevork N. Abazajian</a>, <a href="/search/hep-ph?searchtype=author&query=Blinov%2C+N">Nikita Blinov</a>, <a href="/search/hep-ph?searchtype=author&query=Brinckmann%2C+T">Thejs Brinckmann</a>, <a href="/search/hep-ph?searchtype=author&query=Chen%2C+M">Mu-Chun Chen</a>, <a href="/search/hep-ph?searchtype=author&query=Djurcic%2C+Z">Zelimir Djurcic</a>, <a href="/search/hep-ph?searchtype=author&query=Du%2C+P">Peizhi Du</a>, <a href="/search/hep-ph?searchtype=author&query=Escudero%2C+M">Miguel Escudero</a>, <a href="/search/hep-ph?searchtype=author&query=Hagstotz%2C+S">Steffen Hagstotz</a>, <a href="/search/hep-ph?searchtype=author&query=Kelly%2C+K+J">Kevin J. Kelly</a>, <a href="/search/hep-ph?searchtype=author&query=Lorenz%2C+C+S">Christiane S. Lorenz</a>, <a href="/search/hep-ph?searchtype=author&query=Loverde%2C+M">Marilena Loverde</a>, <a href="/search/hep-ph?searchtype=author&query=Mart%C3%ADnez-Mirav%C3%A9%2C+P">Pablo Mart铆nez-Mirav茅</a>, <a href="/search/hep-ph?searchtype=author&query=Mena%2C+O">Olga Mena</a>, <a href="/search/hep-ph?searchtype=author&query=Meyers%2C+J">Joel Meyers</a>, <a href="/search/hep-ph?searchtype=author&query=Pettus%2C+W">Walter Pettus</a>, <a href="/search/hep-ph?searchtype=author&query=Saviano%2C+N">Ninetta Saviano</a>, <a href="/search/hep-ph?searchtype=author&query=Suliga%2C+A+M">Anna M. Suliga</a>, <a href="/search/hep-ph?searchtype=author&query=Takhistov%2C+V">Volodymyr Takhistov</a>, <a href="/search/hep-ph?searchtype=author&query=T%C3%B3rtola%2C+M">Mariam T贸rtola</a>, <a href="/search/hep-ph?searchtype=author&query=Valle%2C+J+W+F">Jos茅 W. F. Valle</a>, <a href="/search/hep-ph?searchtype=author&query=Wallisch%2C+B">Benjamin Wallisch</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="2203.07377v3-abstract-short" style="display: inline;"> The intersection of the cosmic and neutrino frontiers is a rich field where much discovery space still remains. Neutrinos play a pivotal role in the hot big bang cosmology, influencing the dynamics of the universe over numerous decades in cosmological history. Recent studies have made tremendous progress in understanding some properties of cosmological neutrinos, primarily their energy density. Up… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07377v3-abstract-full').style.display = 'inline'; document.getElementById('2203.07377v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.07377v3-abstract-full" style="display: none;"> The intersection of the cosmic and neutrino frontiers is a rich field where much discovery space still remains. Neutrinos play a pivotal role in the hot big bang cosmology, influencing the dynamics of the universe over numerous decades in cosmological history. Recent studies have made tremendous progress in understanding some properties of cosmological neutrinos, primarily their energy density. Upcoming cosmological probes will measure the energy density of relativistic particles with higher precision, but could also start probing other properties of the neutrino spectra. When convolved with results from terrestrial experiments, cosmology can become even more acute at probing new physics related to neutrinos or even Beyond the Standard Model (BSM). Any discordance between laboratory and cosmological data sets may reveal new BSM physics and/or suggest alternative models of cosmology. We give examples of the intersection between terrestrial and cosmological probes in the neutrino sector, and briefly discuss the possibilities of what different laboratory experiments may see in conjunction with cosmological observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.07377v3-abstract-full').style.display = 'none'; document.getElementById('2203.07377v3-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> 26 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </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">Originally prepared for submission to the Snowmass Community Planning Exercise, 2021; Current version accepted by Physics of the Dark Universe; 136 pages; 9 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/2203.01955">arXiv:2203.01955</a> <span> [<a href="https://arxiv.org/pdf/2203.01955">pdf</a>, <a href="https://arxiv.org/format/2203.01955">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 Astrophysical Phenomena">astro-ph.HE</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 - 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/10.1016/j.dark.2023.101267">10.1016/j.dark.2023.101267 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Neutrino Self-Interactions: A White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Berryman%2C+J+M">Jeffrey M. Berryman</a>, <a href="/search/hep-ph?searchtype=author&query=Blinov%2C+N">Nikita Blinov</a>, <a href="/search/hep-ph?searchtype=author&query=Brdar%2C+V">Vedran Brdar</a>, <a href="/search/hep-ph?searchtype=author&query=Brinckmann%2C+T">Thejs Brinckmann</a>, <a href="/search/hep-ph?searchtype=author&query=Bustamante%2C+M">Mauricio Bustamante</a>, <a href="/search/hep-ph?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/hep-ph?searchtype=author&query=Das%2C+A">Anirban Das</a>, <a href="/search/hep-ph?searchtype=author&query=de+Gouv%C3%AAa%2C+A">Andr茅 de Gouv锚a</a>, <a href="/search/hep-ph?searchtype=author&query=Denton%2C+P+B">Peter B. Denton</a>, <a href="/search/hep-ph?searchtype=author&query=Dev%2C+P+S+B">P. S. Bhupal Dev</a>, <a href="/search/hep-ph?searchtype=author&query=Dutta%2C+B">Bhaskar Dutta</a>, <a href="/search/hep-ph?searchtype=author&query=Esteban%2C+I">Ivan Esteban</a>, <a href="/search/hep-ph?searchtype=author&query=Fiorillo%2C+D+F+G">Damiano F. G. Fiorillo</a>, <a href="/search/hep-ph?searchtype=author&query=Gerbino%2C+M">Martina Gerbino</a>, <a href="/search/hep-ph?searchtype=author&query=Ghosh%2C+S">Subhajit Ghosh</a>, <a href="/search/hep-ph?searchtype=author&query=Ghosh%2C+T">Tathagata Ghosh</a>, <a href="/search/hep-ph?searchtype=author&query=Grohs%2C+E">Evan Grohs</a>, <a href="/search/hep-ph?searchtype=author&query=Han%2C+T">Tao Han</a>, <a href="/search/hep-ph?searchtype=author&query=Hannestad%2C+S">Steen Hannestad</a>, <a href="/search/hep-ph?searchtype=author&query=Hostert%2C+M">Matheus Hostert</a>, <a href="/search/hep-ph?searchtype=author&query=Huber%2C+P">Patrick Huber</a>, <a href="/search/hep-ph?searchtype=author&query=Hyde%2C+J">Jeffrey Hyde</a>, <a href="/search/hep-ph?searchtype=author&query=Kelly%2C+K+J">Kevin J. Kelly</a>, <a href="/search/hep-ph?searchtype=author&query=Kling%2C+F">Felix Kling</a>, <a href="/search/hep-ph?searchtype=author&query=Liu%2C+Z">Zhen Liu</a> , et al. (9 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="2203.01955v1-abstract-short" style="display: inline;"> Neutrinos are the Standard Model (SM) particles which we understand the least, often due to how weakly they interact with the other SM particles. Beyond this, very little is known about interactions among the neutrinos, i.e., their self-interactions. The SM predicts neutrino self-interactions at a level beyond any current experimental capabilities, leaving open the possibility for beyond-the-SM in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.01955v1-abstract-full').style.display = 'inline'; document.getElementById('2203.01955v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.01955v1-abstract-full" style="display: none;"> Neutrinos are the Standard Model (SM) particles which we understand the least, often due to how weakly they interact with the other SM particles. Beyond this, very little is known about interactions among the neutrinos, i.e., their self-interactions. The SM predicts neutrino self-interactions at a level beyond any current experimental capabilities, leaving open the possibility for beyond-the-SM interactions across many energy scales. In this white paper, we review the current knowledge of neutrino self-interactions from a vast array of probes, from cosmology, to astrophysics, to the laboratory. We also discuss theoretical motivations for such self-interactions, including neutrino masses and possible connections to dark matter. Looking forward, we discuss the capabilities of searches in the next generation and beyond, highlighting the possibility of future discovery of this beyond-the-SM physics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.01955v1-abstract-full').style.display = 'none'; document.getElementById('2203.01955v1-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </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">Editors: Nikita Blinov, Mauricio Bustamante, Kevin J. Kelly, Yue Zhang. 29 pages, 16 figures, plus references. Contribution to Snowmass 2021</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> CERN-TH-2022-024, DESY-22-035, FERMILAB-PUB-22-099-T </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physics of the Dark Universe Volume 42, December 2023, 101267 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.06215">arXiv:2102.06215</a> <span> [<a href="https://arxiv.org/pdf/2102.06215">pdf</a>, <a href="https://arxiv.org/format/2102.06215">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="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/10.1088/1475-7516/2021/05/013">10.1088/1475-7516/2021/05/013 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Cosmological Evolution of Self-interacting Dark Matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Egana-Ugrinovic%2C+D">Daniel Egana-Ugrinovic</a>, <a href="/search/hep-ph?searchtype=author&query=Essig%2C+R">Rouven Essig</a>, <a href="/search/hep-ph?searchtype=author&query=Gift%2C+D">Daniel Gift</a>, <a href="/search/hep-ph?searchtype=author&query=LoVerde%2C+M">Marilena LoVerde</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="2102.06215v2-abstract-short" style="display: inline;"> We study the evolution of cosmological perturbations in dark-matter models with elastic and velocity-independent self interactions. Such interactions are imprinted in the matter-power spectrum as dark acoustic oscillations, which can be experimentally explored to determine the strength of the self scatterings. Models with self interactions have similarities to warm dark matter, as they lead to sup… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.06215v2-abstract-full').style.display = 'inline'; document.getElementById('2102.06215v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.06215v2-abstract-full" style="display: none;"> We study the evolution of cosmological perturbations in dark-matter models with elastic and velocity-independent self interactions. Such interactions are imprinted in the matter-power spectrum as dark acoustic oscillations, which can be experimentally explored to determine the strength of the self scatterings. Models with self interactions have similarities to warm dark matter, as they lead to suppression of power on small scales when the dark-matter velocity dispersion is sizable. Nonetheless, both the physical origin and the extent of the suppression differ for self-interacting dark matter from conventional warm dark matter, with a dark sound horizon controlling the reduction of power in the former case, and a free-streaming length in the latter. We thoroughly analyze these differences by performing computations of the linear power spectrum using a newly developed Boltzmann code. We find that while current Lyman-$伪$ data disfavor conventional warm dark matter with a mass less than 5.3 keV, when self interactions are included at their maximal value consistent with bounds from the Bullet Cluster, the limits are relaxed to 4.4 keV. Finally, we make use of our analysis to set novel bounds on light scalar singlet dark matter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.06215v2-abstract-full').style.display = 'none'; document.getElementById('2102.06215v2-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> 20 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </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">30 pages, 7 figures, 5 appendices</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.11830">arXiv:2012.11830</a> <span> [<a href="https://arxiv.org/pdf/2012.11830">pdf</a>, <a href="https://arxiv.org/format/2012.11830">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="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.104.063523">10.1103/PhysRevD.104.063523 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Self-interacting neutrinos, the Hubble parameter tension, and the Cosmic Microwave Background </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Brinckmann%2C+T">Thejs Brinckmann</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+J+H">Jae Hyeok Chang</a>, <a href="/search/hep-ph?searchtype=author&query=LoVerde%2C+M">Marilena LoVerde</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="2012.11830v2-abstract-short" style="display: inline;"> We perform a comprehensive study of cosmological constraints on non-standard neutrino self-interactions using cosmic microwave background (CMB) and baryon acoustic oscillation data. We consider different scenarios for neutrino self-interactions distinguished by the fraction of neutrino states allowed to participate in self-interactions and how the relativistic energy density, N$_{\textrm{eff}}$, i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.11830v2-abstract-full').style.display = 'inline'; document.getElementById('2012.11830v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.11830v2-abstract-full" style="display: none;"> We perform a comprehensive study of cosmological constraints on non-standard neutrino self-interactions using cosmic microwave background (CMB) and baryon acoustic oscillation data. We consider different scenarios for neutrino self-interactions distinguished by the fraction of neutrino states allowed to participate in self-interactions and how the relativistic energy density, N$_{\textrm{eff}}$, is allowed to vary. Specifically, we study cases in which: all neutrino states self-interact and N$_{\textrm{eff}}$ varies; two species free-stream, which we show alleviates tension with laboratory constraints, while the energy in the additional interacting states varies; and a variable fraction of neutrinos self-interact with either the total N$_{\textrm{eff}}$ fixed to the Standard Model value or allowed to vary. In no case do we find compelling evidence for new neutrino interactions or non-standard values of N$_{\textrm{eff}}$. In several cases we find additional modes with neutrino decoupling occurring at lower redshifts $z_{\textrm{dec}} \sim 10^{3-4}$. We do a careful analysis to examine whether new neutrino self-interactions solve or alleviate the so-called $H_0$ tension and find that, when all Planck 2018 CMB temperature and polarization data is included, none of these examples ease the tension more than allowing a variable N$_{\textrm{eff}}$ comprised of free-streaming particles. Although we focus on neutrino interactions, these constraints are applicable to any light relic particle. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.11830v2-abstract-full').style.display = 'none'; document.getElementById('2012.11830v2-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 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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">44 pages, 6 tables, 13 figures, 12 appendix figures. Matches accepted version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> YITP-SB-2020-40 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 104, 063523 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.11106">arXiv:1909.11106</a> <span> [<a href="https://arxiv.org/pdf/1909.11106">pdf</a>, <a href="https://arxiv.org/format/1909.11106">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 - Theory">hep-th</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="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/10.1103/PhysRevD.101.103502">10.1103/PhysRevD.101.103502 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Trans-Planckian Censorship and Inflationary Cosmology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Bedroya%2C+A">Alek Bedroya</a>, <a href="/search/hep-ph?searchtype=author&query=Brandenberger%2C+R">Robert Brandenberger</a>, <a href="/search/hep-ph?searchtype=author&query=Loverde%2C+M">Marilena Loverde</a>, <a href="/search/hep-ph?searchtype=author&query=Vafa%2C+C">Cumrun Vafa</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="1909.11106v3-abstract-short" style="display: inline;"> We study the implications of the recently proposed Trans-Planckian Censorship Conjecture (TCC) for early universe cosmology and in particular inflationary cosmology. The TCC leads to the conclusion that if we want inflationary cosmology to provide a successful scenario for cosmological structure formation, the energy scale of inflation has to be lower than $10^9$ GeV. Demanding the correct amplitu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.11106v3-abstract-full').style.display = 'inline'; document.getElementById('1909.11106v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.11106v3-abstract-full" style="display: none;"> We study the implications of the recently proposed Trans-Planckian Censorship Conjecture (TCC) for early universe cosmology and in particular inflationary cosmology. The TCC leads to the conclusion that if we want inflationary cosmology to provide a successful scenario for cosmological structure formation, the energy scale of inflation has to be lower than $10^9$ GeV. Demanding the correct amplitude of the cosmological perturbations then forces the generalized slow-roll parameter $蔚$ of the model to be very small ($<10^{-31}$). This leads to the prediction of a negligible amplitude of primordial gravitational waves. For slow-roll inflation models, it also leads to severe fine tuning of initial conditions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.11106v3-abstract-full').style.display = 'none'; document.getElementById('1909.11106v3-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </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 pages, 1 figure</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 101, 103502 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.04763">arXiv:1903.04763</a> <span> [<a href="https://arxiv.org/pdf/1903.04763">pdf</a>, <a href="https://arxiv.org/format/1903.04763">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="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Messengers from the Early Universe: Cosmic Neutrinos and Other Light Relics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Green%2C+D">Daniel Green</a>, <a href="/search/hep-ph?searchtype=author&query=Amin%2C+M+A">Mustafa A. Amin</a>, <a href="/search/hep-ph?searchtype=author&query=Meyers%2C+J">Joel Meyers</a>, <a href="/search/hep-ph?searchtype=author&query=Wallisch%2C+B">Benjamin Wallisch</a>, <a href="/search/hep-ph?searchtype=author&query=Abazajian%2C+K+N">Kevork N. Abazajian</a>, <a href="/search/hep-ph?searchtype=author&query=Abidi%2C+M">Muntazir Abidi</a>, <a href="/search/hep-ph?searchtype=author&query=Adshead%2C+P">Peter Adshead</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmed%2C+Z">Zeeshan Ahmed</a>, <a href="/search/hep-ph?searchtype=author&query=Ansarinejad%2C+B">Behzad Ansarinejad</a>, <a href="/search/hep-ph?searchtype=author&query=Armstrong%2C+R">Robert Armstrong</a>, <a href="/search/hep-ph?searchtype=author&query=Baccigalupi%2C+C">Carlo Baccigalupi</a>, <a href="/search/hep-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/hep-ph?searchtype=author&query=Barron%2C+D">Darcy Barron</a>, <a href="/search/hep-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/hep-ph?searchtype=author&query=Baumann%2C+D">Daniel Baumann</a>, <a href="/search/hep-ph?searchtype=author&query=Bechtol%2C+K">Keith Bechtol</a>, <a href="/search/hep-ph?searchtype=author&query=Bennett%2C+C">Charles Bennett</a>, <a href="/search/hep-ph?searchtype=author&query=Benson%2C+B">Bradford Benson</a>, <a href="/search/hep-ph?searchtype=author&query=Beutler%2C+F">Florian Beutler</a>, <a href="/search/hep-ph?searchtype=author&query=Bischoff%2C+C">Colin Bischoff</a>, <a href="/search/hep-ph?searchtype=author&query=Bleem%2C+L">Lindsey Bleem</a>, <a href="/search/hep-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/hep-ph?searchtype=author&query=Borrill%2C+J">Julian Borrill</a>, <a href="/search/hep-ph?searchtype=author&query=Buckley-Geer%2C+E">Elizabeth Buckley-Geer</a>, <a href="/search/hep-ph?searchtype=author&query=Burgess%2C+C">Cliff Burgess</a> , et al. (114 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="1903.04763v1-abstract-short" style="display: inline;"> The hot dense environment of the early universe is known to have produced large numbers of baryons, photons, and neutrinos. These extreme conditions may have also produced other long-lived species, including new light particles (such as axions or sterile neutrinos) or gravitational waves. The gravitational effects of any such light relics can be observed through their unique imprint in the cosmic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.04763v1-abstract-full').style.display = 'inline'; document.getElementById('1903.04763v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.04763v1-abstract-full" style="display: none;"> The hot dense environment of the early universe is known to have produced large numbers of baryons, photons, and neutrinos. These extreme conditions may have also produced other long-lived species, including new light particles (such as axions or sterile neutrinos) or gravitational waves. The gravitational effects of any such light relics can be observed through their unique imprint in the cosmic microwave background (CMB), the large-scale structure, and the primordial light element abundances, and are important in determining the initial conditions of the universe. We argue that future cosmological observations, in particular improved maps of the CMB on small angular scales, can be orders of magnitude more sensitive for probing the thermal history of the early universe than current experiments. These observations offer a unique and broad discovery space for new physics in the dark sector and beyond, even when its effects would not be visible in terrestrial experiments or in astrophysical environments. A detection of an excess light relic abundance would be a clear indication of new physics and would provide the first direct information about the universe between the times of reheating and neutrino decoupling one second later. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.04763v1-abstract-full').style.display = 'none'; document.getElementById('1903.04763v1-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 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </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">5 pages + references; 1 figure; science white paper submitted to the Astro2020 decadal survey</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1903.03689">arXiv:1903.03689</a> <span> [<a href="https://arxiv.org/pdf/1903.03689">pdf</a>, <a href="https://arxiv.org/format/1903.03689">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="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Neutrino Mass from Cosmology: Probing Physics Beyond the Standard Model </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Dvorkin%2C+C">Cora Dvorkin</a>, <a href="/search/hep-ph?searchtype=author&query=Gerbino%2C+M">Martina Gerbino</a>, <a href="/search/hep-ph?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/hep-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/hep-ph?searchtype=author&query=Bird%2C+S">Simeon Bird</a>, <a href="/search/hep-ph?searchtype=author&query=Rivero%2C+A+D">Ana Diaz Rivero</a>, <a href="/search/hep-ph?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/hep-ph?searchtype=author&query=Fuller%2C+G">George Fuller</a>, <a href="/search/hep-ph?searchtype=author&query=Lattanzi%2C+M">Massimiliano Lattanzi</a>, <a href="/search/hep-ph?searchtype=author&query=Loverde%2C+M">Marilena Loverde</a>, <a href="/search/hep-ph?searchtype=author&query=Mu%C3%B1oz%2C+J+B">Julian B. Mu帽oz</a>, <a href="/search/hep-ph?searchtype=author&query=Sherwin%2C+B">Blake Sherwin</a>, <a href="/search/hep-ph?searchtype=author&query=Slosar%2C+A">An啪e Slosar</a>, <a href="/search/hep-ph?searchtype=author&query=Villaescusa-Navarro%2C+F">Francisco Villaescusa-Navarro</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="1903.03689v1-abstract-short" style="display: inline;"> Recent advances in cosmic observations have brought us to the verge of discovery of the absolute scale of neutrino masses. Nonzero neutrino masses are known evidence of new physics beyond the Standard Model. Our understanding of the clustering of matter in the presence of massive neutrinos has significantly improved over the past decade, yielding cosmological constraints that are tighter than any… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.03689v1-abstract-full').style.display = 'inline'; document.getElementById('1903.03689v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1903.03689v1-abstract-full" style="display: none;"> Recent advances in cosmic observations have brought us to the verge of discovery of the absolute scale of neutrino masses. Nonzero neutrino masses are known evidence of new physics beyond the Standard Model. Our understanding of the clustering of matter in the presence of massive neutrinos has significantly improved over the past decade, yielding cosmological constraints that are tighter than any laboratory experiment, and which will improve significantly over the next decade, resulting in a guaranteed detection of the absolute neutrino mass scale. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1903.03689v1-abstract-full').style.display = 'none'; document.getElementById('1903.03689v1-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> 8 March, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2019. </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">Science White Paper submitted to the US Astro2020 Decadal Survey</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1902.01055">arXiv:1902.01055</a> <span> [<a href="https://arxiv.org/pdf/1902.01055">pdf</a>, <a href="https://arxiv.org/format/1902.01055">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="Astrophysics of Galaxies">astro-ph.GA</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 - 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"> Probing the Fundamental Nature of Dark Matter with the Large Synoptic Survey Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Drlica-Wagner%2C+A">Alex Drlica-Wagner</a>, <a href="/search/hep-ph?searchtype=author&query=Mao%2C+Y">Yao-Yuan Mao</a>, <a href="/search/hep-ph?searchtype=author&query=Adhikari%2C+S">Susmita Adhikari</a>, <a href="/search/hep-ph?searchtype=author&query=Armstrong%2C+R">Robert Armstrong</a>, <a href="/search/hep-ph?searchtype=author&query=Banerjee%2C+A">Arka Banerjee</a>, <a href="/search/hep-ph?searchtype=author&query=Banik%2C+N">Nilanjan Banik</a>, <a href="/search/hep-ph?searchtype=author&query=Bechtol%2C+K">Keith Bechtol</a>, <a href="/search/hep-ph?searchtype=author&query=Bird%2C+S">Simeon Bird</a>, <a href="/search/hep-ph?searchtype=author&query=Boddy%2C+K+K">Kimberly K. Boddy</a>, <a href="/search/hep-ph?searchtype=author&query=Bonaca%2C+A">Ana Bonaca</a>, <a href="/search/hep-ph?searchtype=author&query=Bovy%2C+J">Jo Bovy</a>, <a href="/search/hep-ph?searchtype=author&query=Buckley%2C+M+R">Matthew R. Buckley</a>, <a href="/search/hep-ph?searchtype=author&query=Bulbul%2C+E">Esra Bulbul</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+C">Chihway Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Chapline%2C+G">George Chapline</a>, <a href="/search/hep-ph?searchtype=author&query=Cohen-Tanugi%2C+J">Johann Cohen-Tanugi</a>, <a href="/search/hep-ph?searchtype=author&query=Cuoco%2C+A">Alessandro Cuoco</a>, <a href="/search/hep-ph?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/hep-ph?searchtype=author&query=Dawson%2C+W+A">William A. Dawson</a>, <a href="/search/hep-ph?searchtype=author&query=Rivero%2C+A+D">Ana D铆az Rivero</a>, <a href="/search/hep-ph?searchtype=author&query=Dvorkin%2C+C">Cora Dvorkin</a>, <a href="/search/hep-ph?searchtype=author&query=Erkal%2C+D">Denis Erkal</a>, <a href="/search/hep-ph?searchtype=author&query=Fassnacht%2C+C+D">Christopher D. Fassnacht</a>, <a href="/search/hep-ph?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">Juan Garc铆a-Bellido</a>, <a href="/search/hep-ph?searchtype=author&query=Giannotti%2C+M">Maurizio Giannotti</a> , et al. (75 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="1902.01055v2-abstract-short" style="display: inline;"> Astrophysical and cosmological observations currently provide the only robust, empirical measurements of dark matter. Future observations with Large Synoptic Survey Telescope (LSST) will provide necessary guidance for the experimental dark matter program. This white paper represents a community effort to summarize the science case for studying the fundamental physics of dark matter with LSST. We d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.01055v2-abstract-full').style.display = 'inline'; document.getElementById('1902.01055v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1902.01055v2-abstract-full" style="display: none;"> Astrophysical and cosmological observations currently provide the only robust, empirical measurements of dark matter. Future observations with Large Synoptic Survey Telescope (LSST) will provide necessary guidance for the experimental dark matter program. This white paper represents a community effort to summarize the science case for studying the fundamental physics of dark matter with LSST. We discuss how LSST will inform our understanding of the fundamental properties of dark matter, such as particle mass, self-interaction strength, non-gravitational couplings to the Standard Model, and compact object abundances. Additionally, we discuss the ways that LSST will complement other experiments to strengthen our understanding of the fundamental characteristics of dark matter. More information on the LSST dark matter effort can be found at https://lsstdarkmatter.github.io/ . <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1902.01055v2-abstract-full').style.display = 'none'; document.getElementById('1902.01055v2-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> 24 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 February, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2019. </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">96 pages, 22 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-19-048-A-AE </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1804.10180">arXiv:1804.10180</a> <span> [<a href="https://arxiv.org/pdf/1804.10180">pdf</a>, <a href="https://arxiv.org/format/1804.10180">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="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/10.1088/1475-7516/2018/06/044">10.1088/1475-7516/2018/06/044 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing Decoupling in Dark Sectors with the Cosmic Microwave Background </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Choi%2C+G">Gongjun Choi</a>, <a href="/search/hep-ph?searchtype=author&query=Chiang%2C+C">Chi-Ting Chiang</a>, <a href="/search/hep-ph?searchtype=author&query=LoVerde%2C+M">Marilena LoVerde</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="1804.10180v2-abstract-short" style="display: inline;"> The acoustic peaks in the angular power spectrum of cosmic microwave background (CMB) temperature and polarization anisotropies play an important role as a probe of the nature of new relativistic particles contributing to the radiation density in the early universe, parametrized by $螖N_{eff}$. The amplitude and phase of the acoustic oscillations provide information about whether the extra species… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.10180v2-abstract-full').style.display = 'inline'; document.getElementById('1804.10180v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1804.10180v2-abstract-full" style="display: none;"> The acoustic peaks in the angular power spectrum of cosmic microwave background (CMB) temperature and polarization anisotropies play an important role as a probe of the nature of new relativistic particles contributing to the radiation density in the early universe, parametrized by $螖N_{eff}$. The amplitude and phase of the acoustic oscillations provide information about whether the extra species are free-streaming particles, like neutrinos, or tightly-coupled, like the photons, during eras probed by the CMB. On the other hand, some extensions of the Standard Model produce new relativistic particles that decouple from their own non-gravitational interactions after neutrinos, but prior to photons. We study the signature of new relativistic species that decouple during this intermediate epoch. We argue that the decoupling species will cause a scale-dependent change in the amplitude and phase shift of the acoustic oscillations, different from the usual constant shifts on small scales. For intermediate decoupling times, the phase and amplitude shifts depend not only on $螖N_{eff}$ but the redshift $z_{dec,X}$ at which the new species decoupled. For $螖N_{eff} >0.334$, a Stage IV CMB experiment could determine $N_{eff}$ at the percent level and $z_{dec,X}$ at the $\sim 10\%$ level. For smaller values, $螖N_{eff}\sim 0.1$, constraints on $z_{dec,X}$ weaken but remain $\sim 20-50\%$ for $z_{dec,X} \sim \mathcal{O}(10^3-10^4)$. As an application, we study the contributions to $螖N_{eff}$ and determine the $z_{dec,X}$ values for simple implementations of the so-called $N$naturalness model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1804.10180v2-abstract-full').style.display = 'none'; document.getElementById('1804.10180v2-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 April, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2018. </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">29 pages + references, 7 figures, 3 tables; refs added, version accepted by JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> YITP-SB-18-09 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP06(2018)044 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.02743">arXiv:1610.02743</a> <span> [<a href="https://arxiv.org/pdf/1610.02743">pdf</a>, <a href="https://arxiv.org/format/1610.02743">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> <p class="title is-5 mathjax"> CMB-S4 Science Book, First Edition </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Abazajian%2C+K+N">Kevork N. Abazajian</a>, <a href="/search/hep-ph?searchtype=author&query=Adshead%2C+P">Peter Adshead</a>, <a href="/search/hep-ph?searchtype=author&query=Ahmed%2C+Z">Zeeshan Ahmed</a>, <a href="/search/hep-ph?searchtype=author&query=Allen%2C+S+W">Steven W. Allen</a>, <a href="/search/hep-ph?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/hep-ph?searchtype=author&query=Arnold%2C+K+S">Kam S. Arnold</a>, <a href="/search/hep-ph?searchtype=author&query=Baccigalupi%2C+C">Carlo Baccigalupi</a>, <a href="/search/hep-ph?searchtype=author&query=Bartlett%2C+J+G">James G. Bartlett</a>, <a href="/search/hep-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/hep-ph?searchtype=author&query=Benson%2C+B+A">Bradford A. Benson</a>, <a href="/search/hep-ph?searchtype=author&query=Bischoff%2C+C+A">Colin A. Bischoff</a>, <a href="/search/hep-ph?searchtype=author&query=Borrill%2C+J">Julian Borrill</a>, <a href="/search/hep-ph?searchtype=author&query=Buza%2C+V">Victor Buza</a>, <a href="/search/hep-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/hep-ph?searchtype=author&query=Caldwell%2C+R">Robert Caldwell</a>, <a href="/search/hep-ph?searchtype=author&query=Carlstrom%2C+J+E">John E. Carlstrom</a>, <a href="/search/hep-ph?searchtype=author&query=Chang%2C+C+L">Clarence L. Chang</a>, <a href="/search/hep-ph?searchtype=author&query=Crawford%2C+T+M">Thomas M. Crawford</a>, <a href="/search/hep-ph?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/hep-ph?searchtype=author&query=De+Bernardis%2C+F">Francesco De Bernardis</a>, <a href="/search/hep-ph?searchtype=author&query=de+Haan%2C+T">Tijmen de Haan</a>, <a href="/search/hep-ph?searchtype=author&query=Alighieri%2C+S+d+S">Sperello di Serego Alighieri</a>, <a href="/search/hep-ph?searchtype=author&query=Dunkley%2C+J">Joanna Dunkley</a>, <a href="/search/hep-ph?searchtype=author&query=Dvorkin%2C+C">Cora Dvorkin</a>, <a href="/search/hep-ph?searchtype=author&query=Errard%2C+J">Josquin Errard</a> , et al. (61 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="1610.02743v1-abstract-short" style="display: inline;"> This book lays out the scientific goals to be addressed by the next-generation ground-based cosmic microwave background experiment, CMB-S4, envisioned to consist of dedicated telescopes at the South Pole, the high Chilean Atacama plateau and possibly a northern hemisphere site, all equipped with new superconducting cameras. CMB-S4 will dramatically advance cosmological studies by crossing critical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.02743v1-abstract-full').style.display = 'inline'; document.getElementById('1610.02743v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.02743v1-abstract-full" style="display: none;"> This book lays out the scientific goals to be addressed by the next-generation ground-based cosmic microwave background experiment, CMB-S4, envisioned to consist of dedicated telescopes at the South Pole, the high Chilean Atacama plateau and possibly a northern hemisphere site, all equipped with new superconducting cameras. CMB-S4 will dramatically advance cosmological studies by crossing critical thresholds in the search for the B-mode polarization signature of primordial gravitational waves, in the determination of the number and masses of the neutrinos, in the search for evidence of new light relics, in constraining the nature of dark energy, and in testing general relativity on large scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.02743v1-abstract-full').style.display = 'none'; document.getElementById('1610.02743v1-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 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1412.4671">arXiv:1412.4671</a> <span> [<a href="https://arxiv.org/pdf/1412.4671">pdf</a>, <a href="https://arxiv.org/format/1412.4671">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="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> <p class="title is-5 mathjax"> Testing Inflation with Large Scale Structure: Connecting Hopes with Reality </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/hep-ph?searchtype=author&query=Alvarez%2C+M">Marcelo Alvarez</a>, <a href="/search/hep-ph?searchtype=author&query=Baldauf%2C+T">Tobias Baldauf</a>, <a href="/search/hep-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/hep-ph?searchtype=author&query=Dalal%2C+N">Neal Dalal</a>, <a href="/search/hep-ph?searchtype=author&query=de+Putter%2C+R">Roland de Putter</a>, <a href="/search/hep-ph?searchtype=author&query=Dor%C3%A9%2C+O">Olivier Dor茅</a>, <a href="/search/hep-ph?searchtype=author&query=Green%2C+D">Daniel Green</a>, <a href="/search/hep-ph?searchtype=author&query=Hirata%2C+C">Chris Hirata</a>, <a href="/search/hep-ph?searchtype=author&query=Huang%2C+Z">Zhiqi Huang</a>, <a href="/search/hep-ph?searchtype=author&query=Huterer%2C+D">Dragan Huterer</a>, <a href="/search/hep-ph?searchtype=author&query=Jeong%2C+D">Donghui Jeong</a>, <a href="/search/hep-ph?searchtype=author&query=Johnson%2C+M+C">Matthew C. Johnson</a>, <a href="/search/hep-ph?searchtype=author&query=Krause%2C+E">Elisabeth Krause</a>, <a href="/search/hep-ph?searchtype=author&query=Loverde%2C+M">Marilena Loverde</a>, <a href="/search/hep-ph?searchtype=author&query=Meyers%2C+J">Joel Meyers</a>, <a href="/search/hep-ph?searchtype=author&query=Meerburg%2C+P+D">P. Daniel Meerburg</a>, <a href="/search/hep-ph?searchtype=author&query=Senatore%2C+L">Leonardo Senatore</a>, <a href="/search/hep-ph?searchtype=author&query=Shandera%2C+S">Sarah Shandera</a>, <a href="/search/hep-ph?searchtype=author&query=Silverstein%2C+E">Eva Silverstein</a>, <a href="/search/hep-ph?searchtype=author&query=Slosar%2C+A">An啪e Slosar</a>, <a href="/search/hep-ph?searchtype=author&query=Smith%2C+K">Kendrick Smith</a>, <a href="/search/hep-ph?searchtype=author&query=Zaldarriaga%2C+M">Matias Zaldarriaga</a>, <a href="/search/hep-ph?searchtype=author&query=Assassi%2C+V">Valentin Assassi</a>, <a href="/search/hep-ph?searchtype=author&query=Braden%2C+J">Jonathan Braden</a>, <a href="/search/hep-ph?searchtype=author&query=Hajian%2C+A">Amir Hajian</a> , et al. (3 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="1412.4671v1-abstract-short" style="display: inline;"> The statistics of primordial curvature fluctuations are our window into the period of inflation, where these fluctuations were generated. To date, the cosmic microwave background has been the dominant source of information about these perturbations. Large scale structure is however from where drastic improvements should originate. In this paper, we explain the theoretical motivations for pursuing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4671v1-abstract-full').style.display = 'inline'; document.getElementById('1412.4671v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1412.4671v1-abstract-full" style="display: none;"> The statistics of primordial curvature fluctuations are our window into the period of inflation, where these fluctuations were generated. To date, the cosmic microwave background has been the dominant source of information about these perturbations. Large scale structure is however from where drastic improvements should originate. In this paper, we explain the theoretical motivations for pursuing such measurements and the challenges that lie ahead. In particular, we discuss and identify theoretical targets regarding the measurement of primordial non-Gaussianity. We argue that when quantified in terms of the local (equilateral) template amplitude $f_{\rm NL}^{\rm loc}$ ($f_{\rm NL}^{\rm eq}$), natural target levels of sensitivity are $螖f_{\rm NL}^{\rm loc, eq.} \simeq 1$. We highlight that such levels are within reach of future surveys by measuring 2-, 3- and 4-point statistics of the galaxy spatial distribution. This paper summarizes a workshop held at CITA (University of Toronto) on October 23-24, 2014. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1412.4671v1-abstract-full').style.display = 'none'; document.getElementById('1412.4671v1-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, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2014. </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 + references</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" 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