1
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Leane RK, Linden T. First Analysis of Jupiter in Gamma Rays and a New Search for Dark Matter. Phys Rev Lett 2023; 131:071001. [PMID: 37656854 DOI: 10.1103/physrevlett.131.071001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/24/2021] [Revised: 04/12/2023] [Accepted: 06/23/2023] [Indexed: 09/03/2023]
Abstract
We present the first dedicated γ-ray analysis of Jupiter, using 12 years of data from the Fermi Telescope. We find no robust evidence of γ-ray emission, and set upper limits of ∼10^{-9} GeV cm^{-2} s^{-1} on the Jovian γ-ray flux. We point out that Jupiter is an advantageous dark matter (DM) target due to its large surface area (compared with other solar system planets), and cool core temperature (compared with the Sun). These properties allow Jupiter to both capture and retain lighter DM, providing a complementary probe of sub-GeV DM. We therefore identify and perform a new search for DM-sourced γ-rays in Jupiter, where DM annihilates to long-lived particles, which can escape the Jovian surface and decay into γ rays. We consequently constrain DM-proton scattering cross sections as low as about 10^{-40} cm^{2}, showing Jupiter is up to 10 orders of magnitude more sensitive than direct detection. This sensitivity is reached under the assumption that the mediator decay length is sufficient to escape Jupiter, and the equilibrium between DM capture and annihilation; sensitivities can be lower depending on the DM model. Our work motivates follow-up studies with upcoming MeV telescopes such as AMEGO and e-ASTROGAM.
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Affiliation(s)
- Rebecca K Leane
- SLAC National Accelerator Laboratory, Stanford University, Stanford, California 94035, USA
| | - Tim Linden
- Stockholm University and The Oskar Klein Centre for Cosmoparticle Physics, Alba Nova, 10691 Stockholm, Sweden
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2
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Cappiello CV. Analytic Approach to Light Dark Matter Propagation. Phys Rev Lett 2023; 130:221001. [PMID: 37327432 DOI: 10.1103/physrevlett.130.221001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/01/2023] [Revised: 04/28/2023] [Accepted: 05/11/2023] [Indexed: 06/18/2023]
Abstract
If dark matter interacts too strongly with nuclei, it could be slowed to undetectable speeds in Earth's crust or atmosphere before reaching a detector. For sub-GeV dark matter, approximations appropriate for heavier dark matter fail, necessitating the use of computationally expensive simulations. We present a new, analytic approximation for modeling attenuation of light dark matter in Earth. We show that our approach agrees well with Monte Carlo results, and can be much faster at large cross sections. We use this method to reanalyze constraints on subdominant dark matter.
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Affiliation(s)
- Christopher V Cappiello
- Department of Physics, Engineering Physics, and Astronomy, Queen's University, Kingston, Ontario, K7N 3N6, Canada; Arthur B. McDonald Canadian Astroparticle Physics Research Institute, Kingston, Ontario, K7L 3N6, Canada; and Perimeter Institute for Theoretical Physics, Waterloo, Ontario, N2L 2Y5, Canada
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3
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Frumkin R, Kuflik E, Lavie I, Silverwater T. Roadmap to Thermal Dark Matter beyond the Weakly Interacting Dark Matter Unitarity Bound. Phys Rev Lett 2023; 130:171001. [PMID: 37172246 DOI: 10.1103/physrevlett.130.171001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/26/2022] [Revised: 01/30/2023] [Accepted: 03/31/2023] [Indexed: 05/14/2023]
Abstract
We study the general properties of the freeze-out of a thermal relic. We give analytic estimates of the relic abundance for an arbitrary freeze-out process, showing when instantaneous freeze-out is appropriate and how it can be corrected when freeze-out is slow. This is used to generalize the relationship between the dark matter mass and coupling that matches the observed abundance. The result encompasses well-studied particular examples, such as weakly interacting massive particles (WIMPs), strongly interacting massive particles, coannihilation, coscattering, inverse decays, and forbidden channels, and generalizes beyond them. In turn, this gives an approximate perturbative unitarity bound on the dark matter mass for an arbitrary thermal freeze-out process. We show that going beyond the maximal masses allowed for freeze-out via dark matter self-annihilations [WIMP-like, m_{DM}≫O(100 TeV)] predicts that there are nearly degenerate states with the dark matter and that the dark matter is generically metastable.
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Affiliation(s)
- Ronny Frumkin
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - Eric Kuflik
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - Itay Lavie
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - Tal Silverwater
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
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4
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Frumkin R, Hochberg Y, Kuflik E, Murayama H. Thermal Dark Matter from Freeze-Out of Inverse Decays. Phys Rev Lett 2023; 130:121001. [PMID: 37027852 DOI: 10.1103/physrevlett.130.121001] [Citation(s) in RCA: 1] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/22/2022] [Revised: 12/26/2022] [Accepted: 02/14/2023] [Indexed: 06/19/2023]
Abstract
We propose a new thermal dark matter candidate whose abundance is determined by the freeze-out of inverse decays. The relic abundance depends parametrically only on a decay width, while matching the observed value requires that the coupling determining the width-and the width itself-should be exponentially small. The dark matter is therefore very weakly coupled to the standard model, evading conventional searches. This inverse decay dark matter can be discovered by searching for the long-lived particle that decays into the dark matter at future planned experiments.
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Affiliation(s)
- Ronny Frumkin
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - Yonit Hochberg
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - Eric Kuflik
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - Hitoshi Murayama
- Ernest Orlando Lawrence Berkeley National Laboratory, University of California, Berkeley, California 94720, USA
- Department of Physics, University of California, Berkeley, California 94720, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Kashiwa 277-8583, Japan
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5
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Giovanetti C, Lisanti M, Liu H, Ruderman JT. Joint Cosmic Microwave Background and Big Bang Nucleosynthesis Constraints on Light Dark Sectors with Dark Radiation. Phys Rev Lett 2022; 129:021302. [PMID: 35867453 DOI: 10.1103/physrevlett.129.021302] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/17/2021] [Revised: 03/08/2022] [Accepted: 06/03/2022] [Indexed: 06/15/2023]
Abstract
Dark sectors provide a compelling theoretical framework for thermally producing sub-GeV dark matter, and motivate an expansive new accelerator and direct-detection experimental program. We demonstrate the power of constraining such dark sectors using the measured effective number of neutrino species, N_{eff}, from the cosmic microwave background (CMB) and primordial elemental abundances from big bang nucleosynthesis. As a concrete example, we consider a dark matter particle of arbitrary spin that interacts with the standard model via a massive dark photon, accounting for an arbitrary number of light degrees of freedom in the dark sector. We exclude dark matter masses below ∼4 MeV at 95% confidence for all dark matter spins and dark photon masses. These bounds hold regardless of additional new light, inert degrees of freedom in the dark sector, and for dark matter-electron scattering cross sections many orders of magnitude below current experimental constraints. The strength of these constraints will only continue to improve with future CMB experiments.
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Affiliation(s)
- Cara Giovanetti
- Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, New York 10003, USA
| | - Mariangela Lisanti
- Department of Physics, Princeton University, Princeton, New Jersey 08544, USA
- Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Ave, New York, New York 10010, USA
| | - Hongwan Liu
- Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, New York 10003, USA
- Department of Physics, Princeton University, Princeton, New Jersey 08544, USA
| | - Joshua T Ruderman
- Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, New York 10003, USA
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6
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Abstract
Identifying the nature of dark matter (DM) has long been a pressing question for particle physics. In the face of ever-more-powerful exclusions and null results from large-exposure searches for TeV-scale DM interacting with nuclei, a significant amount of attention has shifted to lighter (sub-GeV) DM candidates. Direct detection of the light DM in our galaxy by observing DM scattering off a target system requires new approaches compared to prior searches. Lighter DM particles have less available kinetic energy, and achieving a kinematic match between DM and the target mandates the proper treatment of collective excitations in condensed matter systems, such as charged quasiparticles or phonons. In this context, the condensed matter physics of the target material is crucial, necessitating an interdisciplinary approach. In this review, we provide a self-contained introduction to direct detection of keV-GeV DM with condensed matter systems. We give a brief survey of DM models and basics of condensed matter, while the bulk of the review deals with the theoretical treatment of DM-nucleon and DM-electron interactions. We also review recent experimental developments in detector technology, and conclude with an outlook for the field of sub-GeV DM detection over the next decade.
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Affiliation(s)
- Yonatan Kahn
- Department of Physics, University of Illinois at Urbana-Champaign, Urbana, IL 61801, United States of America
- Illinois Center for Advanced Studies of the Universe, University of Illinois at Urbana-Champaign, Urbana, IL 61801, United States of America
| | - Tongyan Lin
- Department of Physics, University of California, San Diego, CA 92093, United States of America
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7
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Tsai YD, McGehee R, Murayama H. Resonant Self-Interacting Dark Matter from Dark QCD. Phys Rev Lett 2022; 128:172001. [PMID: 35570435 DOI: 10.1103/physrevlett.128.172001] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/02/2021] [Revised: 01/07/2022] [Accepted: 03/10/2022] [Indexed: 06/15/2023]
Abstract
We present new models utilizing QCD-like dark sectors to resolve small-scale structure problems. These models of resonant self-interacting dark matter in a dark sector with QCD are based on analogies to the meson spectra in standard model QCD. We introduce a simple model that realizes resonant self-interaction (analogous to the ϕ-K-K system) and thermal freeze-out, in which dark mesons are made of two light quarks. We also consider asymmetric dark matter composed of heavy and light dark quarks to realize a resonant self-interaction (analogous to the ϒ(4S)-B-B system) and discuss the experimental probes of both setups. Finally, we comment on the possible resonant self-interactions already built into SIMP and ELDER mechanisms while using lattice results to determine feasibility.
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Affiliation(s)
- Yu-Dai Tsai
- Department of Physics and Astronomy, University of California, Irvine, California 92697-4575, USA
- Fermilab, Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
- University of Chicago, Kavli Institute for Cosmological Physics, Chicago, Illinois 60637, USA
| | - Robert McGehee
- Department of Physics, University of California, Berkeley, California 94720, USA
- Ernest Orlando Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
| | - Hitoshi Murayama
- Department of Physics, University of California, Berkeley, California 94720, USA
- Ernest Orlando Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Kashiwa 277-8583, Japan
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8
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Rogers KK, Dvorkin C, Peiris HV. Limits on the Light Dark Matter-Proton Cross Section from Cosmic Large-Scale Structure. Phys Rev Lett 2022; 128:171301. [PMID: 35570432 DOI: 10.1103/physrevlett.128.171301] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/03/2021] [Accepted: 03/24/2022] [Indexed: 06/15/2023]
Abstract
We set the strongest limits to date on the velocity-independent dark matter (DM)-proton cross section σ for DM masses m=10 keV to 100 GeV, using large-scale structure traced by the Lyman-alpha forest: e.g., a 95% lower limit σ<6×10^{-30} cm^{2}, for m=100 keV. Our results complement direct detection, which has limited sensitivity to sub-GeV DM. We use an emulator of cosmological simulations, combined with data from the smallest cosmological scales used to date, to model and search for the imprint of primordial DM-proton collisions. Cosmological bounds are improved by up to a factor of 25.
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Affiliation(s)
- Keir K Rogers
- Dunlap Institute for Astronomy and Astrophysics, University of Toronto, 50 St. George Street, Toronto, Ontario M5S 3H4, Canada
| | - Cora Dvorkin
- Department of Physics, Harvard University, 17 Oxford Street, Cambridge, Massachusetts 02138, USA
| | - Hiranya V Peiris
- Department of Physics and Astronomy, University College London, Gower Street, London WC1E 6BT, United Kingdom
- Oskar Klein Centre for Cosmoparticle Physics, Department of Physics, Stockholm University, AlbaNova University Center, Stockholm 10691, Sweden
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9
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Kamada A, Kuwahara T. LHC lifetime frontier and visible decay searches in composite asymmetric dark matter models. J High Energy Phys 2022; 2022:176. [PMID: 35370396 PMCID: PMC8959273 DOI: 10.1007/jhep03(2022)176] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Key Words] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 12/14/2021] [Revised: 03/17/2022] [Accepted: 03/22/2022] [Indexed: 06/14/2023]
Abstract
The LHC lifetime frontier will probe dark sector in near future, and the visible decay searches at fixed-target experiments have been exploring dark sector. Composite asymmetric dark matter with dark photon portal is a promising framework explaining the coincidence problem between dark matter and visible matter. Dark strong dynamics provides rich structure in the dark sector: the lightest dark nucleon is the dark matter, while strong annihilation into dark pions depletes the symmetric components of the dark matter. Dark photons alleviate cosmological problems. Meanwhile, dark photons make dark hadrons long-lived in terrestrial experiments. Moreover, the dark hadrons are produced through the very same dark photon. In this study, we discuss the visible decay searches for composite asymmetric dark matter models. For a few GeV dark nucleons, the LHC lifetime frontier, MATHUSLA and FASER, has a potential to discover their decay when kinetic mixing angle of dark photon is ϵ ≳ 10 -4. On the other hand, fixed-target experiments, in particular SeaQuest, will have a great sensitivity to dark pions with a mass below GeV and with kinetic mixing ϵ ≳ 10 -4 in addition to the LHC lifetime frontier. These projected sensitivities to dark hadrons in dark photon parameter space are comparable with the future sensitivities of dark photon searches, such as Belle-II and LHCb.
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Affiliation(s)
- Ayuki Kamada
- Institute of Theoretical Physics, Faculty of Physics, University of Warsaw, ul. Pasteura 5, PL–02–093 Warsaw, Poland
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, The University of Tokyo, Kashiwa, 277-8583 Japan
- Center for Theoretical Physics of the Universe, Institute for Basic Science (IBS), Daejeon, 34126 Korea
| | - Takumi Kuwahara
- Center for Theoretical Physics of the Universe, Institute for Basic Science (IBS), Daejeon, 34126 Korea
- Center for High Energy Physics, Peking University, Beijing, 100871 China
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10
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Reichert M, Wang ZW. Gravitational Waves from dark composite dynamics. EPJ Web Conf 2022. [DOI: 10.1051/epjconf/202227408003] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 12/24/2022] Open
Abstract
We discuss the stochastic gravitational-wave spectrum from dark confinement and chiral phase transitions in the early Universe. Specifically, we look at pure Yang-Mills theory for an arbitrary number of colours as well as SU(3) with quarks in different representations. We utilise thermodynamic Lattice data and map it to effective models, such as the Polyakov-loop and the PNJL model. This allows us to compute gravitational-wave parameters and the corresponding gravitational-wave signal. We compare the signal to future gravitational-wave observatories such as the Big Bang Observer and DECIGO.
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11
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Bringmann T, Depta PF, Hufnagel M, Ruderman JT, Schmidt-Hoberg K. Dark Matter from Exponential Growth. Phys Rev Lett 2021; 127:191802. [PMID: 34797149 DOI: 10.1103/physrevlett.127.191802] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/25/2021] [Revised: 08/20/2021] [Accepted: 09/14/2021] [Indexed: 06/13/2023]
Abstract
We propose a novel mechanism for the production of dark matter (DM) from a thermal bath based on the idea that DM particles χ can transform heat bath particles ψ: χψ→χχ. For a small initial abundance of χ, this leads to an exponential growth of the DM number density in close analogy to other familiar exponential growth processes in nature. We demonstrate that this mechanism complements freeze-in and freeze-out production in a generic way, opening new parameter space to explain the observed DM abundance, and we discuss observational prospects for such scenarios.
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Affiliation(s)
- Torsten Bringmann
- Department of Physics, University of Oslo, Box 1048, N-0316 Oslo, Norway
| | - Paul Frederik Depta
- Deutsches Elektronen-Synchrotron DESY, Notkestraße 85, D-22607 Hamburg, Germany
| | - Marco Hufnagel
- Service de Physique Théorique, Université Libre de Bruxelles, Boulevard du Triomphe, CP225, B-1050 Brussels, Belgium
| | - Joshua T Ruderman
- Deutsches Elektronen-Synchrotron DESY, Notkestraße 85, D-22607 Hamburg, Germany
- Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, New York 10003, USA
- Kavli Institute for Theoretical Physics, University of California, Santa Barbara, California 93106, USA
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
| | - Kai Schmidt-Hoberg
- Deutsches Elektronen-Synchrotron DESY, Notkestraße 85, D-22607 Hamburg, Germany
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12
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Xing CY, Zhu SH. Dark Matter Freeze-Out via Catalyzed Annihilation. Phys Rev Lett 2021; 127:061101. [PMID: 34420347 DOI: 10.1103/physrevlett.127.061101] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/20/2021] [Revised: 05/31/2021] [Accepted: 07/12/2021] [Indexed: 06/13/2023]
Abstract
We present a new paradigm of dark matter freeze-out, where the annihilation of dark matter particles is catalyzed. We discuss in detail the regime in which the depletion of dark matter proceeds via 2χ→2A^{'} and 3A^{'}→2χ processes, where χ and A^{'} denote dark matter and the catalyst, respectively. In this regime, the dark matter number density is depleted polynomially rather than exponentially (Boltzmann suppression) as in classical weakly interacting massive particles and strongly interacting massive particles. The paradigm applies for a secluded weakly interacting dark sector with dark matter in the MeV-TeV mass range. The catalyzed annihilation paradigm is compatible with cosmic microwave background and big bang nucleosynthesis constraints, with enhanced indirect detection signals.
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Affiliation(s)
- Chuan-Yang Xing
- Department of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China
| | - Shou-Hua Zhu
- Department of Physics and State Key Laboratory of Nuclear Physics and Technology, Peking University, Beijing 100871, China
- Collaborative Innovation Center of Quantum Matter, Beijing, 100871, China
- Center for High Energy Physics, Peking University, Beijing 100871, China
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13
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Tsai YD, deNiverville P, Liu MX. Dark Photon and Muon g-2 Inspired Inelastic Dark Matter Models at the High-Energy Intensity Frontier. Phys Rev Lett 2021; 126:181801. [PMID: 34018792 DOI: 10.1103/physrevlett.126.181801] [Citation(s) in RCA: 3] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 01/01/2020] [Revised: 10/19/2020] [Accepted: 03/11/2021] [Indexed: 06/12/2023]
Abstract
We study hidden-sector particles at past (CERN-Hamburg-Amsterdam-Rome-Moscow Collaboration and NuCal), present (NA62, SeaQuest, and DarkQuest), and future (LongQuest) experiments at the high-energy intensity frontier. We focus on exploring the minimal vector portal and the next-to-minimal models in which the productions and decays are decoupled. These next-to-minimal models have mostly been devised to explain experimental anomalies while avoiding existing constraints. We demonstrate that proton fixed-target experiments provide one of the most powerful probes for the MeV to few GeV mass range of these models, using inelastic dark matter (iDM) as an example. We consider an iDM model with a small mass splitting that yields the observed dark matter relic abundance, and a scenario with a sizable mass splitting that can also explain the muon g-2 anomaly. We set strong limits based on the CERN-Hamburg-Amsterdam-Rome-Moscow Collaboration and NuCal experiments, which come close to excluding iDM as a full-abundance thermal dark matter candidate in the MeV to GeV mass range. We also make projections based on NA62, SeaQuest, and DarkQuest and update the constraints of the minimal dark photon parameter space. We find that NuCal sets the only existing constraint in ε∼10^{-8}-10^{-4} regime, reaching ∼800 MeV in dark photon mass due to the resonant enhancement of proton bremsstrahlung production. These studies also motivate LongQuest, a three-stage retooling of the SeaQuest experiment with short (≲5 m), medium (∼5 m), and long (≳35 m) baseline tracking stations and detectors as a multipurpose machine to explore new physics.
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Affiliation(s)
- Yu-Dai Tsai
- Fermilab, Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
- Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA
| | - Patrick deNiverville
- Center for Theoretical Physics of the Universe, IBS, Daejeon 34126, Korea
- Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
| | - Ming Xiong Liu
- Los Alamos National Laboratory, Los Alamos, New Mexico 87545, USA
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14
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Leane RK, Smirnov J. Exoplanets as Sub-GeV Dark Matter Detectors. Phys Rev Lett 2021; 126:161101. [PMID: 33961477 DOI: 10.1103/physrevlett.126.161101] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/08/2020] [Revised: 11/28/2020] [Accepted: 03/15/2021] [Indexed: 06/12/2023]
Abstract
We present exoplanets as new targets to discover dark matter (DM). Throughout the Milky Way, DM can scatter, become captured, deposit annihilation energy, and increase the heat flow within exoplanets. We estimate upcoming infrared telescope sensitivity to this scenario, finding actionable discovery or exclusion searches. We find that DM with masses above about an MeV can be probed with exoplanets, with DM-proton and DM-electron scattering cross sections down to about 10^{-37} cm^{2}, stronger than existing limits by up to six orders of magnitude. Supporting evidence of a DM origin can be identified through DM-induced exoplanet heating correlated with galactic position, and hence DM density. This provides new motivation to measure the temperature of the billions of brown dwarfs, rogue planets, and gas giants peppered throughout our Galaxy.
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Affiliation(s)
- Rebecca K Leane
- Center for Theoretical Physics, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA
- SLAC National Accelerator Laboratory, Stanford University, Stanford, California 94039, USA
| | - Juri Smirnov
- Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, Ohio 43210, USA
- Department of Physics, The Ohio State University, Columbus, Ohio 43210, USA
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15
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Kramer ED, Kuflik E, Levi N, Outmezguine NJ, Ruderman JT. Heavy Thermal Dark Matter from a New Collision Mechanism. Phys Rev Lett 2021; 126:081802. [PMID: 33709734 DOI: 10.1103/physrevlett.126.081802] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/13/2020] [Revised: 12/02/2020] [Accepted: 02/02/2021] [Indexed: 06/12/2023]
Abstract
We propose a new thermal freeze-out mechanism that results in dark matter masses exceeding the unitarity bound by many orders of magnitude, without violating perturbative unitarity or modifying the standard cosmology. The process determining the relic abundance is χζ^{†}→ζζ, where χ is the dark matter candidate. For m_{ζ}<m_{χ}<3m_{ζ}, χ is cosmologically long-lived and scatters against the exponentially more abundant ζ. Therefore, such a process allows for exponentially heavier dark matter for the same interaction strength as a particle undergoing ordinary 2→2 freeze-out, or equivalently, exponentially weaker interactions for the same mass. We demonstrate this mechanism in a leptophilic dark matter model, which allows for dark matter masses up to 10^{9} GeV.
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Affiliation(s)
- Eric David Kramer
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - Eric Kuflik
- Racah Institute of Physics, Hebrew University of Jerusalem, Jerusalem 91904, Israel
| | - Noam Levi
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
| | | | - Joshua T Ruderman
- Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, New York 10003, USA
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16
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17
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Barak L, Bloch IM, Cababie M, Cancelo G, Chaplinsky L, Chierchie F, Crisler M, Drlica-Wagner A, Essig R, Estrada J, Etzion E, Moroni GF, Gift D, Munagavalasa S, Orly A, Rodrigues D, Singal A, Haro MS, Stefanazzi L, Tiffenberg J, Uemura S, Volansky T, Yu TT. SENSEI: Direct-Detection Results on sub-GeV Dark Matter from a New Skipper CCD. Phys Rev Lett 2020; 125:171802. [PMID: 33156657 DOI: 10.1103/physrevlett.125.171802] [Citation(s) in RCA: 30] [Impact Index Per Article: 7.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/04/2020] [Revised: 08/17/2020] [Accepted: 09/11/2020] [Indexed: 06/11/2023]
Abstract
We present the first direct-detection search for sub-GeV dark matter using a new ∼2-gram high-resistivity Skipper CCD from a dedicated fabrication batch that was optimized for dark matter searches. Using 24 days of data acquired in the MINOS cavern at the Fermi National Accelerator Laboratory, we measure the lowest rates in silicon detectors of events containing one, two, three, or four electrons, and achieve world-leading sensitivity for a large range of sub-GeV dark matter masses. Data taken with different thicknesses of the detector shield suggest a correlation between the rate of high-energy tracks and the rate of single-electron events previously classified as "dark current." We detail key characteristics of the new Skipper CCDs, which augur well for the planned construction of the ∼100-gram SENSEI experiment at SNOLAB.
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Affiliation(s)
- Liron Barak
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
| | - Itay M Bloch
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
| | - Mariano Cababie
- Department of Physics, FCEN, University of Buenos Aires and IFIBA, CONICET, Buenos Aires, Argentina
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
| | - Gustavo Cancelo
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
| | - Luke Chaplinsky
- C.N. Yang Institute for Theoretical Physics, Stony Brook University, Stony Brook, New York 11794, USA
- Department of Physics and Astronomy, Stony Brook University, Stony Brook, New York 11794, USA
| | - Fernando Chierchie
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
| | - Michael Crisler
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
| | - Alex Drlica-Wagner
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
- Kavli Institute for Cosmological Physics, University of Chicago, Chicago, Illinois 60637, USA
- Department of Astronomy and Astrophysics, University of Chicago, Chicago Illinois 60637, USA
| | - Rouven Essig
- C.N. Yang Institute for Theoretical Physics, Stony Brook University, Stony Brook, New York 11794, USA
| | - Juan Estrada
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
| | - Erez Etzion
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
| | | | - Daniel Gift
- C.N. Yang Institute for Theoretical Physics, Stony Brook University, Stony Brook, New York 11794, USA
- Department of Physics and Astronomy, Stony Brook University, Stony Brook, New York 11794, USA
| | - Sravan Munagavalasa
- C.N. Yang Institute for Theoretical Physics, Stony Brook University, Stony Brook, New York 11794, USA
- Department of Physics and Astronomy, Stony Brook University, Stony Brook, New York 11794, USA
| | - Aviv Orly
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
| | - Dario Rodrigues
- Department of Physics, FCEN, University of Buenos Aires and IFIBA, CONICET, Buenos Aires, Argentina
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
| | - Aman Singal
- Department of Physics and Astronomy, Stony Brook University, Stony Brook, New York 11794, USA
| | - Miguel Sofo Haro
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
- Centro Atómico Bariloche, CNEA/CONICET/IB, Bariloche, Argentina
| | - Leandro Stefanazzi
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
| | - Javier Tiffenberg
- Fermi National Accelerator Laboratory, PO Box 500, Batavia Illinois 60510, USA
| | - Sho Uemura
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
| | - Tomer Volansky
- School of Physics and Astronomy, Tel-Aviv University, Tel-Aviv 69978, Israel
| | - Tien-Tien Yu
- Department of Physics and Institute for Fundamental Science, University of Oregon, Eugene, Oregon 97403, USA
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Smirnov J, Beacom JF. New Freezeout Mechanism for Strongly Interacting Dark Matter. Phys Rev Lett 2020; 125:131301. [PMID: 33034501 DOI: 10.1103/physrevlett.125.131301] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 02/27/2020] [Revised: 07/06/2020] [Accepted: 08/10/2020] [Indexed: 06/11/2023]
Abstract
We present a new mechanism for thermally produced dark matter, based on a semi-annihilation-like process, χ+χ+SM→χ+SM, with intriguing consequences for the properties of dark matter. First, its mass is low, ≲1 GeV (but ≳5 keV to avoid structure-formation constraints). Second, it is strongly interacting, leading to kinetic equilibrium between the dark and visible sectors, avoiding the structure-formation problems of χ+χ+χ→χ+χ models. Third, in the 3→2 process, one dark matter particle is consumed, giving the standard-model particle a monoenergetic recoil. We show that this new scenario is presently allowed, which is surprising (perhaps a "minor miracle"). However, it can be systematically tested by novel analyses in present and near-term experiments. In particular, the Co-SIMP model for thermal-relic dark matter can explain the XENON1T excess.
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Affiliation(s)
- Juri Smirnov
- Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, Ohio 43210, USA
- Department of Physics, The Ohio State University, Columbus, Ohio 43210, USA
| | - John F Beacom
- Center for Cosmology and AstroParticle Physics (CCAPP), The Ohio State University, Columbus, Ohio 43210, USA
- Department of Physics, The Ohio State University, Columbus, Ohio 43210, USA
- Department of Astronomy, The Ohio State University, Columbus, Ohio 43210, USA
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Cai C, Zhang HH, Cacciapaglia G, Rosenlyst M, Frandsen MT. Higgs Boson Emerging from the Dark. Phys Rev Lett 2020; 125:021801. [PMID: 32701315 DOI: 10.1103/physrevlett.125.021801] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/08/2019] [Revised: 04/09/2020] [Accepted: 06/15/2020] [Indexed: 06/11/2023]
Abstract
We propose a new nonthermal mechanism of dark matter production based on vacuum misalignment. A global X-charge asymmetry is generated at high temperatures, under which both the will-be Higgs boson and the dark matter are charged. At lower energies, the vacuum changes alignment and breaks the U(1)_{X}, leading to the emergence of the Higgs bosonand of a fraction of charge asymmetry stored in the stable dark matter relic. This mechanism can be present in a wide variety of models based on vacuum misalignment, and we demonstrate it in a composite Higgs template model, where all the necessary ingredients are naturally present. A light pseudo-scalar η is always predicted, with interesting implications for cosmology, future supernova observations and exotic Z→γη decays.
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Affiliation(s)
- Chengfeng Cai
- School of Physics, Sun Yat-Sen University, Guangzhou 510275, China
| | - Hong-Hao Zhang
- School of Physics, Sun Yat-Sen University, Guangzhou 510275, China
| | - Giacomo Cacciapaglia
- Institut de Physique des 2 Infinis (IP2I), CNRS/IN2P3, UMR5822, 69622 Villeurbanne, France and Université de Lyon, Université Claude Bernard Lyon 1, 69001 Lyon, France
| | - Martin Rosenlyst
- CP3-Origins, University of Southern Denmark, Campusvej 55, DK-5230 Odense M, Denmark
| | - Mads T Frandsen
- CP3-Origins, University of Southern Denmark, Campusvej 55, DK-5230 Odense M, Denmark
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Trickle T, Zhang Z, Zurek KM. Detecting Light Dark Matter with Magnons. Phys Rev Lett 2020; 124:201801. [PMID: 32501088 DOI: 10.1103/physrevlett.124.201801] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/01/2019] [Revised: 02/03/2020] [Accepted: 04/14/2020] [Indexed: 06/11/2023]
Abstract
Scattering of light dark matter with sub-eV energy deposition can be detected with collective excitations in condensed matter systems. When dark matter has spin-independent couplings to atoms or ions, it has been shown to efficiently excite phonons. Here we show that, if dark matter couples to the electron spin, magnon excitations in materials with magnetic dipole order offer a promising detection path. We derive general formulae for single magnon excitation rates from dark matter scattering, and demonstrate as a proof of principle the projected reach of a yttrium iron garnet target for several dark matter models with spin-dependent interactions. This highlights the complementarity of various collective excitations in probing different dark matter interactions.
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Affiliation(s)
- Tanner Trickle
- Department of Physics, University of California, Berkeley, California 94720, USA
- Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
- Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - Zhengkang Zhang
- Department of Physics, University of California, Berkeley, California 94720, USA
- Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
- Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
| | - Kathryn M Zurek
- Department of Physics, University of California, Berkeley, California 94720, USA
- Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
- Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
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Dror JA, Elor G, McGehee R. Directly Detecting Signals from Absorption of Fermionic Dark Matter. Phys Rev Lett 2020; 124:181301. [PMID: 32441951 DOI: 10.1103/physrevlett.124.181301] [Citation(s) in RCA: 4] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/05/2019] [Revised: 03/02/2020] [Accepted: 04/16/2020] [Indexed: 06/11/2023]
Abstract
We present a new class of direct detection signals; absorption of fermionic dark matter. We enumerate the operators through dimension six which lead to fermionic absorption, study their direct detection prospects, and summarize additional constraints on their suppression scale. Such dark matter is inherently unstable as there is no symmetry which prevents dark matter decays. Nevertheless, we show that fermionic dark matter absorption can be observed in direct detection and neutrino experiments while ensuring consistency with the observed dark matter abundance and required lifetime. For dark matter masses well below the GeV scale, dedicated searches for these signals at current and future experiments can probe orders of magnitude of unexplored parameter space.
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Affiliation(s)
- Jeff A Dror
- Theory Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
- Berkeley Center for Theoretical Physics, University of California, Berkeley, California 94720, USA
| | - Gilly Elor
- Department of Physics, Box 1560, University of Washington, Seattle, Washington 98195, USA
| | - Robert McGehee
- Theory Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
- Berkeley Center for Theoretical Physics, University of California, Berkeley, California 94720, USA
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D'Agnolo RT, Pappadopulo D, Ruderman JT, Wang PJ. Thermal Relic Targets with Exponentially Small Couplings. Phys Rev Lett 2020; 124:151801. [PMID: 32357019 DOI: 10.1103/physrevlett.124.151801] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/26/2019] [Revised: 01/16/2020] [Accepted: 03/12/2020] [Indexed: 06/11/2023]
Abstract
If dark matter was produced in the early Universe by the decoupling of its annihilations into known particles, there is a sharp experimental target for the size of its coupling. We show that if dark matter was produced by inelastic scattering against a lighter particle from the thermal bath, then its coupling can be exponentially smaller than the coupling required for its production from annihilations. As an application, we demonstrate that dark matter produced by inelastic scattering against electrons provides new thermal relic targets for direct detection and fixed target experiments.
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Affiliation(s)
- Raffaele Tito D'Agnolo
- SLAC National Accelerator Laboratory, 2575 Sand Hill Road, Menlo Park, California 94025, USA
| | | | - Joshua T Ruderman
- Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, New York 10003, USA
| | - Po-Jen Wang
- Center for Cosmology and Particle Physics, Department of Physics, New York University, New York, New York 10003, USA
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Curtin D, Drewes M, McCullough M, Meade P, Mohapatra RN, Shelton J, Shuve B, Accomando E, Alpigiani C, Antusch S, Carlos Arteaga-Velázquez J, Batell B, Bauer M, Blinov N, Salomé Caballero-Mora K, Hyeok Chang J, Chun EJ, Co RT, Cohen T, Cox P, Craig N, Csáki C, Cui Y, D'Eramo F, Delle Rose L, Bhupal Dev PS, Dienes KR, Dror JA, Essig R, Evans JA, Evans JL, Fernández Tellez A, Fischer O, Flacke T, Fradette A, Frugiuele C, Fuchs E, Gherghetta T, Giudice GF, Gorbunov D, Gupta RS, Hagedorn C, Hall LJ, Harris P, Carlos Helo J, Hirsch M, Hochberg Y, Hook A, Ibarra A, Ipek S, Jung S, Knapen S, Kuflik E, Liu Z, Lombardo S, Lubatti HJ, McKeen D, Molinaro E, Moretti S, Nagata N, Neubert M, Miguel No J, Olaiya E, Perez G, Peskin ME, Pinner D, Pospelov M, Reece M, Robinson DJ, Rodríguez Cahuantzi M, Santonico R, Schlaffer M, Shepherd-Themistocleous CH, Spray A, Stolarski D, Subieta Vasquez MA, Sundrum R, Thamm A, Thomas B, Tsai Y, Tweedie B, West SM, Young C, Yu F, Zaldivar B, Zhang Y, Zurek K, Zurita J. Long-lived particles at the energy frontier: the MATHUSLA physics case. Rep Prog Phys 2019; 82:116201. [PMID: 31185458 DOI: 10.1088/1361-6633/ab28d6] [Citation(s) in RCA: 9] [Impact Index Per Article: 1.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 06/09/2023]
Abstract
We examine the theoretical motivations for long-lived particle (LLP) signals at the LHC in a comprehensive survey of standard model (SM) extensions. LLPs are a common prediction of a wide range of theories that address unsolved fundamental mysteries such as naturalness, dark matter, baryogenesis and neutrino masses, and represent a natural and generic possibility for physics beyond the SM (BSM). In most cases the LLP lifetime can be treated as a free parameter from the [Formula: see text]m scale up to the Big Bang Nucleosynthesis limit of [Formula: see text] m. Neutral LLPs with lifetimes above [Formula: see text]100 m are particularly difficult to probe, as the sensitivity of the LHC main detectors is limited by challenging backgrounds, triggers, and small acceptances. MATHUSLA is a proposal for a minimally instrumented, large-volume surface detector near ATLAS or CMS. It would search for neutral LLPs produced in HL-LHC collisions by reconstructing displaced vertices (DVs) in a low-background environment, extending the sensitivity of the main detectors by orders of magnitude in the long-lifetime regime. We study the LLP physics opportunities afforded by a MATHUSLA-like detector at the HL-LHC, assuming backgrounds can be rejected as expected. We develop a model-independent approach to describe the sensitivity of MATHUSLA to BSM LLP signals, and compare it to DV and missing energy searches at ATLAS or CMS. We then explore the BSM motivations for LLPs in considerable detail, presenting a large number of new sensitivity studies. While our discussion is especially oriented towards the long-lifetime regime at MATHUSLA, this survey underlines the importance of a varied LLP search program at the LHC in general. By synthesizing these results into a general discussion of the top-down and bottom-up motivations for LLP searches, it is our aim to demonstrate the exceptional strength and breadth of the physics case for the construction of the MATHUSLA detector.
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Affiliation(s)
- David Curtin
- Department of Physics, University of Toronto, Toronto, ON M5S 1A7, Canada
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Acanfora F, Esposito A, Polosa AD. Sub-GeV dark matter in superfluid He-4: an effective theory approach. Eur Phys J C Part Fields 2019; 79:549. [PMID: 31327931 PMCID: PMC6598953 DOI: 10.1140/epjc/s10052-019-7057-0] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.6] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 02/08/2019] [Accepted: 06/08/2019] [Indexed: 06/10/2023]
Abstract
We employ an effective field theory to study the detectability of sub-GeV dark matter through its interaction with the gapless excitations of superfluid4 He. In a quantum field theory language, the possible interactions between the dark matter and the superfluid phonon are solely dictated by symmetry. We compute the rate for the emission of one and two phonons, and show that these two observables combined allow for a large exclusion region for the dark matter masses. Our approach allows a direct calculation of the differential distributions, even though it is limited only to the region of softer phonon excitations, where the effective field theory is well defined. The method presented here is easily extendible to different models of dark matter.
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Affiliation(s)
- Francesca Acanfora
- Dipartimento di Fisica, Sapienza Università di Roma, P.le A Moro 2, Rome, 00185 Italy
| | - Angelo Esposito
- Theoretical Particle Physics Laboratory (LPTP), Institute of Physics, EPFL, 1015 Lausanne, Switzerland
| | - Antonio D. Polosa
- Dipartimento di Fisica and INFN, Sapienza Università di Roma, P.le Aldo Moro 2, 00185 Rome, Italy
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Abstract
Sub-GeV dark matter particles up-scattered by cosmic rays gain enough kinetic energy to pass the thresholds of large volume detectors on Earth. We then use public Super-Kamiokande and MiniBooNE data to derive a novel limit on the scattering cross section of dark matter with electrons that extends down to sub-keV masses, closing a previously allowed wide region of parameter space. We finally discuss search strategies and prospects at existing and planned neutrino facilities.
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Affiliation(s)
- Yohei Ema
- DESY, Notkestraße 85, D-22607 Hamburg, Germany
- KEK Theory Center, Tsukuba 305-0801, Japan
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Chu X, Garcia-Cely C, Murayama H. Velocity Dependence from Resonant Self-Interacting Dark Matter. Phys Rev Lett 2019; 122:071103. [PMID: 30848653 DOI: 10.1103/physrevlett.122.071103] [Citation(s) in RCA: 4] [Impact Index Per Article: 0.8] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 10/23/2018] [Revised: 11/24/2018] [Indexed: 06/09/2023]
Abstract
The dark matter density distribution in small-scale astrophysical objects may indicate that dark matter is self-interacting, while observations from clusters of galaxies suggest that the corresponding cross section depends on the velocity. Using a model-independent approach, we show that resonant self-interacting dark matter can naturally explain such a behavior. In contrast to what is often assumed, this does not require a light mediator. We present explicit realizations of this mechanism and discuss the corresponding astrophysical constraints.
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Affiliation(s)
- Xiaoyong Chu
- Institute of High Energy Physics, Austrian Academy of Sciences, Nikolsdorfer Gasse 18, 1050 Vienna, Austria
| | - Camilo Garcia-Cely
- Deutsches Elektronen-Synchrotron DESY, Notkestrasse 85, 22607 Hamburg, Germany
| | - Hitoshi Murayama
- Deutsches Elektronen-Synchrotron DESY, Notkestrasse 85, 22607 Hamburg, Germany
- Department of Physics, University of California, Berkeley, California 94720, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, Kashiwa 277-8583, Japan
- Ernest Orlando Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
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32
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Bernal N, Cosme C, Tenkanen T, Vaskonen V. Scalar singlet dark matter in non-standard cosmologies. Eur Phys J C Part Fields 2019; 79:30. [PMID: 30872965 PMCID: PMC6383953 DOI: 10.1140/epjc/s10052-019-6550-9] [Citation(s) in RCA: 5] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Grants] [Track Full Text] [Figures] [Subscribe] [Scholar Register] [Received: 07/09/2018] [Accepted: 12/21/2018] [Indexed: 06/09/2023]
Abstract
We study production of dark matter (DM) in models with a non-standard expansion history. We consider both freeze-out and freeze-in mechanisms for producing the observed DM abundance in a model where the DM consists of scalar singlet particles coupled to the Standard Model sector via the Higgs portal. We show that a non-standard expansion phase can lead to a significant change in the DM abundance and therefore to observational ramifications. For example, for DM freeze-in the required portal coupling can be much larger, whereas for DM freeze-out much smaller values become allowed. We evaluate the relevant constraints and discuss prospects for direct detection of such DM.
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Affiliation(s)
- Nicolás Bernal
- Centro de Investigaciones, Universidad Antonio Nariño, Carrera 3 Este # 47A-15, Bogotá, Colombia
| | - Catarina Cosme
- Departamento de Física e Astronomia, Faculdade de Ciências da Universidade do Porto and Centro de Física do Porto, Rua do Campo Alegre 687, 4169-007 Porto, Portugal
| | - Tommi Tenkanen
- Astronomy Unit, Queen Mary University of London, Mile End Road, London, E1 4NS UK
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Agnes P, Albuquerque IFM, Alexander T, Alton AK, Araujo GR, Asner DM, Ave M, Back HO, Baldin B, Batignani G, Biery K, Bocci V, Bonfini G, Bonivento W, Bottino B, Budano F, Bussino S, Cadeddu M, Cadoni M, Calaprice F, Caminata A, Canci N, Candela A, Caravati M, Cariello M, Carlini M, Carpinelli M, Catalanotti S, Cataudella V, Cavalcante P, Cavuoti S, Cereseto R, Chepurnov A, Cicalò C, Cifarelli L, Cocco AG, Covone G, D'Angelo D, D'Incecco M, D'Urso D, Davini S, De Candia A, De Cecco S, De Deo M, De Filippis G, De Rosa G, De Vincenzi M, Demontis P, Derbin AV, Devoto A, Di Eusanio F, Di Pietro G, Dionisi C, Downing M, Edkins E, Empl A, Fan A, Fiorillo G, Fomenko K, Franco D, Gabriele F, Gabrieli A, Galbiati C, Garcia Abia P, Ghiano C, Giagu S, Giganti C, Giovanetti GK, Gorchakov O, Goretti AM, Granato F, Gromov M, Guan M, Guardincerri Y, Gulino M, Hackett BR, Hassanshahi MH, Herner K, Hosseini B, Hughes D, Humble P, Hungerford EV, Ianni A, Ianni A, Ippolito V, James I, Johnson TN, Kahn Y, Keeter K, Kendziora CL, Kochanek I, Koh G, Korablev D, Korga G, Kubankin A, Kuss M, La Commara M, Lai M, Li X, Lisanti M, Lissia M, Loer B, Longo G, Ma Y, Machado AA, Machulin IN, Mandarano A, Mapelli L, Mari SM, Maricic J, Martoff CJ, Messina A, Meyers PD, Milincic R, Mishra-Sharma S, Monte A, Morrocchi M, Mount BJ, Muratova VN, Musico P, Nania R, Navrer Agasson A, Nozdrina AO, Oleinik A, Orsini M, Ortica F, Pagani L, Pallavicini M, Pandola L, Pantic E, Paoloni E, Pazzona F, Pelczar K, Pelliccia N, Pesudo V, Picciau E, Pocar A, Pordes S, Poudel SS, Pugachev DA, Qian H, Ragusa F, Razeti M, Razeto A, Reinhold B, Renshaw AL, Rescigno M, Riffard Q, Romani A, Rossi B, Rossi N, Sablone D, Samoylov O, Sands W, Sanfilippo S, Sant M, Santorelli R, Savarese C, Scapparone E, Schlitzer B, Segreto E, Semenov DA, Shchagin A, Sheshukov A, Singh PN, Skorokhvatov MD, Smirnov O, Sotnikov A, Stanford C, Stracka S, Suffritti GB, Suvorov Y, Tartaglia R, Testera G, Tonazzo A, Trinchese P, Unzhakov EV, Verducci M, Vishneva A, Vogelaar B, Wada M, Waldrop TJ, Wang H, Wang Y, Watson AW, Westerdale S, Wojcik MM, Wojcik M, Xiang X, Xiao X, Yang C, Ye Z, Zhu C, Zichichi A, Zuzel G. Constraints on Sub-GeV Dark-Matter-Electron Scattering from the DarkSide-50 Experiment. Phys Rev Lett 2018; 121:111303. [PMID: 30265123 DOI: 10.1103/physrevlett.121.111303] [Citation(s) in RCA: 14] [Impact Index Per Article: 2.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 05/15/2018] [Revised: 07/16/2018] [Indexed: 06/08/2023]
Abstract
We present new constraints on sub-GeV dark-matter particles scattering off electrons based on 6780.0 kg d of data collected with the DarkSide-50 dual-phase argon time projection chamber. This analysis uses electroluminescence signals due to ionized electrons extracted from the liquid argon target. The detector has a very high trigger probability for these signals, allowing for an analysis threshold of three extracted electrons, or approximately 0.05 keVee. We calculate the expected recoil spectra for dark matter-electron scattering in argon and, under the assumption of momentum-independent scattering, improve upon existing limits from XENON10 for dark-matter particles with masses between 30 and 100 MeV/c^{2}.
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Affiliation(s)
- P Agnes
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | - I F M Albuquerque
- Instituto de Física, Universidade de São Paulo, São Paulo 05508-090, Brazil
| | - T Alexander
- Pacific Northwest National Laboratory, Richland, Washington 99352, USA
| | - A K Alton
- Physics Department, Augustana University, Sioux Falls, South Dakota 57197, USA
| | - G R Araujo
- Instituto de Física, Universidade de São Paulo, São Paulo 05508-090, Brazil
| | - D M Asner
- Brookhaven National Laboratory, Upton, New York 11973, USA
| | - M Ave
- Instituto de Física, Universidade de São Paulo, São Paulo 05508-090, Brazil
| | - H O Back
- Pacific Northwest National Laboratory, Richland, Washington 99352, USA
| | - B Baldin
- Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
| | - G Batignani
- INFN Pisa, Pisa 56127, Italy
- Physics Department, Università degli Studi di Pisa, Pisa 56127, Italy
| | - K Biery
- Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
| | - V Bocci
- INFN Sezione di Roma, Roma 00185, Italy
| | - G Bonfini
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | | | - B Bottino
- Physics Department, Università degli Studi di Genova, Genova 16146, Italy
- INFN Genova, Genova 16146, Italy
| | - F Budano
- INFN Roma Tre, Roma 00146, Italy
- Mathematics and Physics Department, Università degli Studi Roma Tre, Roma 00146, Italy
| | - S Bussino
- INFN Roma Tre, Roma 00146, Italy
- Mathematics and Physics Department, Università degli Studi Roma Tre, Roma 00146, Italy
| | - M Cadeddu
- INFN Cagliari, Cagliari 09042, Italy
- Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
| | - M Cadoni
- INFN Cagliari, Cagliari 09042, Italy
- Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
| | - F Calaprice
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | | | - N Canci
- Department of Physics, University of Houston, Houston, Texas 77204, USA
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - A Candela
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - M Caravati
- INFN Cagliari, Cagliari 09042, Italy
- Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
| | | | - M Carlini
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - M Carpinelli
- Chemistry and Pharmacy Department, Università degli Studi di Sassari, Sassari 07100, Italy
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
| | - S Catalanotti
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - V Cataudella
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - P Cavalcante
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
- Virginia Tech, Blacksburg, Virginia 24061, USA
| | - S Cavuoti
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | | | - A Chepurnov
- Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow 119234, Russia
| | - C Cicalò
- INFN Cagliari, Cagliari 09042, Italy
| | - L Cifarelli
- Physics Department, Università degli Studi di Bologna, Bologna 40126, Italy
- INFN Bologna, Bologna 40126, Italy
| | | | - G Covone
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - D D'Angelo
- Physics Department, Università degli Studi di Milano, Milano 20133, Italy
- INFN Milano, Milano 20133, Italy
| | - M D'Incecco
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - D D'Urso
- Chemistry and Pharmacy Department, Università degli Studi di Sassari, Sassari 07100, Italy
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
| | - S Davini
- INFN Genova, Genova 16146, Italy
| | - A De Candia
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - S De Cecco
- INFN Sezione di Roma, Roma 00185, Italy
- Physics Department, Sapienza Università di Roma, Roma 00185, Italy
| | - M De Deo
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - G De Filippis
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - G De Rosa
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - M De Vincenzi
- INFN Roma Tre, Roma 00146, Italy
- Mathematics and Physics Department, Università degli Studi Roma Tre, Roma 00146, Italy
| | - P Demontis
- Chemistry and Pharmacy Department, Università degli Studi di Sassari, Sassari 07100, Italy
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
- Interuniversity Consortium for Science and Technology of Materials, Firenze 50121, Italy
| | - A V Derbin
- Saint Petersburg Nuclear Physics Institute, Gatchina 188350, Russia
| | - A Devoto
- INFN Cagliari, Cagliari 09042, Italy
- Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
| | - F Di Eusanio
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - G Di Pietro
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
- INFN Milano, Milano 20133, Italy
| | - C Dionisi
- INFN Sezione di Roma, Roma 00185, Italy
- Physics Department, Sapienza Università di Roma, Roma 00185, Italy
| | - M Downing
- Amherst Center for Fundamental Interactions and Physics Department, University of Massachusetts, Amherst, Massachusetts 01003, USA
| | - E Edkins
- Department of Physics and Astronomy, University of Hawai'i, Honolulu, Hawai'i 96822, USA
| | - A Empl
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | - A Fan
- Physics and Astronomy Department, University of California, Los Angeles, California 90095, USA
| | - G Fiorillo
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - K Fomenko
- Joint Institute for Nuclear Research, Dubna 141980, Russia
| | - D Franco
- APC, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, USPC, Paris 75205, France
| | - F Gabriele
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - A Gabrieli
- Chemistry and Pharmacy Department, Università degli Studi di Sassari, Sassari 07100, Italy
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
| | - C Galbiati
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
- Gran Sasso Science Institute, L'Aquila 67100, Italy
| | - P Garcia Abia
- CIEMAT, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Madrid 28040, Spain
| | - C Ghiano
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - S Giagu
- INFN Sezione di Roma, Roma 00185, Italy
- Physics Department, Sapienza Università di Roma, Roma 00185, Italy
| | - C Giganti
- LPNHE, CNRS/IN2P3, Sorbonne Université, Université Paris Diderot, Paris 75252, France
| | - G K Giovanetti
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - O Gorchakov
- Joint Institute for Nuclear Research, Dubna 141980, Russia
| | - A M Goretti
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - F Granato
- Physics Department, Temple University, Philadelphia, Pennsylvania 19122, USA
| | - M Gromov
- Skobeltsyn Institute of Nuclear Physics, Lomonosov Moscow State University, Moscow 119234, Russia
| | - M Guan
- Institute of High Energy Physics, Beijing 100049, China
| | - Y Guardincerri
- Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
| | - M Gulino
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
- Engineering and Architecture Faculty, Università di Enna Kore, Enna 94100, Italy
| | - B R Hackett
- Department of Physics and Astronomy, University of Hawai'i, Honolulu, Hawai'i 96822, USA
| | - M H Hassanshahi
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - K Herner
- Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
| | | | - D Hughes
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - P Humble
- Pacific Northwest National Laboratory, Richland, Washington 99352, USA
| | - E V Hungerford
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | - Al Ianni
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - An Ianni
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | | | - I James
- INFN Roma Tre, Roma 00146, Italy
- Mathematics and Physics Department, Università degli Studi Roma Tre, Roma 00146, Italy
| | - T N Johnson
- Department of Physics, University of California, Davis, California 95616, USA
| | - Y Kahn
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - K Keeter
- School of Natural Sciences, Black Hills State University, Spearfish, South Dakota 57799, USA
| | - C L Kendziora
- Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
| | - I Kochanek
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - G Koh
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - D Korablev
- Joint Institute for Nuclear Research, Dubna 141980, Russia
| | - G Korga
- Department of Physics, University of Houston, Houston, Texas 77204, USA
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - A Kubankin
- Radiation Physics Laboratory, Belgorod National Research University, Belgorod 308007, Russia
| | - M Kuss
- INFN Pisa, Pisa 56127, Italy
| | - M La Commara
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - M Lai
- INFN Cagliari, Cagliari 09042, Italy
- Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
| | - X Li
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - M Lisanti
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - M Lissia
- INFN Cagliari, Cagliari 09042, Italy
| | - B Loer
- Pacific Northwest National Laboratory, Richland, Washington 99352, USA
| | - G Longo
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - Y Ma
- Institute of High Energy Physics, Beijing 100049, China
| | - A A Machado
- Physics Institute, Universidade Estadual de Campinas, Campinas 13083, Brazil
| | - I N Machulin
- National Research Centre Kurchatov Institute, Moscow 123182, Russia
- National Research Nuclear University MEPhI, Moscow 115409, Russia
| | - A Mandarano
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
- Gran Sasso Science Institute, L'Aquila 67100, Italy
| | - L Mapelli
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - S M Mari
- INFN Roma Tre, Roma 00146, Italy
- Mathematics and Physics Department, Università degli Studi Roma Tre, Roma 00146, Italy
| | - J Maricic
- Department of Physics and Astronomy, University of Hawai'i, Honolulu, Hawai'i 96822, USA
| | - C J Martoff
- Physics Department, Temple University, Philadelphia, Pennsylvania 19122, USA
| | - A Messina
- INFN Sezione di Roma, Roma 00185, Italy
- Physics Department, Sapienza Università di Roma, Roma 00185, Italy
| | - P D Meyers
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - R Milincic
- Department of Physics and Astronomy, University of Hawai'i, Honolulu, Hawai'i 96822, USA
| | - S Mishra-Sharma
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - A Monte
- Amherst Center for Fundamental Interactions and Physics Department, University of Massachusetts, Amherst, Massachusetts 01003, USA
| | | | - B J Mount
- School of Natural Sciences, Black Hills State University, Spearfish, South Dakota 57799, USA
| | - V N Muratova
- Saint Petersburg Nuclear Physics Institute, Gatchina 188350, Russia
| | - P Musico
- INFN Genova, Genova 16146, Italy
| | - R Nania
- INFN Bologna, Bologna 40126, Italy
| | - A Navrer Agasson
- LPNHE, CNRS/IN2P3, Sorbonne Université, Université Paris Diderot, Paris 75252, France
| | - A O Nozdrina
- National Research Centre Kurchatov Institute, Moscow 123182, Russia
- National Research Nuclear University MEPhI, Moscow 115409, Russia
| | - A Oleinik
- Radiation Physics Laboratory, Belgorod National Research University, Belgorod 308007, Russia
| | - M Orsini
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - F Ortica
- Chemistry, Biology and Biotechnology Department, Università degli Studi di Perugia, Perugia 06123, Italy
- INFN Perugia, Perugia 06123, Italy
| | - L Pagani
- Department of Physics, University of California, Davis, California 95616, USA
| | - M Pallavicini
- Physics Department, Università degli Studi di Genova, Genova 16146, Italy
- INFN Genova, Genova 16146, Italy
| | - L Pandola
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
| | - E Pantic
- Department of Physics, University of California, Davis, California 95616, USA
| | - E Paoloni
- INFN Pisa, Pisa 56127, Italy
- Physics Department, Università degli Studi di Pisa, Pisa 56127, Italy
| | - F Pazzona
- Chemistry and Pharmacy Department, Università degli Studi di Sassari, Sassari 07100, Italy
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
| | - K Pelczar
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - N Pelliccia
- Chemistry, Biology and Biotechnology Department, Università degli Studi di Perugia, Perugia 06123, Italy
- INFN Perugia, Perugia 06123, Italy
| | - V Pesudo
- CIEMAT, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Madrid 28040, Spain
| | - E Picciau
- INFN Cagliari, Cagliari 09042, Italy
- Physics Department, Università degli Studi di Cagliari, Cagliari 09042, Italy
| | - A Pocar
- Amherst Center for Fundamental Interactions and Physics Department, University of Massachusetts, Amherst, Massachusetts 01003, USA
| | - S Pordes
- Fermi National Accelerator Laboratory, Batavia, Illinois 60510, USA
| | - S S Poudel
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | - D A Pugachev
- National Research Centre Kurchatov Institute, Moscow 123182, Russia
| | - H Qian
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - F Ragusa
- Physics Department, Università degli Studi di Milano, Milano 20133, Italy
- INFN Milano, Milano 20133, Italy
| | - M Razeti
- INFN Cagliari, Cagliari 09042, Italy
| | - A Razeto
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | - B Reinhold
- Department of Physics and Astronomy, University of Hawai'i, Honolulu, Hawai'i 96822, USA
| | - A L Renshaw
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | | | - Q Riffard
- APC, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, USPC, Paris 75205, France
| | - A Romani
- Chemistry, Biology and Biotechnology Department, Università degli Studi di Perugia, Perugia 06123, Italy
- INFN Perugia, Perugia 06123, Italy
| | - B Rossi
- INFN Napoli, Napoli 80126, Italy
| | - N Rossi
- INFN Sezione di Roma, Roma 00185, Italy
| | - D Sablone
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - O Samoylov
- Joint Institute for Nuclear Research, Dubna 141980, Russia
| | - W Sands
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - S Sanfilippo
- INFN Roma Tre, Roma 00146, Italy
- Mathematics and Physics Department, Università degli Studi Roma Tre, Roma 00146, Italy
| | - M Sant
- Chemistry and Pharmacy Department, Università degli Studi di Sassari, Sassari 07100, Italy
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
| | - R Santorelli
- CIEMAT, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas, Madrid 28040, Spain
| | - C Savarese
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
- Gran Sasso Science Institute, L'Aquila 67100, Italy
| | | | - B Schlitzer
- Department of Physics, University of California, Davis, California 95616, USA
| | - E Segreto
- Physics Institute, Universidade Estadual de Campinas, Campinas 13083, Brazil
| | - D A Semenov
- Saint Petersburg Nuclear Physics Institute, Gatchina 188350, Russia
| | - A Shchagin
- Radiation Physics Laboratory, Belgorod National Research University, Belgorod 308007, Russia
| | - A Sheshukov
- Joint Institute for Nuclear Research, Dubna 141980, Russia
| | - P N Singh
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | - M D Skorokhvatov
- National Research Centre Kurchatov Institute, Moscow 123182, Russia
- National Research Nuclear University MEPhI, Moscow 115409, Russia
| | - O Smirnov
- Joint Institute for Nuclear Research, Dubna 141980, Russia
| | - A Sotnikov
- Joint Institute for Nuclear Research, Dubna 141980, Russia
| | - C Stanford
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | | | - G B Suffritti
- Chemistry and Pharmacy Department, Università degli Studi di Sassari, Sassari 07100, Italy
- INFN Laboratori Nazionali del Sud, Catania 95123, Italy
- Interuniversity Consortium for Science and Technology of Materials, Firenze 50121, Italy
| | - Y Suvorov
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
- Physics and Astronomy Department, University of California, Los Angeles, California 90095, USA
- National Research Centre Kurchatov Institute, Moscow 123182, Russia
| | - R Tartaglia
- INFN Laboratori Nazionali del Gran Sasso, Assergi (AQ) 67100, Italy
| | | | - A Tonazzo
- APC, Université Paris Diderot, CNRS/IN2P3, CEA/Irfu, Obs de Paris, USPC, Paris 75205, France
| | - P Trinchese
- Physics Department, Università degli Studi "Federico II" di Napoli, Napoli 80126, Italy
- INFN Napoli, Napoli 80126, Italy
| | - E V Unzhakov
- Saint Petersburg Nuclear Physics Institute, Gatchina 188350, Russia
| | - M Verducci
- INFN Sezione di Roma, Roma 00185, Italy
- Physics Department, Sapienza Università di Roma, Roma 00185, Italy
| | - A Vishneva
- Joint Institute for Nuclear Research, Dubna 141980, Russia
| | - B Vogelaar
- Virginia Tech, Blacksburg, Virginia 24061, USA
| | - M Wada
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - T J Waldrop
- Physics Department, Augustana University, Sioux Falls, South Dakota 57197, USA
| | - H Wang
- Physics and Astronomy Department, University of California, Los Angeles, California 90095, USA
| | - Y Wang
- Physics and Astronomy Department, University of California, Los Angeles, California 90095, USA
| | - A W Watson
- Physics Department, Temple University, Philadelphia, Pennsylvania 19122, USA
| | - S Westerdale
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - M M Wojcik
- M. Smoluchowski Institute of Physics, Jagiellonian University, 30-348 Krakow, Poland
| | - M Wojcik
- Institute of Applied Radiation Chemistry, Lodz University of Technology, 93-590 Lodz, Poland
| | - X Xiang
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - X Xiao
- Physics and Astronomy Department, University of California, Los Angeles, California 90095, USA
| | - C Yang
- Institute of High Energy Physics, Beijing 100049, China
| | - Z Ye
- Department of Physics, University of Houston, Houston, Texas 77204, USA
| | - C Zhu
- Physics Department, Princeton University, Princeton, New Jersey 08544, USA
| | - A Zichichi
- Physics Department, Università degli Studi di Bologna, Bologna 40126, Italy
- INFN Bologna, Bologna 40126, Italy
| | - G Zuzel
- M. Smoluchowski Institute of Physics, Jagiellonian University, 30-348 Krakow, Poland
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Gluscevic V, Boddy KK. Constraints on Scattering of keV-TeV Dark Matter with Protons in the Early Universe. Phys Rev Lett 2018; 121:081301. [PMID: 30192595 DOI: 10.1103/physrevlett.121.081301] [Citation(s) in RCA: 6] [Impact Index Per Article: 1.0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/20/2017] [Revised: 07/29/2018] [Indexed: 06/08/2023]
Abstract
We present the first cosmological constraint on dark matter scattering with protons in the early Universe for the entire range of dark matter masses between 1 keV and 1 TeV. This constraint is derived from the Planck measurements of the cosmic microwave background (CMB) temperature and polarization anisotropy, and the CMB lensing anisotropy. It improves upon previous CMB constraints by many orders of magnitude, where limits are available, and closes the gap in coverage for low-mass dark matter candidates. We focus on two canonical interaction scenarios: spin-independent and spin-dependent scattering with no velocity dependence. Our results exclude (with 95% confidence) spin-independent interactions with cross sections greater than 5.3×10^{-27} cm^{2} for 1 keV, 3.0×10^{-26} cm^{2} for 1 MeV, 1.7×10^{-25} cm^{2} for 1 GeV, and 1.6×10^{-23} cm^{2} for 1 TeV dark matter mass. Finally, we discuss the implications of this study for dark matter physics and future observations.
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Affiliation(s)
- Vera Gluscevic
- School of Natural Sciences, Institute for Advanced Study, Einstein Drive, Princeton, New Jersey 08540, USA
| | - Kimberly K Boddy
- Department of Physics & Astronomy, Johns Hopkins University, Baltimore, Maryland 21218, USA, Department of Physics & Astronomy, University of Hawaii, Honolulu, Hawaii 96822, USA
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Schutz K, Lin T, Safdi BR, Wu CL. Constraining a Thin Dark Matter Disk with Gaia. Phys Rev Lett 2018; 121:081101. [PMID: 30192577 DOI: 10.1103/physrevlett.121.081101] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 12/04/2017] [Revised: 05/04/2018] [Indexed: 06/08/2023]
Abstract
If a component of the dark matter has dissipative interactions, it could collapse to form a thin dark disk in our Galaxy that is coplanar with the baryonic disk. It has been suggested that dark disks could explain a variety of observed phenomena, including periodic comet impacts. Using the first data release from the Gaia space observatory, we search for a dark disk via its effect on stellar kinematics in the Milky Way. Our new limits disfavor the presence of a thin dark matter disk, and we present updated measurements on the total matter density in the Solar neighborhood.
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Affiliation(s)
- Katelin Schutz
- Berkeley Center for Theoretical Physics, University of California, Berkeley, California 94720, USA
| | - Tongyan Lin
- Berkeley Center for Theoretical Physics, University of California, Berkeley, California 94720, USA
- Theoretical Physics Group, Lawrence Berkeley National Laboratory, Berkeley, California 94720, USA
- Department of Physics, University of California, San Diego, California 92093, USA
| | - Benjamin R Safdi
- Leinweber Center for Theoretical Physics, Department of Physics, University of Michigan, Ann Arbor, Michigan 48109, USA
| | - Chih-Liang Wu
- Center for Theoretical Physics, Massachusetts Institute of Technology, Cambridge, Massachusetts 02139, USA
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D'Eramo F, Profumo S. Sub-GeV Dark Matter Shining at Future MeV γ-Ray Telescopes. Phys Rev Lett 2018; 121:071101. [PMID: 30169080 DOI: 10.1103/physrevlett.121.071101] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 06/12/2018] [Revised: 07/16/2018] [Indexed: 06/08/2023]
Abstract
We propose a novel framework where light (sub-GeV) dark matter (DM) is detectable with future MeV γ-ray telescopes without conflicting with cosmic microwave background (CMB) data. The stable DM particle χ has a very low thermal relic abundance due to its large pair-annihilation cross section. The DM number density is stored in a slightly heavier, metastable partner ψ with suppressed pair-annihilation rates, that does not perturb the CMB, and whose late-time decays ψ→χ fill the Universe with χ DM particles. We provide explicit, model-independent realizations for this framework, and discuss constraints on late-time decays, and thus on parameters of this setup, from CMB, big bang nucleosynthesis, and large scale structure.
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Affiliation(s)
- Francesco D'Eramo
- Dipartimento di Fisica ed Astronomia, Università di Padova, Via Marzolo 8, 35131 Padova, Italy
- INFN, Sezione di Padova, Via Marzolo 8, 35131 Padova, Italy
| | - Stefano Profumo
- Department of Physics, 1156 High Street, University of California Santa Cruz, Santa Cruz, California 95064, USA
- Santa Cruz Institute for Particle Physics, 1156 High Street, Santa Cruz, California 95064, USA
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Kachulis C, Abe K, Bronner C, Hayato Y, Ikeda M, Iyogi K, Kameda J, Kato Y, Kishimoto Y, Marti L, Miura M, Moriyama S, Nakahata M, Nakano Y, Nakayama S, Okajima Y, Orii A, Pronost G, Sekiya H, Shiozawa M, Sonoda Y, Takeda A, Takenaka A, Tanaka H, Tasaka S, Tomura T, Akutsu R, Kajita T, Kaneyuki K, Nishimura Y, Okumura K, Tsui KM, Labarga L, Fernandez P, Blaszczyk FDM, Gustafson J, Kearns E, Raaf JL, Stone JL, Sulak LR, Berkman S, Tobayama S, Goldhaber M, Elnimr M, Kropp WR, Mine S, Locke S, Weatherly P, Smy MB, Sobel HW, Takhistov V, Ganezer KS, Hill J, Kim JY, Lim IT, Park RG, Himmel A, Li Z, O'Sullivan E, Scholberg K, Walter CW, Ishizuka T, Nakamura T, Jang JS, Choi K, Learned JG, Matsuno S, Smith SN, Amey J, Litchfield RP, Ma WY, Uchida Y, Wascko MO, Cao S, Friend M, Hasegawa T, Ishida T, Ishii T, Kobayashi T, Nakadaira T, Nakamura K, Oyama Y, Sakashita K, Sekiguchi T, Tsukamoto T, Abe KE, Hasegawa M, Suzuki AT, Takeuchi Y, Yano T, Hayashino T, Hiraki T, Hirota S, Huang K, Jiang M, Nakamura KE, Nakaya T, Quilain B, Patel ND, Wendell RA, Anthony LHV, McCauley N, Pritchard A, Fukuda Y, Itow Y, Murase M, Muto F, Mijakowski P, Frankiewicz K, Jung CK, Li X, Palomino JL, Santucci G, Vilela C, Wilking MJ, Yanagisawa C, Ito S, Fukuda D, Ishino H, Kibayashi A, Koshio Y, Nagata H, Sakuda M, Xu C, Kuno Y, Wark D, Di Lodovico F, Richards B, Tacik R, Kim SB, Cole A, Thompson L, Okazawa H, Choi Y, Ito K, Nishijima K, Koshiba M, Totsuka Y, Suda Y, Yokoyama M, Calland RG, Hartz M, Martens K, Simpson C, Suzuki Y, Vagins MR, Hamabe D, Kuze M, Yoshida T, Ishitsuka M, Martin JF, Nantais CM, Tanaka HA, Konaka A, Chen S, Wan L, Zhang Y, Wilkes RJ, Minamino A. Search for Boosted Dark Matter Interacting with Electrons in Super-Kamiokande. Phys Rev Lett 2018; 120:221301. [PMID: 29906152 DOI: 10.1103/physrevlett.120.221301] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/16/2017] [Revised: 03/23/2018] [Indexed: 06/08/2023]
Abstract
A search for boosted dark matter using 161.9 kt yr of Super-Kamiokande IV data is presented. We search for an excess of elastically scattered electrons above the atmospheric neutrino background, with a visible energy between 100 MeV and 1 TeV, pointing back to the Galactic center or the Sun. No such excess is observed. Limits on boosted dark matter event rates in multiple angular cones around the Galactic center and Sun are calculated. Limits are also calculated for a baseline model of boosted dark matter produced from cold dark matter annihilation or decay. This is the first experimental search for boosted dark matter from the Galactic center or the Sun interacting in a terrestrial detector.
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Affiliation(s)
- C Kachulis
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
| | - K Abe
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - C Bronner
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - Y Hayato
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - M Ikeda
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - K Iyogi
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - J Kameda
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Kato
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - Y Kishimoto
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Ll Marti
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - M Miura
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - S Moriyama
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - M Nakahata
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Nakano
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - S Nakayama
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Okajima
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - A Orii
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - G Pronost
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - H Sekiya
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - M Shiozawa
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Sonoda
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - A Takeda
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - A Takenaka
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - H Tanaka
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - S Tasaka
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
| | - T Tomura
- Kamioka Observatory, Institute for Cosmic Ray Research, University of Tokyo, Kamioka, Gifu 506-1205, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - R Akutsu
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - T Kajita
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K Kaneyuki
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Nishimura
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - K Okumura
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K M Tsui
- Research Center for Cosmic Neutrinos, Institute for Cosmic Ray Research, University of Tokyo, Kashiwa, Chiba 277-8582, Japan
| | - L Labarga
- Department of Theoretical Physics, University Autonoma Madrid, Madrid 28049, Spain
| | - P Fernandez
- Department of Theoretical Physics, University Autonoma Madrid, Madrid 28049, Spain
| | - F D M Blaszczyk
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
| | - J Gustafson
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
| | - E Kearns
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - J L Raaf
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
| | - J L Stone
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - L R Sulak
- Department of Physics, Boston University, Boston, Massachusetts 02215, USA
| | - S Berkman
- Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T1Z4, Canada
| | - S Tobayama
- Department of Physics and Astronomy, University of British Columbia, Vancouver, British Columbia, V6T1Z4, Canada
| | - M Goldhaber
- Physics Department, Brookhaven National Laboratory, Upton, New York 11973, USA
| | - M Elnimr
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - W R Kropp
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - S Mine
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - S Locke
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - P Weatherly
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - M B Smy
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - H W Sobel
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - V Takhistov
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
| | - K S Ganezer
- Department of Physics, California State University, Dominguez Hills, Carson, California 90747, USA
| | - J Hill
- Department of Physics, California State University, Dominguez Hills, Carson, California 90747, USA
| | - J Y Kim
- Department of Physics, Chonnam National University, Kwangju 500-757, Korea
| | - I T Lim
- Department of Physics, Chonnam National University, Kwangju 500-757, Korea
| | - R G Park
- Department of Physics, Chonnam National University, Kwangju 500-757, Korea
| | - A Himmel
- Department of Physics, Duke University, Durham, North Carolina 27708, USA
| | - Z Li
- Department of Physics, Duke University, Durham, North Carolina 27708, USA
| | - E O'Sullivan
- Department of Physics, Duke University, Durham, North Carolina 27708, USA
| | - K Scholberg
- Department of Physics, Duke University, Durham, North Carolina 27708, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - C W Walter
- Department of Physics, Duke University, Durham, North Carolina 27708, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - T Ishizuka
- Junior College, Fukuoka Institute of Technology, Fukuoka, Fukuoka 811-0295, Japan
| | - T Nakamura
- Department of Physics, Gifu University, Gifu, Gifu 501-1193, Japan
| | - J S Jang
- GIST College, Gwangju Institute of Science and Technology, Gwangju 500-712, Korea
| | - K Choi
- Department of Physics and Astronomy, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - J G Learned
- Department of Physics and Astronomy, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - S Matsuno
- Department of Physics and Astronomy, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - S N Smith
- Department of Physics and Astronomy, University of Hawaii, Honolulu, Hawaii 96822, USA
| | - J Amey
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - R P Litchfield
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - W Y Ma
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - Y Uchida
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - M O Wascko
- Department of Physics, Imperial College London, London SW7 2AZ, United Kingdom
| | - S Cao
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - M Friend
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Hasegawa
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Ishida
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Ishii
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Kobayashi
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Nakadaira
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - K Nakamura
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Oyama
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - K Sakashita
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Sekiguchi
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - T Tsukamoto
- High Energy Accelerator Research Organization (KEK), Tsukuba, Ibaraki 305-0801, Japan
| | - K E Abe
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
| | - M Hasegawa
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
| | - A T Suzuki
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
| | - Y Takeuchi
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - T Yano
- Department of Physics, Kobe University, Kobe, Hyogo 657-8501, Japan
| | - T Hayashino
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - T Hiraki
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - S Hirota
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - K Huang
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - M Jiang
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - K E Nakamura
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - T Nakaya
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - B Quilain
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - N D Patel
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
| | - R A Wendell
- Department of Physics, Kyoto University, Kyoto, Kyoto 606-8502, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - L H V Anthony
- Department of Physics, University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - N McCauley
- Department of Physics, University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - A Pritchard
- Department of Physics, University of Liverpool, Liverpool L69 7ZE, United Kingdom
| | - Y Fukuda
- Department of Physics, Miyagi University of Education, Sendai, Miyagi 980-0845, Japan
| | - Y Itow
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8602, Japan
- Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, Nagoya University, Nagoya, Aichi 464-8602, Japan
| | - M Murase
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8602, Japan
| | - F Muto
- Institute for Space-Earth Environmental Research, Nagoya University, Nagoya, Aichi 464-8602, Japan
| | - P Mijakowski
- National Centre For Nuclear Research, Warsaw 00-681, Poland
| | - K Frankiewicz
- National Centre For Nuclear Research, Warsaw 00-681, Poland
| | - C K Jung
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - X Li
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - J L Palomino
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - G Santucci
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - C Vilela
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - M J Wilking
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - C Yanagisawa
- Department of Physics and Astronomy, State University of New York at Stony Brook, New York 11794-3800, USA
| | - S Ito
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - D Fukuda
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - H Ishino
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - A Kibayashi
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - Y Koshio
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - H Nagata
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - M Sakuda
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - C Xu
- Department of Physics, Okayama University, Okayama, Okayama 700-8530, Japan
| | - Y Kuno
- Department of Physics, Osaka University, Toyonaka, Osaka 560-0043, Japan
| | - D Wark
- Department of Physics, Oxford University, Oxford OX1 3PU, United Kingdom
- STFC, Rutherford Appleton Laboratory, Harwell Oxford, and Daresbury Laboratory, Warrington OX11 0QX, United Kingdom
| | - F Di Lodovico
- School of Physics and Astronomy, Queen Mary University of London, London E1 4NS, United Kingdom
| | - B Richards
- School of Physics and Astronomy, Queen Mary University of London, London E1 4NS, United Kingdom
| | - R Tacik
- Department of Physics, University of Regina, 3737 Wascana Parkway, Regina, Saskatchewan S4SOA2, Canada
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
| | - S B Kim
- Department of Physics, Seoul National University, Seoul 151-742, Korea
| | - A Cole
- Department of Physics and Astronomy, University of Sheffield, Sheffield S10 2TN, United Kingdom
| | - L Thompson
- Department of Physics and Astronomy, University of Sheffield, Sheffield S10 2TN, United Kingdom
| | - H Okazawa
- Department of Informatics in Social Welfare, Shizuoka University of Welfare, Yaizu, Shizuoka 425-8611, Japan
| | - Y Choi
- Department of Physics, Sungkyunkwan University, Suwon 440-746, Korea
| | - K Ito
- Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan
| | - K Nishijima
- Department of Physics, Tokai University, Hiratsuka, Kanagawa 259-1292, Japan
| | - M Koshiba
- The University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
| | - Y Totsuka
- The University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
| | - Y Suda
- Department of Physics, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
| | - M Yokoyama
- Department of Physics, University of Tokyo, Bunkyo, Tokyo 113-0033, Japan
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - R G Calland
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - M Hartz
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - K Martens
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - C Simpson
- Department of Physics, Oxford University, Oxford OX1 3PU, United Kingdom
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - Y Suzuki
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - M R Vagins
- Department of Physics and Astronomy, University of California, Irvine, Irvine, California 92697-4575, USA
- Kavli Institute for the Physics and Mathematics of the Universe (WPI), The University of Tokyo Institutes for Advanced Study, University of Tokyo, Kashiwa, Chiba 277-8583, Japan
| | - D Hamabe
- Department of Physics, Tokyo Institute of Technology, Meguro, Tokyo 152-8551, Japan
| | - M Kuze
- Department of Physics, Tokyo Institute of Technology, Meguro, Tokyo 152-8551, Japan
| | - T Yoshida
- Department of Physics, Tokyo Institute of Technology, Meguro, Tokyo 152-8551, Japan
| | - M Ishitsuka
- Department of Physics, Faculty of Science and Technology, Tokyo University of Science, Noda, Chiba 278-8510, Japan
| | - J F Martin
- Department of Physics, University of Toronto, Toronto, Ontario M5S 1A7, Canada
| | - C M Nantais
- Department of Physics, University of Toronto, Toronto, Ontario M5S 1A7, Canada
| | - H A Tanaka
- Department of Physics, University of Toronto, Toronto, Ontario M5S 1A7, Canada
| | - A Konaka
- TRIUMF, 4004 Wesbrook Mall, Vancouver, British Columbia V6T2A3, Canada
| | - S Chen
- Department of Engineering Physics, Tsinghua University, Beijing 100084, China
| | - L Wan
- Department of Engineering Physics, Tsinghua University, Beijing 100084, China
| | - Y Zhang
- Department of Engineering Physics, Tsinghua University, Beijing 100084, China
| | - R J Wilkes
- Department of Physics, University of Washington, Seattle, Washington 98195-1560, USA
| | - A Minamino
- Faculty of Engineering, Yokohama National University, Yokohama 240-8501, Japan
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Abstract
We review several current aspects of dark matter theory and experiment. We overview the present experimental status, which includes current bounds and recent claims and hints of a possible signal in a wide range of experiments: direct detection in underground laboratories, gamma-ray, cosmic ray, x-ray, neutrino telescopes, and the LHC. We briefly review several possible particle candidates for a weakly interactive massive particle (WIMP) and dark matter that have recently been considered in the literature. We pay particular attention to the lightest neutralino of supersymmetry as it remains the best motivated candidate for dark matter and also shows excellent detection prospects. Finally we briefly review some alternative scenarios that can considerably alter properties and prospects for the detection of dark matter obtained within the standard thermal WIMP paradigm.
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Affiliation(s)
- Leszek Roszkowski
- National Centre for Nuclear Research, Hoża 69, 00-681 Warsaw, Poland. Department of Physics and Astronomy, University of Sheffield, Sheffield S3 7RH, United Kingdom
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An H, Pospelov M, Pradler J, Ritz A. Directly Detecting MeV-Scale Dark Matter Via Solar Reflection. Phys Rev Lett 2018; 120:141801. [PMID: 29694128 DOI: 10.1103/physrevlett.120.141801] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/22/2017] [Revised: 11/15/2017] [Indexed: 06/08/2023]
Abstract
If dark matter (DM) particles are lighter than a few MeV/c^{2} and can scatter off electrons, their interaction within the solar interior results in a considerable hardening of the spectrum of galactic dark matter received on Earth. For a large range of the mass versus cross section parameter space, {m_{e},σ_{e}}, the "reflected" component of the DM flux is far more energetic than the end point of the ambient galactic DM energy distribution, making it detectable with existing DM detectors sensitive to an energy deposition of 10-10^{3} eV. After numerically simulating the small reflected component of the DM flux, we calculate its subsequent signal due to scattering on detector electrons, deriving new constraints on σ_{e} in the MeV and sub-MeV range using existing data from the XENON10/100, LUX, PandaX-II, and XENON1T experiments, as well as making projections for future low threshold direct detection experiments.
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Affiliation(s)
- Haipeng An
- Walter Burke Institute for Theoretical Physics, California Institute of Technology, Pasadena, California 91125, USA
- Department of Physics, Tsinghua University, Beijing 100084, China
| | - Maxim Pospelov
- Department of Physics and Astronomy, University of Victoria, Victoria, British Columbia V8P 5C2, Canada
- Perimeter Institute for Theoretical Physics, Waterloo, Ontario N2J 2W9, Canada
| | - Josef Pradler
- Institute of High Energy Physics, Austrian Academy of Sciences, 1050 Vienna, Austria
| | - Adam Ritz
- Department of Physics and Astronomy, University of Victoria, Victoria, British Columbia V8P 5C2, Canada
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Kamada A, Kim HJ, Kim H, Sekiguchi T. Self-Heating Dark Matter via Semiannihilation. Phys Rev Lett 2018; 120:131802. [PMID: 29694186 DOI: 10.1103/physrevlett.120.131802] [Citation(s) in RCA: 2] [Impact Index Per Article: 0.3] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 08/08/2017] [Revised: 01/30/2018] [Indexed: 06/08/2023]
Abstract
The freeze-out of dark matter (DM) depends on the evolution of the DM temperature. The DM temperature does not have to follow the standard model one, when the elastic scattering is not sufficient to maintain the kinetic equilibrium. We study the temperature evolution of the semiannihilating DM, where a pair of the DM particles annihilate into one DM particle and another particle coupled to the standard model sector. We find that the kinetic equilibrium is maintained solely via semiannihilation until the last stage of the freeze-out. After the freeze-out, semiannihilation converts the mass deficit to the kinetic energy of DM, which leads to nontrivial evolution of the DM temperature. We argue that the DM temperature redshifts like radiation as long as the DM self-interaction is efficient. We dub this novel temperature evolution as self-heating. Notably, the structure formation is suppressed at subgalactic scales like keV-scale warm DM but with GeV-scale self-heating DM if the self-heating lasts roughly until the matter-radiation equality. The long duration of the self-heating requires the large self-scattering cross section, which in turn flattens the DM density profile in inner halos. Consequently, self-heating DM can be a unified solution to apparent failures of cold DM to reproduce the observed subgalactic scale structure of the Universe.
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Affiliation(s)
- Ayuki Kamada
- Center for Theoretical Physics of the Universe, Institute for Basic Science (IBS), Daejeon 34126, Korea
| | - Hee Jung Kim
- Department of Physics, KAIST, Daejeon 34141, Korea
| | - Hyungjin Kim
- Center for Theoretical Physics of the Universe, Institute for Basic Science (IBS), Daejeon 34126, Korea
- Department of Physics, KAIST, Daejeon 34141, Korea
- Department of Particle Physics and Astrophysics, Weizmann Institute of Science, Rehovot 7610001, Israel
| | - Toyokazu Sekiguchi
- Center for Theoretical Physics of the Universe, Institute for Basic Science (IBS), Daejeon 34126, Korea
- Research Center for the Early Universe (RESCEU), Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan
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Arcadi G, Dutra M, Ghosh P, Lindner M, Mambrini Y, Pierre M, Profumo S, Queiroz FS. The waning of the WIMP? A review of models, searches, and constraints. Eur Phys J C Part Fields 2018; 78:203. [PMID: 31258403 PMCID: PMC6560773 DOI: 10.1140/epjc/s10052-018-5662-y] [Citation(s) in RCA: 33] [Impact Index Per Article: 5.5] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 11/12/2017] [Accepted: 02/22/2018] [Indexed: 06/08/2023]
Abstract
Weakly Interacting Massive Particles (WIMPs) are among the best-motivated dark matter candidates. No conclusive signal, despite an extensive search program that combines, often in a complementary way, direct, indirect, and collider probes, has been detected so far. This situation might change in near future due to the advent of one/multi-TON Direct Detection experiments. We thus, find it timely to provide a review of the WIMP paradigm with focus on a few models which can be probed at best by these facilities. Collider and Indirect Detection, nevertheless, will not be neglected when they represent a complementary probe.
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Affiliation(s)
- Giorgio Arcadi
- Max Planck Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - Maíra Dutra
- Laboratoire de Physique Théorique, CNRS, Univ. Paris-Sud, Université Paris-Saclay, 91405 Orsay, France
| | - Pradipta Ghosh
- Laboratoire de Physique Théorique, CNRS, Univ. Paris-Sud, Université Paris-Saclay, 91405 Orsay, France
- Centre de Physique Théorique, Ecole Polytechnique, CNRS, Université Paris-Saclay, 91128 Palaiseau Cedex, France
| | - Manfred Lindner
- Max Planck Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
| | - Yann Mambrini
- Laboratoire de Physique Théorique, CNRS, Univ. Paris-Sud, Université Paris-Saclay, 91405 Orsay, France
| | - Mathias Pierre
- Laboratoire de Physique Théorique, CNRS, Univ. Paris-Sud, Université Paris-Saclay, 91405 Orsay, France
| | - Stefano Profumo
- Department of Physics, University of California, Santa Cruz, 1156 High St, Santa Cruz, CA 95060 USA
- Santa Cruz Institute for Particle Physics, Santa Cruz, 1156 High St, Santa Cruz, CA 95060 USA
| | - Farinaldo S. Queiroz
- Max Planck Institut für Kernphysik, Saupfercheckweg 1, 69117 Heidelberg, Germany
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Choi SM, Lee HM, Seo MS. SIMP dark matter and its cosmic abundances. EPJ Web Conf 2018. [DOI: 10.1051/epjconf/201816806009] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
We give a review on the thermal average of the annihilation cross-sections for 3 → 2 and general higher-order processes. Thermal average of higher order annihilations highly depend on the velocity of dark matter, especially, for the case with resonance poles. We show such examples for scalar dark matter in gauged Z3 models.
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Choi SM, Kang YJ, Lee HM. Forbidden Channels and SIMP Dark Matter. EPJ Web Conf 2018. [DOI: 10.1051/epjconf/201816806010] [Citation(s) in RCA: 0] [Impact Index Per Article: 0] [Reference Citation Analysis] [What about the content of this article? (0)] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/14/2022] Open
Abstract
In this review, we focus on dark matter production from thermal freeze-out with forbidden channels and SIMP processes. We show that forbidden channels can be dominant to produce dark matter depending on the dark photon and / or dark Higgs mass compared to SIMP.
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Davis JH. Probing Sub-GeV Mass Strongly Interacting Dark Matter with a Low-Threshold Surface Experiment. Phys Rev Lett 2017; 119:211302. [PMID: 29219413 DOI: 10.1103/physrevlett.119.211302] [Citation(s) in RCA: 3] [Impact Index Per Article: 0.4] [Reference Citation Analysis] [What about the content of this article? (0)] [Affiliation(s)] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Received: 09/06/2017] [Indexed: 06/07/2023]
Abstract
Using data from the ν-cleus detector, based on the surface of Earth, we place constraints on dark matter in the form of strongly interacting massive particles (SIMPs) which interact with nucleons via nuclear-scale cross sections. For large SIMP-nucleon cross sections, the sensitivity of traditional direct dark matter searches using underground experiments is limited by the energy loss experienced by SIMPs, due to scattering with the rock overburden and experimental shielding on their way to the detector apparatus. Hence, a surface-based experiment is ideal for a SIMP search, despite the much larger background resulting from the lack of shielding. We show using data from a recent surface run of a low-threshold cryogenic detector that values of the SIMP-nucleon cross section up to approximately 10^{-27} cm^{2} can be excluded for SIMPs with masses above 100 MeV.
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Affiliation(s)
- Jonathan H Davis
- Theoretical Particle Physics and Cosmology, Department of Physics, King's College London, London WC2R 2LS, United Kingdom
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