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Gammev: Fermilab Axion-Like Particle Photon Regeneration Results
GammeV: Fermilab Axion-like Particle Photon Regeneration Results William Wester Fermilab, MS222, Batavia IL, USA presented on behalf of the GammeV Collaboration DOI: http://dx.doi.org/10.3204/DESY-PROC-2008-02/wester william GammeV is an axion-like particle photon regeneration experiment conducted at Fermilab that employs the light shining through a wall technique. We obtain limits on the cou- pling of a photon to an axion-like particle that extend previous limits for both scalar and pseudoscalar axion-like particles in the milli-eV mass range. We are able to exclude the axion-like particle interpretation of the anomalous PVLAS 2006 result by more than 5 standard deviations. 1 Introduction The question, What are the particles that make up the dark matter of the universe?, is one of the most fundamental scientific questions today. Besides weakly interacting massive particles (WIMPs) such as neutralinos, axion-like particles or other weakly interacting sub-eV particles (WISPs) are highly motivated dark matter particle candidates since they have properties that might explain the cosmic abundance of dark matter. The milli-eV mass scale is of particular interest in modern particle physics since that mass scale may be constructed with a see-saw between the Planck and TeV mass scales, and may be related to neutrino mass differences, the dark energy density expressed in (milli-eV)4, and known dark matter candidates such as gravitinos and axion-like particles. In 2006, the PVLAS experiment reported [1] anomalous polarization effects in the presence of a magnetic field including polarization rotation and el- lipticity generation that could be interpreted as being mediated by an axion-like particle in the milli-eV mass range with a unexpectedly strong coupling to photons. -
Circular and Linear Magnetic Birefringences in Xenon at =1064 Nm
Downloaded from orbit.dtu.dk on: Oct 06, 2021 Circular and linear magnetic birefringences in xenon at =1064 nm Cadene, Agathe; Fouche, Mathilde; Rivere, Alice; Battesti, Remy; Coriani, Sonia; Rizzo, Antonio; Rizzo, Carlo Published in: Journal of Chemical Physics Link to article, DOI: 10.1063/1.4916049 Publication date: 2015 Document Version Publisher's PDF, also known as Version of record Link back to DTU Orbit Citation (APA): Cadene, A., Fouche, M., Rivere, A., Battesti, R., Coriani, S., Rizzo, A., & Rizzo, C. (2015). Circular and linear magnetic birefringences in xenon at =1064 nm. Journal of Chemical Physics, 142(12), [124313]. https://doi.org/10.1063/1.4916049 General rights Copyright and moral rights for the publications made accessible in the public portal are retained by the authors and/or other copyright owners and it is a condition of accessing publications that users recognise and abide by the legal requirements associated with these rights. Users may download and print one copy of any publication from the public portal for the purpose of private study or research. You may not further distribute the material or use it for any profit-making activity or commercial gain You may freely distribute the URL identifying the publication in the public portal If you believe that this document breaches copyright please contact us providing details, and we will remove access to the work immediately and investigate your claim. Circular and linear magnetic birefringences in xenon at λ = 1064 nm Agathe Cadène, Mathilde Fouché, Alice Rivère, -
A Statistical Framework for the Characterisation of WIMP Dark Matter with the LUX-ZEPLIN Experiment
A statistical framework for the characterisation of WIMP dark matter with the LUX-ZEPLIN experiment Ibles Olcina Samblas Department of Physics A thesis submitted for the degree of Doctor of Philosophy November 2019 Abstract Several pieces of astrophysical evidence, from galactic to cosmological scales, indicate that most of the mass in the universe is composed of an invisible and essentially collisionless substance known as dark matter. A leading particle candidate that could provide the role of dark matter is the Weakly Interacting Massive Particle (WIMP), which can be searched for directly on Earth via its scattering off atomic nuclei. The LUX-ZEPLIN (LZ) experiment, currently under construction, employs a multi-tonne dual-phase xenon time projection chamber to search for WIMPs in the low background environment of the Davis Campus at the Sanford Underground Research Facility (South Dakota, USA). LZ will probe WIMP interactions with unprecedented sensitivity, starting to explore regions of the WIMP parameter space where new backgrounds are expected to arise from the elastic scattering of neutrinos off xenon nuclei. In this work the theoretical and computational framework underlying the calculation of the sensitivity of the LZ experiment to WIMP-nucleus scattering interactions is presented. After its planned 1000 live days of exposure, LZ will be able to achieve a 3σ discovery for spin independent cross sections above 3.0 10 48 cm2 at 40 GeV/c2 WIMP mass or exclude at × − 90% CL a cross section of 1.3 10 48 cm2 in the absence of signal. The sensitivity of LZ × − to spin-dependent WIMP-neutron and WIMP-proton interactions is also presented. -
Strategies for the Detection of Dark Matter
Bernard Sadoulet Dept. of Physics /LBNL UC Berkeley UC Institute for Nuclear and Particle Astrophysics and Cosmology (INPAC) Strategies for the Detection of Dark Matter What do we know? What have we achieved so far? Strategies for the future Strategies for the Detection f Dark Matter Hanoi 10 Aug 06 1 B.Sadoulet 1. What do we know? 2. What has been achieved? 3. Strategies for the future Standard Model of Cosmology A surprising but consistent picture Non Baryonic Λ Dark Matter Ω Ωmatter Not ordinary matter (Baryons) Nucleosynthesis Ω >> Ω = 0.047 ± 0.006 from m b WMAP Mostly cold: Not light neutrinos≠ small scale structure mv < .17eV Large Scale structure+baryon oscillation + Lyman α Strategies for the Detection f Dark Matter Hanoi 10 Aug 06 2 B.Sadoulet 1. What do we know? 2. What has been achieved? 3. Strategies for the future Ongoing Systematic Mapping dark matter and energy non baryonic Λ Quintessence baryonic clumped H2? ? gas Primordial Black Holes VMO Mirror branes ? exotic particles dust Energy in bulk MACHOs thermal non-thermal SuperWIMPs Light Neutrinos WIMPs Axions Wimpzillas Most baryonic forms excluded (independently of BBN, CMB) Particles: well defined if thermal (difficult when athermal) Additional dimensions? Strategies for the Detection f Dark Matter Hanoi 10 Aug 06 3 B.Sadoulet 1. What do we know? 2. What has been achieved? 3. Strategies for the future Standard Model of Particle Physics Fantastic success but Model is unstable Why is W and Z at ≈100 Mp? Need for new physics at that scale supersymmetry additional dimensions Flat: Cheng et al. -
Book of Abstracts Ii Contents
DMSS: A Dark Matter Summer School Monday, 16 July 2018 - Friday, 20 July 2018 Other Institute Book of Abstracts ii Contents Introduction to Dark Matter .................................. 1 Supersymmetry ......................................... 1 Large Scale Structure Formation ................................ 1 Roundtable Discussions ..................................... 1 Dark Matter in the Milky Way ................................. 1 Neutrinos ............................................ 1 Direct Detection of Dark Matter ................................ 1 Roundtable Discussions ..................................... 1 Indirect Dark Matter Searches ................................. 2 Statistical Methods used in Dark Matter ............................ 2 Axions .............................................. 2 Cosmic Microwave Background ................................ 2 Non-SUSY Dark Matter ..................................... 2 Roundtable Discussions ..................................... 2 Dark Matter at the LHC ..................................... 2 Dark Energy ........................................... 2 Roundtable Discussions ..................................... 3 Roundtable Discussions ..................................... 3 Dark Matter search activity at the University of Montreal .................. 3 Extra Dimensions in High-Mass Diphoton Spectrum at 13 TeV ............... 3 The XENONnT Time Projection Chamber .......................... 4 Calibration of the XENON1T experiment at low energies using a Kr83m source . 4 Gravitational-wave -
Arxiv:2101.08781V1 [Hep-Ph] 21 Jan 2021
MI-TH-2135 PASSAT at Future Neutrino Experiments: Hybrid Beam-Dump-Helioscope Facilities to Probe Light Axion-Like Particles P. S. Bhupal Dev,1, ∗ Doojin Kim,2, y Kuver Sinha,3, z and Yongchao Zhang4, 1, x 1Department of Physics and McDonnell Center for the Space Sciences, Washington University, St. Louis, MO 63130, USA 2Mitchell Institute for Fundamental Physics and Astronomy, Department of Physics and Astronomy, Texas A&M University, College Station, TX 77843, USA 3Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019, USA 4School of Physics, Southeast University, Nanjing 211189, China There are broadly three channels to probe axion-like particles (ALPs) produced in the laboratory: through their subsequent decay to Standard Model (SM) particles, their scattering with SM particles, or their subsequent conversion to photons. Decay and scattering are the most commonly explored channels in beam-dump type experiments, while conversion has typically been utilized by light- shining-through-wall (LSW) experiments. A new class of experiments, dubbed PASSAT (Particle Accelerator helioScopes for Slim Axion-like-particle deTection), has been proposed to make use of the ALP-to-photon conversion in a novel way: ALPs, after being produced in a beam-dump setup, turn into photons in a magnetic field placed near the source. It has been shown that such hybrid beam-dump-helioscope experiments can probe regions of parameter space that have not been investigated by other laboratory-based experiments, hence providing complementary information; in particular, they probe a fundamentally different region than decay or LSW experiments. We propose the implementation of PASSAT in future neutrino experiments, taking a DUNE-like experiment as an example. -
LUX Detector
LUX results and LZ sensitivity to dark matter WIMPs Vitaly A. Kudryavtsev University of Sheffield for the LUX and LZ Collaborations Outline n Dark matter direct detection with two-phase noble element instruments. n LUX detector. n LUX results: o WIMPs – spin-independent interactions; o WIMPs – spin-dependent interactions; o Axions and axion-like particles (ALPs). o Modulation search. n LZ detector. n Backgrounds n Sensitivity to WIMPs. n Conclusions. ICNFP2018, 6 July 2018 Vitaly Kudryavtsev 2 Principle of WIMP detection in LXe TPC n Liquid xenon time projection chamber – LXe TPC. n S1 – primary scintillation. n S2 –secondary scintillation, proportional to ionisation. n Position reconstruction based on the light pattern in the PMTs and delay between S2 and S1. ICNFP2018, 6 July 2018 Vitaly Kudryavtsev 3 Advantages of LXe n Good scintillator. n Two-phase -> TPC with good position resolution. n Self-shielding. n Good discrimination between electron recoils (ERs) and nuclear recoils (NRs). n High atomic mass: spin-independent cross- section ∝ A2 n Presence of even-odd isotopes (odd number of neutrons) for spin-dependent studies. n Other physics: o Axion search, o Neutrinoless double-beta decay. LZ Collaboration, LZ TDR, 1703.09144v1 [physics.ins-det] ICNFP2018, 6 July 2018 Vitaly Kudryavtsev 4 LUX Collaboration ² Brown University ² University at Albany, SUNY ² Imperial College London ² University College London ² LIP Coimbra, Portugal ² University of California, Berkeley ² Lawrence Berkley National Laboratory ² University of California, Davis -
Signal Processing in the PVLAS Experiment
Signal Processing in the PVLAS Experiment E. ZAVATTINI1, G. ZAVATTINI4, G. RUOSO2, E. POLACCO3, E. MILOTTI,1, M. KARUZA1, U. GASTALDI 2, G. DI DOMENICO4, F. DELLA VALLE1, R. CIMINO5, S. CARUSOTTO3, G. CANTATORE1, M. BREGANT1 1 - Università e I.N.F.N. Trieste, Via Valerio 2, 34127 Trieste, ITALY 2 - Lab. Naz.di Legnaro dell’I.N.F.N., Viale dell’Università 2, 35020 Legnaro, ITALY 3 - Università e I.N.F.N. Pisa, Via F. Buonarroti 2, 56100 Pisa, ITALY 4 - Università e I.N.F.N. Ferrara, Via del Paradiso 12, 44100 Ferrara, ITALY 5 - Lab. Naz.di Frascati dell’I.N.F.N., Via E. Fermi 40, 00044 Frascati, ITALY [email protected] http://www.ts.infn.it/experiments/pvlas/ Abstract: - Nonlinear interactions of light with light are well known in quantum electronics, and it is quite common to generate harmonic or subharmonic beams from a primary laser with photonic crystals. One suprising result of quantum electrodynamics is that because of the quantum fluctuations of charged fields, the same can happen in vacuum. The virtual charged particle pairs can be polarized by an external field and vacuum can thus become birefringent: the PVLAS experiment was originally meant to explore this strange quantum regime with optical methods. Since its inception PVLAS has found a new, additional goal: in fact vacuum can become a dichroic medium if we assume that it is filled with light neutral particles that couple to two photons, and thus PVLAS can search for exotic particles as well. PVLAS implements a complex signal processing scheme: here we describe the double data acquisition chain and the data analysis methods used to process the experimental data. -
Axions (A0) and Other Very Light Bosons, Searches for See the Related Review(S): Axions and Other Similar Particles
Citation: M. Tanabashi et al. (Particle Data Group), Phys. Rev. D 98, 030001 (2018) Axions (A0) and Other Very Light Bosons, Searches for See the related review(s): Axions and Other Similar Particles A0 (Axion) MASS LIMITS from Astrophysics and Cosmology These bounds depend on model-dependent assumptions (i.e. — on a combination of axion parameters). VALUE (MeV) DOCUMENT ID TECN COMMENT We do not use the following data for averages, fits, limits, etc. ••• ••• >0.2 BARROSO 82 ASTR Standard Axion >0.25 1 RAFFELT 82 ASTR Standard Axion >0.2 2 DICUS 78C ASTR Standard Axion MIKAELIAN 78 ASTR Stellar emission >0.3 2 SATO 78 ASTR Standard Axion >0.2 VYSOTSKII 78 ASTR Standard Axion 1 Lower bound from 5.5 MeV γ-ray line from the sun. 2 Lower bound from requiring the red giants’ stellar evolution not be disrupted by axion emission. A0 (Axion) and Other Light Boson (X 0) Searches in Hadron Decays Limits are for branching ratios. VALUE CL% DOCUMENT ID TECN COMMENT We do not use the following data for averages, fits, limits, etc. ••• ••• <2 10 10 95 1 AAIJ 17AQ LHCB B+ K+ X 0 (X 0 µ+ µ ) × − → → − <3.7 10 8 90 2 AHN 17 KOTO K0 π0 X 0, m = 135 MeV × − L → X 0 11 3 0 0 + <6 10− 90 BATLEY 17 NA48 K± π± X (X µ µ−) × 4 → 0 0 →+ WON 16 BELL η γ X (X π π−) 9 5 0→ 0 0 → 0 + <1 10− 95 AAIJ 15AZ LHCB B K∗ X (X µ µ−) × 6 6 0 → 0 0 →+ <1.5 10− 90 ADLARSON 13 WASA π γ X (X e e−), × m→ = 100 MeV→ X 0 <2 10 8 90 7 BABUSCI 13B KLOE φ η X0 (X 0 e+ e ) × − → → − 8 ARCHILLI 12 KLOE φ η X0, X 0 e+ e → → − <2 10 15 90 9 GNINENKO 12A BDMP π0 γ X 0 (X 0 e+ e ) × − → → − -
Dark Matter in Nuclear Physics
Dark Matter in Nuclear Physics George Fuller (UCSD), Andrew Hime (LANL), Reyco Henning (UNC), Darin Kinion (LLNL), Spencer Klein (LBNL), Stefano Profumo (Caltech) Michael Ramsey-Musolf (Caltech/UW Madison), Robert Stokstad (LBNL) Introduction A transcendent accomplishment of nuclear physics and observational cosmology has been the definitive measurement of the baryon content of the universe. Big Bang Nucleosynthesis calculations, combined with measurements made with the largest new telescopes of the primordial deuterium abundance, have inferred the baryon density of the universe. This result has been confirmed by observations of the anisotropies in the Cosmic Microwave Background. The surprising upshot is that baryons account for only a small fraction of the observed mass and energy in the universe. It is now firmly established that most of the mass-energy in the Universe is comprised of non-luminous and unknown forms. One component of this is the so- called “dark energy”, believed to be responsible for the observed acceleration of the expansion rate of the universe. Another component appears to be composed of non-luminous material with non-relativistic kinematics at the current epoch. The relationship between the dark matter and the dark energy is unknown. Several national studies and task-force reports have found that the identification of the mysterious “dark matter” is one of the most important pursuits in modern science. It is now clear that an explanation for this phenomenon will require some sort of new physics, likely involving a new particle or particles, and in any case involving physics beyond the Standard Model. A large number of dark matter studies, from theory to direct dark matter particle detection, involve nuclear physics and nuclear physicists. -
Gammev: Fermilab Axion-Like Particle Photon Regeneration Results
GammeV: Fermilab Axion-like Particle Photon Regeneration Results William Wester Fermilab, MS222, Batavia IL, USA presented on behalf of the GammeV Collaboration DOI: http://dx.doi.org/10.3204/DESY-PROC-2008-02/wester william GammeV is an axion-like particle photon regeneration experiment conducted at Fermilab that employs the light shining through a wall technique. We obtain limits on the cou- pling of a photon to an axion-like particle that extend previous limits for both scalar and pseudoscalar axion-like particles in the milli-eV mass range. We are able to exclude the axion-like particle interpretation of the anomalous PVLAS 2006 result by more than 5 standard deviations. 1 Introduction The question, What are the particles that make up the dark matter of the universe?, is one of the most fundamental scientific questions today. Besides weakly interacting massive particles (WIMPs) such as neutralinos, axion-like particles or other weakly interacting sub-eV particles (WISPs) are highly motivated dark matter particle candidates since they have properties that might explain the cosmic abundance of dark matter. The milli-eV mass scale is of particular interest in modern particle physics since that mass scale may be constructed with a see-saw between the Planck and TeV mass scales, and may be related to neutrino mass differences, the dark energy density expressed in (milli-eV)4, and known dark matter candidates such as gravitinos and axion-like particles. In 2006, the PVLAS experiment reported [1] anomalous polarization effects in the presence of a magnetic field including polarization rotation and el- lipticity generation that could be interpreted as being mediated by an axion-like particle in the milli-eV mass range with a unexpectedly strong coupling to photons. -
Where the Complications Start
4 P. Grang´eet al.: The fine-tuning problem revisited in the light of the Taylor-Lagrange renormalization scheme the necessary (ultra-soft) cut-o in the calculation of the integral. After an evident change of variable, we get 3M 4 X M 2 ⇥ = H dX f H X (16) 1b,H 32⌅2v2 X +1 Λ2 ↵0 ⌃ ⌥ 3M 4 1 M 2 = H dX 1 f H X . 32⌅2v2 − X +1 Λ2 ↵0 ⌃ ⌥ ⌃ ⌥ The first term under the integral can be reduced to a pseudo-function, using (11). Indeed, with Z =1/X,we have dZ M 2 1 dXf(X)= f H (17) Z2 Λ2 Z ↵0 ↵0 ⌃ ⌥ 1 = dZ Pf Z2 ↵0 ⌃ ⌥ 1 = =0. −Z ⇧ where the complications start ⇧ a ⇧ one explicit mass scale of the Standard Model is a mass-squared parameter The notation f(u) simply indicates⇧ that f(u) should be taken at the value |u = a, the lower limit of integration be- defining the leading orderFig. shape 1. Radiativeof the Mexican corrections Hat to the Higgs mass in the Stan- dard Model in second order of perturbation theory. For simplic- ing taken care of by the definition of the pseudo-function. V()ϕ D 2 n mass. The “cancellation” of massless bosons to give ity, we have not shown contributions from ghosts or Goldstone This result is reminiscent of the property d p(p ) = 0, a massive boson, as anticipated by Anderson and • to get the correct shape for electroweak developed in the 1964 papers, is the famous Higgs for any n, in DR [15].