Search

Your search keyword '"WIMP"' showing total 89 results
Start Over Descriptor "WIMP" Publisher hal ccsd
89 results on '"WIMP"'

1. Détection directionnelle de WIMP et recherche d'axions en dimensions supplémentaires avec le détecteur MIMAC

Author

Beaufort, Cyprien and Beaufort, Cyprien

Subjects
axions, [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], WIMP, MIMAC, extra dimensions, NEWS-G, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Facteur de quenching en ionisation, directionality, direct detection, dimensions supplémentaires, Ionization Quenching Factor, détection directe, [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], directionnalité
Abstract

While converging observations motivate the existence of a dark matter accounting for 84% of the mass of the universe, the nature of such a particle remains unknown and extensive searches are carried out, in particular concerning the WIMP and the axion. Directional detection correlates the direction of WIMP-induced nuclear recoils with the motion of the solar system in the galactic dark matter halo, thus providing a unique signature for WIMP identification even beyond the neutrino floor. The gaseous directional detector MIMAC measures the energy of a particle and reconstructs its track in 3D. This thesis investigates directional detection in the keV-range, for probing WIMPs with masses down to GeV, only accessible when operating the MIMAC detector at high gain (>10^4). We demonstrate that in these conditions, the interplay between the ionic and the electronic signals distorts the track reconstruction while it improves the detector sensitivity. The development of SimuMimac, a new simulation tool reproducing the MIMAC measurements, leads us to a procedure for extracting the electronic current from any measurements, allowing for head-tail recognition and providing new directional tools. We evaluate the directional performance of the MIMAC detector by the reconstruction of mono-energetic neutron spectra at 27 keV and 8 keV, achieving a 15° angular resolution and thus demonstrating for the first time that a detector can successfully access directionality in the keV-range. In this low-energy region, a nuclear recoil only releases part of its energy as ionization, and the kinetic energy must be inferred from the Ionization Quenching Factor (IQF). We measure the IQF of protons in methane in the keV-range and we conclude that this crucial quantity should no longer be determined by simulations. When operating at high gain, the MIMAC detector could also search for axions propagating in large extra dimensions. In this framework, axions with masses in the keV-range would be trapped into the solar gravitational field, for which we derive a number density of 10^7 cm^{-3} on Earth. By refining the model and updating the constraints, we reduce by orders of magnitude the $a\rightarrow\gamma\gamma$ event rate for the higher-dimensional axion in a MIMAC-like detector. The axion remains a promising probe for extra dimensions while it offers explanations for multiple puzzling solar observations., Alors que de multiples observations indiquent que la matière noire représenterait 84% de la masse de l'univers, la nature de cette particule demeure inconnue et les recherches expérimentales s'intensifient, notamment concernant le WIMP et l'axion. La détection directionnelle constitue une signature unique pour l'identification de WIMP par la corrélation entre la direction des reculs nucléaires induits par des WIMP et le mouvement du système solaire dans le halo galactique. Le détecteur gazeux directionnel MIMAC mesure l'énergie d'une particule et reconstruit sa trace en 3D. Cette thèse étudie la détection directionnelle dans la gamme du keV qui n'est accessible qu'en travaillant à haut gain (>10^4). Nous démontrons que dans ces conditions, le signal ionique vient perturber la reconstruction de la trace tout en améliorant la sensibilité du détecteur. L'implémentation de SimuMimac, un nouvel outil de simulation en accord avec les données, nous a conduit à élaborer une procédure pour extraire le courant électronique dans nos mesures, permettant de ce fait la reconnaissance du sens de la trace et le développement de nouveaux outils directionnels. Les performances directionnelles de MIMAC sont évaluées par la reconstruction de spectres neutroniques mono-énergétiques à 27 keV et 8 keV. Nous obtenons une résolution angulaire de 15° ce qui démontre pour la première fois qu'un détecteur peut accéder à la directionnalité dans la gamme du keV. À ces basses énergies, seule une partie de l'énergie d'un recul nucléaire est déposée sous forme d'ionisation et l'énergie cinétique doit donc être déterminée à l'aide du facteur de quenching en ionisation. Nous avons mesuré ce facteur pour des protons dans du méthane et nous en concluons que cette quantité essentielle doit systématiquement être mesurée et non plus simulée. En travaillant à haut gain, MIMAC pourrait aussi détecter des axions se propageant dans des dimensions supplémentaires. Une partie de ces axions pourrait être attrapée dans le champ gravitationnel solaire et nous calculons une densité de 10^7 cm^{-3} au niveau de la Terre. En affinant le modèle et les contraintes correspondantes, nous réduisons de plusieurs ordres de grandeur le taux d'événement $a\rightarrow\gamma\gamma$ dans un détecteur tel que MIMAC. En plus d'expliquer plusieurs observations solaires, l'axion constitue une particule prometteuse pour tester l'existence de dimensions supplémentaires.

Published
2022

2. Computational Approach to Design a Liquid Argon time-of-flight Positron Emission Tomography (LAr-TOF-PET) Scanner Using Monte Carlo Method

Author

A. Zabihi, M. Wada, A. Ramirez, A. Renshaw, X. Li, C. Galbiati, Michela Lai, D. Franco, F. Gabriele, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
electron, radiation detector, monte carlo method, positron emission tomography, medicine, LAr+Xe scintillator, Geant4, hypothetical particles, advancing LAr detector technology, weakly interacting massive particles, photomultipliers, commercial PET scanners, localization, Sensitivity, SiPM technology, Cherenkov, Time-Of-Flight PET, LAr-TOF-PET, time resolution, Monte Carlo, photomultiplier, Total-Body PET, electronics, Detectors, Monte Carlo methods, Liquid Argonv, annihilation, quality, cryogenics, Scintillators, technology, argon, time projection chambers, positron, readout, time information, silicon photomultipliers, performance, timing resolution, WIMP, SiPM, argon time-of-flight Positron Emission Tomography scanner, time-of-flight, dark matter, improved time resolution, cryogenic electronics, ionization, Image quality, cancer, Timing, Field-Of-View total-body scanner, liquid, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], positron annihilations, spatial resolution, scintillation induced ionization electrons, scintillation counter, electron positron, detector, PET images, low-dose PET scans, silicon, resolution, Liquids, liquid argon, time projection chamber, radiation, low-radioactivity liquid argon scintillator, DarkSide Collaboration, silicon radiation detectors, LAr+Xe scintillation light, gamma ray, liquid scintillation detectors
Abstract

International audience; This paper presents the design of a new Positron Emission Tomography (PET) with improved time resolution, Time-Of-Flight PET (TOF-PET). Using the time information improves image quality and reduces the radiation dose inoculated to patients. Extended Field-Of-View (FOV) total-body scanner built from low-radioactivity liquid argon (LAr) scintillator (LAr-TOF-PET) and silicon photomultipliers (SiPMs) are readout by fast cryogenic electronics. This new concept is based on the emerging technology coming from the field of direct dark matter searches for weakly interacting massive particles (WIMPs). The DarkSide Collaboration has been particularly successful in demonstrating the true power of the advancing LAr detector technology. SiPM technology has many broader applications in science and industry, most notably in medical physics, where exquisite timing resolution of SiPMs could revolutionize PET, one of the key tools in a diagnosis of cancer, allowing one to substantially improve precision and at the same time minimize adverse side-effects to the patient. We simulated this design using Geant4 toolkit while following the National Electrical Manufacturers Association’s evaluation tests for performance assessment. We will present results that highlight a 200-fold increase in sensitivity, spatial resolutions comparable to commercial PET scanners and produce PET images from 15-30 second scans, faster than traditional 30-35-minute scans. Further studies will involve optimizing the layer thickness of LAr+Xe. Moreover, scintillation induced ionization electrons can produce Cherenkov radiation along with the LAr+Xe scintillation light. With the LAr+Xe scintillator and SiPMs of 3Dπ, we can use the precise TOF info of gamma rays to improve the localization of individual positron annihilations, and as one example benefit, provide low-dose PET scans for patients who may be at high risk for exposure to radiation.

Published
2021
Full Text
View/download PDF

3. Combined Dark Matter searches from dwarf spheroidal galaxies observations by Fermi-LAT, HAWC, H.E.S.S., MAGIC, and VERITAS

Author

Daniel Kerszberg, Céline Armand, Eric Charles, Mattia di Mauro, Chiara Giuri, J. Patrick Harding, Tjark Miener, Emmanuel Moulin, Louise Oakes, Vincent Poireau, Elisa Pueschel, Javier Rico, Lucia Rinchiuso, Daniel Salazar-Gallegos, Kirsten Tollefson, Benjamin Zitzer, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, HAWC, H.E.S.S., MAGIC, and VERITAS

Subjects
History, WIMP, background, Astrophysics::High Energy Astrophysical Phenomena, dark matter: mass, dark matter: annihilation, Astrophysics::Cosmology and Extragalactic Astrophysics, GeV, sensitivity, MAGIC, GLAST, Computer Science Applications, Education, HESS, overlap, TeV, VERITAS, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], HAWC, Astrophysics::Galaxy Astrophysics
Abstract

Dwarf spheroidal galaxies (dSphs) are ideal targets for Dark Matter (DM) indirect searches due to their high DM content and their negligible expected astrophysical background. In this presentation, we report on the combined analysis of the observations of 20 dSphs by Fermi-LAT, HAWC, H.E.S.S., MAGIC, and VERITAS collaborations in the search for DM, focusing on the Weakly Interacting Massive Particles (WIMPs) scenario. The combined analysis allows us to maximize the sensitivity by combining individual data sets from all five experiments for which the energy ranges of the search overlap. New constraints, spanning a range of DM masses from 5 GeV to 100 TeV, on the velocity-weighted cross section for DM self annihilation will be presented.

Published
2021
Full Text
View/download PDF

4. Search for dark matter annihilation signals from UFOs with H.E.S.S

Author

Malyshev, D., Montanari, A., Moulin, E., Glawion, D., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and H.E.S.S.

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), model: annihilation, WIMP, Astrophysics::High Energy Astrophysical Phenomena, dark matter: mass, FOS: Physical sciences, dark matter: annihilation, Astrophysics::Cosmology and Extragalactic Astrophysics, GeV, GLAST, cross section: annihilation, thermal, gamma ray: emission, gamma ray: VHE, dark matter: halo, HESS, many-body problem, TeV, galaxy, distribution function, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics
Abstract

Cosmological N-body simulations show that Milky-Way-sized galaxies harbor a population of unmerged dark matter subhalos. These subhalos could shine in gamma rays and be eventually detected in gamma-ray surveys as unidentified sources. We search for very-high-energy (VHE, $E\geq 100$ GeV) gamma-ray emission using H.E.S.S. observations carried out from a thorough selection of unidentified Fermi-LAT Objects (UFOs) as dark matter subhalo candidates. Provided that the dark matter mass is higher than a few hundred GeV, the emission of the UFOs can be well described by dark matter annihilation models. No significant VHE gamma-ray emission is detected in any UFO dataset nor in their combination. We, therefore, derive constraints on the product of the velocity-weighted annihilation cross-section $\langle \sigma v\rangle$ by the $J$-factor on dark matter models describing the UFO emissions. Upper limits at 95% confidence level are derived on $\langle \sigma v\rangle J$ in $W^+W^-$ and $\tau^+\tau^-$ annihilation channels for the TeV dark matter particles. Focusing on thermal WIMPs, strong constraints on the $J$-factors are obtained from H.E.S.S. observations. Adopting model-dependent predictions from cosmological N-body simulations on the $J$-factor distribution function for Milky Way (MW)-sized galaxies, only $\lesssim 0.3$ TeV mass dark matter models marginally allow to explain observed UFO emission., Comment: 10 pages, 3 figures, Proceedings of the 37th International Cosmic Ray Conference (ICRC2021)

Published
2021

5. Multi-Messenger Cosmological Probes for New Physics in the Light of Ya.B. Zeldovich’s Legacy

Author

M. Yu. Khlopov, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Physics, 010308 nuclear & particles physics, WIMP, new physics, Physics beyond the Standard Model, Astronomy, Astronomy and Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, baryogenesis, 16. Peace & justice, 01 natural sciences, dark matter, General Relativity and Quantum Cosmology, Space and Planetary Science, 0103 physical sciences, baryon: asymmetry, neutrino: mass, inflation, dark energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], 010303 astronomy & astrophysics, black hole: primordial
Abstract

International audience; The modern Standard cosmological scenario, reflecting to large extent the development of Zeldovich’s legacy in cosmoparticle physics, involves inflation, baryosynthesis and dark matter/energy. Physics of all these elements of the cosmological paradigm lays Beyond the Standard model (BSM) of elementary particles and involves in its turn cosmological probes for its study. To specify this physics the idea of multi-messenger probes of new physics is proposed, involving the set of additional model dependent consequences of physical models for inflation, baryosynthesis and dark matter. We give a brief review of Cosmophenomenology of new physics, involving multi-component dark matter, metastable particles, Primordial black holes (PBHs) and antimatter domains in baryon asymmetrical Universe.

Published
2021
Full Text
View/download PDF

6. Search for dark matter annihilation signals from unidentified Fermi-LAT objects with H.E.S.S

Author

Abdalla, H., Aharonian, F., Benkhali, F. Ait, Angüner, E.O., Arcaro, C., Armand, C., Armstrong, T., Ashkar, H., Backes, M., Baghmanyan, V., Barbosa Martins, V., Barnacka, A., Barnard, M., Becherini, Y., Berge, D., Bernlöhr, K., Bi, B., Böttcher, M., Boisson, C., Bolmont, J., de Bony de Lavergne, M., Breuhaus, M., Brose, R., Brun, F., Brun, P., Bryan, M., Büchele, M., Bulik, T., Bylund, T., Cangemi, F., Caroff, S., Carosi, A., Casanova, S., Chambery, P., Chand, J. Catalano T., Chandra, S., Chen, A., Cotter, G., Curyło, M., Dalgleish, H., Mbarubucyeye, J. Damascene, Davids, I.D., Davies, J., Deil, C., Devin, J., Dirson, L., Djannati-Ataï, A., Dmytriiev, A., Donath, A., Doroshenko, V., Dreyer, L., Plessis, L. Du, Duffy, C., Dyks, J., Egberts, K., Eichhorn, F., Einecke, S., Emery, G., Ernenwein, J.-P., Feijen, K., Fegan, S., Fiasson, A., de Clairfontaine, G. Fichet, Fontaine, G., Funk, S., Füßling, M., Gabici, S., Gallant, Y.A., Giavitto, G., Giunti, L., Glawion, D., Glicenstein, J.F., Gottschall, D., Grondin, M.-H., Hattingh, S., Hahn, J., Haupt, M., Hermann, G., Hinton, J.A., Hofmann, W., Hoischen, C., Holch, T.L., Holler, M., Hörbe, M., Horns, D., Huang, Z., Huber, D., Jamrozy, M., Jankowsky, D., Jankowsky, F., Jardin-Blicq, A., Joshi, V., Jung-Richardt, I., Kasai, E., Katarzyński, K., Katz, U., Khangulyan, D., Khélifi, B., Klepser, S., Kluźniak, W., Komin, Nu., Konno, R., Kosack, K., Kostunin, D., Kreter, M., Mezek, G. Kukec, Kundu, A., Lamanna, G., Lemière, A., Lemoine-Goumard, M., Lenain, J.-P., Leuschner, F., Levy, C., Lohse, T., Luashvili, A., Lypova, I., Mackey, J., Majumdar, J., Malyshev, D., Marandon, V., Marchegiani, P., Marcowith, A., Mares, A., Martí-Devesa, G., Marx, R., Maurin, G., Meintjes, P.J., Meyer, M., Mitchell, A., Moderski, R., Mohrmann, L., Montanari, A., Moore, C., Morris, P., Moulin, E., Muller, J., Murach, T., Nakashima, K., Nayerhoda, A., de Naurois, M., Ndiyavala, H., Niemiec, J., Oakes, L., Odaka, H., Peyaud, B., Piel, Q., Noel, A., Oberholzer, L., O'Brien, P., Ohm, S., Olivera-Nieto, L., de Ona Wilhelmi, E., Ostrowski, M., Panter, M., Panny, S., Parsons, R.D., Peron, G., Pita, S., Poireau, V., Prokhorov, D.A., Prokoph, H., Pühlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Rauth, R., Reichherzer, P., Reimer, A., Reimer, O., Remy, Q., Renaud, M., Rieger, F., Rinchiuso, L., Romoli, C., Rowell, G., Rudak, B., Ricarte, H. Rueda, Ruiz-Velasco, E., Sahakian, V., Sailer, S., Salzmann, H., Sanchez, D.A., Santangelo, A., Sasaki, M., Scalici, M., Schäfer, J., Schüssler, F., Schutte, H.M., Schwanke, U., Seglar-Arroyo, M., Senniappan, M., Seyffert, A.S., Shafi, N., Shapopi, J.N.S., Shiningayamwe, K., Simoni, R., Sinha, A., Sol, H., Spackman, H., Specovius, A., Spencer, S., Spir-Jacob, M., Stawarz, Ł., Sun, L., Steenkamp, R., Stegmann, C., Steinmassl, S., Steppa, C., Takahashi, T., Tanaka, T., Tavernier, T., Taylor, A.M., Terrier, R., Morgan, C. Thorpe, Thiersen, J.H.E., Tiziani, D., Tluczykont, M., Tomankova, L., Trichard, C., Tsirou, M., Tsuji, M., Tuffs, R., Uchiyama, Y., van der Walt, D.J., van Eldik, C., van Rensburg, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Viana, A., Vincent, P., Vink, J., Völk, H.J., Wadiasingh, Z., Wagner, S.J., Watson, J., Werner, F., White, R., Wierzcholska, A., Wong, Yu Wun, Yassin, H., Yusafzai, A., Zacharias, M., Zanin, R., Zargaryan, D., Zdziarski, A.A., Zech, A., Zhu, S.J., Zmija, A., Zorn, J., Zouari, S., Żywucka, N., Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), H.E.S.S., H.E.S.S. Collaboration, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), High Energy Astrophys. & Astropart. Phys (API, FNWI), and Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
MATÉRIA ESCURA, scale: TeV, High-energy astronomy, WIMP, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Population, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, GeV, 01 natural sciences, GLAST, cross section: annihilation, thermal, HESS, 0103 physical sciences, education, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, [PHYS]Physics [physics], education.field_of_study, Annihilation, 010308 nuclear & particles physics, dark matter: mass, Gamma ray, Astronomy and Astrophysics, dark matter: annihilation, Galaxy, Distribution function, gamma ray: emission, gamma ray: VHE, Space and Planetary Science, Product (mathematics), many-body problem, HESS - Abteilung Hinton, High Energy Physics::Experiment, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract

Cosmological $N$-body simulations show that Milky Way-sized galaxies harbor a population of unmerged dark matter subhalos. These subhalos could shine in gamma-rays and be eventually detected in gamma-ray surveys as unidentified sources. We performed a thorough selection among unidentified Fermi-LAT Objects (UFOs) to identify them as possible TeV-scale dark matter subhalo candidates. We search for very-high-energy (E $\gtrsim$ 100 GeV) gamma-ray emissions using H.E.S.S. observations towards four selected UFOs. Since no significant very-high-energy gamma-ray emission is detected in any dataset of the four observed UFOs nor in the combined UFO dataset, strong constraints are derived on the product of the velocity-weighted annihilation cross section $\langle \sigma v \rangle$ by the $J$-factor for the dark matter models. The 95% C.L. observed upper limits derived from combined H.E.S.S. observations reach $\langle \sigma v \rangle J$ values of 3.7$\times$10$^{-5}$ and 8.1$\times$10$^{-6}$ GeV$^2$cm$^{-2}$s$^{-1}$ in the $W^+W^-$ and $\tau^+\tau^-$ channels, respectively, for a 1 TeV dark matter mass. Focusing on thermal WIMPs, the H.E.S.S. constraints restrict the $J$-factors to lie in the range 6.1$\times$10$^{19}$ - 2.0$\times$10$^{21}$ GeV$^2$cm$^{-5}$, and the masses to lie between 0.2 and 6 TeV in the $W^+W^-$ channel. For the $\tau^+\tau^-$ channel, the $J$-factors lie in the range 7.0$\times$10$^{19}$ - 7.1$\times$10$^{20}$ GeV$^2$cm$^{-5}$ and the masses lie between 0.2 and 0.5 TeV. Assuming model-dependent predictions from cosmological N-body simulations on the $J$-factor distribution for Milky Way-sized galaxies, the dark matter models with masses greater than 0.3 TeV for the UFO emissions can be ruled out at high confidence level., Comment: 11 pages, 7 figures, matches accepted version in The Astrophysical Journal

Published
2021
Full Text
View/download PDF

7. Bound states of WIMP dark matter in Higgs-portal models. Part I. Cross-sections and transition rates

Author

Kalliopi Petraki, Ruben Oncala, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), and Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Nuclear and High Energy Physics, Particle physics, High Energy Physics::Lattice, Dark matter, FOS: Physical sciences, QC770-798, Weak interaction, 01 natural sciences, WIMP: dark matter, Standard Model, thermal, Higgs particle: doublet, decoupling, dark matter: coupling, High Energy Physics - Phenomenology (hep-ph), weak interaction, WIMP, Nuclear and particle physics. Atomic energy. Radioactivity, monopole: bound state, 0103 physical sciences, Bound state, mediation, 010306 general physics, Physics, electroweak interaction, 010308 nuclear & particles physics, dark matter: relic density, Electroweak interaction, High Energy Physics::Phenomenology, singlet, dark matter: annihilation, Decoupling (cosmology), stability, Cosmology of Theories beyond the SM, bound state: formation, multiplet: 2, High Energy Physics - Phenomenology, force: long-range, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Beyond Standard Model, Higgs boson, High Energy Physics::Experiment, WIMP: bound state
Abstract

We investigate the role of the Higgs \emph{doublet} in the thermal decoupling of multi-TeV dark matter coupled to the Weak interactions of the Standard Model and the Higgs. The Higgs doublet can mediate a long-range force that affects the annihilation processes and binds dark matter into bound states. More importantly, the emission of a Higgs doublet by a pair of dark matter particles can give rise to extremely rapid monopole bound-state formation processes and bound-to-bound transitions. We compute these effects in the unbroken electroweak phase. To this end, we consider the simplest renormalisable fermionic model, consisting of a singlet and a doublet under $SU_{L}(2)$ that are stabilised by a $\mathbb{Z}_2$ symmetry, in the regime where the two multiplets coannihilate. In a companion paper, we use the results to show that the formation of metastable bound states via Higgs-doublet emission and their decay decrease the relic density very significantly., v1: 65 pages, 16 figures, 10 tables; v2: minor changes, published version

Published
2021
Full Text
View/download PDF

8. Results on Low-Mass Weakly Interacting Massive Particles from an 11 kg d Target Exposure of DAMIC at SNOLAB

Author

Letessier Selvon, A., Aguilar-Arevalo, A., Amidei, D., Baxter, D., Cancelo, G., Vergara, B. A. Cervantes, Chavarria, A. E., D’Olivo, J. C., Estrada, J., Favela-Perez, F., Gaïor, R., Guardincerri, Y., Hoppe, E. W., Hossbach, T. W., Kilminster, B., Lawson, I., Lee, S. J., Letessier-Selvon, A., Matalon, A., Mitra, P., Overman, C. T., Piers, A., Privitera, P., Ramanathan, K., Da Rocha, J., Sarkis, Y., Settimo, M., Smida, R., Thomas, R., Tiffenberg, J., Traina, M., Vilar, R., Virto, A. L., Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), DAMIC, Agence Nationale de la Recherche (France), University of Chicago, National Science Foundation (US), Universidad Nacional Autónoma de México, and Gordon and Betty Moore Foundation

Subjects
WIMP nucleon: scattering, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Silicon, WIMP, Dark matter, energy spectrum, FOS: Physical sciences, General Physics and Astronomy, chemistry.chemical_element, silicon: target, dark matter: direct detection, 01 natural sciences, 7. Clean energy, High Energy Physics - Experiment, Nuclear physics, High Energy Physics - Experiment (hep-ex), Ionization, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010306 general physics, ComputingMilieux_MISCELLANEOUS, CCD, Physics, CDMS, background, 010308 nuclear & particles physics, Scattering, dark matter: mass, Sigma, dark matter: scattering, chemistry, ionization: spatial distribution, radioactivity, Weakly interacting massive particles, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

DAMIC Collaboration: et al., We present constraints on the existence of weakly interacting massive particles (WIMPs) from an 11 kg d target exposure of the DAMIC experiment at the SNOLAB underground laboratory. The observed energy spectrum and spatial distribution of ionization events with electron-equivalent energies >200eVee in the DAMIC CCDs are consistent with backgrounds from natural radioactivity. An excess of ionization events is observed above the analysis threshold of 50eVee. While the origin of this low-energy excess requires further investigation, our data exclude spin-independent WIMP-nucleon scattering cross sections σχ−n as low as 3×10−41cm2 for WIMPs with masses mχ from 7 to 10GeVc−2. These results are the strongest constraints from a silicon target on the existence of WIMPs with mχ, We acknowledge financial support from the following agencies and organizations: National Science Foundation through Grant No. NSF PHY-1806974 and Kavli Institute for Cosmological Physics at The University of Chicago through an endowment from the Kavli Foundation; Gordon and Betty Moore Foundation through Grant No. GBMF6210 to the University of Washington; Fermi National Accelerator Laboratory (Contract No. DE-AC02-07CH11359); Institut Lagrange de Paris Laboratoire d’Excellence (under Reference No. ANR-10-LABX-63) supported by French state funds managed by the Agence Nationale de la Recherche within the Investissements d’Avenir program under Reference No. ANR-11-IDEX0004-02; Swiss National Science Foundation through Grant No. 200021_153654 and via the Swiss Canton of Zurich; Mexico’s Consejo Nacional de Ciencia y Tecnología (Grant No. 240666) and Dirección General de Asuntos del Personal Academico–Universidad Nacional Autónoma de Mexico (Programa de Apoyo a Proyectos de Investigación e Innovación Tecnológica Grants No. IB100413 and No. IN112213); STFC Global Challenges Research Fund (Foundation Awards Grant No. ST/R002908/1).

Published
2020
Full Text
View/download PDF

9. Consequences of DM/antiDM Oscillations for Asymmetric WIMP Dark Matter

Author

Gabrijela Zaharijas, Marco Cirelli, Geraldine Servant, Paolo Panci, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Service de Physique Théorique (SPhT), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Abdus Salam International Centre for Theoretical Physics [Trieste] (ICTP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and CIRELLI, Marco

Subjects
Particle physics, Antiparticle, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, Cosmic microwave background, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Parameter space, 01 natural sciences, Asymmetry, [PHYS] Physics [physics], Baryon asymmetry, High Energy Physics - Phenomenology (hep-ph), WIMP, 0103 physical sciences, physics of the early universe, 010306 general physics, cosmology of theories beyond the SM, media_common, Particle Physics - Phenomenology, Physics, [PHYS]Physics [physics], dark matter theory, 010308 nuclear & particles physics, Astronomy and Astrophysics, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Assuming the existence of a primordial asymmetry in the dark sector, a scenario usually dubbed Asymmetric Dark Matter (aDM), we study the effect of oscillations between dark matter and its antiparticle on the re-equilibration of the initial asymmetry before freeze-out, which enable efficient annihilations to recouple. We calculate the evolution of the DM relic abundance and show how oscillations re-open the parameter space of aDM models, in particular in the direction of allowing large (WIMP-scale) DM masses. A typical wimp with a mass at the EW scale (\sim 100 GeV - 1 TeV) presenting a primordial asymmetry of the same order as the baryon asymmetry naturally gets the correct relic abundance if the DM-number-violating Delta(DM) = 2 mass term is in the \sim meV range. The re-establishment of annihilations implies that constraints from the accumulation of aDM in astrophysical bodies are evaded. On the other hand, the ordinary bounds from BBN, CMB and indirect detection signals on annihilating DM have to be considered., Comment: 27 pages, 6+1 figures; v2: version submitted to JCAP for publication, one new figure and one new table added, summary plots slightly revised, a few clarifications added, main point emphasized, results unchanged

Published
2020
Full Text
View/download PDF

10. Energy resolution and linearity in the keV to MeV range measured in XENON1T

Author

Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Althueser, L., Amaro, F.D., Antochi, V.C., Angelino, E., Angevaare, J., Arneodo, F., Barge, D., Baudis, L., Bauermeister, B., Bellagamba, L., Benabderrahmane, M.L., Berger, T., Breur, P.A., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Capelli, C., Cardoso, J.M.R., Cichon, D., Cimmino, B., Clark, M., Coderre, D., Colijn, A.P., Conrad, J., Cussonneau, J.P., Decowski, M.P., Depoian, A., Di Gangi, P., Di Giovanni, A., Di Stefano, R., Diglio, S., Elykov, A., Eurin, G., Ferella, A.D., Fulgione, W., Gaemers, P., Gaior, R., Gallo Rosso, A., Galloway, M., Gao, F., Garbini, M., Grandi, L., Hasterok, C., Hils, C., Hiraide, K., Hoetzsch, L., Hogenbirk, E., Howlett, J., Iacovacci, M., Itow, Y., Joerg, F., Kato, N., Kazama, S., Kobayashi, M., Koltman, G., Kopec, A., Landsman, H., Lang, R.F., Levinson, L., Lin, Q., Lindemann, S., Lindner, M., Lombardi, F., Lopes, J.A.M., López Fune, E., Macolino, C., Mahlstedt, J., Manenti, L., Manfredini, A., Marignetti, F., Marrodán Undagoitia, T., Martens, K., Masbou, J., Masson, D., Mastroianni, S., Messina, M., Miuchi, K., Molinario, A., Morå, K., Moriyama, S., Mosbacher, Y., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Odgers, K., Palacio, J., Pelssers, B., Peres, R., Pienaar, J., Pizzella, V., Plante, G., Qin, J., Qiu, H., Ramírez García, D., Reichard, S., Rocchetti, A., Rupp, N., Dos Santos, J.M.F., Sartorelli, G., Šarčević, N., Scheibelhut, M., Schindler, S., Schreiner, J., Schulte, D., Schumann, M., Scotto Lavina, L., Selvi, M., Semeria, F., Shagin, P., Shockley, E., Silva, M., Simgen, H., Takeda, A., Therreau, C., Thers, D., Toschi, F., Trinchero, G., Tunnell, C., Vargas, M., Volta, G., Wack, O., Wang, H., Wei, Y., Weinheimer, C., Weiss Xu, M., Wenz, D., Wittweg, C., Wulf, J., Xu, Z., Yamashita, M., Ye, J., Zavattini, G., Zhang, Y., Zhu, T., Zopounidis, J.P., Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), and XENON

Subjects
double-beta decay: neutrinoless, Physics::Instrumentation and Detectors, WIMP, saturation, energy resolution, dark matter: detector, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], sensitivity, time projection chamber, xenon, Automatic Keywords, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], readout, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det]
Abstract

Xenon dual-phase time projection chambers designed to search for Weakly Interacting Massive Particles have so far shown a relative energy resolution which degrades with energy above $\sim$200 keV. This has limited their sensitivity in the search for rare events like the neutrinoless double-beta decay of $^{136}$Xe at its $Q$-value, $Q_{\beta\beta}\simeq$ 2.46 MeV. For the XENON1T dual-phase time projection chamber, we demonstrate that the relative energy resolution at 1 $\sigma/\mu$ is as low as (0.79$\pm$0.02) % in its one-ton fiducial mass, and for single-site interactions at $Q_{\beta\beta}$. We achieve this by using a signal correction method to rectify the saturation effects of the signal readout system. The very good energy resolution from keV to MeV energies demonstrated in XENON1T opens up new windows for the xenon dual-phase dark matter detectors to simultaneously search for other rare events.

Published
2020

11. The Dark Side of 4321

Author

Diego Guadagnoli, Peter Stangl, Meril Reboud, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), and Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)

Subjects
Nuclear and High Energy Physics, Particle physics, leptoquark: vector particle, Physics beyond the Standard Model, Dark matter, FOS: Physical sciences, Parameter space, dark matter: direct detection, 01 natural sciences, WIMP: dark matter, fermion: multiplet, XENON, High Energy Physics - Phenomenology (hep-ph), WIMP, Z', 0103 physical sciences, Heavy Quark Physics, fermion: dark matter, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Leptoquark, freeze-out, mediation: gauge, 010306 general physics, numerical calculations, Multiplet, Physics, Gauge boson, 010308 nuclear & particles physics, new physics, dark matter: relic density, Cosmology of Theories beyond the SM, High Energy Physics - Phenomenology, SU(4), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Beyond Standard Model, lcsh:QC770-798, Phenomenology (particle physics)
Abstract

The evidence of Dark Matter (DM) is one of the strongest observational arguments in favour of physics beyond the Standard Model. Despite expectations, a similar evidence has been lacking so far in collider searches, with the possible exception of $B$-physics discrepancies, a coherent set of persistent deviations in a homogeneous dataset consisting of $b \to c$ and $b \to s$ semi-leptonic transitions. We explore the question whether DM and the $B$ discrepancies may have a common origin. We do so in the context of the so-called 4321 gauge model, a UV-complete and calculable setup that yields a $U_1$ leptoquark, the by far most successful single mediator able to explain the $B$ anomalies, along with other new gauge bosons, including a $Z^\prime$. Adding to this setup a 'minimal' DM fermionic multiplet, consisting of a ${\bf 4}$ under the 4321's $SU(4)$, we find the resulting model in natural agreement with the relic-density observation and with the most severe direct-detection bounds, in the sense that the parameter space selected by $B$ physics is also the one favoured by DM phenomenology. The DM candidate is a particle with a mass in the WIMP range, freeze-out dynamics includes a co-annihilator (the 'rest' of the ${\bf 4}$ multiplet), and the most important gauge mediator in the DM sector is the $Z^\prime$., Comment: 33 pages, 7 figures

Published
2020
Full Text
View/download PDF

12. Search for dark matter towards the Galactic Centre with 11 years of ANTARES data

Author

Albert, A., André, M., Anghinolfi, M., Ardid, M., Aubert, J. -J., Aublin, J., Baret, B., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bissinger, M., Boumaaza, J., Bouta, M., Bouwhuis, M. C., Brânzaş, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chabab, M., Chau, T. N., Cherkaoui El Moursli, R., Chiarusi, T., Circella, M., Coleiro, A., Colomer, M., Coniglione, R., Coyle, P., Creusot, A., Díaz, A. F., Deschamps, A., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., El Khayati, N., Enzenhöfer, A., Ettahiri, A., Fermani, P., Ferrara, G., Filippini, F., Fusco, L., Gay, P., Glotin, H., Gozzini, R., Gracia Ruiz, R., Graf, K., Guidi, C., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernández-Rey, J. J., Hößl, J., Hofestädt, J., Huang, F., Illuminati, G., James, C. W., de Jong, M., de Jong, P., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Khan-Chowdhury, N. R., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Le Breton, R., Lefèvre, D., Leonora, E., Levi, G., Lincetto, M., Lopez-Coto, D., Loucatos, S., Maggi, G., Manczak, J., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J. A., Mele, R., Melis, K., Migliozzi, P., Moser, M., Moussa, A., Muller, R., Nauta, L., Navas, S., Nezri, E., Nielsen, C., Nuñez-Castiñeyra, A., O'Fearraigh, B., Organokov, M., Păvălaş, G. E., Pellegrino, C., Perrin-Terrin, M., Piattelli, P., Poirè, C., Popa, V., Pradier, T., Randazzo, N., Reck, S., Riccobene, G., Sánchez-Losa, A., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schüssler, F., Spurio, M., Stolarczyk, Th., Strandberg, B., Taiuti, M., Tayalati, Y., Thakore, T., Tingay, S. J., Trovato, A., Vallage, B., Van Elewyck, V., Versari, F., Viola, S., Vivolo, D., Wilms, J., Zaborov, D., Zegarelli, A., Zornoza, J. D., Zúñiga, J., Aartsen, IceCube Collaboration: M. G., Ackermann, M., Adams, J., Aguilar, J. A., Ahlers, M., Ahrens, M., Alispach, C., Andeen, K., Anderson, T., Ansseau, I., Anton, G., Argüelles, C., Auffenberg, J., Axani, S., Bagherpour, H., Bai, X., A. Balagopal V., Barbano, A., Barwick, S. W., Bastian, B., Baum, V., Baur, S., Bay, R., Beatty, J. J., Becker, K. -H., Becker Tjus, J., Benzvi, S., Berley, D., Bernardini, E., Besson, D. Z., Binder, G., Bindig, D., Blaufuss, E., Blot, S., Bohm, C., Böser, S., Botner, O., Böttcher, J., Bourbeau, E., Bourbeau, J., Bradascio, F., Braun, J., Bron, S., Brostean-Kaiser, J., Burgman, A., Buscher, J., Busse, R. S., Carver, T., Chen, C., Cheung, E., Chirkin, D., Choi, S., Clark, B. A., Clark, K., Classen, L., Coleman, A., Collin, G. H., Conrad, J. M., Coppin, P., Correa, P., Cowen, D. F., Cross, R., Dave, P., De Clercq, C., Delaunay, J. J., Dembinski, H., Deoskar, K., De Ridder, S., Desiati, P., de Vries, K. D., de Wasseige, G., de With, M., Deyoung, T., Diaz, A., Díaz-Vélez, J. C., Dujmovic, H., Dunkman, M., Dvorak, E., Eberhardt, B., Ehrhardt, T., Eller, P., Engel, R., Evenson, P. A., Fahey, S., Fazely, A. R., Felde, J., Filimonov, K., Finley, C., Fox, D., Franckowiak, A., Friedman, E., Fritz, A., Gaisser, T. K., Gallagher, J., Ganster, E., Garrappa, S., Gerhardt, L., Ghorbani, K., Glauch, T., Glüsenkamp, T., Goldschmidt, A., Gonzalez, J. G., Grant, D., Grégoire, T., Griffith, Z., Griswold, S., Günder, M., Gündüz, M., Haack, C., Hallgren, A., Halliday, R., Halve, L., Halzen, F., Hanson, K., Haungs, A., Hebecker, D., Heereman, D., Heix, P., Helbing, K., Hellauer, R., Henningsen, F., Hickford, S., Hignight, J., Hill, G. C., Hoffman, K. D., Hoffmann, R., Hoinka, T., Hokanson-Fasig, B., Hoshina, K., Huber, M., Huber, T., Hultqvist, K., Hünnefeld, M., Hussain, R., In, S., Iovine, N., Ishihara, A., Jansson, M., Japaridze, G. S., Jeong, M., Jero, K., Jones, B. J. P., Jonske, F., Joppe, R., Kang, D., Kang, W., Kappes, A., Kappesser, D., Karg, T., Karl, M., Karle, A., Kauer, M., Kellermann, M., Kelley, J. L., Kheirandish, A., Kim, J., Kintscher, T., Kiryluk, J., Kittler, T., Klein, S. R., Koirala, R., Kolanoski, H., Köpke, L., Kopper, C., Kopper, S., Koskinen, D. J., Kowalski, M., Krings, K., Krückl, G., Kulacz, N., Kurahashi, N., Kyriacou, A., Lanfranchi, J. L., Larson, M. J., Lauber, F., Lazar, J. P., Leonard, K., Leszczyńska, A., Liu, Q. R., Lohfink, E., Lozano Mariscal, C. J., Lu, L., Lucarelli, F., Ludwig, A., Lünemann, J., Luszczak, W., Lyu, Y., W. Y., Ma, Madsen, J., Mahn, K. B. M., Makino, Y., Mallik, P., Mallot, K., Mancina, S., Mariş, I. C., Maruyama, R., Mase, K., Maunu, R., Mcnally, F., Meagher, K., Medici, M., Medina, A., Meier, M., Meighen-Berger, S., Merino, G., Meures, T., Micallef, J., Mockler, D., Momenté, G., Montaruli, T., Moore, R. W., Morse, R., Moulai, M., Muth, P., Nagai, R., Naumann, U., Neer, G., Nguyen, L. V., Niederhausen, H., Nisa, M. U., Nowicki, S. C., Nygren, D. R., Obertacke Pollmann, A., Oehler, M., Olivas, A., O'Murchadha, A., O'Sullivan, E., Palczewski, T., Pandya, H., Pankova, D. V., Park, N., Peiffer, P., Pérez de los Heros, C., Philippen, S., Pieloth, D., Pieper, S., Pinat, E., Pizzuto, A., Plum, M., Porcelli, A., Price, P. B., Przybylski, G. T., Raab, C., Raissi, A., Rameez, M., Rauch, L., Rawlins, K., Rea, I. C., Rehman, A., Reimann, R., Relethford, B., Renschler, M., Renzi, G., Resconi, E., Rhode, W., Richman, M., Robertson, S., Rongen, M., Rott, C., Ruhe, T., Ryckbosch, D., Rysewyk Cantu, D., Safa, I., Sanchez Herrera, S. E., Sandrock, A., Sandroos, J., Santander, M., Sarkar, S., Satalecka, K., Schaufel, M., Schieler, H., Schlunder, P., Schmidt, T., Schneider, A., Schneider, J., Schröder, F. G., Schumacher, L., Sclafani, S., Seckel, D., Seunarine, S., Shefali, S., Silva, M., Snihur, R., Soedingrekso, J., Soldin, D., Song, M., Spiczak, G. M., Spiering, C., Stachurska, J., Stamatikos, M., Stanev, T., Stein, R., Stettner, J., Steuer, A., Stezelberger, T., Stokstad, R. G., Stös(s)l, A., Strotjohann, N. L., Stürwald, T., Stuttard, T., Sullivan, G. W., Taboada, I., Tenholt, F., Ter-Antonyan, S., Terliuk, A., Tilav, S., Tollefson, K., Tomankova, L., Tönnis, C., Toscano, S., Tosi, D., Trettin, A., Tselengidou, M., Tung, C. F., Turcati, A., Turcotte, R., Turley, C. F., Ty, B., Unger, E., Unland Elorrieta, M. A., Usner, M., Vandenbroucke, J., Van Driessche, W., van Eijk, D., van Eijndhoven, N., van Santen, J., Verpoest, S., Vraeghe, M., Walck, C., Wallace, A., Wallraff, M., Wandkowsky, N., Watson, T. B., Weaver, C., Weindl, A., Weiss, M. J., Weldert, J., Wendt, C., Werthebach, J., Whelan, B. J., Whitehorn, N., Wiebe, K., Wiebusch, C. H., Wille, L., Williams, D. R., Wills, L., Wolf, M., Wood, J., Wood, T. R., Woschnagg, K., Wrede, G., Wulff, J., D. L., Xu, X. W., Xu, Xu, Y., Yanez, J. P., Yodh, G., Yoshida, S., Yuan, T., Zöcklein, M., Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de France (IUF), Ministère de l'Education nationale, de l’Enseignement supérieur et de la Recherche (M.E.N.E.S.R.), Institut méditerranéen d'océanologie (MIO), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Université de Toulon - UFR Sciences et Techniques (UTLN UFR ScT), Université de Toulon (UTLN), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, ANTARES, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Clermont Auvergne (UCA), Albert A., Andre M., Anghinolfi M., Anton G., Ardid M., Aubert J.-J., Aublin J., Baret B., Basa S., Belhorma B., Bertin V., Biagi S., Bissinger M., Boumaaza J., Bourret S., Bouta M., Bouwhuis M.C., Branzas H., Bruijn R., Brunner J., Busto J., Capone A., Caramete L., Carr J., Celli S., Chabab M., Chau T.N., Cherkaoui El Moursli R., Chiarusi T., Circella M., Coleiro A., Colomer M., Coniglione R., Costantini H., Coyle P., Creusot A., Diaz A.F., de Wasseige G., Deschamps A., Distefano C., Di Palma I., Domi A., Donzaud C., Dornic D., Drouhin D., Eberl T., El Bojaddaini I., El Khayati N., Elsasser D., Enzenhofer A., Ettahiri A., Fassi F., Fermani P., Ferrara G., Filippini F., Fusco L., Gay P., Glotin H., Gozzini R., Gracia Ruiz R., Graf K., Guidi C., Hallmann S., van Haren H., Heijboer A.J., Hello Y., Hernandez-Rey J.J., Hossl J., Hofestadt J., Illuminati G., James C.W., de Jong M., de Jong P., Jongen M., Kadler M., Kalekin O., Katz U., Khan-Chowdhury N.R., Kouchner A., Kreter M., Kreykenbohm I., Kulikovskiy V., Lahmann R., Le Breton R., Lefevre D., Leonora E., Levi G., Lincetto M., Lopez-Coto D., Loucatos S., Maggi G., Manczak J., Marcelin M., Margiotta A., Marinelli A., Martinez-Mora J.A., Mele R., Melis K., Migliozzi P., Moser M., Moussa A., Muller R., Nauta L., Navas S., Nezri E., Nielsen C., Nunez-Castineyra A., O'Fearraigh B., Organokov M., Pavalas G.E., Pellegrino C., Perrin-Terrin M., Piattelli P., Poire C., Popa V., Pradier T., Quinn L., Randazzo N., Riccobene G., Sanchez-Losa A., Salah-Eddine A., Samtleben D.F.E., Sanguineti M., Sapienza P., Schussler F., Spurio M., Stolarczyk T., Strandberg B., Taiuti M., Tayalati Y., Thakore T., Tingay S.J., Trovato A., Vallage B., Van Elewyck V., Versari F., Viola S., Vivolo D., Wilms J., Zaborov D., Zegarelli A., Zornoza J.D., Zuniga J., KM3NeT (IHEF, IoP, FNWI), ATLAS (IHEF, IoP, FNWI), Albert, A, Andre, M, Anghinolfi, M, Anton, G, Ardid, M, Aubert, Jj, Aublin, J, Baret, B, Basa, S, Belhorma, B, Bertin, V, Biagi, S, Bissinger, M, Boumaaza, J, Bourret, S, Bouta, M, Bouwhuis, Mc, Branzas, H, Bruijn, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Celli, S, Chabab, M, Chau, Tn, El Moursli, Rc, Chiarusi, T, Circella, M, Coleiro, A, Colomer, M, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Diaz, Af, de Wasseige, G, Deschamps, A, Distefano, C, Di Palma, I, Domi, A, Donzaud, C, Dornic, D, Drouhin, D, Eberl, T, El Bojaddaini, I, El Khayati, N, Elsasser, D, Enzenhofer, A, Ettahiri, A, Fassi, F, Fermani, P, Ferrara, G, Filippini, F, Fusco, L, Gay, P, Glotin, H, Gozzini, R, Ruiz, Rg, Graf, K, Guidi, C, Hallmann, S, van Haren, H, Heijboer, Aj, Hello, Y, Hernandez-Rey, Jj, Hossl, J, Hofestadt, J, Illuminati, G, Jamesa, Cw, de Jong, M, de Jong, P, Jongen, M, Kadler, M, Kalekin, O, Katz, U, Khan-Chowdhury, Nr, Kouchner, A, Kreter, M, Kreykenbohm, I, Kulikovskiy, V, Lahmann, R, Le Breton, R, Lefevre, D, Leonora, E, Levi, G, Lincetto, M, Lopez-Coto, D, Loucatos, S, Maggi, G, Manczak, J, Marcelin, M, Margiotta, A, Marinelli, A, Martinez-Mora, Ja, Mele, R, Melis, K, Migliozzi, P, Moser, M, Moussa, A, Muller, R, Nauta, L, Navas, S, Nezri, E, Nielsen, C, Nunez-Castineyra, A, O'Fearraigh, B, Organokov, M, Pavalas, Ge, Pellegrino, C, Perrin-Terrin, M, Piattelli, P, Poire, C, Popa, V, Pradier, T, Quinn, L, Randazzoa, N, Riccobene, G, Sanchez-Losa, A, Salah-Eddine, A, Samtleben, Dfe, Sanguineti, M, Sapienza, P, Schussler, F, Spurio, M, Stolarczyk, T, Strandberg, B, Taiuti, M, Tayalati, Y, Thakore, T, Tingay, Sj, Trovato, A, Vallage, B, Van Elewyck, V, Versari, F, Viola, S, Vivolo, D, Wilms, J, Zaborov, D, Zegarelli, A, Zornoza, Jd, Zuniga, J, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), Generalitat Valenciana, Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne (UCA)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherche pour le Développement (IRD)-Aix Marseille Université (AMU)-Université de Toulon (UTLN)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Toulon (UTLN)-Aix Marseille Université (AMU)-Institut de Recherche pour le Développement (IRD), Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Albert, A., Andre, M., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J. -J., Aublin, J., Baret, B., Basa, S., Belhorma, B., Bertin, V., Biagi, S., Bissinger, M., Boumaaza, J., Bourret, S., Bouta, M., Bouwhuis, M. C., Branzas, H., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chabab, M., Chau, T. N., Cherkaoui El Moursli, R., Chiarusi, T., Circella, M., Coleiro, A., Colomer, M., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Diaz, A. F., de Wasseige, G., Deschamps, A., Distefano, C., Di Palma, I., Domi, A., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., El Bojaddaini, I., El Khayati, N., Elsasser, D., Enzenhofer, A., Ettahiri, A., Fassi, F., Fermani, P., Ferrara, G., Filippini, F., Fusco, L., Gay, P., Glotin, H., Gozzini, R., Gracia Ruiz, R., Graf, K., Guidi, C., Hallmann, S., van Haren, H., Heijboer, A. J., Hello, Y., Hernandez-Rey, J. J., Hossl, J., Hofestadt, J., Illuminati, G., James, C. W., de Jong, M., de Jong, P., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Khan-Chowdhury, N. R., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Le Breton, R., Lefevre, D., Leonora, E., Levi, G., Lincetto, M., Lopez-Coto, D., Loucatos, S., Maggi, G., Manczak, J., Marcelin, M., Margiotta, A., Marinelli, A., Martinez-Mora, J. A., Mele, R., Melis, K., Migliozzi, P., Moser, M., Moussa, A., Muller, R., Nauta, L., Navas, S., Nezri, E., Nielsen, C., Nunez-Castineyra, A., O'Fearraigh, B., Organokov, M., Pavalas, G. E., Pellegrino, C., Perrin-Terrin, M., Piattelli, P., Poire, C., Popa, V., Pradier, T., Quinn, L., Randazzo, N., Riccobene, G., Sanchez-Losa, A., Salah-Eddine, A., Samtleben, D. F. E., Sanguineti, M., Sapienza, P., Schussler, F., Spurio, M., Stolarczyk, T., Strandberg, B., Taiuti, M., Tayalati, Y., Thakore, T., Tingay, S. J., Trovato, A., Vallage, B., Van Elewyck, V., Versari, F., Viola, S., Vivolo, D., Wilms, J., Zaborov, D., Zegarelli, A., Zornoza, J. D., and Zuniga, J.

Subjects
ANTARES, Dark matter indirect detection, Galactic Centre, Neutrino telescope, Astrofísica, Physics::Instrumentation and Detectors, neutrino: energy: high, astro-ph.HE, Astrophysics, 01 natural sciences, neutrino: flux, WIMP, S046PHB, hal-02431461, detector [neutrino], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Annihilation, 4. Education, Astrophysics::Instrumentation and Methods for Astrophysics, dark matter: density: high, lcsh:QC1-999, neutrino: detector, Neutrino detector, density: high [dark matter], annihilation, Dark matter, indirect detection, Weakly interacting massive particles, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Nuclear and High Energy Physics, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Partícules (Física nuclear), Standard Model, S030DMA, 0103 physical sciences, Neutrins, 010306 general physics, Particles (Nuclear physics), Telescopis, 010308 nuclear & particles physics, Galaxy, Automatic Keywords, FISICA APLICADA, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], spectral, High Energy Physics::Experiment, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], lcsh:Physics, Telescopes
Abstract

Neutrino detectors participate in the indirect search for the fundamental constituents of dark matter (DM) in form of weakly interacting massive particles (WIMPs). In WIMP scenarios, candidate DM particles can pair-annihilate into Standard Model products, yielding considerable fluxes of high-energy neutrinos. A detector like ANTARES, located in the Northern Hemisphere, is able to perform a complementary search looking towards the Galactic Centre, where a high density of dark matter is thought to accumulate. Both this directional information and the spectral features of annihilating DM pairs are entered into an unbinned likelihood method to scan the data set in search for DM-like signals in ANTARES data. Results obtained upon unblinding 3170 days of data reconstructed with updated methods are presented, which provides a larger, and more accurate, data set than a previously published result using 2101 days. A non-observation of dark matter is converted into limits on the velocity-averaged cross section for WIMP pair annihilation., Centre National de la Recherche Scientifique (CNRS), French Atomic Energy Commission, Commission Europeenne (FEDER fund), European Union (EU), Institut Universitaire de France (IUF), IdEx program at Sorbonne Paris Cite ANR-10-LABX-0023 ANR-11-IDEX-0005-02, UnivEarthS Labex program at Sorbonne Paris Cite ANR-10-LABX-0023 ANR-11-IDEX-0005-02, Labex OCEVU ANR-11-LABX-0060, French National Research Agency (ANR) ANR-11-IDEX-0001-02, Region Ile-de-France, Region Grand-Est, Region Provence-Alpes-Cote d'Azur, Federal Ministry of Education & Research (BMBF), Instituto Nazionale di Fisica Nucleare(INFN), Italy, Netherlands Organization for Scientific Research (NWO) Netherlands Government, Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia, Executive Unit for Financing Higher Education, Research, Development and Innovation (UEFISCDI), Romania, Ministerio de Ciencia, Innovacion y Universidades(MCIU): Programa Estatal de Generacion de Conocimiento PGC2018-096663-B-C41 PGC2018-096663-A-C42 PGC2018-096663-B-C43 PGC2018-096663-B-C44, Severo Ochoa Centre of Excellence and MultiDark Consolider (MCIU), Junta de Andalucia SOMM17/6104/UGR, Generalitat Valenciana: Grisolia, Spain GRISOLIA/2018/119, Ministry of Higher Education, Scientific Research and Training, Morocco

Published
2020
Full Text
View/download PDF

13. Hunt for dark subhalos in the galactic stellar field using computer vision

Author

Petac, Mihael, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), and Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
dark matter: interaction, matter: power spectrum, neural network, WIMP, satellite, FOS: Physical sciences, dark matter: signature, Astrophysics::Cosmology and Extragalactic Astrophysics, thermal, phase space, High Energy Physics - Phenomenology (hep-ph), dark matter: halo, star, gas, cloud, structure, distribution function, cluster, Astrophysics::Galaxy Astrophysics, computer, down: mass, neutrino: sterile, suppression, sensitivity, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology, gravitation, Astrophysics of Galaxies (astro-ph.GA), trajectory, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], network, galaxy, higher-dimensional, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

The lack of tangible evidence for non-gravitational interactions between dark and visible sectors drives the need for exploring new avenues of inferring dark matter properties through purely gravitational probes. In particular, addressing small-scale distribution of dark matter could lead to valuable new insights into its particle nature, either confirming predictions of the collisionless cold dark matter hypothesis or favouring models with suppressed small-scale matter power spectrum. In this work we propose a novel machine learning approach for constraining the abundance of galactic dark matter subhaloes through the analysis of Milky Way's stellar field that has been only recently mapped with sufficient coverage thanks to the Gaia mission. Our method is based on convolutional neural networks which represent a powerful tool for identifying characteristic perturbations in spatial maps of stellar number density and velocity distribution moments. For generating the training data we develop a robust and computationally efficient algorithm, capable of generating mock stellar fields from an arbitrary underlying phase-space distribution of stars. By preforming a preliminary study of the outlined approach on synthetic datasets we demonstrate that sensitivities down to (or even below) $10^8 M_\odot$ could be reached. Furthermore, our results show that the accuracy of the advocated technique crucially depends on the kinematic properties of mapped stars and could be further improved by applying it to abundant stellar populations with particularly low velocity dispersion, such as the galactic thin disc stars., 10 pages, 5 figures, 2 tables

Published
2019

14. Hunting for heavy Dark Matter in the Galactic Center with ground-based Cherenkov telescopes

Author

Nicholas L. Rodd, Lucia Rinchiuso, Tracy R. Slatyer, Emmanuel Moulin, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), scale: TeV, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Wino, FOS: Physical sciences, photon: spectrum, Astrophysics, dark matter: density, 7. Clean energy, WIMP: dark matter, thermal, High Energy Physics - Phenomenology (hep-ph), WIMP, HESS, Cherenkov radiation, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), energy: high, Annihilation, background, photon: annihilation, Galactic Center, Electroweak interaction, scale: electroweak interaction, dark matter: annihilation, Cherenkov Telescope Array, sensitivity, Universe, High Energy Physics - Phenomenology, Cherenkov counter, dark matter: heavy, gamma ray, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

A TeV scale electroweak particle is a well motivated candidate for the dark matter (DM) of our Universe. Yet such a particle may only be detectable using indirect detection instruments sensitive to TeV-scale gamma rays that can result from dark matter annihilations. We present a mock analysis of the sensitivity for the present ground-based Cherenkov telescope array H.E.S.S. (High Energy Spectroscopic System) to detect TeV scale DM in the Galactic Center region. The work combines next-to-leading-logarithmic order calculations for the annihilation photon spectrum, as well as a comprehensive treatment of detector effects and expected backgrounds. Forecast limits on the sensitivity of H.E.S.S. have been derived across the important TeV mass range, assuming different DM density profiles and focusing on the canonical WIMP dark matter candidate Wino.These limits test our present and future ability to probe the predicted thermal cross section for some of the most promising DM candidates that could be discovered in the coming decade., Comment: 7 pages, 4 figures, 36th International Cosmic Ray Conference

Published
2019
Full Text
View/download PDF

15. Unidentified Fermi Objects in the view of H.E.S.S. -- Possible Dark Matter Clumps

Author

Emmanuel Moulin, Louise Oakes, Dorit Glawion, Denys Malyshev, Lucia Rinchiuso, Aion Viana, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and H.E.S.S.

Subjects
WIMP, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Elementary particle, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Weak interaction, 0603 philosophy, ethics and religion, 7. Clean energy, 01 natural sciences, GLAST, weak interaction, dark matter: halo, 0103 physical sciences, 010303 astronomy & astrophysics, HESS: performance, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Annihilation, resolution, dark matter: annihilation, 06 humanities and the arts, stability, gamma ray: emission, Weakly interacting massive particles, 060302 philosophy, many-body problem, Halo, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract

There is strong evidence about the existence of unknown dark matter in the Universe. Many different theories about this dark matter exist, but most probably it is made of a new kind of fundamental particle that has to be massive, stable, electrically neutral, and having only weak interaction with standard matter (weakly interacting massive particles). In principle, those particles could produce gamma rays by their annihilation or decay. Therefore, a Gamma-ray signal from a dark matter origin would provide one of the clearest and most concluding evidences for dark matter. High resolution cosmological N-body simulations have shown that dark matter subhalos in the Milky Way halo may developed in the Universe. Those subhalos could pop-up in gamma-ray surveys as unidentified sources. In this paper we present H.E.S.S. observations of unidentified sources selected from Fermi-LAT catalogs. These sources fulfill main features which would characterize a dark matter subhalo, namely, having no obvious counterpart at other wavelengths and being steady hard sources., Proceedings of the 36th International Cosmic Ray Conference, 2019, Madison, WI, USA

Published
2019
Full Text
View/download PDF

16. Development of Spherical Proportional Counter for light WIMP search within NEWS-G collaboration

Author

Gilles Geribier, Ali Dastgheibi-Fard, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), NEWS-G, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), and Université Grenoble Alpes (UGA)

Subjects
Nuclear and High Energy Physics, Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Spherical Proportional Counter, Dark matter, FOS: Physical sciences, Proportional counter, chemistry.chemical_element, fabrication, 01 natural sciences, 7. Clean energy, WIMP: dark matter, 99-00, Nuclear physics, Neon, WIMP, 0103 physical sciences, Calibration, Neutron, neon, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], lead: nuclide, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Instrumentation, background: radioactivity, Spherical detector, Physics, Range (particle radiation), Dark matter search, 010308 nuclear & particles physics, detector: surface, Light WIMP search, Detector, Instrumentation and Detectors (physics.ins-det), dark matter: detector, energy: calibration, 00-01, chemistry, proportional chamber, High Energy Physics::Experiment, Astrophysics - Instrumentation and Methods for Astrophysics, performance
Abstract

International audience; The Spherical gaseous detector (or Spherical Proportional Counter, SPC) has a broad range of applications. In this work, we will focus on the light WIMP Dark Matter particle search, that is, below a few GeV. The NEWS-G collaboration operates a 60 cm diameter detector at Modane underground laboratory (LSM). Running the detector at 3 bars of Neon gas, some competitive limits have been set down to 0.5 GeV WIMP mass thanks to an energy threshold of around 100 eV. To reach better performances, the next generation of SPC (140 cm), NEWS-G_SNO, is under construction. We will focus here on the fabrication method, the different low energy calibration methods using 37 Ar, neutron and UV laser, on the cleaning methods to remove the surface contamination and mitigation of 210 Pb bulk contamination.

Published
2019
Full Text
View/download PDF

17. Dark matter capture by the Sun: revisiting velocity distribution uncertainties

Author

Emmanuel Nezri, V. Bertin, A. Nuñez-Castiñeyra, Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), and Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, Inverse transform sampling, FOS: Physical sciences, WIMP: mass, Context (language use), Astrophysics, 01 natural sciences, WIMP: dark matter, High Energy Physics - Phenomenology (hep-ph), benchmark, WIMP, 0103 physical sciences, distribution function, Physics, mass: density, 010308 nuclear & particles physics, Astronomy and Astrophysics, Escape velocity, Astrophysics - Astrophysics of Galaxies, Galaxy, solar, dark matter: capture, High Energy Physics - Phenomenology, Distribution function, Astrophysics of Galaxies (astro-ph.GA), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], direct detection, history, galaxy, dark matter: velocity, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Among the different strategies aiming to detect WIMP dark matter (DM), a neutrino signal coming from the Sun would be a smoking gun. This possibility relies on the DM capture by the Sun driven by the local DM distribution assumptions: the local mass density and the velocity distribution. In this context, we revisit those astrophysical hypotheses (also relevant for direct detection). We focus especially on the DM velocity distribution considering different possibilities beyond the popular Maxwellian distribution. Namely, some alternatives can be considered through analytical approaches and by looking into cosmological simulations of spiral galaxies. Most of the fitting formulas used to constrain the local velocity distribution function fail to describe the peak and the high velocity tail of the velocity distribution observed in simulations, the latter being improved when adding the local escape velocity of DM into the benchmark fitting models. In addition we test the predictions by the Eddington inversion method and also illustrate the importance of the galactic dynamical history. We estimate the resulting uncertainties on the DM capture rate by the Sun and conclude that different velocity distributions will affect the capture rate of DM by the Sun up to a $15-20\%$. On top of that, the calculation of the intrinsic variance of the capture rate leads to poorly controlled uncertainties especially for high WIMP masses ($>$30 GeV) raising concerns about the capture scenario., 20 pages, 7 figures, JCAP format

Published
2019
Full Text
View/download PDF

18. Ultracompact minihalos associated with stellar-mass primordial black holes

Author

Joseph Silk, Kazunori Kohri, Tomohiro Nakama, Institut d'Astrophysique de Paris (IAP), and Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Stellar mass, WIMP, media_common.quotation_subject, interferometer, Dark matter, FOS: Physical sciences, Primordial black hole, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, dark matter, black hole: formation, Pulsar, dark matter: halo, binary: coalescence, 0103 physical sciences, 010306 general physics, Astrophysics::Galaxy Astrophysics, media_common, pulsar, Physics, non-Gaussianity: primordial, 010308 nuclear & particles physics, gravitational radiation, Universe, Redshift, Cosmology, black hole: binary, Weakly interacting massive particles, gravitational radiation: emission, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The possibility that primordial black hole binary mergers of stellar mass can explain the signals detected by the gravitational-wave interferometers has attracted much attention. In this scenario, primordial black holes can comprise only part of the entire dark matter, say, of order 0.1 %. This implies that most of the dark matter is accounted for by a different component, such as Weakly Interacting Massive Particles. We point out that in this situation, very compact dark matter minihalos, composed of the dominant component of the dark matter, are likely to be formed abundantly in the early Universe, with their formation redshift and abundance depending on primordial non-Gaussianity. They may be detected in future experiments via pulsar observations., Comment: 10 pages, 2 figures

Published
2019
Full Text
View/download PDF

19. Next Generation Search for Axion and ALP Dark Matter with the International Axion Observatory

Author

S. Basso, I. Lomskaya, I. G. Irastorza, Javier Redondo, Olivier Limousin, A. Nunez, Ioannis Giomataris, Lluis Garrido, Jochen Kaminski, Milica Krčmar, Alessio Notari, Amanda Weltman, A. A. Nozik, A. Lindner, P. Vedrine, D. Costa, L. Gastaldo, David Gascon, I. Tkackev, J. F. Castel, Ricardo Graciani, V. S. Pantuev, Matthias Schott, Andreas Ringwald, Krešimir Jakovčić, J. M. Carmona, Pierre Brun, Cristiano Germani, Thierry Lasserre, E. Ferrer-Ribas, Jordi Salvado, M. J. Pivovaroff, S. Cebrián, K. Perez, U. Schneekloth, C. Nones, F. Mescia, G. Tagliaferri, E. V. Unzhakov, V. N. Muratova, E. Armengaud, T. Schiffer, Sergey Troitsky, F. Tavecchio, Biljana Lakić, G. Pareschi, N. Golubev, David Attié, Julia Vogel, J. Galan, N. Bykovskiy, X.F. Navick, C. Cogollos, G. Luzón, C. Krieger, H. Mirallas, J. Ruz, S. Schmidt, E. Ruiz-Choliz, H. Ten Kate, P. Laurent, G. Galanti, T. Dafni, Klaus Kurt Desch, Jordi Miralda-Escudé, H. Silva, A. V. Derbin, Marie-Anne Descalle, S. N. Gninenko, I. Dratchnev, A. Ortiz de Solórzano, B. Dobrich, T. Papaevangelou, G. Ghisellini, Maurizio Giannotti, E. Picatoste, M. M. Civitani, Alexey Dudarev, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay

Subjects
Particle physics, CERN Lab, Physics::Instrumentation and Detectors, Dark matter, Observatories, axion: detector, 7. Clean energy, 01 natural sciences, Cosmology, High Energy Physics::Theory, Primakoff effect, Sensitivity, WIMP, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Axion, activity report, Physics, Helioscope, Large Hadron Collider, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Toroidal magnetic fields, Detectors, observatory, 13. Climate action, Couplings, axion-like particles, proposed experiment, CERN Axion Solar Telescope, axion: solar, Telescopes
Abstract

International audience; More than 80 years after the postulation of dark matter, its nature remains one of the fundamental questions in cosmology. Axions are currently one of the leading candidates for the hypothetical, non-baryonic dark matter that is expected to account for about 25% of the energy density of the Universe. Especially in the light of the Large Hadron Collider at CERN slowly closing in on Weakly-Interacting Massive Particle (WIMP) searches, axions and axion-like particles (ALPs) provide a viable alternative approach to solving the dark matter problem. The fact that makes them particularly appealing is that they were initially introduced to solve a long-standing problem in quantum chromodynamics and the Standard Model of particle physics.Helioscopes are a type of axion experiment searching for axions produced in the core of the Sun via the Primakoff effect. The International Axion Observatory (IAXO) is a next generation axion helioscope aiming at a sensitivity to the axion-photon coupling of 1 − 1.5 orders of magnitude beyond the current most sensitive axion helioscope, which is the CERN Axion Solar Telescope (CAST). IAXO will be able to challenge the stringent bounds from supernova SN1987A and test the axion interpretation of anomalous white-dwarf cooling. Beyond standard axions, this new experiment will also be able to search for a large variety of axion-like particles and other novel excitations at the low-energy frontier of elementary particle physics. BabyIAXO is proposed as an intermediate-scale experiment increasing the sensitivity to axion-photon couplings down to a few 10$^{−11}$ GeV$^{−1}$ and thus delivering significant physics results while demonstrating the feasibility of the full-scale IAXO experiment. Here we introduce the IAXO and BabyIAXO experiments, report on the current status of both and outline the expected IAXO science reach.

Published
2018
Full Text
View/download PDF

20. Analyse des données de l'expérience EDELWEISS-LT pour la recherche de WIMP de basse masse

Author

Queguiner, Emeline, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Lyon, and Jules Gascon

Subjects
WIMP, EDELWEISSS, Analyse de données, Direct detection, Data analysis, Likelihood, Maximum de vraisemblance, Bruit de fond, Matière noire, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Background, EDELWEISS, Dark matter, Détection directe
Abstract

Many astrophysical and cosmological observations lead to postulate the existence of an unknown matter, called dark matter. Ordinary matter can explain only 5 % of the energy content of the Universe : the main components would be the dark energy (70 %) and dark matter (25 %). This latter is invisible and manifest itself only via its gravitational effects. Several particles, grouped under the generic term of WIMP (Weakly Interacting Massive Particles), could correspond to this theory and are actively searched. Many experiments have been developed for this purpose and are based on three strategies: the production of these particles with colliders, the observation of the particles produced by their annihilation in astrophysical objects or the direct detection of these particles via their interaction with the nucleus of the atoms constituent of a detector. It is on this last method that the EDELWEISS experiment is based. It is a dark matter direct detection experiment dedicated to the search for WIMP with masses between 1 GeV and 1 TeV. Its primary purpose is to detect nuclear recoils induced by elastic scattering of dark matter particles in detectors. Since the expected event rates < 10 /(kg.year) are several orders of magnitude lower than those induced by ambient radioactivity, a double measurement of ionization and heat is used to discriminate electron-induced recoils arising from β and γ interactions from WIMP-induced nuclear recoils. In addition, the experiment was placed underground to guard against cosmic radiation, inducing events in the detectors. These are germanium bolometers, called FID, cooled to cryogenic temperatures (18 mK) and operating at low field (1 V/cm). Since 2015, the new strategy of the experiment consists of focusing on WIMPs with mass below 10 GeV, an interessant research area where experiments using cryogenic detectors can exploit their ability to operate with experimental thresholds well below 1 keV. The operation of the experiment has been improved to achieve this goal. The aim of this thesis is to analyze the data set recorded by EDELWEISS in 2015 and 2016. These used the FID detectors subjected to a greater electric field than previously to improve their sensitivity. It is expected that the limit on the spin-independent WIMP-nucleon crosssection extracted from these data will be greatly impacted by a dominant background, called heat-only events. That is why they are studied in detail in this work. They are characterized by a rise in heat seen by thermal sensors without any ionization signal on the collecting electrodes. This study resulted in to highlight a model for these events that can be used in the WIMP search analyses. Following these results, a maximum likelihood analysis was constructed. This method of analysis makes it possible to statistically subtract the background noise from the experiment by exploiting the difference between the energy spectra of signal and backgrounds. In this way, limits on the spin-independent WIMP-nucleon cross-section are obtained. They will be compared to the results of other experiments; De nombreuses observations astrophysiques et cosmologiques tendent à prouver que la matière ordinaire (dite baryonique) ne constituerait qu'environ 5 % du contenu énergétique de l'Univers. Les principales composantes de celui-ci seraient l'énergie noire (à 70 %) ainsi que la matière noire (à 25 %). Cette dernière serait invisible et seuls ses effets gravitationnels traduiraient sa présence dans l'Univers. Plusieurs particules, regroupées sous le terme générique de WIMP (Weakly Interacting Massive Particles), pourraient correspondre à cette théorie et sont activement recherchées. Plusieurs dispositifs expérimentaux ont été développés dans ce but et s'appuyent sur les stratégies suivantes : la production de ces particules au sein de collisionneurs, l'observation de particules produites via l'annihilation de WIMP ou encore la détection directe de ces particules via leur interaction avec le noyau des atomes constitutifs d'un détecteur. C'est sur cette dernière méthode que s'appuie l'expérience EDELWEISS. Il s'agit d'une expérience de détection directe de matière noire dédiée à la recherche de WIMP de masse comprise entre 1 GeV et 1 TeV. Son but premier est de détecter les reculs nucléaires induits par la diffusion élastique de particule de matière noire dans les détecteurs. Les taux d'événements attendus < 10 /(kg.an) étant de plusieurs ordres de grandeur inférieurs à ceux induits par la radioactivité ambiante, une double mesure de l'ionisation et de la chaleur est employée pour discriminer les reculs électroniques induits par les bruits de fonds β et γ des reculs nucléaires induits par les WIMPs. De plus, l'expérience a été placée en site souterrain pour se prémunir des rayonnements cosmiques, induisant des événements dans les détecteurs. Ceux utilisés par l'expérience sont des bolomètres en germanium, appelés FID, refroidis à des températures cryogéniques (18 mK) et opérant à bas champ (1 V/cm). Depuis 2015, la nouvelle stratégie de l'expérience consiste à se focaliser sur les WIMPs de masse inférieure à 10 GeV, zone de recherche privilégiée pour les expériences utilisant des détecteurs cryogéniques. Le fonctionnement de l'expérience a donc été amélioré afin d'atteindre cet objectif.Le but de cette thèse consiste à analyser les campagnes de données de l'expérience, effectuées en 2015 et 2016. Celles-ci utilisaient les détecteurs FID soumis à un champ électrique plus important que précédemment afin d'améliorer leur sensibilité. La limite extraite à partir de ces données s'appuie sur la statistique de Poisson et a permis de mettre en évidence que le bruit de fond dominant de l'expérience à basse énergie impacte grandement les résultats. C'est pourquoi une étude de ces événements, appelés heat-only, a été réalisée. Ceux-ci se caractérisent par une élévation de chaleur vue par les senseurs thermiques sans que les électrodes du détecteur ne mesurent d'ionisation en son sein. Une étude de ce bruit de fond a été réalisée et a permis de mettre en évidence la possibilité de modéliser ces événements. Suite à ces résultats, une analyse par maximum de vraisemblance a été construite. Cette méthode d'analyse permet de soustraire de manière statistique les bruits de fond de l'expérience grâce à leurs spectres en énergie différents de ceux attendus pour un signal de matière noire. De cette façon, une limite sur la section efficace des WIMP a été calculée en utilisant pour la première fois des détecteurs FID soumis à des champs électriques supérieurs aux valeurs utilisées jusqu'à présent

Published
2018

21. Analysis of the data of the EDELWEISS-LT experiment searching for low-mass WIMP

Author

Queguiner, Emeline, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université de Lyon, Jules Gascon, and STAR, ABES

Subjects
WIMP, EDELWEISSS, Analyse de données, Direct detection, Data analysis, Likelihood, Maximum de vraisemblance, Bruit de fond, Matière noire, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Background, EDELWEISS, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Dark matter, Détection directe
Abstract

Many astrophysical and cosmological observations lead to postulate the existence of an unknown matter, called dark matter. Ordinary matter can explain only 5 % of the energy content of the Universe : the main components would be the dark energy (70 %) and dark matter (25 %). This latter is invisible and manifest itself only via its gravitational effects. Several particles, grouped under the generic term of WIMP (Weakly Interacting Massive Particles), could correspond to this theory and are actively searched. Many experiments have been developed for this purpose and are based on three strategies: the production of these particles with colliders, the observation of the particles produced by their annihilation in astrophysical objects or the direct detection of these particles via their interaction with the nucleus of the atoms constituent of a detector. It is on this last method that the EDELWEISS experiment is based. It is a dark matter direct detection experiment dedicated to the search for WIMP with masses between 1 GeV and 1 TeV. Its primary purpose is to detect nuclear recoils induced by elastic scattering of dark matter particles in detectors. Since the expected event rates < 10 /(kg.year) are several orders of magnitude lower than those induced by ambient radioactivity, a double measurement of ionization and heat is used to discriminate electron-induced recoils arising from β and γ interactions from WIMP-induced nuclear recoils. In addition, the experiment was placed underground to guard against cosmic radiation, inducing events in the detectors. These are germanium bolometers, called FID, cooled to cryogenic temperatures (18 mK) and operating at low field (1 V/cm). Since 2015, the new strategy of the experiment consists of focusing on WIMPs with mass below 10 GeV, an interessant research area where experiments using cryogenic detectors can exploit their ability to operate with experimental thresholds well below 1 keV. The operation of the experiment has been improved to achieve this goal. The aim of this thesis is to analyze the data set recorded by EDELWEISS in 2015 and 2016. These used the FID detectors subjected to a greater electric field than previously to improve their sensitivity. It is expected that the limit on the spin-independent WIMP-nucleon crosssection extracted from these data will be greatly impacted by a dominant background, called heat-only events. That is why they are studied in detail in this work. They are characterized by a rise in heat seen by thermal sensors without any ionization signal on the collecting electrodes. This study resulted in to highlight a model for these events that can be used in the WIMP search analyses. Following these results, a maximum likelihood analysis was constructed. This method of analysis makes it possible to statistically subtract the background noise from the experiment by exploiting the difference between the energy spectra of signal and backgrounds. In this way, limits on the spin-independent WIMP-nucleon cross-section are obtained. They will be compared to the results of other experiments, De nombreuses observations astrophysiques et cosmologiques tendent à prouver que la matière ordinaire (dite baryonique) ne constituerait qu'environ 5 % du contenu énergétique de l'Univers. Les principales composantes de celui-ci seraient l'énergie noire (à 70 %) ainsi que la matière noire (à 25 %). Cette dernière serait invisible et seuls ses effets gravitationnels traduiraient sa présence dans l'Univers. Plusieurs particules, regroupées sous le terme générique de WIMP (Weakly Interacting Massive Particles), pourraient correspondre à cette théorie et sont activement recherchées. Plusieurs dispositifs expérimentaux ont été développés dans ce but et s'appuyent sur les stratégies suivantes : la production de ces particules au sein de collisionneurs, l'observation de particules produites via l'annihilation de WIMP ou encore la détection directe de ces particules via leur interaction avec le noyau des atomes constitutifs d'un détecteur. C'est sur cette dernière méthode que s'appuie l'expérience EDELWEISS. Il s'agit d'une expérience de détection directe de matière noire dédiée à la recherche de WIMP de masse comprise entre 1 GeV et 1 TeV. Son but premier est de détecter les reculs nucléaires induits par la diffusion élastique de particule de matière noire dans les détecteurs. Les taux d'événements attendus < 10 /(kg.an) étant de plusieurs ordres de grandeur inférieurs à ceux induits par la radioactivité ambiante, une double mesure de l'ionisation et de la chaleur est employée pour discriminer les reculs électroniques induits par les bruits de fonds β et γ des reculs nucléaires induits par les WIMPs. De plus, l'expérience a été placée en site souterrain pour se prémunir des rayonnements cosmiques, induisant des événements dans les détecteurs. Ceux utilisés par l'expérience sont des bolomètres en germanium, appelés FID, refroidis à des températures cryogéniques (18 mK) et opérant à bas champ (1 V/cm). Depuis 2015, la nouvelle stratégie de l'expérience consiste à se focaliser sur les WIMPs de masse inférieure à 10 GeV, zone de recherche privilégiée pour les expériences utilisant des détecteurs cryogéniques. Le fonctionnement de l'expérience a donc été amélioré afin d'atteindre cet objectif.Le but de cette thèse consiste à analyser les campagnes de données de l'expérience, effectuées en 2015 et 2016. Celles-ci utilisaient les détecteurs FID soumis à un champ électrique plus important que précédemment afin d'améliorer leur sensibilité. La limite extraite à partir de ces données s'appuie sur la statistique de Poisson et a permis de mettre en évidence que le bruit de fond dominant de l'expérience à basse énergie impacte grandement les résultats. C'est pourquoi une étude de ces événements, appelés heat-only, a été réalisée. Ceux-ci se caractérisent par une élévation de chaleur vue par les senseurs thermiques sans que les électrodes du détecteur ne mesurent d'ionisation en son sein. Une étude de ce bruit de fond a été réalisée et a permis de mettre en évidence la possibilité de modéliser ces événements. Suite à ces résultats, une analyse par maximum de vraisemblance a été construite. Cette méthode d'analyse permet de soustraire de manière statistique les bruits de fond de l'expérience grâce à leurs spectres en énergie différents de ceux attendus pour un signal de matière noire. De cette façon, une limite sur la section efficace des WIMP a été calculée en utilisant pour la première fois des détecteurs FID soumis à des champs électriques supérieurs aux valeurs utilisées jusqu'à présent

Published
2018

22. Astroparticle Physics with H.E.S.S.: recents results and nearfuture prospects

Author

Emmanuel Moulin, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, and H.E.S.S.

Subjects
Physics beyond the Standard Model, QC1-999, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, magnetic field, Astrophysics::Cosmology and Extragalactic Astrophysics, invariance: Lorentz, 01 natural sciences, 7. Clean energy, WIMP: dark matter, law.invention, Telescope, WIMP, law, HESS, 0103 physical sciences, 010306 general physics, 010303 astronomy & astrophysics, Cherenkov radiation, Astroparticle physics, Physics, new physics, Astrophysics::Instrumentation and Methods for Astrophysics, electron: cosmic radiation, Astronomy, imaging, Galaxy, violation: Lorentz, electron: spectrum, Cherenkov counter, gamma ray: VHE, Intergalactic travel, axion-like particles, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; H.E.S.S. is an array of five Imaging Atmospheric Cherenkov Telescopes located in Namibia. It is designed for observations of astrophysical sources emitting very-high-energy (VHE) gamma rays in the energy range from a few ten GeVs to several ten TeVs. The H.E.S.S. instrument consists of four identical 12 m diameter telescopes and a 28 m diameter telescope placed at the center of the array. An ambitious Astroparticle Physics program is being carried out by the H.E.S.S. collaboration searching for New Physics in the VHE gamma-ray sky. The program includes the search for WIMP dark matter and axion-like particles, tests of Lorentz invariance, cosmic-ray electron measurements, and search for intergalactic magnetic fields. I will present the latest results on dark matter search from the observations of the Galactic Centre region, the search for Lorentz invariance violation with the 2014 flare observation of Markarian 501, and the first measurement of the cosmic-ray electron spectrum up to 20 TeV. The future of the H.E.S.S. Astroparticle Physics program will be discussed.

Published
2018
Full Text
View/download PDF

23. Search for Ultra-low Mass Dark Matter

Author

Pierre Brun, Laurent Chevalier, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay

Subjects
Physics, Particle physics, photon: hidden sector, Large Hadron Collider, Photon, dark matter: mass, Dark matter, mass: upper limit, WIMP: dark matter, Standard Model, field theory: scalar, CERN LHC Coll, WIMP, axion, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], axion-like particles, Strong CP problem, proposed experiment, strong interaction: CP, Scalar field, Axion, talk: Point a Pitre 2018/06/25, experimental results
Abstract

International audience; The absence of observation of dark matter candidates above the GeV scale, at the LHC and in dedicated WIMP search experiments, led physicists to explore other mass domains, in particular below the electron-volt. Beside, the so-called strong CP problem is still an issue in the standard model. It can be solved by adding a new scalar field called axion. This scalar field could be a dark matter candidate. Depending of its coupling and in the range of mass ≈ [10^{−22},1] eV, it may solve the two issues described above at once. After the description of the strong CP problem and its simplest solution, I briefly present some mass limits for axions and similar fields (Axion Like Particle, Hidden Photon) and some of the experiments from which these limits have been extracted. At the end of this document, new limits on Hidden Photon are presented with a new experiment: Shuket.

Published
2018
Full Text
View/download PDF

24. Fermion masses and mixings and dark matter constraints in a model with radiative seesaw mechanism

Author

Nicolás Bernal, Ivo de Medeiros Varzielas, A. E. Cárcamo Hernández, Sergey Kovalenko, Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), and Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Down quark, fermion: mass, 7. Clean energy, 01 natural sciences, High Energy Physics - Phenomenology (hep-ph), neutrino: mass, dark matter: scalar, lepton: mass, Physics, fermion: mixing, Cabibbo–Kobayashi–Maskawa matrix, new physics, phase: CP, lepton: mixing, Mass matrix, Coupling (probability), High Energy Physics - Phenomenology, Seesaw mechanism, Cabibbo angle, neutrino: Majorana, Neutrino, quark: mixing, Quark, Nuclear and High Energy Physics, Particle physics, WIMP, FOS: Physical sciences, Discrete Symmetries, double-beta decay: (0neutrino), 0103 physical sciences, CP: violation, fermion: dark matter, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Neutrino Physics, 010306 general physics, numerical calculations, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, potential: scalar, quark: mass, seesaw model, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Beyond Standard Model, lcsh:QC770-798, [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics::Experiment, neutrino: mixing, texture, symmetry: family, Lepton, neutrino: mass: hierarchy, Quark Masses and SM Parameters
Abstract

We formulate a predictive model of fermion masses and mixings based on a $\Delta(27)$ family symmetry. In the quark sector the model leads to the viable mixing inspired texture where the Cabibbo angle comes from the down quark sector and the other angles come from both up and down quark sectors. In the lepton sector the model generates a predictive structure for charged leptons and, after radiative seesaw, an effective neutrino mass matrix with only one real and one complex parameter. We carry out a detailed analysis of the predictions in the lepton sector, where the model is only viable for inverted neutrino mass hierarchy, predicting a strict correlation between $\theta_{23}$ and $\theta_{13}$. We show a benchmark point that leads to the best-fit values of $\theta_{12}$, $\theta_{13}$, predicting a specific $\sin^2\theta_{23} \simeq 0.51$ (within the $3 \sigma$ range), a leptonic CP-violating Dirac phase $\delta \simeq 281.6 ^\circ$ and for neutrinoless double-beta decay $m_{ee} \simeq 41.3$ meV. We turn then to an analysis of the dark matter candidates in the model, which are stabilized by an unbroken $\mathbb{Z}_2$ symmetry. We discuss the possibility of scalar dark matter, which can generate the observed abundance through the Higgs portal by the standard WIMP mechanism. An interesting possibility arises if the lightest heavy Majorana neutrino is the lightest $\mathbb{Z}_2$-odd particle. The model can produce a viable fermionic dark matter candidate, but only as a feebly interacting massive particle (FIMP), with the smallness of the coupling to the visible sector protected by a symmetry and directly related to the smallness of the light neutrino masses., Comment: 24 pages, 5 figures. Version accepted for publication in JHEP

Published
2018
Full Text
View/download PDF

25. Anatomy of Eddington-like inversion methods in the context of dark matter searches

Author

Thomas Lacroix, Martin Stref, Julien Lavalle, Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire Univers et Particules de Montpellier ( LUPM ), and Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM )

Subjects
velocity, Cosmology and Nongalactic Astrophysics (astro-ph.CO), WIMP, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, galaxy: dark matter, FOS: Physical sciences, Context (language use), Primordial black hole, dark matter: phase space, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, anisotropy, Gravitational microlensing, gravitation: potential, 01 natural sciences, Gravitational potential, High Energy Physics - Phenomenology (hep-ph), dark matter: halo, 0103 physical sciences, galaxy: mass, distribution function, 010303 astronomy & astrophysics, Physics, mass: density, 010308 nuclear & particles physics, Astronomy and Astrophysics, Observable, suppression, Astrophysics - Astrophysics of Galaxies, Dark matter halo, High Energy Physics - Phenomenology, annihilation, Astrophysics of Galaxies (astro-ph.GA), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [ PHYS.HPHE ] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Halo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, signature, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Irrespective of the dark matter (DM) candidate, several potentially observable signatures derive from the velocity distribution of DM in halos, in particular in the Milky Way (MW) halo. Examples include direct searches for weakly-interacting massive particles (WIMPs), $p$-wave suppressed or Sommerfeld-enhanced annihilation signals, microlensing events of primordial black holes (PBHs), {\em etc}. Most current predictions are based on the Maxwellian approximation which is not only theoretically inconsistent in bounded systems, but also not supported by cosmological simulations. A more consistent method sometimes used in calculations for direct WIMP searches relies on the so-called Eddington inversion method, which relates the DM phase-space distribution function (DF) to its mass density profile and the total gravitational potential of the system. Originally built upon the isotropy assumption, this method can be extended to anisotropic systems. We investigate these inversion methods in the context of Galactic DM searches, motivated by the fact that the MW is a strongly constrained system, and should be even more so with the ongoing Gaia survey. We still draw conclusions that apply to the general case. In particular, we illustrate how neglecting the radial boundary of the DM halo leads to theoretical inconsistencies. We also show that several realistic configurations of the DM halo and the MW baryonic content entail ill-defined DFs, significantly restricting the configuration space over which these inversion methods can apply. We propose consistent solutions to these issues. Finally, we compute several observables inferred from constrained Galactic mass models relevant to DM searches (WIMPs or PBHs), {\em e.g.} moments and inverse moments of the DM speed and relative speed distributions., 46 pages, 15 figures, minor changes, matches the published version

Published
2018
Full Text
View/download PDF

26. Towards a Mixed-Reality Interface for Mind-Mapping

Author

Martin Hachet, Philippe Giraudeau, Popular interaction with 3d content (Potioc), Laboratoire Bordelais de Recherche en Informatique (LaBRI), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-École Nationale Supérieure d'Électronique, Informatique et Radiocommunications de Bordeaux (ENSEIRB)-Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-École Nationale Supérieure d'Électronique, Informatique et Radiocommunications de Bordeaux (ENSEIRB)-Inria Bordeaux - Sud-Ouest, Institut National de Recherche en Informatique et en Automatique (Inria)-Institut National de Recherche en Informatique et en Automatique (Inria), Université de Bordeaux (UB)-Centre National de la Recherche Scientifique (CNRS)-École Nationale Supérieure d'Électronique, Informatique et Radiocommunications de Bordeaux (ENSEIRB), Université de Bordeaux (UB)-École Nationale Supérieure d'Électronique, Informatique et Radiocommunications de Bordeaux (ENSEIRB)-Centre National de la Recherche Scientifique (CNRS)-Université de Bordeaux (UB)-École Nationale Supérieure d'Électronique, Informatique et Radiocommunications de Bordeaux (ENSEIRB)-Centre National de la Recherche Scientifique (CNRS)-Inria Bordeaux - Sud-Ouest, and Université de Bordeaux (UB)-École Nationale Supérieure d'Électronique, Informatique et Radiocommunications de Bordeaux (ENSEIRB)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Computer science, Interface (Java), H5m [Information interfaces and presentation (eg, Digital content, [SCCO.COMP]Cognitive science/Computer science, 02 engineering and technology, computer.software_genre, Mind-Mapping, HCI)]: Miscellaneous, WIMP, Human–computer interaction, 0202 electrical engineering, electronic engineering, information engineering, Learning, 0501 psychology and cognitive sciences, [INFO.INFO-HC]Computer Science [cs]/Human-Computer Interaction [cs.HC], 050107 human factors, Mixed-Reality interface, Multimedia, 05 social sciences, ACM Classification Keywords, [SDV.NEU.SC]Life Sciences [q-bio]/Neurons and Cognition [q-bio.NC]/Cognitive Sciences, 020207 software engineering, Cognition, Mixed reality, Author Keywords, computer
Abstract

International audience; In this work, we have explored an approach based on the hybridisation of physical and digital content for mind-mapping activities at schools. Based on the literature in the fields of cognitive science and HCI, we have designed a mixed-reality (MR) interface called Reality-Map. We conducted a pilot study with 11 participants suggesting that learning and manipulating information about the brain and their cognitive functions could be improved by the use of such a MR interface compared to a traditional WIMP interface.

Published
2017
Full Text
View/download PDF

27. Low-mass WIMP searches with the EDELWEISS experiment

Author

J. Gascon, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), EDELWEISS, Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
History, Dark matter, WIMP: mass, EDELWEISS, dark matter: direct detection, 01 natural sciences, WIMP: dark matter, Education, thermal, Nuclear physics, WIMP, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Direct search, 010306 general physics, semiconductor detector: germanium, Physics, 010308 nuclear & particles physics, background, Third generation, Computer Science Applications, talk: Sudbury 2017/07/24, cryogenics, Weakly interacting massive particles, radioactivity, Underground laboratory, Frejus, readout, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], performance, experimental results
Abstract

The EDELWEISS experiment is a direct search for Weakly Interacting Massive Particles (WIMP) dark matter using an array of twenty-four 860 g cryogenic germanium detectors equipped with a full charge and thermal signal readout. The experiment is located in the ultra-low radioactivity environment of the Modane underground laboratory in the Frejus tunnel. WIMP limits, background rejection factors and measurements of cosmogenic activation recorded in long exposures are used to assess the performance of the third generation of EDELWEISS detectors in view of the search for WIMPs in the mass range from 1 to 20 GeV/c2. The developments in progress to pursue this goal in the coming years are also presented.

Published
2017
Full Text
View/download PDF

28. Status and Prospects of the EDELWEISS-III Direct WIMP Search Experiment

Author

R. Maisonobe, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Particle physics, WIMP, Dark matter, EDELWEISS, 7. Clean energy, 01 natural sciences, WIMP: dark matter, radioactivity: induced, 0103 physical sciences, germanium: detector, General Materials Science, Direct search, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, activity report, Physics, 010308 nuclear & particles physics, background, Condensed Matter Physics, Atomic and Molecular Physics, and Optics, Third generation, cosmic radiation, Underground laboratory, Data analysis, Cryogenic detectors, Germanium detectors, performance
Abstract

The EDELWEISS collaboration is performing a direct search for WIMP dark matter using an array of up to twenty-four 820–890 g cryogenic germanium detectors equipped with a full charge and thermal signal readout. The experiment is located in the ultra-low-radioactivity background environment of the Modane underground laboratory, in the French–Italian Frejus tunnel. We present the analysis of data obtained in extended data taking periods. WIMP limits, background rejection factors and measurements of cosmogenic activation are used to assess the performance of the third generation of EDELWEISS detectors in view of the search for WIMPs in the mass range from 1 to $$20~\hbox {GeV}/\hbox {c}^{2}$$ . The developments in progress to pursue this goal in the coming years are also presented.

Published
2017
Full Text
View/download PDF

29. Preliminary Results of the $Fermi$ High-Latitude Extended Source Catalog

Author

Regina Caputo, Manuel Meyer, Mattia Di Mauro, Matthew J.A. Wood, Jonathan Biteau, Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and Fermi-LAT

Subjects
WIMP, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, deflection, Population, Dark matter, FOS: Physical sciences, magnetic field, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, gamma ray: absorption, 7. Clean energy, 01 natural sciences, blazar, cascade: electromagnetic, dark matter: halo, 0103 physical sciences, 010306 general physics, Blazar, education, Astrophysics::Galaxy Astrophysics, gamma ray: energy, Background radiation, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), coherence: length, education.field_of_study, electron positron, interpretation of experiments: GLAST, 010308 nuclear & particles physics, dark matter: annihilation, flux, gamma ray: emission, angular resolution, 13. Climate action, Weakly interacting massive particles, Intergalactic travel, photon: background, galaxy, Astrophysics - High Energy Astrophysical Phenomena, numerical calculations: Monte Carlo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], radiation: background, Fermi Gamma-ray Space Telescope
Abstract

We report on preliminary results from the Fermi High-Latitude Extended Sources Catalog (FHES), a comprehensive search for spatially extended gamma-ray sources at high Galactic latitudes ($|b|>5^\circ$) based on data from the Fermi Large Area Telescope (LAT). While the majority of high-latitude LAT sources are extragalactic blazars that appear point-like within the LAT angular resolution, there are several physics scenarios that predict the existence of populations of spatially extended sources. If Dark Matter consists of Weakly Interacting Massive Particles, the annihilation or decay of these particles in subhalos of the Milky Way would appear as a population of unassociated gamma-ray sources with finite angular extent. Gamma-ray emission from blazars could also be extended (so-called pair halos) due to the deflection of electron-positron pairs in the intergalactic magnetic field (IGMF). The pairs are produced in the absorption of gamma rays in the intergalactic medium and subsequently up-scatter photons of background radiation fields to gamma-ray energies. Measurement of pair halos could provide constraints on the strength and coherence length scale of the IGMF. In a dedicated search, we find 21 extended sources and 16 sources not previously characterized as extended. Limits on the flux of the extended source components are used to derive constraints on the strength of the IGMF using spectral and spatial templates derived from Monte Carlo simulations of electromagnetic cascades. This allows us to constrain the IGMF to be stronger than $3\times10^{-16}\,$G for a coherence length $\lambda \gtrsim 10\,$kpc., Comment: Proc. 35th ICRC, Busan, South Korea, PoS(ICRC2017)647

Published
2017
Full Text
View/download PDF

30. M31 gamma ray emission - a closer look at different explanations

Author

Jovana Petrović, Tijana Prodanovic, Pasquale D. Serpico, Christopher Eckner, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), and Fermi-LAT

Subjects
WIMP, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Population, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, GLAST, cross section: annihilation, Pulsar, Millisecond pulsar, structure, education, Astrophysics::Galaxy Astrophysics, pulsar, Physics, education.field_of_study, Annihilation, Galactic Center, dark matter: annihilation, Galaxy, gamma ray: emission, Weakly interacting massive particles, adiabatic, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], upper limit
Abstract

International audience; A new measurement of a spatially extended gamma-ray signal from the center of M31 was published recently (Ackermann et al. 2017, ApJ 836, 208), reporting that the emission broadly resembles the Galactic center excess (GCE) of the Milky Way (MW). In this contribution we discuss the possibilities that the signal originates from a population of millisecond pulsars (MSPs), or alternatively the annihilation of dark matter (DM) particles. As an astrophysical interpretation in terms of MSPs appears viable, we derive upper limits on the annihilation cross section in the bb/τ +τ −-channel of weakly interacting massive particles (WIMPs) in a mass range from 1 GeV to 10 TeV, taking into consideration different DM density profiles and including the effect of substructure and adiabatic contraction.

Published
2017
Full Text
View/download PDF

31. First detection of radon progeny recoil tracks by MIMAC

Author

L. Lebreton, Jose Busto, Jerome Bouvier, O. Guillaudin, Jürgen Brunner, D. Santos, D. Fouchez, I. Giomataris, T. Descombes, P. Colas, Jean-François Muraz, Q. Riffard, G. Bosson, D. Maire, E. Ferrer-Ribas, Ch. Fourel, O. Bourrion, C. Tao, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Institut de Radioprotection et de Sûreté Nucléaire (IRSN), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and MIMAC

Subjects
Elastic scattering, Physics, Time projection chamber, 010308 nuclear & particles physics, Physics::Instrumentation and Detectors, Dark matter, Astrophysics::Instrumentation and Methods for Astrophysics, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], 7. Clean energy, 01 natural sciences, Particle detector, Dark matter halo, Nuclear physics, Recoil, WIMP, 0103 physical sciences, Measuring instrument, 010306 general physics, Nuclear Experiment, Instrumentation, Mathematical Physics
Abstract

11 pages, 12 figures, submitted to PRD; International audience; The MIMAC experiment is a $\mu$-TPC matrix project for directional dark matter search. Directional detection is a strategy based on the measurement of the WIMP flux anisotropy due to the solar system motion with respect to the dark matter halo. The main purpose of MIMAC project is the measurement of the energy and the direction of nuclear recoils in 3D produced by elastic scattering of WIMPs. Since June 2012 a bi-chamber prototype is operating at the Modane underground laboratory. In this paper, we report the first ionization energy and 3D track observations of nuclear recoils produced by the radon progeny. This measurement shows the capability of the MIMAC detector and opens the possibility to explore the low energy recoil directionality signature.

Published
2017
Full Text
View/download PDF

32. Removing krypton from xenon by cryogenic distillation to the ppq level

Author

Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Amaro, F. D., Anthony, M., Arneodo, F., Barrow, P., Baudis, L., Bauermeister, B., Benabderrahmane, M. L., Berger, T., Breur, P. A., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Bütikofer, L., Calvén, J., Cardoso, J. M. R., Cervantes, M., Cichon, D., Coderre, D., Colijn, A. P., Conrad, J., Cussonneau, J. P., Decowski, M. P., Perio, P., Di Gangi, P., Di Giovanni, A., Diglio, S., Duchovni, E., Eurin, G., Fei, J., Ferella, A. D., Fieguth, A., Franco, D., Fulgione, W., Andrea Gallo Rosso, Galloway, M., Gao, F., Garbini, M., Geis, C., Goetzke, L. W., Grandi, L., Greene, Z., Grignon, C., Hasterok, C., Hogenbirk, E., Huhmann, C., Itay, R., Kaminsky, B., Kessler, G., Kish, A., Landsman, H., Lang, R. F., Lellouch, D., Levinson, L., Le Calloch, M., Lin, Q., Lindemann, S., Lindner, M., Lopes, J. A. M., Manfredini, A., Maris, I., Marrodán Undagoitia, T., Masbou, J., Massoli, F. V., Masson, D., Mayani, D., Meng, Y., Messina, M., Micheneau, K., Miguez, B., Molinario, A., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Orrigo, S. E. A., Pakarha, P., Pelssers, B., Persiani, R., Piastra, F., Pienaar, J., C Piro, M., Pizzella, V., Plante, G., Priel, N., Rauch, L., Reichard, S., Reuter, C., Rizzo, A., Rosendahl, S., Rupp, N., Saldanha, R., Dos Santos, J. M. F., Sartorelli, G., Scheibelhut, M., Schindler, S., Schreiner, J., Schumann, M., Scotto Lavina, L., Selvi, M., Shagin, P., Shockley, E., Silva, M., Simgen, H., Sivers, M. V., Stein, A., Thers, D., Tiseni, A., Trinchero, G., Tunnell, C., Upole, N., Wang, H., Wei, Y., Weinheimer, C., Wulf, J., Ye, J., Zhang, Y., Cristescu, I., Xenon, Collaboration, Laboratoire SUBATECH Nantes (SUBATECH), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), XENON (IHEF, IoP, FNWI), Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Amaro, F.D., Anthony, M., Arneodo, F., Barrow, P., Baudis, L., Bauermeister, B., Benabderrahmane, M.L., Berger, T., Breur, P.A., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Bütikofer, L., Calvén, J., Cardoso, J.M.R., Cervantes, M., Cichon, D., Coderre, D., Colijn, A.P., Conrad, J., Cussonneau, J.P., Decowski, M.P., Perio, P. de, Gangi, P. Di, Giovanni, A. Di, Diglio, S., Duchovni, E., Eurin, G., Fei, J., Ferella, A.D., Fieguth, A., Franco, D., Fulgione, W., Gallo Rosso, A., Galloway, M., Gao, F., Garbini, M., Geis, C., Goetzke, L.W., Grandi, L., Greene, Z., Grignon, C., Hasterok, C., Hogenbirk, E., Huhmann, C., Itay, R., Kaminsky, B., Kessler, G., Kish, A., Landsman, H., Lang, R.F., Lellouch, D., Levinson, L., Calloch, M. Le, Lin, Q., Lindemann, S., Lindner, M., Lopes, J.A.M., Manfredini, A., Maris, I., Undagoitia, T. Marrodán, Masbou, J., Massoli, F.V., Masson, D., Mayani, D., Meng, Y., Messina, M., Micheneau, K., Miguez, B., Molinario, A., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Orrigo, S.E.A., Pakarha, P., Pelssers, B., Persiani, R., Piastra, F., Pienaar, J., Piro, M.-C., Pizzella, V., Plante, G., Priel, N., Rauch, L., Reichard, S., Reuter, C., Rizzo, A., Rosendahl, S., Rupp, N., Saldanha, R., Santos, J.M.F., Sartorelli, G., Scheibelhut, M., Schindler, S., Schreiner, J., Schumann, M., Lavina, L. Scotto, Selvi, M., Shagin, P., Shockley, E., Silva, M., Simgen, H., Sivers, M., Stein, A., Thers, D., Tiseni, A., Trinchero, G., Tunnell, C., Upole, N., Wang, H., Wei, Y., Weinheimer, C., Wulf, J., Ye, J., Zhang, Y., and Cristescu, I.

Subjects
Cryostat, Physics - Instrumentation and Detectors, Xenon, Physics and Astronomy (miscellaneous), WIMP, Dark matter, Analytical chemistry, FOS: Physical sciences, chemistry.chemical_element, lcsh:Astrophysics, Weakly Interact Massive Particle, Sciences de l'ingénieur, 01 natural sciences, 7. Clean energy, lcsh:QB460-466, 0103 physical sciences, Dark Matter, lcsh:Nuclear and particle physics. Atomic energy. Radioactivity, Sensitivity (control systems), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Computer science, information & general works, Engineering (miscellaneous), Liquid Xenon, ComputingMilieux_MISCELLANEOUS, Physics, Air separation, Physique, 010308 nuclear & particles physics, Distillation Column, Krypton, Order (ring theory), Instrumentation and Detectors (physics.ins-det), Astronomie, chemistry, Direct Search, ddc:000, lcsh:QC770-798, TPC, Order of magnitude
Abstract

The XENON1T experiment aims for the direct detection of dark matter in a detector filled with 3.3 tons of liquid xenon. In order to achieve the desired sensitivity, the background induced by radioactive decays inside the detector has to be sufficiently low. One major contributor is the β-emitter 85Kr which is present in the xenon. For XENON1T a concentration of natural krypton in xenon natKr/Xe, 0, SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2017
Full Text
View/download PDF

33. Results from the search for dark matter in the Milky Way with 9 years of data of the ANTARES neutrino telescope

Author

Vladimir Kulikovskiy, Emanuele Leonora, Bruny Baret, A. Mathieu, A. Trovato, G. Illuminati, Michel André, Jutta Schnabel, Maria Tselengidou, Anne Deschamps, D. Turpin, C. Perrina, Hervé Glotin, A. Enzenhöfer, V. Van Elewyck, Matteo Sanguineti, M. Saldaña, C. Mueller, J. Barrios-Martí, C. Vallée, V. Giordano, Daniele Vivolo, G. Riccobene, I. Kreykenbohm, Dominique Lefèvre, M. Taiuti, I. El Bojaddaini, R. Mele, L. Quinn, L. Caramete, C. Lachaud, S. Galatà, T. Grégoire, C. Tönnis, Kay Graf, Karel Melis, Dominik Elsässer, M. Kreter, Gisela Anton, J.J. Hernández-Rey, J. Busto, Yahya Tayalati, Y. Hello, K. Roensch, C. Racca, Th. Stolarczyk, Ivan Felis, S. Basa, Matthias Kadler, J. Carr, J. Hößl, M. Circella, S. Wagner, H. van Haren, C. Pellegrino, R. Gracia Ruiz, T. Michael, J. Zúñiga, Antonio Capone, Miguel Ardid, C. Sieger, Jörn Wilms, Maurizio Spurio, Joao A B Coelho, A.J. Heijboer, P. Coyle, S.F. Biagi, F. Schüssler, P. Piattelli, Uli Katz, M. de Jong, I. Salvadori, Luigi Antonio Fusco, Corinne Donzaud, M. Jongen, C. Distefano, A. Albert, M. Marcelin, D. F. E. Samtleben, O. Kalekin, Annarita Margiotta, P. Migliozzi, Robert Lahmann, D. Drouhin, T. Seitz, A. Gleixner, T. Avgitas, M. Anghinolfi, V. Popa, H. Costantini, Abdelilah Moussa, Steffen Hallmann, J-J. Aubert, J.D. Zornoza, S. Loucatos, T. Pradier, R. Coniglione, J. Hofestädt, V. Bertin, A. Creusot, Tommaso Chiarusi, Antoine Kouchner, Jürgen Brunner, I. Di Palma, E. Nezri, R. Bruijn, B. Vallage, C. Hugon, Silvia Celli, Thomas Eberl, M. Lotze, A. Vizzoca, C. W. James, S. Bourret, D. Dornic, G. De Bonis, S. Geißelsöder, A. Sánchez-Losa, Alexis Coleiro, D. Kießling, A. Marinelli, K. Geyer, M.C. Bouwhuis, R. Bormuth, J.A. Martínez-Mora, Paolo Sapienza, G.E. Păvălaş, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Laboratoire de Physique de Clermont (LPC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Clermont Auvergne [2017-2020] (UCA [2017-2020])-Centre National de la Recherche Scientifique (CNRS), ANTARES, Albert, A., André, M., Anghinolfi, M., Anton, G., Ardid, M., Aubert, J.-J., Avgitas, T., Baret, B., Barrios-Martí, J., Basa, S., Bertin, V., Biagi, S., Bormuth, R., Bourret, S., Bouwhuis, M.C., Bruijn, R., Brunner, J., Busto, J., Capone, A., Caramete, L., Carr, J., Celli, S., Chiarusi, T., Circella, M., Coelho, J.A.B., Coleiro, A., Coniglione, R., Costantini, H., Coyle, P., Creusot, A., Deschamps, A., De Bonis, G., Distefano, C., Di Palma, I., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., El Bojaddaini, I., Elsässer, D., Enzenhöfer, A., Felis, I., Fusco, L.A., Galatà, S., Gay, P., Geißelsöder, S., Geyer, K., Giordano, V., Gleixner, A., Glotin, H., Grégoire, T., Gracia Ruiz, R., Graf, K., Hallmann, S., van Haren, H., Heijboer, A.J., Hello, Y., Hernández-Rey, J.J., Hößl, J., Hofestädt, J., Hugon, C., Illuminati, G., James, C.W., de Jong, M., Jongen, M., Kadler, M., Kalekin, O., Katz, U., Kießling, D., Kouchner, A., Kreter, M., Kreykenbohm, I., Kulikovskiy, V., Lachaud, C., Lahmann, R., Lefèvre, D., Leonora, E., Lotze, M., Loucatos, S., Marcelin, M., Margiotta, A., Marinelli, A., Martínez-Mora, J.A., Mathieu, A., Mele, R., Melis, K., Michael, T., Migliozzi, P., Moussa, A., Mueller, C., Nezri, E., Păvălaş, G.E., Pellegrino, C., Perrina, C., Piattelli, P., Popa, V., Pradier, T., Quinn, L., Racca, C., Riccobene, G., Roensch, K., Sánchez-Losa, A., Saldaña, M., Salvadori, I., Samtleben, D.F.E., Sanguineti, M., Sapienza, P., Schnabel, J., Schüssler, F., Seitz, T., Sieger, C., Spurio, M., Stolarczyk, Th., Taiuti, M., Tayalati, Y., Trovato, A., Tselengidou, M., Turpin, D., Tönnis, C, Vallage, B., Vallée, C., Van Elewyck, V., Vivolo, D., Vizzoca, A., Wagner, S., Wilms, J., Zornoza, J.D., Zúñiga, J., Albert, A, Andre, M, Anghinolfi, M, Anton, G, Ardid, M, Aubert, Jj, Avgitas, T, Baret, B, Barrios-Marti, J, Basa, S, Bertin, V, Biagi, S, Bormuth, R, Bourret, S, Bouwhuis, Mc, Bruijn, R, Brunner, J, Busto, J, Capone, A, Caramete, L, Carr, J, Celli, S, Chiarusi, T, Circella, M, Coelho, Jab, Coleiro, A, Coniglione, R, Costantini, H, Coyle, P, Creusot, A, Deschamps, A, De Bonis, G, Distefano, C, Di Palma, I, Donzaud, C, Dornic, D, Drouhin, D, Eberl, T, El Bojaddaini, I, Elsasser, D, Enzenhofer, A, Felis, I, Fusco, La, Galata, S, Gay, P, Geisselsoder, S, Geyer, K, Giordano, V, Gleixner, A, Glotin, H, Gregoire, T, Ruiz, Rg, Graf, K, Hallmann, S, Van Haren, H, Heijboer, Aj, Hello, Y, Hernandez-Rey, Jj, Hossl, J, Hofestadt, J, Hugon, C, Illuminati, G, James, Cw, de Jong, M, Jongen, M, Kadler, M, Kalekin, O, Katz, U, Kiessling, D, Kouchner, A, Kreter, M, Kreykenbohm, I, Kulikovskiy, V, Lachaud, C, Lahmann, R, Lefevre, D, Leonora, E, Lotze, M, Loucatos, S, Marcelin, M, Margiotta, A, Marinelli, A, Maritnez-Mora, Ja, Mathieu, A, Mele, R, Melis, K, Michael, T, Migliozzi, P, Moussa, A, Mueller, C, Nezri, E, Pavalas, Ge, Pellegrino, C, Perrina, C, Piattelli, P, Popa, V, Pradier, T, Quinn, L, Racca, C, Riccobene, G, Roensch, K, Sanchez-Losa, A, Saldana, M, Salvadori, I, Samtleben, Dfe, Sanguineti, M, Sapienza, P, Schnabel, J, Schussler, F, Seitz, T, Sieger, C, Spurio, M, Stolarczyk, T, Taiuti, M, Tayalati, Y, Trovato, A, Tselengidou, M, Turpin, D, Tonnis, C, Vallage, B, Vallee, C, Van Elewyck, V, Vivolo, D, Vizzoca, A, Wagner, S, Wilms, J, Zornoza, Jd, Zuniga, J, Centre Tecnològic de Vilanova i la Geltrú, Universitat Politècnica de Catalunya. LAB - Laboratori d'Aplicacions Bioacústiques, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), KM3NeT (IHEF, IoP, FNWI), Andre, M., Aubert, J. -J., Barrios-Marti, J., Bouwhuis, M. C., Coelho, J. A. B., Elsasser, D., Enzenhofer, A., Fusco, L. A., Galata, S., Geisselsoder, S., Gregoire, T., Heijboer, A. J., Hernandez-Rey, J. J., Hossl, J., Hofestadt, J., James, C. W., Kiessling, D., Lefevre, D., Martinez-Mora, J. A., Pavalas, G. E., Sanchez-Losa, A., Saldana, M., Samtleben, D. F. E., Schussler, F., Stolarczyk, T., Tonnis, C., Vallee, C., Zornoza, J. D., Zuniga, J., and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
Astrofísica, MathematicsofComputing_GENERAL, Astrophysics, Neutrino telescope, 01 natural sciences, law.invention, WIMP, law, 010303 astronomy & astrophysics, Neutrino Telescope, Galactic Centre, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Annihilation, Astrophysics::Instrumentation and Methods for Astrophysics, TheoryofComputation_GENERAL, ANTARES, Dark matter, Indirect detection, lcsh:QC1-999, Milky Way, Neutrino detector, Dark matter (Astronomy), Computer Science::Mathematical Software, Matèria fosca (Astronomia), Halo, Astrophysics - High Energy Astrophysical Phenomena, Particle physics, Nuclear and High Energy Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Energia fosca (Astronomia), Computer Science::Digital Libraries, Telescope, 0103 physical sciences, Neutrins, Neutrinos, Via Làctia, Muon, 010308 nuclear & particles physics, 13. Climate action, Física::Astronomia i astrofísica [Àrees temàtiques de la UPC], FISICA APLICADA, High Energy Physics::Experiment, lcsh:Physics
Abstract

[EN] Using data recorded with the ANTARES telescope from 2007 to 2015, a new search for dark matter annihilation in the Milky Way has been performed. Three halo models and five annihilation channels, WIMP + WIMP -> b (b) over bar, W+W-, tau(+)tau(-), mu(+)mu(-) and v (v) over bar, with WIMP masses ranging from 50 2 GeV/C-2 to 100 Tev/C-2, were considered. No excess over the expected background was found, and limits on the thermally averaged annihilation cross-section were set., The authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Institut Universitaire de France (IUF), IdEx program and UnivEarthS Labex program at Sorbonne Paris Cite (ANR-10-LABX-0023 and ANR-11-IDEX-0005-02), Labex OCEVU (ANR-11-LABX-0060) and the A*MIDEX project (ANR-11-IDEX-0001-02), Region Ile-de-France (DIM-ACAV), Region Alsace (contrat CPER), Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung and Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Stichting voor Fundamenteel Onderzoek der Materie (FOM), Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS), Romania; Ministerio de Economia y Competitividad (MINECO): Plan Estatal de Investigacion (refs. FPA2015-65150-C3-1-P, -2-P and -3-P, (MINECO/FEDER)), Severo Ochoa Centre of Excellence and MultiDark Consolider (MINECO), and Prometeo and Grisolia programs (Generalitat Valenciana), Spain; Ministry of Higher Education, Scientific Research and Professional Training, Morocco. We also acknowledge the technical support of Ifremer, AIM and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities.

Published
2017
Full Text
View/download PDF

34. Multidimensional effective field theory analysis for direct detection of dark matter

Author

P. Cushman, David G. Cerdeño, F. Livet, H. E. Rogers, Vuk Mandic, École normale supérieure - Cachan (ENS Cachan), and École normale supérieure - Cachan ( ENS Cachan )

Subjects
Particle physics, dimension: 5, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Isoscalar, Dark matter, Nuclear Theory, Massive particle, FOS: Physical sciences, WIMP: mass, Parameter space, dark matter: direct detection, Bayesian inference, 01 natural sciences, High Energy Physics - Experiment, energy dependence, Momentum, High Energy Physics - Experiment (hep-ex), WIMP, [ PHYS.HEXP ] Physics [physics]/High Energy Physics - Experiment [hep-ex], isoscalar, 0103 physical sciences, Effective field theory, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010303 astronomy & astrophysics, scattering amplitude: momentum dependence, Physics, 010308 nuclear & particles physics, background, nucleus, statistical analysis: Bayesian, tension, effective field theory: higher-dimensional, dark matter: scattering, efficiency, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The scattering of dark matter particles off nuclei in direct detection experiments can be described in terms of a multidimensional effective field theory (EFT). A new systematic analysis technique is developed using the EFT approach and Bayesian inference methods to exploit, when possible, the energy-dependent information of the detected events, experimental efficiencies, and backgrounds. Highly dimensional likelihoods are calculated over the mass of the weakly interacting massive particle (WIMP) and multiple EFT coupling coefficients, which can then be used to set limits on these parameters and choose models (EFT operators) that best fit the direct detection data. Expanding the parameter space beyond the standard spin-independent isoscalar cross section and WIMP mass reduces tensions between previously published experiments. Combining these experiments to form a single joint likelihood leads to stronger limits than when each experiment is considered on its own. Simulations using two nonstandard operators (3 and 8) are used to test the proposed analysis technique in up to five dimensions and demonstrate the importance of using multiple likelihood projections when determining constraints on WIMP mass and EFT coupling coefficients. In particular, this shows that an explicit momentum dependence in dark matter scattering can be identified., 21 pages, 11 figures

Published
2017
Full Text
View/download PDF

35. Gravitational focusing of Imperfect Dark Matter

Author

Eugeny Babichev, Sabir Ramazanov, Laboratoire de Physique Théorique d'Orsay [Orsay] (LPT), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Théorique d'Orsay [Orsay] ( LPT ), Université Paris-Sud - Paris 11 ( UP11 ) -Centre National de la Recherche Scientifique ( CNRS ), and Centre National de la Recherche Scientifique (CNRS)-Université Paris-Sud - Paris 11 (UP11)

Subjects
High Energy Physics - Theory, Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), WIMP, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, gravitation: effect, Scalar field dark matter, FOS: Physical sciences, Lambda-CDM model, General Relativity and Quantum Cosmology (gr-qc), gravitation: potential, 01 natural sciences, General Relativity and Quantum Cosmology, Horava-Lifshitz, pressure: low, [ PHYS.GRQC ] Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], nonrelativistic, dark matter: halo, Quantum mechanics, 0103 physical sciences, energy: density, 010306 general physics, Light dark matter, enhancement, Physics, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], Hot dark matter, solar system, fluid: pressure, particle: interaction, Dark matter halo, High Energy Physics - Theory (hep-th), Physics::Space Physics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], dark matter: energy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Dark fluid, signature, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Motivated by the projectable Horava--Lifshitz model/mimetic matter scenario, we consider a particular modification of standard gravity, which manifests as an imperfect low pressure fluid. While practically indistinguishable from a collection of non-relativistic weakly interacting particles on cosmological scales, it leaves drastically different signatures in the Solar system. The main effect stems from gravitational focusing of the flow of Imperfect Dark Matter passing near the Sun. This entails strong amplification of Imperfect Dark Matter energy density compared to its average value in the surrounding halo. The enhancement is many orders of magnitude larger than in the case of Cold Dark Matter, provoking deviations of the metric in the second order in the Newtonian potential. Effects of gravitational focusing are prominent enough to substantially affect the planetary dynamics. Using the existing bound on the PPN parameter $\beta_{PPN}$, we deduce a stringent constraint on the unique constant of the model., Comment: 34 pages, 1 figure. Clarifications and references added. Matches published version

Published
2017
Full Text
View/download PDF

36. $\mathcal O(10) M_\odot$ primordial black holes and string axion dark matter

Author

Inomata , Keisuke, Kawasaki , Masahiro, Mukaida , Kyohei, Tada , Yuichiro, Yanagida , Tsutomu, Institut d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Lagrange de Paris, Sorbonne Université (SU), Sorbonne Universités, Institut d'Astrophysique de Paris ( IAP ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut national des sciences de l'Univers ( INSU - CNRS ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), WIMP, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], FOS: Physical sciences, axion: string, power spectrum, dark matter, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), O(10), gravitational radiation: emission, axion, LIGO, inflation, strong interaction: CP, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, 85A40, 83C57, 83C35, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

LIGO-Virgo collaboration has found black holes as heavy as $M \sim 30M_\odot$ through the detections of the gravitational waves emitted during their mergers. Primordial black holes (PBHs) produced by inflation could be an origin of such events. While it is tempting to presume that these PBHs constitute all Dark Matter (DM), there exists a number of constraints for PBHs with $\mathcal{O} (10) M_\odot$ which contradict with the idea of PBHs as all DM. Also, it is known that weakly interacting massive particle (WIMP) that is a common DM candidate is almost impossible to coexist with PBHs. These observations motivate us to pursue another candidate of DM. In this paper, we assume that the string axion solving the strong CP problem makes up all DM, and discuss the coexistence of string axion DM and inflationary PBHs for LIGO events., Comment: 12 pages, 8 figures; v2: published version

Published
2017
Full Text
View/download PDF

37. Effective field theory search for high-energy nuclear recoils using the XENON100 dark matter detector

Author

Sara Diglio, F. V. Massoli, Qing Lin, J. Calvén, Ch. Weinheimer, Marc Schumann, P. Pakarha, W. Fulgione, J. Ye, A. Manfredini, M. Murra, Ben Farmer, Luke Goetzke, M. V. Sivers, Jean-Pierre Cussonneau, F. Lombardi, M.-C. Piro, L. Buetikofer, J.M.F. dos Santos, D. Masson, Bart Pelssers, C. Geis, C. Hasterok, C. Reuter, M. Messina, F. Agostini, M. L. Benabderrahmane, A. Rizzo, P. Di Gangi, P. de Perio, B. Kaminsky, Ethan Brown, Julien Masbou, Teresa Marrodán Undagoitia, Sebastian Lindemann, H. Simgen, L. Scotto Lavina, Yanxi Zhang, Yuehuan Wei, K. Morå, Zhou Wang, C. Tunnell, A. Di Giovanni, A. D. Ferella, M. Selvi, G. Eurin, Kaixuan Ni, Hongwei Wang, Giacomo Bruno, Gabriella Sartorelli, Uwe Oberlack, J. A. M. Lopes, A. Kish, L. Levinson, J. Pienaar, M. Garbini, Ioana Codrina Maris, V. Pizzella, C. Grignon, April S. Brown, K. Micheneau, R. Itay, G. Kessler, M. Alfonsi, S. Bruenner, J. Wulf, Laura Baudis, J. Naganoma, Jelle Aalbers, Z. Greene, J. Schreiner, Ran Budnik, M. P. Decowski, M. Vargas, Auke-Pieter Colijn, P. A. Breur, Manfred Lindner, F. D. Amaro, Guillaume Plante, A. Stein, M. Cervantes, R. Persiani, D. Cichon, P. Barrow, D. Lellouch, A. Fieguth, D. Coderre, Boris Bauermeister, Manuel Gameiro da Silva, F. Arneodo, A. Tiseni, J. Fei, A. Molinario, M. Scheibelhut, João Cardoso, Elena Aprile, F. Gao, Gian Carlo Trinchero, S. Schindler, N. Rupp, S. Reichard, F. Piastra, T. Berger, S. Rosendahl, N. Priel, Shingo Kazama, Jan Conrad, M. Anthony, R. F. Lang, E. Hogenbirk, P. Shagin, D. Mayani, Dominique Thers, L. Rauch, H. Landsman, A. Gallo Rosso, A. Di Galloway, Laboratoire de physique subatomique et des technologies associées (SUBATECH), Université de Nantes - Faculté des Sciences et des Techniques, Université de Nantes (UN)-Université de Nantes (UN)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), Institut Mines-Télécom [Paris] (IMT)-Institut Mines-Télécom [Paris] (IMT), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), XENON, Laboratoire de physique subatomique et des technologies associées ( SUBATECH ), IMT Atlantique Bretagne-Pays de la Loire ( IMT Atlantique ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ) -Université de Nantes ( UN ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Amaro, F.D., Anthony, M., Arneodo, F., Barrow, P., Baudis, L., Bauermeister, B., Benabderrahmane, M.L., Berger, T., Breur, P.A., Brown, A., Brown, E., Bruenner, S., Bruno, G., Budnik, R., Bütikofer, L., Calvén, J., Cardoso, J.M.R., Cervantes, M., Cichon, D., Coderre, D., Colijn, A.P., Conrad, J., Cussonneau, J.P., Decowski, M.P., De Perio, P., Di Gangi, P., Di Giovanni, A., Diglio, S., Eurin, G., Fei, J., Ferella, A.D., Fieguth, A., Fulgione, W., Gallo Rosso, A., Galloway, M., Gao, F., Garbini, M., Geis, C., Goetzke, L.W., Greene, Z., Grignon, C., Hasterok, C., Hogenbirk, E., Itay, R., Kaminsky, B., Kazama, S., Kessler, G., Kish, A., Landsman, H., Lang, R.F., Lellouch, D., Levinson, L., Lin, Q., Lindemann, S., Lindner, M., Lombardi, F., Lopes, J.A.M., Manfredini, A., Maris, I., Marrodán Undagoitia, T., Masbou, J., Massoli, F.V., Masson, D., Mayani, D., Messina, M., Micheneau, K., Molinario, A., Morå, K., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Pakarha, P., Pelssers, B., Persiani, R., Piastra, F., Pienaar, J., Pizzella, V., Piro, M.-C., Plante, G., Priel, N., Rauch, L., Reichard, S., Reuter, C., Rizzo, A., Rosendahl, S., Rupp, N., Dos Santos, J.M.F., Sartorelli, G., Scheibelhut, M., Schindler, S., Schreiner, J., Schumann, M., Scotto Lavina, L., Selvi, M., Shagin, P., Silva, M., Simgen, H., Sivers, M.V., Stein, A., Thers, D., Tiseni, A., Trinchero, G., Tunnell, C., Vargas, M., Wang, H., Wang, Z., Wei, Y., Weinheimer, C., Wulf, J., Ye, J., Farmer, B., Zhang, Y., Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), Université de Nantes (UN)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-IMT Atlantique Bretagne-Pays de la Loire (IMT Atlantique), and XENON (IHEF, IoP, FNWI)

Subjects
WIMP nucleon: scattering, Particle physics, data analysis method, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics and Astronomy (miscellaneous), Physics::Instrumentation and Detectors, WIMP, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, chemistry.chemical_element, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Nuclear physics, XENON, Xenon, statistical analysis, 0103 physical sciences, Effective field theory, Dark Matter, 010306 general physics, S030UDM, nucleus: recoil, Physics, Coupling constant, effective field theory: nonrelativistic, 010308 nuclear & particles physics, Scattering, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, dark matter: detector, chemistry, Weakly interacting massive particles, Direct Search, High Energy Physics::Experiment, TPC, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], recoil: energy, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

International audience; We report on weakly interacting massive particles (WIMPs) search results in the XENON100 detector using a nonrelativistic effective field theory approach. The data from science run II (34 kg×224.6 live days) were reanalyzed, with an increased recoil energy interval compared to previous analyses, ranging from (6.6–240) keVnr. The data are found to be compatible with the background-only hypothesis. We present 90% confidence level exclusion limits on the coupling constants of WIMP-nucleon effective operators using a binned profile likelihood method. We also consider the case of inelastic WIMP scattering, where incident WIMPs may up-scatter to a higher mass state, and set exclusion limits on this model as well.

Published
2017
Full Text
View/download PDF

38. Performance of the EDELWEISS-III experiment for direct dark matter searches

Author

B. Paul, Matthew R. Robinson, R. Maisonobe, A. Giuliani, C. Augier, P. Pari, E. Olivieri, V. Sanglard, J. Lin, S. Scorza, G. Garde, S. Hervé, N. Fourches, E. Yakushev, V. A. Kudryavtsev, M. Grollier, A. S. Zolotarova, M. Gros, C. Nones, Marc Weber, E. Queguiner, X. F. Navick, L. Hehn, T. de Boissière, F. Charlieux, Q. Arnaud, D.V. Poda, D. Tcherniakhovski, E. Armengaud, J. Billard, Yong Jin, C. Kéfélian, Alain Benoit, X. Zhang, P. Camus, L. Dumoulin, H. Rodenas, N. Foerster, A. Menshikov, T. Bergmann, K. Eitel, M. De Jesus, B. Schmidt, B. Siebenborn, V. Humbert, A. Juillard, H. Le-Sueur, H. Kraus, L. Vagneron, L. Bergé, V.B. Brudanin, M. Chapellier, M. Mancuso, V. Kozlov, G. Heuermann, J. Gascon, S. Marnieros, A. Cazes, S. V. Rozov, D. Filosofov, G. Bres, A. Broniatowski, Matthias Kleifges, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre de Nanosciences et de Nanotechnologies [Orsay] (C2N), Université Paris-Sud - Paris 11 (UP11)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Institut Rayonnement Matière de Saclay (IRAMIS), EDELWEISS, Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris-Sud - Paris 11 (UP11)-Centre National de la Recherche Scientifique (CNRS)-Université Paris-Saclay, Institut de Recherches sur les lois Fondamentales de l'Univers ( IRFU ), Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay, Institut de Physique Nucléaire de Lyon ( IPNL ), Université Claude Bernard Lyon 1 ( UCBL ), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Néel ( NEEL ), Université Grenoble Alpes [Saint Martin d'Hères]-Centre National de la Recherche Scientifique ( CNRS ), Centre de Sciences Nucléaires et de Sciences de la Matière ( CSNSM ), Université Paris-Sud - Paris 11 ( UP11 ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Rayonnement Matière de Saclay ( IRAMIS ), Hélium : du fondamental aux applications (NEEL - HELFA), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Electronique (NEEL - ElecLab), and Cryogénie (NEEL - Cryo)

Subjects
Physics - Instrumentation and Detectors, Dark matter, energy resolution, FOS: Physical sciences, EDELWEISS, 7. Clean energy, 01 natural sciences, Nuclear physics, WIMP, Ionization, 0103 physical sciences, germanium: detector, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, gamma ray: irradiation, Instrumentation and Methods for Astrophysics (astro-ph.IM), [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation, background: radioactivity, Mathematical Physics, nucleus: recoil, Physics, 010308 nuclear & particles physics, background, Detector, Instrumentation and Detectors (physics.ins-det), stability, Semiconductor detector, Full width at half maximum, efficiency, Ionization energy, Astrophysics - Instrumentation and Methods for Astrophysics, performance
Abstract

We present the results of measurements demonstrating the efficiency of the EDELWEISS-III array of cryogenic germanium detectors for direct dark matter searches. The experimental setup and the FID (Fully Inter-Digitized) detector array is described, as well as the efficiency of the double measurement of heat and ionization signals in background rejection. For the whole set of 24 FID detectors used for coincidence studies, the baseline resolutions for the fiducial ionization energy are mainly below 0.7 keV$_{ee}$ (FHWM) whereas the baseline resolutions for heat energies are mainly below 1.5 keV$_{ee}$ (FWHM). The response to nuclear recoils as well as the very good discrimination capability of the FID design has been measured with an AmBe source. The surface $\beta$- and $\alpha$-decay rejection power of $R_{\rm surf} < 4 \times 10^{-5}$ per $\alpha$ at 90% C.L. has been determined with a $^{210}$Pb source, the rejection of bulk $\gamma$-ray events has been demonstrated using $\gamma$-calibrations with $^{133}$Ba sources leading to a value of $R_{\gamma{\rm -mis-fid}} < 2.5 \times 10^{-6}$ at 90% C.L.. The current levels of natural radioactivity measured in the detector array are shown as the rate of single $\gamma$ background. The fiducial volume fraction of the FID detectors has been measured to a weighted average value of $(74.6 \pm 0.4)\%$ using the cosmogenic activation of the $^{65}$Zn and $^{68,71}$Ge isotopes. The stability and uniformity of the detector response is also discussed. The achieved resolutions, thresholds and background levels of the upgraded EDELWEISS-III detectors in their setup are thus well suited to the direct search of WIMP dark matter over a large mass range.

Published
2017
Full Text
View/download PDF

39. DarkSide

Author

Bottino, Bianca, Bossa, M., Mandarano, A., Savarese, C., Razeto, A., Bonfini, G., Candela, A., Carlini, M., Cavalcante, P., Deo, M. De, D'Incecco, M., Gabriele, F., Goretti, A.M., Ianni, A., Orsini, M., Rossi, N., Sablone, D., Tartaglia, R., Pallavicini, M., Testera, G., Cariello, M., Marini, L., Musico, P., Pagani, L., Davini, S., Mari, S.M., Budano, F., Bussino, S., De Vincenzi, M., James, I., Fiorillo, G., Catalanotti, S., Cocco, A.G., Covone, G., Granato, F., Rossi, B., Trinchese, P., Walker, S., Devoto, A., Cadeddu, M., Cadoni, M., Lissia, M., Ranucci, G., Brigatti, A., D'Angelo, D., Lombardi, P., Parmeggiano, S., Saggese, P., Franco, D., Agnes, P., Tonazzo, A., De Cecco, S., Giganti, C., Galbiati, C., Meyers, P.D., Albuquerque, I.F.M., Brodsky, J., Cao, H., Calaprice, F., Koh, G., Li, Xiaojian, Qian, H., Sands, W., Shields, E., Stanford, C., Wada, M., Westerdale, S., Xiang, X., Xu, J., Zhu, C., Pordes, S., Biery, K., Forster, G., Herner, K., Guardincerri, Y., Kendziora, C.L., Yoo, J., Wang, H., Fan, A., Suvorov, Y., Pocar, A., Monte, A., Randle, K., Maricic, J., Edkins, E., Hackett, B.R., Milincic, R., Reinhold, B., Hungerford, E.V., Renshaw, A.L., Canci, N., Empl, A., Korga, G., Singh, P.N., Martoff, C.J., Napolitano, J., Miletic, T., Watson, A.W., Pantic, E., Johnson, T.N., Chepurnov, A., Gromov, M., Smirnov, O., Fomenko, K., Korablev, D., Sotnikov, A., Wishneva, A., Wojcik, M.M., Pelczar, K., Zuzel, G., Derbin, A., Muratova, V.N., Semenov, D.A., Unzhakov, E.V., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
cross section, Physics::Instrumentation and Detectors, WIMP, background, Astrophysics::Instrumentation and Methods for Astrophysics, dip, spin, dark matter, Gran Sasso, liquid argon, WIMP nucleon, neutral particle, recoil, atmosphere, High Energy Physics::Experiment, photomultiplier: silicon, Nuclear Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], upper limit
Abstract

International audience; The DarkSide project at Laboratori Nazionali del Gran Sasso (LNGS) is a dark matter direct search experiment based on the detection of rare nuclear recoils possibly induced by hypothetical dark matter particles, which are supposed to be neutral, massive (> 10 GeV) and weakly interacting (WIMP). DarkSide aims to perform background-free WIMP searches using a series of dual-phase liquid argon time projection chambers filled with ultra-pure liquid argon. The detector currently operating at LNGS is DarkSide-50, a detector which holds 46 kg of active liquid argon and is now filled with argon extracted from underground and taking data in its final configuration. Combining the underground argon data with the preceding search made with atmospheric argon, a 90% C.L. upper limit on the WIMP-nucleon spin-independent cross section of 2.0×10−44 cm2 is set. The next phase of the experiment foresees the construction of a new detector with an active mass of ∼ 20 and equipped with silicon photomultipliers, called DarkSide-20k.

Published
2016
Full Text
View/download PDF

40. Optimizing Cryogenic Detectors for Low-Mass WIMP Searches

Author

J. Billard, Q. Arnaud, A. Juillard, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)

Subjects
Physics, Particle physics, Physics::Instrumentation and Detectors, 010308 nuclear & particles physics, Detector, Dark matter, Scale (descriptive set theory), Parameter space, Condensed Matter Physics, 01 natural sciences, Atomic and Molecular Physics, and Optics, WIMP, 0103 physical sciences, High Energy Physics::Experiment, General Materials Science, Gradient boosting, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Neutrino, 010306 general physics, Low Mass, ComputingMilieux_MISCELLANEOUS
Abstract

This paper describes the methodology and results from a study dedicated to the optimization of cryogenic detectors for low-mass WIMP searches. Considering a data-driven background model from the EDELWEISS-III experiment, and two analysis methods, namely profile likelihood and boosted decision tree, we indentify the main experimental constraints and performances that have to be improved. We found that there is a clear difference in how to optimize the detector setup whether focusing on WIMPs with masses below 5 GeV or above. Finally, in the case of a hundred-kg scale experiment, we discuss the requirements to probe most of the parameter space region delimited by the ultimate neutrino bound below 6 GeV.

Published
2016
Full Text
View/download PDF

41. Gamma-ray signatures of Dark Matter

Author

Marco CIRELLI, Aldo Morselli, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), and Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
WIMP, QC1-999, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, dark matter: signature, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Photon energy, 7. Clean energy, 01 natural sciences, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, gamma ray: energy, Physics, radio wave, energy: high, 010308 nuclear & particles physics, Galactic Center, Bremsstrahlung, Gamma ray, Astronomy, photon: energy, Galaxy, bremsstrahlung: emission, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

International audience; I review the ways in which Dark Matter can produce gamma-rays (and lower energy photons) and I apply the considerations to three specific examples: the tests of multi-TeV pure-WIMP candidates based on high energy gamma-rays from the Galactic Center or dwarfs, the importance of bremsstrahlung emission for light DM, the updated constraints on DM from all-sky radio surveys of the Milky Way.

Published
2016
Full Text
View/download PDF

42. The DarkSide physics program and its recent results

Author

d'Angelo, D., Agnes, P., Agostino, L., Albuquerque, I.F.M., Alexander, T., Alton, A.K., Arisaka, K., Back, H.O., Baldin, B., Biery, K., Bonfini, G., Bossa, M., Bottino, B., Brigatti, A., Brodsky, J., Budano, F., Bussino, S., Cadeddu, M., Cadonati, L., Cadoni, M., Calaprice, F., Canci, N., Candela, A., Cao, H., Cariello, M., Carlini, M., Catalanotti, S., Cavalcante, P., Chepurnov, A., Cocco, A.G., Covone, G., Crippa, L., d'Incecco, M., Davini, S., de Cecco, S., de Deo, M., de Vincenzi, M., Derbin, A., Devoto, A., Di Eusanio, F., Di Pietro, G., Edkins, E., Empl, A., Fan, A., Fiorillo, G., Fomenko, K., Forster, G., Franco, D., Gabriele, F., Galbiati, C., Giganti, C., Goretti, A.M., Granato, F., Grandi, L., Gromov, M., Guan, M., Guardincerri, Y., Hackett, B.R., Herner, K., Hungerford, E.V., Ianni, Al., Ianni, An., James, I., Jollet, C., Keeter, K., Kendziora, C.L., Kobychev, V., Koh, G., Korablev, D., Korga, G., Kubankin, A., Lissia, M., Li, Xiaojian, Lombardi, P., Luitz, S., Machulin, I.N., Mandarano, A., Maricic, J., Marini, L., Mari, S.M., Martoff, C.J., Ma, Y., Meregaglia, A., Meyers, P.D., Miletic, T., Milincic, R., Montanari, D., Monte, A., Montuschi, M., Monzani, M., Mosteiro, P., Mount, B.J., Muratova, V.N., Musico, P., Napolitano, J., Nelson, A., Odrowski, S., Orsini, M., Ortica, F., Pagani, L., Pallavicini, M., Pantic, E., Parmeggiano, S., Pelczar, K., Pelliccia, N., Perasso, S., Pocar, A., Pordes, S., Pugachev, D.A., Qian, H., Randle, K., Ranucci, G., Razeto, A., Reinhold, B., Renshaw, A.L., Romani, A., Rossi, B., Rossi, N., Rountree, D., Sablone, D., Saggese, P., Saldanha, R., Sands, W., Sangiorgio, S., Savarese, C., Segreto, E., Semenov, D.A., Shields, E., Singh, P.N., Skorokhvatov, M.D., Smirnov, O., Sotnikov, A., Stanford, C., Suvorov, Y., Tartaglia, R., Tatarowicz, J., Testera, G., Tonazzo, A., Trinchese, P., Unzhakov, E.V., Vishneva, A., Vogelaar, B., Wada, M., Walker, S., Wang, H., Wang, Y., Watson, A.W., Westerdale, S., Wilhelmi, J., Wojcik, M.M., Xiang, X., Xu, J., Yang, C., Yoo, J., Zavatarelli, S., Zec, A., Zhong, W., Zhu, C., Zuzel, G., AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), D'Angelo, D., Agnes, P., Agostino, L., Albuquerque, I. F. M., Alexander, T., Alton, A. K., Arisaka, K., Back, H. O., Baldin, B., Biery, K., Bonfini, G., Bossa, M., Bottino, B., Brigatti, A., Brodsky, J., Budano, Federico, Bussino, Severino Angelo Maria, Cadeddu, M., Cadonati, L., Cadoni, M., Calaprice, F., Canci, N., Candela, A., Cao, H., Cariello, M., Carlini, M., Catalanotti, S., Cavalcante, P., Chepurnov, A., Cocco, A. G., Covone, G., Crippa, L., D'Incecco, M., Davini, S., De Cecco, S., De Deo, M., DE VINCENZI, Mario, Derbin, A., Devoto, A., Di Eusanio, F., Di Pietro, G., Edkins, E., Empl, A., Fan, A., Fiorillo, G., Fomenko, K., Forster, G., Franco, D., Gabriele, F., Galbiati, C., Giganti, C., Goretti, A. M., Granato, F., Grandi, L., Gromov, M., Guan, M., Guardincerri, Y., Hackett, B. R., Herner, K., Hungerford, E. V., Ianni, A. l., Ianni, A. n., James, Irina, Jollet, C., Keeter, K., Kendziora, C. L., Kobychev, V., Koh, G., Korablev, D., Korga, G., Kubankin, A., Lissia, M., Li, X., Lombardi, P., Luitz, S., Machulin, I. N., Mandarano, A., Maricic, J., Marini, L., Mari, Stefano Maria, Martoff, C. J., Ma, Y., Meregaglia, A., Meyers, P. D., Miletic, T., Milincic, R., Montanari, D., Monte, A., Montuschi, M., Monzani, M., Mosteiro, P., Mount, B. J., Muratova, V. N., Musico, P., Napolitano, J., Nelson, A., Odrowski, S., Orsini, M., Ortica, F., Pagani, L., Pallavicini, M., Pantic, E., Parmeggiano, S., Pelczar, K., Pelliccia, N., Perasso, S., Pocar, A., Pordes, S., Pugachev, D. A., Qian, H., Randle, K., Ranucci, G., Razeto, A., Reinhold, B., Renshaw, A. L., Romani, A., Rossi, B., Rossi, N., Rountree, D., Sablone, D., Saggese, P., Saldanha, R., Sands, W., Sangiorgio, S., Savarese, C., Segreto, E., Semenov, D. A., Shields, E., Singh, P. N., Skorokhvatov, M. D., Smirnov, O., Sotnikov, A., Stanford, C., Suvorov, Y., Tartaglia, R., Tatarowicz, J., Testera, G., Tonazzo, A., Trinchese, P., Unzhakov, E. V., Vishneva, A., Vogelaar, B., Wada, M., Walker, S., Wang, H., Wang, Y., Watson, A. W., Westerdale, S., Wilhelmi, J., Wojcik, M. M., Xiang, X., Xu, J., Yang, C., Yoo, J., Zavatarelli, S., Zec, A., Zhong, W., Zhu, C., Zuzel, G., Budano, F., Bussino, S., De Vincenzi, M., Ianni, A. L., Ianni, A. N., James, I., Mari, S. M., Maldonato, Nelson Mauro, Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), and Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
statistical analysis, WIMP, Cherenkov counter: water, direct detection, dark matter: detector, time projection chamber: liquid argon, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], activity report, deep underground detector, experimental results, Gran Sasso
Abstract

International audience; DarkSide (DS) at Gran Sasso underground laboratory is a direct Dark Matter search program based on Time Projection Chambers (TPC) with liquid Argon from underground sources. The DarkSide-50 (DS-50) TPC, with 150 kg of Argon is installed inside active neutron and muon detectors. DS-50 has been taking data since November 2013 with Atmospheric Argon (AAr) and since April 2015 with Underground Argon (UAr), depleted in radioactive 39Ar by a factor ∼ 1400. The exposure of 1422 kg d of AAr has demonstrated that the operation of DS-50 for three years in a background free condition is a solid reality, thanks to the superb performance of the Pulse Shape Analysis. The first release of results from an exposure of 2616 kg d of UAr has shown no candidate Dark Matter events. We have set the best limit for Spin-Independent elastic nuclear scattering of WIMPs obtained by Argon-based detectors, corresponding to a cross-section of 2 10−44 cm2 at a WIMP mass of 100 GeV. We present the detector design and performance, the results from the AAr run and the first results from the UAr run and we briefly introduce the future of the DarkSide program.

Published
2016
Full Text
View/download PDF

43. Readout technologies for directional WIMP Dark Matter detection

Author

J. A. Kadyk, T. N. Thorpe, A. Buonaura, H. Nishimura, Giuliana Galati, M. T. Hedges, Gabriela Druitt, Kentaro Miuchi, Ken'ichi Kuge, Hiroyuki Sekiya, M. Garcia-Sciveres, T. Hashimoto, L. Consiglio, H. Mirallas, Toru Tanimori, M. Tanaka, P. Monacelli, S. E. Vahsen, Javier Galan, Tetsuya Mizumoto, J. P. Lopez, T. Asada, G. De Lellis, A. Takada, I. G. Irastorza, O. Guillaudin, M. Ali Guler, M. Yoshimoto, A. B. Aleksandrov, Jerome Bouvier, T. Dafni, Maria Cristina Montesi, N. J. C. Spooner, F. Mayet, Philip Lewis, F.J. Iguaz, J. Lamblin, N. Di Marco, V. Gentile, T. Papevangelou, Ryosuke Taishaku, Adele Lauria, Natalia Guerrero, H. Tomita, Q. Riffard, J. P. Richer, Valeri Tioukov, S. Komura, Cosmin Deaconu, Y. Giomataris, Joseph D. Parker, Tatsuya Sawano, Daniel P. Snowden-Ifft, I. Jaegle, S. Cebrián, D. Loomba, Jocelyn Monroe, G. Bosson, Gianfranca De Rosa, A. Umemoto, E. Zayas, Taishi Katsuragawa, H. Kubo, Ihn Sik Seong, Nicola D'Ambrosio, Tatsuhiro Naka, P. Colas, J. Billard, F. Pupilli, E. R. Lee, Y. Mizumura, Koji Nakamura, O. Bourrion, Y. Yamaguchi, James Battat, D. Santos, E. Ferrer-Ribas, J. A. Garcia, Richard Eggleston, J. L. Harton, G. Luzón, M. Leyton, J. G. Garza, Atsuhiko Ochi, A. Di Crescenzo, K. Burdge, T. Descombes, A. Sugiyama, Takahiro Fusayasu, N. S. Phan, E. Baracchini, T. Ikeda, A. Takeda, Institut de Physique Nucléaire de Lyon (IPNL), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), MIMAC, Battat, J. B. R., Irastorza, I. G., Aleksandrov, A., Asada, T., Baracchini, E., Billard, J., Bosson, G., Bourrion, O., Bouvier, J., Buonaura, Annarita, Burdge, K., Cebrián, S., Colas, P., Consiglio, L., Dafni, T., D’Ambrosio, N., Deaconu, C., DE LELLIS, Giovanni, Descombes, T., DI CRESCENZO, Antonia, Di Marco, N., Druitt, G., Eggleston, R., Ferrer Ribas, E., Fusayasu, T., Galán, J., Galati, Giuliana, García, J. A., Garza, J. G., Gentile, V., Garcia Sciveres, M., Giomataris, Y., Guerrero, N., Guillaudin, O., Guler, A. M., Harton, J., Hashimoto, T., Hedges, M. T., Iguaz, F. J., Ikeda, T., Jaegle, I., Kadyk, J. A., Katsuragawa, T., Komura, S., Kubo, H., Kuge, K., Lamblin, J., Lauria, Adele, Lee, E. R., Lewis, P., Leyton, M., Loomba, D., Lopez, J. P., Luzón, G., Mayet, F., Mirallas, H., Miuchi, K., Mizumoto, T., Mizumura, Y., Monacelli, P., Monroe, J., Montesi, MARIA CRISTINA, Naka, T., Nakamura, K., Nishimura, H., Ochi, A., Papevangelou, T., Parker, J. D., Phan, N. S., Pupilli, F., Richer, J. P., Riffard, Q., Rosa, G., Santos, D., Sawano, T., Sekiya, H., Seong, I. S., Snowden Ifft, D. P., Spooner, N. J. C., Sugiyama, A., Taishaku, R., Takada, A., Takeda, A., Tanaka, M., Tanimori, T., Thorpe, T. N., Tioukov, V., Tomita, H., Umemoto, A., Vahsen, S. E., Yamaguchi, Y., Yoshimoto, M., Zayas, E., Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics - Instrumentation and Detectors, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics::Instrumentation and Detectors, Dark matter, General Physics and Astronomy, FOS: Physical sciences, 01 natural sciences, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), Recoil, Optics, WIMP, 0103 physical sciences, High spatial resolution, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, 010308 nuclear & particles physics, business.industry, Detector, Instrumentation and Detectors (physics.ins-det), Signature (logic), 3. Good health, business, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The measurement of the direction of WIMP-induced nuclear recoils is a compelling but technologically challenging strategy to provide an unambiguous signature of the detection of Galactic dark matter. Most directional detectors aim to reconstruct the dark-matter-induced nuclear recoil tracks, either in gas or solid targets. The main challenge with directional detection is the need for high spatial resolution over large volumes, which puts strong requirements on the readout technologies. In this paper we review the various detector readout technologies used by directional detectors. In particular, we summarize the challenges, advantages and drawbacks of each approach, and discuss future prospects for these technologies., Comment: 58 pages, 26 figures, accepted by Physics Reports

Published
2016
Full Text
View/download PDF

44. Search for low-mass WIMPs in a 0.6 kg day exposure of the DAMIC experiment at SNOLAB

Author

Aguilar Arevalo, A., Amidei, D., Bertou, X., Butner, M., Cancelo, G., Castañeda Vazquez, Alejandro, Cervantes Vergara, Brenda, Chavarria, A. E., Chavez, C., Mello Neto, J. R. T., D'Olivo, J. C., Estrada, J., Fernández Moroni, Guillermo, Gaior, R., Guardincerri, Y., Hernandez Torres, P., Izraelevitch, F., Kavner, A., Kilminster, B., Lawson, Ian, Letessier Selvon, A., Liao, J., Mello, V. B. B., Molina, J., Peña, J. R., Privitera, Paolo, Ramanathan, K., Sarkis, Y., Schwarz, T., Sengul, C., Settimo, M., Sofo Haro, M., Thomas, R., Tiffenger, J., Tiouchichine, E., Torres Machado, Diego, Trillaud, Frederic, You, X., Zhou, J., Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), DAMIC, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), and Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS )

Subjects
WIMP: direct detection, Physics - Instrumentation and Detectors, Cosmology and Nongalactic Astrophysics (astro-ph.CO), [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Ciencias Físicas, Dark matter, FOS: Physical sciences, S030DI1, 01 natural sciences, WIMP nucleon: elastic scattering, dark matter, High Energy Physics - Experiment, Nuclear physics, purl.org/becyt/ford/1 [https], High Energy Physics - Experiment (hep-ex), High Energy Physics - Phenomenology (hep-ph), WIMP, Ionization, 0103 physical sciences, Energy spectrum, ionization, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Electron equivalent, 010306 general physics, low-mass WIMPs, cross section: elastic scattering, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), CCD, Physics, 010308 nuclear & particles physics, Detector, silicon, CCDs, DAMIC, purl.org/becyt/ford/1.3 [https], Instrumentation and Detectors (physics.ins-det), Astronomía, High Energy Physics - Phenomenology, Underground laboratory, Astrophysics - Instrumentation and Methods for Astrophysics, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], energy spectrum: measured, CIENCIAS NATURALES Y EXACTAS, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present results of a dark matter search performed with a 0.6 kg day exposure of the DAMIC experiment at the SNOLAB underground laboratory. We measure the energy spectrum of ionization events in the bulk silicon of charge-coupled devices down to a signal of 60 eV electron equivalent. The data are consistent with radiogenic backgrounds, and constraints on the spin-independent WIMP-nucleon elastic-scattering cross section are accordingly placed. A region of parameter space relevant to the potential signal from the CDMS-II Si experiment is excluded using the same target for the first time. This result obtained with a limited exposure demonstrates the potential to explore the low-mass WIMP region (, 11 pages, 11 figures

Published
2016
Full Text
View/download PDF

45. The veto system of the DarkSide-50 experiment

Author

E. Shields, J. Yoo, Nicomede Pelliccia, A. G. Cocco, B. Reinhold, E. Pantic, C. Giganti, Laura Cadonati, Cécile Jollet, Fausto Ortica, Mariano Cadoni, Andrea Ianni, Sandra Zavatarelli, M. Carlini, E. Edkins, P. N. Singh, K. Fomenko, F. Budano, O. Smirnov, K. Biery, Yanchu Wang, M. D. Skorokhvatov, N. Rossi, L. Agostino, Henning O. Back, L. Grandi, Griffin Foster, H. Cao, S. Parmeggiano, B. R. Hackett, B. Baldin, S. Perasso, A. Zec, Paolo Musico, T. Miletic, A. Fan, D. A. Pugachev, E. V. Unzhakov, E. Segreto, J. Tatarowicz, Ivone F. M. Albuquerque, C. Savarese, A. K. Alton, S. Pordes, S. Walker, Hui Wang, L. Pagani, K. Arisaka, P. Trinchese, P. J. Mosteiro, E. V. Hungerford, S. Davini, A. Brigatti, M. Orsini, L. Crippa, G. Fiorillo, D. Sablone, C. J. Martoff, G. Bonfini, R. Saldanha, Michele Montuschi, A. Candela, S. Odrowski, P. D. Meyers, Thomas Alexander, Jingke Xu, S. Westerdale, G. Testera, D. A. Semenov, K. Pelczar, Cristiano Galbiati, Yanhui Ma, G. Di Pietro, Giovanni Covone, J. Wilhelmi, R. Milincic, M. De Deo, A. Nelson, M. Wada, M. D'Incecco, Stefano Maria Mari, A. S. Kubankin, R. Tartaglia, K. J. Keeter, Frank Calaprice, X. Xiang, Severino Angelo Maria Bussino, G. Koh, Anselmo Meregaglia, H. Qian, Y. Guardincerri, A. Sotnikov, A. Mandarano, S. Catalanotti, D. Franco, W. Zhong, B. J. Mount, Y. Suvorov, M. Gromov, S. Luitz, V. N. Muratova, V. V. Kobychev, A. S. Chepurnov, W. Sands, C. Zhu, P. Cavalcante, B. Bottino, M. E. Monzani, A. Devoto, F. Di Eusanio, C. Stanford, A. Pocar, Denis Korablev, Samuele Sangiorgio, Aldo Romani, J. Brodsky, P. Saggese, P. Agnes, S. D. Rountree, D. Montanari, M. Cadeddu, Paolo Lombardi, M. Lissia, A. Monte, A. V. Derbin, S. De Cecco, Chung-Yao Yang, L. Marini, M. Bossa, B. Rossi, Alan Watson, G. Zuzel, Gioacchino Ranucci, K. Herner, F. Gabriele, Jim Napolitano, K. Randle, A. Tonazzo, A. Vishneva, X. Li, C. L. Kendziora, Irina James, J. Maricic, G. Korga, F. Granato, I. N. Machulin, N. Canci, Marco Pallavicini, D. D'Angelo, Anton Empl, M. M. Wojcik, A. L. Renshaw, Aldo Ianni, A. M. Goretti, M. Cariello, A. Razeto, T. N. Johnson, R. B. Vogelaar, Min-Xin Guan, M. De Vincenzi, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), DarkSide, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS), Agnes, P., Agostino, L., Albuquerque, I. F. M., Alexander, T., Alton, A. K., Arisaka, K., Back, H. O., Baldin, B., Biery, K., Bonfini, G., Bossa, M., Bottino, B., Brigatti, A., Brodsky, J., Budano, F., Bussino, S., Cadeddu, M., Cadonati, L., Cadoni, M., Calaprice, F., Canci, N., Candela, A., Cao, H., Cariello, M., Carlini, M., Catalanotti, S., Cavalcante, P., Chepurnov, A., Cocco, A. G., Covone, G., Crippa, L., D'Angelo, D., D'Incecco, M., Davini, S., De Cecco, S., De Deo, M., De Vincenzi, M., Derbin, A., Devoto, A., Di Eusanio, F., Di Pietro, G., Edkins, E., Empl, A., Fan, A., Fiorillo, Giuliana, Fomenko, K., Foster, G., Franco, D., Gabriele, F., Galbiati, C., Giganti, C., Goretti, A. M., Granato, F., Grandi, L., Gromov, M., Guan, M., Guardincerri, Y., Hackett, B. R., Herner, K. R., Hungerford, E. V., Ianni, Aldo, Ianni, Andrea, James, I., Johnson, T., Jollet, C., Keeter, K., Kendziora, C. L., Kobychev, V., Koh, G., Korablev, D., Korga, G., Kubankin, A., Li, X., Lissia, M., Lombardi, P., Luitz, S., Ma, Y., Machulin, I. N., Mandarano, A., Mari, S. M., Maricic, J., Marini, L., Martoff, C. J., Meregaglia, A., Meyers, P. D., Miletic, T., Milincic, R., Montanari, D., Monte, A., Montuschi, M., Monzani, M. E., Mosteiro, P., Mount, B. J., Muratova, V. N., Musico, P., Napolitano, J., Nelson, A., Odrowski, S., Orsini, M., Ortica, F., Pagani, L., Pallavicini, M., Pantic, E., Parmeggiano, S., Pelczar, K., Pelliccia, N., Perasso, S., Pocar, A., Pordes, S., Pugachev, D. A., Qian, H., Randle, K., Ranucci, G., Razeto, A., Reinhold, B., Renshaw, A. L., Romani, A., Rossi, B., Rossi, N., Rountree, S. D., Sablone, D., Saggese, P., Saldanha, R., Sands, W., Sangiorgio, S., Savarese, C., Segreto, E., Semenov, D. A., Shields, E., Singh, P. N., Skorokhvatov, M. D., Smirnov, O., Sotnikov, A., Stanford, C., Suvorov, Y., Tartaglia, R., Tatarowicz, J., Testera, G., Tonazzo, A., Trinchese, P., Unzhakov, E. V., Vishneva, A., Vogelaar, R. B., Wada, M., Walker, S., Wang, H., Wang, Y., Watson, A. W., Westerdale, S., Wilhelmi, J., Wojcik, M. M., Xiang, X., Xu, J., Yang, C., Yoo, J., Zavatarelli, S., Zec, A., Zhong, W., Zhu, C., Zuzel, G., AstroParticule et Cosmologie ( APC - UMR 7164 ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Observatoire de Paris-Université Paris Diderot - Paris 7 ( UPD7 ) -Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ), Laboratoire de Physique Nucléaire et de Hautes Énergies ( LPNHE ), Université Pierre et Marie Curie - Paris 6 ( UPMC ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Paris Diderot - Paris 7 ( UPD7 ) -Centre National de la Recherche Scientifique ( CNRS ), Institut Pluridisciplinaire Hubert Curien ( IPHC ), Centre National de la Recherche Scientifique ( CNRS ) -Université de Strasbourg ( UNISTRA ), Bussino, Severino Angelo Maria, DE VINCENZI, Mario, Fiorillo, G., James, Irina, Mari, Stefano Maria, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), ANR-10-LABX-0023,UnivEarthS,Earth - Planets - Universe: observation, modeling, transfer(2010), and ANR-11-IDEX-0005,USPC,Université Sorbonne Paris Cité(2011)

Subjects
fast neutrons), Physics - Instrumentation and Detectors, axions, gas and liquid scintillators), Cherenkov detector, Cherenkov and transition radiation, Physics::Instrumentation and Detectors, Cherenkov counter: water, Nuclear Theory, scintillation counter: liquid, FOS: Physical sciences, Scintillator, 01 natural sciences, Particle detector, High Energy Physics - Experiment, law.invention, thermal, Dark Matter detectors (WIMPs, axions, etc.), Nuclear physics, High Energy Physics - Experiment (hep-ex), WIMP, [ PHYS.HEXP ] Physics [physics]/High Energy Physics - Experiment [hep-ex], law, etc.), 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Neutron detection, Neutron, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010306 general physics, Nuclear Experiment, [ PHYS.PHYS.PHYS-INS-DET ] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation, Dark Matter detectors (WIMPs, Mathematical Physics, Event reconstruction, nucleus: recoil, Physics, 010308 nuclear & particles physics, Detector, Instrumentation and Detectors (physics.ins-det), Scintillators, scintillation and light emission processes (solid, gas and liquid scintillators), Neutron detectors (cold, thermal, fast neutrons), Neutron detectors (cold, scintillation and light emission processes (solid, Scintillators, High Energy Physics::Experiment, performance
Abstract

International audience; Nuclear recoil events produced by neutron scatters form one of the most important classes of background in WIMP direct detection experiments, as they may produce nuclear recoils that look exactly like WIMP interactions. In DarkSide-50, we both actively suppress and measure the rate of neutron-induced background events using our neutron veto, composed of a boron-loaded liquid scintillator detector within a water Cherenkov detector. This paper is devoted to the description of the neutron veto system of DarkSide-50, including the detector structure, the fundamentals of event reconstruction and data analysis, and basic performance parameters.

Published
2016
Full Text
View/download PDF

46. Constraints on low-mass WIMPs from the EDELWEISS-III dark matter search

Author

EDELWEISS Collaboration, Armengaud, E., Arnaud, Q., Augier, C., Benoît, A., Bergé, L., Bergmann, T., Billard, J., Blümer, J., de Boissière, T., Bres, G., Broniatowski, A., Brudanin, V., Camus, P., Cazes, A., Chapellier, M., Charlieux, F., Dumoulin, L., Eitel, K., Filosofov, D., Foerster, N., Fourches, N., Garde, G., Gascon, J., Gerbier, G., Giuliani, A., Grollier, M., Gros, M., Hehn, L., Hervé, S., Heuermann, G., Humbert, V., De Jésus, M., Jin, Y., Jokisch, S., Juillard, A., Kéfélian, C., Kleifges, M., Kozlov, V., Kraus, H., Kudryavtsev, V. A., Le-Sueur, H., Lin, J., Mancuso, M., Marnieros, S., Menshikov, A., Navick, X. -F., Nones, C., Olivieri, E., Pari, P., Paul, B., Piro, M. -C., Poda, D. V., Queguiner, E., Robinson, M., Rodenas, H., Rozov, S., Sanglard, V., Schmidt, B., Scorza, S., Siebenborn, B., Tcherniakhovski, D., Vagneron, L., Weber, M., Yakushev, E., Zhang, X., Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Matière noire (MANOIR), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Centre de Sciences Nucléaires et de Sciences de la Matière (CSNSM), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Electronique (ElecLab), Cryogénie (Cryo), Laboratoire de photonique et de nanostructures (LPN), Centre National de la Recherche Scientifique (CNRS), Institut Rayonnement Matière de Saclay (IRAMIS), EDELWEISS, Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Hélium : du fondamental aux applications (NEEL - HELFA), Electronique (NEEL - ElecLab), and Cryogénie (NEEL - Cryo)

Subjects
Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Physics - Instrumentation and Detectors, Physics::Instrumentation and Detectors, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, EDELWEISS, 01 natural sciences, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), WIMP, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], 010306 general physics, Elastic scattering, Physics, Range (particle radiation), 010308 nuclear & particles physics, Scattering, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Instrumentation and Detectors (physics.ins-det), Weakly interacting massive particles, High Energy Physics::Experiment, Low Mass, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the results of a search for elastic scattering from galactic dark matter in the form of Weakly Interacting Massive Particles (WIMPs) in the 4-30 GeV/$c^2$ mass range. We make use of a 582 kg-day fiducial exposure from an array of 800 g Germanium bolometers equipped with a set of interleaved electrodes with full surface coverage. We searched specifically for $\sim 2.5-20$ keV nuclear recoils inside the detector fiducial volume. As an illustration the number of observed events in the search for 5 (resp. 20) GeV/$c^2$ WIMPs are 9 (resp. 4), compared to an expected background of 6.1 (resp. 1.4). A 90% CL limit of $4.3\times 10^{-40}$ cm$^2$ (resp. $9.4\times 10^{-44}$ cm$^2$) is set on the spin-independent WIMP-nucleon scattering cross-section for 5 (resp. 20) GeV/$c^2$ WIMPs. This result represents a 41-fold improvement with respect to the previous EDELWEISS-II low-mass WIMP search for 7 GeV/$c^2$ WIMPs. The derived constraint is in tension with hints of WIMP signals from some recent experiments, thus confirming results obtained with different detection techniques., Matches published version

Published
2016
Full Text
View/download PDF

47. High-energy gamma-ray sources of cosmological origin

Author

Pierre Brun, Johann Cohen-Tanugi, Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Laboratoire Univers et Particules de Montpellier (LUPM), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
WIMP, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Scalar field dark matter, Energy Engineering and Power Technology, Primordial black holes, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Physics and Astronomy(all), 01 natural sciences, Baryonic dark matter, 0103 physical sciences, Warm dark matter, constituent, Rayons gamma, 010303 astronomy & astrophysics, Light dark matter, Trous noirs primordiaux, Physics, 010308 nuclear & particles physics, Hot dark matter, Gamma rays, General Engineering, Astronomy, dark matter: annihilation, Matière noire, gamma ray: UHE, gamma ray, Weakly interacting massive particles, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Dark fluid
Abstract

International audience; The current generation of instruments in gamma-ray astrophysics launched a new era in the search for a dark matter signal in the high-energy sky. Such searches are said indirect, in the sense that the presence of a dark matter particle is inferred from the detection of products of its pair-annihilation or decay. They have recently started to probe the natural domain of existence for weakly interacting massive particles (WIMPs), the favorite dark matter candidates today. In this article, we review the basic framework for indirect searches and we present a status of current limits obtained with gamma-ray observations. We also devote a section to another possible class of cosmological gamma-ray sources, primordial black holes, also considered as a potential constituent of dark matter.

Published
2016
Full Text
View/download PDF

48. Uncertainties on propagation parameters: impact on the interpretation of the positron fraction

Author

S. Aupetit, Geneviève Bélanger, Vivian Poulin, S. Rosier-Lees, Mathieu Boudaud, Li Tao, Manuela Vecchi, Pierre Salati, C. Goy, V. Poireau, Antje Putze, Sami Caroff, Yoann Génolini, Laboratoire d'Annecy-le-Vieux de Physique Théorique (LAPTH), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Centre National de la Recherche Scientifique (CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National d’Études Spatiales [Paris] (CNES)

Subjects
WIMP, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, anomaly, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, positron: flux, 01 natural sciences, dark matter, Positron, Pulsar, 0103 physical sciences, propagation, 010303 astronomy & astrophysics, pulsar, Mont Blanc, Physics, Mathieu, 010308 nuclear & particles physics, Galaxy, Interstellar medium, cosmic radiation: primary, Weakly interacting massive particles, High Energy Physics::Experiment, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], signature, positron: cosmic radiation
Abstract

International audience; The positron fraction in cosmic rays has recently been measured with improved accuracy up to 500 GeV, and it was found to be a steadily increasing function of energy above 10 GeV. This behaviour contrasts with standard astrophysical mechanisms, in which positrons are secondary particles, produced in the interactions of primary cosmic rays during their propagation in the interstellar medium. The observed anomaly in the positron fraction triggered a lot of excitement, as it could be interpreted as an indirect signature of the presence of dark matter species in the Galaxy, the so-called weakly interacting massive particles (WIMPs). Alternatively, it could be produced by nearby sources, such as pulsars. These hypotheses are probed in [1], in light of the latest AMS-02 positron fraction measurements. The cosmic ray positron transport in the Galaxy is described using a semi-analytic two-zone model. For consistency, the secondary and primary components of the positron flux are calculated together with the same propagation model. We show that the results inferred for both hypotheses crucially depend on the propagation parameters, estimated with the Boron-to-Carbon ratio. Their uncertainties turn out to be very significant, and overshadow even the statical errors from the positron data.

Published
2015
Full Text
View/download PDF

49. Prospects for Indirect Dark Matter Searches with the Cherenkov Telescope Array (CTA)

Author

Trygve Buanes, Csaba Balázs, Emmanuel Moulin, Christian Farnier, Mark I. Wilkinson, Gabrijela Zaharijas, Miguel A. Sánchez-Conde, Javier Rico, A. Morselli, Torsten Bringmann, M. Hayashida, Matthew Wood, Michael Daniel, Kazunori Kohri, Takashi Saito, N. Mirabal, Jennifer Gaskins, Michele Doro, Hannes Zechlin, Germán A. Gómez-Vargas, V. Lefranc, Mattia Fornasa, John Carr, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département de Physique des Particules (ex SPP) (DPhP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, GRAPPA (ITFA, IoP, FNWI), Faculty of Science, IoP (FNWI), and Département de Physique des Particules (ex SPP) (DPP)

Subjects
astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Milky Way, Astrophysics::High Energy Astrophysical Phenomena, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Dark matter, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astronomy, Segue, Astrophysics::Cosmology and Extragalactic Astrophysics, Cherenkov Telescope Array, 01 natural sciences, Galactic halo, WIMP, Weakly interacting massive particles, 0103 physical sciences, 010306 general physics, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, Dwarf galaxy
Abstract

The Cherenkov Telescope Array (CTA) will have a unique chance of discovery for a large range of masses in Weakly Interacting Massive Particles models of dark matter. The principal target for dark matter searches with CTA is the centre of the Galactic Halo. The best strategy is to perform CTA observations within a few degrees of the Galactic Centre, with the Galactic Centre itself and the most intense diffuse emission regions removed from the analysis. Assuming a cuspy dark matter density profile for the Milky Way, 500 hours of observations in this region provide sensitivities to and below the thermal cross-section of dark matter annihilations, for masses between a few hundred GeV and a few tens of TeV; therefore CTA will have a significant chance of discovery in some models. Since the dark matter density in the Milky Way is far from certain in the inner kpc region, other targets are also proposed for observation, like ultra-faint dwarf galaxies such as Segue 1 with 100 hours per year proposed. Beyond these two observational targets, further alternatives, such as Galactic dark clumps, will be considered closer to the actual date of CTA operations. Sensitivity predictions for dark matter searches are given on the various targets taking into account the latest instrument response functions expected for CTA together with a discussion on the systematic uncertainties from the backgrounds., In Proceedings of the 34th International Cosmic Ray Conference (ICRC2015), The Hague, The Netherlands. All CTA contributions at arXiv:1508.05894

Published
2015

50. Recent results from the EDELWEISS-III WIMP search experiment

Author

Antoine Cazes, Institut de Physique Nucléaire de Lyon (IPNL), Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Matière noire (MANOIR), Institut de Physique des 2 Infinis de Lyon (IP2I Lyon), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), EDELWEISS, and Flores, Sylvie

Subjects
Nuclear physics, Physics, WIMP, [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Dark matter, European Underground Rare Event Calorimeter Array, Underground laboratory, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], EDELWEISS, Mass analysis, 7. Clean energy
Abstract

International audience; The EDELWEISS experiment is dedicated to the direct detection of Dark Matter. The current setup (EDELWEISS-III) aims at exploring a spin-independent WIMP-nucleon cross section down to the 109 pb range, and extend the coverage for masses below 20 GeV. Since July 2014, the experiment is taking data with 24 state-of-the-art cryogenic FID800 Germanium detectors installed in the radio pure environment of the Modane underground laboratory - the deepest of its kind in Europe. These proceedings present the current status of the EDELWEISS-III experiment andshow first preliminary results highlighting our new low WIMP mass analysis and the current background budget.

Published
2015

Catalog

Books, media, physical & digital resources
See catalog results