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9 results on '"boson: dark matter"'

1. Adiabatically compressed wave dark matter halo and intermediate-mass ratio inspirals

Author

Hyungjin Kim, Alessandro Lenoci, Isak Stomberg, and Xiao Xue

Subjects
geometry, approximation: semiclassical, FOS: Physical sciences, mass [black hole], General Relativity and Quantum Cosmology (gr-qc), angular momentum, General Relativity and Quantum Cosmology, mass, density, High Energy Physics - Phenomenology (hep-ph), dark matter: halo, approximation, semiclassical, quantum chromodynamics, black hole, mass, ddc:530, black hole: Schwarzschild, capture, mass: density, dark matter, halo, LISA, boson: dark matter, Hamiltonian formalism, Schwarzschild [black hole], gravitational radiation, halo [dark matter], density [mass], black hole: mass, suppression, Navarro-Frenk-White profile, Astrophysics - Astrophysics of Galaxies, gravitational radiation detector, High Energy Physics - Phenomenology, semiclassical [approximation], axion, Astrophysics of Galaxies (astro-ph.GA), adiabatic, Kerr, dark matter [boson], galaxy, boson, dark matter, soliton
Abstract

Physical review / D 107(8), 083005 (2023). doi:10.1103/PhysRevD.107.083005, The adiabatic growth of a central massive black hole could compress the surrounding dark matter halo, leading to a steeper profile of the dark matter halo. This phenomenon is called adiabatic compression. We investigate the adiabatic compression of wave dark matter—a light bosonic dark matter candidate with its mass smaller than a few eV. Using the adiabatic theorem, we show that the adiabatic compression leads to a much denser wave dark matter halo similar to the particle dark matter halo in the semiclassical limit. The compressed wave halo differs from that of the particle halo near the center where the semiclassical approximation breaks down, and the central profile depends on dark matter and the central black hole mass as they determine whether the soliton and low angular momentum modes can survive over the astrophysical timescale without being absorbed by the black hole. Such a compressed profile has several astrophysical implications. As one example, we study the gravitational waves from the inspiral between a central intermediate-mass black hole and a compact solar-mass object within the wave dark matter halo. Due to the enhanced mass density, the compressed wave dark matter halo exerts stronger dynamical friction on the orbiting object, leading to the dephasing of the gravitational waves. The pattern of dephasing is distinctive from that of inspirals in the particle dark matter halo because of the difference in density profile and because of the relatively suppressed dynamical friction force, originating from the wave nature of dark matter. We investigate the prospects of future gravitational wave detectors, such as the Laser Interferometer Space Antenna, and identify physics scenarios where the wave dark matter halo can be reconstructed from gravitational wave observations., Published by Inst., Woodbury, NY

Published
2023
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2. Search for New Physics in Electronic Recoil Data from XENONnT

Author

XENON Collaboration, Aprile, E., Abe, K., Agostini, F., Ahmed Maouloud, S., Althueser, L., Andrieu, B., Angelino, E., Angevaare, J. R., Antochi, V. C., Antón Martin, D., Arneodo, F., Baudis, L., Baxter, A. L., Bellagamba, L., Biondi, R., Bismark, A., Brown, A., Bruenner, S., Bruno, G., Budnik, R., Bui, T. K., Cai, C., Capelli, C., Cardoso, J. M. R., Cichon, D., Clark, M., Colijn, A. P., Conrad, J., Cuenca-García, J. J., Cussonneau, J. P., D’Andrea, V., Decowski, M. P., Di Gangi, P., Di Pede, S., Di Giovanni, A., Di Stefano, R., Diglio, S., Eitel, K., Elykov, A., Farrell, S., Ferella, A. D., Ferrari, C., Fischer, H., Fulgione, W., Gaemers, P., Gaior, R., Gallo Rosso, A., Galloway, M., Gao, F., Gardner, R., Glade-Beucke, R., Grandi, L., Grigat, J., Guida, M., Hammann, R., Higuera, A., Hils, C., Hoetzsch, L., Howlett, J., Iacovacci, M., Itow, Y., Jakob, J., Joerg, F., Joy, A., Kato, N., Kara, M., Kavrigin, P., Kazama, S., Kobayashi, M., Koltman, G., Kopec, A., Kuger, F., Landsman, H., Lang, R. F., Levinson, L., Li, I., Li, S., Liang, S., Lindemann, S., Lindner, M., Liu, K., Loizeau, J., Lombardi, F., Long, J., Lopes, J. A. M., Ma, Y., Macolino, C., Mahlstedt, J., Mancuso, A., Manenti, L., Marignetti, F., Marrodán Undagoitia, T., Martens, K., Masbou, J., Masson, D., Masson, E., Mastroianni, S., Messina, M., Miuchi, K., Mizukoshi, K., Molinario, A., Moriyama, S., Morå, K., Mosbacher, Y., Murra, M., Müller, J., Ni, K., Oberlack, U., Paetsch, B., Palacio, J., Paschos, P., Peres, R., Peters, C., Pienaar, J., Pierre, M., Pizzella, V., Plante, G., Qi, J., Qin, J., Ramírez García, D., Reichard, S., Rocchetti, A., Rupp, N., Sanchez, L., Dos Santos, J. M. F., Sarnoff, I., Sartorelli, G., Schreiner, J., Schulte, D., Schulte, P., Schulze Eißing, H., Schumann, M., Scotto Lavina, L., Selvi, M., Semeria, F., Shagin, P., Shi, S., Shockley, E., Silva, M., Simgen, H., Stephen, J., Takeda, A., Tan, P.-L., Terliuk, A., Thers, D., Toschi, F., Trinchero, G., Tunnell, C., Tönnies, F., Valerius, K., Volta, G., Wei, Y., Weinheimer, C., Weiss, M., Wenz, D., Wittweg, C., Wolf, T., Xu, D., Xu, Z., Yamashita, M., Yang, L., Ye, J., Yuan, L., Zavattini, G., Zhong, M., Zhu, T., IoP (FNWI), XENON (IHEF, IoP, FNWI), Astroparticle Physics (IHEF, IoP, FNWI), Aprile, E, Abe, K, Agostini, F, Ahmed Maouloud, S, Althueser, L, Andrieu, B, Angelino, E, Angevaare, J R, Antochi, V C, Antón Martin, D, Arneodo, F, Baudis, L, Baxter, A L, Bellagamba, L, Biondi, R, Bismark, A, Brown, A, Bruenner, S, Bruno, G, Budnik, R, Bui, T K, Cai, C, Capelli, C, Cardoso, J M R, Cichon, D, Clark, M, Colijn, A P, Conrad, J, Cuenca-García, J J, Cussonneau, J P, D'Andrea, V, Decowski, M P, Di Gangi, P, Di Pede, S, Di Giovanni, A, Di Stefano, R, Diglio, S, Eitel, K, Elykov, A, Farrell, S, Ferella, A D, Ferrari, C, Fischer, H, Fulgione, W, Gaemers, P, Gaior, R, Gallo Rosso, A, Galloway, M, Gao, F, Gardner, R, Glade-Beucke, R, Grandi, L, Grigat, J, Guida, M, Hammann, R, Higuera, A, Hils, C, Hoetzsch, L, Howlett, J, Iacovacci, M, Itow, Y, Jakob, J, Joerg, F, Joy, A, Kato, N, Kara, M, Kavrigin, P, Kazama, S, Kobayashi, M, Koltman, G, Kopec, A, Kuger, F, Landsman, H, Lang, R F, Levinson, L, Li, I, Li, S, Liang, S, Lindemann, S, Lindner, M, Liu, K, Loizeau, J, Lombardi, F, Long, J, Lopes, J A M, Ma, Y, Macolino, C, Mahlstedt, J, Mancuso, A, Manenti, L, Marignetti, F, Marrodán Undagoitia, T, Martens, K, Masbou, J, Masson, D, Masson, E, Mastroianni, S, Messina, M, Miuchi, K, Mizukoshi, K, Molinario, A, Moriyama, S, Morå, K, Mosbacher, Y, Murra, M, Müller, J, Ni, K, Oberlack, U, Paetsch, B, Palacio, J, Paschos, P, Peres, R, Peters, C, Pienaar, J, Pierre, M, Pizzella, V, Plante, G, Qi, J, Qin, J, Ramírez García, D, Reichard, S, Rocchetti, A, Rupp, N, Sanchez, L, Dos Santos, J M F, Sarnoff, I, Sartorelli, G, Schreiner, J, Schulte, D, Schulte, P, Schulze Eißing, H, Schumann, M, Scotto Lavina, L, Selvi, M, Semeria, F, Shagin, P, Shi, S, Shockley, E, Silva, M, Simgen, H, Stephen, J, Takeda, A, Tan, P-L, Terliuk, A, Thers, D, Toschi, F, Trinchero, G, Tunnell, C, Tönnies, F, Valerius, K, Volta, G, Wei, Y, Weinheimer, C, Weiss, M, Wenz, D, Wittweg, C, Wolf, T, Xu, D, Xu, Z, Yamashita, M, Yang, L, Ye, J, Yuan, L, Zavattini, G, Zhong, M, Zhu, T, and HEP, INSPIRE

Subjects
xenon: target, neutrino: solar, [PHYS.HEXP] Physics [physics]/High Energy Physics - Experiment [hep-ex], WIMP, electronic recoil, General Physics and Astronomy, FOS: Physical sciences, coupling constant: upper limit, dark matter: direct detection, WIMP: dark matter, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), recoil, Dark Matter, ddc:530, coupling: (axion 2electron), Xenon nT, xenon: liquid, photon: hidden sector, boson: dark matter, axion: dark matter, background, new physics: search for, Physics, dark matter: detector, neutrino: magnetic moment, Xenon nT, Dark Matter, WIMP, electronic recoil, coupling: (axion 2photon), axion: solar, experimental results
Abstract

We report on a blinded analysis of low-energy electronic-recoil data from the first science run of the XENONnT dark matter experiment. Novel subsystems and the increased 5.9 tonne liquid xenon target reduced the background in the (1, 30) keV search region to $(15.8 \pm 1.3)$ events/(tonne$\times$year$\times$keV), the lowest ever achieved in a dark matter detector and $\sim$5 times lower than in XENON1T. With an exposure of 1.16 tonne-years, we observe no excess above background and set stringent new limits on solar axions, an enhanced neutrino magnetic moment, and bosonic dark matter., Comment: 10 pages, 6 figures. Data points are available in https://zenodo.org/record/7311940

Published
2022

3. Gravitational focusing of wave dark matter

Author

Hyungjin Kim and Alessandro Lenoci

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), boson: dark matter, density [dark matter], FOS: Physical sciences, halo [dark matter], Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, solar system, gravitation: potential, Astrophysics - Astrophysics of Galaxies, High Energy Physics - Phenomenology, modulation, High Energy Physics - Phenomenology (hep-ph), dark matter: halo, velocity: dispersion, Astrophysics of Galaxies (astro-ph.GA), dispersion [velocity], potential [gravitation], ddc:530, dark matter [boson], structure, capture, signature, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Physical review / D 105(6), 063032 (2022). doi:10.1103/PhysRevD.105.063032, A massive astrophysical object deforms the local distribution of dark matter, resulting in a local overdensity of dark matter. This phenomenon is often referred to as gravitational focusing. In the solar system, the gravitational focusing due to the Sun induces modulations of dark matter signals on terrestrial experiments. We consider the gravitational focusing of light bosonic dark matter with a mass of less than about 10 eV. The wave nature of such dark matter candidates leads to unique signatures in the local overdensity and in the spectrum, both of which can be experimentally relevant. We provide a formalism that captures both the gravitational focusing and the stochasticity of wave dark matter, paying particular attention to the similarity and difference to particle dark matter. Distinctive patterns in the density contrast and spectrum are observed when the de Broglie wavelength of dark matter becomes comparable or less than the size of the system and/or when the velocity dispersion of dark matter is sufficiently small. While gravitational focusing effects generally remain at a few percent level for a relaxed halo dark matter component, they could be much larger for dark matter substructures. With a few well-motivated dark matter substructures, we investigate how each substructure responds to the gravitational potential of the Sun. The limit at which wave dark matter behaves similar to particle dark matter is also discussed., Published by Inst., Melville, NY

Published
2022
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4. Gravitational Focusing of Wave Dark Matter

Author

Kim, Hyungjin and Lenoci, Alessandro

Subjects
modulation, boson: dark matter, dark matter: halo, velocity: dispersion, Astrophysics::Cosmology and Extragalactic Astrophysics, structure, dark matter: density, solar system, gravitation: potential, capture, signature
Abstract

A massive astrophysical object deforms a local distribution of dark matter, resulting in a local overdensity of dark matter. This phenomenon is often referred to as gravitational focusing. In the solar system, the gravitational focusing due to the Sun induces modulations of dark matter signals on terrestrial experiments. We consider the gravitational focusing of a light bosonic dark matter with a mass of less than about 10 eV. The wave nature of such dark matter candidates leads to unique signatures both in the local overdensity and in the spectrum, both of which can be experimentally relevant. We provide a formalism that captures both the gravitational focusing and the stochasticity of wave dark matter, paying particular attention to the similarity and difference to particle dark matter. Distinctive patterns in the density contrast and spectrum are observed when the de Broglie wavelength of dark matter becomes comparable or less than the size of the system and/or when the velocity dispersion of dark matter is sufficiently small. While gravitational focusing effects generally remain at a few percent level for a relaxed halo dark matter component, they could be much larger for dark matter substructures. With a few well-motivated dark matter substructures, we investigate how each substructure responds to the gravitational potential of the Sun. The limit at which wave dark matter behaves similar to particle dark matter is also discussed.

Published
2021
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5. Excess electronic recoil events in XENON1T

Author

A. Manfredini, L. Scotto Lavina, A. D. Ferella, Hongwei Wang, L. Levinson, Ch. Weinheimer, D. Masson, J. Pienaar, Qing Lin, Auke-Pieter Colijn, Laura Baudis, E. Angelino, João Cardoso, T. Zhu, J. R. Angevaare, F. Gao, Jelle Aalbers, P. Gaemers, F. Toschi, A. Di Giovanni, R. Di Stefano, W. Fulgione, Gabriella Sartorelli, M. Clark, Kentaro Miuchi, C. Therreau, Yuehuan Wei, F. D. Amaro, H. Landsman, A. Depoian, Guillaume Plante, J. Ye, M. Selvi, Joern Mahlstedt, M. L. Benabderrahmane, Ethan Brown, D. Wenz, J. Qin, M. Alfonsi, R. Peres, D. Schulte, J. Long, J. P. Zopounidis, S. Moriyama, Boris Bauermeister, G. Eurin, R. Gaior, C. Hasterok, Ran Budnik, J.M.F. dos Santos, A. Kopec, Xavier Mougeot, Yoshitaka Itow, Michelle Galloway, C. Macolino, F. Agostini, N. Kato, J. Palacio, E. Shockley, A. Mancuso, M. Weiss, S. Reichard, Yanxi Zhang, L. Grandi, J. Schreiner, Sebastian Lindemann, M. P. Decowski, Shingo Kazama, Laura Manenti, G. Koltman, Marc Schumann, Manfred Lindner, R. F. Lang, E. López Fune, N. Rupp, P. Di Gangi, Guido Zavattini, F. Lombardi, Jan Conrad, S. Mastroianni, Uwe Oberlack, C. Hils, Masanori Kobayashi, F. Marignetti, S. Bruenner, Kaixuan Ni, K. Mizukoshi, F. Semeria, D. Ramírez García, V. Pizzella, N. Šarčević, Giacomo Bruno, T. Berger, Sara Diglio, A. Takeda, Masaki Yamashita, Y. Mosbacher, J. Howlett, Gian Carlo Trinchero, H. Qiu, A. Elykov, Lorenzo Bellagamba, F. Arneodo, Katsuki Hiraide, J. Naganoma, A. Rocchetti, D. Barge, B. Cimmino, G. Volta, M. Murra, V. C. Antochi, C. Capelli, P. Shagin, L. Hoetzsch, K. Morå, Julien Masbou, H. Simgen, Dominique Thers, C. Wittweg, K. Odgers, D. Coderre, Manuel Gameiro da Silva, A. Molinario, M. Scheibelhut, April S. Brown, Jean-Pierre Cussonneau, Z. Xu, D. Cichon, Bart Pelssers, K. Martens, M. Messina, Elena Aprile, F. Joerg, C. Tunnell, M. Vargas, T. Marrodán Undagoitia, J. A. M. Lopes, M. Iacovacci, L. Althueser, Columbia University [New York], Oskar Klein Centre [Stockholm], Stockholm University, University of Bologna, Johannes Gutenberg - Universität Mainz (JGU), Westfälische Wilhelms-Universität Münster (WWU), University of Coimbra [Portugal] (UC), Università degli studi di Torino (UNITO), University of Amsterdam [Amsterdam] (UvA), New York University [Abu Dhabi], NYU System (NYU), Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Althueser, L., Amaro, F. D., Antochi, V. C., Angelino, E., Angevaare, J. R., Arneodo, F., Barge, D., Baudis, L., Bauermeister, B., Bellagamba, L., Benabderrahmane, M. L., Berger, T., 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., Galloway, M., Gao, F., Grandi, L., Hasterok, C., Hils, C., Hiraide, K., Hoetzsch, L., 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., Long, J., Lopes, J. A. M., López Fune, E., Macolino, C., Mahlstedt, J., Mancuso, A., Manenti, L., Manfredini, A., Marignetti, F., Marrodán Undagoitia, T., Martens, K., Masbou, J., Masson, D., Mastroianni, S., Messina, M., Miuchi, K., Mizukoshi, 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., 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., Wang, H., Wei, Y., Weinheimer, C., Weiss, M., Wenz, D., Wittweg, C., Xu, Z., Yamashita, M., Ye, J., Zavattini, G., Zhang, Y., Zhu, T., Zopounidis, J. P., Mougeot, X., 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)-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), 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), Laboratoire d'Intégration des Systèmes et des Technologies (LIST), Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, XENON, University of Bologna/Università di Bologna, Istituto Nazionale di Fisica Nucleare, Sezione di Bologna (INFN, Sezione di Bologna), Istituto Nazionale di Fisica Nucleare (INFN), Johannes Gutenberg - Universität Mainz = Johannes Gutenberg University (JGU), Westfälische Wilhelms-Universität Münster = University of Münster (WWU), Università degli studi di Torino = University of Turin (UNITO), Istituto Nazionale di Fisica Nucleare, Sezione di Torino (INFN, Sezione di Torino), National Institute for Subatomic Physics [Amsterdam] (NIKHEF), Universität Zürich [Zürich] = University of Zurich (UZH), Rensselaer Polytechnic Institute (RPI), Weizmann Institute of Science [Rehovot, Israël], Max-Planck-Institut für Kernphysik (MPIK), Max-Planck-Gesellschaft, Istituto Nazionale di Fisica Nucleare, Sezione di Napoli (INFN, Sezione di Napoli), Purdue University [West Lafayette], Albert-Ludwigs-Universität Freiburg, Université de Nantes - UFR des Sciences et des Techniques (UN UFR ST), 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 (IMT Atlantique), University of L'Aquila [Italy] (UNIVAQ), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Kavli Institute for Cosmological Physics [Chicago] (KICP), University of Chicago, The University of Tokyo (UTokyo), Nagoya University, Konan University [Kobe, Japan], University of California [San Diego] (UC San Diego), University of California (UC), Rice University [Houston], University of California [Los Angeles] (UCLA), Laboratoire National Henri Becquerel (LNHB), Département Métrologie Instrumentation & Information (DM2I), Laboratoire d'Intégration des Systèmes et des Technologies (LIST (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Direction de Recherche Technologique (CEA) (DRT (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Laboratoire d'Intégration des Systèmes et des Technologies (LIST (CEA)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Département d'instrumentation Numérique (DIN (CEA-LIST)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA), XENON collaboration, 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), University of California, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Laboratoire d'Intégration des Systèmes et des Technologies (LIST), IoP (FNWI), and XENON (IHEF, IoP, FNWI)

Subjects
xenon: target, axions, solar axion, magnetic moment, dimension: 3, neutrino: solar, Physics beyond the Standard Model, Solar neutrino, dark matter: direct detection, 01 natural sciences, 7. Clean energy, High Energy Physics - Experiment, Dark matter, direct detection, axion, High Energy Physics - Experiment (hep-ex), neutrino, XENON, High Energy Physics - Phenomenology (hep-ph), background: low, Recoil, electron: recoil, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], beta-rays, Particle Physics Experiments, coupling: (axion 2electron), multi-purpose particle detector, nuclear instrumentation, ComputingMilieux_MISCELLANEOUS, instrumentation, Physics, xenon: liquid, boson: dark matter, axion 2nucleon, tritium, new physics: search for, semileptonic decay, boson: vector, tension, neutrino: magnetic moment, High Energy Physics - Phenomenology, axion 2photon, low background, boson, Neutrino, ionizing radiation, Nucleon, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), dark matter detector, electronic recoil, Electron capture, XENON1T detector, Dark matter, low-energy electronic recoil data, FOS: Physical sciences, [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], dark matter, NO, Nuclear physics, PE2_2, PE2_1, tritium: semileptonic decay, 0103 physical sciences, solar axion model, surface, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], axion: coupling, PE2_4, 010306 general physics, pseudoscalar, Axion, dark matter: vector, dark matter, XENON1T detector, electronic recoil, solar neutrino, detector, Dark Matter, Axions, Beta Decay, Liquid Xenon, TPC, 010308 nuclear & particles physics, axion 2electron, coupling: (axion 2nucleon), dark matter: detector, model: axion, Gran Sasso, metrology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], axion, stellar constraints, coupling: (axion 2photon), High Energy Physics::Experiment, particle dark matter, direct detection, beta decay, axion: solar, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], experimental results
Abstract

We report results from searches for new physics with low-energy electronic recoil data recorded with the XENON1T detector. With an exposure of 0.65 t-y and an unprecedentedly low background rate of $76\pm2$ events/(t y keV) between 1 and 30 keV, the data enables sensitive searches for solar axions, an enhanced neutrino magnetic moment, and bosonic dark matter. An excess over known backgrounds is observed at low energies and most prominent between 2 and 3 keV. The solar axion model has a 3.4$\sigma$ significance, and a 3D 90% confidence surface is reported for axion couplings to electrons, photons, and nucleons. This surface is inscribed in the cuboid defined by $g_{ae}, Comment: 26 pages, 15 figures. v2 added Ar37 background discussion and best-fit mass of bosonic dark matter, v3 updated Ar37 discussion, tritium estimation, and solar axion energy spectrum. Data in Fig. 2, 4, and 15, including unbinned energy points in Fig. 4, are available in 10.5281/zenodo.4088778

Published
2020
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6. Core mass-halo mass relation of bosonic and fermionic dark matter halos harboring a supermassive black hole

Author

Pierre-Henri Chavanis, Laboratoire de Physique Théorique (LPT), Institut de Recherche sur les Systèmes Atomiques et Moléculaires Complexes (IRSAMC), Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National des Sciences Appliquées - Toulouse (INSA Toulouse), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), and Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Université Toulouse III - Paul Sabatier (UT3)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Star (game theory), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, condensation: Bose-Einstein, 01 natural sciences, General Relativity and Quantum Cosmology, dark matter: halo, velocity: dispersion, 0103 physical sciences, thermodynamical, black hole, fermion: dark matter, 010306 general physics, Axion, Astrophysics::Galaxy Astrophysics, axion: star, halo: mass, Boson, Physics, Condensed Matter::Quantum Gases, boson: dark matter, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Order (ring theory), Scattering length, Fermion, stability, Pauli principle, Cosmology, Dark matter halo, Black hole, Automatic Keywords, collapse, scattering length, gravitation: self-force, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Atomic physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We study the core mass-halo mass relation of bosonic dark matter halos, in the form of self-gravitating Bose-Einstein condensates, harboring a supermassive black hole. We use the ``velocity dispersion tracing'' relation according to which the velocity dispersion in the core ${v}_{c}^{2}\ensuremath{\sim}G{M}_{c}/{R}_{c}$ is of the same order as the velocity dispersion in the halo ${v}_{h}^{2}\ensuremath{\sim}G{M}_{h}/{r}_{h}$ (this relation can be justified from thermodynamical arguments) and the approximate analytical mass-radius relation of the quantum core in the presence of a central black hole obtained in our previous paper [P.H. Chavanis, Eur. Phys. J. Plus 134, 352 (2019)]. For a given minimum halo mass $({M}_{h}{)}_{\mathrm{min}}\ensuremath{\sim}{10}^{8}\text{ }\text{ }{M}_{\ensuremath{\bigodot}}$ determined by the observations, the only free parameter of our model is the scattering length ${a}_{s}$ of the bosons (their mass $m$ is then determined in order to match the characteristics of the minimum halo). For noninteracting bosons and for bosons with a repulsive self-interaction, we find that the core mass ${M}_{c}$ increases with the halo mass ${M}_{h}$ and achieves a maximum value $({M}_{c}{)}_{\mathrm{max}}$ at some halo mass $({M}_{h}{)}_{*}$ before decreasing. The whole series of equilibria is stable. For bosons with an attractive self-interaction, we find that the core mass achieves a maximum value $({M}_{c}{)}_{\mathrm{max}}$ at some halo mass $({M}_{h}{)}_{*}$ before decreasing. The series of equilibria becomes unstable above a maximum halo mass $({M}_{h}{)}_{\mathrm{max}}\ensuremath{\ge}({M}_{h}{)}_{*}$. In the absence of black hole $({M}_{h}{)}_{\mathrm{max}}=({M}_{h}{)}_{*}$. At that point, the quantum core (similar to a dilute axion star) collapses. We perform a similar study for fermionic dark matter halos. We find that they behave similarly to bosonic dark matter halos with a repulsive self-interaction, the Pauli exclusion principle for fermions playing the role of the repulsive self-interaction for bosons.

Published
2020
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7. Searches for electron interactions induced by new physics in the EDELWEISS-III germanium bolometers

Author

M. De Jesus, M. Chapellier, A. Giuliani, F. Charlieux, J. Gascon, L. Dumoulin, R. Maisonobe, B. Paul, C. Augier, Ph. Camus, V. A. Kudryavtsev, M. Kleifges, C. Nones, A. Juillard, J. Billard, S. Scorza, Luc Bergé, V. Kozlov, Alain Benoit, D. Misiak, Denis Tcherniakhovski, K. Eitel, M. Weber, P. Pari, E. Olivieri, S. Marnieros, H. Kraus, E. Queguiner, A. Cazes, H. Le Sueur, M. Gros, E. Armengaud, Yong Jin, L. Vagneron, D.V. Poda, B. Siebenborn, A. S. Zolotarova, V. Sanglard, S. V. Rozov, A. Broniatowski, X-F. Navick, E. Yakushev, 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), 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), 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), 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]), Cryogénie (NEEL - Cryo), and Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)

Subjects
Physics - Instrumentation and Detectors, Physics beyond the Standard Model, Dark matter, galaxy: dark matter, FOS: Physical sciences, Cosmic ray, coupling constant: upper limit, S029AEC, Electron, Astrophysics::Cosmology and Extragalactic Astrophysics, EDELWEISS, 7. Clean energy, 01 natural sciences, High Energy Physics - Experiment, Nuclear physics, Galactic halo, High Energy Physics - Experiment (hep-ex), galaxy: halo, bolometer, cosmic rays, 0103 physical sciences, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Experiments in gravity, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], axion: coupling, 010306 general physics, Axion, S030UDM, Physics, photon: hidden sector, axion: dark matter, boson: dark matter, 010308 nuclear & particles physics, new physics, dark matter: mass, S029HPH, Instrumentation and Detectors (physics.ins-det), 3. Good health, Massless particle, germanium, S029IAN, electron: interaction, electron: lifetime, axion-like particles, axion: solar, absorption, cosmology, experimental results
Abstract

We make use of the EDELWEISS-III array of germanium bolometers to search for electron interactions at the keV scale induced by phenomena beyond the Standard Model. A 90% C.L. lower limit is set on the electron lifetime decaying to invisibles, $��> 1.2\times 10^{24}$ years. We investigate the emission of axions or axionlike particles (ALPs) by the Sun, constraining the coupling parameters $g_{ae}, 8 pages, 5 figures, matches published version

Published
2018
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8. Fundamental physics with the Hubble Frontier Fields: constraining Dark Matter models with the abundance of extremely faint and distant galaxies

Author

Alexander Merle, Andrea Grazian, Marco Castellano, Norma G. Sanchez, Aurel Schneider, Maximilian Totzauer, Nicola Menci, Observatoire de Paris - Site de Paris (OP), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS), FRA, DEU, Observatoire de Paris - Site de Paris ( OP ), and Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Centre National de la Recherche Scientifique ( CNRS )

Subjects
High Energy Physics - Theory, Sterile neutrino, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astrophysics, coupling: scalar, scalar particle: decay, 01 natural sciences, [ PHYS.HTHE ] Physics [physics]/High Energy Physics - Theory [hep-th], High Energy Physics - Phenomenology (hep-ph), 010303 astronomy & astrophysics, Physics, density, boson: dark matter, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], redshift: high, formation, Coupling (probability), High Energy Physics - Phenomenology, Neutrino, Astrophysics - Cosmology and Nongalactic Astrophysics, Structure formation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Scalar (mathematics), Dark matter, FOS: Physical sciences, mixing angle, Astrophysics::Cosmology and Extragalactic Astrophysics, condensation: Bose-Einstein, mass: scalar, dark matter, 0103 physical sciences, galaxies: formation, structure, fuzzy, 010308 nuclear & particles physics, neutrino: sterile: mass, High Energy Physics::Phenomenology, Astronomy and Astrophysics, lepton: asymmetry, Astrophysics - Astrophysics of Galaxies, Galaxy, Redshift, High Energy Physics - Theory (hep-th), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), High Energy Physics::Experiment, galaxies: abundances, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], coupling: Yukawa, resonance: production
Abstract

We show that the measured abundance of ultra-faint lensed galaxies at $z\approx 6$ in the Hubble Frontier Fields (HFF) provides stringent constraints on the parameter space of i) Dark Matter models based on keV sterile neutrinos; ii) the "fuzzy" wavelike Dark Matter models, based on Bose-Einstein condensate of ultra-light particles. For the case of the sterile neutrinos, we consider two production mechanisms: resonant production through the mixing with active neutrinos and the decay of scalar particles. For the former model, we derive constraints for the combination of sterile neutrino mass $m_{\nu}$ and mixing parameter $\sin^2(2\theta)$ which provide the tightest lower bounds on the mixing angle (and hence on the lepton asymmetry) derived so far by methods independent of baryonic physics. For the latter we compute the allowed combinations of the scalar mass, its coupling to the Higgs field, and the Yukawa coupling of the scalar to the sterile neutrinos. We compare our results to independent, existing astrophysical bounds on sterile neutrinos in the same mass range. For the case of "fuzzy" Dark Matter, we show that the observed number density $\approx 1/{\rm Mpc}^3$ of high-redshift galaxies in the HFF sets a lower limit $m_\psi\geq 8\cdot 10^{-22}$ eV (at 3-$\sigma$ confidence level) on the particle mass, a result that strongly disfavors wavelike bosonic Dark Matter as a viable model for structure formation. We discuss the impact on our results of uncertainties due to systematics in the selection of highly magnified, faint galaxies at high redshifts., Comment: 28 pages, accepted for publication in The Astrophysical Journal

Published
2017
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9. Constraining the mass of light bosonic dark matter using SDSS Lyman-$\alpha$ forest

Author

David J. E. Marsh, Nathalie Palanque-Delabrouille, Julien Baur, Christophe Yèche, Eric Armengaud, 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 Recherches sur les lois Fondamentales de l'Univers ( IRFU ), and Commissariat à l'énergie atomique et aux énergies alternatives ( CEA ) -Université Paris-Saclay

Subjects
effect: quantum, cosmological model, Structure formation, matter: power spectrum, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Dark matter, sloan digital sky survey, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, 7. Clean energy, Spectral line, dark matter, mass: constraint, statistical analysis, 0103 physical sciences, Warm dark matter, large-scale structure of Universe – dark matter, quasar, structure, 010303 astronomy & astrophysics, matter: density, numerical methods: hydrodynamics, Physics, boson: dark matter, fuzzy, 010308 nuclear & particles physics, Matter power spectrum, dark matter: mass, formation, Astronomy and Astrophysics, Quasar, field theory: scalar, 13. Climate action, Space and Planetary Science, nonlinear, Matter wave, large-scale structure of Universe, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

If a significant fraction of the dark matter in the Universe is made of an ultra-light scalar field, named fuzzy dark matter (FDM) with a mass $m_a$ of the order of $10^{-22}-10^{-21}$ eV, then its de Broglie wavelength is large enough to impact the physics of large scale structure formation. In particular, the associated cut-off in the linear matter power spectrum modifies the structure of the intergalactic medium (IGM) at the scales probed by the Lyman-$\alpha$ forest of distant quasars. We study this effect by making use of dedicated cosmological simulations which take into account the hydrodynamics of the IGM. We explore heuristically the amplitude of quantum pressure for the FDM masses considered here and conclude that quantum effects should not modify significantly the non-linear evolution of matter density at the scales relevant to the measured Lyman-$\alpha$ flux power, and for $m_a \geq 10^{-22}$ eV. We derive a scaling law between $m_a$ and the mass of the well-studied thermal warm dark matter (WDM) model that is best adapted to the Lyman-$\alpha$ forest data, and differs significantly from the one infered by a simple linear extrapolation. By comparing FDM simulations with the Lyman-$\alpha$ flux power spectra determined from the BOSS survey, and marginalizing over relevant nuisance parameters, we exclude FDM masses in the range $10^{-22} \leq m_a < 2.3\times 10^{-21}$ eV at 95 % CL. Adding higher-resolution Lyman-$\alpha$ spectra extends the exclusion range up to $2.9\times 10^{-21}$ eV. This provides a significant constraint on FDM models tailored to solve the "small-scale problems" of $\Lambda$CDM., Comment: Matches accepted version

Published
2017
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