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59 results on '"Astrophysics and astroparticle physics"'

1. Search for inelastic scattering of WIMP dark matter in XENON1T

Author

A. Manfredini, L. Scotto Lavina, Hardy Simgen, A. D. Ferella, R. Budnik, Yuehuan Wei, L. Grandi, G. Koltman, C. Weinheimer, K. Martens, F. Arneodo, M. Messina, Lorne Levinson, F. Joerg, Kaixuan Ni, D. Cichon, N. Kato, C. Macolino, L. Hoetzsch, A. Elykov, T. Wolf, Elena Aprile, João Cardoso, M. Pierre, D. Ramírez García, F. Gao, Keita Mizukoshi, P. Shagin, J. A. M. Lopes, Y. Mosbacher, Y. Ma, Masaki Yamashita, P. Di Gangi, S. Moriyama, T. Zhu, F. D. Amaro, Guillaume Plante, Fabrizio Marignetti, M. Vargas, H. Landsman, M. P. Decowski, April S. Brown, Boris Bauermeister, Jochen Schreiner, D. Masson, T. Marrodán Undagoitia, L. Bellagamba, A. Rocchetti, S. Liang, Manfred Lindner, L. Althueser, K. Odgers, J. Howlett, Katsuki Hiraide, F. Lombardi, M. Alfonsi, S. Andaloro, J.M.F. dos Santos, F. Agostini, R. Di Stefano, V. Pizzella, Giacomo Bruno, J. Naganoma, N. Šarčević, J. Qin, Sebastian Lindemann, G. Sartorelli, J. Pienaar, C. Capelli, N. Rupp, Gian Carlo Trinchero, K. Morå, Michelle Galloway, H. Schulze Eißing, E. Angelino, S. Bruenner, A. Molinario, S. Mastroianni, Jean-Pierre Cussonneau, M. Iacovacci, A. Di Giovanni, Bart Pelssers, C. Tunnell, C. Wittweg, J. P. Zopounidis, D. Coderre, Manuel Gameiro da Silva, M. Scheibelhut, Jelle Aalbers, A. Depoian, M. Selvi, D. Schulte, Kathrin Valerius, A. Kopec, S. Reichard, Qing Lin, J. Qi, J. Palacio, J. Ye, B. Cimmino, M. Clark, Atsushi Takeda, Shingo Kazama, G. Volta, Uwe Oberlack, V. C. Antochi, Ethan Brown, Kentaro Miuchi, C. Therreau, J. Cuenca, Y. Zhang, Julien Masbou, Z. Xu, M. Murra, W. Fulgione, Laura Manenti, C. Hils, Sara Diglio, J. Mahlstedt, G. Zavattini, Laura Baudis, P. Gaemers, F. Toschi, M. L. Benabderrahmane, J. Long, J. R. Angevaare, E. Shockley, Jan Conrad, Masanori Kobayashi, R. Gaior, Yoshitaka Itow, M. Weiss, D. Thers, Marc Schumann, F. Semeria, R. F. Lang, A. P. Colijn, D. Wenz, R. Peres, A. Mancuso, Aprile, E., Aalbers, J., Agostini, F., Alfonsi, M., Althueser, L., Amaro, F. D., Andaloro, S., Angelino, E., Angevaare, J. R., Antochi, V. C., Arneodo, F., Baudis, L., Bauermeister, B., Bellagamba, L., Benabderrahmane, M. L., 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., Cuenca, J., Cussonneau, J. P., Decowski, M. P., Depoian, A., Di Gangi, P., Di Giovanni, A., Di Stefano, R., Diglio, S., Elykov, A., Ferella, A. D., Fulgione, W., Gaemers, P., Gaior, R., Galloway, M., Gao, F., Grandi, L., 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., Liang, S., Lin, Q., Lindemann, S., Lindner, M., Lombardi, F., Long, J., Lopes, J. A. M., Ma, Y., Macolino, C., Mahlstedt, J., Mancuso, A., Manenti, L., Manfredini, A., Marignetti, F., Marrodan Undagoitia, T., Martens, K., Masbou, J., Masson, D., Mastroianni, S., Messina, M., Miuchi, K., Mizukoshi, K., Molinario, A., Mora, K., Moriyama, S., Mosbacher, Y., Murra, M., Naganoma, J., Ni, K., Oberlack, U., Odgers, K., Palacio, J., Pelssers, B., Peres, R., Pienaar, J., Pierre, M., Pizzella, V., Plante, G., Qi, J., Qin, J., Ramirez Garcia, D., Reichard, S., Rocchetti, A., Rupp, N., Dos Santos, J. M. F., Sartorelli, G., Sarcevic, N., Scheibelhut, M., Schreiner, J., Schulte, D., Schulze Eissing, H., 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., Valerius, K., Vargas, M., Volta, G., Wei, Y., Weinheimer, C., Weiss, M., Wenz, D., Wittweg, C., Wolf, T., Xu, Z., Yamashita, M., Ye, J., Zavattini, G., Zhang, Y., Zhu, T., Zopounidis, J. P., XENON Collaboration, 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), 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), 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 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), XENON, IoP (FNWI), and XENON (IHEF, IoP, FNWI)

Subjects
xenon: target, Photon, Physics::Instrumentation and Detectors, Parameter space, 01 natural sciences, WIMP: dark matter, High Energy Physics - Experiment, astro-ph.CO, High Energy Physics - Experiment (hep-ex), XENON, Recoil, WIMP, WIMP nucleus: cross section, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Dark Matter, parameter space, Nuclear Experiment, ComputingMilieux_MISCELLANEOUS, nucleus: recoil, Physics, Dark Matter, Inelastic scattering, XENON, Direct Dark Matter, photon, Astrophysics::Instrumentation and Methods for Astrophysics, Direct Dark Matter, Weakly interacting massive particles, signature, Astrophysics - Cosmology and Nongalactic Astrophysics, Particle physics, Inelastic scattering, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Dark matter, FOS: Physical sciences, WIMP: mass, Astrophysics::Cosmology and Extragalactic Astrophysics, NO, PE2_2, PE2_1, 0103 physical sciences, ddc:530, 010306 general physics, 010308 nuclear & particles physics, Scattering, WIMP nucleus: interaction, Dark, matter, WIMP: interaction, High Energy Physics::Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics, experimental results
Abstract

We report the results of a search for the inelastic scattering of weakly interacting massive particles (WIMPs) in the XENON1T dark matter experiment. Scattering off $^{129}$Xe is the most sensitive probe of inelastic WIMP interactions, with a signature of a 39.6 keV de-excitation photon detected simultaneously with the nuclear recoil. Using an exposure of 0.89 tonne-years, we find no evidence of inelastic WIMP scattering with a significance of more than 2$\sigma$. A profile-likelihood ratio analysis is used to set upper limits on the cross-section of WIMP-nucleus interactions. We exclude new parameter space for WIMPs heavier than 100 GeV/c${}^2$, with the strongest upper limit of $3.3 \times 10^{-39}$ cm${}^2$ for 130 GeV/c${}^2$ WIMPs at 90\% confidence level., Comment: 9 pages, 4 figures

Published
2021
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2. Simultaneous estimation of astrophysical and cosmological stochastic gravitational-wave backgrounds with terrestrial detectors

Author

Nelson Christensen, K. Martinovic, P. M. Meyers, Mairi Sakellariadou, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
gravitational radiation: stochastic, gr-qc, media_common.quotation_subject, FOS: Physical sciences, Binary number, detector: network, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Omega, General Relativity and Quantum Cosmology, Einstein Telescope, binary: coalescence, 0103 physical sciences, Sensitivity (control systems), LIGO, cosmic string, 010306 general physics, media_common, Physics, General Relativity and Cosmology, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, statistical analysis: Bayesian, critical phenomena, binary: compact, Universe, detector: sensitivity, Cosmic string, VIRGO, 13. Climate action, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics and astroparticle physics
Abstract

The recent Advanced LIGO and Advanced Virgo joint observing runs have not claimed a stochastic gravitational-wave background detection, but one expects this to change as the sensitivity of the detectors improves. The challenge of claiming a true detection will be immediately succeeded by the difficulty of relating the signal to the sources that contribute to it. In this paper, we consider backgrounds that comprise compact binary coalescences and additional cosmological sources, and we set simultaneous upper limits on these backgrounds. We find that the Advanced LIGO/Advanced Virgo network, operating at design sensitivity, will not allow for separation of the sources we consider. Third-generation detectors, sensitive to most individual compact binary mergers, can reduce the astrophysical signal via subtraction of individual sources, and potentially reveal a cosmological background. Our Bayesian analysis shows that, assuming a detector network containing Cosmic Explorer and Einstein Telescope and reasonable levels of individual source subtraction, we can detect cosmological signals ΩCS(25 Hz)=4.5×10−13 for cosmic strings, and ΩBPL(25 Hz)=2.2×10−13 for a broken power-law model of an early Universe phase transition. The recent Advanced LIGO and Advanced Virgo joint observing runs have not claimed a stochastic gravitational-wave background detection, but one expects this to change as the sensitivity of the detectors improves. The challenge of claiming a true detection will be immediately succeeded by the difficulty of relating the signal to the sources that contribute to it. In this paper, we consider backgrounds that comprise compact binary coalescences and additional cosmological sources, and we set simultaneous upper limits on these backgrounds. We find that the Advanced LIGO, Advanced Virgo network, operating at design sensitivity, will not allow for separation of the sources we consider. Third generation detectors, sensitive to most individual compact binary mergers, can reduce the astrophysical signal via subtraction of individual sources, and potentially reveal a cosmological background. Our Bayesian analysis shows that, assuming a detector network containing Cosmic Explorer and Einstein Telescope and reasonable levels of individual source subtraction, we can detect cosmological signals $\Omega_{\rm{CS}} (25\,\rm{Hz})=4.5 \times 10^{-13}$ for cosmic strings, and $\Omega_{\rm BPL}(25\,\rm{Hz})= 2.2 \times 10^{-13}$ for a broken power law model of an early universe phase transition.

Published
2021
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3. Prospects for detecting heavy WIMP dark matter with the Cherenkov Telescope Array: The Wino and Higgsino

Author

Oscar Macias, Tracy R. Slatyer, Lucia Rinchiuso, Nicholas L. Rodd, Emmanuel Moulin, Département de Physique des Particules (ex SPP) (DPP), 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, and Département de Physique des Particules (ex SPP) (DPhP)

Subjects
Cherenkov Telescope Array, scale: TeV, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Wino, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Cherenkov counter: atmosphere, WIMP: dark matter, 01 natural sciences, thermal, Standard Model, mass: scale, WIMP, 0103 physical sciences, Higgsino, 010306 general physics, Cherenkov radiation, Physics, background, 010308 nuclear & particles physics, Astrophysics::Instrumentation and Methods for Astrophysics, imaging, sensitivity, cosmic radiation, Weakly interacting massive particles, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

TeV-scale particles that couple to the standard model through the weak force represent a compelling class of dark matter candidates. The search for such Weakly Interacting Massive Particles (WIMPs) has already spanned multiple decades, and whilst it has yet to provide any definitive evidence for their existence, viable parameter space remains. In this paper, we show that the upcoming Cherenkov Telescope Array (CTA) has significant sensitivity to uncharted parameter space at the TeV mass scale. To do so, we focus on two prototypical dark matter candidates, the Wino and Higgsino. Sensitivity forecasts for both models are performed including the irreducible background from misidentified cosmic rays, as well as a range of estimates for the Galactic emissions at TeV energies. For each candidate, we find substantial expected improvements over existing bounds from current imaging atmospheric Cherenkov telescopes. In detail, for the Wino we find a sensitivity improvement of roughly an order of magnitude in $\langle \sigma v \rangle$, whereas for the Higgsino we demonstrate that CTA has the potential to become the first experiment that has sensitivity to the thermal candidate. Taken together, these enhanced sensitivities demonstrates the discovery potential for dark matter at CTA in the 1-100 TeV mass range.

Published
2021
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4. INTEGRAL x-ray constraints on sub-GeV dark matter

Author

Elena Pinetti, Bradley J. Kavanagh, Nicolao Fornengo, Marco Cirelli, SCOAP, European Commission, European Research Council, Centre National de la Recherche Scientifique (France), Ministero dell'Istruzione, dell'Università e della Ricerca, Università Italo Francese, Università di Torino, Istituto Nazionale di Fisica Nucleare, Agencia Estatal de Investigación (España), Ministerio de Ciencia, Innovación y Universidades (España), CIRELLI, Marco, Laboratoire de Physique Théorique et Hautes Energies (LPTHE), and Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, Cosmic microwave background, Dark matter, Cosmic background radiation, Flux, FOS: Physical sciences, Astrophysics, cosmic background radiation, 01 natural sciences, 7. Clean energy, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, X-ray: emission, 010306 general physics, Light dark matter, ComputingMilieux_MISCELLANEOUS, Physics, 010308 nuclear & particles physics, dark matter: mass, Gamma ray, Compton scattering, dark matter: flux, Galaxy, [PHYS.HPHE] Physics [physics]/High Energy Physics - Phenomenology [hep-ph], High Energy Physics - Phenomenology, gamma ray: emission, Compton scattering: inverse, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

Light dark matter (DM), defined here as having a mass between 1 MeV and about 1 GeV, is an interesting possibility both theoretically and phenomenologically, at one of the frontiers of current progress in the field of DM searches. Its indirect detection via gamma rays is challenged by the scarcity of experiments in the MeV–GeV region. We look therefore at lower-energy x-ray data from the INTEGRAL telescope, and compare them with the predicted DM flux. We derive bounds which are competitive with existing ones from other techniques. Crucially, we include the contribution from inverse Compton scattering on galactic radiation fields and the cosmic microwave background, which leads to much stronger constraints than in previous studies for DM masses above 20 MeV., Funded by SCOAP3., We also acknowledge the following organizations for support: European Research Council (ERC) under the EU Seventh Framework Programme (Grant No. FP7/2007-2013)/ERC Starting Grant (Agreement No. 278234—“NEWDARK” project); CNRS 80|Prime grant (“DAMEFER” project) (M. C.); Departments of Excellence grant awarded by the Italian Ministry of Education, University and Research (MIUR) (N. F. and E. P.); Research grant of the Università Italo-Francese, under Bando Vinci 2020 (E. P.); Research grant The Dark Universe: A Synergic Multimessenger Approach, Grant No. 2017X7X85K funded by the Italian Ministry of Education, University and Research (MIUR); Research grant The Anisotropic Dark Universe, Grant No. CSTO161409, funded by Compagnia di Sanpaolo and University of Torino; Research grant TASP (Theoretical Astroparticle Physics) funded by Istituto Nazionale di Fisica Nucleare (INFN) (N. F. and E. P.); Spanish Agencia Estatal de Investigación (AEI, MICIU) for the support to the Unidad de Excelencia María de Maeztu Instituto de Física de Cantabria, Ref. No. MDM-2017-0765 (B. J. K.).

Published
2021
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5. Sum of the masses of the Milky Way and M31: A likelihood-free inference approach

Author

Ofer Lahav, Niall Jeffrey, Yehuda Hoffman, P. Lemos, I Noam Libeskind, L. Whiteway, Astrophysique, Laboratoire de physique de l'ENS - ENS Paris (LPENS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Sorbonne Université (SU)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), 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), Laboratoire de physique de l'ENS - ENS Paris (LPENS (UMR_8023)), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-École normale supérieure - Paris (ENS Paris), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
Cold dark matter, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Approximations of π, Milky Way, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Lambda, 01 natural sciences, Combinatorics, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], 010303 astronomy & astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, Physics, 010308 nuclear & particles physics, Local Group, Density estimation, 16. Peace & justice, Astrophysics - Astrophysics of Galaxies, Galaxy, Andromeda, Astrophysics of Galaxies (astro-ph.GA), Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

We use Density Estimation Likelihood-Free Inference, $\Lambda$ Cold Dark Matter simulations of $\sim 2M$ galaxy pairs, and data from Gaia and the Hubble Space Telescope to infer the sum of the masses of the Milky Way and Andromeda (M31) galaxies, the two main components of the Local Group. This method overcomes most of the approximations of the traditional timing argument, makes the writing of a theoretical likelihood unnecessary, and allows the non-linear modelling of observational errors that take into account correlations in the data and non-Gaussian distributions. We obtain an $M_{200}$ mass estimate $M_{\rm MW+M31} = 4.6^{+2.3}_{-1.8} \times 10^{12} M_{\odot}$ ($68 \%$ C.L.), in agreement with previous estimates both for the sum of the two masses and for the individual masses. This result is not only one of the most reliable estimates of the sum of the two masses to date, but is also an illustration of likelihood-free inference in a problem with only one parameter and only three data points., Comment: 14 pages, 9 figures. Accepted by Physical Review D

Published
2021
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6. Machine learning gravitational waves from binary black hole mergers

Author

Alessandro Nagar, Walter Del Pozzo, Matteo Breschi, Gunnar Riemenschneider, Stefano Schmidt, R. Gamba, Piero Rettegno, Sebastiano Bernuzzi, G. Pagano, Institut des Hautes Etudes Scientifiques (IHES), and IHES

Subjects
binary: mass, data analysis method, principal component analysis, Phase (waves), Binary number, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Parameter space, Machine learning, computer.software_genre, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational waves, Binary black hole, binary: coalescence, 0103 physical sciences, Waveform, 010306 general physics, numerical calculations, Physics, spin: precession, black hole: spin, 010308 nuclear & particles physics, business.industry, Gravitational wave, gravitational radiation, Amplitude, wave: model, machine learning, black hole: binary, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], mass ratio, Artificial intelligence, business, computer, Gravitational waves, machine learning, Dimensionless quantity, Astrophysics and astroparticle physics
Abstract

We apply machine learning methods to build a time-domain model for gravitational waveforms from binary black hole mergers, called mlgw. The dimensionality of the problem is handled by representing the waveform's amplitude and phase using a principal component analysis. We train mlgw on about $\mathcal{O}(10^3)$ TEOBResumS and SEOBNRv4 effective-one-body waveforms with mass ratios $q\in[1,20]$ and aligned dimensionless spins $s\in[-0.80,0.95]$. The resulting models are faithful to the training sets at the ${\sim}10^{-3}$ level (averaged on the parameter space). The speed up for a single waveform generation is a factor 10 to 50 (depending on the binary mass and initial frequency) for TEOBResumS and approximately an order of magnitude more for SEOBNRv4. Furthermore, mlgw provides a closed form expression for the waveform and its gradient with respect to the orbital parameters; such an information might be useful for future improvements in GW data analysis. As demonstration of the capabilities of mlgw to perform a full parameter estimation, we re-analyze the public data from the first GW transient catalog (GWTC-1). We find broadly consistent results with previous analyses at a fraction of the cost, although the analysis with spin aligned waveforms gives systematic larger values of the effective spins with respect to previous analyses with precessing waveforms. Since the generation time does not depend on the length of the signal, our model is particularly suitable for the analysis of the long signals that are expected to be detected by third-generation detectors. Future applications include the analysis of waveform systematics and model selection in parameter estimation., Comment: 15 pages, 11 figures, submitted to Phys. Rev. D

Published
2021
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7. Gamma-ray image reconstruction of the Andromeda galaxy

Author

Francesca Calore, Céline Armand, 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), and 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)

Subjects
History, Andromeda Galaxy, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, Iterative reconstruction, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, GLAST, Education, High Energy Physics - Phenomenology (hep-ph), Bulge, 0103 physical sciences, Fitting algorithm, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Image (category theory), Gamma ray, Galaxy, Computer Science Applications, High Energy Physics - Phenomenology, gamma ray, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], spectral, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

We analyze about 12 years of Fermi-LAT data in the direction of the Andromeda galaxy (M31). We robustly characterize its spectral and morphological properties against systematic uncertainties related to the modeling of the Galactic diffuse emission. We perform this work by adapting and exploiting the potential of the skyFACT adaptive template fitting algorithm. We reconstruct the gamma-ray image of M31 in a template-independent way, and we show that flat spatial models are preferred by data, indicating an extension of the $\gamma$-ray emission of about 0.3-0.4 degree for the bulge of M31. This study also suggests that a second component, extending to at least 1 degree, contributes to the observed total emission. We quantify systematic uncertainties related to mis-modeling of Galactic foreground emission at the level of 2.9%., Comment: 14 pages, 8 figures, 5 tables

Published
2021
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8. Higher-order effects in the dynamics of hierarchical triple systems. Quadrupole-squared terms

Author

Clifford M. Will, 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
Binary number, Perturbation (astronomy), FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, Binary system, 010306 general physics, Solar and Stellar Astrophysics (astro-ph.SR), Mathematical physics, Physics, Orbital elements, Earth and Planetary Astrophysics (astro-ph.EP), 010308 nuclear & particles physics, Secular evolution, Equations of motion, Astrophysics - Astrophysics of Galaxies, Orbit, Astrophysics - Solar and Stellar Astrophysics, Astrophysics of Galaxies (astro-ph.GA), Quadrupole, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Earth and Planetary Astrophysics, Astrophysics and astroparticle physics
Abstract

We analyze the secular evolution of hierarchical triple systems to second-order in the quadrupolar perturbation induced on the inner binary by the distant third body. The Newtonian three-body equations of motion, expanded in powers of the ratio of semimajor axes $a/A$, become a pair of effective one-body Keplerian equations of motion, perturbed by a sequence of multipolar perturbations, denoted quadrupole, $O[(a/A)^3]$, octupole, $O[(a/A)^4]$, and so on. In the Lagrange planetary equations for the evolution of the instantaneous orbital elements, second-order effects arise from obtaining the first-order solution for each element, consisting of a constant (or slowly varying) piece and an oscillatory perturbative piece, and reinserting it back into the equations to obtain a second-order solution. After an average over the two orbital timescales to obtain long-term evolutions, these second-order quadrupole ($Q^2$) terms would be expected to produce effects of order $(a/A)^6$. However we find that the orbital average actually enhances the second-order terms by a factor of the ratio of the outer to the inner orbital periods, $ \sim (A/a)^{3/2}$. For systems with a low-mass third body, the $Q^2$ effects are small, but for systems with a comparable-mass or very massive third body, such as a Sun-Jupiter system orbiting a solar-mass star, or a $100 \, M_\odot$ binary system orbiting a $10^6 \, M_\odot$ massive black hole, the $Q^2$ effects can completely suppress flips of the inner orbit from prograde to retrograde and back that occur in the first-order solutions. These results are in complete agreement with those of Luo, Katz and Dong, derived using a "Corrected Double-Averaging" method., Comment: 16 pages, 7 figures

Published
2021
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9. Sidereal filtering: A novel robust method to search for continuous gravitational waves

Author

S. Mastrogiovanni, I. La Rosa, P. Astone, C. Palomba, S. D'Antonio, Luca Rei, S. Frasca, O. J. Piccinni, P. Leaci, L. Pierini, 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
data analysis method, interferometer, detector: noise, hierarchy, Gravitational Waves, Continuous Waves, Data Analysis, 01 natural sciences, programming, Robustness (computer science), 0103 physical sciences, numerical methods, hardware, LIGO, 010306 general physics, numerical calculations, Physics, 010308 nuclear & particles physics, Gravitational wave, Noise (signal processing), Detector, gravitational radiation, Filter (signal processing), gravitational radiation detector, detector: sensitivity, Sidereal time, Harmonic, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Algorithm, Astrophysics and astroparticle physics
Abstract

International audience; In this paper we introduce a novel filtering method for the search of continuous gravitational wave signals in the data of interferometric detectors, based on the estimation of the harmonic content of the detector sidereal pattern. Thanks to the very specific properties of the sidereal modulation, the method is powerful in discriminating among continuous wave signals of astrophysical origin and detector artefacts or noise outliers. We describe here the statistical properties of the filter by using both software and hardware simulated signals injected in the data of the LIGO second science run O2 and we give an estimate of the method sensitivity. A study of the method robustness with respect to a nonoptimal correction of the signal frequency variation, referring in particular to the spin-down, is also presented. This novel filtering procedure is well suited for directed searches of sources with known—or loosely known—position and largely unknown frequency and spin-down, and for the follow-up of all-sky candidates. Used as an initial processing step it has, moreover, the potential to improve the sensitivity of wide-band hierarchical searches.

Published
2021
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10. Isotropic X-ray bound on Primordial Black Hole Dark Matter

Author

Pasquale D. Serpico, J. Iguaz, Thomas Siegert, 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
Cosmology and Nongalactic Astrophysics (astro-ph.CO), gamma ray: background, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, positron: annihilation, Primordial black hole, Astrophysics, dark matter: density, spin, 01 natural sciences, 7. Clean energy, evaporation, High Energy Physics - Phenomenology (hep-ph), Positron, 0103 physical sciences, X-ray: emission, Sensitivity (control systems), 010306 general physics, Spin-½, Physics, 010308 nuclear & particles physics, Isotropy, sensitivity, flux, High Energy Physics - Phenomenology, 13. Climate action, Annihilation radiation, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Order of magnitude, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

We revisit the constraints on evaporating primordial black holes (PBHs) from the isotropic X-ray and soft gamma-ray background in the mass range $10^{16}-10^{18}$ g. We find that they are stronger than usually inferred due to two neglected effects: i) The contribution of the annihilation radiation due to positrons emitted in the evaporation process. ii) The high-latitude, Galactic contribution to the measured isotropic flux. We study the dependence of the bounds from the datasets used, the positron annihilation conditions, and the inclusion of the astrophysical background. We push the exclusion limit for non-spinning PBH with monochromatic mass function as the totality of dark matter to 1.5$\times 10^{17}\,$g, which represents a $\sim$15$\%$ improvement with respect to earlier bounds and translates into almost an order of magnitude improvement in the PBH fraction in the already probed region. We also show that the inclusion of spin and/or an extended, log-normal mass function lead to tighter bounds. Our study suggests that the isotropic flux is an extremely promising target for future missions in improving the sensitivity to PBHs as candidates for dark matter., 10 pages, 14 figures Clarification added and a software output interpretation mistake corrected; only minor changes to the results

Published
2021
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11. Probing new light gauge bosons with gravitational-wave interferometers using an adapted semicoherent method

Author

A. J. Tanasijczuk, C. Palomba, Iuri La Rosa, O. J. Piccinni, Giacomo Bruno, Luca Rei, Sabrina D'Antonio, P. Leaci, L. Pierini, Sebastien Clesse, Federico De Lillo, S. Frasca, A. L. Miller, P. Astone, A. Depasse, Laboratoire d'Annecy de Physique des Particules (LAPP), and 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)

Subjects
data analysis method, Coherence time, Particle physics, dark matter: interaction, experimental methods, interferometer, Dark matter, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Dark photon, Gravitational waves, numerical methods, 0103 physical sciences, Bosons, Interferometers, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], numerical calculations, neutron star, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Boson, Physics, Gauge boson, 010308 nuclear & particles physics, Gravitational wave, photon, High Energy Physics::Phenomenology, modulation: frequency, gravitational radiation, Doppler effect, gravitational radiation detector, LIGO, coherence, detector: sensitivity, Interferometry, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics and astroparticle physics
Abstract

We adapt a method, originally developed for searches for quasi-monochromatic, quasi-infinite gravitational-wave signals, to directly detect new light gauge bosons with laser interferometers, which could be candidates for dark matter. To search for these particles, we optimally choose the analysis coherence time as a function of boson mass, such that all of the signal power will be confined to one frequency bin. We focus on the dark photon, a gauge boson that could couple to baryon or baryon-lepton number, and explain that its interactions with gravitational-wave interferometers result in a narrow-band, stochastic signal. We provide an end-to-end analysis scheme, estimate its computational cost, and investigate follow-up techniques to confirm or rule out dark matter candidates. Furthermore, we derive a theoretical estimate of the sensitivity, and show that it is consistent with both the empirical sensitivity determined through simulations, and results from a cross-correlation search. Finally, we place Feldman-Cousins upper limits using data from LIGO Livingston's second observing run, which give a new and strong constraint on the coupling of gauge bosons to the interferometer., Comment: 16 pages, 14 figures

Published
2021
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12. Bounds on axionlike particles from the diffuse supernova flux

Author

Alessandro Mirizzi, Francesca Calore, Joerg Jaeckel, Pierluca Carenza, Maurizio Giannotti, 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
Particle physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, magnetic field: galaxy, 01 natural sciences, 7. Clean energy, GLAST, Physics::Geophysics, High Energy Physics - Phenomenology (hep-ph), photon: coupling, supernova, 0103 physical sciences, gamma ray: flux, nucleon nucleon: bremsstrahlung, Nuclear Experiment, 010306 general physics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, nucleon, Bremsstrahlung, Gamma ray, High Energy Physics - Phenomenology, Supernova, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Diffuse flux, axion-like particles, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Nucleon, Astrophysics and astroparticle physics, Production rate
Abstract

The cumulative emission of Axion-Like Particles (ALPs) from all past core-collapse supernovae (SNe) would lead to a diffuse flux with energies ${\mathcal O}(50)$ MeV. We use this to constrain ALPs featuring couplings to photons and to nucleons. ALPs coupled only to photons are produced in the SN core via the Primakoff process, and then converted into gamma rays in the Galactic magnetic field. We set a bound on $g_{a\gamma} \lesssim 5 \times 10^{-10}~{\rm GeV}^{-1}$ for $m_a \lesssim 10^{-11}~{\rm eV}$, using recent measurements of the diffuse gamma-ray flux observed by the Fermi-LAT telescope. However, if ALPs couple also with nucleons, their production rate in SN can be considerably enhanced due to the ALPs nucleon-nucleon bremsstrahlung process. Assuming the largest ALP-nucleon coupling phenomenologically allowed, bounds on the diffuse gamma-ray flux lead to a much stronger $g_{a\gamma} \lesssim 6 \times 10^{-13}~{\rm GeV}^{-1}$ for the same mass range. If ALPs are heavier than $\sim$ keV, the decay into photons becomes significant, leading again to a diffuse gamma-ray flux. In the case of only photon coupling, we find, e.g. $g_{a\gamma} \lesssim 5 \times 10^{-11}~{\rm GeV}^{-1}$ for $m_a \sim 5~{\rm keV}$. Allowing for a (maximal) coupling to nucleons, the limit improves to the level of $g_{a\gamma} \lesssim 10^{-19}~{\rm GeV}^{-1}$ for $m_a \sim 20~{\rm MeV}$, which represents the strongest constraint to date., Comment: 12 pages, 7 figures. v2: minor changes to match the published version

Published
2020
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13. Nonrelativistic formation of scalar clumps as a candidate for dark matter

Author

Philippe Brax, Patrick Valageas, Jose A. R. Cembranos, 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), and IPARCOS Institute and EMFTEL Department, Universidad Complutense de Madrid

Subjects
Cold dark matter, oscillation: acoustic, 01 natural sciences, 7. Clean energy, General Relativity and Quantum Cosmology, Gravitation, pressure, High Energy Physics - Phenomenology (hep-ph), energy: density, fluid: scalar, Physics, velocity: acoustic, High Energy Physics - Phenomenology, density: perturbation, Quantum electrodynamics, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Baryon acoustic oscillations, self-force, Scalar field, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), constraint, Dark matter, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), resonance: parametric, Instability, nonrelativistic, gravitation: lens, fluctuation: scalar, 0103 physical sciences, soliton: scalar, 010306 general physics, Axion, dark matter: formation, background, 010308 nuclear & particles physics, monodromy, Scalar (physics), Física, tachyon: stability, temperature, redshift, field theory: scalar, axion, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], soliton: mass, nonlinear, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

We propose a new mechanism for the formation of dark matter clumps in the radiation era. We assume that a light scalar field is decoupled from matter and oscillates harmonically around its vacuum expectation value. We include self-interactions and consider the nonrelativistic regime. The scalar dynamics are described by a fluid approach where the fluid pressure depends on both quantum and self-interaction effects. When the squared speed of sound of the scalar fluid becomes negative, an instability arises and the fluctuations of the scalar energy-density field start growing. They eventually become nonlinear and clumps form. Subsequently, the clumps aggregate and reach a universal regime. Afterwards, they play the role of cold dark matter. We apply this mechanism first to a model with a negative quartic term stabilised by a positive self-interaction of order six, and then to axion monodromy, where a subdominant cosine potential corrects a mass term. In the first case, the squared speed of sound becomes negative when the quartic term dominates, leading to a tachyonic instability. For axion monodromy, the instability starts very slowly after the squared speed of sound first becomes negative and then oscillates around zero. Initially the density perturbations perform acoustic oscillations due to the quantum pressure. Eventually, they start growing exponentially due to a parametric resonance. In both scenarios, the scalar-field clumps span a wide range of scales and masses, running from the size of atoms to that of galactic molecular clouds, and from $10^{-3} \, {\rm gram}$ to thousands of solar masses. Because of finite-size effects, both from the source and the lens, these dark matter clumps are far beyond the reach of microlensing observations., 40 pages, 19 figures, published version

Published
2020
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14. Revisiting primordial black hole capture into neutron stars

Author

Peter Tinyakov, Pasquale D. Serpico, Yoann Génolini, 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
Bondi accretion, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Primordial black hole, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, galaxy: halo, star, accretion, 0103 physical sciences, BURSTS, 010306 general physics, COLLAPSE, neutron star, Astrophysics::Galaxy Astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Gravitational wave, dark matter: mass, gravitational radiation: energy loss, Généralités, transmutation, Accretion (astrophysics), Universe, black hole: capture, Stars, Neutron star, 13. Climate action, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics and astroparticle physics
Abstract

Primordial black holes (PBH), produced through a variety of processes in the early universe, could fill galactic halos accounting for a fraction or the totality of the dark matter. In particular, PBH with substellar masses could be captured by stars, start to swallow their material, and eventually turn them into BH, hence originating a peculiar new type of stellar catastrophic event. Here we revisit this process in the most favorable case of PBH capture by neutron stars. We detail a number of novel features in the capture phase, during the settling within the star and mass growth of the PBH, and illustrate some phenomenological consequences. In particular, we point out that in the subsonic regime the PBH drag takes the form of a Bondi accretion. As a result, the onset of the final transmutation of the NS into a stellar sized BH is expected with the PBH seed in slight off-center position. We also compute the gravitational wave energy-loss and signals associated to different phases of the PBH-stellar interaction. In particular, the emission associated to the accretion phase is periodic with a few kHz frequency; in the rare case of a nearby Galactic event and for light PBH, it could constitute a warning of the forthcoming transmutation., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2020
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15. StarTrack predictions of the stochastic gravitational-wave background from compact binary mergers

Author

Tania Regimbau, C. Belczynski, C. Périgois, Tomasz Bulik, Laboratoire d'Annecy de Physique des Particules (LAPP), and 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)

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), gravitational radiation: stochastic, Population, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, Compact star, 01 natural sciences, Omega, General Relativity and Quantum Cosmology, binary: coalescence, 0103 physical sciences, energy: density, Sensitivity (control systems), KAGRA, LIGO, 010306 general physics, education, Physics, LISA, education.field_of_study, 010308 nuclear & particles physics, gravitational radiation: background, Order (ring theory), binary: compact, gravitational radiation detector, Redshift, detector: sensitivity, VIRGO, frequency: low, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Eccentricity (mathematics), Astrophysics and astroparticle physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We model the gravitational-wave background created by double compact objects from isolated binary evolution across cosmic time using the \textbf{\textit{StarTrack}} binary population code. We include population I/II stars as well as metal-free population III stars. Merging and non-merging double compact object binaries are taken into account. In order to model the low frequency signal in the band of the space antenna LISA, we account for the evolution of the redshift and the eccentricity. We find an energy density of $\Omega_{GW} \sim 1.0 \times 10^{-9}$ at the reference frequency of 25 Hz for population I/II only, making the background detectable at 3 $\sigma$ after about 7 years of observation with the current generation of ground based detectors, such as LIGO, Virgo and Kagra, operating at design sensitivity. The contribution from population III is one order of magnitude below the population I/II for the total background, but dominates the residual background, after detected sources have been removed, in 3G detectors. It modifies the shape of the spectrum which starts deviating from the usual power law $\Omega_{GW}(f) \sim f^{2/3}$ after $\sim 10$ Hz. The contribution from the population of non merging binaries, on the other hand, is negligible, being orders of magnitude below. Finally, we observe that the eccentricity has no impact in the frequency band of LISA or ground based detectors., Comment: new version: 15 pages, 5 figures, 3 tables, published in PRD

Published
2020
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16. Electroweak strings with dark scalar condensates and their stability

Author

Péter Forgács, Árpád Lukács, Laboratoire de Mathématiques et Physique Théorique (LMPT), Centre National de la Recherche Scientifique (CNRS)-Université de Tours, Université de Tours (UT)-Centre National de la Recherche Scientifique (CNRS), and Université de Tours-Centre National de la Recherche Scientifique (CNRS)

Subjects
High Energy Physics - Theory, Particle physics, Spontaneous symmetry breaking, Scalar (mathematics), Dark matter, 01 natural sciences, Instability, Computer Science::Digital Libraries, dark matter, 0103 physical sciences, Gauge theory, 010306 general physics, cosmic string, Physics, electroweak interaction: mixing angle, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], condensation: scalar, Electroweak interaction, High Energy Physics::Phenomenology, spontaneous symmetry breaking, stability, Cosmic string, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], gauge field theory: U(1), mixing: kinetic, Astrophysics and astroparticle physics
Abstract

The stability of "visible" electroweak-type cosmic strings is investigated in an extension of the Standard Model (SM) by a minimal dark sector, consisting of a U(1) gauge field, broken spontaneously by a scalar. The "visible" and dark sectors are coupled through a Higgs-portal and a gauge-kinetic mixing term. It is found that strings whose core is "filled" with a dark scalar condensate exhibit better stability properties than their analogues in the SM, when the electroweak mixing angle is close to $\theta_{\rm W}=\pi/2$. They become unstable as one lets $\theta_{\rm W}$ approach its physical value. The instability mechanism appears to be a $W$-boson condensation mechanism found in previous studies on the stability of electroweak strings., Comment: 9 figures

Published
2020
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17. Detecting the anisotropic astrophysical gravitational wave background in the presence of shot noise through cross-correlations

Author

Pedro G. Ferreira, David Alonso, Giulia Cusin, Cyril Pitrou, 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
High Energy Physics - Theory, data analysis method, noise, gravitational radiation: anisotropy, Physics::General Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Gravitational-wave observatory, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics, power spectrum, 01 natural sciences, General Relativity and Quantum Cosmology, Gravitational wave background, 0103 physical sciences, Range (statistics), [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Sensitivity (control systems), numerical calculations, 010306 general physics, Anisotropy, Instrumentation and Methods for Astrophysics (astro-ph.IM), Physics, background: anisotropy, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], 010308 nuclear & particles physics, Gravitational wave, gravitational radiation: background, gravitational radiation, Shot noise, sensitivity, Astrophysics - Astrophysics of Galaxies, Galaxy, detector: sensitivity, observatory, Automatic Keywords, High Energy Physics - Theory (hep-th), Astrophysics of Galaxies (astro-ph.GA), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, Astrophysics - Instrumentation and Methods for Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

The spatial and temporal discreteness of gravitational wave sources leads to shot noise that may, in some regimes, swamp any attempts at measuring the anisotropy of the gravitational wave background. Cross-correlating a gravitational wave background map with a sufficiently dense galaxy survey can alleviate this issue, and potentially recover some of the underlying properties of the gravitational wave background. We quantify the shot noise level and we explicitly show that cross-correlating the gravitational wave background and a galaxy catalog improves the chances of a first detection of the background anisotropy with a gravitational wave observatory operating in the frequency range (10Hz,100Hz), given sufficient sensitivity., 8 pages, 1 figure

Published
2020
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18. Neutron flux and spectrum in the Dresden Felsenkeller underground facility studied by moderated $^3$He counters

Author

Grieger, M., Hensel, T., Agramunt, J., Bemmerer, D., Degering, D., Dillmann, I., Fraile, L. M., Jordan, D., K��ster, U., Marta, M., M��ller, S. E., Sz��cs, T., Ta��n, J. L., Zuber, K., Institut Laue-Langevin (ILL), and ILL

Subjects
n: background, data analysis method, Physics - Instrumentation and Detectors, shielding, Astrophysics::High Energy Astrophysical Phenomena, n: energy spectrum, FOS: Physical sciences, bibliography, Instrumentation and Detectors (physics.ins-det), [PHYS.NEXP]Physics [physics]/Nuclear Experiment [nucl-ex], sensitivity, High Energy Physics - Experiment, FLUKA, High Energy Physics - Experiment (hep-ex), n: detector, proportional chamber, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], helium: nuclide, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Nuclear Experiment (nucl-ex), entropy, numerical calculations: Monte Carlo, Nuclear Experiment, n: flux, Astrophysics and astroparticle physics
Abstract

Ambient neutrons may cause significant background for underground experiments. Therefore, it is necessary to investigate their flux and energy spectrum in order to devise a proper shielding. Here, two sets of altogether ten moderated $^3$He neutron counters are used for a detailed study of the ambient neutron background in tunnel IV of the Felsenkeller facility, underground below 45 meters of rock in Dresden/Germany. One of the moderators is lined with lead and thus sensitive to neutrons of energies higher than 10 MeV. For each $^3$He counter-moderator assembly, the energy dependent neutron sensitivity was calculated with the FLUKA code. The count rates of the ten detectors were then fitted with the MAXED and GRAVEL packages. As a result, both the neutron energy spectrum from 10$^{-9}$ MeV to 300 MeV and the flux integrated over the same energy range were determined experimentally. The data show that at a given depth, both the flux and the spectrum vary significantly depending on local conditions. Energy integrated fluxes of $(0.61 \pm 0.05)$, $(1.96 \pm 0.15)$, and $(4.6 \pm 0.4) \times 10^{-4}$ cm$^{-2}$ s$^{-1}$, respectively, are measured for three sites within Felsenkeller tunnel IV which have similar muon flux but different shielding wall configurations. The integrated neutron flux data and the obtained spectra for the three sites are matched reasonably well by FLUKA Monte Carlo calculations that are based on the known muon flux and composition of the measurement room walls., 10 figures, 4 tables; to be published in Phys. Rev. D

Published
2020
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19. Hybrid and quark star matter based on a nonperturbative equation of state

Author

Konstantin Otto, Micaela Oertel, Bernd-Jochen Schaefer, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)-Observatoire de Paris, 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 Paris Diderot - Paris 7 (UPD7)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
Quark, Equation of state, Particle physics, Nuclear Theory, density: fluctuation, pressure: high, High Energy Physics::Lattice, FOS: Physical sciences, nonperturbative, 01 natural sciences, 11.10.Wx, Nuclear Theory (nucl-th), High Energy Physics - Phenomenology (hep-ph), 26.60.Kp, Quark star, 05.10.Cc, mean field approximation, 0103 physical sciences, Functional renormalization group, neutron star, 010306 general physics, equation of state, High Energy Astrophysical Phenomena (astro-ph.HE), quark: matter, Physics, hybrid, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Hyperon, Renormalization group, High Energy Physics - Phenomenology, Neutron star, Strange matter, 13. Climate action, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], renormalization group, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics and astroparticle physics
Abstract

With the recent dawn of the multi-messenger astronomy era a new window has opened to explore the constituents of matter and their interactions under extreme conditions. One of the pending challenges of modern physics is to probe the microscopic equation of state (EoS) of cold and dense matter via macroscopic neutron star observations such as their masses and radii. Still unanswered issues concern the detailed composition of matter in the core of neutron stars at high pressure and the possible presence of e.g. hyperons or quarks. By means of a non-perturbative functional renormalization group approach the influence of quantum and density fluctuations on the quark matter EoS in $\beta$-equilibrium is investigated within two- and three-flavor quark-meson model truncations and compared to results obtained with common mean-field approximations where important fluctuations are usually ignored. We find that they strongly impact the quark matter EoS., Comment: 15 pages, 7 figures, 2 tables, to be published in PRD

Published
2020
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20. Constraining primordial black hole masses with the isotropic gamma ray background

Author

Joseph Silk, Jérémy Auffinger, Alexandre Arbey, 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 d'Astrophysique de Paris (IAP), Institut national des sciences de l'Univers (INSU - CNRS)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique de l'ENS Lyon (Phys-ENS), École normale supérieure - Lyon (ENS Lyon)-Centre National de la Recherche Scientifique (CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon, 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), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), and École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL)

Subjects
black hole: rotation, Astrophysics and Astronomy, Cosmology and Nongalactic Astrophysics (astro-ph.CO), background: primordial, gamma ray: background, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Primordial black hole, Astrophysics, 01 natural sciences, dark matter: parametrization, General Relativity and Quantum Cosmology, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, black hole: Schwarzschild, 010306 general physics, Particle Physics - Phenomenology, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, radiation: Hawking, Isotropy, Gamma ray, hep-ph, black hole: mass, High Energy Physics - Phenomenology, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Kerr, astro-ph.CO, Monochromatic color, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Schwarzschild radius, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics, Hawking radiation
Abstract

Primordial black holes can represent all or most of the dark matter in the window $10^{17}-10^{22}\,$g. Here we present an extension of the constraints on PBHs of masses $10^{13}-10^{18}\,$g arising from the isotropic diffuse gamma ray background. Primordial black holes evaporate by emitting Hawking radiation that should not exceed the observed background. Generalizing from monochromatic distributions of Schwarzschild black holes to extended mass functions of Kerr rotating black holes, we show that the lower part of this mass window can be closed for near-extremal black holes., Comment: 5 pages, 3 figures, ERRATUM corrected in Fig. 4

Published
2020
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21. Equilibrium axisymmetric halo model for the Milky Way and its implications for direct and indirect dark matter searches

Author

Mihael Petač, Laboratoire Univers et Particules de Montpellier (LUPM), 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
Milky Way, Dark matter, FOS: Physical sciences, Astrophysics, dark matter: density, 01 natural sciences, Bayesian, flux: time dependence, symmetry: axial, anisotropy: velocity, High Energy Physics - Experiment, dark matter: coupling, High Energy Physics - Experiment (hep-ex), phase space, High Energy Physics - Phenomenology (hep-ph), near detector, 0103 physical sciences, conservation law, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], Sensitivity (control systems), 010306 general physics, halo: rotation, Physics, 010308 nuclear & particles physics, dark matter: mass, Galactic Center, scattering: operator, Relative velocity, Coupling (probability), sensitivity, Astrophysics - Astrophysics of Galaxies, Baryon, High Energy Physics - Phenomenology, modulation, halo: model, annihilation, dark matter: heavy, kinematics, Astrophysics of Galaxies (astro-ph.GA), [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], direct detection, Halo, dark matter: velocity, galaxy, velocity dependence, numerical calculations: Monte Carlo, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

We for the first time provide self-consistent axisymmetric phase-space distribution models for the Milky Way's dark matter (DM) halo which are carefully matched against the latest kinematic measurements through Bayesian analysis. By using broad priors on the individual galactic components, we derive conservative estimates for the astrophysical factors entering the interpretation of direct and indirect DM searches. While the resulting DM density profiles are in good agreement with previous studies, implying $\rho_\odot \approx 10^{-2} \, M_\odot / \mathrm{pc}^3$, the presence of baryonic disc leads to significant differences in the local DM velocity distribution in comparison with the standard halo model. For direct detection, this implies roughly 30% stronger cross-section limits at DM masses near detectors maximum sensitivity and up to an order of magnitude weaker limits at the lower end of the mass range. Furthermore, by performing Monte-Carlo simulations for the upcoming DARWIN and DarkSide-20k experiments, we demonstrate that upon successful detection of heavy DM with coupling just below the current limits, the carefully constructed axisymmetric models can eliminate bias and reduce uncertainties by more then 50% in the reconstructed DM coupling and mass, but also help in a more reliable determination of the scattering operator. Furthermore, the velocity anisotropies induced by the baryonic disc can lead to significantly larger annual modulation amplitude and sizable differences in the directional distribution of the expected DM-induced events. For indirect searches, we provide the differential $J$-factors and compute several moments of the relative velocity distribution that are needed for predicting the rate of velocity-dependent annihilations. However, we find that accurate predictions are still hindered by large uncertainties regarding the DM distribution near the galactic center., Comment: Article consists of 44 pages, 15 figures. We additionally provide the tabulated values of astrophysical factors (in total 18 files) obtained in this work

Published
2020
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22. Peculiar acceleration of stellar-origin black hole binaries: Measurement and biases with LISA

Author

Antoine Klein, Chiara Caprini, Enrico Barausse, Nicola Tamanini, Camille Bonvin, 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), 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), 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), 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
coalescence, long-lived, Astrophysics, 01 natural sciences, General Relativity and Quantum Cosmology, star: cluster, accretion, LIGO, [PHYS]Physics [physics], Physics, lifetime, education.field_of_study, Hubble constant, formation, Astrophysics::Instrumentation and Methods for Astrophysics, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - Instrumentation and Methods for Astrophysics, Active galactic nucleus, Astrophysics::High Energy Astrophysical Phenomena, Population, astro-ph.IM, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], AGN, 010306 general physics, education, Luminosity distance, Instrumentation and Methods for Astrophysics (astro-ph.IM), Astrophysics::Galaxy Astrophysics, LISA, 010308 nuclear & particles physics, Gravitational wave, nucleus, acceleration, black hole: mass, redshift, calibration, Galaxy, Redshift, VIRGO, frequency: low, black hole: binary, 13. Climate action, gravitational radiation: emission, galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Hubble's law, Astrophysics and astroparticle physics
Abstract

We investigate the ability of the Laser Interferometer Space Antenna (LISA) to measure the center of mass acceleration of stellar-origin black hole binaries emitting gravitational waves. Our analysis is based on the idea that the acceleration of the center of mass induces a time variation in the redshift of the gravitational wave, which in turn modifies its waveform. We confirm that while the cosmological acceleration is too small to leave a detectable imprint on the gravitational waveforms observable by LISA, larger peculiar accelerations may be measurable for sufficiently long lived sources. We focus on stellar mass black hole binaries, which will be detectable at low frequencies by LISA and near coalescence by ground based detectors. These sources may have large peculiar accelerations, for instance, if they form in nuclear star clusters or in AGN accretion disks. If that is the case, we find that in an astrophysical population calibrated to the LIGO-Virgo observed merger rate, LISA will be able to measure the peculiar acceleration of a small but significant fraction of the events if the mission lifetime is extended beyond the nominal duration of 4 years. In this scenario LISA will be able to assess whether black hole binaries form close to galactic centers, particularly in AGN disks, and will thus help discriminate between different formation mechanisms. Although for a nominal 4 years LISA mission the peculiar acceleration effect cannot be measured, a consistent fraction of events may be biased by strong peculiar accelerations which, if present, may imprint large systematic errors on some waveform parameters. In particular, estimates of the luminosity distance could be strongly biased and consequently induce large systematic errors on LISA measurements of the Hubble constant with stellar mass black hole binaries., Comment: 21 pages, 2 figures, 3 tables; v2 matches published version

Published
2020
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23. Dark matter relic density from conformally or disformally coupled light scalars

Author

Philippe Brax, Sebastian Trojanowski, Carsten van de Bruck, Institut de Physique Théorique - UMR CNRS 3681 (IPHT), and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)

Subjects
Particle physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Dark matter, Scalar (mathematics), FOS: Physical sciences, Conformal map, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, mass: scale, High Energy Physics - Phenomenology (hep-ph), conformal, 0103 physical sciences, Thermal, Mass scale, dark matter: scalar, 010306 general physics, freeze-out: thermal, fermion: model, media_common, Physics, Large Hadron Collider, 010308 nuclear & particles physics, dark matter: relic density, WIMP: relic density, WIMP: stability, Universe, field theory: scalar, High Energy Physics - Phenomenology, CERN LHC Coll, Weakly interacting massive particles, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], history, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

Thermal freeze-out is a prominent example of dark matter (DM) production mechanism in the early Universe that can yield the correct relic density of stable weakly interacting massive particles (WIMPs). At the other end of the mass scale, many popular extensions of the Standard Model predict the existence of ultra-light scalar fields. These can be coupled to matter, preferentially in a universal and shift-symmetry-preserving way. We study the impact of such conformal and disformal couplings on the relic density of WIMPs, without introducing modifications to the thermal history of the Universe. This can either result in an additional thermal contribution to the DM relic density or suppress otherwise too large abundances compared to the observed levels. In this work, we assume that the WIMPs only interact with the standard model via the light scalar portal. We use simple models of fermionic or scalar DM, although a similar discussion holds for more sophisticated scenarios, and predict that their masses should be between $\sim 100~\textrm{GeV}$ and several $\textrm{TeV}$ to comply both with the DM abundance and current bounds on the couplings of the light scalars to matter at the LHC. Future searches will tighten these bounds., 17 pages, 3 figures

Published
2020
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24. High-energy neutrinos from cosmic ray interactions in the Local Bubble

Author

Dmitri Semikoz, M. Kachelrieß, M. Bouyahiaoui, 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), 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), 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), 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
High energy, gamma ray: background, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Flux, Cosmic ray, Astrophysics, cosmic radiation: interaction, Vela, 01 natural sciences, GLAST, neutrino: flux, IceCube, 0103 physical sciences, 010306 general physics, muon: flux, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Muon, 010308 nuclear & particles physics, bubble, High Energy Physics::Phenomenology, neutrino: UHE, cascade, Local Bubble, High Energy Physics::Experiment, galaxy, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], cosmic radiation: flux, Astrophysics and astroparticle physics
Abstract

A surprisingly large flux of extraterrestrial high-energy neutrinos was discovered by the IceCube experiment. While the flux of muon neutrinos with energies $E>100$ TeV is consistent with the extragalactic gamma-ray background (EBL) determined by Fermi-LAT, the softer component of the cascade neutrino flux at $E300$ GeV was found in the data of Fermi-LAT. The gamma-ray excess at TeV energies and the neutrino excess at $E, 9 pages, 10 figures; v2: added discussion of the importance of other sources

Published
2020
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25. GPU-accelerated massive black hole binary parameter estimation with LISA

Author

A. J. K. Chua, Stanislav Babak, Michael L. Katz, Shane L. Larson, Sylvain Marsat, 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
binary: mass, higher-order, Computation, Binary number, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Monte Carlo: Markov chain, symbols.namesake, binary: spin, 0103 physical sciences, black hole, 010306 general physics, Physics, [PHYS]Physics [physics], LISA, Spins, 010308 nuclear & particles physics, Estimation theory, statistical analysis: Bayesian, spin: alignment, Redshift, gravitational radiation detector, Computational physics, Black hole, Fourier transform, Orders of magnitude (time), black hole: binary, injection, black hole: coalescence, gravitational radiation: emission, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], mass ratio, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

The Laser Interferometer Space Antenna (LISA) is slated for launch in the early 2030s. A main target of the mission is massive black hole binaries that have an expected detection rate of $\sim20$ yr$^{-1}$. We present a parameter estimation analysis for a variety of massive black hole binaries. This analysis is performed with a graphics processing unit (GPU) implementation comprising the phenomhm waveform with higher-order harmonic modes and aligned spins; a fast frequency-domain LISA detector response function; and a GPU-native likelihood computation. The computational performance achieved with the GPU is shown to be 500 times greater than with a similar CPU implementation, which allows us to analyze full noise-infused injections at a realistic Fourier bin width for the LISA mission in a tractable and efficient amount of time. With these fast likelihood computations, we study the effect of adding aligned spins to an analysis with higher-order modes by testing different configurations of spins in the injection, as well as the effect of varied and fixed spins during sampling. Within these tests, we examine three different binaries with varying mass ratios, redshifts, sky locations, and detector-frame total masses ranging over three orders of magnitude. We discuss varied correlations between the total masses and mass ratios; unique spin posteriors for the larger mass binaries; and the constraints on parameters when fixing spins during sampling, allowing us to compare to previous analyses that did not include aligned spins., Comment: 27 pages, 13 figures

Published
2020
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26. Ghostly Galaxies as Solitons of Bose-Einstein Dark Matter

Author

Tom Broadhurst, Ivan De Martino, Hoang Nhan Luu, Henry Sze-hoi Tye, George F. Smoot, Paris Centre for Cosmological Physics (PCCP), Université Paris Diderot - Paris 7 (UPD7), 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), 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 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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Physics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), 010308 nuclear & particles physics, Milky Way, Dark matter, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Astrophysics - Astrophysics of Galaxies, Galaxy, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Galaxy formation and evolution, 010306 general physics, Low Mass, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Axion, Astrophysics::Galaxy Astrophysics, Boson, Dwarf galaxy, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

The large dark cores of common dwarf galaxies are unexplained by the standard heavy particle interpretation of dark matter. This puzzle is exacerbated by the discovery of a very large but barely visible, dark matter dominated galaxy Antlia II orbiting the Milky Way, uncovered by tracking star motions with the {\t Gaia} satellite. Although Antlia II has a low mass, its visible radius is more than double any known dwarf galaxy, with an unprecedentedly low density core. We show that Antlia II favors dark matter as a Bose-Einstein condensate, for which the ground state is a stable soliton with a core radius given by the de Broglie wavelength. The lower the galaxy mass, the larger the de Broglie wavelength, so the least massive galaxies should have the widest soliton cores of lowest density. An ultra-light boson of $m_\psi \sim 1.1 \times10^{-22}$ eV, accounts well for the large size and slowly moving stars within Antlia II, and agrees with boson mass estimates derived from the denser cores of more massive dwarf galaxies. For this very light boson, Antlia II is close to the lower limiting Jeans scale for galaxy formation permitted by the Uncertainty Principle, so other examples are expected but none significantly larger in size. This simple explanation for the puzzling dark cores of dwarf galaxies implies dark matter as an ultra-light boson, such as an axion generic in String Theory., Comment: 9 pages, 5 figure. Accepted for publication on Physical Review D

Published
2020
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27. LHAASO telescope sensitivity to diffuse gamma-ray signals from the Galaxy

Author

Andrii Neronov, Dmitri Semikoz, 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
Astrophysics::High Energy Astrophysical Phenomena, Dark matter, Flux, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic radiation: interaction, 01 natural sciences, IceCube, 0103 physical sciences, gamma ray: flux, 010306 general physics, Physics, cosmic radiation: spectrum, 010308 nuclear & particles physics, dark matter: decay, Gamma ray, Astrophysics::Instrumentation and Methods for Astrophysics, sensitivity, Galaxy, Interstellar medium, gamma ray: VHE, cosmic radiation: galaxy, Neutrino, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy (signal processing), Astrophysics and astroparticle physics
Abstract

We estimate the sensitivity of LHAASO telescope for the large angular scale diffuse $\ensuremath{\gamma}$-ray flux in multi-TeV---multi-PeV energy range. We discuss possible sources of the signal in this energy range including the guaranteed flux from cosmic ray interactions in the interstellar medium and possible flux from decaying dark matter. We show that LHAASO will be able to detect the diffuse cosmic ray induced $\ensuremath{\gamma}$-ray flux up to high Galactic latitude regions thus providing firm identification of the Galactic cosmic ray component of the astrophysical neutrino signal detected by IceCube and clarification of the nature of the knee feature of the cosmic ray spectrum. Comparing the diffuse flux sensitivity with the diffuse $\ensuremath{\gamma}$-ray flux expected from the dark matter decays, we show LHAASO will be able to detect the $\ensuremath{\gamma}$-ray signal from dark matter particles of PeV--EeV mass decaying on the time scale up to $3\ifmmode\times\else\texttimes\fi{}{10}^{29}\text{ }\text{ }\mathrm{s}$.

Published
2020
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28. Fast Neutrino Flavor Conversion Modes in Multidimensional Core-collapse Supernova Models: the Role of the Asymmetric Neutrino Distributions

Author

Tomoya Takiwaki, Sajad Abbar, Huaiyu Duan, Maria Cristina Volpe, Kohsuke Sumiyoshi, 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), 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), 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), 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
High Energy Physics - Theory, Particle physics, Astrophysics::High Energy Astrophysical Phenomena, protoneutron star, multipole, FOS: Physical sciences, Neutrino decoupling, 01 natural sciences, Boltzmann equation, symbols.namesake, 0103 physical sciences, 010306 general physics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, neutrino: gas, 010308 nuclear & particles physics, [PHYS.HTHE]Physics [physics]/High Energy Physics - Theory [hep-th], High Energy Physics::Phenomenology, supernova: model, crossing, Type II supernova, Supernova, collapse, High Energy Physics - Theory (hep-th), Boltzmann constant, neutrino: flavor, symbols, High Energy Physics::Experiment, Neutrino, higher-dimensional, Astrophysics - High Energy Astrophysical Phenomena, Multipole expansion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], neutrino: angular distribution, neutrino: decoupling, Astrophysics and astroparticle physics
Abstract

A dense neutrino gas, such as the one anticipated in the supernova environment, can experience fast neutrino flavor conversions on scales much shorter than those expected in vacuum probably provided that the angular distributions of $\nu_e$ and $\bar\nu_e$ cross each other. We perform a detailed investigation of the neutrino angular distributions obtained by solving the Boltzmann equations for fixed matter profiles of some representative snapshots during the post-bounce phase of core-collapse supernovae in multidimensional calculations of an $11.2\mathrm{M}_{\odot}$ and a $27\mathrm{M}_{\odot}$ progenitor models. Although the $11.2\mathrm{M}_{\odot}$ model features $\nu_e - \bar\nu_e$ angular crossings and the associated fast modes at different time snapshots, the $27\mathrm{M}_{\odot}$ model does not show any crossings within the decoupling region. We show that this can be understood by studying the multipole components of the neutrino distributions. In fact, there is a higher chance for the occurrence of $\nu_e - \bar\nu_e$ angular crossings for the zones where the multipole components of the neutrino distributions are strong enough. We also show that there can exist more than one crossings between the angular distributions of $\nu_e$ and $\bar{\nu}_e$. In addition, apart from the crossings within the neutrino decoupling region, there is a class of $\nu_e-\bar\nu_e$ angular crossings which appears very deep inside the proto-neutron star., Comment: Version accepted in PRD

Published
2020
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29. Primordial Rotating Black Holes

Author

J. A. de Freitas Pacheco, Joseph Silk, Joseph Louis LAGRANGE (LAGRANGE), Université Côte d'Azur (UCA)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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
black hole: rotation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Primordial black hole, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, dark matter: density, 01 natural sciences, General Relativity and Quantum Cosmology, accretion, 0103 physical sciences, 010306 general physics, media_common, Physics, preheating, 010308 nuclear & particles physics, formation, black hole: mass, Universe, Accretion (astrophysics), quantum gravity, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Quantum gravity, Astrophysics::Earth and Planetary Astrophysics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], black hole: primordial, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

Primordial black holes formed in an early post-inflation matter-dominated epoch during preheating provide a novel pathway for a source of the dark matter that utilizes known physics in combination with plausible speculations about the role of quantum gravity. Two cases are considered here: survival of Planck-scale relics and an early universe accretion scenario for formation of primordial black holes of asteroid-scale masses., 7 pages, PRD submitted

Published
2020
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30. Detecting the brightest HAWC sources with IceCube in the upcoming years

Author

Viviana Niro, 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
Astrophysics::High Energy Astrophysical Phenomena, Hadron, Flux, FOS: Physical sciences, Astrophysics, 01 natural sciences, IceCube, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, TeV, 010306 general physics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Sigma, Running time, flux, observatory, High Energy Physics - Phenomenology, gamma ray, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Neutrino, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, HAWC, Energy (signal processing), Astrophysics and astroparticle physics
Abstract

Among the gamma-ray sources detected by the HAWC observatory, we consider in details in this work the gamma-ray sources eHWC J1907+063 and eHWC J2019+368. These two sources belong to the three most luminous sources detected by HAWC, with emission above 100 TeV. In addition to those, we have considered also a source for which IceCube currently report an excess in neutrinos, the 2HWC J1857+027 source. For these sources, we show the prediction for neutrinos at the IceCube detector. Moreover, we present the calculation of the statistical significance, considering 10 and 20 years of running time, and we comment on the current results reported by the collaboration. We found that a detection at 3$\sigma$ or more should be within reach of the next decade for the sources eHWC J1907+063 and eHWC J2019+368. Instead, the detection at about 3$\sigma$ of the 2HWC J1857+027 source will depend on the specific value of the flux, on the extension of the source and on the cut-off energy., Comment: 16 pages, 8 figures, 2 tables

Published
2020
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31. Science with the TianQin observatory: Preliminary result on extreme-mass-ratio inspirals

Author

Yi-Ming Hu, Jianwei Mei, Huimin Fan, Alberto Sesana, Enrico Barausse, Tie-Guang Zi, Xuefeng Zhang, Jian-dong Zhang, 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), Fan, H, Hu, Y, Barausse, E, Sesana, A, Zhang, J, Zhang, X, Zi, T, and Mei, J

Subjects
FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Compact star, 01 natural sciences, General Relativity and Quantum Cosmology, localization, Gravitation, Settore FIS/05 - Astronomia e Astrofisica, Observatory, strong field, 0103 physical sciences, black hole, 010306 general physics, capture, Luminosity distance, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Mass ratio, redshift, Redshift, gravitational radiation detector, moment, Black hole, observatory, gravitation, Quadrupole, network, fractional, Kerr, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], mass ratio, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

Systems consisting of a massive black hole and a stellar-origin compact object (CO), known as extreme-mass-ratio inspirals (EMRIs), are of great significance for space-based gravitational-wave detectors, as they will allow for testing gravitational theories in the strong field regime, and for checking the validity of the black hole no-hair theorem. In this work, we present a calculation of the EMRI rate and parameter estimation capabilities of the TianQin observatory, for various astrophysical models for these sources. We find that TianQin can observe EMRIs involving COs with mass of 10$M_\odot$ up to redshift $\sim2$. We also find that detections could reach tens or hundreds per year in the most optimistic astrophysical scenarios. Intrinsic parameters are expected to be recovered to within fractional errors of $\sim 10^{-6}$, while typical errors on the luminosity distance and sky localization are 10% and 10 deg$^2$, respectively. TianQin observation of EMRIs can also constrain possible deviations from the Kerr quadrupole moment to within fractional errors $\lesssim10^{-4}$. We also find that a network of multiple detectors would allow for improvements in both detection rates (by a factor $\sim 1.5$ -$3$) and in parameter estimation precision (20-fold improvement for the sky localization and fivefold improvement for the other parameters)., Comment: 13 pages, 5 figures

Published
2020
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32. Signatures of secondary leptons in radio-neutrino detectors in ice

Author

Daniel García-Fernández, Anna Nelles, and Christian Glaser

Subjects
background [atmosphere], Particle physics, lepton: secondary, lepton, Physics::Instrumentation and Detectors, air, Astrophysics::High Energy Astrophysical Phenomena, ice, FOS: Physical sciences, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, interaction [lepton], lepton: interaction, muon, atmosphere: background, ddc:530, secondary [lepton], detector [neutrino], neutrino: interaction, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), radio wave, Muon, showers: atmosphere, interaction [neutrino], Detector, High Energy Physics::Phenomenology, sensitivity, Air shower, neutrino: detector, Cover (topology), Neutrino detector, cosmic radiation, High Energy Physics::Experiment, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, signature, Lepton, Astrophysics and astroparticle physics, atmosphere [showers]
Abstract

Physical review / D 102(8), 083011 (2020). doi:10.1103/PhysRevD.102.083011, The detection of the radio emission following a neutrino interaction in ice is a promising technique to obtain significant sensitivities to neutrinos with energies above Petaelectronvolts (10$^{15}$ eV). The detectable radio emission stems from particle showers in the ice. So far, detector simulations have considered only the radio emission from the primary interaction of the neutrino. For this study, existing simulation tools have been extended to cover secondary interactions from muons and taus. We find that secondary interactions of both leptons add up to 25% to the effective volume of neutrino detectors. Also, muon and tau neutrinos can create several detectable showers, with the result that double signatures do not constitute an exclusive signature for tau neutrinos. We also find that the background of atmospheric muons from cosmic rays is non-negligible for in-ice arrays and that an air shower veto should be considered helpful for radio detectors., Published by Inst.302363, Melville, NY

Published
2020
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33. Establishing the significance of continuous gravitational-wave detections from known pulsars

Author

S. Mastrogiovanni, Maximiliano Isi, O. J. Piccinni, Matthew Pitkin, 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), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP)

Subjects
data analysis method, Gaussian, modulation: phase, FOS: Physical sciences, detector: noise, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, General Relativity and Quantum Cosmology, Amplitude modulation, symbols.namesake, Pulsar, statistical analysis, 0103 physical sciences, numerical methods, 010306 general physics, numerical calculations, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Noise (signal processing), Gravitational wave, Detector, gravitational radiation: background, noise: non-Gaussianity, gravitational radiation, binary: compact, wave: model, gravitational radiation: emission, Orbital motion, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Phase modulation, Algorithm, Astrophysics and astroparticle physics
Abstract

We present a method for assigning a statistical significance to detection candidates in targeted searches for continuous gravitational waves from known pulsars, without assuming the detector noise is Gaussian and stationary. We take advantage of the expected Doppler phase modulation of the signal induced by Earth's orbital motion, as well as the amplitude modulation induced by Earth's spin, to effectively blind the search to real astrophysical signals from a given location in the sky. We use this "sky-shifting" to produce a large number of noise-only data realizations to empirically estimate the background of a search and assign detection significances, in a similar fashion to the use of timeslides in searches for compact binaries. We demonstrate the potential of this approach by means of simulated signals, as well as hardware injections into real detector data. In a study of simulated signals in non-Gaussian noise, we find that our method outperforms another common strategy for evaluating detection significance. We thus demonstrate that this and similar techniques have the potential to enable a first confident detection of continuous gravitational waves., Comment: 17 pages, 10 figures

Published
2020
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34. Inference of proto-neutron star properties from gravitational-wave data in core-collapse supernovae

Author

Alejandro Torres-Forné, Patricio Maturana-Russel, Pablo Cerdá-Durán, Renate Meyer, José A. Font, Martin Obergaulinger, Nelson Christensen, Marie-Anne Bizouard, Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
noise, Gravitational-wave observatory, gravitational radiation: stochastic, Astrophysics::High Energy Astrophysical Phenomena, protoneutron star, Degrees of freedom (physics and chemistry), FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), 01 natural sciences, 7. Clean energy, General Relativity and Quantum Cosmology, Einstein Telescope, effect: nonlinear, supernova, 0103 physical sciences, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], LIGO, numerical calculations, 010306 general physics, Instrumentation and Methods for Astrophysics (astro-ph.IM), equation of state, Physics, Solar mass, mass: solar, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, oscillation, gravitational radiation detector, gravitation: collapse, detector: sensitivity, star: massive, Supernova, Stars, wave: model, VIRGO, 13. Climate action, gravitational radiation: emission, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], galaxy, Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics and astroparticle physics
Abstract

The eventual detection of gravitational waves from core-collapse supernovae (CCSN) will help improve our current understanding of the explosion mechanism of massive stars. The stochastic nature of the late post-bounce gravitational wave signal due to the non-linear dynamics of the matter involved and the large number of degrees of freedom of the phenomenon make the source parameter inference problem very challenging. In this paper we take a step towards that goal and present a parameter estimation approach which is based on the gravitational waves associated with oscillations of proto-neutron stars (PNS). Numerical simulations of CCSN have shown that buoyancy-driven g-modes are responsible for a significant fraction of the gravitational wave signal and their time-frequency evolution is linked to the physical properties of the compact remnant through universal relations, as demonstrated in [1]. We use a set of 1D CCSN simulations to build a model that relates the evolution of the PNS properties with the frequency of the dominant g-mode, which is extracted from the gravitational-wave data using a new algorithm we have developed for our study. The model is used to infer the time evolution of a combination of the mass and the radius of the PNS. The performance of the method is estimated employing simulations of 2D CCSN waveforms covering a progenitor mass range between 11 and 40 solar masses and different equations of state. Considering signals embedded in Gaussian gravitational wave detector noise, we show that it is possible to infer PNS properties for a galactic source using Advanced LIGO and Advanced Virgo data at design sensitivities. Third generation detectors such as Einstein Telescope and Cosmic Explorer will allow to test distances of ${\cal O}(100\, {\rm kpc})$.

Published
2020
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35. Signatures of secondary leptons in radio-neutrino detectors in ice

Author

García-Fernández, Daniel, Nelles, Anna, and Glaser, Christian

Subjects
radio wave, lepton: secondary, showers: atmosphere, lepton, Physics::Instrumentation and Detectors, air, Astrophysics::High Energy Astrophysical Phenomena, High Energy Physics::Phenomenology, ice, Astrophysics::Cosmology and Extragalactic Astrophysics, sensitivity, lepton: interaction, neutrino: detector, cosmic radiation, muon, atmosphere: background, High Energy Physics::Experiment, neutrino: interaction, signature, Astrophysics and astroparticle physics
Abstract

The detection of the radio emission following a neutrino interaction in ice is a promising technique to obtain significant sensitivities to neutrinos with energies above Petaelectronvolts (1015 eV). The detectable radio emission stems from particle showers in the ice. So far, detector simulations have considered only the radio emission from the primary interaction of the neutrino. For this study, existing simulation tools have been extended to cover secondary interactions from muons and taus. We find that secondary interactions of both leptons add up to 25% to the effective volume of neutrino detectors. Also, muon and tau neutrinos can create several detectable showers, with the result that double signatures do not constitute an exclusive signature for tau neutrinos. We also find that the background of atmospheric muons from cosmic rays is non-negligible for in-ice arrays and that an air shower veto should be considered helpful for radio detectors.

Published
2020
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36. GW190412: Observation of a binary-black-hole coalescence with asymmetric masses

Author

T. D. Abbott, A. Królak, E. A. Muñiz, M. C. Heintze, Benno Willke, L. Rei, L. McCuller, X. Liu, T. B. Littenberg, B. D'Angelo, B. Edelman, V. Gayathri, S. Di Pace, S. Walsh, Miriam Cabero, Alessandra Buonanno, R. Metzdorff, Gabrielle Allen, C. J. Moore, A. S. Sengupta, M. J. Yap, S. H. R. Yuen, O. de Varona, M. Fishbach, R. Benkel, P. Fulda, Antoine Heidmann, E. A. Chase, M. Bejger, S. Morisaki, F. Marion, K. Toland, R. Tenorio, N. A. Holland, J. B. Camp, R. Macas, D. Estevez, M. Gosselin, Y. K. Lecoeuche, F. Clara, R. G. Ormiston, R. Taylor, Y. Ma, D. Schaetzl, M. Phelps, N. Gohlke, G. Valdes, S. E. Dwyer, J. Blackman, M. Haney, Archisman Ghosh, Patrick Brady, T. J. Cullen, D. J. Vine, R. Passaquieti, C. Wong, Fabien Kéfélian, J. H. Hough, N. Kijbunchoo, S. R. Thondapu, R. Chierici, A. Grimaldi, O. Durante, F. Meylahn, B. B. Lane, Carl-Johan Haster, C. Kimball, L. Rolland, Jade Powell, D. Mukherjee, D. J. Stops, V. Mangano, Fabrizio Barone, M. T. Hübner, N. Man, F. J. Hayes, T. Dal Canton, H. K. Gulati, I. Magaña Hernandez, C. McIsaac, N. De Lillo, S. Banagiri, Sascha Husa, J. Li, A. K. Zadrożny, H. Estelles, S. Galaudage, A. M. Baer, P. Leaci, F. Feng, K. R. Corley, D. J. McManus, X. Li, H. Fong, Nergis Mavalvala, Jerome Degallaix, A. Mullavey, D. Steinmeyer, C. Casentini, S. Anand, G. D. Hammond, Javed Rana, Stefan Grimm, V. Kondrashov, O. A. Hannuksela, B. F. Neil, P. Weßels, J. A. Clark, M. Di Giovanni, A. W. Jones, R. M. Martin, A. Ananyeva, R. De Pietri, N. Letendre, Nikhil Sarin, H. Qi, J. Calderón Bustillo, D. Lumaca, M. Walker, P. J. Veitch, David A. Williams, I. W. Harry, Z. A. Warden, O. Palashov, Rocco Romano, M. Kinley-Hanlon, S. G. Crowder, Jinsook Kim, D. C. Coyne, K. Mason, C. J. Perez, C. K. Cheong, M. Vasúth, Xin Chen, David A. Nichols, M. Mondin, S. Karki, Sean T. McWilliams, F. Piergiovanni, J. C. Mills, A. Di Lieto, M. Saleem, Chang-Hwan Lee, D. E. Cohen, A. M. Holgado, K. G. Arun, D. M. Wilken, F. Aubin, G. Stratta, Jesper Munch, S. Grunewald, T. Vo, F. Wellmann, T. Zhang, K. Merfeld, Thibaut Jacqmin, P. Kumar, R. D. Rodriguez-Soto, Doğa Veske, J. Feicht, C. Messick, M. Delfavero, G. Pagliaroli, A. K. Y. Li, Jonathan Cripe, M. De Laurentis, M. Fitz-Axen, A. Mhaske, R. Bork, M. Sakellariadou, Daniel E. Holz, M. Rizzo, A. Viceré, Yi Chen, B. W. Schulte, T. Mistry, G. Pratten, F. Vetrano, J. R. Smith, R. L. Savage, S. Khan, A. L. Stuver, G. Pillant, B. Patricelli, D. S. Wu, Margaret Millhouse, M. Davier, W. Parker, M. Favata, A. Basti, Ryan N. Lang, M. Fazio, K. Holt, A. S. Ubhi, N. Demos, Francisco Hernandez Vivanco, T. Prestegard, P. J. Easter, L. M. DeMarchi, Chunglee Kim, O. J. Piccinni, A. Cirone, A. A. van Veggel, D. Barta, V. Bossilkov, H. Cao, P. Raffai, Francesco Pannarale, D. Meacher, A. Rocchi, S. Raja, Olivier Minazzoli, Eyal Schwartz, B. Goncharov, M. Razzano, B. Grace, E. Genin, S. M. Aronson, S. McCormick, Aldo Ejlli, Z. Yang, F. Bergamin, N. Mukund, D. Tsuna, Roger Jones, J.-D. Fournier, Eric Thrane, X. Fan, C. Michel, M. Kasprzack, Sarah Caudill, P. Hopkins, Francesco Chiadini, P. Charlton, F. Badaracco, J. G. Rollins, R. M. Magee, Haixing Miao, J. W. Westhouse, H. Ohta, F. Di Giovanni, J. Lee, K. L. Dooley, Aaron Zimmerman, D. Nothard, P. Barneo, N. Singh, Samuele Cortese, Haocun Yu, E. Z. Hamilton, Lisa Barsotti, A. P. Spencer, K. Chakravarti, D. D. Brown, E. Biggs, K. Barkett, R. S. Bankar, S. S. Eikenberry, Marica Valentini, T. Di Girolamo, D. H. Reitze, Y. Setyawati, Vicky Kalogera, O. Halim, M. Tonelli, G. González, J. H. Briggs, M. M. Fejer, Guoying Zhao, I. Cordero-Carrión, H. M. Lee, M. C. Milovich-Goff, Anthony A. Amato, N. van Bakel, E. C. Ferreira, R. K. Lanza, J. D. Merritt, A. Masserot, F. Y. Khalili, J. Zweizig, K. Kawabe, Karan Jani, R. Shink, Gijs Nelemans, F. Nocera, E. D. Hall, Jolien D. E. Creighton, P. Booker, R. Bhandare, A. Bisht, V. Kringel, W. Kastaun, L. Yang, B. C. Pant, K. Ueno, Maximiliano Isi, C. G. Hoy, N. N. Janthalur, E. M. Gretarsson, Ying Guo, Peter Fritschel, P. Godwin, G. Oganesyan, T. A. Callister, Maria Ilaria Del Principe, K. W. Tsang, K. Siellez, J. H. Romie, I. Ferrante, Nicolas Sanchis-Gual, D. Huet, B. D. Lackey, B. L. Swinkels, Z. Frei, T. R. Corbitt, P. Grassia, E. J. Daw, M. Punturo, P. H. Nguyen, S. G. Rosofsky, W. M. Farr, Sebastian Steinlechner, C. A. Rose, C. J. Richardson, M. Agathos, V. Martinez, Soumen Roy, G. Greco, E. Floden, Gianpietro Cagnoli, Andrew Lundgren, W. S. Kim, J. Baird, Rana X. Adhikari, T. Tsutsui, F. Donovan, K. Y. Ng, Stephane Perries, A. Balsamo, S. Khadka, C. I. Torrie, Jan Harms, V. Dattilo, H. S. Cho, G. Moreno, A. Effler, R. DeSalvo, J. Petermann, H. Wittel, J. J. Oh, L. E. Sanchez, J. C. Barayoga, R. Cavalieri, J. Bosveld, Z. Zhou, K. Haughian, Antonio Marquina, Edoardo Milotti, E. Lalande, H. Radkins, S. M. Aston, B. Idzkowski, M. Canepa, T. A. Ferreira, E. M. Santos, W. Z. Korth, O. Schwarm, Geoffrey Lovelace, Satyanarayan Ray Pitambar Mohapatra, P. Rettegno, F. Baldaccini, A. Allocca, M. Nery, A. K. Srivastava, Enrico Calloni, V. Sordini, L. Salconi, D. V. Martynov, R. Goetz, G. S. Wallace, A. Singha, M. Croquette, G. Vedovato, Z. Doctor, J. Gniesmer, R. M. S. Schofield, M. Curylo, J. Jiang, S. Marsat, V. Hui, M. Drago, M. Cho, M. A. Page, Richard J. Oram, Samuel Deléglise, R. Huxford, K. Shukla, E. A. Trail, B. A. Boom, D. Sigg, P. Puppo, F. Cleva, C. Vorvick, J. Bartlett, P. W. F. Forsyth, M. Khursheed, F. Brighenti, Aniello Grado, Andrew Melatos, M. Lorenzini, S. Chung, Ellen S. Howell, I. A. Bilenko, L. Haegel, T. B. Edo, A. Sharma, M. G. Benjamin, Parthanil Roy, F. Linde, Laura Cadonati, M. Zanolin, A. Perreca, S. D. Linker, J. C. Driggers, M. Zevin, S. M. Gaebel, S. R. Mohite, V. D'Emilio, R. Sturani, G. Riemenschneider, K. AultONeal, G. Venugopalan, I. Belahcene, David Keitel, Benjamin J. Owen, D. M. Wysocki, Andrew Mehta, J. F. J. van den Brand, I. A. O. MacMillan, S. Meshkov, N. Krupinski, J. S. Lange, B. E. Ewing, P. A. Altin, M. Stover, S. Miller, E. A. Huerta, K. Prasai, L. Cunningham, B. C. Barish, B. Sassolas, Yang Yang, F. Ohme, Xing-Jiang Zhu, M. Rakhmanov, V. Sipala, L. Naticchioni, R. P. Fisher, Nathan K. Johnson-McDaniel, S. P. Vyatchanin, I. Khan, T. Dietrich, V. B. Adya, Tristan Briant, Chad Hanna, V. Tiwari, G. Carullo, C. Pankow, P. M. Meyers, J. Neilson, D. George, David J. Ottaway, A. Ain, L. Sun, M. Tápai, C. L. Romel, Fiodor Sorrentino, Y. Boetzel, Mark Hannam, Binlei Ding, A. Gupta, A. Lartaux-Vollard, M. Pürrer, O. D. Aguiar, M. Tacca, P. Ehrens, Wolfango Plastino, Seog Oh, A. Cumming, M. Laxen, Martin Hendry, Cecilio García-Quirós, M. C. Díaz, K. Chatziioannou, F. Di Renzo, Suvadeep Bose, T. R. Saravanan, D. Rose, F. Garufi, R. Jaume, R. A. Eisenstein, B. J. J. Slagmolen, C. Di Giorgio, S. Caride, R. Gouaty, J. Hanks, S. E. Gossan, Carlos O. Lousto, H. Masalehdan, Salvatore Vitale, J. Zhang, L. F. Ortega, V. Srivastava, A. Strunk, M. Oliver, Surendra Nadh Somala, M. Fyffe, D. Bersanetti, C. North, R. Schnabel, Thomas Dent, P. Corban, S. J. Cooper, G. H. Ogin, James Whelan, H. Pan, D. Buskulic, A. V. Bhandari, C. Zhao, Alicia M. Sintes, R. Kashyap, Jishnu Suresh, B. L. Pearlstone, R. Fittipaldi, G. D. Meadors, S. W. Ballmer, J. Z. Wang, T. Souradeep, T. Hardwick, Junwei Cao, A. A. Ciobanu, John Veitch, J. Lehmann, B. Rajbhandari, P. Ajith, L. Zhang, T. Zelenova, C. De Rossi, C. Périgois, C. Whittle, M. Masso-Reid, Sheelu Abraham, E. Chassande-Mottin, S. A. Usman, D. Singh, M. Manske, R. A. Mercer, Zhihui Du, G. Ciani, G. Gemme, T. D. Creighton, P. Jones, Leopoldo Milano, M. P. Ross, A. Parida, A. E. Pace, T. M. Evans, A. Bozzi, Sheila Rowan, S. Sunil, Giovanni Carapella, A. Corsi, M. Colleoni, A. Dasgupta, A. K. Prajapati, A. R. Wade, Rosa Poggiani, C. M. Mow-Lowry, A. Markowitz, J. A. Giaime, S. Soni, S. Farinon, E. Mejuto Villa, A. Lazzarini, F. Carbognani, C. Gray, T. Z. Summerscales, K. A. Thorne, S. Antier, M. Chan, E. Katsavounidis, S. J. Jadhav, S. C. Tait, R. Flaminio, J.-P. Coulon, S. H. Huttner, N. Arnaud, R. K. L. Lo, V. Sequino, C. Affeldt, J. D. Lough, J. Casanueva Diaz, S. B. Coughlin, M. MacInnis, E. Cesarini, P. Rapagnani, Colm Talbot, M. Colpi, R. Birney, Andreas Freise, Paul D. Lasky, Z. Márka, W. H. Wang, F. Travasso, R. L. Byer, C. Van Den Broeck, Y.-J. Huang, E. Sowell, G. Vajente, D. M. Macleod, Piotr Jaranowski, M. Llorens-Monteagudo, Soma Mukherjee, J. R. Sanders, A. Aich, A. Gopakumar, David Coward, A. Miani, J. Castañeda, T. J. Hansen, P. Brockill, S. Sayah, V. V. Frolov, Tania Regimbau, A. J. Tanasijczuk, Sebastien Clesse, N. Bode, A. Macquet, Matthew Pitkin, T. Sadecki, J. M. Isac, M. C. Araya, H. S. Chen, T. G. F. Li, Michela Mapelli, C. Collins, S. Mastrogiovanni, S. Y. Hoback, N. Radulesco, L.-W. Wei, Shao-Jiang Wang, R. Bonnand, Zachariah B. Etienne, L. Kuo, Jennifer Watchi, S. A. Pai, H. Shen, Fausto Acernese, F. Muciaccia, C. Mishra, M. Cieślar, J. Warner, M. Granata, A. Perego, C. V. Kalaghatgi, D. DeBra, Eric B. Flynn, S. Biscoveanu, L. Xiao, A. Grant, M. Breschi, B. Gateley, Aaron Buikema, A. Lockwood, M. Mantovani, M. Lormand, F. Cavalier, A. Bals, E. Maynard, J. S. Areeda, R. De Rosa, M. C. Tringali, I. Nardecchia, A. L. James, G. Baltus, A. K. Divakarla, Santosh Roy, E. Maros, G. Pagano, Patrick Das Gupta, M. Eisenmann, G. L. Mansell, I. Di Palma, D. Pascucci, M. S. Shahriar, P. Ruggi, V. Pierro, M. Turconi, Srishti Tiwari, Q. Chu, D. L. Ferguson, F. Morawski, V. Frey, S. Leavey, C. Bradaschia, D. I. Jones, Shiuh Chao, S. Hochheim, N. A. Robertson, Robert J. McCarthy, J. K. Blackburn, Linqing Wen, R. Bassiri, G. Koekoek, Daniele A. Steer, Hai-Ping Cheng, D. C. Vander-Hyde, Sanjeev Kumar, D. B. Kozak, Arunava Mukherjee, Y. Minenkov, G. Kuehn, L. K. Nuttall, G. Intini, C. Lazzaro, Patricia Schmidt, A. Trovato, R. K. Hasskew, G. Mitselmakher, J. Oberling, D. D'Urso, P. Thomas, David Jonathan Hofman, K. Agatsuma, S. Doravari, R. Coyne, L. Terkowski, M. Branchesi, S. Chua, D. Y. 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V., Królak, A., Krupinski, N., Kuehn, G., Kumar, A., Kumar, P., Kumar, Rahul, Kumar, Rakesh, Kumar, S., Kuo, L., Kutynia, A., Lackey, B. D., Laghi, D., Lalande, E., Lam, T. L., Lamberts, A., Landry, M., Lane, B. B., Lang, R. N., Lange, J., Lantz, B., Lanza, R. K., La Rosa, I., Lartaux-Vollard, A., Lasky, P. D., Laxen, M., Lazzarini, A., Lazzaro, C., Leaci, P., Leavey, S., Lecoeuche, Y. K., Lee, C. H., Lee, H. M., Lee, H. W., Lee, J., Lee, K., Lehmann, J., Leroy, N., Letendre, N., Levin, Y., Li, A. K. Y., Li, J., Li, K., Li, T. G. F., Li, X., Linde, F., Linker, S. D., Linley, J. N., Littenberg, T. B., Liu, J., Liu, X., Llorens-Monteagudo, M., Lo, R. K. L., Lockwood, A., London, L. T., Longo, A., Lorenzini, M., Loriette, V., Lormand, M., Losurdo, G., Lough, J. D., Lousto, C. O., Lovelace, G., Lück, H., Lumaca, D., Lundgren, A. P., Ma, Y., Macas, R., Macfoy, S., Macinnis, M., Macleod, D. M., Macmillan, I. A. O., Macquet, A., Magaña Hernandez, I., Magaña-Sandoval, F., Magee, R. M., Majorana, E., Maksimovic, I., Malik, A., Man, N., Mandic, V., Mangano, V., Mansell, G. L., Manske, M., Mantovani, M., Mapelli, M., Marchesoni, F., Marion, F., Márka, S., Márka, Z., Markakis, C., Markosyan, A. S., Markowitz, A., Maros, E., Marquina, A., Marsat, S., Martelli, F., Martin, I. W., Martin, R. M., Martinez, V., Martynov, D. V., Masalehdan, H., Mason, K., Massera, E., Masserot, A., Massinger, T. J., Masso-Reid, M., Mastrogiovanni, S., Matas, A., Matichard, F., Mavalvala, N., Maynard, E., Mccann, J. J., Mccarthy, R., Mcclelland, D. E., Mccormick, S., Mcculler, L., Mcguire, S. C., Mcisaac, C., Mciver, J., Mcmanus, D. J., Mcrae, T., Mcwilliams, S. T., Meacher, D., Meadors, G. D., Mehmet, M., Mehta, A. K., Mejuto Villa, E., Melatos, A., Mendell, G., Mercer, R. A., Mereni, L., Merfeld, K., Merilh, E. L., Merritt, J. D., Merzougui, M., Meshkov, S., Messenger, C., Messick, C., Metzdorff, R., Meyers, P. M., Meylahn, F., Mhaske, A., Miani, A., Miao, H., Michaloliakos, I., Michel, C., Middleton, H., Milano, L., Miller, A. L., Miller, S., Millhouse, M., Mills, J. C., Milotti, E., Milovich-Goff, M. C., Minazzoli, O., Minenkov, Y., Mishkin, A., Mishra, C., Mistry, T., Mitra, S., Mitrofanov, V. P., Mitselmakher, G., Mittleman, R., Mo, G., Mogushi, K., Mohapatra, S. R. P., Mohite, S. R., Molina-Ruiz, M., Mondin, M., Montani, M., Moore, C. J., Moraru, D., Morawski, F., Moreno, G., Morisaki, S., Mours, B., Mow-Lowry, C. M., Mozzon, S., Muciaccia, F., Mukherjee, Arunava, Mukherjee, D., Mukherjee, S., Mukherjee, Subroto, Mukund, N., Mullavey, A., Munch, J., Muñiz, E. A., Murray, P. G., Nagar, A., Nardecchia, I., Naticchioni, L., Nayak, R. K., Neil, B. F., Neilson, J., Nelemans, G., Nelson, T. J. N., Nery, M., Neunzert, A., Ng, K. Y., Ng, S., Nguyen, C., Nguyen, P., Nichols, D., Nichols, S. A., Nissanke, S., Nocera, F., Noh, M., North, C., Nothard, D., Nuttall, L. K., Oberling, J., O’Brien, B. D., Oganesyan, G., Ogin, G. H., Oh, J. J., Oh, S. H., Ohme, F., Ohta, H., Okada, M. A., Oliver, M., Olivetto, C., Oppermann, P., Oram, Richard J., O’Reilly, B., Ormiston, R. G., Ortega, L. F., O’Shaughnessy, R., Ossokine, S., Osthelder, C., Ottaway, D. J., Overmier, H., Owen, B. J., Pace, A. E., Pagano, G., Page, M. A., Pagliaroli, G., Pai, A., Pai, S. A., Palamos, J. R., Palashov, O., Palomba, C., Pan, H., Panda, P. K., Pang, P. T. H., Pankow, C., Pannarale, F., Pant, B. C., Paoletti, F., Paoli, A., Parida, A., Parker, W., Pascucci, D., Pasqualetti, A., Passaquieti, R., Passuello, D., Patricelli, B., Payne, E., Pearlstone, B. L., Pechsiri, T. C., Pedersen, A. J., Pedraza, M., Pele, A., Penn, S., Perego, A., Perez, C. J., Périgois, C., Perreca, A., Perriès, S., Petermann, J., Pfeiffer, H. P., Phelps, M., Phukon, K. S., Piccinni, O. J., Pichot, M., Piendibene, M., Piergiovanni, F., Pierro, V., Pillant, G., Pinard, L., Pinto, I. M., Piotrzkowski, K., Pirello, M., Pitkin, M., Plastino, W., Poggiani, R., Pong, D. Y. T., Ponrathnam, S., Popolizio, P., Porter, E. K., Powell, J., Prajapati, A. K., Prasai, K., Prasanna, R., Pratten, G., Prestegard, T., Principe, M., Prodi, G. A., Prokhorov, L., Punturo, M., Puppo, P., Pürrer, M., Qi, H., Quetschke, V., Quinonez, P. J., Raab, F. J., Raaijmakers, G., Radkins, H., Radulesco, N., Raffai, P., Rafferty, H., Raja, S., Rajan, C., Rajbhandari, B., Rakhmanov, M., Ramirez, K. E., Ramos-Buades, A., Rana, Javed, Rao, K., Rapagnani, P., Raymond, V., Razzano, M., Read, J., Regimbau, T., Rei, L., Reid, S., Reitze, D. H., Rettegno, P., Ricci, F., Richardson, C. J., Richardson, J. W., Ricker, P. M., Riemenschneider, G., Riles, K., Rizzo, M., Robertson, N. A., Robinet, F., Rocchi, A., Rodriguez-Soto, R. D., Rolland, L., Rollins, J. G., Roma, V. J., Romanelli, M., Romano, R., Romel, C. L., Romero-Shaw, I. M., Romie, J. H., Rose, C. A., Rose, D., Rose, K., Rosińska, D., Rosofsky, S. G., Ross, M. P., Rowan, S., Rowlinson, S. J., Roy, P. K., Roy, Santosh, Roy, Soumen, Ruggi, P., Rutins, G., Ryan, K., Sachdev, S., Sadecki, T., Sakellariadou, M., Salafia, O. S., Salconi, L., Saleem, M., Samajdar, A., Sanchez, E. J., Sanchez, L. E., Sanchis-Gual, N., Sanders, J. R., Santiago, K. A., Santos, E., Sarin, N., Sassolas, B., Sathyaprakash, B. S., Sauter, O., Savage, R. L., Savant, V., Sawant, D., Sayah, S., Schaetzl, D., Schale, P., Scheel, M., Scheuer, J., Schmidt, P., Schnabel, R., Schofield, R. M. S., Schönbeck, A., Schreiber, E., Schulte, B. W., Schutz, B. F., Schwarm, O., Schwartz, E., Scott, J., Scott, S. M., Seidel, E., Sellers, D., Sengupta, A. S., Sennett, N., Sentenac, D., Sequino, V., Sergeev, A., Setyawati, Y., Shaddock, D. A., Shaffer, T., Shahriar, M. S., Sharifi, S., Sharma, A., Sharma, P., Shawhan, P., Shen, H., Shikauchi, M., Shink, R., Shoemaker, D. H., Shoemaker, D. M., Shukla, K., Shyamsundar, S., Siellez, K., Sieniawska, M., Sigg, D., Singer, L. P., Singh, D., Singh, N., Singha, A., Singhal, A., Sintes, A. M., Sipala, V., Skliris, V., Slagmolen, B. J. J., Slaven-Blair, T. J., Smetana, J., Smith, J. R., Smith, R. J. E., Somala, S., Son, E. J., Soni, S., Sorazu, B., Sordini, V., Sorrentino, F., Souradeep, T., Sowell, E., Spencer, A. P., Spera, M., Srivastava, A. K., Srivastava, V., Staats, K., Stachie, C., Standke, M., Steer, D. A., Steinke, M., Steinlechner, J., Steinlechner, S., Steinmeyer, D., Stevenson, S., Stocks, D., Stops, D. J., Stover, M., Strain, K. A., Stratta, G., Strunk, A., Sturani, R., Stuver, A. L., Sudhagar, S., Sudhir, V., Summerscales, T. Z., Sun, L., Sunil, S., Sur, A., Suresh, J., Sutton, P. J., Swinkels, B. L., Szczepańczyk, M. J., Tacca, M., Tait, S. C., Talbot, C., Tanasijczuk, A. J., Tanner, D. B., Tao, D., Tápai, M., Tapia, A., Tapia San Martin, E. N., Tasson, J. D., Taylor, R., Tenorio, R., Terkowski, L., Thirugnanasambandam, M. P., Thomas, M., Thomas, P., Thompson, J. E., Thondapu, S. R., Thorne, K. A., Thrane, E., Tinsman, C. L., Saravanan, T. R., Tiwari, Shubhanshu, Tiwari, S., Tiwari, V., Toland, K., Tonelli, M., Tornasi, Z., Torres-Forné, A., Torrie, C. I., Tosta e Melo, I., Töyrä, D., Trail, E. A., Travasso, F., Traylor, G., Tringali, M. C., Tripathee, A., Trovato, A., Trudeau, R. J., Tsang, K. W., Tse, M., Tso, R., Tsukada, L., Tsuna, D., Tsutsui, T., Turconi, M., Ubhi, A. S., Udall, R., Ueno, K., Ugolini, D., Unnikrishnan, C. S., Urban, A. L., Usman, S. A., Utina, A. C., Vahlbruch, H., Vajente, G., Valdes, G., Valentini, M., van Bakel, N., van Beuzekom, M., van den Brand, J. F. J., Van Den Broeck, C., Vander-Hyde, D. C., van der Schaaf, L., Van Heijningen, J. V., van Veggel, A. A., Vardaro, M., Varma, V., Vass, S., Vasúth, M., Vecchio, A., Vedovato, G., Veitch, J., Veitch, P. J., Venkateswara, K., Venugopalan, G., Verkindt, D., Veske, D., Vetrano, F., Viceré, A., Viets, A. D., Vinciguerra, S., Vine, D. J., Vinet, J. -Y., Vitale, S., Vivanco, Francisco Hernandez, Vo, T., Vocca, H., Vorvick, C., Vyatchanin, S. P., Wade, A. R., Wade, L. E., Wade, M., Walet, R., Walker, M., Wallace, G. S., Wallace, L., Walsh, S., Wang, J. Z., Wang, S., Wang, W. H., Ward, R. L., Warden, Z. A., Warner, J., Was, M., Watchi, J., Weaver, B., Wei, L. -W., Weinert, M., Weinstein, A. J., Weiss, R., Wellmann, F., Wen, L., Weßels, P., Westhouse, J. W., Wette, K., Whelan, J. T., Whiting, B. F., Whittle, C., Wilken, D. M., Williams, D., Willis, J. L., Willke, B., Winkler, W., Wipf, C. C., Wittel, H., Woan, G., Woehler, J., Wofford, J. K., Wong, C., Wright, J. L., Wu, D. S., Wysocki, D. M., Xiao, L., Yamamoto, H., Yang, L., Yang, Y., Yang, Z., Yap, M. J., Yazback, M., Yeeles, D. W., Yu, Hang, Yu, Haocun, Yuen, S. H. R., Zadrożny, A. K., Zadrożny, A., Zanolin, M., Zelenova, T., Zendri, J. -P., Zevin, M., Zhang, J., Zhang, L., Zhang, T., Zhao, C., Zhao, G., Zhou, M., Zhou, Z., Zhu, X. J., Zimmerman, A. B., Zucker, M. E., Zweizig, J., Laboratoire des matériaux avancés (LMA), 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, 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 l'Accélérateur Linéaire (LAL), 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), 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), Astrophysique Relativiste Théories Expériences Métrologie Instrumentation Signaux (ARTEMIS), 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)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA), Institut des Fonctions Optiques pour les Technologies de l'informatiON (Institut FOTON), Université de Rennes 1 (UR1), Université de Rennes (UNIV-RENNES)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Université de Rennes (UNIV-RENNES)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-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 Kastler Brossel (LKB [Collège de France]), École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Sorbonne Université (SU)-Collège de France (CdF (institution)), Institut Lumière Matière [Villeurbanne] (ILM), Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS), 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), Observatoire de la Côte d'Azur (OCA), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ecole Superieure de Physique et de Chimie Industrielles de la Ville de Paris (ESPCI Paris), Université Paris sciences et lettres (PSL), 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), Institut des Hautes Etudes Scientifiques (IHES), IHES, LIGO Scientific, Virgo, The LIGO Scientific Collaboration, The Virgo Collaboration, 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 Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), 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 Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-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)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université de Rennes (UR)-Institut National des Sciences Appliquées - Rennes (INSA Rennes), Institut National des Sciences Appliquées (INSA)-Institut National des Sciences Appliquées (INSA)-École Nationale Supérieure des Sciences Appliquées et de Technologie (ENSSAT)-Centre National de la Recherche Scientifique (CNRS), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF (institution))-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), Institut des Hautes Études Scientifiques (IHES), RS: FSE Grav. waves and fundamental physics, Grav. waves and fundamental physics, RS: FSE MSP, IoP (FNWI), Gravitation and Astroparticle Physics Amsterdam, Other Research IHEF (IoP, FNWI), Faculty of Science, Astroparticle Physics (IHEF, IoP, FNWI), Arene, M., Becsy, B., Calderon Bustillo, J., Castaneda, J., Cavaglia, M., Cerda-Duran, P., Cieslar, M., Cordero-Carrion, I., Dalya, G., D'Angelo, B., D'Antonio, S., Deleglise, S., D'Emilio, V., De Varona, O., Diaz, M. C., D'Urso, D., Fronze, G., Garcia-Quiros, C., Ghosh, A., Gonzalez, G., Guixe, G., Hubner, M. T., Johnson-Mcdaniel, N. K., Kefelian, F., Kim, C., Krolak, A., Kumar, R., Luck, H., Magana Hernandez, I., Magana-Sandoval, F., Marka, S., Marka, Z., Mukherjee, A., Muniz, E. A., O'Brien, B. D., Oram, R. J., O'Reilly, B., O'Shaughnessy, R., Perigois, C., Perries, S., Purrer, M., Rana, J., Rosinska, D., Roy, S., Schonbeck, A., Szczepanczyk, M. J., Tapai, M., Torres-Forne, A., Tosta E Melo, I., Toyra, D., Van Bakel, N., Van Beuzekom, M., Van Den Brand, J. F. J., Van Der Schaaf, L., Van Veggel, A. A., Vasuth, M., Vicere, A., Vivanco, F. H., Wessels, P., Yu, H., Zadrozny, A. K., Zadrozny, A., National Science Foundation (US), Science and Technology Facilities Council (UK), Agencia Estatal de Investigación (España), Generalitat de Catalunya, Govern de les Illes Balears, Generalitat Valenciana, European Commission, Sub Subatomic Physics (SAP), Subatomic Physics, Université Nice Sophia Antipolis (... - 2019) (UNS), Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), (Astro)-Particles Physics, LIGO Scientific Collaboration, and Virgo Collaboration

Subjects
Physics and Astronomy (miscellaneous), Astronomy, Gravitational wave detection, Gravitational wave sources, Gravitational waves, Astronomical black holes, agn discs, Astrophysics, detector: network, 01 natural sciences, General Relativity and Quantum Cosmology, Physics, Particles & Fields, star-clusters, gravitational waves, black holes, gravitational waves, black holes, AGN DISCS, LIGO, Virgo, black hole, general relativity, gravitational wave, QC, QB, Physics, Settore FIS/01, astro-ph.HE, High Energy Astrophysical Phenomena (astro-ph.HE), GRAVITATIONAL WAVE-FORMS, PROGENITORS, COMPACT BINARIES, black hole: spin, PERTURBATIONS, Physical Sciences, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Gravitational wave detection, Astrophysics - High Energy Astrophysical Phenomena, METALLICITY, mass: asymmetry, metallicity, data analysis method, General relativity, MERGERS, gr-qc, Astrophysics::High Energy Astrophysical Phenomena, multipole, PREDICTIONS, FOS: Physical sciences, gravitational waves,black holes, General Relativity and Quantum Cosmology (gr-qc), Astronomy & Astrophysics, gravitational radiation: direct detection, Gravitational waves, Theory of relativity, Binary black hole, Settore FIS/05 - Astronomia e Astrofisica, Astronomical black holes, binary: coalescence, 0103 physical sciences, numerical methods, ddc:530, STAR-CLUSTERS, 010306 general physics, numerical calculations, STFC, Astrophysique, Gravitational wave sources, Science & Technology, mass: solar, 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, RCUK, black hole: mass, Mass ratio, EVOLUTION, gravitational radiation detector, Black hole, detector: sensitivity, Physics and Astronomy, black hole: binary, relativity theory, gravitational radiation: emission, mass ratio, Multipole expansion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

LIGO Scientific Collaboration and Virgo Collaboration: et al., We report the observation of gravitational waves from a binary-black-hole coalescence during the first two weeks of LIGO’s and Virgo’s third observing run. The signal was recorded on April 12, 2019 at 05∶30∶44 UTC with a network signal-to-noise ratio of 19. The binary is different from observations during the first two observing runs most notably due to its asymmetric masses: a ∼30 M⊙ black hole merged with a ∼8M⊙ black hole companion. The more massive black hole rotated with a dimensionless spin magnitude between 0.22 and 0.60 (90% probability). Asymmetric systems are predicted to emit gravitational waves with stronger contributions from higher multipoles, and indeed we find strong evidence for gravitational radiation beyond the leading quadrupolar order in the observed signal. A suite of tests performed on GW190412 indicates consistency with Einstein’s general theory of relativity. While the mass ratio of this system differs from all previous detections, we show that it is consistent with the population model of stellar binary black holes inferred from the first two observing runs., The authors gratefully acknowledge the support of the United States National Science Foundation (NSF) for the construction and operation of the LIGO Laboratory and Advanced LIGO as well as the Science and Technology Facilities Council (STFC) of the United Kingdom, the Max-Planck-Society (MPS), and the State of Niedersachsen/Germany for support of the construction of Advanced LIGO and construction and operation of the GEO600 detector. Additional support for Advanced LIGO was provided by the Australian Research Council. The authors gratefully acknowledge the Italian Istituto Nazionale di Fisica Nucleare (INFN), the French Centre National de la Recherche Scientifique (CNRS) and the Netherlands Organization for Scientific Research, for the construction and operation of the Virgo detector and the creation and support of the EGO consortium. The authors also gratefully acknowledge research support from these agencies as well as by the Council of Scientific and Industrial Research of India, the Department of Science and Technology, India, the Science & Engineering Research Board (SERB), India, the Ministry of Human Resource Development, India, the Spanish Agencia Estatal de Investigación, the Vicepresidencia i Conselleria d’Innovació, Recerca i Turisme and the Conselleria d’Educació i Universitat del Govern de les Illes Balears, the Conselleria d’Innovació, Universitats, Ciencia i Societat Digital de la Generalitat Valenciana and the CERCA Programme Generalitat de Catalunya, Spain, the National Science Centre of Poland, the Swiss National Science Foundation (SNSF), the Russian Foundation for Basic Research, the Russian Science Foundation, the European Commission, the European Regional Development Funds (ERDF), the Royal Society, the Scottish Funding Council, the Scottish Universities Physics Alliance, the Hungarian Scientific Research Fund (OTKA), the French Lyon Institute of Origins (LIO), the Belgian Fonds de la Recherche Scientifique (FRS-FNRS), Actions de Recherche Concertees (ARC) and Fonds Wetenschappelijk Onderzoek–Vlaanderen (FWO), Belgium, the Paris Île-de-France Region, the National Research, Development and Innovation Office Hungary (NKFIH), the National Research Foundation of Korea, Industry Canada and the Province of Ontario through the Ministry of Economic Development and Innovation, the Natural Science and Engineering Research Council Canada, the Canadian Institute for Advanced Research, the Brazilian Ministry of Science, Technology, Innovations, and Communications, the International Center for Theoretical Physics South American Institute for Fundamental Research (ICTPSAIFR), the Research Grants Council of Hong Kong, the National Natural Science Foundation of China (NSFC), the Leverhulme Trust, the Research Corporation, the Ministry of Science and Technology (MOST), Taiwan and the Kavli Foundation. The authorsgratefully acknowledge the support of the NSF, STFC, INFN and CNRS for provision of computational resources.

Published
2020
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37. Investigating the detection of dark matter subhalos as extended sources with Fermi-LAT

Author

Francesca Calore, Mattia Di Mauro, Martin Stref, 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
Structure formation, Cold dark matter, WIMP, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, satellite, Massive particle, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, GLAST, cross section: annihilation, High Energy Physics - Phenomenology (hep-ph), dark matter: halo, 0103 physical sciences, structure, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, dark matter: mass, formation, Astrophysics - Astrophysics of Galaxies, Galaxy, Dark matter halo, flux, High Energy Physics - Phenomenology, gamma ray, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Astrophysics of Galaxies (astro-ph.GA), Halo, galaxy, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], signature, Fermi Gamma-ray Space Telescope, Astrophysics and astroparticle physics
Abstract

Cold dark matter (DM) models for structure formation predict that DM subhalos are present in the Galaxy. In the standard paradigm of DM as weakly interacting massive particle, subhalos are expected to shine in gamma rays and to provide a signal detectable with current instruments, notably with the Large Area Telescope (LAT) aboard the Fermi~satellite. This is the main motivation behind searches for DM signals towards dwarf spheroidal galaxies and unidentified Fermi-LAT sources. A significant angular extension detected from unassociated sources located at relatively high latitudes is considered a "smoking gun" signature for identifying DM subhalos. In the present work, we systematically explore, by means of state-of-the-art models of cold DM halos in the Galaxy, the detectability of extended subhalos with Fermi-LAT. We simulate a DM signal exploring different assumptions of subhalos distribution in the Galaxy and DM profile, and reconstruct its flux through a realistic Fermi-LAT analysis pipeline. In the most optimistic case, we show that a detection of extended DM subhalos can be made for annihilation cross sections higher than $3 \times 10^{-26}$ cm$^3$/s (for a 100 GeV DM mass), still compatible with existing gamma-ray constraints, and that, in this case, the preference for extension of the source (vs point-like hypothesis) is significant. For fainter signals, instead, halos not only do not show significant extension, but they are not even detectable significantly as point-like sources., Comment: 12 pages, 11 figures. Comments as welcome!

Published
2020
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38. Collective Oscillations of Majorana Neutrinos in Strong Magnetic Fields and Self-induced Flavor Equilibrium

Author

Sajad Abbar, 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), 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), 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, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)

Subjects
Particle physics, magnetic field: high, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 01 natural sciences, Bohr magneton, symbols.namesake, 0103 physical sciences, supernova, site, 010306 general physics, neutron star, Equipartition theorem, Astrophysics::Galaxy Astrophysics, Physics, magnetic moment: transition, High Energy Astrophysical Phenomena (astro-ph.HE), flavor, Magnetic moment, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, Neutron star, Supernova, MAJORANA, oscillation: collective, neutrino: transition, symbols, neutrino: Majorana, High Energy Physics::Experiment, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, Hamiltonian (quantum mechanics), [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics and astroparticle physics
Abstract

We study collective oscillations of Majorana neutrinos in some of the most extreme astrophysical sites such as neutron star merger remnants and magneto-rotational core-collapse supernovae which include dense neutrino media in the presence of strong magnetic fields. We show that neutrinos can reach flavor equilibrium if neutrino transition magnetic moment $\mu_\nu$ is strong enough, namely when $\mu_\nu/\mu_{\rm{B}} \gtrsim 10^{-14}-10^{-15}$ with $\mu_{\rm{B}}$ being the Bohr magneton. This sort of flavor equilibrium, which is not necessarily flavor equipartition, can occur on (short) scales determined by the strength of the magnetic term. Our findings can have interesting implications for the physics of such violent astrophysical environments., Comment: minor modifications to match the published version in PRD

Published
2020
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39. Radio Signal of Axion-Photon Conversion in Neutron Stars: A Ray Tracing Analysis

Author

Marco Chianese, Christoph Weniger, Mikaël Leroy, Thomas D. P. Edwards, Leroy, M., Chianese, M., Edwards, T. D. P., Weniger, C., École normale supérieure - Cachan (ENS Cachan), IoP (FNWI), ITFA (IoP, FNWI), and GRAPPA (ITFA, IoP, FNWI)

Subjects
Particle physics, Photon, dimension: 3, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Parameter space, axion: parameter space, 01 natural sciences, phase space, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, 010306 general physics, neutron star, Axion, photon: flux, Physics, radio wave, axion: dark matter, 010308 nuclear & particles physics, 3. Good health, Neutron star, High Energy Physics - Phenomenology, Phase space, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], broadening, Radio wave, Doppler broadening, Astrophysics and astroparticle physics
Abstract

Axion dark matter can resonantly convert into photons in the magnetospheres of neutron stars (NSs). It has recently been shown that radio observations of nearby NSs can therefore provide a highly sensitive probe of the axion parameter space. Here we extend existing calculations by performing the first three-dimensional computation of the photon flux, taking into account the isotropic phase-space distribution of axions and the structure of the NS magnetosphere. In particular, we study the overall magnitude of the flux and its possible time variation. We find that overall signal strength is robust to our more realistic analysis. In addition, we find that the variance of the signal with respect to the NS rotation is washed out by the additional trajectories in our treatment. Nevertheless, we show that SKA observations towards J0806.4-4123 are sensitive to $g_{a\gamma\gamma}\sim 3\times10^{-13}\mathrm{\,GeV^{-1}}$ at $m_a\sim 7\times10^{-6}\mathrm{\,eV}$, even when accounting for Doppler broadening. Finally, we provide the necessary code to calculate the photon flux for any given NS system., Comment: 12 pages, 6 figures

Published
2019
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40. Electron-interacting dark matter: Implications from DAMA/LIBRA-phase2 and prospects for liquid xenon detectors and NaI detectors

Author

Benjamin Roberts, Victor V. Flambaum, Systèmes de Référence Temps Espace (SYRTE), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)

Subjects
DAMA/LIBRA, Cosmology and Nongalactic Astrophysics (astro-ph.CO), detector: performance, Physics::Instrumentation and Detectors, Dark matter, FOS: Physical sciences, chemistry.chemical_element, Electron, 01 natural sciences, WIMP: dark matter, Nuclear physics, High Energy Physics - Phenomenology (hep-ph), Xenon, WIMP, 0103 physical sciences, 010306 general physics, enhancement, scintillation counter, energy: low, Physics, Scintillation, xenon: liquid, 010308 nuclear & particles physics, atom: wave function, DAMA, modulation, High Energy Physics - Phenomenology, chemistry, electron: scattering, Weakly interacting massive particles, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], direct detection, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Event (particle physics), Astrophysics and astroparticle physics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We investigate the possibility for the direct detection of low-mass (GeV scale) weakly interacting massive particles (WIMP) dark matter in scintillation experiments. Such WIMPs are typically too light to leave appreciable nuclear recoils but may be detected via their scattering off atomic electrons. In particular, the DAMA Collaboration [R. Bernabei et al., Nucl. Phys. At. Energy 19, 307 (2018)] has recently presented strong evidence of an annual modulation in the scintillation rate observed at energies as low as 1 keV. Despite a strong enhancement in the calculated event rate at low energies, we find that an interpretation in terms of electron-interacting WIMPs cannot be consistent with existing constraints. We also demonstrate the importance of correct treatment of the atomic wave functions and show the resulting event rate is very sensitive to the low-energy performance of the detectors, meaning it is crucial that the detector uncertainties be taken into account. Finally, we demonstrate that the potential scintillation event rate can be much larger than may otherwise be expected, meaning that competitive searches can be performed for mχ∼GeV scale WIMPs using the conventional prompt (S1) scintillation signals. This is important given the recent and upcoming very large liquid xenon detectors.

Published
2019
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41. Coherent radio emission from the electron beam sudden appearance

Author

Takao Kuwabara, M. Relich, Izumi I.S. Ohta, Pavel Motloch, Aongus O'Murchadha, Florian Partous, Krijn de Vries, Shunsuke Ueyama, Hiroyuki Sagawa, Yusuke Inome, Thomas Meures, R. Gaior, Tatsunobu Shibata, Daisuke Ikeda, John N. Matthews, T. Yamamoto, Kael Hanson, Masaki Fukushima, B. K. Shin, Gordon Thomson, K. Mase, A. Ishihara, Nick van Eijndhoven, Michael DuVernois, S. Yoshida, 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), Physics, Elementary Particle Physics, Faculty of Sciences and Bioengineering Sciences, and 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)

Subjects
Physics and Astronomy (miscellaneous), air, [PHYS.PHYS.PHYS-ACC-PH]Physics [physics]/Physics [physics]/Accelerator Physics [physics.acc-ph], Astrophysics::High Energy Astrophysical Phenomena, ice, FOS: Physical sciences, Cosmic ray, Electron, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, neutrino, Optics, law, 0103 physical sciences, electron: beam, 010306 general physics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, astro-ph.HE, radio wave, 010308 nuclear & particles physics, business.industry, Detector, cascade, Transition radiation, 13. Climate action, cosmic radiation, frequency, Cathode ray, transition radiation: coherence, Neutrino, business, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Radio wave, Astrophysics and astroparticle physics
Abstract

International audience; We report on the measurement of coherent radio emission from the electron beam sudden appearance at the Telescope Array Electron Light Source facility. This emission was detected by four independent radio detector setups sensitive to frequencies ranging from 50 MHz up to 12.5 GHz. We show that this phenomenon can be understood as a special case of coherent transition radiation by comparing the observed results with simulations. The in-nature application of this signal is given by the emission of cosmic ray or neutrino induced particle cascades traversing different media such as air, rock and ice.

Published
2019
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42. Local fading accelerator and the origin of TeV cosmic ray electrons

Author

Jacco Vink, Stefano Gabici, S. Recchia, Felix Aharonian, 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), 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)-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), 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: energy, lepton: energy, Inverse, Astrophysics, Electron, GeV, 01 natural sciences, cosmic radiation: TeV, Luminosity, Positron, Diffusion (business), attenuation, pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, energy: high, cosmic radiation: spectrum, Computer Science::Computation and Language (Computational Linguistics and Natural Language and Speech Processing), shock waves, electron: spectrum, Supernova, positron, Production (computer science), Astrophysics - High Energy Astrophysical Phenomena, Particle physics, accelerator, Astrophysics::High Energy Astrophysical Phenomena, energy loss, Population, FOS: Physical sciences, Cosmic ray, cosmic radiation: diffusion, energy dependence, Pulsar, 0103 physical sciences, supernova, synchrotron, positron: acceleration, Fading, 010306 general physics, education, 010308 nuclear & particles physics, particle: energy, electron: cosmic radiation, acceleration, [PHYS.PHYS.PHYS-GEN-PH]Physics [physics]/Physics [physics]/General Physics [physics.gen-ph], injection, Compton scattering: inverse, 13. Climate action, Physics::Accelerator Physics, High Energy Physics::Experiment, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Energy (signal processing), Astrophysics and astroparticle physics
Abstract

The cosmic ray electron spectrum exhibits a break at a particle energy of $\ensuremath{\sim}1\text{ }\text{ }\mathrm{TeV}$ and extends without any attenuation up to $\ensuremath{\sim}20\text{ }\text{ }\mathrm{TeV}$. Synchrotron and inverse Compton energy losses strongly constrain the time of emission of $\ensuremath{\sim}20\text{ }\text{ }\mathrm{TeV}$ electrons to $\ensuremath{\approx}2\ifmmode\times\else\texttimes\fi{}{10}^{4}\text{ }\text{ }\mathrm{yr}$ and the distance of the potential source(s) to $\ensuremath{\approx}100--500\text{ }\text{ }\mathrm{pc}$, depending on the cosmic ray diffusion coefficient. This suggests that maybe one nearby discrete source may explain the observed spectrum of high energy electrons. Given the strong energy dependence ($\ensuremath{\propto}1/E$) of the cooling time of TeV electrons, the spectral shape of the electron spectrum above the $\ensuremath{\sim}1\text{ }\text{ }\mathrm{TeV}$ break strongly depends on the history of injection of these electrons from the source. In this paper we show that a local, continuous (on timescales of $\ensuremath{\sim}{10}^{5}\text{ }\text{ }\mathrm{yr}$) but fading electron accelerator, with a characteristic decay time of $\ensuremath{\sim}{10}^{4}\text{ }\text{ }\mathrm{yr}$, can naturally account for the entire spectrum of cosmic ray electrons in the TeV domain. Although the standard ``nearby pulsar'' scenario naturally meets this time condition, it is (almost) excluded by recent measurements of the positron fraction, which above $\ensuremath{\sim}100\text{ }\text{ }\mathrm{GeV}$ saturates at a level well below 0.5 and drops above $\ensuremath{\sim}400--500\text{ }\text{ }\mathrm{GeV}$. The second potential source population, the supernova remnants, accelerate mostly electrons, rather than positrons. However, they hardly can provide an effective production of multi-TeV electrons via the standard diffusive shock acceleration scenario for $\ensuremath{\sim}{10}^{5}\text{ }\text{ }\mathrm{yr}$. A third possibility are stellar wind shocks, which however are likely to be continuous with nearly constant luminosity on timescales $\ensuremath{\gg}10\text{ }\text{ }\mathrm{kyr}$ and probably cannot match the time requirement of our potential source. Therefore, we face a real challenge in the identification of the origin of the source of multi-TeV electrons. Thus, the link of this source with known particle accelerators would require a dramatic revision of the standard paradigms of acceleration and escape in such objects.

Published
2019
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43. Nonlinear flavor development of a two-dimensional neutrino gas

Author

Joshua D. Martin, Sajad Abbar, Huaiyu Duan, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, 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), 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), 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), 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
Particle physics, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], perturbation, media_common.quotation_subject, collective, Perturbation (astronomy), FOS: Physical sciences, two-beam, 01 natural sciences, Asymmetry, neutrino: density, Nuclear Theory (nucl-th), symbols.namesake, High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, Wavenumber, Periodic boundary conditions, structure, flavor: oscillation, 010306 general physics, dimension: 2, Flavor, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), neutrino: gas, 010308 nuclear & particles physics, High Energy Physics::Phenomenology, diffusion, boundary condition, Nonlinear system, High Energy Physics - Phenomenology, Fourier transform, neutrino antineutrino: asymmetry, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], symbols, nonlinear, High Energy Physics::Experiment, Neutrino, higher-dimensional, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], statistical, Astrophysics and astroparticle physics
Abstract

We present a numerical survey of the nonlinear flavor development of dense neutrino gases. This study is based on the stationary, two-dimensional ($x$ and $z$), two-beam, monochromatic neutrino line model with a periodic boundary condition along the $x$ direction. Similar to a previous work, we find that small-scale flavor structures can develop in a neutrino gas even if the physical conditions are nearly homogeneous along the $x$ axis initially. The power diffusion from the large-scale to small-scale structures increases with the neutrino density and helps to establish a semi-exponential dependence of the magnitudes of the Fourier moments on the corresponding wave numbers. The overall flavor conversion probabilities in the neutrino gases with small initial sinusoidal perturbations reach certain equilibrium values at large distances which are mainly determined by the neutrino-antineutrino asymmetry. Similar phenomena also exist in a neutrino gas with a localized initial perturbation, albeit only inside an expanding flavor conversion region. Our work suggests that a statistical treatment may be possible for the collective flavor oscillations of a dense neutrino gas in a multi-dimensional environment., 10 pages, 5 figures

Published
2019
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44. QED effects are negligible for neutron-star spin-down

Author

Paul Ripoche, Jeremy S. Heyl, École normale supérieure - Cachan (ENS Cachan), and Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Magnetar, 7. Clean energy, 01 natural sciences, Magnetic field, Neutron star, Pulsar, Vacuum energy, Quantum electrodynamics, 0103 physical sciences, Vacuum polarization, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Magnetic dipole, Spin-½, Astrophysics and astroparticle physics
Abstract

The energy loss of a rotationally powered pulsar is primarily carried away as electromagnetic radiation and a particle wind. Considering that the magnetic field strength of pulsars ranges from about $1{0}^{8}$ to $1{0}^{15}\text{ }\text{ }\mathrm{G}$, one could expect quantum electrodynamics (QED) to play a role in their spin-down, especially for strongly magnetized ones (magnetars). In fact several authors have argued that QED corrections will dominate the spin-down for slowly rotating stars. They called this effect quantum vacuum friction (QVF). However, QVF was originally derived using a problematic self-torque technique, which leads to a dramatic overestimation of this spin-down effect. Here, instead of using QVF, we explicitly calculate the energy loss from rotating neutron stars using the Poynting vector and a model for a particle wind, and we include the QED one-loop corrections. We express the excess emission as QED one-loop corrections to the radiative magnetic moment of a neutron star. We do find a small component of the spin-down luminosity that originates from the vacuum polarization. However, it never exceeds one percent of the classical magnetic dipole radiation in neutron stars for all physically interesting field strengths. Therefore, we find that the radiative corrections of QED are irrelevant in the energetics of neutron-star spin-down.

Published
2019
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45. Science with the TianQin observatory: Preliminary results on massive black hole binaries

Author

Wen-Fan Feng, Yan Wang, Jianwei Mei, Zhen Jiang, Shun-Jia Huang, Alberto Sesana, Hai-Tian Wang, Enrico Barausse, Yi-Fan Wang, Yi-Ming Hu, Jun Luo, 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), Wang, H, Jiang, Z, Sesana, A, Barausse, E, Huang, S, Wang, Y, Feng, W, Hu, Y, Mei, J, and Luo, J

Subjects
noise, coalescence, Cosmology and Nongalactic Astrophysics (astro-ph.CO), media_common.quotation_subject, astro-ph.GA, interferometer, FOS: Physical sciences, Astrophysics, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, 7. Clean energy, General Relativity and Quantum Cosmology, localization, Settore FIS/05 - Astronomia e Astrofisica, Observatory, Astrophysics - Astrophysics of Galaxie, 0103 physical sciences, astro-ph.HE, astro-ph.CO, black hole, Astrophysics - Cosmology and Nongalactic Astrophysic, 010306 general physics, Luminosity distance, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Gravitational wave, gravitational radiation, redshift, Astrophysics - Astrophysics of Galaxies, Redshift, Black hole, messenger, observatory, Interferometry, black hole: binary, Sky, Astrophysics of Galaxies (astro-ph.GA), [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], history, Detection rate, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

We investigate the prospects of detecting gravitational waves from coalescing massive black hole binaries in the Universe with the TianQin observatory, a space-based gravitational wave interferometer proposed to be launched in the 2030s. To frame the scientific scope of the mission, in this paper, we carry out a preliminary estimation of the signal-to-noise ratio, detection rate and parameter estimation precision of massive black hole binaries detectable by TianQin. In order to make our results as robust as possible, we consider several models of the growth history of massive black holes, exploring the effect of some key astrophysical prescriptions as well the impact of the employed computational methods. In the most optimistic model, TianQin can detect as many as approximately 60 mergers per year. If TianQin detects a merger at redshift of 15, it will be capable of estimating its luminosity distance to within an accuracy of 10%; for a nearby event at redshift approximately 2, TianQin can issue early warnings 24 hours before coalescence, with a timing accuracy of around three hours and a sky localization ability of approximately 80 deg$^2$, thus enabling multi-messenger observations., Comment: 17 pages, 6 figures

Published
2019
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46. New code for equilibriums and quasiequilibrium initial data of compact objects. IV. Rotating relativistic stars with mixed poloidal and toroidal magnetic fields

Author

Charalampos Markakis, Kotaro Fujisawa, Yoshiharu Eriguchi, Eric Gourgoulhon, Kōji Uryū, Keisuke Taniguchi, Shijun Yoshida, Antonios Tsokaros, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and 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)

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Toroid, 010308 nuclear & particles physics, Numerical analysis, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Compact star, 01 natural sciences, General Relativity and Quantum Cosmology, Magnetic field, Computational physics, symbols.namesake, Neutron star, Stars, 0103 physical sciences, symbols, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Magnetohydrodynamic drive, Einstein, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics::Galaxy Astrophysics, Astrophysics and astroparticle physics
Abstract

A new code for computing fully general relativistic solutions of strongly magnetized rapidly rotating compact stars is developed as a part of the COCAL (Compact Object CALculator) code. The full set of Einstein's equations, Maxwell's equations and magnetohydrodynamic equations are consistently solved assuming perfect conductivity, stationarity, and axisymmetry, and strongly magnetized solutions associated with mixed poloidal and toroidal components of magnetic fields are successfully obtained in generic (non-circular) spacetimes. We introduce the formulation of the problem and the numerical method in detail, then present examples of extremely magnetized compact star solutions and their convergence tests. It is found that, in extremely magnetized stars, the stellar matter can be expelled from the region of strongest toroidal fields. Hence we conjecture that a toroidal electro-vacuum region may appear inside of the extremely magnetized compact stars, which may seem like the neutron star becoming the strongest toroidal solenoid coil in the universe., 30 pages, 4 figures

Published
2019
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47. Influence of a planar boundary on the electric field emitted by a particle shower

Author

Lilian Martin, Antony Escudie, D. García-Fernández, Benoît Revenu, 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), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), 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)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), 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), 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)-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, and Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)

Subjects
Field (physics), air, Astrophysics::High Energy Astrophysical Phenomena, ice, pole, FOS: Physical sciences, Context (language use), Cosmic ray, 01 natural sciences, Particle shower, Electric field, 0103 physical sciences, 010306 general physics, Monte Carlo, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, radio wave, showers: atmosphere, 010308 nuclear & particles physics, tracks, Computational physics, electric field, cosmic radiation: primary, Air shower, frequency: low, [SDU]Sciences of the Universe [physics], interface, Antenna (radio), Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Radio wave, Astrophysics and astroparticle physics
Abstract

International audience; The radio detection of cosmic rays consists in the estimation of the properties of a primary cosmic ray by observing the electric field emitted by the extensive air shower (EAS) created when the primary cosmic ray enters the atmosphere. This technique is fully operative nowadays and presents a good degree of maturity. In addition, several projects intend to employ this technique for the detection of neutrinos. In order for the technique to be useful, accurate methods for computing the electric field created by a particle shower in the context of a particular experiment must exist. Although current ground-based radio experiments lie on the air-soil interface and some planned experiments on the South Pole envision antennas near the air-ice interface, most of the analytical approaches and Monte Carlo codes used for calculating the electric field either do not take into account the effect of the boundary or calculate the radiation fields only (direct, reflected and transmitted radiation fields). When the particle shower and the antenna are close to the boundary, compared to the observation wavelength, the far-field approximation breaks down, which is the case for the low-frequency EXTASIS experiment, for instance. We present in this work a new formula for calculating the exact field emitted by a particle track in two semi-infinite media separated by a planar boundary. We also explore the validity of the far-field approximation and make some predictions for EAS using a simple shower model.

Published
2019
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48. Dark matter and bubble nucleation in old neutron stars

Author

Joseph Silk, C. Albertus, A. Herrero, M. A. Pérez-García, 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
Quark, Particle physics, Nuclear Theory, [PHYS.NUCL]Physics [physics]/Nuclear Theory [nucl-th], Dark matter, Hadron, Nucleation, FOS: Physical sciences, 01 natural sciences, energy: injection, bubble: nucleation, Nuclear Theory (nucl-th), High Energy Physics - Phenomenology (hep-ph), 0103 physical sciences, thermodynamical, 010306 general physics, neutron star, equation of state, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), quark: matter, 010308 nuclear & particles physics, Equation of state (cosmology), formation, High Energy Physics - Phenomenology, Strange matter, Neutron star, dark matter: scattering, [PHYS.HPHE]Physics [physics]/High Energy Physics - Phenomenology [hep-ph], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], matter: droplet, Energy (signal processing), Astrophysics and astroparticle physics
Abstract

We study the probability for nucleation of quark matter droplets in the dense cold cores of old neutron stars induced by the presence of a self-annihilating dark matter component, $\chi$. Using a parameterized form of the equation of state for hadronic and quark phases of ordinary matter, we explore the thermodynamic conditions under which droplet formation is facilitated by the energy injection from $\chi$ self-annihilations. We obtain the droplet nucleation time as a function of the dark matter candidate mass, $m_\chi$. We discuss further observational consequences., Comment: 9 pages, 3 figures. Accepted in Phys. Rev. D

Published
2019
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49. Where do the AMS-02 antihelium events come from?

Author

Joseph Silk, Ilias Cholis, Pierre Salati, Marc Kamionkowski, Vivian Poulin, 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), 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), media_common.quotation_subject, nucleosynthesis: big bang, Dark matter, Cosmic background radiation, FOS: Physical sciences, helium: flux, Cosmic ray, Astrophysics, cosmic background radiation, 01 natural sciences, Orders of magnitude (bit rate), helium: nucleus, High Energy Physics - Phenomenology (hep-ph), GAPS, 0103 physical sciences, fission, cloud, Sensitivity (control systems), AMS, 010306 general physics, Astrophysics::Galaxy Astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, dark matter: annihilation, sensitivity, Galaxy, Universe, Baryon, baryon, flux, High Energy Physics - Phenomenology, inverse scattering method, 13. Climate action, gamma ray, cosmic radiation, hydrogen, [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, Astrophysics and astroparticle physics
Abstract

We discuss the origin of the anti-helium-3 and -4 events possibly detected by AMS-02. Using up-to-date semi-analytical tools, we show that spallation from primary hydrogen and helium nuclei onto the ISM predicts a $\overline{{}^3{\rm He}}$ flux typically one to two orders of magnitude below the sensitivity of AMS-02 after 5 years, and a $\overline{{}^4{\rm He}}$ flux roughly 5 orders of magnitude below the AMS-02 sensitivity. We argue that dark matter annihilations face similar difficulties in explaining this event. We then entertain the possibility that these events originate from anti-matter-dominated regions in the form of anti-clouds or anti-stars. In the case of anti-clouds, we show how the isotopic ratio of anti-helium nuclei might suggest that BBN has happened in an inhomogeneous manner, resulting in anti-regions with a anti-baryon-to-photon ratio $\bar{\eta}\simeq10^{-3}\eta$. We discuss properties of these regions, as well as relevant constraints on the presence of anti-clouds in our Galaxy. We present constraints from the survival of anti-clouds in the Milky-Way and in the early Universe, as well as from CMB, gamma-ray and cosmic-ray observations. In particular, these require the anti-clouds to be almost free of normal matter. We also discuss an alternative where anti-domains are dominated by surviving anti-stars. We suggest that part of the unindentified sources in the 3FGL catalog can originate from anti-clouds or anti-stars. AMS-02 and GAPS data could further probe this scenario., Comment: 16 pages, 4 figures. Comments welcome! v2: Discussion about constraints on anti-matter in our Galaxy and in the early Universe greatly improved. A number of typos corrected. Conclusions unaffected. Some Refs added. v3: some minor text corrections/improvements. updated to match published version

Published
2019
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50. Predictive model of BEC dark matter halos with a solitonic core and an isothermal atmosphere

Author

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

Subjects
Cosmology and Nongalactic Astrophysics (astro-ph.CO), Cold dark matter, Dark matter, FOS: Physical sciences, General Relativity and Quantum Cosmology (gr-qc), Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, General Relativity and Quantum Cosmology, 0103 physical sciences, 010306 general physics, Galaxy rotation curve, Astrophysics::Galaxy Astrophysics, Mathematical physics, Boson, Condensed Matter::Quantum Gases, Physics, 010308 nuclear & particles physics, Equation of state (cosmology), Fermion, Dark matter halo, 98.62.Gq, [PHYS.GRQC]Physics [physics]/General Relativity and Quantum Cosmology [gr-qc], Relaxation (physics), 95.35.+d, 95.30.Sf, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics and astroparticle physics
Abstract

International audience; We develop a model of Bose-Einstein condensate dark matter halos with a solitonic core and an isothermal atmosphere based on a generalized Gross-Pitaevskii equation [P. H. Chavanis, Eur. Phys. J. Plus 132, 248 (2017)EPJPA32190-544410.1140/epjp/i2017-11544-3]. This equation provides a heuristic coarse-grained parametrization of the ordinary Gross-Pitaevskii equation accounting for violent relaxation and gravitational cooling. It involves a cubic nonlinearity taking into account the self-interaction of the bosons, a logarithmic nonlinearity associated with an effective temperature, and a source of dissipation. It leads to superfluid dark matter halos with a core-halo structure. The quantum potential or the self-interaction of the bosons generates a solitonic core that solves the cusp problem of the cold dark matter model. The logarithmic nonlinearity generates an isothermal atmosphere accounting for the flat rotation curves of the galaxies. The dissipation ensures that the system relaxes towards an equilibrium configuration. In the Thomas-Fermi approximation, a dark matter halo is equivalent to a barotropic gas with an equation of state P=2πasℏ2ρ2/m3+ρkBT/m, where as is the scattering length of the bosons and m is their individual mass. We numerically solve the equation of hydrostatic equilibrium and determine the density profiles and rotation curves of dark matter halos. We impose that the surface density of the halos has the universal value Σ0=ρ0rh=141 M⊙/pc2 obtained from the observations. For a boson with ratio as/m3=3.28×103 fm/(eV/c2)3, we find a minimum halo mass (Mh)min=1.86×108 M⊙ and a minimum halo radius (rh)min=788 pc. This ultracompact halo corresponds to a pure soliton which is the ground state of the Gross-Pitaevskii-Poisson equation. For (Mh)min(Mh)* we find two branches of solutions corresponding to (i) purely isothermal halos without soliton and (ii) isothermal halos harboring a central soliton. The purely isothermal halos (gaseous phase) are stable. For Mh>(Mh)c=6.86×1010 M⊙, they are indistinguishable from the observational Burkert profile. For (Mh)*1012 M⊙ may undergo a gravothermal catastrophe leading ultimately to the formation of a supermassive black hole (for smaller halos, the gravothermal catastrophe is inhibited by quantum effects). We relate the bifurcation point and the point above which supermassive black holes may form to the canonical and microcanonical critical points (Mh)CCP=3.27×109 M⊙ and (Mh)MCP∼2×1012 M⊙ of the “thermal” self-gravitating bosonic gas. Our model has no free parameter so it is completely predictive. Extension of this model to noninteracting bosons and fermions will be presented in forthcoming papers.

Published
2019
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