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19 results on '"Moscoso, L."'

1. Multimessenger science reach and analysis method for common sources of gravitational waves and high-energy neutrinos

Author

Vedovato, G., Van, Elewyck V., Tse, M., Sutton, P., Salemi, F., Rollins, J., Re, V., Raffai, P., Prodi, G., Pradier, T., Papa, M.A., Moscoso, L., Márka, Z., Márka, S., Kouchner, A., Klimenko, S., Jones, G., Finley, C., Drago, M., Donzaud, C., Di, Palma I., Corsi, A., Chassande-Mottin, E., Bouhou, B., Bartos, I., Baret, B., Baret, B, Bartos, I, Bouhou, B, Chassande-Mottin, E, Corsi, A, Di Palma, I, Donzaud, C, Drago, M, Finley, C, Jones, G, Klimenko, S, Kouchner, A, Marka, S, Marka, Z, Moscoso, L, Papa, MA, Pradier, T, Prodi, G, Raffai, P, Re, V, Rollins, J, Salemi, F, Sutton, P, Tse, M, Van, Elewyck V, Vedovato, G, APC - Astrophysique des Hautes Energies (APC - AHE), Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO)-AstroParticule et Cosmologie (APC (UMR_7164)), 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)-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), AstroParticule et Cosmologie (APC (UMR_7164)), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Institut Pluridisciplinaire Hubert Curien (IPHC), Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA), 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)-Université Paris Diderot - Paris 7 (UPD7)-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), 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), and Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Strasbourg (UNISTRA)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Nuclear and High Energy Physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, muon, 0103 physical sciences, Neutrino, Range (statistics), Physics::Atomic and Molecular Clusters, 010306 general physics, Gravitational radiation detectors, 010303 astronomy & astrophysics, gamma-ray sources, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, mass spectrometers, and other instrumentation and techniques, Muon, Gravitational wave, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Detector, gamma-ray bursts, pion, Astronomy, cosmic ray detectors, and other elementary particle detectors, Galaxy, Supernova, Supernovae, 13. Climate action, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gamma-ray burst, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the baseline multimessenger analysis method for the joint observations of gravitational waves (GW) and high-energy neutrinos (HEN), together with a detailed analysis of the expected science reach of the joint search. The analysis method combines data from GW and HEN detectors, and uses the blue-luminosity-weighted distribution of galaxies. We derive expected GW+HEN source rate upper limits for a wide range of source parameters covering several emission models. Using published sensitivities of externally triggered searches, we derive joint upper limit estimates both for the ongoing analysis with the initial LIGO-Virgo GW detectors with the partial IceCube detector (22 strings) HEN detector and for projected results to advanced LIGO-Virgo detectors with the completed IceCube (86 strings). We discuss the constraints these upper limits impose on some existing GW+HEN emission models., Comment: *Corresponding author: ibartos@phys.columbia.edu

Published
2012

2. Sedimentation and Fouling of Optical Surfaces at the ANTARES Site

Author

Amram, P, Anghinolfi, M, Anvar, C, Ardellier-Desages, FE, Aslanides, E, Aubert, JJ, Azoulay, R, Bailey, D, Basa, S, Battaglieri, M, Belloti, R, Beltramelli, J, Benhammou, Y, Berthier, R, Bertin, V, Billault, M, Blaes, R, Bland, RW, Blondeau, F, de Botton, N, Boulesteix, J, Brooks, CB, Brunner, J, Cafagna, F, Calzas, A, Capone, A, Caponetto, L, Carloganu, C, Carmona, E, Carr, J, Cartwright, SL, Cecchini, S, Ciacio, F, Circella, M, Compere, C, Cooper, S, Coyle, P, Cuneo, S, Danilov, M, van Dantzig, R, De Marzo, C, Destelle, JJ, De Vita, R, Dispau, G, Druillole, F, Engelen, J, Feinstein, F, Ferdi, C, Festy, D, Fopma, J, Gallone, JM, Giacomelli, G, Goret, P, Gournay, JF, Hallewell, G, Heijboer, A, Hernandez-Rey, JJ, Hubbard, JR, Jaquet, M, de Jong, M, Karolak, M, Keller, P, Kooijman, P, Kouchner, A, Kudryavtsev, VA, Lafoux, H, Lagier, P, Lamare, P, Languillat, JC, Laubier, L, Laugier, JP, Leilde, B, Le Provost, H, Van Suu, AL, Lo Nigro, L, Lo Presti, D, Loucatos, S, Louis, F, Lyashuk, V, Magnier, P, Marcelin, M, Margiotta, A, Masullo, R, Mazeas, F, Mazeau, B, Mazure, A, McMillan, JE, Migneco, E, Millot, C, Mols, P, Montanet, F, Montaruli, T, Moscoso, L, Musumeci, M, Nezri, E, Nooren, GJ, Oberski, JEJ, Olivetto, C, Oppelt-Pohl, A, Palanque-Delabrouille, N, Papaleo, R, Payre, P, Perrin, P, Petruccetti, M, Petta, C, Piattelli, P, Poinsignon, J, Potheau, R, Queinec, Y, Racca, C, Raia, G, Randazzo, N, Rethore, F, Riccobene, G, Ricol, JS, Ripani, M, Roca-Blay, V, Romeyer, A, Rostovstev, A, Russo, GV, Sacquin, Y, Salusti, E, Schuller, JP, Schuster, W, Soirat, JP, Souvorova, O, Spooner, NJC, Spurio, M, Stolarczyk, T, Stubert, D, Taiuti, M, Tao, C, Thompson, LF, Tilav, S, Triay, R, Usik, A, Valdy, P, Valente, V, Varlamov, I, Vaudaine, G, Vernin, P, Vladimirsky, E, Vorobiev, M, Huberts, PD, de Wolf, E, Zakharov, V, Zavatarelli, S, Zornoza, JD, Zuniga, J, Aloisi, JC, Kerherve, P, Monaco, A, Collaboration, ANTARES, Collaboration, CEFREM, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches Subatomiques (IReS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Cancéropôle du Grand Est-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), ANTARES, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), ANTARES (IHEF, IoP, FNWI), Amram P., Anghinolfi M., Anvar S., Ardellier-Desages F.E., Aslanides E., Aubert J.-J., Azoulay R., Bailey D., Basa S., Battaglieri M., Bellotti R., Beltramelli J., Benhammou Y., Berthier R., Bertin V., Billault M., Blaes R., Bland R.W., Blondeau F., de Botton N., Boulesteix J., Brooks C.B., Brunner J., Cafagna F., Calzas A., Capone A., Caponetto L., Carloganu C., Carmona E., Carr J., Cartwright S.L., Cecchini S., Ciacio F., Circella M., Compere C., Cooper S., Coyle P., Cuneo S., Danilov M., van Dantzig R., de Marzo C., Destelle J.-J., de Vita R., Dispau G., Druillole F., Engelen J., Feinstein F., Ferdi C., Festy D., Fopma J., Gallone J.-M., Giacomelli G., Goret P., Gournay J.-F., Hallewell G., Heijboer A., Hernandez-Rey J.J., Hubbard J.R., Jaquet M., de Jong M., Karolak M., Keller P., Kooijman P., Kouchner A., Kudryavtsev V.A., Lafoux H., Lagier P., Lamare P., Languillat J.-C., Laubier L., Laugier J.-P., Leilde B., le Provost H., le Van Suu A., Lo Nigro L., Lo Presti D., Loucatos S., Louis F., Lyashuk V., Magnier P., Marcelin M., Margiotta A., Masullo R., Mazeas F., Mazeau B., Mazure A., McMillan J.E., Migneco E., Millot C., Mols P., Montanet F., Montaruli T., Moscoso L., Musumeci M., Nezri E., Nooren G.J., Oberski J.E.J., Olivetto C., Oppelt-Pohl A., Palanque-Delabrouille N., Papaleo R., Payre P., Perrin P., Petruccetti M., Petta C., Piattelli P., Poinsignon J., Potheau R., Queinec Y., Racca C., Raia G., Randazzo N., Rethore F., Riccobene G., Ricol J.-S., Ripani M., Roca-Blay V., Romeyer A., Rostovstev A., Russo G.V., Sacquin Y., Salusti E., Schuller J.-P., Schuster W., Soirat J.-P., Souvorova O., Spooner N.J.C., Spurio M., Stolarczyk T., Stubert D., Taiuti M., Tao C., Thompson L.F., Tilav S., Triay R., Usik A., Valdy P., Valente V., Varlamov I., Vaudaine G., Vernin P., Vladimirsky E., Vorobiev M., de Witt Huberts P., de Wolf E., Zakharov V., Zavatarelli S., Zornoza J. de D., Zuniga J., Aloisi J.-C., Kerherve P., Monaco A., and Damoiseaux, Magali

Subjects
Photomultiplier, Transmission loss, Equator, Mineralogy, FOS: Physical sciences, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Neutrino telescope, 01 natural sciences, law.invention, Telescope, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], High Energy Physics - Phenomenology (hep-ph), law, 0103 physical sciences, fouling, neutrino telescope, sea water properties, sedimentation, undersea cherenkov detectors, 14. Life underwater, 010306 general physics, Cherenkov radiation, Zenith, Physics, Undersea Cherenkov detectors, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), Sea water propertie, Astronomy and Astrophysics, Fouling, Sedimentation, High Energy Physics - Phenomenology, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Física nuclear, Neutrino
Abstract

ANTARES is a project leading towards the construction and deployment of a neutrino telescope in the deep Mediterranean Sea. The telescope will use an array of photomultiplier tubes to detect the Cherenkov light emitted by muons resulting from the interaction with matter of high energy neutrinos. In the vicinity of the deployment site the ANTARES collaboration has performed a series of in-situ measurements to study the change in light transmission through glass surfaces during immersions of several months. The average loss of light transmission is estimated to be only ~2% at the equator of a glass sphere one year after deployment. It decreases with increasing zenith angle, and tends to saturate with time. The transmission loss, therefore, is expected to remain small for the several year lifetime of the ANTARES detector whose optical modules are oriented downwards. The measurements were complemented by the analysis of the ^{210}Pb activity profile in sediment cores and the study of biofouling on glass plates. Despite a significant sedimentation rate at the site, in the 0.02 - 0.05 cm.yr^{-1} range, the sediments adhere loosely to the glass surfaces and can be washed off by water currents. Further, fouling by deposits of light-absorbing particulates is only significant for surfaces facing upwards., 18 pages, 14 figures (pdf), submitted to Astroparticle Physics

Published
2003

3. Search for Cosmic Neutrino Point Sources with Four Year Data of the ANTARES Telescope

Author

Adrián-Martínez, S., Samarai, Imen Al, Albert, A., André, M., Anghinolfi, M., Anton, G., Anvar, S., Ardid, M., Astraatmadja, T., Aubert , J., Baret, B., Basa, S., Bertin, V., Biagi, S., Bigongiari, C., Bogazzi, C., Bou-Cabo, M., Bouhou, B., Bouwhuis, M., Brunner, J., Busto, J., Capone, A., Carloganu, C., Carr, J., Cecchini, S., Charif, Z., Charvis, Ph., Chiarusi, T., Circella, M., Coniglione, R., Core, L., Costantini, H., Coyle, P., Creusot, A., Curtil, C., De Bonis, G., Decowski, P., Dekeyser, I., Deschamps, A., Distefano, C., Donzaud, C., Dornic, D., Dorosti, Q., Drouhin, D., Eberl, T., Emanuele, U., Enzenhöfer, A., Ernenwein, J., Escoffier, S., Fehn, K., Fermani, P., Ferri, M., Ferry, S., Flaminio, V., Folger, F., Fritsch, U., Fuda, J-L., Galatà, S., Gay, P., Geyer, K., Giacomelli, G., Giordano, V., Gleixner, A., Gómez-González, J., Graf, K., Guillard, G., Hallewell, G., Hamal, M., Van Haren, H., Heijboer, J., Hello, Y., Hernández-Rey, J., Herold, B., Hößl, J., Hsu, C., De Jong, M., Kadler, M., Kalekin, O., Kappes, A., Katz, U., Kavatsyuk, O., Kooijman, P., Kopper, C., Kouchner, A., Kreykenbohm, I., Kulikovskiy, V., Lahmann, R., Lambard, G., Larosa, G., Lattuada, D., Lefèvre, Dominique, Lim, G., Lo Presti, D., Loehner, H., Loucatos, S., Louis, F., Mangano, S., Marcelin, M., Margiotta, A., Martínez-Mora, J., Meli, A., Montaruli, T., Morganti, M., Moscoso, L., Motz, H., Neff, M., Nezri, E., Palioselitis, D., Păvălaş, E., Payet, K., Petrovic, J., Piattelli, P., Popa, V., Pradier, T., Presani, E., Racca, C., Reed, C., Riccobene, G., Richardt, C., Richter, R., Riviere, C., Robert, A., Roensch, K., Rostovtsev, A., Ruiz-Rivas, J., Rujoiu, M., Russo, G., Samtleben, D., Sanchez-Losa, A., Sapienza, P., Schmid, J., Schnabel, J., Schöck, F., Schuller, J., Schussler, F., Seitz, T., Shanidze, R., Simeone, F., Spies, A., Spurio, M., Steijger, J., Stolarczyk, Th., Taiuti, M., TAMBURINI, Christian, Trovato, A., Vallage, B., Vallée, Corentin, Van Elewyck, V., Vecchi, M., Vernin, P., Visser, E., Wagner, S., Wijnker, G., Wilms, J., De Wolf, E., Yepes, H., Zaborov, D., Zornoza, J., Zúñiga, J., Ernenwein, P., Leonora, E., Presti, D., Schuller, P., Institut d’Investigació per a la Gestió Integrada de Zones Costaneres (IGIC), Universitat Politècnica de València (UPV), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Swedish Institute of Space Physics [Uppsala] (IRF), Erlangen Centre for Astroparticle Physics (ECAP), Friedrich-Alexander Universität Erlangen-Nürnberg (FAU), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, National Institute for Subatomic Physics [Amsterdam] (NIKHEF), 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Enrico Fermi - Dipartimento di Fisica, University of Pisa - Università di Pisa, Instituto de Fisica Corpuscular (IFIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC)-Universitat de València (UV), Dipartimento di Fisica [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome] (UNIROMA), Laboratoire de Physique Corpusculaire - Clermont-Ferrand (LPC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Dipartimento di Fisica [Bologna], Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Géoazur (GEOAZUR 7329), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud]), Laboratori Nazionali del Sud (INFN), Istituto Nazionale di Fisica Nucleare (INFN), Centre d'océanologie de Marseille (COM), Université de la Méditerranée - Aix-Marseille 2-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Groupe de Recherche en Physique des Hautes Energies (GRPHE), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-IUT de Colmar, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Département de Physique des Particules (ex SPP) (DPhP), 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, Institute of Biological, Environmental and Rural Sciences (IBERS), Biotechnology and Biological Sciences Research Council (BBSRC)-Aberystwyth University, Franche-Comté Électronique Mécanique, Thermique et Optique - Sciences et Technologies (UMR 6174) (FEMTO-ST), Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Centre National de la Recherche Scientifique (CNRS)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC), Royal Netherlands Institute for Sea Research (NIOZ), Faculty of Technology, Delft University of Technology (TU Delft), Dipartimento di Fisica e Astronomia [Catania], Università degli studi di Catania = University of Catania (Unict), University of Groningen [Groningen], Département d'Electronique, des Détecteurs et d'Informatique pour la Physique (ex SEDI) (DEDIP), Physiologie & médecine expérimentale du Cœur et des Muscles [U 1046] (PhyMedExp), Institut National de la Santé et de la Recherche Médicale (INSERM)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Dept. of Physics, University of Wisconsin-Madison, Science Faculty CP230, Université libre de Bruxelles (ULB), Institute of Space Science [Bucharest-Măgurele] (ISS), Département Recherches Subatomiques (DRS-IPHC), Institut Pluridisciplinaire Hubert Curien (IPHC), Université de Strasbourg (UNISTRA)-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de 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), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Département de Physique Nucléaire (ex SPhN) (DPHN), instituto Geofísico, Escuela Politécnica Nacional (EPN), ANTARES, APC - Astrophysique des Hautes Energies (APC - AHE), 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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), 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)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), ANTARES (IHEF, IoP, FNWI), 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Department of Physics [Roma La Sapienza], Università degli Studi di Roma 'La Sapienza' = Sapienza University [Rome], Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de la Méditerranée - Aix-Marseille 2, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut Universitaire de Technologie de Colmar, Département de Physique des Particules (ex SPP) (DPP), IBERS, Institute of Biological, Environmental and Rural Sciences, Biotechnology and Biological Sciences Research Council, Université de Technologie de Belfort-Montbeliard (UTBM)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Franche-Comté (UFC), Université Bourgogne Franche-Comté [COMUE] (UBFC)-Université Bourgogne Franche-Comté [COMUE] (UBFC)-Centre National de la Recherche Scientifique (CNRS), Università degli studi di Catania [Catania], Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université de Strasbourg (UNISTRA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Montaruli, Teresa, S. Adrián-Martínez, I. Al Samarai, A. Albert, M. André, M. Anghinolfi, G. Anton, S. Anvar, M. Ardid, T. Astraatmadja, J-J. Aubert, B. Baret, S. Basa, V. Bertin, S. Biagi, C. Bigongiari, C. Bogazzi, M. Bou-Cabo, B. Bouhou, M. C. Bouwhui, J. Brunner, J. Busto, A. Capone, C. Cârloganu, J. Carr, S. Cecchini, Z. Charif, Ph. Charvi, T. Chiarusi, M. Circella, R. Coniglione, L. Core, H. Costantini, P. Coyle, A. Creusot, C. Curtil, G. De Boni, M. P. Decowski, I. Dekeyser, A. Deschamp, C. Distefano, C. Donzaud, D. Dornic, Q. Dorosti, D. Drouhin, T. Eberl, U. Emanuele, A. Enzenhöfer, J-P. Ernenwein, S. Escoffier, K. Fehn, P. Fermani, M. Ferri, S. Ferry, V. Flaminio, F. Folger, U. Fritsch, J-L. Fuda, S. Galatà, P. Gay, K. Geyer, G. Giacomelli, V. Giordano, A. Gleixner, J. P. Gómez-González, K. Graf, G. Guillard, G. Hallewell, M. Hamal, H. van Haren, A. J. Heijboer, Y. Hello, J. J. Hernández-Rey, B. Herold, J. Hößl, C. C. Hsu, M. de Jong, M. Kadler, O. Kalekin, A. Kappe, U. Katz, O. Kavatsyuk, P. Kooijman, C. Kopper, A. Kouchner, I. Kreykenbohm, V. Kulikovskiy, R. Lahmann, G. Lambard, G. Larosa, D. Lattuada, E. Leonora, D. Lefèvre, G. Lim, D. Lo Presti, H. Loehner, S. Loucato, F. Loui, S. Mangano, M. Marcelin, A. Margiotta, J. A. Martínez-Mora, A. Meli, T. Montaruli, M. Morganti, H. Motz, M. Neff, E. Nezri, D. Palioseliti, G. E. Păvălaş, K. Payet, J. Petrovic, P. Piattelli, V. Popa, T. Pradier, E. Presani, C. Racca, C. Reed, G. Riccobene, R. Richter, C. Rivière, A. Robert, K. Roensch, A. Rostovtsev, J. Ruiz-Riva, M. Rujoiu, D. F. E. Samtleben, P. Sapienza, J. Schmid, J. Schnabel, J-P. Schuller, F. Schüssler, T. Seitz, R. Shanidze, F. Simeone, A. Spie, M. Spurio, J. J. M. Steijger, Th. Stolarczyk, A. Sánchez-Losa, M. Taiuti, C. Tamburini, A. Trovato, B. Vallage, C. Vallée, V. Van Elewyck, M. Vecchi, P. Vernin, E. Visser, S. Wagner, G. Wijnker, J. Wilm, E. de Wolf, H. Yepe, D. Zaborov, J. D. Zornoza, J. Zúñiga, Institut de Recherches Subatomiques (IReS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Cancéropôle du Grand Est-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), National Institute for Subatomic Physics Nikhef [Amsterdam] (NIKHEF), Laboratoire Francis PERRIN (LFP - URA 2453), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC)-Universitat de València (UV), Universitat Politecnica de Valencia (UPV), 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), Università degli Studi di Roma 'La Sapienza' [Rome], Università di Bologna [Bologna] (UNIBO), Institut national des sciences de l'Univers (INSU - CNRS)-Institut de Recherche pour le Développement (IRD [France-Sud])-Centre National de la Recherche Scientifique (CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA), National Institute for Nuclear Physics (INFN), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Universitaire de Technologie de Colmar-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Université de Franche-Comté (UFC)-Centre National de la Recherche Scientifique (CNRS)-Ecole Nationale Supérieure de Mécanique et des Microtechniques (ENSMM)-Université de Technologie de Belfort-Montbeliard (UTBM), 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)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Département d'Electronique, des Détecteurs et d'Informatique (ex SEDI) (DEDI), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Université Libre de Bruxelles [Bruxelles] (ULB), Laboratoire des technologies de la microélectronique (LTM), Université Joseph Fourier - Grenoble 1 (UJF)-Commissariat à l'Énergie Atomique et aux Énergies Alternatives (CEA) - Grenoble-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Escuela Politécnica Nacional, Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), KVI - Center for Advanced Radiation Technology, S., Adrián-Martínez, I., Al Samarai, A., Albert, M., André, M., Anghinolfi, G., Anton, S., Anvar, M., Ardid, T., Astraatmadja, J-J., Aubert, B., Baret, S., Basa, V., Bertin, S., Biagi, C., Bigongiari, C., Bogazzi, M., Bou-Cabo, B., Bouhou, M. C., Bouwhui, J., Brunner, J., Busto, A., Capone, C., Cârloganu, J., Carr, S., Cecchini, Z., Charif, Ph., Charvi, T., Chiarusi, M., Circella, R., Coniglione, L., Core, H., Costantini, P., Coyle, A., Creusot, C., Curtil, G., De Boni, M. P., Decowski, I., Dekeyser, A., Deschamp, C., Distefano, C., Donzaud, D., Dornic, Q., Dorosti, D., Drouhin, T., Eberl, U., Emanuele, A., Enzenhöfer, J-P., Ernenwein, S., Escoffier, K., Fehn, P., Fermani, M., Ferri, S., Ferry, V., Flaminio, F., Folger, U., Fritsch, J-L., Fuda, S., Galatà, P., Gay, K., Geyer, G., Giacomelli, V., Giordano, A., Gleixner, J. P., Gómez-González, K., Graf, G., Guillard, G., Hallewell, M., Hamal, H., van Haren, A. J., Heijboer, Y., Hello, J. J., Hernández-Rey, B., Herold, J., Hößl, C. C., Hsu, M., de Jong, M., Kadler, O., Kalekin, A., Kappe, U., Katz, O., Kavatsyuk, P., Kooijman, C., Kopper, A., Kouchner, I., Kreykenbohm, V., Kulikovskiy, R., Lahmann, G., Lambard, G., Larosa, D., Lattuada, E., Leonora, D., Lefèvre, G., Lim, D., Lo Presti, H., Loehner, S., Loucato, F., Loui, S., Mangano, M., Marcelin, A., Margiotta, J. A., Martínez-Mora, A., Meli, T., Montaruli, M., Morganti, H., Motz, M., Neff, E., Nezri, D., Palioseliti, G. E., Păvălaş, K., Payet, J., Petrovic, P., Piattelli, V., Popa, T., Pradier, E., Presani, C., Racca, C., Reed, G., Riccobene, R., Richter, C., Rivière, A., Robert, K., Roensch, A., Rostovtsev, J., Ruiz-Riva, M., Rujoiu, D. F. E., Samtleben, P., Sapienza, J., Schmid, J., Schnabel, J-P., Schuller, F., Schüssler, T., Seitz, R., Shanidze, F., Simeone, A., Spie, M., Spurio, J. J. M., Steijger, Th., Stolarczyk, A., Sánchez-Losa, M., Taiuti, C., Tamburini, Trovato, A, B., Vallage, C., Vallée, V., Van Elewyck, M., Vecchi, P., Vernin, E., Visser, S., Wagner, G., Wijnker, J., Wilm, E., de Wolf, H., Yepe, D., Zaborov, J. D., Zornoza, and and J., Zúñiga

Subjects
cosmic neutrinos, UNIVERSE, Flux, Vela, 01 natural sciences, law.invention, High Energy Physics - Experiment, High Energy Physics - Experiment (hep-ex), law, SIGNALS, ABSORPTION, [PHYS.HEXP]Physics [physics]/High Energy Physics - Experiment [hep-ex], MAXIMUM-LIKELIHOOD, 010303 astronomy & astrophysics, ATMOSPHERIC MUONS, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), COSMIC cancer database, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], ASTRONOMY, neutrinos, astroparticle physics, Física nuclear, Neutrino, Astrophysics - High Energy Astrophysical Phenomena, REMNANT RX J1713.7-3946, Particle physics, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], Astrophysics::High Energy Astrophysical Phenomena, Neutrino telescope, [SDU.STU]Sciences of the Universe [physics]/Earth Sciences, FOS: Physical sciences, ddc:500.2, Telescope, cosmic rays, 0103 physical sciences, Point (geometry), ALGORITHM, Neutrinos, DETECTOR, Cosmic rays, UNDERWATER CHERENKOV NEUTRINO TELESCOPES, 010308 nuclear & particles physics, Astronomy and Astrophysics, HIGH-ENERGY PHOTONS, Space and Planetary Science, FISICA APLICADA, Astroparticle physics
Abstract

In this paper, a time-integrated search for point sources of cosmic neutrinos is presented using the data collected from 2007 to 2010 by the ANTARES neutrino telescope. No statistically significant signal has been found and upper limits on the neutrino flux have been obtained. Assuming an E ¿2 n; spectrum, these flux limits are at 1-10 ¿10¿8 GeV cm¿2 s¿1 for declinations ranging from ¿90° to 40°. Limits for specific models of RX J1713.7¿3946 and Vela X, which include information on the source morphology and spectrum, are also given., The authors acknowledge the financial support of the funding agencies: Centre National de la Recherche Scientifique (CNRS), Commissariat a l'energie atomique et aux energies alternatives (CEA), Commission Europeenne (FEDER fund and Marie Curie Program), Region Alsace (contrat CPER), Region Provence-Alpes-Cote d'Azur, Departement du Var and Ville de La Seyne-sur-Mer, France; Bundesministerium fur Bildung und Forschung (BMBF), Germany; Istituto Nazionale di Fisica Nucleare (INFN), Italy; Stichting voor Fundamenteel Onderzoek der Materie (FOM), Nederlandse organisatie voor Wetenschappelijk Onderzoek (NWO), the Netherlands; Council of the President of the Russian Federation for young scientists and leading scientific schools supporting grants, Russia; National Authority for Scientific Research (ANCS - UEFISCDI), Romania; Ministerio de Ciencia e Innovacion (MICINN), Prometeo of Generalitat Valenciana and MultiDark, Spain; Agence de l'Oriental and CNRST, Morocco. We also acknowledge the technical support of Ifremer, AIM, and Foselev Marine for the sea operation and the CC-IN2P3 for the computing facilities.

Published
2012

4. AMADEUS - The Acoustic Neutrino Detection Test System of the Deep-Sea ANTARES Neutrino Telescope

Author

Aguilar, J.A., Samarai, Imen Al, Albert, A., Anghinolfi, M., Anton, G., Anvar, S., Ardid, M., Assis Jesus, A.C., Astraatmadja, T., Aubert, J.-J., Auer, R., Barbarito, E., Baret, B., Basa, S., Bazzotti, M., Bertin, V., Biagi, S., Bigongiari, C., Bou-Cabo, M., Bouwhuis, M.C., Brown, A., Brunner, J., Busto, J., Camarena, F., Capone, A., Carminati, G., Carr, J., Cassano, B., Castorina, E., Cavasinni, V., Cecchini, S., Ceres, A., Charvis, Ph., Chiarusi, T., Chon Sen, N., Circella, M., Coniglione, R., Costantini, H., Cottini, N., Coyle, P., Curtil, C., De Bonis, G., Decowski, M.P., Dekeyser, I., Deschamps, Anne, Distefano, C., Donzaud, C., Dornic, D., Drouhin, D., Eberl, T., Emanuele, U., Ernenwein, J.-P., Escoffier, S., Fehr, F., Flaminio, V., Fritsch, U., Fuda, J.-L., Gay, Pascal, Giacomelli, G., G'Omez-Gonz'Alez, J.P., Graf, K., Guillard, G., Halladjian, G., Hallewell, G., Van Haren, H., Heijboer, A.J., Heine, E., Hello, Y., Hern'Andez-Rey, J.J., Herold, B., H¨oßl, J., De Jong, M., Kalantar-Nayestanaki, N., Kalekin, O., Kappes, A., Katz, U., Keller, P., Kooijman, P., Kopper, C., Kouchner, A., Kretschmer, W., Lahmann, R., Lamare, P., Lambard, G., Larosa, G., Laschinsky E, H., Le Provost, H., Lefèvre, Dominique, Lelaizant, G., Lim, G., Lo Presti, D., Loehner, H., Loucatos, S., Louis, F., Lucarelli, F., Mangano, S., Marcelin, M., Margiotta, A., Martinez-Mora, J.A., Mazure, A., Mongelli, M., Montaruli, T., Morganti, M., Moscoso, L., Motz, H., Naumann, C., Neff, M., Ostasch, R., Palioselitis, D., Payre, P., Petrovic, J., Picot Clémente, N., Picq, C., Popa, V., Pradier, T., Presani, E., Racca, C., Radu, A., Reed, C., Riccobene, G., Richardt, C., Rujoiu, M., Ruppi, M., Russo, G.V., Salesa, F., Sapienza, P., Schoeck, F., Schuller, J.-P., Shanidze, R., Simeone, F., Spurio, M., Steijger, J.J.M., Stolarczyk, Th., Taiuti, M., TAMBURINI, Christian, Tasca, L., Toscano, S., Vallage, B., Van Elewyck, V., Vannoni, G., Vecchi, M., Vernin, P., Wijnker, G., De Wolf, E., Yepes, H., Zaborov, D., Zornoza, J.D., Z'U˜niga, J., Cârloganu, C., Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Groupe de Recherche en Physique des Hautes Energies (GRPHE), Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-IUT de Colmar, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA)), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, 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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Géoazur (GEOAZUR 6526), Institut de Recherche pour le Développement (IRD)-Université Pierre et Marie Curie - Paris 6 (UPMC)-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), Centre d'océanologie de Marseille (COM), Université de la Méditerranée - Aix-Marseille 2-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Corpusculaire - Clermont-Ferrand (LPC), Université Blaise Pascal - Clermont-Ferrand 2 (UBP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut Pluridisciplinaire Hubert Curien (IPHC), Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), APC - Astrophysique des Hautes Energies (APC - AHE), 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)-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)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Département d'Electronique, des Détecteurs et d'Informatique pour la Physique (ex SEDI) (DEDIP), 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, ANTARES, Université de Haute-Alsace (UHA) Mulhouse - Colmar (Université de Haute-Alsace (UHA))-Institut Universitaire de Technologie de Colmar, 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), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), Observatoire de la Côte d'Azur, COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université de la Méditerranée - Aix-Marseille 2, 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)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO)-Alma Mater Studiorum Università di Bologna [Bologna] (UNIBO), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut Universitaire de Technologie de Colmar-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)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-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)-Dipartimento di Astronomia, Universita degli Studi di Bologna, Università di Bologna [Bologna] (UNIBO)-Università di Bologna [Bologna] (UNIBO), and Département d'Electronique, des Détecteurs et d'Informatique (ex SEDI) (DEDI)

Subjects
Thermo-acoustic model, [PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], ANTARES, [SDU.ASTR.HE]Sciences of the Universe [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [SPI.OPTI]Engineering Sciences [physics]/Optics / Photonic, 95.55.Vj, 95.85.Ry, 13.15.+g, 43.30.+m, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], AMADEUS, Neutrino telescope, Acoustic neutrino detection
Abstract

The AMADEUS system described in this article is integrated into the ANTARES neutrino telescope in the Mediterranean Sea and aims at the investigation of techniques for acoustic detection of neutrinos in the deep sea. Installed at water depths between 2000 and 2400m, its acoustic sensors employ piezo-electric elements for the broad-band recording of signals with frequencies ranging up to 125 kHz with typical sensitivities around −145 dB re. 1V/μPa (including preamplifier). Completed in May 2008, AMADEUS consists of six "acoustic clusters", each comprising six acoustic sensors that are arranged at distances of roughly 1m from each other. Three acoustic clusters each are installed along two vertical mechanical structures (so-called lines) of the ANTARES detector at a horizontal distance of 240m. Vertical spacings within a line range from 15m to 125m. Each cluster contains custom-designed electronics boards to amplify and digitise the acoustic data from the sensors. The data transmission to shore is done via optical fibres, using the TCP/IP protocol. An on-shore computer cluster, currently consisting of four dedicated servers, is used to process, filter and store the selected data. The daily volume of recorded data is about 10 - 20 GByte. The system is operating continuously and automatically, requiring only little human intervention. AMADEUS allows for extensive studies of both transient signals and ambient noise in the deep sea as well as signal correlations on several length scales and localisation of acoustic point sources. Thus the system is excellently suited to assess the background conditions that affect the measurement of bipolar pulses expected to originate from neutrino interactions. This in turn allows for feasibility studies of a future large-scale acoustic neutrino telescope in the Mediterranean Sea.

Published
2010

5. AGAPEROS: Searches for microlensing in the LMC with the Pixel Method - 1, Data treatment and pixel light curves production

Author

Melchior, A L., Afonso, C., Ansari, R., Aubourg, E., Baillon, P., Bareyre, P., Bauer, F., Beaulieu, J.P., Bouquet, A., Brehin, S., Cavalier, F., Char, S., Couchot, F., Coutures, C., Ferlet, R., Fernandez, J., Gaucherel, C., Giraud-Heraud, Y., Glicenstein, J.F., Goldman, B., Gondolo, P., Gros, M., Guibert, J., Gry, C., Hardin, D., Kaplan, J., De Kat, J., Lachieze-Rey, M., Laurent, B., Lesquoy, E., Magneville, C., Mansoux, B., Marquette, J B., Maurice, E., Milsztajn, A., Moniez, M., Moreau, O., Moscoso, L., Palanque-Delabrouille, N., Perdereau, O., Prevot, L., Renault, C., Queinnec, F., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), EROS, 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), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics and Astronomy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

The presence and abundance of MAssive Compact Halo Objects (MACHOs) towards the Large Magellanic Cloud (LMC) can be studied with microlensing searches. The 10 events detected by the EROS and MACHO groups suggest that objects with 0.5 Mo could fill 50% of the dark halo. This preferred mass is quite surprising, and increasing the presently small statistics is a crucial issue. Additional microlensing of stars too dim to be resolved in crowded fields should be detectable using the Pixel Method. We present here an application of this method to the EROS 91-92 data (one tenth of the whole existing data set). We emphasize the data treatment required for monitoring pixel fluxes. Geometric and photometric alignments are performed on each image. Seeing correction and error estimates are discussed. 3.6" x 3.6" super-pixel light curves, thus produced, are very stable over the 120 days time-span. Fluctuations at a level of 1.8% of the flux in blue and 1.3% in red are measured on the pixel light curves. This level of stability is comparable with previous estimates. The data analysis dedicated to the search of possible microlensing events together with refined simulations will be presented in a companion paper. Recent surveys monitoring millions of light curves of resolved stars in the LMC have discovered several microlensing events. Unresolved stars could however significantly contribute to the microlensing rate towards the LMC. Monitoring pixels, as opposed to individual stars, should be able to detect stellar variability as a variation of the pixel flux. We present a first application of this new type of analysis (Pixel Method) to the LMC Bar. We describe the complete procedure applied to the EROS 91-92 data (one tenth of the existing CCD data set) in order to monitor pixel fluxes. First, geometric and photometric alignments are applied to each images. Averaging the images of each night reduces significantly the noise level. Second, one light curve for each of the 2.1 10^6 pixels is built and pixels are lumped into 3.6"x3.6" super-pixels, one for each elementary pixel. An empirical correction is then applied to account for seeing variations. We find that the final super-pixel light curves fluctuate at a level of 1.8% of the flux in blue and 1.3% in red. We show that this noise level corresponds to about twice the expected photon noise and confirms previous assumptions used for the estimation of the contribution of unresolved stars. We also demonstrate our ability to correct very efficiently for seeing variations affecting each pixel flux. The technical results emphasised here show the efficacy of the Pixel Method and allow us to study luminosity variations due to possible microlensing events and variable stars in two companion papers.

Published
1999

6. A Deep Sea Telescope for High Energy Neutrinos

Author

Aslanides, E., Aubert, J. J., Basa, S., Bernard, F., Bertin, V., Billault, M., Blanc, P. E., Brunner, J., Calzas, A., Cassol, F., Carr, J., Carloganu, C., Destelle, J. J., Duval, P. Y., Hubaut, F., Kajfasz, E., Jaquet, M., Laugier, D., Le Suu, A., Liotard, P. L., Martin, L., Montanet, F., Navas, S., Olivetto, C., Payre, P., Pohl, A., Potheau, R., Raymond, M., Talby, M., Tao, C., Vigeolas, E., Anvar, S., Azoulay, R., Bland, R. W., Blondeau, F., Botton, N., Bottu, N., Carton, H., Deck, P., Desages, F. E., Dispau, G., Feinstein, F., Goret, P., Gosset, L., Gournay, F., Hubbard, J. R., Karolak, M., Antoine Kouchner, Lachartre, D., Lafoux, H., Lamare, P., Languillat, J. C., Laugier, J. P., Le Provost, H., Loucatos, S., Magnier, P., Mazeau, B., Mols, P., Moscoso, L., Palanque-Delabrouille, N., Perrin, P., Poinsignon, J., Queinec, Y., Sacquin, Y., Schuller, P., Stolarczyk, T., Tabary, A., Tayalati, Y., Vernin, P., Vignaud, D., Vilanova, D., Benhammou, Y., Drouhin, F., Huss, D., Pallares, A., Tzvetanov, T., Danilov, M., Kagan, R., Rostovstev, A., Carmona, E., Cases, R., Hernandez, J. J., Zuniga, J., Racca, C., Zghiche, A., Dantzig, R., Engelen, J., Heijboer, A., Jong, M., Kok, E., Kooijman, P., Nooren, G. J., Oberski, J., Witt Huberts, P., Wolf, E., Evans, D., Mahout, G., Kenyon, I., Jovanovic, P., Newman, P., Mcmahon, T., Cooper, S., Fopma, J., Jelley, N., Schuster, W., Tilav, S., Wark, D., Cartwright, S., Kudryavtsev, V., Mcmillan, J., Spooner, N., Thompson, L., Triay, R., Mazure, A., Amram, P., Boulesteix, J., Marcelin, M., Blanc, F., Coustillier, G., Fuda, J. L., Millot, C., Drogou, J. F., Festy, D., Herrouin, G., Le Guen, Y., Lemoine, L., Massol, A., Mazeas, F., Jean-Pierre Morel, Rolin, J. F., Valdy, P., Brooks, B., Compere, C., Centre de Physique des Particules de Marseille (CPPM), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), Institut de Recherches Subatomiques (IReS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Cancéropôle du Grand Est-Université Louis Pasteur - Strasbourg I-Centre National de la Recherche Scientifique (CNRS), ANTARES, and Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Physics::Instrumentation and Detectors, High Energy Physics::Experiment
Abstract

The ANTARES Collaboration proposes to construct a large area water Cherenkov detector in the deep Mediterranean Sea, optimised for the detection of muons from high-energy astrophysical neutrinos. This paper presents the scientific motivation for building such a device, along with a review of the technical issues involved in its design and construction. The observation of high energy neutrinos will open a new window on the universe. The primary aim is to study particle acceleration mechanisms in energetic astrophysical objects such as AGN's and GRB's, which may also shed light on the origin of ultra-high-energy cosmic rays. At lower energies, non-baryonic dark matter may be detected through the neutrinos produced when gravitationally captured WIMPs annihilate in the cores of the Earth and the Sun. Neutrino oscillations can be measured by studying distortions in the energy spectrum of upward-going atmospheric nu's. The characteristics of the proposed site are an important consideration in detector design. Water properties and detector environment parameters were measured. These tests have shown that the proposed site provides a good-quality environment for the detector, and have also demonstrated the feasibility of the deployment technique. The present proposal concerns the construction and deployment of a detector with surface area 0.1 km^2. The conceptual design for such a detector is discussed, and the physics performance evaluated. An overview of costs and schedules is presented. It is concluded that a 0.1 km^2 detector is technically feasible at realistic cost, and offers an exciting and varied physics and astrophysics programme. Such a detector will also provide practical experience which will be invaluable in the design and operation of future detectors on the astrophysically desirable 1 km^2 scale.

Published
1999

7. The effect of metallicity on the Cepheid distance scale and its implications for the Hubble constant ($H_0$) determination

Author

Beaulieu, J. P., Sasselov, D. D., Renault, C., Grison, P., Ferlet, R., Vidal-Madjar, A., Maurice, E., Prévot, L., Aubourg, E., Bareyre, P., Brehin, S., Coutures, C., Delabrouille, N., de Kat, J., Gros, M., Laurent, B., Lachièze-Rey, M., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Queinnec, F., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Ansari, R., Cavalier, F., Moniez, M., Gry, C., Guibert, J., Moreau, O., Tajhmady, F., Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), 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), Centre d'Analyse des Images de l'INSU (CENTRE D'ANALYSE DES IMAGES DE L'INSU), Centre National de la Recherche Scientifique (CNRS), EROS, Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), and 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)

Subjects
galaxies : distances, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars : fundamental parameters, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics, Stars : cepheids
Abstract

Recent HST determinations of the expansion's rate of the Universe (the Hubble constant, H_0) assumed that the Cepheid Period-Luminosity relation at V and I are independent of metallicity (Freedman, et al., 1996, Saha et al., 1996, Tanvir et al., 1995). The three groups obtain different vales for H_0. We note that most of this discrepancy stems from the asumption (by both groups) that the Period-Luminosity relation is independent of metallicity. We come to this conclusion as a result of our study of the Period-Luminosity relation of 481 Cepheids with 3 millions two colour measurements in the Large Magellanic Cloud and the Small Magellanic Cloud obtained as a by-product of the EROS microlensing survey. We find that the derived interstellar absorption corrections are particularly sensitive to the metallicity and when our result is applied to recent estimates based on HST Cepheids observations it makes the low-H_0 values higher and the high-H_0 value lower, bringing those discrepant estimates into agrement around $H_0 \approx 70 km/s Mpc^{-1}$., Comment: 4 pages, Latex, with 2 .ps accepted for publication astronomy and astrophysics Letters

Published
1997

8. ANTARES Proposal: Towards a Large Scale High Energy Cosmic Neutrino - undersea detector

Author

Amram, P., Arpesella, C., Aslanides, E., Aubert, J.J., Azoulay, R., Bailey, D., Basa, S., Berthier, R., Bertin, V., Billault, M., Biller, S., Blanc, F., Blanc, P.E., Blondeau, F., Boulesteix, J., Brooks, B., Calzas, A., Carloganu, C., Carr, J., Carton, P H., Cases, R., Cribier, M., de Botton, N., Desages, F., Destelle, J.J., Dispau, G., Drogou, J F., Feinstein, F., Festy, D., Fuda, J.-L., Galumian, P., Goret, P., Gosset, L., Gournay, J F., Hernandez, J J., Herrouin, G., Hubaut, F., Jelley, N., Kajfasz, E., Lachartre, D., Lamare, P., Languillat, J C., Laubier, L., Laugier, J P., Le Gac, R., Le Provost, H., Le van Suu, A., Lemoine, L., Loiseau, D., Loucatos, S., Magnier, P., Marcelin, M., Martin, Lilian, Mazeas, F., Mazure, A., Mcnutt, J., Meessen, C., Millot, C., Mols, P., Montanet, F., Moorhead, M E., Moscoso, L., Navas, S., Olivetto, C., Payre, P., Perrin, P., Poinsignon, J., Potheau, R., Raymond, M., Sacquin, Y., Schuller, J P., Soirat, J P., Tabary, A., Talby, M., Triay, R., Valdy, P., Velasco, J., Vigeolas, E., Vignaud, D., Vilanova, D., Wark, D., Zuniga, J., Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and ANTARES

Subjects
Physics::Instrumentation and Detectors
Abstract

The ANTARES collaboration propose to observe high energy cosmic neutrinos using a deep sea Cherenkov detector. The sky survey with high energy neutrinos is complementary to the observations with photons and will shed a new light on the understanding of the origin of cosmics rays. We propose to explore the possibility of a km-scale detector to be installed in a deep site in the Mediterranean sea, for which a broad collaboration will be needed. With the help of collaborators and partners which have experience in sea science engineering (COM, CSTN, CTME, IFREMER, France Télécom Câbles, INSU-CNRS...) we will test the sea engineering part of a detector including test deployments close to the Toulon coast (France) where technical support is available and where several sites at depths down to 2500~m are easily accessible. We propose to build and install a demonstrator (a fully equipped 3-dimensional test array) the design of which can be extended to a km-scale detector. During the same time, autonomous systems allowing to measure undersea optical parameters in view of the selection of a site for the future km-scale detector will be realized.

Published
1997

9. Eros Variable Stars: Discovery of Beat Cepheids in the Small Magellanic Cloud and the effect of metallicity on pulsation

Author

Beaulieu, J P., Krockenberger, M., Sasselov, D D., Renault, C., Ferlet, R., Vidal-Madjar, A., Maurice, E., Prvt, L., Aubourg, E., Bareyre, P., Brehin, S., Coutures, C., Delabrouille, N., De Kat, J., Gros, M., Laurent, B., Lachize-Rey, M., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Queinnec, F., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Ansari, R., Cavalier, F., Moniez, M., Gry, C., Lantz, Simone, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), and 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)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Information need, Bibliographic database, Astrophysics (astro-ph), FOS: Physical sciences, Open access, Information market, Astrophysics, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Scientific research, Electronic document, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Scientific technical information, Technological watch, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Publication, Firm cooperation
Abstract

We report the discovery of eleven beat Cepheids in the Small Magellanic Cloud, using data obtained by the EROS microlensing survey. Four stars are beating in the fundamental and first overtone mode (F/1OT), seven are beating in the first and second overtone (1OT/2OT). The SMC F/1OT ratio is systematically higher than the LMC F/1OT, while the 1OT/2OT period ratio in the SMC Cepheids is the same as the LMC one., 4 pages, Latex file with 4 .ps figures. accepted for publication in A A Letters

Published
1997

10. Metallicity Effects on the Cepheid Extragalactic Distance Scale from EROS photometry in LMC and SMC

Author

Sasselov, D.D., Beaulieu, J.P., Renault, C., Grison, P., Ferlet, R., Vidal-Madjar, A., Maurice, E., Prévot, L., Aubourg, E., Bareyre, P., Brehin, S., Coutures, C., Delabrouille, N., De Kat, J., Gros, M., Laurent, B., Lachièze-Rey, M., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Queinnec, F., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Ansari, R., Cavalier, F., Moniez, M., Gry, C., Guibert, J., Moreau, O., Tajhmady, F., Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Centre d'Analyse des Images de l'INSU (CENTRE D'ANALYSE DES IMAGES DE L'INSU), Centre National de la Recherche Scientifique (CNRS), Girod, Dominique, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and 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)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics
Abstract

This is an investigation of the period-luminosity relation of classical Cepheids in samples of different metallicity. It is based on 481 Cepheids in the Large and Small Magellanic Clouds from the blue and red filter CCD observations (most similar to V_J & R_J) of the French EROS microlensing project. The data-set is complete and provides an excellent basis for a differential analysis between LMC and SMC. In comparison to previous studies of effects on the PL-relation, the EROS data-set offers extremely well-sampled light curves and well-filled instability strips. This allows reliable separation of Cepheids pulsating in the fundamental and the first overtone mode and derivation of differential reddening. Our main result concerns the determination of distances to galaxies which are inferred by using the LMC as a base and using two color photometry to establish the amount of reddening. We find a zero-point offset between SMC and LMC which amounts to a difference between inferred and true distance modulus of 0.14 \pm 0.06 mag in the VI_c system. The offset is exactly the same in both sets of PL-relations - of the fundamental and of the first overtone mode Cepheids. No effect is seen on the slopes of the PL-relations, although the fundamental and the first overtone mode Cepheids have different PL slopes. We attribute the color and the zero-point offset to the difference in metallicity between the SMC and LMC Cepheids. A metallicity effect of that small magnitude still has important consequencies for the inferred Cepheid distances and the determination of H_0. When applied to recent estimates based on HST Cepheid observations, our metallicity dependence makes the low-H_0 values (Sandage et al. 1994) higher and the high-H_0 values (Freedman et al. 1994b) lower, thus bringing those, 14 pages, Latex, with 8 .ps accepted for publication in astronomy and astrophysics

Published
1997

11. Observational Limits on Machos in the Galactic Halo

Author

EROS Collaboration, Renault, C., Afonso, C., Aubourg, E., Bareyre, P., Bauer, F., Brehin, S., Coutures, C., Gaucherel, C., Glicenstein, J. F., Goldman, B., Gros, M., Hardin, D., de Kat, J., Lachieze-Rey, M., Laurent, B., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Palanque-Delabrouille, N., Queinnec, F., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Ansari, R., Cavalier, F., Couchot, F., Mansoux, B., Moniez, M., Perdereau, O., Beaulieu, J. -Ph., Ferlet, R., Grison, Ph., Vidal-Madjar, A., Guibert, J., Moreau, O., Maurice, E., Prevot, L., Gry, C., Char, S., Fernandez, J., Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'Analyse des Images de l'INSU (CENTRE D'ANALYSE DES IMAGES DE L'INSU), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), EROS, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), and Girod, Dominique

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics
Abstract

We present final results from the first phase of the EROS search for gravitational microlensing of stars in the Magellanic Clouds by unseen deflectors (machos: MAssive Compact Halo Objects). The search is sensitive to events with time scales between 15 minutes and 200 days corresponding to deflector masses in the range 1.e-7 to a few solar masses. Two events were observed that are compatible with microlensing by objects of mass of about 0.1 Mo. By comparing the results with the expected number of events for various models of the Galaxy, we conclude that machos in the mass range [1.e-7, 0.02] Mo make up less than 20% (95% C.L.) of the Halo dark matter., 4 pages, 3 Postscript figures, to be published in Astronomy & Astrophysics

Published
1996

12. Experimental limits on the contribution of sub-stellar and stellar objects to the galactic halo

Author

Ansari, R., Cavalier, F., Moniez, M., Aubourg, E., Bareyre, P., Brehin, S., Gros, M., Lachieze-Rey, M., Laurent, B., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Queinnec, F., Renault, C., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Beaulieu, J.-P., Ferlet, R., Grison, Ph., Vidal-Madjar, A., Guibert, J., Moreau, O., Tajahmady, F., Maurice, E., Prevot, L., Gry, C., Laboratoire de l'Accélérateur Linéaire (LAL), 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), Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Centre d'Analyse des Images de l'INSU (CENTRE D'ANALYSE DES IMAGES DE L'INSU), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), EROS, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), and Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

EROS (Exp\'erience de Recherche d'Objets Sombres) has been monitoring the luminosity of 4 million stars in the Large Magellanic Cloud in order to search for gravitational microlensing by unseen objects in the galactic halo. We present here the results from 3 years of EROS Schmidt plates data. Two stars exhibit light curves that are consistent with a sizeable microlensing effect. CCD data obtained later on revealed that one of these stars is an eclipsing binary system. Combining Schmidt plates data and the published results from our 16 CCD camera, we set upper limits on the number of unseen objects in the halo in the mass range $[10^{-7},1]\Msol$. (Submitted for publication in Astronomy and Astrophysics), Comment: LaTex File (using A&A macros) without figure. The Complete paper is available via WWW at http://www.lal.in2p3.fr/EROS/eros.html and via anon FTP at ftp://ftp.lal.in2p3.fr/pub/Eros/Papiers (see index files)

Published
1995

13. Determination of the atmospheric neutrino spectra with the Frejus detector

Author

Daum, K., Rhode, W., Bareyre, P., Barloutaud, R., Chardin, G., Degrange, B., Ernwein, J., Kuznik, B., Meyer, H., Mosca, L., Moscoso, L., Perdereau, O., Schubnell, M., Tisserant, S., Wei, Y., Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), and FREJUS

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
Published
1995

14. Eros variable stars: fundamental-mode and first-overtone cepheids in the bar of the large magellanic cloud

Author

Yasu, Y., Ferlet, R., Vidal-Madjar, A., Maurice, E., Prevot, L., Gry, C., Guibert, J., Moreau, O., Tajahmady, F., Aubourg, E., Bareyre, P., Brehin, S., Gros, M., Lachieze-Rey, M., Laurent, B., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Queinnec, F., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Ansari, R., Cavalier, F., Moniez, M., 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), and EROS

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present CCD phase-binned light curves at 490\,nm for 97 Cepheid variable stars in the bar of the LMC. The photometry was obtained as part of the French EROS project and has excellent phase coverage, permitting accurate decomposition into Fourier components. We identify as `sinusoidal' or s-Cepheids those stars with periods less than 5.5\,d and small second-harmonic components. These stars comprise $\sim$30\% of our sample and most form a sequence $\sim$1 mag\ brighter than the LMC classical Cepheids in the period-luminosity diagram. They are also generally bluer and have lower-amplitude light curves. We infer that the s-Cepheids are first-overtone pulsators because, when their periods are converted to expected fundamental-mode values, they obey a common period-luminosity-colour relation with classical Cepheids. This also confirms the reality of the colour term in the Cepheid period-luminosity-colour relation. Further, the blue edge of the classical Cepheid instability strip agrees well with the theoretical calculations for the fundamental mode made by Chiosi et al.\ (1993) for the Hertzsprung-Russell and period-luminosity diagrams, but we find that our observed s-Cepheids are $>0.2$\,mag\ brighter and bluer than the Chiosi et al.\ predictions for the first-overtone. We identify a number of features in plots of our stars' Fourier-component amplitude ratios and phase differences. These features have been identified with resonances between different pulsation modes. In the LMC we find these features seem to occur at periods very similar to Galactic ones for classical Cepheids, but at different periods for s-Cepheids. We discover a double-mode Cepheid in the LMC, for which $P({\rm first\ overtone})/P({\rm fundamental}) = 0.710 \pm 0.001$, very similar to observed ratios for Galactic double-mode Cepheids.

Published
1995

15. Eros catalogue of eclipsing binary stars in the bar of the large magellanic cloud

Author

Ferlet, R., Vidal-Madjar, A., Maurice, E., Prevot, L., Gry, C., Guibert, J., Moreau, O., Tajahmady, F., Aubourg, E., Bareyre, P., Brehin, S., Gros, M., Lachieze-Rey, M., Laurent, B., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Queinnec, F., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Ansari, R., Cavalier, F., Moniez, M., 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), and EROS

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], e-book, business model, publishing, digital library, GeneralLiterature_REFERENCE(e.g.,dictionaries,encyclopedias,glossaries)
Abstract

Digitalization is everywhere in publihing process but difficulties still remain on e-books business. Digital libraries show new ways for e-books dissemination. Publishing and libraries economy will be re-built on different foundations in the future.

Published
1995

16. Search for very low-mass objects in the galactic halo

Author

EROS Collaboration, Aubourg, E., Bareyre, P., Brehin, S., Gros, M., Lachieze-Rey, M., Laurent, B., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Queinnec, F., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Ansari, R., Cavalier, F., Moniez, M., Beaulieu, J. P., Ferlet, R., Grison, Ph., Vidal-Madjar, A., Maurice, E., Prevot, L., Gry, C., Guibert, J., Moreau, O., Tajahmady, F., 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), and EROS

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We present results from a search for gravitational microlensing of stars in the Large Magellanic Cloud by low mass objects in the Galactic Halo. The search uses the CCD light curves of about 82,000 stars with up to 46 measurements per night over a period of 10 months. No light curve exhibits a form that is consistent with a microlensing event of maximum amplification greater than 1.2. This null result makes it unlikely that the Halo is dominated by objects in the mass range $5 10^{-8}M_{\odot} < M, to appear in Astronomy & Astrophysics (Accepted for publication in January 1995), 5 pages in uuencoded, compressed postscript, including figures

Published
1995

17. The Eros search for dark halo objects

Author

Aubourg, E., Babeyre, P., Brehin, S., Gros, M., Lachieze-Rey, M., Laurent, B., Lesquoy, E., Magneville, C., Milsztajn, A., Moscoso, L., Queinnez, F., Rich, J., Spiro, M., Vigroux, L., Zylberajch, S., Ansari, R., Cavalier, F., Moniez, M., Beaulieu, J.P., Ferlet, R., Grison, Ph., Vidal-Madjar, A., Guibert, J., Moreau, O., Tajahmady, F., Maurice, E., Prevot, L., Gry, C., 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), and EROS

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO]
Published
1993

18. Multimessenger astronomy with gravitational waves and high-energy neutrinos

Author

Caltech, ; California Institute of Technology - CALTECH, APC - AHE ; AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot - CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, APC - ADAMIS ; AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot - CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, Service d'Electronique, des Détecteurs et d'Informatique (SEDI) ; CEA, Department of Physics ; Columbia University, LIGO Laboratory ; California Institute of Technology, Albert-Einstein-Institut ; Max-Planck-Institut, Laboratoire d'Annecy le Vieux de Physique des Particules (LAPP) ; CNRS - IN2P3 - Université de Savoie, Department of Physics [Beer-Sheva] ; Ben Gurion University, Oskar Klein Centre and Department of Physics ; Stockholm University, Department of Physics and Optical Engineering ; ORT Braude, Observatory of Rome ; INAF, Dept. of Physics ; University of Wisconsin-Madison, School of Physics and Astronomy ; Cardiff University, University of Minnesota ; University of Minnesota, Division of Theoretical Astronomy ; National Astronomical Observatory of Japan, Department of applied physics ; Fukuoka University, Racah Institute of Physics ; Hebew University of Jerusalem, Institut Pluridisciplinaire Hubert Curien (IPHC) ; CNRS - Université de Strasbourg, Instituto Argentino de Radioastronomia ; CONICET - IAR - CCT La Plata, Department of Physics and Astrophysics ; The Weizmann Institute of Science, Ando, S., Baret, B., Bouhou, B., Chassande-Mottin, E., Kouchner, A., Moscoso, L., Van Elewyck, V., Bartos, I., Márka, S., Márka, Z., Corsi, A., Di Palma, I., Papa, M. A., Dietz, A., Donzaud, C., Eichler, D., Finley, C., Guetta, D., Halzen, F., Jones, G., Sutton, P. J., Kandhasamy, S., Mandic, V., Thrane, E., Kotake, K., Piran, T., Pradier, T., Romero, G. E., Waxman, E., Caltech, ; California Institute of Technology - CALTECH, APC - AHE ; AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot - CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, APC - ADAMIS ; AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot - CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, Service d'Electronique, des Détecteurs et d'Informatique (SEDI) ; CEA, Department of Physics ; Columbia University, LIGO Laboratory ; California Institute of Technology, Albert-Einstein-Institut ; Max-Planck-Institut, Laboratoire d'Annecy le Vieux de Physique des Particules (LAPP) ; CNRS - IN2P3 - Université de Savoie, Department of Physics [Beer-Sheva] ; Ben Gurion University, Oskar Klein Centre and Department of Physics ; Stockholm University, Department of Physics and Optical Engineering ; ORT Braude, Observatory of Rome ; INAF, Dept. of Physics ; University of Wisconsin-Madison, School of Physics and Astronomy ; Cardiff University, University of Minnesota ; University of Minnesota, Division of Theoretical Astronomy ; National Astronomical Observatory of Japan, Department of applied physics ; Fukuoka University, Racah Institute of Physics ; Hebew University of Jerusalem, Institut Pluridisciplinaire Hubert Curien (IPHC) ; CNRS - Université de Strasbourg, Instituto Argentino de Radioastronomia ; CONICET - IAR - CCT La Plata, Department of Physics and Astrophysics ; The Weizmann Institute of Science, Ando, S., Baret, B., Bouhou, B., Chassande-Mottin, E., Kouchner, A., Moscoso, L., Van Elewyck, V., Bartos, I., Márka, S., Márka, Z., Corsi, A., Di Palma, I., Papa, M. A., Dietz, A., Donzaud, C., Eichler, D., Finley, C., Guetta, D., Halzen, F., Jones, G., Sutton, P. J., Kandhasamy, S., Mandic, V., Thrane, E., Kotake, K., Piran, T., Pradier, T., Romero, G. E., and Waxman, E.

Abstract

Revised version, to appear in Reviews of Modern Physics (Colloquium Series). Section II on Potential GW+HEN emitters thoroughly updated. Section IV expanded with recent experimental results from joint GW+HEN searches with ANTARES, IceCube, LIGO and VIRGO, and with an extended discussion of the reach and implications of future searches., Many of the astrophysical sources and violent phenomena observed in our Universe are potential emitters of gravitational waves (GW) and high-energy neutrinos (HEN). Both GWs and HENs may escape very dense media and travel unaffected over cosmological distances, carrying information from the innermost regions of the astrophysical engines. Such messengers could also reveal new, hidden sources that have not been observed by conventional photon-based astronomy. Coincident observation of GWs and HENs may thus play a critical role in multimessenger astronomy. This is particularly true at the present time owing to the advent of a new generation of dedicated detectors: IceCube, ANTARES, VIRGO and LIGO. Given the complexity of the instruments, a successful joint analysis of this data set will be possible only if the expertise and knowledge of the data is shared between the two communities. This review aims at providing an overview of both theoretical and experimental state-of-the-art and perspectives for such a GW+HEN multimessenger astronomy.

19. Multimessenger astronomy with gravitational waves and high-energy neutrinos

Author

Caltech, ; California Institute of Technology - CALTECH, APC - AHE ; AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot - CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, APC - ADAMIS ; AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot - CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, Service d'Electronique, des Détecteurs et d'Informatique (SEDI) ; CEA, Department of Physics ; Columbia University, LIGO Laboratory ; California Institute of Technology, Albert-Einstein-Institut ; Max-Planck-Institut, Laboratoire d'Annecy le Vieux de Physique des Particules (LAPP) ; CNRS - IN2P3 - Université de Savoie, Department of Physics [Beer-Sheva] ; Ben Gurion University, Oskar Klein Centre and Department of Physics ; Stockholm University, Department of Physics and Optical Engineering ; ORT Braude, Observatory of Rome ; INAF, Dept. of Physics ; University of Wisconsin-Madison, School of Physics and Astronomy ; Cardiff University, University of Minnesota ; University of Minnesota, Division of Theoretical Astronomy ; National Astronomical Observatory of Japan, Department of applied physics ; Fukuoka University, Racah Institute of Physics ; Hebew University of Jerusalem, Institut Pluridisciplinaire Hubert Curien (IPHC) ; CNRS - Université de Strasbourg, Instituto Argentino de Radioastronomia ; CONICET - IAR - CCT La Plata, Department of Physics and Astrophysics ; The Weizmann Institute of Science, Ando, S., Baret, B., Bouhou, B., Chassande-Mottin, E., Kouchner, A., Moscoso, L., Van Elewyck, V., Bartos, I., Márka, S., Márka, Z., Corsi, A., Di Palma, I., Papa, M. A., Dietz, A., Donzaud, C., Eichler, D., Finley, C., Guetta, D., Halzen, F., Jones, G., Sutton, P. J., Kandhasamy, S., Mandic, V., Thrane, E., Kotake, K., Piran, T., Pradier, T., Romero, G. E., Waxman, E., Caltech, ; California Institute of Technology - CALTECH, APC - AHE ; AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot - CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, APC - ADAMIS ; AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot - CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, AstroParticule et Cosmologie (APC - UMR 7164) ; CNRS - CEA - IN2P3 - Observatoire de Paris - Université Paris VII - Paris Diderot, Service d'Electronique, des Détecteurs et d'Informatique (SEDI) ; CEA, Department of Physics ; Columbia University, LIGO Laboratory ; California Institute of Technology, Albert-Einstein-Institut ; Max-Planck-Institut, Laboratoire d'Annecy le Vieux de Physique des Particules (LAPP) ; CNRS - IN2P3 - Université de Savoie, Department of Physics [Beer-Sheva] ; Ben Gurion University, Oskar Klein Centre and Department of Physics ; Stockholm University, Department of Physics and Optical Engineering ; ORT Braude, Observatory of Rome ; INAF, Dept. of Physics ; University of Wisconsin-Madison, School of Physics and Astronomy ; Cardiff University, University of Minnesota ; University of Minnesota, Division of Theoretical Astronomy ; National Astronomical Observatory of Japan, Department of applied physics ; Fukuoka University, Racah Institute of Physics ; Hebew University of Jerusalem, Institut Pluridisciplinaire Hubert Curien (IPHC) ; CNRS - Université de Strasbourg, Instituto Argentino de Radioastronomia ; CONICET - IAR - CCT La Plata, Department of Physics and Astrophysics ; The Weizmann Institute of Science, Ando, S., Baret, B., Bouhou, B., Chassande-Mottin, E., Kouchner, A., Moscoso, L., Van Elewyck, V., Bartos, I., Márka, S., Márka, Z., Corsi, A., Di Palma, I., Papa, M. A., Dietz, A., Donzaud, C., Eichler, D., Finley, C., Guetta, D., Halzen, F., Jones, G., Sutton, P. J., Kandhasamy, S., Mandic, V., Thrane, E., Kotake, K., Piran, T., Pradier, T., Romero, G. E., and Waxman, E.

Abstract

Revised version, to appear in Reviews of Modern Physics (Colloquium Series). Section II on Potential GW+HEN emitters thoroughly updated. Section IV expanded with recent experimental results from joint GW+HEN searches with ANTARES, IceCube, LIGO and VIRGO, and with an extended discussion of the reach and implications of future searches., Many of the astrophysical sources and violent phenomena observed in our Universe are potential emitters of gravitational waves (GW) and high-energy neutrinos (HEN). Both GWs and HENs may escape very dense media and travel unaffected over cosmological distances, carrying information from the innermost regions of the astrophysical engines. Such messengers could also reveal new, hidden sources that have not been observed by conventional photon-based astronomy. Coincident observation of GWs and HENs may thus play a critical role in multimessenger astronomy. This is particularly true at the present time owing to the advent of a new generation of dedicated detectors: IceCube, ANTARES, VIRGO and LIGO. Given the complexity of the instruments, a successful joint analysis of this data set will be possible only if the expertise and knowledge of the data is shared between the two communities. This review aims at providing an overview of both theoretical and experimental state-of-the-art and perspectives for such a GW+HEN multimessenger astronomy.

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