Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope
The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions ar...
Ausführliche Beschreibung
Gespeichert in:
| Autor*in: |
Adrián-Martínez, S. [verfasserIn] |
|---|
| Format: |
E-Artikel |
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| Sprache: |
Englisch |
| Erschienen: |
2016transfer abstract |
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| Umfang: |
9 |
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| Übergeordnetes Werk: |
Enthalten in: Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells - 2012transfer abstract, Amsterdam [u.a.] |
|---|---|
| Übergeordnetes Werk: |
volume:78 ; year:2016 ; pages:43-51 ; extent:9 |
| Links: |
|---|
| DOI / URN: |
10.1016/j.astropartphys.2016.02.001 |
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| Katalog-ID: |
ELV035447443 |
|---|
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| 245 | 1 | 0 | |a Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope |
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| 520 | |a The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. | ||
| 520 | |a The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. | ||
| 700 | 1 | |a Albert, A. |4 oth | |
| 700 | 1 | |a André, M. |4 oth | |
| 700 | 1 | |a Anton, G. |4 oth | |
| 700 | 1 | |a Ardid, M. |4 oth | |
| 700 | 1 | |a Aubert, J.-J. |4 oth | |
| 700 | 1 | |a Baret, B. |4 oth | |
| 700 | 1 | |a Barrios-Martí, J. |4 oth | |
| 700 | 1 | |a Basa, S. |4 oth | |
| 700 | 1 | |a Bertin, V. |4 oth | |
| 700 | 1 | |a Biagi, S. |4 oth | |
| 700 | 1 | |a Bogazzi, C. |4 oth | |
| 700 | 1 | |a Bormuth, R. |4 oth | |
| 700 | 1 | |a Bou-Cabo, M. |4 oth | |
| 700 | 1 | |a Bouwhuis, M.C. |4 oth | |
| 700 | 1 | |a Bruijn, R. |4 oth | |
| 700 | 1 | |a Brunner, J. |4 oth | |
| 700 | 1 | |a Busto, J. |4 oth | |
| 700 | 1 | |a Capone, A. |4 oth | |
| 700 | 1 | |a Caramete, L. |4 oth | |
| 700 | 1 | |a Carr, J. |4 oth | |
| 700 | 1 | |a Chiarusi, T. |4 oth | |
| 700 | 1 | |a Circella, M. |4 oth | |
| 700 | 1 | |a Coniglione, R. |4 oth | |
| 700 | 1 | |a Costantini, H. |4 oth | |
| 700 | 1 | |a Coyle, P. |4 oth | |
| 700 | 1 | |a Creusot, A. |4 oth | |
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| 700 | 1 | |a Deschamps, A. |4 oth | |
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| 700 | 1 | |a Donzaud, C. |4 oth | |
| 700 | 1 | |a Dornic, D. |4 oth | |
| 700 | 1 | |a Drouhin, D. |4 oth | |
| 700 | 1 | |a Dumas, A. |4 oth | |
| 700 | 1 | |a Eberl, T. |4 oth | |
| 700 | 1 | |a Elsässer, D. |4 oth | |
| 700 | 1 | |a Enzenhöfer, A. |4 oth | |
| 700 | 1 | |a Fehn, K. |4 oth | |
| 700 | 1 | |a Felis, I. |4 oth | |
| 700 | 1 | |a Fermani, P. |4 oth | |
| 700 | 1 | |a Flaminio, V. |4 oth | |
| 700 | 1 | |a Folger, F. |4 oth | |
| 700 | 1 | |a Fusco, L.A. |4 oth | |
| 700 | 1 | |a Galatà, S. |4 oth | |
| 700 | 1 | |a Gay, P. |4 oth | |
| 700 | 1 | |a Geißelsöder, S. |4 oth | |
| 700 | 1 | |a Geyer, K. |4 oth | |
| 700 | 1 | |a Giordano, V. |4 oth | |
| 700 | 1 | |a Gleixner, A. |4 oth | |
| 700 | 1 | |a Gracia-Ruiz, R. |4 oth | |
| 700 | 1 | |a Gómez-González, J.P. |4 oth | |
| 700 | 1 | |a Graf, K. |4 oth | |
| 700 | 1 | |a van Haren, H. |4 oth | |
| 700 | 1 | |a Heijboer, A.J. |4 oth | |
| 700 | 1 | |a Hello, Y. |4 oth | |
| 700 | 1 | |a Hernández-Rey, J.J. |4 oth | |
| 700 | 1 | |a Herrero, A. |4 oth | |
| 700 | 1 | |a Hößl, J. |4 oth | |
| 700 | 1 | |a Hofestädt, J. |4 oth | |
| 700 | 1 | |a Hugon, C. |4 oth | |
| 700 | 1 | |a James, C.W. |4 oth | |
| 700 | 1 | |a de Jong, M. |4 oth | |
| 700 | 1 | |a Kadler, M. |4 oth | |
| 700 | 1 | |a Kalekin, O. |4 oth | |
| 700 | 1 | |a Katz, U. |4 oth | |
| 700 | 1 | |a Kießling, D. |4 oth | |
| 700 | 1 | |a Kooijman, P. |4 oth | |
| 700 | 1 | |a Kouchner, A. |4 oth | |
| 700 | 1 | |a Kreykenbohm, I. |4 oth | |
| 700 | 1 | |a Kulikovskiy, V. |4 oth | |
| 700 | 1 | |a Lahmann, R. |4 oth | |
| 700 | 1 | |a Lambard, G. |4 oth | |
| 700 | 1 | |a Lattuada, D. |4 oth | |
| 700 | 1 | |a Lefèvre, D. |4 oth | |
| 700 | 1 | |a Leonora, E. |4 oth | |
| 700 | 1 | |a Loucatos, S. |4 oth | |
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| 700 | 1 | |a Marcelin, M. |4 oth | |
| 700 | 1 | |a Margiotta, A. |4 oth | |
| 700 | 1 | |a Marinelli, A. |4 oth | |
| 700 | 1 | |a Martínez-Mora, J.A. |4 oth | |
| 700 | 1 | |a Martini, S. |4 oth | |
| 700 | 1 | |a Mathieu, A. |4 oth | |
| 700 | 1 | |a Michael, T. |4 oth | |
| 700 | 1 | |a Migliozzi, P. |4 oth | |
| 700 | 1 | |a Moussa, A. |4 oth | |
| 700 | 1 | |a Mueller, C. |4 oth | |
| 700 | 1 | |a Neff, M. |4 oth | |
| 700 | 1 | |a Nezri, E. |4 oth | |
| 700 | 1 | |a Păvălaş, G.E. |4 oth | |
| 700 | 1 | |a Pellegrino, C. |4 oth | |
| 700 | 1 | |a Perrina, C. |4 oth | |
| 700 | 1 | |a Piattelli, P. |4 oth | |
| 700 | 1 | |a Popa, V. |4 oth | |
| 700 | 1 | |a Pradier, T. |4 oth | |
| 700 | 1 | |a Racca, C. |4 oth | |
| 700 | 1 | |a Riccobene, G. |4 oth | |
| 700 | 1 | |a Richter, R. |4 oth | |
| 700 | 1 | |a Roensch, K. |4 oth | |
| 700 | 1 | |a Rostovtsev, A. |4 oth | |
| 700 | 1 | |a Saldaña, M. |4 oth | |
| 700 | 1 | |a Samtleben, D.F.E. |4 oth | |
| 700 | 1 | |a Sánchez-Losa, A. |4 oth | |
| 700 | 1 | |a Sanguineti, M. |4 oth | |
| 700 | 1 | |a Sapienza, P. |4 oth | |
| 700 | 1 | |a Schmid, J. |4 oth | |
| 700 | 1 | |a Schnabel, J. |4 oth | |
| 700 | 1 | |a Schulte, S. |4 oth | |
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| 700 | 1 | |a Tamburini, C. |4 oth | |
| 700 | 1 | |a Trovato, A. |4 oth | |
| 700 | 1 | |a Tselengidou, M. |4 oth | |
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2016transfer abstract |
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10.1016/j.astropartphys.2016.02.001 doi GBVA2016016000009.pica (DE-627)ELV035447443 (ELSEVIER)S0927-6505(16)30013-5 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Adrián-Martínez, S. verfasserin aut Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope 2016transfer abstract 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. Albert, A. oth André, M. oth Anton, G. oth Ardid, M. oth Aubert, J.-J. oth Baret, B. oth Barrios-Martí, J. oth Basa, S. oth Bertin, V. oth Biagi, S. oth Bogazzi, C. oth Bormuth, R. oth Bou-Cabo, M. oth Bouwhuis, M.C. oth Bruijn, R. oth Brunner, J. oth Busto, J. oth Capone, A. oth Caramete, L. oth Carr, J. oth Chiarusi, T. oth Circella, M. oth Coniglione, R. oth Costantini, H. oth Coyle, P. oth Creusot, A. oth Dekeyser, I. oth Deschamps, A. oth De Bonis, G. oth Distefano, C. oth Donzaud, C. oth Dornic, D. oth Drouhin, D. oth Dumas, A. oth Eberl, T. oth Elsässer, D. oth Enzenhöfer, A. oth Fehn, K. oth Felis, I. oth Fermani, P. oth Flaminio, V. oth Folger, F. oth Fusco, L.A. oth Galatà, S. oth Gay, P. oth Geißelsöder, S. oth Geyer, K. oth Giordano, V. oth Gleixner, A. oth Gracia-Ruiz, R. oth Gómez-González, J.P. oth Graf, K. oth van Haren, H. oth Heijboer, A.J. oth Hello, Y. oth Hernández-Rey, J.J. oth Herrero, A. oth Hößl, J. oth Hofestädt, J. oth Hugon, C. oth James, C.W. oth de Jong, M. oth Kadler, M. oth Kalekin, O. oth Katz, U. oth Kießling, D. oth Kooijman, P. oth Kouchner, A. oth Kreykenbohm, I. oth Kulikovskiy, V. oth Lahmann, R. oth Lambard, G. oth Lattuada, D. oth Lefèvre, D. oth Leonora, E. oth Loucatos, S. oth Mangano, S. oth Marcelin, M. oth Margiotta, A. oth Marinelli, A. oth Martínez-Mora, J.A. oth Martini, S. oth Mathieu, A. oth Michael, T. oth Migliozzi, P. oth Moussa, A. oth Mueller, C. oth Neff, M. oth Nezri, E. oth Păvălaş, G.E. oth Pellegrino, C. oth Perrina, C. oth Piattelli, P. oth Popa, V. oth Pradier, T. oth Racca, C. oth Riccobene, G. oth Richter, R. oth Roensch, K. oth Rostovtsev, A. oth Saldaña, M. oth Samtleben, D.F.E. oth Sánchez-Losa, A. oth Sanguineti, M. oth Sapienza, P. oth Schmid, J. oth Schnabel, J. oth Schulte, S. oth Schüssler, F. oth Seitz, T. oth Sieger, C. oth Spurio, M. oth Steijger, J.J.M. oth Stolarczyk, Th. oth Taiuti, M. oth Tamburini, C. oth Trovato, A. oth Tselengidou, M. oth Tönnis, C. oth Turpin, D. oth Vallage, B. oth Vallée, C. oth Van Elewyck, V. oth Visser, E. oth Vivolo, D. oth Wagner, S. oth Wilms, J. oth Zornoza, J.D. oth Zúñiga, J. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:78 year:2016 pages:43-51 extent:9 https://doi.org/10.1016/j.astropartphys.2016.02.001 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 78 2016 43-51 9 045F 540 |
| spelling |
10.1016/j.astropartphys.2016.02.001 doi GBVA2016016000009.pica (DE-627)ELV035447443 (ELSEVIER)S0927-6505(16)30013-5 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Adrián-Martínez, S. verfasserin aut Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope 2016transfer abstract 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. Albert, A. oth André, M. oth Anton, G. oth Ardid, M. oth Aubert, J.-J. oth Baret, B. oth Barrios-Martí, J. oth Basa, S. oth Bertin, V. oth Biagi, S. oth Bogazzi, C. oth Bormuth, R. oth Bou-Cabo, M. oth Bouwhuis, M.C. oth Bruijn, R. oth Brunner, J. oth Busto, J. oth Capone, A. oth Caramete, L. oth Carr, J. oth Chiarusi, T. oth Circella, M. oth Coniglione, R. oth Costantini, H. oth Coyle, P. oth Creusot, A. oth Dekeyser, I. oth Deschamps, A. oth De Bonis, G. oth Distefano, C. oth Donzaud, C. oth Dornic, D. oth Drouhin, D. oth Dumas, A. oth Eberl, T. oth Elsässer, D. oth Enzenhöfer, A. oth Fehn, K. oth Felis, I. oth Fermani, P. oth Flaminio, V. oth Folger, F. oth Fusco, L.A. oth Galatà, S. oth Gay, P. oth Geißelsöder, S. oth Geyer, K. oth Giordano, V. oth Gleixner, A. oth Gracia-Ruiz, R. oth Gómez-González, J.P. oth Graf, K. oth van Haren, H. oth Heijboer, A.J. oth Hello, Y. oth Hernández-Rey, J.J. oth Herrero, A. oth Hößl, J. oth Hofestädt, J. oth Hugon, C. oth James, C.W. oth de Jong, M. oth Kadler, M. oth Kalekin, O. oth Katz, U. oth Kießling, D. oth Kooijman, P. oth Kouchner, A. oth Kreykenbohm, I. oth Kulikovskiy, V. oth Lahmann, R. oth Lambard, G. oth Lattuada, D. oth Lefèvre, D. oth Leonora, E. oth Loucatos, S. oth Mangano, S. oth Marcelin, M. oth Margiotta, A. oth Marinelli, A. oth Martínez-Mora, J.A. oth Martini, S. oth Mathieu, A. oth Michael, T. oth Migliozzi, P. oth Moussa, A. oth Mueller, C. oth Neff, M. oth Nezri, E. oth Păvălaş, G.E. oth Pellegrino, C. oth Perrina, C. oth Piattelli, P. oth Popa, V. oth Pradier, T. oth Racca, C. oth Riccobene, G. oth Richter, R. oth Roensch, K. oth Rostovtsev, A. oth Saldaña, M. oth Samtleben, D.F.E. oth Sánchez-Losa, A. oth Sanguineti, M. oth Sapienza, P. oth Schmid, J. oth Schnabel, J. oth Schulte, S. oth Schüssler, F. oth Seitz, T. oth Sieger, C. oth Spurio, M. oth Steijger, J.J.M. oth Stolarczyk, Th. oth Taiuti, M. oth Tamburini, C. oth Trovato, A. oth Tselengidou, M. oth Tönnis, C. oth Turpin, D. oth Vallage, B. oth Vallée, C. oth Van Elewyck, V. oth Visser, E. oth Vivolo, D. oth Wagner, S. oth Wilms, J. oth Zornoza, J.D. oth Zúñiga, J. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:78 year:2016 pages:43-51 extent:9 https://doi.org/10.1016/j.astropartphys.2016.02.001 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 78 2016 43-51 9 045F 540 |
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10.1016/j.astropartphys.2016.02.001 doi GBVA2016016000009.pica (DE-627)ELV035447443 (ELSEVIER)S0927-6505(16)30013-5 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Adrián-Martínez, S. verfasserin aut Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope 2016transfer abstract 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. Albert, A. oth André, M. oth Anton, G. oth Ardid, M. oth Aubert, J.-J. oth Baret, B. oth Barrios-Martí, J. oth Basa, S. oth Bertin, V. oth Biagi, S. oth Bogazzi, C. oth Bormuth, R. oth Bou-Cabo, M. oth Bouwhuis, M.C. oth Bruijn, R. oth Brunner, J. oth Busto, J. oth Capone, A. oth Caramete, L. oth Carr, J. oth Chiarusi, T. oth Circella, M. oth Coniglione, R. oth Costantini, H. oth Coyle, P. oth Creusot, A. oth Dekeyser, I. oth Deschamps, A. oth De Bonis, G. oth Distefano, C. oth Donzaud, C. oth Dornic, D. oth Drouhin, D. oth Dumas, A. oth Eberl, T. oth Elsässer, D. oth Enzenhöfer, A. oth Fehn, K. oth Felis, I. oth Fermani, P. oth Flaminio, V. oth Folger, F. oth Fusco, L.A. oth Galatà, S. oth Gay, P. oth Geißelsöder, S. oth Geyer, K. oth Giordano, V. oth Gleixner, A. oth Gracia-Ruiz, R. oth Gómez-González, J.P. oth Graf, K. oth van Haren, H. oth Heijboer, A.J. oth Hello, Y. oth Hernández-Rey, J.J. oth Herrero, A. oth Hößl, J. oth Hofestädt, J. oth Hugon, C. oth James, C.W. oth de Jong, M. oth Kadler, M. oth Kalekin, O. oth Katz, U. oth Kießling, D. oth Kooijman, P. oth Kouchner, A. oth Kreykenbohm, I. oth Kulikovskiy, V. oth Lahmann, R. oth Lambard, G. oth Lattuada, D. oth Lefèvre, D. oth Leonora, E. oth Loucatos, S. oth Mangano, S. oth Marcelin, M. oth Margiotta, A. oth Marinelli, A. oth Martínez-Mora, J.A. oth Martini, S. oth Mathieu, A. oth Michael, T. oth Migliozzi, P. oth Moussa, A. oth Mueller, C. oth Neff, M. oth Nezri, E. oth Păvălaş, G.E. oth Pellegrino, C. oth Perrina, C. oth Piattelli, P. oth Popa, V. oth Pradier, T. oth Racca, C. oth Riccobene, G. oth Richter, R. oth Roensch, K. oth Rostovtsev, A. oth Saldaña, M. oth Samtleben, D.F.E. oth Sánchez-Losa, A. oth Sanguineti, M. oth Sapienza, P. oth Schmid, J. oth Schnabel, J. oth Schulte, S. oth Schüssler, F. oth Seitz, T. oth Sieger, C. oth Spurio, M. oth Steijger, J.J.M. oth Stolarczyk, Th. oth Taiuti, M. oth Tamburini, C. oth Trovato, A. oth Tselengidou, M. oth Tönnis, C. oth Turpin, D. oth Vallage, B. oth Vallée, C. oth Van Elewyck, V. oth Visser, E. oth Vivolo, D. oth Wagner, S. oth Wilms, J. oth Zornoza, J.D. oth Zúñiga, J. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:78 year:2016 pages:43-51 extent:9 https://doi.org/10.1016/j.astropartphys.2016.02.001 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 78 2016 43-51 9 045F 540 |
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10.1016/j.astropartphys.2016.02.001 doi GBVA2016016000009.pica (DE-627)ELV035447443 (ELSEVIER)S0927-6505(16)30013-5 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Adrián-Martínez, S. verfasserin aut Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope 2016transfer abstract 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. Albert, A. oth André, M. oth Anton, G. oth Ardid, M. oth Aubert, J.-J. oth Baret, B. oth Barrios-Martí, J. oth Basa, S. oth Bertin, V. oth Biagi, S. oth Bogazzi, C. oth Bormuth, R. oth Bou-Cabo, M. oth Bouwhuis, M.C. oth Bruijn, R. oth Brunner, J. oth Busto, J. oth Capone, A. oth Caramete, L. oth Carr, J. oth Chiarusi, T. oth Circella, M. oth Coniglione, R. oth Costantini, H. oth Coyle, P. oth Creusot, A. oth Dekeyser, I. oth Deschamps, A. oth De Bonis, G. oth Distefano, C. oth Donzaud, C. oth Dornic, D. oth Drouhin, D. oth Dumas, A. oth Eberl, T. oth Elsässer, D. oth Enzenhöfer, A. oth Fehn, K. oth Felis, I. oth Fermani, P. oth Flaminio, V. oth Folger, F. oth Fusco, L.A. oth Galatà, S. oth Gay, P. oth Geißelsöder, S. oth Geyer, K. oth Giordano, V. oth Gleixner, A. oth Gracia-Ruiz, R. oth Gómez-González, J.P. oth Graf, K. oth van Haren, H. oth Heijboer, A.J. oth Hello, Y. oth Hernández-Rey, J.J. oth Herrero, A. oth Hößl, J. oth Hofestädt, J. oth Hugon, C. oth James, C.W. oth de Jong, M. oth Kadler, M. oth Kalekin, O. oth Katz, U. oth Kießling, D. oth Kooijman, P. oth Kouchner, A. oth Kreykenbohm, I. oth Kulikovskiy, V. oth Lahmann, R. oth Lambard, G. oth Lattuada, D. oth Lefèvre, D. oth Leonora, E. oth Loucatos, S. oth Mangano, S. oth Marcelin, M. oth Margiotta, A. oth Marinelli, A. oth Martínez-Mora, J.A. oth Martini, S. oth Mathieu, A. oth Michael, T. oth Migliozzi, P. oth Moussa, A. oth Mueller, C. oth Neff, M. oth Nezri, E. oth Păvălaş, G.E. oth Pellegrino, C. oth Perrina, C. oth Piattelli, P. oth Popa, V. oth Pradier, T. oth Racca, C. oth Riccobene, G. oth Richter, R. oth Roensch, K. oth Rostovtsev, A. oth Saldaña, M. oth Samtleben, D.F.E. oth Sánchez-Losa, A. oth Sanguineti, M. oth Sapienza, P. oth Schmid, J. oth Schnabel, J. oth Schulte, S. oth Schüssler, F. oth Seitz, T. oth Sieger, C. oth Spurio, M. oth Steijger, J.J.M. oth Stolarczyk, Th. oth Taiuti, M. oth Tamburini, C. oth Trovato, A. oth Tselengidou, M. oth Tönnis, C. oth Turpin, D. oth Vallage, B. oth Vallée, C. oth Van Elewyck, V. oth Visser, E. oth Vivolo, D. oth Wagner, S. oth Wilms, J. oth Zornoza, J.D. oth Zúñiga, J. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:78 year:2016 pages:43-51 extent:9 https://doi.org/10.1016/j.astropartphys.2016.02.001 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 78 2016 43-51 9 045F 540 |
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10.1016/j.astropartphys.2016.02.001 doi GBVA2016016000009.pica (DE-627)ELV035447443 (ELSEVIER)S0927-6505(16)30013-5 DE-627 ger DE-627 rakwb eng 540 540 DE-600 620 VZ 690 VZ 50.92 bkl Adrián-Martínez, S. verfasserin aut Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope 2016transfer abstract 9 nicht spezifiziert zzz rdacontent nicht spezifiziert z rdamedia nicht spezifiziert zu rdacarrier The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. Albert, A. oth André, M. oth Anton, G. oth Ardid, M. oth Aubert, J.-J. oth Baret, B. oth Barrios-Martí, J. oth Basa, S. oth Bertin, V. oth Biagi, S. oth Bogazzi, C. oth Bormuth, R. oth Bou-Cabo, M. oth Bouwhuis, M.C. oth Bruijn, R. oth Brunner, J. oth Busto, J. oth Capone, A. oth Caramete, L. oth Carr, J. oth Chiarusi, T. oth Circella, M. oth Coniglione, R. oth Costantini, H. oth Coyle, P. oth Creusot, A. oth Dekeyser, I. oth Deschamps, A. oth De Bonis, G. oth Distefano, C. oth Donzaud, C. oth Dornic, D. oth Drouhin, D. oth Dumas, A. oth Eberl, T. oth Elsässer, D. oth Enzenhöfer, A. oth Fehn, K. oth Felis, I. oth Fermani, P. oth Flaminio, V. oth Folger, F. oth Fusco, L.A. oth Galatà, S. oth Gay, P. oth Geißelsöder, S. oth Geyer, K. oth Giordano, V. oth Gleixner, A. oth Gracia-Ruiz, R. oth Gómez-González, J.P. oth Graf, K. oth van Haren, H. oth Heijboer, A.J. oth Hello, Y. oth Hernández-Rey, J.J. oth Herrero, A. oth Hößl, J. oth Hofestädt, J. oth Hugon, C. oth James, C.W. oth de Jong, M. oth Kadler, M. oth Kalekin, O. oth Katz, U. oth Kießling, D. oth Kooijman, P. oth Kouchner, A. oth Kreykenbohm, I. oth Kulikovskiy, V. oth Lahmann, R. oth Lambard, G. oth Lattuada, D. oth Lefèvre, D. oth Leonora, E. oth Loucatos, S. oth Mangano, S. oth Marcelin, M. oth Margiotta, A. oth Marinelli, A. oth Martínez-Mora, J.A. oth Martini, S. oth Mathieu, A. oth Michael, T. oth Migliozzi, P. oth Moussa, A. oth Mueller, C. oth Neff, M. oth Nezri, E. oth Păvălaş, G.E. oth Pellegrino, C. oth Perrina, C. oth Piattelli, P. oth Popa, V. oth Pradier, T. oth Racca, C. oth Riccobene, G. oth Richter, R. oth Roensch, K. oth Rostovtsev, A. oth Saldaña, M. oth Samtleben, D.F.E. oth Sánchez-Losa, A. oth Sanguineti, M. oth Sapienza, P. oth Schmid, J. oth Schnabel, J. oth Schulte, S. oth Schüssler, F. oth Seitz, T. oth Sieger, C. oth Spurio, M. oth Steijger, J.J.M. oth Stolarczyk, Th. oth Taiuti, M. oth Tamburini, C. oth Trovato, A. oth Tselengidou, M. oth Tönnis, C. oth Turpin, D. oth Vallage, B. oth Vallée, C. oth Van Elewyck, V. oth Visser, E. oth Vivolo, D. oth Wagner, S. oth Wilms, J. oth Zornoza, J.D. oth Zúñiga, J. oth Enthalten in Elsevier Science Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells 2012transfer abstract Amsterdam [u.a.] (DE-627)ELV016257995 volume:78 year:2016 pages:43-51 extent:9 https://doi.org/10.1016/j.astropartphys.2016.02.001 Volltext GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 50.92 Meerestechnik VZ AR 78 2016 43-51 9 045F 540 |
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3540 |
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ELV035447443 |
| language_de |
englisch |
| fullrecord |
<?xml version="1.0" encoding="UTF-8"?><collection xmlns="http://www.loc.gov/MARC21/slim"><record><leader>01000caa a22002652 4500</leader><controlfield tag="001">ELV035447443</controlfield><controlfield tag="003">DE-627</controlfield><controlfield tag="005">20230625204254.0</controlfield><controlfield tag="007">cr uuu---uuuuu</controlfield><controlfield tag="008">180603s2016 xx |||||o 00| ||eng c</controlfield><datafield tag="024" ind1="7" ind2=" "><subfield code="a">10.1016/j.astropartphys.2016.02.001</subfield><subfield code="2">doi</subfield></datafield><datafield tag="028" ind1="5" ind2="2"><subfield code="a">GBVA2016016000009.pica</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(DE-627)ELV035447443</subfield></datafield><datafield tag="035" ind1=" " ind2=" "><subfield code="a">(ELSEVIER)S0927-6505(16)30013-5</subfield></datafield><datafield tag="040" ind1=" " ind2=" "><subfield code="a">DE-627</subfield><subfield code="b">ger</subfield><subfield code="c">DE-627</subfield><subfield code="e">rakwb</subfield></datafield><datafield tag="041" ind1=" " ind2=" "><subfield code="a">eng</subfield></datafield><datafield tag="082" ind1="0" ind2=" "><subfield code="a">540</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">540</subfield><subfield code="q">DE-600</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">620</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="082" ind1="0" ind2="4"><subfield code="a">690</subfield><subfield code="q">VZ</subfield></datafield><datafield tag="084" ind1=" " ind2=" "><subfield code="a">50.92</subfield><subfield code="2">bkl</subfield></datafield><datafield tag="100" ind1="1" ind2=" "><subfield code="a">Adrián-Martínez, S.</subfield><subfield code="e">verfasserin</subfield><subfield code="4">aut</subfield></datafield><datafield tag="245" ind1="1" ind2="0"><subfield code="a">Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2016transfer abstract</subfield></datafield><datafield tag="300" ind1=" " ind2=" "><subfield code="a">9</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zzz</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">z</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">nicht spezifiziert</subfield><subfield code="b">zu</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices.</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices.</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Albert, A.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">André, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Anton, G.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Ardid, M.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Aubert, J.-J.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Baret, B.</subfield><subfield code="4">oth</subfield></datafield><datafield tag="700" ind1="1" ind2=" "><subfield code="a">Barrios-Martí, J.</subfield><subfield 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|
| author |
Adrián-Martínez, S. |
| spellingShingle |
Adrián-Martínez, S. ddc 540 ddc 620 ddc 690 bkl 50.92 Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope |
| authorStr |
Adrián-Martínez, S. |
| ppnlink_with_tag_str_mv |
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540 540 DE-600 620 VZ 690 VZ 50.92 bkl Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope |
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Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells |
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ELV016257995 |
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Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells |
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Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope |
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Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope |
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Adrián-Martínez, S. |
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Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells |
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Flexible, metal-free composite counter electrodes for efficient fiber-shaped dye-sensitized solar cells |
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Adrián-Martínez, S. |
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Elektronische Aufsätze |
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Adrián-Martínez, S. |
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10.1016/j.astropartphys.2016.02.001 |
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540 620 690 |
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time calibration with atmospheric muon tracks in the antares neutrino telescope |
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Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope |
| abstract |
The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. |
| abstractGer |
The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. |
| abstract_unstemmed |
The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of ∼10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. |
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GBV_USEFLAG_U GBV_ELV SYSFLAG_U GBV_ILN_20 GBV_ILN_252 |
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Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope |
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https://doi.org/10.1016/j.astropartphys.2016.02.001 |
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Albert, A. André, M. Anton, G. Ardid, M. Aubert, J.-J. Baret, B. Barrios-Martí, J. Basa, S. Bertin, V. Biagi, S. Bogazzi, C. Bormuth, R. Bou-Cabo, M. Bouwhuis, M.C. Bruijn, R. Brunner, J. Busto, J. Capone, A. Caramete, L. Carr, J. Chiarusi, T. Circella, M. Coniglione, R. Costantini, H. Coyle, P. Creusot, A. Dekeyser, I. Deschamps, A. De Bonis, G. Distefano, C. Donzaud, C. Dornic, D. Drouhin, D. Dumas, A. Eberl, T. Elsässer, D. Enzenhöfer, A. Fehn, K. Felis, I. Fermani, P. Flaminio, V. Folger, F. Fusco, L.A. Galatà, S. Gay, P. Geißelsöder, S. Geyer, K. Giordano, V. Gleixner, A. Gracia-Ruiz, R. Gómez-González, J.P. Graf, K. van Haren, H. Heijboer, A.J. Hello, Y. Hernández-Rey, J.J. Herrero, A. Hößl, J. Hofestädt, J. Hugon, C. James, C.W. de Jong, M. Kadler, M. Kalekin, O. Katz, U. Kießling, D. Kooijman, P. Kouchner, A. Kreykenbohm, I. Kulikovskiy, V. Lahmann, R. Lambard, G. Lattuada, D. Lefèvre, D. Leonora, E. Loucatos, S. Mangano, S. Marcelin, M. Margiotta, A. Marinelli, A. Martínez-Mora, J.A. Martini, S. Mathieu, A. Michael, T. Migliozzi, P. Moussa, A. Mueller, C. Neff, M. Nezri, E. Păvălaş, G.E. Pellegrino, C. Perrina, C. Piattelli, P. Popa, V. Pradier, T. Racca, C. Riccobene, G. Richter, R. Roensch, K. Rostovtsev, A. Saldaña, M. Samtleben, D.F.E. Sánchez-Losa, A. Sanguineti, M. Sapienza, P. Schmid, J. Schnabel, J. Schulte, S. Schüssler, F. Seitz, T. Sieger, C. Spurio, M. Steijger, J.J.M. Stolarczyk, Th Taiuti, M. Tamburini, C. Trovato, A. Tselengidou, M. Tönnis, C. Turpin, D. Vallage, B. Vallée, C. Van Elewyck, V. Visser, E. Vivolo, D. Wagner, S. Wilms, J. Zornoza, J.D. Zúñiga, J. |
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Albert, A. André, M. Anton, G. Ardid, M. Aubert, J.-J. Baret, B. Barrios-Martí, J. Basa, S. Bertin, V. Biagi, S. Bogazzi, C. Bormuth, R. Bou-Cabo, M. Bouwhuis, M.C. Bruijn, R. Brunner, J. Busto, J. Capone, A. Caramete, L. Carr, J. Chiarusi, T. Circella, M. Coniglione, R. Costantini, H. Coyle, P. Creusot, A. Dekeyser, I. Deschamps, A. De Bonis, G. Distefano, C. Donzaud, C. Dornic, D. Drouhin, D. Dumas, A. Eberl, T. Elsässer, D. Enzenhöfer, A. Fehn, K. Felis, I. Fermani, P. Flaminio, V. Folger, F. Fusco, L.A. Galatà, S. Gay, P. Geißelsöder, S. Geyer, K. Giordano, V. Gleixner, A. Gracia-Ruiz, R. Gómez-González, J.P. Graf, K. van Haren, H. Heijboer, A.J. Hello, Y. Hernández-Rey, J.J. Herrero, A. Hößl, J. Hofestädt, J. Hugon, C. James, C.W. de Jong, M. Kadler, M. Kalekin, O. Katz, U. Kießling, D. Kooijman, P. Kouchner, A. Kreykenbohm, I. Kulikovskiy, V. Lahmann, R. Lambard, G. Lattuada, D. Lefèvre, D. Leonora, E. Loucatos, S. Mangano, S. Marcelin, M. Margiotta, A. Marinelli, A. Martínez-Mora, J.A. Martini, S. Mathieu, A. Michael, T. Migliozzi, P. Moussa, A. Mueller, C. Neff, M. Nezri, E. Păvălaş, G.E. Pellegrino, C. Perrina, C. Piattelli, P. Popa, V. Pradier, T. Racca, C. Riccobene, G. Richter, R. Roensch, K. Rostovtsev, A. Saldaña, M. Samtleben, D.F.E. Sánchez-Losa, A. Sanguineti, M. Sapienza, P. Schmid, J. Schnabel, J. Schulte, S. Schüssler, F. Seitz, T. Sieger, C. Spurio, M. Steijger, J.J.M. Stolarczyk, Th Taiuti, M. Tamburini, C. Trovato, A. Tselengidou, M. Tönnis, C. Turpin, D. Vallage, B. Vallée, C. Van Elewyck, V. Visser, E. Vivolo, D. Wagner, S. Wilms, J. Zornoza, J.D. Zúñiga, J. |
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