Performance of the first ANTARES detector line

Ageron, M.; Aguilar, J. A.; Albert, A.; Ameli, F.; Anghinolfi, M.; Anton, G.; Anvar, S.; Ardid, M.; Aubert, J.J.; Aublin, J.; Auer, R.; Basa, S.; Bazzotti, M.; Becherini, Y.; Bertín, V.; Biagi, S.; Bigi, A.; Bigongiari, C.; Bou-Cabo, M.; Bouwhuis, M. C.; Bruijn, R.; Brünner, J.; Burgio, G. F.; Busto, J.; Camarena, F.; Capone, A.; Carminati, G.; Carr, J.; Castel, D.; Castorina, Emanuele; Cavasinni, V.; Cecchini, S.; Charvis, Ph.; Chiarusi, T.; Circella, M.; Colnard, C.; Coniglione, R.; Costantini, H.; Cottini, N.; Coyle, P.; Bonis, G. De; Decowski, P.; Dekeyser, I.; Deschamps, A.; Donzaud, C.; Dornic, D.; Drouhin, D.; Druillole, F.; Eberl, T.; Ernenwein, J.-P.; Escoffier, S.; Falchini, E.; Fehr, F.; Flaminio, V.; Fratini, K.; Fuda, J.-L.; Giacomelli, G.; Graf, Κ.; Guillard, G.; Hallewell, G.; Hello, Y.; Hernández-Rey, J. J.; Jong, M. de; Kalantar‐Nayestanaki, N.; Kalekin, O.; Kappes, A.; Katz, U.; Kooijman, P.; Kopper, C.; Kouchner, A.; Kretschmer, W.; Kuch, S.; Lahmann, R.; Lamare, P.; Lambard, G.; Laschinsky, H.; Lavalle, Julien; Leiprovost, H.; Lefèvre, D.; Lelaizant, G.; Lim, G.; Presti, D. Lo; Loehner, H.; Loucatos, S.; Louis, F.; Lucarelli, F.; Lyons, K.; Mangano, S.; Marcelin, M.; Margiotta, A.; Martínez-Mora, J. A.; Maurin, G.; Mazure, A.; Melissas, M.; Migneco, E.; Montaruli, T.; Morganti, M.; Moscoso, L.; Motz, H.; Naumann, C.; Ostasch, R.; #, G.E. Ip # v # la; Payre, P.; Petrović, J.; Petta, C.; Piattelli, P.; Picq, C.; Pillet, Robert; Popa, V.; Pradier, T.; Presani, E.; Racca, C.; Radu, A.; Reed, C. M.; Richardt, C.; Rujoiu, M.; Ruppi, M.; Russo, Giovanni; Salesa, F.; Sapienza, P.; Ischoeck, F.; Schuller, J. P.; Ishanidze, R.; Simeone, F.; Spurio, M.; Steenhoven, G. van der; Tamburini, Christian; Tasca, L.; Toscano, S.; Vecchi, M.; Vernin, P.; Wijnker, G.; Wolf, E. de; Zaborov, D.; Zornoza, J.D.; Zúñiga, J.

doi:10.1016/j.astropartphys.2009.02.008

Cited by 63 publications

(59 citation statements)

References 9 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…Sudden large increases are apparent for 30 days after day 67 and high levels are maintained until about day 170. Similar observations were made using different PMTs on MILOM and line 1 (Ageron et al, 2009). An increase in counting rate is usually attributed to higher levels of bioluminescence.…”

Section: Resultssupporting

confidence: 68%

Acoustic and optical variations during rapid downward motion episodes in the deep north-western Mediterranean Sea

Haren

Taupier‐Letage

Aguilar

et al. 2011

Deep Sea Research Part I: Oceanographic Research Papers

Self Cite

View full text Add to dashboard Cite

show abstract

Section: Resultssupporting

confidence: 68%

Acoustic and optical variations during rapid downward motion episodes in the deep north-western Mediterranean Sea

Haren

Taupier‐Letage

Aguilar

et al. 2011

Deep Sea Research Part I: Oceanographic Research Papers

Self Cite

View full text Add to dashboard Cite

show abstract

“…The detector has been operated in partial configurations since March 2006 and was completed in May 2008 [2]. First results are published in [6,7,8].…”

Section: Introductionmentioning

confidence: 99%

Measurement of the atmospheric muon flux with a 4GeV threshold in the ANTARES neutrino telescope

Aguilar

Samarai

Albert

et al. 2010

Astroparticle Physics

Self Cite

View full text Add to dashboard Cite

A new method for the measurement of the muon flux in the deep-sea ANTARES neutrino telescope and its dependence on the depth is presented. The method is based on the observation of coincidence signals in adjacent storeys of the detector. This yields an energy threshold of about 4 GeV. The main sources of optical background are the decay of 40 K and the bioluminescence in the sea water. The 40 K background is used to calibrate the efficiency of the photo-multiplier tubes.

show abstract

“…Note that the typical neutrino energies considered in this paper (∼ 10 MeV) are below the detection threshold of some current major detectors such as IceCube and ANTARES [70,71], though SuperKamiokande, Kam-LAND and the Sudbury Neutrino Observatory all have thresholds of order a few MeV [72][73][74]. Whilst GRBs associated to compact object mergers may produce highenergy neutrinos (∼ TeV -PeV) detectable by IceCube and ANTARES, the differential massive time delay associated to these will be miniscule.…”

Section: Detectors and Count Ratesmentioning

confidence: 99%

Multimessenger time delays from lensed gravitational waves

Baker

Trodden

2017

Phys. Rev. D

View full text Add to dashboard Cite

We investigate the potential of high-energy astrophysical events, from which both massless and massive signals are detected, to probe fundamental physics. In particular, we consider how strong gravitational lensing can induce time delays in multi-messenger signals from the same source. Obvious messenger examples are massless photons and gravitational waves, and massive neutrinos, although more exotic applications can also be imagined, such as to massive gravitons or axions. The different propagation times of the massive and massless particles can, in principle, place bounds on the total neutrino mass and probe cosmological parameters. Whilst measuring such an effect may pose a significant experimental challenge, we believe that the 'massive time delay' represents an unexplored fundamental physics phenomenon.

show abstract

Performance of the first ANTARES detector line

Cited by 63 publications

References 9 publications

Acoustic and optical variations during rapid downward motion episodes in the deep north-western Mediterranean Sea

Acoustic and optical variations during rapid downward motion episodes in the deep north-western Mediterranean Sea

Measurement of the atmospheric muon flux with a 4GeV threshold in the ANTARES neutrino telescope

Multimessenger time delays from lensed gravitational waves

Contact Info

Product

Resources

About