A search for neutrino emission from the Fermi bubbles with the ANTARES telescope

Adrián-Martínez, S.; Albert, A.; Samarai, I. Al; André, M.; Anton, G.; Anvar, S.; Ardid, M.; Astraatmadja, T.; Aubert, J.J.; Baret, B.; Barrios-Martí, J.; Basa, S.; Bertín, V.; Biagi, S.; Bigongiari, C.; Bogazzi, C.; Bouhou, B.; Bouwhuis, M. C.; Brünner, J.; Busto, J.; Capone, A.; Caramete, L.; Cârloganu, C.; Carr, J.; Cecchini, S.; Charif, Z.; Charvis, Philippe; Chiarusi, T.; Circella, M.; Classen, F.; Coniglione, R.; Core, L.; Costantini, H.; Coyle, P.; Creusot, A.; Curtil, C.; Bonis, G. De; Dekeyser, I.; Deschamps, A.; Donzaud, C.; Dornic, D.; Dorosti, Q.; Drouhin, D.; Dumas, A.; Eberl, T.; Emanuele, U.; Enzenhöfer, A.; Ernenwein, J.-P.; Escoffier, S.; Fehn, K.; Fermani, P.; Flaminio, V.; Folger, F.; Fritsch, U.; Fusco, L.; Galatà, S.; Geißelsöder, S.; Geyer, K.; Giacomelli, G.; Giordano, V.; Gleixner, A.; Gómez-González, J.; Graf, Κ.; Guillard, G.; Haren, Hans van; Heijboer, A.; Hello, Y.; Hernández-Rey, J. J.; Herold, B.; Hößl, J.; Hugon, C.; James, C. W.; Jong, M. de; Kadler, M.; Kalekin, O.; Kappes, A.; Katz, U.; Kooijman, P.; Kouchner, A.; Kreykenbohm, I.; Kulikovskiy, V.; Lahmann, R.; Lambard, E.; Lambard, G.; Larosa, G.; Lattuada, D.; Lefèvre, D.; Leonora, E.; Presti, D. Lo; Loehner, H.; Loucatos, S.; Louis, F.; Mangano, S.; Marcelin, M.; Margiotta, A.; Martínez-Mora, J. A.; Martini, Séverine; Michael, T.; Montaruli, T.; Morganti, M.; Müller, C.; Neff, M.; Nezri, E.; Palioselitis, D.; Păvălaş, G. E.; Perrina, C.; Popa, V.; Pradier, T.; Racca, C.; Riccobene, G.; Richter, R.; Rivière, C.; Robert, Aymeric; Roensch, K.; Rostovtsev, A.; Samtleben, D. F. E.; Sanguineti, M.; Sapienza, P.; Schmid, Julia; Schnabel, J.; Schulte, S.; Schüßler, F.; Seitz, T.; Shanidze, R.; Sieger, C.; Simeone, F.; Spies, A.; Spurio, M.; Steijger, J. J. M.; Stolarczyk, Th.; Sánchez-Losa, A.; Taiuti, M.; Tamburini, Christian; Tayalati, Y.; Trovato, A.; Vallage, B.; Vallée, C.; Elewyck, V. Van; Vecchi, M.; Vernin, P.; Visser, E.; Wagner, S. J.; Wilms, J.; Wolf, E. de; Yatkin, K.; Yepes, H.; Zornoza, J.D.; Zúñiga, J.

doi:10.1140/epjc/s10052-013-2701-6

Cited by 32 publications

(18 citation statements)

References 24 publications

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“…For comparison, we also show: (i) the atmospheric neutrino flux [34] averaged over 25°-95°zenith angle, (ii) the ANTARES upper limit [32] and (iii) the diffuse flux that best fits the IceCube data [2]. The other two panels show the distribution (normalized to 1) of the flux in sin θ (with θ the declination angle) (b), and in the right ascension, ϕ, (c), for each bubble (solid) and the total for both (dotted).…”

Section: Fig 2 (Color Online) (A)mentioning

confidence: 99%

“…In the baryonic hypothesis, the gamma ray flux from the bubbles should have a neutrino counterpart of similar magnitude [29,31], which should be detectable in muon tracks at a Km 3 detector in the northern hemisphere [31]. Dedicated experimental work on this is in progress [32,33], and an upper limit has been placed by the ANTARES collaboration (see Fig. 2) [32].…”

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confidence: 98%

“…Dedicated experimental work on this is in progress [32,33], and an upper limit has been placed by the ANTARES collaboration (see Fig. 2) [32].…”

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confidence: 99%

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Neutrino events at IceCube and the Fermi bubbles

et al. 2014

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We discuss the possibility that the IceCube neutrino telescope might be observing the Fermi bubbles. If the bubbles discovered in gamma rays originate from accelerated protons, they should be strong emitters of high energy (≳GeV) neutrinos. These neutrinos are detectable as showerlike or tracklike events at a Km 3 neutrino observatory. For a primary cosmic ray flux with spectrum ∝ E −2.1 and cutoff energy at or above 10 PeV, the Fermi bubble flux substantially exceeds the atmospheric background, and could account for up to ∼4-5 of the 28 events detected above ∼30 TeV at IceCube. Running the detector for ∼5-7 more years should be sufficient to discover this flux at high significance. For a primary cosmic ray flux with steeper spectrum, and/or lower cutoff energy, longer running times will be required to overcome the background.

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Section: Fig 2 (Color Online) (A)mentioning

confidence: 99%

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confidence: 98%

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Neutrino events at IceCube and the Fermi bubbles

et al. 2014

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“…One of them will be KM3NeT, the multi-km 3 neutrino detector currently planned in the Mediterranean sea [27]. It's current predecessor ANTARES has already searched for a signal from the FB direction, resulting in a flux upper limit [28]. Relative to IceCube, KM3NeT will have a larger effective area (∼ 6 km 3 instrumented volume) and may detect the FB in about one year of its operation [27].…”

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confidence: 99%

Multimessenger study of the Fermi bubbles: Very high energy gamma rays and neutrinos

2015

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The Fermi Bubbles have been imaged in sub-TeV gamma rays at Fermi-LAT, and, if their origin is hadronic, they might have been seen with low statistics in ∼ 0.1 − 1 PeV neutrinos at IceCube. We discuss the detectability of these objects at the new High Altitude Water Cherenkov (HAWC) gamma ray detector. HAWC will view the North Bubble for ∼ 2 − 3 hours a day, and will map its spectrum at 0.1-100 TeV. For the hard primary proton spectrum required to explain five events at IceCube, a high significance detection at HAWC will be achieved in less than 30 days. The combination of results at HAWC and IceCube will substantiate the hadronic model, or constrain its spectral parameters.

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“…Data from the Fermi Large Area Telescope showed evidence for the emission of high energy gamma rays from two large areas, in the region above and below the Galactic Centre (the so-called "Fermi bubbles" [5]. Assuming a hadronic mechanism for the gamma ray production from the Fermi bubbles, a high energy neutrino flux is also expected.…”

Section: The Physics Casementioning

confidence: 99%

The KM3NeT deep-sea neutrino telescope

Margiotta

2014

Nuclear Instruments and Methods in Physics Research Section A:

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KM3NeT is a deep-sea research infrastructure being constructed in the Mediterranean Sea. It will host the next generation Cherenkov neutrino telescope and nodes for a deep sea multidisciplinary observatory, providing oceanographers, marine biologists, and geophysicists with real time measurements. The neutrino telescope will complement IceCube in its field of view and exceed it substantially in sensitivity. Its main goal is the detection of high energy neutrinos of astrophysical origin. The detector will have a modular structure with six building blocks, each consisting of about one hundred Detection Units (DUs). Each DU will be equipped with 18 multi-PMT digital optical modules. The first phase of construction has started and shore and deep-sea infrastructures hosting the future KM3NeT detector are being prepared offshore Toulon, France and offshore Capo Passero on Sicily, Italy. The technological solutions for the neutrino detector of KM3NeT and the expected performance of the neutrino telescope are presented and discussed.

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A search for neutrino emission from the Fermi bubbles with the ANTARES telescope

Cited by 32 publications

References 24 publications

Neutrino events at IceCube and the Fermi bubbles

Neutrino events at IceCube and the Fermi bubbles

Multimessenger study of the Fermi bubbles: Very high energy gamma rays and neutrinos

The KM3NeT deep-sea neutrino telescope

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