Status of the IceCube Neutrino Observatory

Ahrens, J.; Bahcall, John N.; Bai, X.; Bay, R.; Becka, T.; Becker, K. H.; Berley, D.; Bernardini, E.; Bertrand, Daniel; Besson, D.; Blaufuss, E.; Boersma, D. J.; Böser, S.; Böhm, C.; Botner, O.; Bouchta, A.; Bouhali, O.; Burgess, T.; Carithers, W.; Castermans, T.; Cavin, John; Chinowsky, W.; Chirkin, D.; Collin, Bertrand; Conrad, J.; Cooley, J.; Cowen, D. F.; Davour, Anna; Clercq, C. De; DeYoung, T.; Desiati, P.; Ehrlich, R.; Ellsworth, R. W.; Evenson, P. A.; Fazely, A. R.; Feser, T.; Gaisser, T. K.; Gallagher, J.; Ganugapati, R.; Geenen, H.; Goldschmidt, A.; Goodman, J. A.; Gunasingha, R. M.; Hallgren, A.; Halzen, F.; Hanson, K.; Hardtke, R.; Hauschildt, T.; Hays, D.; Helbing, K.; Hellwig, M.; Herquet, P.; Hill, G. C.; Hubert, D.; Hughey, B.; Hulth, P. O.; Hultqvist, K.; Hundertmark, S.; Jacobsen, J.; Japaridze, G. S.; Jones, Aaron; Karle, A.; Kawai, H.; Kestel, M.; Kitamura, N.; Koch, R.; Köpke, L.; Kowalski, M.; Lamoureux, J.I.; Leich, H.; Liubarsky, I.; Madsen, Jim; Matis, H. S.; McParland, C.; Messarius, T.; Mészáros, P.; Minaeva, Y.; Minor, R.H.; Miočinović, P.; Miyamoto, H.; Morse, R.; Nahnhauer, R.; Neunhöffer, T.; Nießen, P.; Nygren, D. R.; Öğelman, H.; Olbrechts, Ph.; Patton, S.; Paulos, R.; Heros, C. Pérez de los; Pohl, A. C.; Pretz, J.; Price, P. B.; Przybylski, G. T.; Rawlins, K.; Razzaque, S.; Resconi, E.; Rhode, W.; Ribordy, M.; Richter, S.; Sander, H. G.; Schinarakis, K.; Schlenstedt, S.; Schneider, D.; Schwarz, R.; Seckel, D.; Smith, A. J.; Solarz, M.; Spiczak, G. M.; Spiering, C.; Stamatikos, M.; Stanev, T.; Steele, D.; Steffen, P.; Stezelberger, T.; Stokstad, R. G.; Sulanke, K.-H.; Sullivan, G. W.; Sumner, T. J.; Taboada, I.; Tilav, S.; Eijndhoven, N. van; Wagner, Wolfgang; Walck, C.; Wang, R.-R; Wiebusch, C. H.; Wiedemann, C.; Wischnewski, R.; Wissing, H.; Woschnagg, K.; Yoshida, Shigeru

doi:10.1016/j.newar.2003.12.031

Cited by 20 publications

(13 citation statements)

References 14 publications

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“…beyond the energy of current fixed target experiments. With a detector area roughly 1,000 times the area of the MINOS FD, IceCube should have a cosmic ray muon rate of upon completion of construction (Boreal Spring, 2011) of 1,700 Hz [21]. Assuming a temperature data set of comparable quality to the BADC ECMWF data [22] used by the MINOS-FD analysis [5], the statistical uncertainty in α T could be reduced to ±0.001.…”

Section: Methods For Measurement Of Atmospheric K/π Ratiomentioning

confidence: 99%

The atmospheric charged kaon/pion ratio using seasonal variation methods

Grashorn

Jong

Goodman

et al. 2010

Astroparticle Physics

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Observed since the 1950's, the seasonal effect on underground muons is a well studied phenomenon. The interaction height of incident cosmic rays changes as the temperature of the atmosphere changes, which affects the production height of mesons (mostly pions and kaons). The decay of these mesons produces muons that can be detected underground. The production of muons is dominated by pion decay, and previous work did not include the effect of kaons. In this work, the methods of Barrett and MACRO are extended to include the effect of kaons. These efforts give rise to a new method to measure the atmospheric K/$\pi$ ratio at energies beyond the reach of current fixed target experiments. These methods were applied to data from the MINOS far detector. A method is developed for making these measurements at other underground detectors, including OPERA, Super-K, IceCube, Baksan and the MINOS near detector.Comment: 15 pages, 4 figures, submitted to Astropart. Phy

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Section: Methods For Measurement Of Atmospheric K/π Ratiomentioning

confidence: 99%

The atmospheric charged kaon/pion ratio using seasonal variation methods

Grashorn

Jong

Goodman

et al. 2010

Astroparticle Physics

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“…For CC interactions of ν µ 's leading to muon tracks through the volume of a H 2 O-based neutrino telescope, we employ the detection probability presented by Halzen & Hooper (2002). Such detectors include, buried in the ice at the South Pole, (the currently-operating) AMANDA (Ahrens et al 2004b) and (AMANDA's under-construction, km 3 -scale replacement) IceCube (Ahrens et al 2004a), and, in the deep Mediterranean, the prototype-stage, 0.1 km 2 area ANTARES (Korolkova et al 2004) or a future, km 3 -scale upgrade of this device.…”

Section: Event Ratesmentioning

confidence: 99%

Neutrinos from the Galactic Center in the Light of Its Gamma-Ray Detection at TeV Energy

Crocker

Melia

Volkas

2005

ApJ

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We re-evaluate the event rate expected in km 3 -scale detectors for neutrinos from the direction of the Galactic Center (GC) in light of recent spectral measurements obtained by the HESS instrument for ∼TeV γ-radiation from this direction. In the most plausible scenario the re-evaluated event rate is smaller than that previously calculated-and here re-calculated-on the basis of EGRET data. However, the GC TeV γ-ray detections by the Whipple, CANGAROO, and HESS instruments, together with the strong indications for an overabundance of cosmic rays coming from the GC at EeV energies, strengthen the expectation for a detectable, TeV-PeV GC neutrino signal from proton-proton interactions in that region. If the TeV gamma-ray-EeV cosmic ray anisotropy connection is correct, this signal will be detectable within a year and half for km 3 -scale neutrino detectors in the Northern Hemisphere at super-TeV energies and, significantly, should also be detectable in 1.6 years by the South Polar IceCube detector at energies 10 14 eV. The GC neutrino signal should also produce a detectable signal from neutrino showering and resonant W − production by ν e 's in the volume of a km 3 -scale detector.

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“…These started with GASP (Morse & Gaidos, 1990), a gamma-ray telescope at the South Pole, developed through the SPASE cosmic ray air shower array (Smith et al 1989) and then led to the AMANDA neutrino detector (Andrés et al 2000). This was a fore-runner to IceCube, which makes use of a cubic kilometre of pure ice to search for sources of high-energy neutrino emission (Ahrens et al 2004). At a cost of over US$300M, IceCube is the single most expensive scientific experiment ever to be conducted in Antarctica.…”

Section: A Brief History Of Antarctic Astronomymentioning

confidence: 99%

“…AMANDA served as the prototype for IceCube, the largest science experiment yet to take place in Antarctica (Ahrens et al 2004). Almost complete (see Fig.…”

Section: High-energy Astrophysicsmentioning

confidence: 99%

Astronomy in Antarctica

Burton

2004

Organizations and Strategies in Astronomy

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Antarctica provides a unique environment for astronomers to practice their trade. The cold, dry and stable air found above the high Antarctic plateau, as well as the pure ice below, offers new opportunities for the conduct of observational astronomy across both the photon and the particle spectrum. The summits of the Antarctic plateau provide the best seeing conditions, the darkest skies and the most transparent atmosphere of any earth-based observing site. Astronomical activities are now underway at four plateau sites: the Amundsen-Scott South Pole Station, Concordia Station at Dome C, Kunlun Station at Dome A and Fuji Station at Dome F, in addition to long duration ballooning from the coastal station of McMurdo, at stations run by the USA, France / Italy, China, Japan and the USA, respectively. The astronomy conducted from Antarctica includes optical, infrared, terahertz and sub-millimetre astronomy, measurements of cosmic microwave background anisotropies, solar astronomy, as well as high energy astrophysics involving the measurement of cosmic rays, gamma rays and neutrinos. Antarctica is also the richest source of meteorites on our planet.An extensive range of site testing measurements have been made over the high plateau sites. In this paper we summarise the facets of Antarctica that are driving developments in astronomy there, and review the results of the site testing experiments undertaken to quantify those characteristics of the Antarctic plateau relevant for astronomical observation. We also outline the historical development of the astronomy on the continent, and then review the principal scientific results to have emerged over the past three decades of activity in the discipline. These range from determination of the dominant frequencies of the 5 minute solar oscillation in 1979 to the highest angular scale measurements yet made of the power spectrum of the CMBR anisotropies in 2010. They span through infrared views of the galactic ecology in star formation complexes in 1999, the first clear demonstration that the Universe was flat in 2000, the first detection of polarization in the CMBR in 2002, the mapping of the warm molecular gas across the ∼ 300 pc extent of the Central Molecular Zone of our Galaxy in 2003, the measurement of cosmic neutrinos in 2005, and imaging of the thermal Sunyaev Zel'dovich effect in galaxy clusters in 2008.This review also discusses how science is conducted in Antarctica, and in particular the difficulties, as well as the advantages, faced by astronomers seeking to bring their experiments there. It also reviews some of the political issues that will be encountered, both at national and international level. Finally, the review discusses where Antarctic astronomy may be heading in the coming decade, in particular plans for infrared and terahertz astronomy, including the new facilities being considered for these wavebands at the high plateau stations.

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Status of the IceCube Neutrino Observatory

Cited by 20 publications

References 14 publications

The atmospheric charged kaon/pion ratio using seasonal variation methods

The atmospheric charged kaon/pion ratio using seasonal variation methods

Neutrinos from the Galactic Center in the Light of Its Gamma-Ray Detection at TeV Energy

Astronomy in Antarctica

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