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First year performance of the IceCube neutrino telescope

Astroparticle Physics 26:3 (2006) 155-173

Authors:

A Achterberg, M Ackermann, J Adams, J Ahrens, K Andeen, DW Atlee, J Baccus, JN Bahcall, X Bai, B Baret, M Bartelt, SW Barwick, R Bay, K Beattie, T Becka, JK Becker, KH Becker, P Berghaus, D Berley, E Bernardini, D Bertrand, DZ Besson, E Blaufuss, DJ Boersma, C Bohm, S Böser, O Botner, A Bouchta, J Braun, C Burgess, T Burgess, T Castermans, J Cherwinka, D Chirkin, J Clem, DF Cowen, MV D'Agostino, A Davour, CT Day, C De Clercq, L Demirörs, P Desiati, T DeYoung, JC Diaz-Velez, J Dreyer, MR Duvoort, WR Edwards, R Ehrlich, J Eisch, A Elcheikh, RW Ellsworth, PA Evenson, O Fadiran, AR Fazely, T Feser, K Filimonov, BD Fox, TK Gaisser, J Gallagher, R Ganugapati, H Geenen, L Gerhardt, A Goldschmidt, JA Goodman, R Gozzini, MG Greene, S Grullon, A Groß, RM Gunasingha, M Gurtner, A Hallgren, F Halzen, K Han, K Hanson, D Hardtke, R Hardtke, T Harenberg, JE Hart, J Haugen, T Hauschildt, D Hays, J Heise, K Helbing, M Hellwig, P Herquet, GC Hill, J Hodges, KD Hoffman, K Hoshina, D Hubert, B Hughey, PO Hulth, K Hultqvist, S Hundertmark, JP Hülß, A Ishihara, J Jacobsen, GS Japaridze, A Jones, JM Joseph

Abstract:

The first sensors of the IceCube neutrino observatory were deployed at the South Pole during the austral summer of 2004-2005 and have been producing data since February 2005. One string of 60 sensors buried in the ice and a surface array of eight ice Cherenkov tanks took data until December 2005 when deployment of the next set of strings and tanks began. We have analyzed these data, demonstrating that the performance of the system meets or exceeds design requirements. Times are determined across the whole array to a relative precision of better than 3 ns, allowing reconstruction of muon tracks and light bursts in the ice, of air-showers in the surface array and of events seen in coincidence by surface and deep-ice detectors separated by up to 2.5 km. © 2006 Elsevier B.V. All rights reserved.
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Neutrino detectors in ICE: Results and perspectives

Frascati Physics Series 42:SPEC. ISS. (2006) 87-101

Authors:

A Achterberg, M Ackermann, J Adams, J Ahrens, K Andeen, DW Atlee, JN Bahcall, X Bai, B Baret, M Bartelt, SW Barwick, R Bay, K Beattie, T Becka, JK Becker, KH Becker, P Berghaus, D Berley, E Bernardini, D Bertrand, DZ Besson, E Blaufuss, DJ Boersma, C Bohm, J Bolmont, S Böser, O Botner, A Bouchta, J Braun, C Burgess, T Burgess, T Castermans, D Chirkin, J Clem, DF Cowen, MV D'Agostino, A Davour, CT Day, C De Clercq, L Demirörs, F Descamps, P Desiati, T DeYoung, JC Diaz-Velez, J Dreyer, MR Duvoort, WR Edwards, R Ehrlich, J Eisch, RW Ellsworth, PA Evenson, O Fadiran, AR Fazely, T Feser, K Filimonov, BD Fox, TK Gaisser, J Gallagher, R Ganugapati, H Geenen, L Gerhardt, A Goldschmidt, JA Goodman, R Gozzini, S Grullon, A Groß, RM Gunasingha, M Gurtner, A Hallgren, F Halzen, K Han, K Hanson, D Hardtke, R Hardtke, T Harenberg, JE Hart, T Hauschildt, D Hays, J Heise, K Helbing, M Hellwig, P Herquet, GC Hill, J Hodges, KD Hoffman, B Hommez, K Hoshina, D Hubert, B Hughey, PO Hulth, K Hultqvist, S Hundertmark, JP Hülß, A Ishihara, J Jacobsen, GS Japaridze, A Jones, JM Joseph, KH Kampert, A Karle

Abstract:

The AMANDA neutrino detector has been in operation at the South Pole for several years. A number of searches for extraterrestrial sources of high energy neutrinos have been performed. A selection of results is presented in this paper. The much larger IceCube detector will extend the instrumented ice volume to a cubic kilometer and 9 out of 80 planned IceCube strings have been deployed to date. We present the status for both detectors.

Contributions to 2nd TeV Particle Astrophysics Conference (TeV PA II). Madison, Wisconsin 28-31 Aug 2006

TeV particle astrophysics. Proceedings, 2nd Workshop, Madison, USA, August 28-31, 2006 (2006)

Authors:

A Achterberg, others
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Review of particle physics

33:1 (2006) 1-+

Authors:

W-M Yao, C Amsler, D Asner, RM Barnett, J Beringer, PR Burchat, CD Carone, C Caso, O Dahl, G D'Ambrosio, A De Gouvea, M Doser, S Eidelman, JL Feng, T Gherghetta, M Goodman, C Grab, DE Groom, A Gurtu, K Hagiwara, KG Hayes, JJ Hernandez-Rey, K Hikasa, H Jawahery, C Kolda, Y Kwon, ML Mangano, AV Manohar, A Masoni, R Miquel, K Moenig, H Murayama, K Nakamura, S Navas, KA Olive, L Pape, C Patrignani, A Piepke, G Punzi, G Raffelt, JG Smith, M Tanabashi, J Terning, NA Toernqvist, TG Trippe, P Vogel, T Watari, CG Wohl, RL Workman, PA Zyla, B Armstrong, G Harper, VS Lugovsky, PS Schaffner, M Artuso, KS Babu, HR Band, E Barberio, M Battaglia, H Bichel, O Biebel, P Bloch, E Blucher, RN Cahn, D Casper, A Cattai, A Ceccicco, D Chakraborty, RS Chivukula, G Cowan, T Damour, T De Grand, K Desler, MA Dobbs, M Drees, A Edwards, DA Edwards, VD Elvira, J Erler, W Fetscher, BD Fields, B Foster, D Froidevaux, TK Gaisser, L Garren, HJ Gerber, G Gerbier, L Gibbons, FJ Gilman, GF Giudice, AV Gritsan, M Grünewald, HE Haber, C Hagmann, I Hinchliffe, A Hocker, P Igo-Kemenes, JD Jackson, KF Johnson, D Karlen, B Kayser, D Kirkby, SR Klein, K Kleinknecht, JG Knowles, RV Kowalewski, P Kreitz, B Krusche, YV Kuyanov, O Lahav, P Langacker, A Liddle, Z Ligeti, TM Liss, L Littenberg, JC Liu, KS Lugovsky, SB Lugovsky, T Mannel, WJ Marciano, AD Martin, D Milstead, M Narain, P Nason, Y Nir, JA Peacock, SA Prell, A Quadt, S Raby, BN Ratcliff, EA Razuvaev, B Renk, PR Richardson, S Roesler, G Rolandi, MT Roman, LJ Rosenberg, CT Sachrajda, Y Salao, S Sarkar, M Schmitt, O Schneider, D Scott, T Sjöstrand, GF Smoot, P Sokolsky, S Spanier, H Spieler, A Stahl, T Staney, RE Streitmatter, T Sumiyoshi, NP Tkachenko, GH Trilling, G Valencia, K van Bibber, MG Vincter, DR Ward, BR Webber, JD Wells, M Whalley, L Wolfenstein, J Womersley, CL Woody, A Yamamoto, OV Zenin, J Zhang, RY Zhu
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Large-scale galaxy correlations as a test for dark energy

ArXiv astro-ph/0512085 (2005)

Authors:

Alain Blanchard, Marian Douspis, Michael Rowan-Robinson, Subir Sarkar

Abstract:

We have shown earlier that, contrary to popular belief, Einstein--de Sitter (E--deS) models can still fit the {\sl WMAP} data on the cosmic microwave background provided one adopts a low Hubble constant and relaxes the usual assumption that the primordial density perturbation is scale-free. The recent {\sl SDSS} measurement of the large-scale correlation function of luminous red galaxies at $z \sim 0.35$ has however provided a new constraint by detecting a `baryon acoustic peak'. Our best-fit E--deS models do possess a baryonic feature at a similar physical scale as the best-fit $\Lambda$CDM concordance model, but do not fit the new observations as well as the latter. In particular the shape of the correlation function in the range $\sim 10-100 h^{-1}$ Mpc cannot be reproduced properly without violating the CMB angular power spectrum in the multipole range $l \sim 100-1000$. Thus, the combination of the CMB fluctuations and the shape of the correlation function up to $\sim 100 h^{-1}$Mpc, if confirmed, does seem to require dark energy for a homogeneous cosmological model based on (adiabatic) inflationary perturbations.
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