2007ApJ...664..397A

Query : 2007ApJ...664..397A

2007ApJ...664..397A - Astrophys. J., 664, 397-410 (2007/July-3)

Search for neutrino-induced cascades from gamma-ray bursts with AMANDA.

ACHTERBERG A., ACKERMANN M., ADAMS J., AHRENS J., ANDEEN K., AUFFENBERG J., BAHCALL J.N., BAI X., BARET B., BARWICK S.W., BAY R., BEATTIE K., BECKA T., BECKER J.K., BECKER K.-H., BERGHAUS P., BERLEY D., BERNARDINI E., BERTRAND D., BESSON D.Z., BLAUFUSS E., BOERSMA D.J., BOHM C., BOLMONT J., BOSER S., BOTNER O., BOUCHTA A., BRAUN J., BURGESS C., BURGESS T., CASTERMANS T., CHIRKIN D., CHRISTY B., CLEM J., COWEN D.F., D'AGOSTINO M.V., DAVOUR A., DAY C.T., DE CLERCQ C., DEMIRORS L., DESCAMPS F., DESIATI P., DEYOUNG T., DIAZ-VELEZ J.C., DREYER J., DUMM J.P., DUVOORT M.R., EDWARDS W.R., EHRLICH R., EISCH J., ELLSWORTH R.W., EVENSON P.A., FADIRAN O., FAZELY A.R., FILIMONOV K., FOERSTER N.M., FOX B.D., FRANCKOWIAK A., GAISSER T.K., GALLAGHER J., GANUGAPATI R., GEENEN H., GERHARDT L., GOLDSCHMIDT A., GOODMAN J.A., GOZZINI R., GRIESEL T., GRULLON S., GROSS A., GUNASINGHA R.M., GURTNER M., HALLGREN A., HALZEN F., HAN K., HANSON K., HARDTKE D., HARDTKE R., HART J.E., HASEGAWA Y., HAUSCHILDT T., HAYS D., HEISE J., HELBING K., HELLWIG M., HERQUET P., HILL G.C., HODGES J., HOFFMAN K.D., HOMMEZ B., HOSHINA K., HUBERT D., HUGHEY B., HULTH P.O., HULTQVIST K., HULSS J.-P., HUNDERTMARK S., INABA M., ISHIHARA A., JACOBSEN J., JAPARIDZE G.S., JOHANSSON H., JONES A., JOSEPH J.M., KAMPERT K.-H., KARG T., KARLE A., KAWAI H., KELLEY J.L., KITAMURA N., KLEIN S.R., KLEPSER S., KOHNEN G., KOLANOSKI H., KOPKE L., KOWALSKI M., KOWARIK T., KRASBERG M., KUEHN K., LABARE M., LANDSMAN H., LEICH H., LEIER D., LIUBARSKY I., LUNDBERG J., LUNEMANN J., MADSEN J., MASE K., MATIS H.S., McCAULEY T., McPARLAND C.P., MELI A., MESSARIUS T., MESZAROS P., MIYAMOTO H., MOKHTARANI A., MONTARULI T., MOREY A., MORSE R., MOVIT S.M., MUNICH K., NAHNHAUER R., NAM J.W., NIESSEN P., NYGREN D.R., OGELMAN H., OLIVAS A., PATTON S., PENA-GARAY C., PEREZ DE LOS HEROS C., PIEGSA A., PIELOTH D., POHL A.C., PORRATA R., PRETZ J., PRICE P.B., PRZYBYLSKI G.T., RAWLINS K., RAZZAQUE S., RESCONI E., RHODE W., RIBORDY M., RIZZO A., ROBBINS S., ROTH P., ROTT C., RUTLEDGE D., RYCKBOSCH D., SANDER H.-G., SARKAR S., SCHLENSTEDT S., SCHMIDT T., SCHNEIDER D., SECKEL D., SEMBURG B., SEO S.H., SEUNARINE S., SILVESTRI A., SMITH A.J., SOLARZ M., SONG C., SOPHER J.E., SPICZAK G.M., SPIERING C., STAMATIKOS M., STANEV T., STEFFEN P., STEZELBERGER T., STOKSTAD R.G., STOUFER M.C., STOYANOV S., STRAHLER E.A., STRASZHEIM T., SULANKE K.-H., SULLIVAN G.W., SUMNER T.J., TABOADA I., TARASOVA O., TEPE A., THOLLANDER L., TILAV S., TLUCZYKONT M., TOALE P.A., TURCAN D., VAN EIJNDHOVEN N., VANDENBROUCKE J., VAN OVERLOOP A., VISCOMI V., VOIGT B., WAGNER W., WALCK C., WALDMANN H., WALTER M., WANG Y.-R., WENDT C., WIEBUSCH C.H., WIKSTROEM G., WILLIAMS D.R., WISCHNEWSKI R., WISSING H., WOSCHNAGG K., XU X.W., YODH G., YOSHIDA S. and ZORNOZA J.D.

Abstract (from CDS):

Using the neutrino telescope AMANDA-II, we have conducted two analyses searching for neutrino-induced cascades from gamma-ray bursts. No evidence of astrophysical neutrinos was found, and limits are presented for several models. We also present neutrino effective areas which allow the calculation of limits for any neutrino production model. The first analysis looked for a statistical excess of events within a sliding window of 1 or 100 s (for short and long burst classes, respectively) during the years 2001-2003. The resulting upper limit on the diffuse flux normalization times E2 for the Waxman-Bahcall model at 1 PeV is 1.6x10–6 GeV cm–2 s–1 sr–1 (a factor of 120 above the theoretical prediction). For this search 90% of the neutrinos would fall in the energy range 50 TeV to 7 PeV. The second analysis looked for neutrino-induced cascades in coincidence with 73 bursts detected by BATSE in the year 2000. The resulting upper limit on the diffuse flux normalization times E2, also at 1 PeV, is 1.5x10–6 GeV cm–2 s–1 sr–1 (a factor of 110 above the theoretical prediction) for the same energy range. The neutrino-induced cascade channel is complementary to the up-going muon channel. We comment on its advantages for searches of neutrinos from GRBs and its future use with IceCube.

Abstract Copyright: ∼

Journal keyword(s): Gamma Rays: Bursts - Neutrinos - Telescopes

Simbad objects: 78

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Number of rows : 78
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 GRB 000310B gB 00 22 -03.4           ~ 5 0
2 GRB 000217A gB 00 52 +34.7           ~ 8 0
3 GRB 000331B gB 01 12 -44.8           ~ 7 0
4 GRB 000317 gB 01 21 +30.7           ~ 7 0
5 GRB 000331C gB 01 31 +63.1           ~ 8 0
6 GRB 000227 gB 02 40 -03.8           ~ 7 0
7 GRB 000306A gB 03 21 -08.5           ~ 6 0
8 GRB 000321 gB 03 28 +35.9           ~ 6 0
9 GRB 000403 gB 03 38 +23.7           ~ 7 0
10 GRB 000302A gB 03 38 +53.6           ~ 14 0
11 GRB 000222 gB 04 24 +70.5           ~ 6 0
12 GRB 000319 gB 04 42 -14.0           ~ 4 0
13 GRB 000518 gB 04 52 +44.4           ~ 7 0
14 GRB 000320 gB 05 27 +03.4           ~ 5 0
15 GRB 000307 gB 05 55 +05.8           ~ 18 0
16 GRB 000508C gB 06 06 -01.3           ~ 11 0
17 GRB 000312B gB 06 23 +10.9           ~ 6 1
18 GRB 000429 gB 06 32 -04.1           ~ 19 0
19 GRB 000424B gB 06 58 52.3 +49 52 23           ~ 24 0
20 GRB 000225 gB 07 16 +01.1           ~ 8 0
21 GRB 000221 gB 07 16 +73.8           ~ 13 0
22 GRB 000517 gB 07 31 +76.3           ~ 3 0
23 GRB 000524 gB 07 32 -40.9           ~ 9 0
24 GRB 000420B gB 08 26 -15.8           ~ 9 0
25 GRB 000310A gB 08 26 -10.7           ~ 6 0
26 GRB 000415B gB 08 38 +70.5           ~ 7 0
27 GRB 000408B gB 08 53 +68.8           ~ 19 0
28 GRB 000420A gB 09 16.2 -44 40           ~ 5 0
29 GRB 000314 gB 09 18 +42.8           ~ 8 0
30 GRB 000213 gB 09 26 +07.2           ~ 6 0
31 GRB 000513B gB 10 28 -10.2           ~ 7 0
32 GRB 000407 gB 10 55 -71.2           ~ 9 0
33 GRB 000331A gB 11 17.6 -15 01           ~ 3 0
34 GRB 000421 gB 11 37 +16.8           ~ 8 0
35 GRB 000302B gB 11 51 +23.9           ~ 5 0
36 GRB 000220 gB 12 12 +67.3           ~ 9 0
37 GRB 000418 gB 12 25 21 +20 05.0           ~ 219 0
38 GRB 000313B gB 12 57 +20.0           ~ 13 0
39 GRB 000323 gB 13 04 +57.1           ~ 22 0
40 GRB 000415C gB 13 16 -31.0           ~ 10 1
41 GRB 000508A gB 13 25 +03.9           ~ 7 0
42 GRB 000412 gB 13 34 -54.6           ~ 8 0
43 GRB 000410 gB 13 53 -13.5           ~ 5 0
44 GRB 000324 gB 14 06 -21.2           ~ 9 0
45 GRB 000417 gB 15 16 -05.0           ~ 4 0
46 GRB 000306B gB 15 23 +38.7           ~ 9 0
47 GRB 000526 gB 15 25.2 -10 19           ~ 13 0
48 GRB 000424A gB 15 42 +68.4           ~ 5 0
49 GRB 000520 gB 15 48 +01.2           ~ 6 0
50 GRB 000502 gB 16 31 -45.1           ~ 4 0
51 GRB 000228 gB 16 51 +65.5           ~ 3 0
52 GRB 000409 gB 16 53 +78.5           ~ 5 0
53 GRB 000508B gB 16 57 -24.1           ~ 19 0
54 GRB 000326B gB 18 02 -46.2           ~ 5 0
55 GRB 000303 gB 18 06 +60.7           ~ 5 0
56 GRB 000525 gB 18 54 -39.3           ~ 6 0
57 GRB 000401 gB 19 19 +81.8           ~ 5 0
58 GRB 000511B gB 19 31 -06.3           ~ 6 0
59 GRB 000229 gB 20 01 +42.9           ~ 9 0
60 GRB 000330A gB 20 49.6 +32 00           ~ 3 1
61 GRB 000420C gB 21 12 -65.2           ~ 7 0
62 GRB 000312A gB 21 12 +34.2           ~ 10 1
63 GRB 000226A gB 21 28 57.8 -19 45 42           ~ 16 0
64 GRB 000326A gB 22 11 23.5 -26 08 46           ~ 17 0
65 GRB 000511A gB 22 16 -38.3           ~ 10 0
66 GRB 000513A gB 22 34 -47.3           ~ 7 0
67 GRB 000509 gB 22 56.8 -39 16           ~ 3 0
68 GRB 000402 gB 22 59 +04.7           ~ 9 0
69 GRB 000519 gB 23 04 38.6 +01 10 17           ~ 26 0
70 GRB 000301A gB 23 39 27.1 +75 47 13           ~ 15 0
71 GRB 000330B gB 23 53 14 +39 15.6           ~ 4 1
72 GRB 000408A gB ~ ~           ~ 2 0
73 GRB 000313A gB ~ ~           ~ 2 0
74 GRB 000217B gB ~ ~           ~ 3 0
75 GRB 000219 gB ~ ~           ~ 2 0
76 GRB 000415A gB ~ ~           ~ 1 0
77 GRB 000521 gB ~ ~           ~ 2 0
78 GRB 000226B gB ~ ~           ~ 4 0

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