2005ApJ...630..996A

Query : 2005ApJ...630..996A

2005ApJ...630..996A - Astrophys. J., 630, 996-1002 (2005/September-2)

Constraints on very high energy gamma-ray emission from gamma-ray bursts.

ATKINS R., BENBOW W., BERLEY D., BLAUFUSS E., COYNE D.G., DE YOUNG T., DINGUS B.L., DORFAN D.E., ELLSWORTH R.W., FLEYSHER L., FLEYSHER R., GONZALEZ M.M., GOODMAN J.A., HAYS E., HOFFMAN C.M., KELLEY L.A., LANSDELL C.P., LINNEMANN J.T., McENERY J.E., MINCER A.I., MORALES M.F., NEMETHY P., NOYES D., RYAN J.M., SAMUELSON F.W., SAZ PARKINSON P.M., SHOUP A., SINNIS G., SMITH A.J., SULLIVAN G.W., WILLIAMS D.A., WILSON M.E., XU X.W. and YODH G.B.

Abstract (from CDS):

The Milagro Gamma-Ray Observatory employs a water Cerenkov detector to observe extensive air showers produced by high-energy particles interacting in the Earth's atmosphere. Milagro has a wide field of view and high duty cycle, monitoring the northern sky almost continuously in the 100 GeV to 100 TeV energy range. Milagro is thus uniquely capable of searching for very high energy emission from gamma-ray bursts (GRBs) during the prompt emission phase. Detection of >100 GeV counterparts would place powerful constraints on GRB mechanisms. Twenty-five satellite-triggered GRBs occurred within the field of view of Milagro between 2000 January and 2001 December. We have searched for counterparts to these GRBs and found no significant emission from any of the burst positions. Due to the absorption of high-energy gamma rays by the extragalactic background light, detections are only expected to be possible for redshifts less than ∼0.5. Three of the GRBs studied have measured redshifts. GRB 010921 has a redshift low enough (0.45) to allow an upper limit on the fluence to place an observational constraint on potential GRB models.

Abstract Copyright: ∼

Journal keyword(s): Gamma Rays: Bursts - Gamma Rays: Observations

Simbad objects: 29

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Number of rows : 29
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 GRB 000212 gB 00 59 +33.0           ~ 9 0
2 GRB 000317 gB 01 21 +30.7           ~ 7 0
3 GRB 000331C gB 01 31 +63.1           ~ 8 0
4 GRB 010220 gB 02 36 59.0 +61 46 00           ~ 40 0
5 GRB 011130 gB 03 05 26.9 +03 49 30           ~ 44 0
6 GRB 000302A gB 03 38 +53.6           ~ 14 0
7 GRB 011212 gB 05 00 05 +32 07.6           ~ 21 0
8 GRB 000508C gB 06 06 -01.3           ~ 11 0
9 GRB 000408B gB 08 53 +68.8           ~ 19 0
10 GRB 000113 gB 11 20 +14.6           ~ 7 0
11 GRB 000727 gB 11 45 10.5 +17 24 34           ~ 7 0
12 GRB 001105 gB 13 01.9 +35 29           ~ 12 0
13 GRB 010613 gB 13 02 53 -21 11.0           ~ 10 0
14 GRB 001018 gB 13 14 10.3 +11 48 32           ~ 15 0
15 GRB 000630 gB 14 47.2 +41 13           ~ 53 1
16 GRB 000615 gB 15 32.6 +73 48           ~ 27 0
17 GRB 000301C gB 16 20 18.5 +29 26 35           ~ 356 0
18 GRB 000926 gB 17 04 15 +51 46.0           ~ 364 0
19 GRB 001019 gB 17 11.7 +35 20           ~ 8 0
20 GRB 010104 gB 17 49 45 +18 13.6           ~ 8 0
21 GRB 001017 gB 18 08 42 -02 59.6           ~ 3 0
22 GRB 970417A gB 19 21 +54.2           ~ 56 0
23 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1821 2
24 GRB 920925C gB 20 03 +25.5           ~ 18 0
25 4B 941017 gB 20 06.2 +09 49           ~ 93 0
26 GRB 000226A gB 21 28 57.8 -19 45 42           ~ 15 0
27 GRB 010921 gB 22 55 59.90 +40 55 52.9           ~ 171 1
28 [LDM2003] GRB J225559.9+405553 G 22 55 59.9 +40 55 53           ~ 12 1
29 GRB 000330B gB 23 53 14 +39 15.6           ~ 4 1

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