2007ApJ...655..396H

Query : 2007ApJ...655..396H

2007ApJ...655..396H - Astrophys. J., 655, 396-405 (2007/January-3)

Very high energy observations of gamma-ray burst locations with the Whipple telescope.

HORAN D., ATKINS R.W., BADRAN H.M., BLAYLOCK G., BRADBURY S.M., BUCKLEY J.H., BYRUM K.L., CELIK O., CHOW Y.C.K., COGAN P., CUI W., DANIEL M.K., DE LA CALLE PEREZ I., DOWDALL C., FALCONE A.D., FEGAN D.J., FEGAN S.J., FINLEY J.P., FORTIN P., FORTSON L.F., GILLANDERS G.H., GRUBE J., GUTIERREZ K.J., HALL J., HANNA D., HOLDER J., HUGHES S.B., HUMENSKY T.B., KENNY G.E., KERTZMAN M., KIEDA D.B., KILDEA J., KRAWCZYNSKI H., KRENNRICH F., LANG M.J., LEBOHEC S., MAIER G., MORIARTY P., NAGAI T., ONG R.A., PERKINS J.S., PETRY D., QUINN J., QUINN M., RAGAN K., REYNOLDS P.T., ROSE H.J., SCHROEDTER M., SEMBROSKI G.H., STEELE D., SWORDY S.P., TONER J.A., VALCARCEL L., VASSILIEV V.V., WAGNER R.G., WAKELY S.P., WEEKES T.C., WHITE R.J. and WILLIAMS D.A.

Abstract (from CDS):

Gamma-ray burst (GRB) observations at very high energies (VHE; E>100 GeV) can impose tight constraints on some GRB emission models. Many GRB afterglow models predict a VHE component similar to that seen in blazars and plerions, in which the GRB spectral energy distribution has a double-peaked shape extending into the VHE regime. VHE emission coincident with delayed X-ray flare emission has also been predicted. GRB follow-up observations have had high priority in the observing program at the Whipple 10 m gamma-ray telescope, and GRBs will continue to be high-priority targets as the next-generation observatory, VERITAS, comes online. Upper limits on the VHE emission at late times (≳4 hr) from seven GRBs observed with the Whipple Telescope are reported here.

Abstract Copyright: ∼

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

Simbad objects: 20

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Number of rows : 20
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 3B 940217 gB 01 56.3 +04 33           ~ 204 0
2 GRB 021112 gB 02 36 52 +48 50.9           ~ 22 0
3 GRB 031026 gB 03 18.7 +28 22           ~ 21 0
4 M 1 SNR 05 34 30.9 +22 00 53           ~ 6199 1
5 V* CM Tau Psr 05 34 31.9474694616 +22 00 52.153698024           ~ 5267 0
6 1B 910503 gB 05 49.8 +38 44           ~ 133 0
7 3B 940301 gB 06 54.0 +64 21           ~ 70 0
8 SN 2003lw SN* 08 02 30.1 -39 51 03       20.23   SNIc: 549 0
9 SN 2002lt SN* 08 08 59.858 +06 43 37.52           SNIc: 353 1
10 SN 2003dh SN* 10 44 50.030 +21 31 18.15     16.2     SNIcpec 1210 1
11 2B 930131 gB 12 08.2 -08 14           ~ 125 0
12 GRB 990123 gB 15 25 29 +44 45.0     8.95     ~ 990 1
13 QSO B1553+113 BLL 15 55 43.0440048528 +11 11 24.365649948 14.91 14.72 14.57 13.99   ~ 572 1
14 GRB 040422 gB 18 42 01 +01 58.9           ~ 20 0
15 GRB 030501 gB 19 05 30 +06 18.4           ~ 28 0
16 GRB 970417A gB 19 21 +54.2           ~ 56 0
17 SN 1998bw SN* 19 35 03.17 -52 50 46.1   14.09       SNIc 1827 2
18 GRB 920925C gB 20 03 +25.5           ~ 18 0
19 4B 941017 gB 20 06.2 +09 49           ~ 93 0
20 GRB 021204 gB ~ ~           ~ 6 0

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