Table 7: Properties of the prompt emission of BeppoSAX Gamma Ray Bursts reported in Table 6. We indicate the duration and fluence both in the X-ray (2.0-10.0 keV band) and the $\gamma $-ray (40.0-700 keV band). An X following the source name denotes an X-ray-rich GRB or an X-ray flash.
GRB name $\rm\gamma$-ray X-ray $\rm\gamma$-ray X-ray Ref.
  duration duration fluence fluence  
  (T, s) (T, s) $\rm 10^{-7}$ erg cm-2 $\rm 10^{-7}$ erg cm-2  
GRB 960720 8 17 $26\pm3$ $0.8\pm0.2$ 1, 2, 3
GRB 970111 43 60 $430\pm30$ $16\pm1$ 4, 2, 3
GRB 970228 80 80 64.5 15.4 5
GRB 970402 150 150 $82\pm9$ $4.7\pm1.5$ 2
GRB 970508 15 29 14.5 5.3 5
GRB 971214 35 35 64.9 2.34 5,3
GRB 971227 7 7 $6.6\pm0.7$ 1 6,3
GRB 980109 20 20 $32.3\pm3$ - 3,7
GRB 980326 9 9 $7.5\pm1.5$ $2\pm0.3$ 5, 3
GRB 980329 58 68 $650\pm50$ $9.7\pm0.7$ 5,
GRB 980425 31 40 $28.5\pm5$ $7.8\pm0.2$ 2, 3
GRB 980515 15 20 $23\pm3$ - 7, 3
GRB 980519 30 190 $81\pm5$ 18 8,9, 3
GRB 980613 50 50 9.9 2.3 5, 3
GRB 981226X 20 260 $4\pm1$ $5.7\pm1$ 10,3
GRB 980703 90 - $\rm 300\pm100$ - 11
GRB 990123 100 100 $\rm 1790$ 22.9 5, 3
GRB 990217 25 25 $\rm 12.7\pm1.5$ - 7, 3
GRB 990510 75 80 $\rm 181$ 17.9 3, 5
GRB 990625 11 11 - - 3
GRB 990627 28 60 - $\sim$15 3,12
GRB 990704X 23 40 $\rm 10\pm1$ $\rm 15\pm0.8$ 13, 3
GRB 990705 42 45 $\rm 423$ $\rm 22.5$ 5, 3
GRB 990712 30 30 $\rm 65\pm3$ $\rm 28.6$ 5, 3
GRB 990806 30 30 $\sim$42 $\sim$2.5 14, 3
GRB 990907 1 220 - - 3
GRB 990908 50 130 - - 3
GRB 991014 3 10 $\rm 9\pm1$ 1 15,16, 3
GRB 991105 13 40 - - 3
GRB 991106 a - 5 <1.2b   17
GRB 000210 10 115 $\rm 610\pm20$ $\sim$15 18, 3
GRB 000214 115 100 $\rm 61.7$ $\rm 11.6$ 5, 3
GRB 000528 80 120 $\rm 14.4\pm0.4$ - 19, 20
GRB 000529 14 30 - - 3
GRB 000615X 12 120 $\rm 9.8\pm0.9$ $\rm 17\pm1$ 21, 3
GRB 000620 15 20 - - 3
GRB 001011 31 60 - - 3
GRB 001109 60 65 $\rm 49.7\pm1.9$ $\rm 6.4\pm0.33$ 22, 3
GRB 010213 23 25 - - 3
GRB 010214 15 30 $\rm 45\pm0.8$ $\rm 2\pm0.3$ 23
GRB 010220 40 150 - - 3
GRB 010222 170 280 $\rm 753$ $\rm 95$ 5, 3
GRB 010304 15 24 - - 3
GRB 010501 37 41 - - 3
GRB 010412 74 90 - - 3
GRB 010518 25 30 - - 3
GRB 011121 105 100 $\rm 1000\pm20$ $\rm 140\pm3$ 24, 3
GRB 011211 400 400 $\rm 37\pm4$ $\rm 11\pm1$ 24, 3
GRB 020321 70 90 30 0.9 25, 3
GRB 020322 15 50 - - 3
GRB 020409 40 60 - - 3
GRB 020410 1800 >1290 $\sim$290 >47 26, 3
GRB 020427X - 60 <2.9 $3.7\pm0.3$ 27, 3
a Perhaps not a GRB. See Cornelisse et al. (2000).
b Conservative $3\sigma$ upper limit based on GCN 448.
References: 1: Piro et al. (1998a), 2: Frontera et al. (2000a), 3: Frontera et al. (2004), 4: Feroci et al. (1998), 5: Amati et al. (2002), 6: Antonelli et al. (1999), 7: Amati et al. (1999), 8: Nicastro et al. (1999), 9: in't Zand et al. (1999), 10: Frontera et al. (2000b), 11: Amati et al. (1998), 12: Muller et al. (1999b), 13: Feroci et al. (2001), 14: Montanari et al. (2002), 15: Tassone et al. (1999), 16: in't Zand et al. (2000b), 17: Gandolfi et al. (1999), 18: Piro et al. (2002), 19: Guidorzi et al. (2000), 20: in't Zand et al. (2000a), 21: Nicastro et al. (2001), 22: Guidorzi et al. (2003), 23: Guidorzi et al. (2003), 24: Piro et al. (2005), 25: in't Zand et al. (2004), 26: Nicastro et al. (2004), and 27: Amati et al. (2004).
Note 1: When not available, values of 2-10 keV fluences have been calculated from the 2-26 keV fluences and assuming the spectral parameters reported in the references.
Note 2: The X-ray and $\gamma $ fluences reported by Amati et al. (2002) have been obtained by reporting the parameters of the WFC and GRBM spectra fit at z =0 (see Table 2 of the same article).


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