$\begin{figure} \includegraphics[width=8.8cm,clip]{MS2654f6.eps} \end{figure}$

Figure 6: Comparisons between our fitted CB model AG of GRB 000301c, at z=2.033, Eq. (8) and Fig. 5, with the observed optical data. The figure shows (from top to bottom) 1000 times the K-band results, 100 times the J-band, 10 times the I-band, the R-band, 1/10 of the V-band, 1/100 of the B-band and 1/1000 of the U-band. The contributions of the underlying galaxy and an expected (but, in this case, unobservable) SN1998bw-like SN have been subtracted.

$\begin{figure} \includegraphics[width=7.3cm,clip]{MS2654f7a.eps}\vspace*{4mm} \includegraphics[width=7.3cm,clip]{MS2654f7b.eps} \end{figure}$

Figure 7: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000301c. Upper panel: the light curve at 350 GHz. Lower panel: the light curve at 250 GHz.

$\begin{figure} \includegraphics[width=7.3cm,clip]{MS2654f8a.eps}\vspace*{4mm} \includegraphics[width=7.3cm,clip]{MS2654f8b.eps} \end{figure}$

Figure 8: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000301c. Upper panel: the light curve at 100 GHz. Lower panel: the light curve at 22.5 GHz.

$\begin{figure} \includegraphics[width=7.3cm,clip]{MS2654f9a.eps}\vspace*{4mm} \includegraphics[width=7.3cm,clip]{MS2654f9b.eps} \end{figure}$

Figure 9: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000301c. Upper panel: the light curve at 15 GHz. Lower panel: the light curve at 8.46 GHz.

$\begin{figure} \includegraphics[width=7.3cm,clip]{MS2654f10a.eps}\vspace*{4mm} \includegraphics[width=7.3cm,clip]{MS2654f10b.eps} \end{figure}$

Figure 10: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000301c. Upper panel: the light curve at 4.86 GHz. Lower panel: the light curve at 1.43 GHz.

$\begin{figure} \includegraphics[width=7.3cm,clip]{MS2654f11a.eps}\vspace*{4mm} \includegraphics[width=7.3cm,clip]{MS2654f11b.eps} \end{figure}$

Figure 11: The spectrum of the AG of GRB 000301c from radio to optical frequencies. Upper panel: in the time interval between 1 and 5 days after burst. Lower panel: in the time interval between 5 and 10 days after burst. The highest peaking curve in the upper pannel corresponds to the later time and in the lower panel to the earlier time.

$\begin{figure} \includegraphics[width=7.3cm,clip]{MS2654f12a.eps}\vspace*{4mm} \includegraphics[width=7.3cm,clip]{MS2654f12b.eps} \end{figure}$

Figure 12: The spectrum of the AG of GRB 000301c from radio to optical frequencies. Upper panel: in the time interval between 10 and 20 days after burst. Lower panel: in the time interval between 20 and 30 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=8.8cm,clip]{MS2654f13.eps} \end{figure}$

Figure 13: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed optical afterglow of GRB 000926 at z=2.037. The figure shows (from top to bottom) 1000 times the K-band results, 100 times the J-band, 10 times the I-band, the R-band, 1/10 of the V-band, 1/100 of the B-band and 1/1000 of the U-band. The contributions of the underlying galaxy and an expected (but, in this case, unobservable) SN1998bw-like SN have been subtracted.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f14a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f14b.eps} \end{figure}$

Figure 14: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000926. Upper panel: the light curve at 98.48 GHz. Lower panel: the light curve at 22.5 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f15a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f15b.eps} \end{figure}$

Figure 15: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000926. Upper panel: the light curve at 15 GHz. Lower panel: the light curve at 8.46 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f16a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f16b.eps} \end{figure}$

Figure 16: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000926. Upper panel: the light curve at 4.86 GHz. Lower panel: the light curve at 1.43 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f17a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f17b.eps} \end{figure}$

Figure 17: The spectrum of the AG of GRB 000926 from radio to optical frequencies. Upper panel: in the time interval between 0.8 and 1.4 days after burst. Lower panel: in the time interval between 1.4 and 2.5 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f18a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f18b.eps} \end{figure}$

Figure 18: The spectrum of the AG of GRB 000926 from radio to optical frequencies. Upper panel: in the time interval between 2.5 and 4 days after burst. Lower panel: in the time interval between 4 and 8 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f19a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f19b.eps} \end{figure}$

Figure 19: The spectrum of the AG of GRB 000926 from radio to optical frequencies. Upper panel: in the time interval between 8 and 20 days after burst. Lower panel: in the time interval between 20 and 100 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=8.8cm,clip]{MS2654f20.eps} \end{figure}$

Figure 20: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed optical afterglow of GRB 991216 at z=1.02. The figure shows (from top to bottom) 1000 times the K-band results, 100 times the J-band, 10 times the I-band, the R-band, 1/10 of the V-band, 1/100 of the B-band and 1/1000 of the U-band. The contributions of the underlying galaxy and the expected SN1998bw-like SN have been subtracted. In a CB-model fit, there is in this case some evidence for such a SN (DDD 2001).

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f21a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f21b.eps} \end{figure}$

Figure 21: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 991216. Upper panel: the light curve at 350 GHz. Lower panel: the light curve at 100 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f22a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f22b.eps} \end{figure}$

Figure 22: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 991216. Upper panel: the light curve at 15 GHz. Lower panel: the light curve at 8.46 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f23a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f23b.eps} \end{figure}$

Figure 23: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 991216. Upper panel: the light curve at 4.86 GHz. Lower panel: the light curve at 1.43 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f24a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f24b.eps} \end{figure}$

Figure 24: The spectrum of the AG of GRB 991216 from radio to optical frequencies. Upper panel: in the time interval between 0.44 and 2 days after burst. Lower panel: in the time interval between 2 and 4 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f25a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f25b.eps} \end{figure}$

Figure 25: The spectrum of the AG of GRB 991216 from radio to optical frequencies. Upper panel: in the time interval between 4 and 7 days after burst. Lower panel: in the time interval between 7 and 13 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f26a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f26b.eps} \end{figure}$

Figure 26: The spectrum of the AG of GRB 991216 from radio to optical frequencies. Upper panel: in the time interval between 13 and 30 days after burst. Lower panel: in the time interval between 30 and 80 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=8.8cm,clip]{MS2654f27.eps} \end{figure}$

Figure 27: Comparisons between our fitted CB model AG of GRB 991208, at z=0.706, Eq. (8), with the observed optical data. The figure shows (from top to bottom) 1000 times the K-band results, 100 times the J-band, 10 times the I-band, the R-band, 1/10 of the V-band, 1/100 of the B-band and 1/1000 of the U-band. The contribution of the underlying galaxy and associated supernova has been subtracted. The contributions of the underlying galaxy and the expected SN1998bw-like SN have been subtracted. In a CB-model fit, there is in this case strong evidence for such a SN (DDD 2001).

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f28a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f28b.eps} \end{figure}$

Figure 28: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 991208. Upper panel: the light curve at 100 GHz. Lower panel: the light curve at 86.2 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f29a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f29b.eps} \end{figure}$

Figure 29: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 991208. Upper panel: the light curve at 30 GHz. Lower panel: the light curve at 22.5 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f30a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f30b.eps} \end{figure}$

Figure 30: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 991208. Upper panel: the light curve at 15 GHz. Lower panel: the light curve at 8.46 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f31a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f31b.eps} \end{figure}$

Figure 31: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 991208. Upper panel: the light curve at 4.86 GHz. Lower panel: the light curve at 1.43 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f32a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f32b.eps} \end{figure}$

Figure 32: The spectrum of the AG of GRB 991208 from radio to optical frequencies. Upper panel: in the time interval between 2 and 5 days after burst. Lower panel: in the time interval between 5 and 10 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f33.eps} \end{figure}$

Figure 33: The spectrum of the AG of GRB 991208 from radio to optical frequencies in the time interval between 10 and 14.3 days. The highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=8.8cm,clip]{MS2654f34.eps}\par\end{figure}$

Figure 34: Comparisons between our fitted CB model AG of GRB 000418, at z=1.118, Eq. (8), with the observed optical data. The figure shows (from top to bottom) 1000 times the K-band results, 100 times the J-band, 10 times the I-band, the R-band, 1/10 of the V-band, 1/100 of the B-band and 1/1000 of the U-band. The contributions of the underlying galaxy and the expected SN1998bw-like SN have been subtracted. In a CB-model fit, there is in this case strong evidence for such a SN (DDD 2001).

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f35a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f35b.eps} \end{figure}$

Figure 35: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000418. Upper panel: the light curve at 22.46 GHz. Lower panel: the light curve at 15 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f36a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f36b.eps} \end{figure}$

Figure 36: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 000418. Upper panel: the light curve at 8.46 GHz. Lower panel: the light curve at 4.86 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f37a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f37b.eps} \end{figure}$

Figure 37: The spectrum of the AG of GRB 000418 from radio to optical frequencies. Upper panel: in the time interval between 9.5 and 30 days after burst. Lower panel: in the time interval between 30 and 100 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=8.8cm,clip]{MS2654f38.eps} \end{figure}$

Figure 38: Comparisons between our fitted CB model AG of GRB 990510, at z=1.619, Eq. (8), with the observed optical data. The figure shows (from top to bottom) 1000 times the K-band results, 100 times the J-band, 10 times the I-band, the R-band, 1/10 of the V-band, 1/100 of the B-band and 1/1000 of the U-band. The contribution of the underlying galaxy and the (in this case unobservable) associated supernova has been subtracted.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f39a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f39b.eps} \end{figure}$

Figure 39: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 990510. Upper panel: the light curve at 13.68 GHz. Lower panel: the light curve at 8.6-8.7 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f40a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f40b.eps} \end{figure}$

Figure 40: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 990510. Upper panel: the light curve at 4.86 GHz. Lower panel: the spectrum from radio to optical frequencies in the time interval between 1 and 6 days after burst. The highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f41a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f41b.eps} \end{figure}$

Figure 41: The spectrum of the AG of GRB 990510 from radio to optical frequencies. Upper panel: in the time interval between 6 and 20 days after burst. Lower panel: in the time interval between 20 and 40 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=8.8cm,clip]{MS2654f42.eps} \end{figure}$

Figure 42: Comparisons between our fitted CB model AG of GRB 990123, at z=1.600, Eq. (8), and the observed optical data. The figure shows (from top to bottom) 1000 times the K-band results, 100 times the J-band, 10 times the I-band, the R-band, 1/10 of the V-band, 1/100 of the B-band and 1/1000 of the U-band. The contributions of the underlying galaxy and an expected (but, in this case, unobservable) SN1998bw-like SN have been subtracted.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f43a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f43b.eps} \end{figure}$

Figure 43: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 990123. Upper panel: the light curve at 15 GHz. Lower panel: the light curve at 8.46 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f44a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f44b.eps} \end{figure}$

Figure 44: The spectrum of the AG of GRB 990123 from radio to optical frequencies. Upper panel: in the time interval between 0.1 and 1 day after burst. Lower panel: in the time interval between 1 and 3 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f45a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f45b.eps} \end{figure}$

Figure 45: The spectrum of the AG of GRB 990123 from radio to optical frequencies. Upper panel: in the time interval between 3 and 10 days after burst. Lower panel: in the time interval between 10 and 20 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f46.eps} \end{figure}$

Figure 46: Comparisons between our fitted CB model AG of GRB 970508, at z=0.835, Eq. (8), with the observed optical data. The figure shows (from top to bottom), 10 times the I-band, the R-band, 1/10 of the V-band and 1/100 of the B-band. The contributions of the underlying galaxy and the expected SN1998bw-like SN have been subtracted. In a CB-model fit, there is in this case strong evidence for such a SN (DDD 2001).

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f47a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f47b.eps} \end{figure}$

Figure 47: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 970508. Upper panel: the light curve at 8.46 GHz. Lower panel: the light curve at 4.86 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f48a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f48b.eps} \end{figure}$

Figure 48: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 970508. Upper panel: the light curve at 1.43 GHz. Lower panel: the spectral behaviour in the time interval between 0.12 and 6 days after burst. The highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f49a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f49b.eps} \end{figure}$

Figure 49: The spectrum of the AG of GRB 970508 from radio to optical frequencies. Upper panel: in the time interval between 6 and 20 days after burst. Lower panel: in the time interval between 20 and 40 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f50a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f50b.eps} \end{figure}$

Figure 50: The spectrum of the AG of GRB 970508 from radio to optical frequencies. Upper panel: in the time interval between 40 and 100 days after burst. Lower panel: in the time interval between 100 and 470 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f51a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f51b.eps} \end{figure}$

Figure 51: Comparisons between our fitted CB model afterglow of GRB 980425 at z=0.0085, Eq. (8), and its observed radio afterglow. Upper panel: the light curve at 8.64 GHz. Lower panel: the light curve at 4.80 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f52a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f52b.eps} \end{figure}$

Figure 52: Comparisons between our fitted CB model afterglow, Eq. (8), and the observed radio afterglow of GRB 980425. Upper panel: the light curve at 2.49 GHz. Lower panel: the light curve at 1.38 GHz.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f53a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f53b.eps} \end{figure}$

Figure 53: Comparison between the observed spectrum of the AG of GRB 980425 in the radio band and the fitted CB model spectrum. Upper panel: in the time interval between 2.5 and 20 days after burst. Lower panel: in the time interval between 20 and 40 days after burst. The highest peaking curve in the upper pannel corresponds to the later time and in the lower panel to the earlier time.

$\begin{figure} \includegraphics[width=7.2cm,clip]{MS2654f54a.eps}\vspace*{3mm} \includegraphics[width=7.2cm,clip]{MS2654f54b.eps} \end{figure}$

Figure 54: Comparison between the observed spectrum of the AG of GRB 980425 in the radio band and the fitted CB model spectrum. Upper panel: in the time interval between 40 and 70 days after burst. Lower panel: in the time interval between 70 and 150 days after burst. In both cases the highest peaking curve corresponds to the earlier time.

$\begin{figure} \includegraphics[width=8.8cm,clip]{MS2654f55.eps} \end{figure}$

Figure 55: The late spectrum of GRB 980425 in the time interval between 150 and 759 days after burst. The highest peaking line corresponds to the earlier time. The late isolated point is the last optical observation, which must correspond to SN1998bw and not to the AG of the CB of GRB 980425.

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