All Figures

$\begin{figure} \par\includegraphics[width=18cm,clip]{1562fig1.eps} \end{figure}$ Figure 1: Light-curves of six of the studied pulses; a) GRB 911031 (# 973a); b) GRB 911031 (# 973b); c) GRB 941026 (# 3257); d) GRB 960524 (# 3648); e) GRB 951102 (# 3891); f) GRB 980125 (# 6581). The black curves are for BATSE channel 3 and the grey curves for channel 1. The smooth line is the best fit model (Eq. (1)).
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In the text

$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1562fig2.eps} \end{figure}$ Figure 2: Peak photon flux as a function of spectral lag. The best fit is marked by the solid line and approximately corresponds to an inverse relation between flux and lag.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1562fig3.eps} \end{figure}$ Figure 3: Analytic spectral lag, $\Delta t$ , versus the CCF lag CCF13. A good linear correspondence exists, as expected.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{1562fig4.eps} \end{figure}$ Figure 4: CGRO-BATSE data analyzed using high resolution spectroscopy, HRS. a) Low-energy power-law index, $\alpha$ , versus spectral lag. b) HIC power-law index $\eta$ , versus $\alpha$ . c) $\alpha$ versus lag. d) Initial (maximal) peak-energy, $E_{\rm0}$ , versus lag.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{1562fig5.eps} \end{figure}$ Figure 5: Hardness ratio (HR31) as a function of $E_{\rm0}$ , $\alpha$ , and $\eta$ . Only weak correlations emerge, as expected.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1562fig6.eps} \end{figure}$ Figure 6: Dependence of spectral lag on $\Phi _0/F_{\rm tot}$ . The outlier point is from the second pulse in trigger 973.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1562fig7.eps} \end{figure}$ Figure 7: Sky distribution in super-galactic coordinates for the 15 BATSE bursts in the studied sample. These are characterized by having long uncontaminated FRED pulse(s). The dipole moment of the distribution is very large.
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In the text

$\begin{figure} \par\includegraphics[width=18cm,clip]{1562fig1.eps} \end{figure}$	Figure 1: Light-curves of six of the studied pulses; a) GRB 911031 (# 973a); b) GRB 911031 (# 973b); c) GRB 941026 (# 3257); d) GRB 960524 (# 3648); e) GRB 951102 (# 3891); f) GRB 980125 (# 6581). The black curves are for BATSE channel 3 and the grey curves for channel 1. The smooth line is the best fit model (Eq. (1)).
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$\begin{figure} \par\includegraphics[width=7.9cm,clip]{1562fig2.eps} \end{figure}$	Figure 2: Peak photon flux as a function of spectral lag. The best fit is marked by the solid line and approximately corresponds to an inverse relation between flux and lag.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1562fig3.eps} \end{figure}$	Figure 3: Analytic spectral lag, $\Delta t$ , versus the CCF lag CCF13. A good linear correspondence exists, as expected.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{1562fig4.eps} \end{figure}$	Figure 4: CGRO-BATSE data analyzed using high resolution spectroscopy, HRS. a) Low-energy power-law index, $\alpha$ , versus spectral lag. b) HIC power-law index $\eta$ , versus $\alpha$ . c) $\alpha$ versus lag. d) Initial (maximal) peak-energy, $E_{\rm0}$ , versus lag.
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$\begin{figure} \par\includegraphics[width=18cm,clip]{1562fig5.eps} \end{figure}$	Figure 5: Hardness ratio (HR31) as a function of $E_{\rm0}$ , $\alpha$ , and $\eta$ . Only weak correlations emerge, as expected.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1562fig6.eps} \end{figure}$	Figure 6: Dependence of spectral lag on $\Phi _0/F_{\rm tot}$ . The outlier point is from the second pulse in trigger 973.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{1562fig7.eps} \end{figure}$	Figure 7: Sky distribution in super-galactic coordinates for the 15 BATSE bursts in the studied sample. These are characterized by having long uncontaminated FRED pulse(s). The dipole moment of the distribution is very large.
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