All Figures

$\begin{figure} \par\includegraphics[width=17cm,clip]{1231f1.eps} \end{figure}$ Figure 1: RXTE/PCA light curve (PCUs 0 and 2, top panel), hardness ratio ((7-15 keV)/(2-7 keV), middle panel) and total rms (0.03-64 Hz, bottom panel) of XTE J1859+226 during its 1999 outburst. The time resolution for the light- and hardness curves is 16 s except for the last five points, which have one point for each observation.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1231f2.ps} \end{figure}$ Figure 2: Examples of type A, B and C QPOs from our XTE J1859+226 observations. QPO and harmonics peaks are indicated. Upper panel: Obs. 40124-01-12-00. Middle panel: Obs. 40122-01-01-03. Bottom panel: Obs. 40124-01-10-00). The Poisson noise was not subtracted.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1231f3.ps} \end{figure}$ Figure 3: Centroid QPO frequency vs. 0.03-64 Hz fractional rms of the detected QPOs. Each point corresponds to a different observation, except for the few cases in which transitions between different pds shapes have been observed. Error bars are smaller than symbols.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1231f4.ps} \end{figure}$ Figure 4: Same as Fig. 1, but for only the first 25 days of the outburst. See inset for the symbols that are used to represent different QPO types in the lower panel - dots are used if no QPO was detected.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1231f5.ps} \end{figure}$ Figure 5: An example of type-C power spectrum (2-15 keV; Obs.: 40124-01-10-00). The solid line shows the best fit with five Lorentzians (dotted lines). See the correspondent lags in Fig. 6, fourth panel.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1231f6.ps} \end{figure}$ Figure 6: Type-C phase lags vs. frequency for four different QPO frequencies. Bottom panel: an example of type-C^* phase lags. Positive values indicate that the hard (5-13 keV) photons are lagging the soft (2-5 keV) photons. QPO centroid frequency and observation I.D. are indicated for each panel. The dashed lines mark the frequency of the QPO, while the dotted lines mark the subharmonic (if present) and second harmonic frequencies.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f7.ps} \end{figure}$ Figure 7: An example of type C^* PDS (2-15 keV) and phase lags (Obs.: 40124-01-28-00). The dotted vertical line marks the frequency of the QPO.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f8.ps} \end{figure}$ Figure 8: An example of type-A PDS (2-15 keV) and phase lags (Obs.: 40124-01-12-00). The dotted vertical line marks the frequency of the QPO. Lags at frequencies above $\sim$ 10 Hz are, given the lack of statistics, random scattering between $-\pi$ and $\pi$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f9.ps} \end{figure}$ Figure 9: An example of type-B PDS (2-15 keV) and phase lags (Obs.: 40122-01-01-03). The dashed vertical line marks the frequency of the QPO, while the dotted lines mark the subharmonic and second harmonic frequencies.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f10.ps} \end{figure}$ Figure 10: An example of type B-"Cathedral'' PDS (2-15 keV) and phase lags (Obs.: 40124-01-24-00). The dotted vertical line marks the frequency of the QPO.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f11.ps} \end{figure}$ Figure 11: Coherence of the subharmonic peak for different pds types.
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In the text

$\begin{figure} \par\includegraphics[width=17.0cm,clip]{1231f12.ps} \end{figure}$ Figure 12: Three examples of unclassified power spectra (2-15keV) with their phase lags.
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In the text

$\begin{figure} \par\includegraphics[width=16.5cm,clip]{1231f13.eps} \end{figure}$ Figure 13: Light curves and dynamical PDS for observations 40124-01-13-00 (panel a), all five PCUs on), 40124-01-14-00 (panel b), five PCUs on), 40122-01-01-00 (panel c), three PCUs on) and 40124-01-24-00 (panel d), three PCUs on). The lower power value of the type-A QPO peaks with respect to the type-B render them invisible in the dynamical power spectra of panels a) and c). However, these are clearly seen in the total average PDS.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1231f14.ps} \end{figure}$ Figure 14: Light curve of the observations showing transitions between two different QPO types. The two parallel lines have been drawn so as to intersect the transition points. In the inset the lines have been extended to the part of the outburst where QPOs appear. Different grayscales indicate different QPO types. (A color image is available on line) Black points correspond to data in which no QPOs were found.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f15.eps} \end{figure}$ Figure 15: Light curve and color-color diagram for observation 40124-01-38-01. Only three PCUs were on (MJD: 51 485.075).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f16.ps} \end{figure}$ Figure 16: Fractional rms amplitude of the fundamental QPO peak as a function of energy for QPO types A (stars, obs: 40124-01-12-00), B (40122-01-01-03) and C (40124-01-21-00).
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f17.ps} \end{figure}$ Figure 17: Total fractional rms (0.03-64 Hz) vs. time-lags of the fundamental QPO peak.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{1231f18.eps} \end{figure}$ Figure 18: Time-lags of the fundamental QPO peak vs. time-lags of its second harmonic ( left panel) and subharmonic ( right panel).
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{1231f19.ps} \end{figure}$ Figure 19: Left panel: Hardness-Intensity diagram (see Fig. 1 for variables definition). The time resolution is 16 s except for the first and the last eight observations, which have one point for each observation in order to improve the statistics. Different grayscales indicate different QPO types. (A color image is available on line) Right panel: enlargement of the region of the diagram where most of type A-B-C QPOs appear.
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In the text

$\begin{figure} \par\includegraphics[width=17cm,clip]{1231f1.eps} \end{figure}$	Figure 1: RXTE/PCA light curve (PCUs 0 and 2, top panel), hardness ratio ((7-15 keV)/(2-7 keV), middle panel) and total rms (0.03-64 Hz, bottom panel) of XTE J1859+226 during its 1999 outburst. The time resolution for the light- and hardness curves is 16 s except for the last five points, which have one point for each observation.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1231f2.ps} \end{figure}$	Figure 2: Examples of type A, B and C QPOs from our XTE J1859+226 observations. QPO and harmonics peaks are indicated. Upper panel: Obs. 40124-01-12-00. Middle panel: Obs. 40122-01-01-03. Bottom panel: Obs. 40124-01-10-00). The Poisson noise was not subtracted.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1231f3.ps} \end{figure}$	Figure 3: Centroid QPO frequency vs. 0.03-64 Hz fractional rms of the detected QPOs. Each point corresponds to a different observation, except for the few cases in which transitions between different pds shapes have been observed. Error bars are smaller than symbols.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1231f4.ps} \end{figure}$	Figure 4: Same as Fig. 1, but for only the first 25 days of the outburst. See inset for the symbols that are used to represent different QPO types in the lower panel - dots are used if no QPO was detected.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1231f5.ps} \end{figure}$	Figure 5: An example of type-C power spectrum (2-15 keV; Obs.: 40124-01-10-00). The solid line shows the best fit with five Lorentzians (dotted lines). See the correspondent lags in Fig. 6, fourth panel.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f7.ps} \end{figure}$	Figure 7: An example of type C^* PDS (2-15 keV) and phase lags (Obs.: 40124-01-28-00). The dotted vertical line marks the frequency of the QPO.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f8.ps} \end{figure}$	Figure 8: An example of type-A PDS (2-15 keV) and phase lags (Obs.: 40124-01-12-00). The dotted vertical line marks the frequency of the QPO. Lags at frequencies above $\sim$ 10 Hz are, given the lack of statistics, random scattering between $-\pi$ and $\pi$ .
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f9.ps} \end{figure}$	Figure 9: An example of type-B PDS (2-15 keV) and phase lags (Obs.: 40122-01-01-03). The dashed vertical line marks the frequency of the QPO, while the dotted lines mark the subharmonic and second harmonic frequencies.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f10.ps} \end{figure}$	Figure 10: An example of type B-"Cathedral'' PDS (2-15 keV) and phase lags (Obs.: 40124-01-24-00). The dotted vertical line marks the frequency of the QPO.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f11.ps} \end{figure}$	Figure 11: Coherence of the subharmonic peak for different pds types.
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$\begin{figure} \par\includegraphics[width=17.0cm,clip]{1231f12.ps} \end{figure}$	Figure 12: Three examples of unclassified power spectra (2-15keV) with their phase lags.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f15.eps} \end{figure}$	Figure 15: Light curve and color-color diagram for observation 40124-01-38-01. Only three PCUs were on (MJD: 51 485.075).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f16.ps} \end{figure}$	Figure 16: Fractional rms amplitude of the fundamental QPO peak as a function of energy for QPO types A (stars, obs: 40124-01-12-00), B (40122-01-01-03) and C (40124-01-21-00).
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1231f17.ps} \end{figure}$	Figure 17: Total fractional rms (0.03-64 Hz) vs. time-lags of the fundamental QPO peak.
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$\begin{figure} \par\includegraphics[width=16cm,clip]{1231f18.eps} \end{figure}$	Figure 18: Time-lags of the fundamental QPO peak vs. time-lags of its second harmonic ( left panel) and subharmonic ( right panel).
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