All Figures

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1677fig1.ps} \end{figure}$ Figure 1: The IGR J17091-3624 spectrum evolution in 2003-2004. Open circles represent RXTE data (Apr. 2003), crosses - INTEGRAL data (Aug.-Sep. 2003), dark circles - INTEGRAL data (Mar.-Apr. 2004). Corresponding best-fit approximations are shown by dash-dotted, solid and dashed lines, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1677fig2.ps} \end{figure}$ Figure 2: INTEGRAL/IBIS/ISGRI light curve of IGR/XTE J17391-3021 in the 18-60 keV energy band. Each point corresponds to a time bin of $\sim$ 3500 s (one pointing), error bars correspond to 1 $\sigma$ . A detailed profile of the strong outburst on 26-27 Aug., 2003 is shown in the inset.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{1677fig3.ps} \end{figure}$ Figure 3: The spectrum of IGR/XTE J17391-3021, measured with INTEGRAL (crosses) and its best-fit approximation (solid line). The best-fit approximation model of the source spectrum obtained with RXTE in 1998 is shown by a dashed line. We fixed its parameters to values obtained by Smith et al. (1998) and fitted only its normalization to the flux measured with INTEGRAL.
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1677fig4.ps} \end{figure}$ Figure 4: Light curves of IGR J17464-3213 obtained in August-September 2003 with INTEGRAL/IBIS in the 18-60 keV energy band ( upper panel) and RXTE/ASM in the 1.3-12.2 keV energy band ( bottom panel). Each point in INTEGRAL data corresponds to a time bin of $\sim$ 3500 s, in RXTE data - to the one-day averaging. Error bars corresponds to 1 $\sigma$ .
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In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1677fig5.ps} \end{figure}$ Figure 5: Broadband spectrum of IGR J17464-3213 obtained with INTEGRAL (crosses) and RXTE (dark circles) observatories. Best-fit approximation with the blackbody+powerlaw model is presented by solid line, contributions of each component are shown by dotted and dashed lines, respectively.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1677fig6.ps} \end{figure}$ Figure 6: IGR J17597-2201 spectrum changes observed by RXTE and INTEGRAL observatories in 2001 and 2003-2004, respectively. Crosses represent the high/soft state of the source, dark circles - low/hard state. Corresponding best-fit approximations are shown by dashed and solid lines, respectively. The contribution of the galactic ridge to RXTE/PCA spectra was subtracted.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1677fig7.ps} \end{figure}$ Figure 7: Spectra of IGR/SAX J18027-2017 measured with INTEGRAL in 2003 (crosses) and 2004 (filled circles, scaled by a factor of 0.3). Solid and dashed lines represent corresponding best-fit approximations. An extrapolation of the spectral model obtained by BeppoSAX to a wide energy band is shown by dotted line (see text for detail).
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1677fig1.ps} \end{figure}$	Figure 1: The IGR J17091-3624 spectrum evolution in 2003-2004. Open circles represent RXTE data (Apr. 2003), crosses - INTEGRAL data (Aug.-Sep. 2003), dark circles - INTEGRAL data (Mar.-Apr. 2004). Corresponding best-fit approximations are shown by dash-dotted, solid and dashed lines, respectively.
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$\begin{figure} \par\includegraphics[width=8.2cm,clip]{1677fig2.ps} \end{figure}$	Figure 2: INTEGRAL/IBIS/ISGRI light curve of IGR/XTE J17391-3021 in the 18-60 keV energy band. Each point corresponds to a time bin of $\sim$ 3500 s (one pointing), error bars correspond to 1 $\sigma$ . A detailed profile of the strong outburst on 26-27 Aug., 2003 is shown in the inset.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{1677fig3.ps} \end{figure}$	Figure 3: The spectrum of IGR/XTE J17391-3021, measured with INTEGRAL (crosses) and its best-fit approximation (solid line). The best-fit approximation model of the source spectrum obtained with RXTE in 1998 is shown by a dashed line. We fixed its parameters to values obtained by Smith et al. (1998) and fitted only its normalization to the flux measured with INTEGRAL.
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1677fig4.ps} \end{figure}$	Figure 4: Light curves of IGR J17464-3213 obtained in August-September 2003 with INTEGRAL/IBIS in the 18-60 keV energy band ( upper panel) and RXTE/ASM in the 1.3-12.2 keV energy band ( bottom panel). Each point in INTEGRAL data corresponds to a time bin of $\sim$ 3500 s, in RXTE data - to the one-day averaging. Error bars corresponds to 1 $\sigma$ .
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$\begin{figure} \par\includegraphics[width=7.5cm,clip]{1677fig5.ps} \end{figure}$	Figure 5: Broadband spectrum of IGR J17464-3213 obtained with INTEGRAL (crosses) and RXTE (dark circles) observatories. Best-fit approximation with the blackbody+powerlaw model is presented by solid line, contributions of each component are shown by dotted and dashed lines, respectively.
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$\begin{figure} \par\includegraphics[width=7.7cm,clip]{1677fig6.ps} \end{figure}$	Figure 6: IGR J17597-2201 spectrum changes observed by RXTE and INTEGRAL observatories in 2001 and 2003-2004, respectively. Crosses represent the high/soft state of the source, dark circles - low/hard state. Corresponding best-fit approximations are shown by dashed and solid lines, respectively. The contribution of the galactic ridge to RXTE/PCA spectra was subtracted.
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$\begin{figure} \par\includegraphics[width=7.6cm,clip]{1677fig7.ps} \end{figure}$	Figure 7: Spectra of IGR/SAX J18027-2017 measured with INTEGRAL in 2003 (crosses) and 2004 (filled circles, scaled by a factor of 0.3). Solid and dashed lines represent corresponding best-fit approximations. An extrapolation of the spectral model obtained by BeppoSAX to a wide energy band is shown by dotted line (see text for detail).
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