All Figures

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms2663_f1.ps}\par\vspace*{2mm} \includegraphics[width=8.6cm,clip]{ms2663_f2.ps} \end{figure}$ Figure 1: The one day average light curves of X1543-624 and X1556-605 detected with the RXTE ASM in the 1.5-12 keV energy band. The arrows mark the epoch of the BeppoSAX observations of each source. ASM data can be retrieved on the public archive at http://xte.mit.edu/XTE/asmlc/ASM.html
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=-90,width=14.2cm,clip]{ms2663_f3.ps}\v... ...{3.5mm} \includegraphics[angle=-90,width=14.2cm,clip]{ms2663_f4.ps} \end{figure}$ Figure 2: Upper panels: 2-10 keV MECS light curves of the two BeppoSAX observations of X1543-624. Bottom panels: 2-10 keV MECS light curves of X1556-605. Times are expressed in UT of the day reported in each panel. The time binning is 200 s.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=5.5cm,width=5.7cm,clip]{ms2663_f5.ps}... ...3mm} \includegraphics[height=5.5cm,width=5.7cm,clip]{ms2663_f6.ps} \end{figure}$ Figure 3: Colour-colour diagrams of both observations of X1543-624 ( left panel) and X1556-605 ( right panel). The y axis ( hard colour) gives the ratio between the 6.5-10 keV and 5-6.5 keV count rates. The x axis ( soft colour) gives the count rate ratio in the 3-5 keV and 1.8-3 keV energy bands. In both diagrams each point corresponds to a time interval of 200 s. Typical error bars of the two colours are reported in the top right of each panel. Diamonds: first observation; squares: second observation.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.3cm,clip]{ms2663_f7.eps}\hspace*{2mm} \includegraphics[angle=0,width=8.3cm,clip]{ms2663_f8.eps} \end{figure}$ Figure 4: Count rate spectra of the two observations of X1543-624 along with the folded model BB plus DBB, photoelectrically-absorbed ( WABS) and residuals to the model in units of $\sigma$ . Left panel: first observation. Right panel: second observation. The excess above 15 keV can be recovered replacing the BB with a Comptonized BB (see text).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.3cm,clip]{ms2663_f9.eps}\hspace*{2mm} \includegraphics[angle=0,width=8.3cm,clip]{ms2663_f10.eps} \end{figure}$ Figure 5: Count rate spectra of the two observations of X1543-624 along with the folded model DBB plus COMPBB, photoelectrically-absorbed ( WABS) and residuals to the model in units of $\sigma$ . Left panel: first observation. Right panel: second observation.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[angle=0,width=8.8cm,clip]{ms2663_f11.eps} \end{figure}$ Figure 6: Top panel: average count rate spectrum of the two observations of X1556-605 and best fit folded model consisting of a BB plus a DBB photoelectrically-absorbed ( WABS). Bottom panel: residuals to the model in units of $\sigma$ . The excess above 15 keV can be recovered either replacing the BB with a Comptonized BB or replacing the DBB with an USC model (see text).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=7.1cm,width=6cm,clip]{ms2663_f12.ps}\... ...*{4mm} \includegraphics[height=7.1cm,width=6cm,clip]{ms2663_f13.ps} \end{figure}$ Figure 7: Absorption-corrected, EF(E) spectra for the first ( left panel) and second ( right panel) observation of X1543-624 with superimposed the best fit model composed by a DBB ( dotted line) plus COMPBB ( dashed line) plus a Gaussian ( dotted-dashed line) at 6.4 keV (see text). Bottom panels: residuals, in units of $\sigma$ , to the best fit model photoelectrically-absorbed with non-standard values of O and Ne ( VPHABS).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=7.1cm,width=6cm,clip]{ms2663_f14.ps}\... ...e*{4mm} \includegraphics[height=7.1cm,width=6cm,clip]{ms2663_f15.ps}\end{figure}$ Figure 8: Same as in Fig. 7 but for the time averaged spectrum of X1556-605. Left panel: DBB ( dotted line) plus COMPBB ( dashed line). Right panel: BB ( dotted line) plus USC ( dashed line). Bottom panels: residuals, in units of $\sigma$ , to the best fit models, photoelectrically-absorbed ( WABS).
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[height=9.1cm,width=9.5cm,clip]{ms2663_f16.ps}\end{figure}$ Figure 9: The hard (20-200 keV) X-ray luminosity versus the soft (1-20 keV) luminosity for weakly magnetic compact X-ray binaries. Open squares: X-ray bursters detected up to 100 keV and listed in the analoguous figure by B2000; open diamonds: Z sources; crosses: black holes candidates. The "X-ray burster box'' introduced by B2000 is also shown. BHCs are mostly located on the right, but one of them (XTE J1118+480) is inside the X-ray burster box. The position of our two sources ( filled squares) within the X-ray burster box is shown. The points ( a) and ( b) for Sco X-1 denote the minimum and maximum fluxes observed by D'Amico et al. (2001) during their detection of a hard tail; the points ( a) and ( b) for Cyg X-2 denote the cases in which the the hard X-ray tail was detected and not detected, respectively (Di Salvo et al. 2002). The points ( a) and ( b) for Cyg X-1 denote the low/hard state and the high/soft state, respectively. The numbers from 1 to 16 denote the X-ray bursters listed by B2000, while 17 and 18 denote two additional atoll sources included in the figure; 1: Aql X-1; 2: SLX1732-304; 3: 4U0614+09; 4: XB1323-619; 5: SAXJ1808.4-3658; 6: 4U1915-05; 7: SLX1735-269; 8: A1742-294; 9: 4U1608-52; 10: SAXJ1748.9-2021; 11: 1E1724-3045; 12: GS1826-238; 13: KS1731-260; 14: GX354-0; 15: Cen X-4; 16: 4U1705-44; 17: 4U1728-34 Di Salvo et al. 2000b; 18: 4U1820-30 Bloser et al. 2000.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=8.6cm,clip]{ms2663_f1.ps}\par\vspace*{2mm} \includegraphics[width=8.6cm,clip]{ms2663_f2.ps} \end{figure}$	Figure 1: The one day average light curves of X1543-624 and X1556-605 detected with the RXTE ASM in the 1.5-12 keV energy band. The arrows mark the epoch of the BeppoSAX observations of each source. ASM data can be retrieved on the public archive at http://xte.mit.edu/XTE/asmlc/ASM.html
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=-90,width=14.2cm,clip]{ms2663_f3.ps}\v... ...{3.5mm} \includegraphics[angle=-90,width=14.2cm,clip]{ms2663_f4.ps} \end{figure}$	Figure 2: Upper panels: 2-10 keV MECS light curves of the two BeppoSAX observations of X1543-624. Bottom panels: 2-10 keV MECS light curves of X1556-605. Times are expressed in UT of the day reported in each panel. The time binning is 200 s.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=0,width=8.3cm,clip]{ms2663_f7.eps}\hspace*{2mm} \includegraphics[angle=0,width=8.3cm,clip]{ms2663_f8.eps} \end{figure}$	Figure 4: Count rate spectra of the two observations of X1543-624 along with the folded model BB plus DBB, photoelectrically-absorbed ( WABS) and residuals to the model in units of $\sigma$ . Left panel: first observation. Right panel: second observation. The excess above 15 keV can be recovered replacing the BB with a Comptonized BB (see text).
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=0,width=8.3cm,clip]{ms2663_f9.eps}\hspace*{2mm} \includegraphics[angle=0,width=8.3cm,clip]{ms2663_f10.eps} \end{figure}$	Figure 5: Count rate spectra of the two observations of X1543-624 along with the folded model DBB plus COMPBB, photoelectrically-absorbed ( WABS) and residuals to the model in units of $\sigma$ . Left panel: first observation. Right panel: second observation.
Open with DEXTER

$\begin{figure} \par\includegraphics[angle=0,width=8.8cm,clip]{ms2663_f11.eps} \end{figure}$	Figure 6: Top panel: average count rate spectrum of the two observations of X1556-605 and best fit folded model consisting of a BB plus a DBB photoelectrically-absorbed ( WABS). Bottom panel: residuals to the model in units of $\sigma$ . The excess above 15 keV can be recovered either replacing the BB with a Comptonized BB or replacing the DBB with an USC model (see text).
Open with DEXTER

$\begin{figure} \par\includegraphics[height=7.1cm,width=6cm,clip]{ms2663_f14.ps}\... ...e*{4mm} \includegraphics[height=7.1cm,width=6cm,clip]{ms2663_f15.ps}\end{figure}$	Figure 8: Same as in Fig. 7 but for the time averaged spectrum of X1556-605. Left panel: DBB ( dotted line) plus COMPBB ( dashed line). Right panel: BB ( dotted line) plus USC ( dashed line). Bottom panels: residuals, in units of $\sigma$ , to the best fit models, photoelectrically-absorbed ( WABS).
Open with DEXTER