All Figures

$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip,origin=rb]{7365fig1.ps}\end{figure}$ Figure 1: ROTSEIIId differential light curve of the Be/X-ray binary system ( top panel a)) and mean light curve of reference stars properly offsetted ( top panel b)) for the period 2005-2006. The X-ray light curve of the system obtained from RXTE/ASM data is given in the bottom panel for the same time interval as ROTSEIIId observations.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip,origin=rb]{7365fig2.ps} \end{figure}$ Figure 2: Power spectra for the optical counterpart to CXOU J205847.5+414637. Panel a) Lomb-Scargle algorithm; b) Clean algorithm. Frequencies 2.404 and 2.371 d^-1 are shown in the inset of the middle panel for clarity. The lower panel c) is the power spectrum of reference stars used in this study.
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In the text

$\begin{figure} \par\includegraphics[width=7cm,clip]{7365fig3.ps} \end{figure}$ Figure 3: Upper panel: the binned LS periodogram of counterpart to ROTSEIIId data of CXOU J205847.5+414637. A red noise component of a very low power index is seen in the 1-8 d^-1 portion of the spectra. The dashed line represents the model continuum spectra as explained in the text. b) Below is the same power spectra normalized to the model continuum and multiplied by 2 to represent a Poisson distribution for 2 degrees of freedom. $3\sigma$ and $5\sigma$ confidence levels for the modified white noise model are denoted by dashed lines.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.2cm,clip]{7365fig4.ps} \end{figure}$ Figure 4: The phase diagrams of 0.416 d and 0.422 d periodic variability for the differential light curve shown in Fig. 1.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.55cm,clip]{7365fig5.ps} \end{figure}$ Figure 5: The phase diagrams of 0.416 d and 0.422 d periodic variabilities for the time intervals as mentioned in the text, starting from MJD 53499 a) to MJD 53982 d).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=7.4cm,clip]{7365fig6.ps} \end{figure}$ Figure 6: Epoch-folded orbital phase of the Be/X-ray binary system CXOU J205847.5+414637 for RXTE/ASM and ROTSEIIId data (using the ephemeris T = MJD 50411.3+55.03N given by Wilson et al. 2005).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=14.2cm,clip]{7365fig7.ps} \end{figure}$ Figure 7: Broadband (4500-7500 Å) ( top) (with grism 15: resolution $\sim$ 9.1 Å) and moderate resolution ( bottom) (with grism 8, resolution $\sim$ 3.4 Å) spectra of the counterpart to CXOU J205847.5+414637 taken in July 2006.
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In the text

$\begin{figure} \par\includegraphics[width=5.2cm,clip]{7365fig8.ps} \end{figure}$ Figure 8: Series of H $\alpha$ profiles observed May-September 2006. Note low S/N for May and June data. The spectra correspond to the orbital phases of ( top to bottom) 0.01, 0.45, 0.23, 0.61, and 0.30 which, are obtained using the ephemeris T = MJD 50411.3 + 55.03N given by Wilson et al. (2005).
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=13.8cm,clip]{7365fig9.ps} \end{figure}$ Figure 9: Mid band ( top) and blue ( bottom) spectra for the optical counterpart to CXOU J205847.5+414637 taken on July 29 with grism 7 and on September 26 with grism 14. Both spectra have been normalized with a spline fit to continuum and smoothed with a median filter for display. Several strong lines from the Balmer series are indicated by short vertical bars. He I lines are shown by down arrows. Various other lines and DIBs are also indicated. "*'' denotes the region affected by a cosmic ray hit.
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In the text

$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip,origin=rb]{7365fig1.ps}\end{figure}$	Figure 1: ROTSEIIId differential light curve of the Be/X-ray binary system ( top panel a)) and mean light curve of reference stars properly offsetted ( top panel b)) for the period 2005-2006. The X-ray light curve of the system obtained from RXTE/ASM data is given in the bottom panel for the same time interval as ROTSEIIId observations.
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$\begin{figure} \par\includegraphics[angle=270,width=12cm,clip,origin=rb]{7365fig2.ps} \end{figure}$	Figure 2: Power spectra for the optical counterpart to CXOU J205847.5+414637. Panel a) Lomb-Scargle algorithm; b) Clean algorithm. Frequencies 2.404 and 2.371 d^-1 are shown in the inset of the middle panel for clarity. The lower panel c) is the power spectrum of reference stars used in this study.
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$\begin{figure} \par\includegraphics[angle=270,width=7.2cm,clip]{7365fig4.ps} \end{figure}$	Figure 4: The phase diagrams of 0.416 d and 0.422 d periodic variability for the differential light curve shown in Fig. 1.
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$\begin{figure} \par\includegraphics[angle=270,width=7.55cm,clip]{7365fig5.ps} \end{figure}$	Figure 5: The phase diagrams of 0.416 d and 0.422 d periodic variabilities for the time intervals as mentioned in the text, starting from MJD 53499 a) to MJD 53982 d).
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$\begin{figure} \par\includegraphics[angle=270,width=7.4cm,clip]{7365fig6.ps} \end{figure}$	Figure 6: Epoch-folded orbital phase of the Be/X-ray binary system CXOU J205847.5+414637 for RXTE/ASM and ROTSEIIId data (using the ephemeris T = MJD 50411.3+55.03N given by Wilson et al. 2005).
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$\begin{figure} \par\includegraphics[angle=270,width=14.2cm,clip]{7365fig7.ps} \end{figure}$	Figure 7: Broadband (4500-7500 Å) ( top) (with grism 15: resolution $\sim$ 9.1 Å) and moderate resolution ( bottom) (with grism 8, resolution $\sim$ 3.4 Å) spectra of the counterpart to CXOU J205847.5+414637 taken in July 2006.
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$\begin{figure} \par\includegraphics[width=5.2cm,clip]{7365fig8.ps} \end{figure}$	Figure 8: Series of H $\alpha$ profiles observed May-September 2006. Note low S/N for May and June data. The spectra correspond to the orbital phases of ( top to bottom) 0.01, 0.45, 0.23, 0.61, and 0.30 which, are obtained using the ephemeris T = MJD 50411.3 + 55.03N given by Wilson et al. (2005).
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