All Figures

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0147fig1.eps} \end{figure}$ Figure 1: IRS 13 field from the Gemini AO image in the Kp band. IRS 13E is the central, compact group of stars and IRS 13W the brightest source $\sim$ 1 $^{\prime \prime }$ southwest of IRS 13E. The coordinates are in arcsec offset from SgrA $^{\star }$ .
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0147fig2.eps} \end{figure}$ Figure 2: The Fig. 1 field with the star detected after deconvolution by the MCS code (Sect. 2.3). The vector associated with most of the stars represents in amplitude the velocity and the direction of proper motions measured from SHARP data by Ott et al. (2003). For E3A and E3B, only the proper motion of the center of light is determined. The amplitudes reported in Table 6 for the four brightest sources of IRS 13E give the scale of the proper motion vectors. The cross marked X represents the nominal position of the X-ray source at the center of an error box of $\pm$ 0.3 $^{\prime \prime }$ (see Sect. 3.2).
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0147fig3.eps} \end{figure}$ Figure 3: At left, NICMOS images of IRS 13E in the Pa $\alpha$ filter (1.87 $\mu$ m), and at right, difference between this image and the suitably scaled image in the continuum at 1.90 $\mu$ m. Only IRS 13E2 and IRS 13E4 remain which appear as emission line stars.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0147fig4.eps} \end{figure}$ Figure 4: He I 2.06 $\mu$ m and Br $\gamma$ emission line profiles at IRS 13E normalized to 1, from the BEAR data, after subtraction of the interstellar emission (ISM) contribution the observed profiles. The difference of linewidth is noticeable. The multi-component ISM emission, extracted from a ring around IRS 13E in the Br $\gamma$ data cube, is shown in the middle panel. Since He I 2.06 $\mu$ m is coming only from 13E2 (Clénet et al. 2003) the broad profile adjusted on the wings of the Br $\gamma$ profile, of same width as the He I profile, shows the relative intensity of Br $\gamma$ from 13E2 compared to 13E4.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0147fig5.eps} \end{figure}$ Figure 5: Dereddened SED of the IRS 13 sources in W cm^-2 $\mu$ m^-1. The top of the arrows indicates the estimated upper limit of the detectable flux in the 1.1 $\mu$ m and the L-band filters. The various lines represent the best fit between 1 and 4 $\mu$ m of the data points from a two-component model with the parameters of Table 7 and the most adapted $A_{\rm v}$ values.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{0147fig6.eps} \end{figure}$ Figure 6: Map of the residual fitted continuum in the deconvolution operation of the L-band image with the MCS code. The identified stars in this band (Table 2) have been subtracted explaining the dark holes in the map (e.g. at the W position). Source positions are marked by crosses with their names. To limit confusion, for the E3 binary only E3B position is indicated. The apparent halo might be not purely thermal emission of dust and contain more fainter embedded sources (Eckart et al. 2003). An estimation of the halo contrast is given for the brightest pixel (position -3.1 $^{\prime \prime }$ , -0.8 $^{\prime \prime }$ ), which is four times brighter than east of 13E, out of the halo.
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In the text

$\begin{figure} \par\includegraphics[width=8.7cm,clip]{0147fig1.eps} \end{figure}$	Figure 1: IRS 13 field from the Gemini AO image in the Kp band. IRS 13E is the central, compact group of stars and IRS 13W the brightest source $\sim$ 1 $^{\prime \prime }$ southwest of IRS 13E. The coordinates are in arcsec offset from SgrA $^{\star }$ .
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{0147fig3.eps} \end{figure}$	Figure 3: At left, NICMOS images of IRS 13E in the Pa $\alpha$ filter (1.87 $\mu$ m), and at right, difference between this image and the suitably scaled image in the continuum at 1.90 $\mu$ m. Only IRS 13E2 and IRS 13E4 remain which appear as emission line stars.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{0147fig5.eps} \end{figure}$	Figure 5: Dereddened SED of the IRS 13 sources in W cm^-2 $\mu$ m^-1. The top of the arrows indicates the estimated upper limit of the detectable flux in the 1.1 $\mu$ m and the L-band filters. The various lines represent the best fit between 1 and 4 $\mu$ m of the data points from a two-component model with the parameters of Table 7 and the most adapted $A_{\rm v}$ values.
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