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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{4826fig1.ps} \end{figure}$ Figure 1: VLA map at the 6 cm wavelength of the originally proposed HSCN as observed on 2005 April 16. The object is detected as a clearly compact source. Contours are -3, 3, 5, 8, 12, 20, 30, 40 and 50 times 0.035 mJy beam^-1, the rms noise. The ellipse shown at the bottom left is the synthesized beam equivalent to 1 ${\rlap.}^{\prime \prime}$ $48\times 1$ ${\rlap.}^{\prime \prime}$ 38, with a position angle of -38 $.\!\!^\circ$ 2.
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In the text

$\begin{figure} \par\includegraphics[width=16.4cm,clip]{4826fig2.eps} \end{figure}$ Figure 2: The two fields of the previously proposed HSCs of Cygnus X-3 as seen with the CAHA 3.5 m telescope plus the OMEGA2000 camera in the $K_{\rm s}$ -band. The crosses indicate the position of both the HSCN and HSCS in the left and right panel, respectively. No near infrared counterpart is detected for the northern object but a weak source is consistent with the southern one well within the astrometric error.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4826fig3.eps} \end{figure}$ Figure 3: CAHA 3.5 m $K_{\rm s}$ -band image of Cygnus X-3 taken on 2005 April 29 with OMEGA2000. The well known near infrared counterpart of this microquasar is located at the center of the frame and indicated with a circle.
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In the text

$\begin{figure} \par\includegraphics[width=16.7cm,clip]{4826fig4.eps} \end{figure}$ Figure 4: Left. CAHA 3.5 m image of Cygnus X-3 taken on 2005 April 29 with OMEGA2000 in the H₂ filter. Right. The same field after subtraction of the continuum to better search for evidence of extended line emission. None was detected within the sensitivity of our observations as it also occured with our Br $\gamma$ narrow filter observations.
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In the text

$\begin{figure} \par\includegraphics[width=7.6cm,clip]{4826fig3.eps} \end{figure}$	Figure 3: CAHA 3.5 m $K_{\rm s}$ -band image of Cygnus X-3 taken on 2005 April 29 with OMEGA2000. The well known near infrared counterpart of this microquasar is located at the center of the frame and indicated with a circle.
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$\begin{figure} \par\includegraphics[width=16.7cm,clip]{4826fig4.eps} \end{figure}$	Figure 4: Left. CAHA 3.5 m image of Cygnus X-3 taken on 2005 April 29 with OMEGA2000 in the H₂ filter. Right. The same field after subtraction of the continuum to better search for evidence of extended line emission. None was detected within the sensitivity of our observations as it also occured with our Br $\gamma$ narrow filter observations.
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