All Figures

$\begin{figure} {\psfig{figure=Ga201_f1.eps,width=8.8cm,clip=} }\end{figure}$ Figure 1: Composite JHKs ISAAC image showing: a) The core of the lensing cluster A1835, with the position of the long slit used during our spectroscopic survey with ISAAC/VLT, together with the location of objects #1916 and #2582, the reference acquisition star (circles), and a nearby field galaxy seen on the 2D spectra. Large and small dots show the position of the external and internal critical lines at z=10. b) Thumbnail image in the HST-WFPC2 R band, where the object is not detected. c), d), e) J, H, and Ks images respectively. f) Composite JHKs image. All thumbnail images are scaled to the original ISAAC pixel size, without smoothing, and are displayed with a linear scale.
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In the text

$\begin{figure} {\psfig{figure=Ga201_f2cmyk.eps,width=8.8cm,clip=} }\end{figure}$ Figure 2: True color composite images displaying the color difference between the lensed galaxy #1916 and other objects in this field: a) JHK and b) RJH. This object is blue in JHK as compared to cluster galaxies due to its intrinsically blue UV rest frame spectrum in HK, whereas it is red in RJH due to the presence of a break within the J band.
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In the text

$\begin{figure} {\psfig{figure=Ga201_f3.eps,width=8.8cm,clip=} }\end{figure}$ Figure 3: Optical to near-IR spectral energy distribution of the galaxy #1916. Shown are the broadband photometric measurements and associated 1 $~\sigma$ uncertainties for JHKs. Three $\sigma$ upper limits on 4 pixels are given for the non detections in VRI. The solid curve shows a good (98.7% probability) model fit with a synthetic spectrum of a young unreddened starburst with redshift z=10.0 of metallicity $Z=1/5~\mbox{$Z _{\odot}$ }$ , constant star formation, and an age of 3 Myr. The crosses indicate the corresponding broad band fluxes of the model. The upper axis shows the corresponding Ly $\alpha$ redshift.
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In the text

$\begin{figure} {\psfig{figure=Ga201_f4.eps,width=7cm,clip=} }\end{figure}$ Figure 4: 2D spectra showing the detected emission line of #1916, as well the nearby field galaxy and the [O III] $\lambda$ 5007 line of the galaxy #2582 (z=1.68) used as a reference to stack the data sets. 2D spectra are sky subtracted and show the spectral region around the emission-line at 1.33745 $\mu$ m, leading to $z=10.00175 \pm 0.00045$ when identified as Ly $\alpha$ (1215.67 Å). The line is seen on the 2 independent overlapping bands at 1.315 and 1.365 $\mu$ m. No smoothing was applied to these spectra. Both the object #2582 and the nearby field galaxy are identified in Fig. 1.
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In the text

$\begin{figure} {\psfig{figure=Ga201_f5.eps,width=8.8cm,angle=270,clip=} }\end{figure}$ Figure 5: a) 1D spectrum of #1916, extracted from the composite 2D spectrum of the 1.315 and 1.365 $\mu$ m bands. Dotted lines correspond to the position of the main sky OH emission lines. The continuum is not detected. The dashed line displays the level corresponding to 1 $~\sigma$ of the background noise. The displayed spectrum is smoothed to the instrumental resolution. b) Gaussian fit of the red half of the emission line, convolved with the instrumental profile (dotted line). Profiles corresponding to rest frame 60, 100 and 200 km s^-1 are also displayed for comparison (solid thick lines).
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In the text

$\begin{figure} {\psfig{figure=Ga201_f2cmyk.eps,width=8.8cm,clip=} }\end{figure}$	Figure 2: True color composite images displaying the color difference between the lensed galaxy #1916 and other objects in this field: a) JHK and b) RJH. This object is blue in JHK as compared to cluster galaxies due to its intrinsically blue UV rest frame spectrum in HK, whereas it is red in RJH due to the presence of a break within the J band.
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