All Figures

$\begin{figure} \par\includegraphics[width=17.9cm,clip]{Gj011_fig1.eps} \end{figure}$ Figure 1: From left to right, thumbnails of the confirmed Ly $\alpha$ emitter S11_13368 at redshift 5.721. Each thumbnail covers a 24 $^{\prime \prime }$ $\times$ 24 $^{\prime \prime }$ region with a pixel scale of 0 $.\!\!^{\prime\prime}$ 238 pix^-1. The emitter is only detected in the M₈₁₅ and N₈₁₇ images.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{Gj011_fig2.eps} \end{figure}$ Figure 2: A $30\hbox {$^{\prime \prime }$ }\times 30\hbox {$^{\prime \prime }$ }$ region around the confirmed Ly $\alpha$ galaxy S11_13368 at z = 5.721 from the pre-image taken with FORS2. The image has a pixel scale of 0 $.\!\!^{\prime\prime}$ 252 pix^-1. The object is unresolved in this image. The seeing at the time of these observations was $\sim$ 0 $.\!\!^{\prime\prime}$ 5. The exposure time was 3600 s.
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In the text

$\begin{figure} \par\includegraphics[width=7.7cm,clip]{Gj011_fig3.eps} \end{figure}$ Figure 3: A fit of both one- and two-component models to the profile of the Ly $\alpha$ line. a) The two dimensional spectrum centered on the Ly $\alpha$ line. In this unrectified spectrum, the night sky emission lines are not removed. The pixel scale for this image is 0 $.\!\!^{\prime\prime}$ 252 pix^-1 in the spatial direction and 0.86 Å pix^-1 in the dispersion direction. b) Observed Ly $\alpha$ line ( histograms) with the three best-fitting models. For clarity, the models are offset by 3 erg s^-1 cm^-2 Å^-1. The two-component models consist of a two components: a broad, truncated Gaussian and a narrower redshifted Gaussian. The one-component model consists of only a broad, truncated Gaussian. See Table 1 for the parameters of the "broad'' ( solid), "spiky'' ( dotted) and "single component'' ( dashed) models. c) Same model line profiles as in b) but before convolution with the instrument profile. d) Observed data minus model fit (as plotted in b)) residuals, demonstrating a random scatter about the zero flux line. Also shown ( histograms) is the 1 $\sigma$ -error spectrum from the observed data, which includes both sky- and Poisson noise. Note that the red peak is not N V. At this redshift it would appear around 8334 Å.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{Gj011_fig4.eps} \end{figure}$ Figure 4: Size of the star-forming region versus the star-formation rate. The SFR of two galaxies from Heckman et al. (1990) is indicated by a bar, as there are two measurements of the SFR. The arrows represent lower-limits to the SFR and upper-limits to the size of the major axis, (due to seeing limited observations). Error-bars are not included. The plus signs represent three well-known local starbursting galaxies (Heckman et al. 1990).
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In the text

$\begin{figure} \par\includegraphics[width=17.9cm,clip]{Gj011_fig1.eps} \end{figure}$	Figure 1: From left to right, thumbnails of the confirmed Ly $\alpha$ emitter S11_13368 at redshift 5.721. Each thumbnail covers a 24 $^{\prime \prime }$ $\times$ 24 $^{\prime \prime }$ region with a pixel scale of 0 $.\!\!^{\prime\prime}$ 238 pix^-1. The emitter is only detected in the M₈₁₅ and N₈₁₇ images.
Open with DEXTER