Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms2420.f1.ps}\end{figure}$ Figure 1: Galaxy evolutionary tracks (dots) used to define our selection box, represented as the solid line. Filled symbols indicate galaxies in the range 2.9<z<3.5. Star symbols represent simulated colours for galactic stars with I_AB<20.0.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms2420.f2.ps}\end{figure}$ Figure 2: (U-B)_AB against (B-I)_AB for galaxies with I_AB<24 in the CFDF-03 hr field. Almost 14 000 objects are represented; for clarity only half of all objects in this field are shown. The solid line represents the selection box given in Eq. (1). There are 269 candidates (filled circles) which satisfy our selection criteria. The arrows indicate Lyman-break candidates which have a $1\sigma$ upper limit in U. Crosses indicate star-like objects (identified on the basis of their compactness). The three spectroscopically confirmed Lyman-break galaxies are shown with star symbols.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{ms2420.f3.ps}}\end{figure}$ Figure 3: Spectrum of a confirmed Lyman-break galaxy at redshift z=3.08 observed at CFHT using the MOS spectrograph. Spectral features are indicated with the dotted lines.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[clip]{ms2420.f4.ps}}\end{figure}$ Figure 4: Raw and corrected number counts of Lyman-break galaxies in the CFDF (open and filled circles respectively). The errorbars on each point is computed from the amplitude of the field-to-field variance. We also show colour-selected Lyman-break galaxy counts from Metcalfe et al. (2001) (filled squares) and Steidel et al. (1999) (filled triangles).
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{ms2420.f5.ps}}\end{figure}$ Figure 5: The amplitude of the angular correlation function, ${\omega (\theta )}$ , as a function of the angular separation in degrees, for a 20<I_AB<24.5 limited Lyman-break sample of the CFDF-14 hr field (filled black circles). Errorbars represent normal Poisson errors (Eq. (3)). The solid line shows the fitted correlation amplitude, derived using Eq. (5) and assuming a power-law slope of $\delta =0.8$ and a value of $C=4.2A_{\omega }$ for the integral constraint term. The dotted line shows the fitted power-law without the integral constraint correction. The long dashed line shows the fitted correlation amplitude (from Paper I) for field galaxies selected with the same limiting magnitude. Open squares are the ${\omega (\theta )}$ measurements from the Giavalisco et al. (1998) $\mathcal{R}<25.5$ selected Lyman-break sample.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{7.8cm}{!}{\includegraphics[clip]{ms2420.f6.ps}}\end{figure}$ Figure 6: The quadrant-averaged Lyman-break correlation function ${\omega (\theta )}$ for galaxies in the 03 hr and 22 hr fields (triangles and circles respectively). The amplitude of these error bars corresponds to the quadrant-to-quadrant variation in ${\omega (\theta )}$ . The solid line shows the fitted correlation amplitude for Lyman break galaxies in the 14 hr field with a fixed slope applied for one quadrant (Fig. 5).
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{7.7cm}{!}{\includegraphics[clip]{ms2420.f7.ps}}\end{figure}$ Figure 7: Contours of $\chi ^2$ for the mean ${\omega (\theta )}$ computed for Lyman-break galaxies selected with I_AB<24.5 in the CFDF-14 hr and CFDF-22 hr fields. The plus symbols show the best-fitting amplitudes and slopes, the contours correspond to the 1 $\sigma$ (thick contours) and 3 $\sigma$ confidence levels.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{7.7cm}{!}{\includegraphics[clip]{ms2420.f8.ps}}\end{figure}$ Figure 8: Contours of $\chi ^2$ for ${\omega (\theta )}$ for two subsamples of Lyman-break galaxies with 20.0<I_AB<23.5 and 23.5<I_AB<24.5 in the CFDF-14 hr field. The plus symbol shows the best-fitting amplitudes and slope, and two contours correspond to the 1 $\sigma$ (thick contours) and 3 $\sigma$ confidence levels.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[clip]{ms2420.f9.ps}}\end{figure}$ Figure 9: Comparison of the different errors contributing to the global cosmic errors as a function of angular scales for three different magnitude cuts of the CFDF-14 hr sample. The main source of errors are: the finite volume error E₁^1/2 (long-short-dashed line); the discreteness errors E₂^1/2 (short-dashed line), E₃^1/2 (long-dashed line), and the total cosmic error $E^{1/2}\equiv (E_1+E_2+E_3)^{1/2}$ (solid line) (see Bernstein 1994). Filled black circles are the Poissonian errors estimated from Eq. (3). The analytical errors are computed using a " $\Lambda$ CDM bias model'' (see Sect. 4.6).
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{10cm}{!}{\includegraphics[clip]{ms2420.f10.ps}} \end{figure}$ Figure 10: The comoving correlation length, r₀ (in h^-1 Mpc), for three samples of Lyman-break galaxies in the CFDF with the slope value fixed to $\delta =0.8$ (symbols slightly offset for clarity). The circle, square and the triangles represent the mean correlation length for each of the three fields, the correlation length for a magnitude-limited sample of the CFDF-14 hr fields with 20.0<I_AB<23.5 and the correlation length for a magnitude-limited sample of the CFDF-14 hr fields with 23.5<I_AB<24.5 respectively. We plot a range of r₀ measurements from the literature, which are described in detail in Sect. 5.2. The horizontal error bars represent an uncertainty of $10\%$ in the mean redshift. The solid vertical errorbars on r₀ are computed using Poisson statistics. Dotted vertical error bars represent the addition of this redshift error to the Poissonian component. The dotted line on the right part of the figure represents the errorbars for the CFDF-14 hr whole sample when we fit for both the slope and amplitude.
Open with DEXTER

In the text

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[clip]{ms2420.f11.ps}}\end{figure}$ Figure 11: The comoving correlation length r₀ (in h^-1 Mpc) for two magnitude-limited CFDF samples (filled circle symbol for the mean over the three fields, and filled square symbol for the CFDF-14 hr field with I_AB<23.5), as a function of cumulative surface density on the sky. Measurements from other Lyman-break samples (open symbols), and from the mean of HDF-N and -S (open triangles) are displayed. The solid vertical errorbars on r₀ are computed using Poisson statistics. Dotted vertical error bars represent the addition of the redshift error to the Poissonian component.
Open with DEXTER

In the text

$\begin{figure} \par\includegraphics[width=7.5cm,clip]{ms2420.f1.ps}\end{figure}$	Figure 1: Galaxy evolutionary tracks (dots) used to define our selection box, represented as the solid line. Filled symbols indicate galaxies in the range 2.9<z<3.5. Star symbols represent simulated colours for galactic stars with I_AB<20.0.
Open with DEXTER

$\begin{figure} \par\resizebox{8.4cm}{!}{\includegraphics[clip]{ms2420.f3.ps}}\end{figure}$	Figure 3: Spectrum of a confirmed Lyman-break galaxy at redshift z=3.08 observed at CFHT using the MOS spectrograph. Spectral features are indicated with the dotted lines.
Open with DEXTER

$\begin{figure} \par\resizebox{7.5cm}{!}{\includegraphics[clip]{ms2420.f4.ps}}\end{figure}$	Figure 4: Raw and corrected number counts of Lyman-break galaxies in the CFDF (open and filled circles respectively). The errorbars on each point is computed from the amplitude of the field-to-field variance. We also show colour-selected Lyman-break galaxy counts from Metcalfe et al. (2001) (filled squares) and Steidel et al. (1999) (filled triangles).
Open with DEXTER

$\begin{figure} \par\resizebox{7.7cm}{!}{\includegraphics[clip]{ms2420.f7.ps}}\end{figure}$	Figure 7: Contours of $\chi ^2$ for the mean ${\omega (\theta )}$ computed for Lyman-break galaxies selected with I_AB<24.5 in the CFDF-14 hr and CFDF-22 hr fields. The plus symbols show the best-fitting amplitudes and slopes, the contours correspond to the 1 $\sigma$ (thick contours) and 3 $\sigma$ confidence levels.
Open with DEXTER

$\begin{figure} \par\resizebox{7.7cm}{!}{\includegraphics[clip]{ms2420.f8.ps}}\end{figure}$	Figure 8: Contours of $\chi ^2$ for ${\omega (\theta )}$ for two subsamples of Lyman-break galaxies with 20.0<I_AB<23.5 and 23.5<I_AB<24.5 in the CFDF-14 hr field. The plus symbol shows the best-fitting amplitudes and slope, and two contours correspond to the 1 $\sigma$ (thick contours) and 3 $\sigma$ confidence levels.
Open with DEXTER