All Figures

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6514fg1.ps}\end{figure}$ Figure 1: WFCAM on the 3.8 m UK Infrared Telescope. WFCAM is the tall cylindrical structure mounted above the primary mirror. Photo courtesy of P. Hirst.
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In the text

$\begin{figure} \par\includegraphics[width=5cm,clip]{6514fg2.ps}\end{figure}$ Figure 2: WFCAM focal plane on the sky. Dimensions of the field of view are shown along with the 2MASS field (3 simultaneous bands) for comparison. The central diamond shape is the autoguider CCD field.
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In the text

$\begin{figure} \par\includegraphics[width=8cm,clip]{6514fg3.ps}\end{figure}$ Figure 3: WFCAM optical layout showing the overall design on the telescope at top, with details of the cryostat optics below.
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In the text

$\begin{figure} \par\includegraphics[height=4.8cm,width=4.8cm,clip]{6514fg4a.ps}\... ...e*{5mm} \includegraphics[height=4.8cm,width=4.8cm,clip]{6514fg4b.ps}\end{figure}$ Figure 4: $\rho$ Ophiuchi 1 $\times$ 1 degree field showing 2MASS K-band point source detections ( top) and the same field as imaged in K by WFCAM in 30 min ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6514fg5.ps}\end{figure}$ Figure 5: Two K-band stellar magnitudes monitored over 7 epochs over several months in the $\rho$ Oph field. Dashed lines show 5 $\sigma$ error bars on the mean. One star is constant ( top) within errors while the other is variable ( bottom).
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In the text

$\begin{figure} \par\includegraphics[width=7.25cm,clip]{6514fg6.ps}\end{figure}$ Figure 6: Differential number counts as a function of K-band magnitude from the UKIDSS UDS Early Data Release, sampling a dynamic range of approximately 6 mag. At the completeness limit (K=20.6) the majority of sources are distant galaxies, with median redshifts of $z\sim 1$ . The final UDS survey will reach K=23.
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In the text

$\begin{figure} \par\includegraphics[width=8.2cm,clip]{6514fg1.ps}\end{figure}$	Figure 1: WFCAM on the 3.8 m UK Infrared Telescope. WFCAM is the tall cylindrical structure mounted above the primary mirror. Photo courtesy of P. Hirst.
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$\begin{figure} \par\includegraphics[width=5cm,clip]{6514fg2.ps}\end{figure}$	Figure 2: WFCAM focal plane on the sky. Dimensions of the field of view are shown along with the 2MASS field (3 simultaneous bands) for comparison. The central diamond shape is the autoguider CCD field.
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$\begin{figure} \par\includegraphics[width=8cm,clip]{6514fg3.ps}\end{figure}$	Figure 3: WFCAM optical layout showing the overall design on the telescope at top, with details of the cryostat optics below.
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$\begin{figure} \par\includegraphics[height=4.8cm,width=4.8cm,clip]{6514fg4a.ps}\... ...e*{5mm} \includegraphics[height=4.8cm,width=4.8cm,clip]{6514fg4b.ps}\end{figure}$	Figure 4: $\rho$ Ophiuchi 1 $\times$ 1 degree field showing 2MASS K-band point source detections ( top) and the same field as imaged in K by WFCAM in 30 min ( bottom).
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$\begin{figure} \par\includegraphics[width=7.8cm,clip]{6514fg5.ps}\end{figure}$	Figure 5: Two K-band stellar magnitudes monitored over 7 epochs over several months in the $\rho$ Oph field. Dashed lines show 5 $\sigma$ error bars on the mean. One star is constant ( top) within errors while the other is variable ( bottom).
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$\begin{figure} \par\includegraphics[width=7.25cm,clip]{6514fg6.ps}\end{figure}$	Figure 6: Differential number counts as a function of K-band magnitude from the UKIDSS UDS Early Data Release, sampling a dynamic range of approximately 6 mag. At the completeness limit (K=20.6) the majority of sources are distant galaxies, with median redshifts of $z\sim 1$ . The final UDS survey will reach K=23.
Open with DEXTER