Astronomy & Astrophysics

All Figures

$\begin{figure} \par\includegraphics[width=15.4cm,clip]{raw_stk.ps}\end{figure}$ Figure 1: Left: Single raw file (1 hour exposure). Right: Stack from seven input raw files (total exposure time 7 hours). The setting 346_DI1_ $2\times 2$ has been used here. Echelle orders run almost vertically, with wavelength increasing downwards and to the right. The two black lines mark the sky-exposed part of one specific order. The dark continuum is stellar flux. The sky emission lines, as monochromatic images of the entrance slit, mark the slit extension. The inter-order space (bright) can clearly be distinguished from the slit-illuminated CCD areas on the stacked frame.
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In the text

$\begin{figure} \par\includegraphics[width=17.75cm,clip]{extract.ps}\end{figure}$ Figure 2: 2D extracted (bottom) and 1D extracted spectrum (top). The central order marked in Fig. 1 has been selected here. Wavelength scale increases towards the right. The two sky windows are marked. The collapsed 1D sky spectrum has been constructed from these two windows. The features accepted and measured as sky emission lines are marked by open triangles.
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In the text

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{cross.ps}\end{figure}$ Figure 3: Cross-dispersion scans (setting 346_DI1_ $2\times 2$ ). One scan every 50 Å in slit direction is shown. The two areas defined by the broken lines define the two extraction windows for the sky spectrum (SKY1, SKY2). Their width is 4 binned pixels (2 $\hbox {$^{\prime \prime }$ }$ ) each, to be safe for the seeing wings of the object signal.
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In the text

$\begin{figure} \par\includegraphics[width=8.4cm,clip]{resp.ps}\end{figure}$ Figure 4: Master response curves selected for the flux calibration of the sky emission spectrum.
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In the text

$\begin{figure} \par\includegraphics[width=17.4cm,clip]{full.ps}\end{figure}$ Figure 5: Strongly averaged UVES sky emission spectrum. Bottom: flux sampled into 5 Å bins. The continuum flux, indicated by the solid line, is roughly constant at about $1{-}2 \times 10^{-17}$ cgs units ( ${\rm erg\ s^{-1}\ \AA^{-1}\ cm^{-2}\ arcs^{-2}}$ ). The settings used are labelled. Top: the total sky emission flux (line plus continuum) averaged across 50 Å bins, and the continuum flux plotted as solid line. The flux scale is logarithmic, with the same flux units as in the bottom panel.
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In the text

$\begin{figure} \par\includegraphics[width=8.8cm,clip]{diff.ps}\end{figure}$ Figure 6: Residuals of wavelength determinations between the Keck atlas and the UVES atlas. 529 lines redwards of 5200 Å have been measured, with a mean difference of 8 mÅ and a standard deviation of 17 mÅ.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/3460_1.ps}\end{figure}$ Figure 7: The night-sky spectrum as seen by UVES, covering the wavelength range $\lambda \lambda$ 3140-3300 Å. The vertical bars mark line measurements from this atlas.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/3460_2.ps}\end{figure}$ Figure 8: Same as Fig. 7, for range 3300-3460 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/3460_3.ps}\end{figure}$ Figure 9: Same as Fig. 7, for range 3460-3620 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/3460_4.ps}\end{figure}$ Figure 10: Same as Fig. 7, for range 3620-3760 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_1.ps}\end{figure}$ Figure 11: UVES night-sky spectrum, covering 3740-3900 Å. The vertical bars mark line measurements from this atlas. See the text of the Appendix for more general information about these plots.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_2.ps}\end{figure}$ Figure 12: Same as Fig. 11, for range 3900-4060 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_3.ps}\end{figure}$ Figure 13: Same as Fig. 11, for range 4060-4220 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_4.ps}\end{figure}$ Figure 14: Same as Fig. 11, for range 4220-4380 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_5.ps}\end{figure}$ Figure 15: Same as Fig. 11, for range 4380-4540 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_6.ps}\end{figure}$ Figure 16: Same as Fig. 11, for range 4540-4700 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_7.ps}\end{figure}$ Figure 17: Same as Fig. 11, for range 4700-4860 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800L_1.ps}\end{figure}$ Figure 18: UVES night-sky spectrum, covering 4810-5050 Å. See the text of the Appendix for more general information about these plots. The vertical bars mark line measurements from this atlas. The sky spectrum is also plotted on a scale compressed by a factor 10 to better show stronger lines. The full circles mark emission lines with identification in the Keck atlas (Osterbrock et al. 1996).
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800L_2.ps}\end{figure}$ Figure 19: Same as Fig. 18, for range 5050-5290 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800L_3.ps}\end{figure}$ Figure 20: Same as Fig. 18, for range 5290-5530 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800L_4.ps}\end{figure}$ Figure 21: Same as Fig. 18, for range 5530-5770 Å.
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In the text

$\begin{figure} \par\includegraphics[width=14.7cm,clip]{VERSION_ELEC/5800U_1.ps}\end{figure}$ Figure 22: UVES night-sky spectrum, covering 5830-6070 Å. See the text of the Appendix for more general information about these plots. The vertical bars mark line measurements from this atlas. The sky spectrum is also plotted on a scale compressed by a factor 5 to better show stronger lines. The full circles mark emission lines with identification in the Keck atlas (Osterbrock et al. 1996). The crosses mark the (air-corrected) positions of identified OH lines in the Rousselot et al. (2000) and Lidman et al. (2000) lists. Artefacts due to a leaking column are marked by a squared plus.
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In the text

$\begin{figure} \par\includegraphics[width=14.7cm,clip]{VERSION_ELEC/5800U_2.ps}\end{figure}$ Figure 23: Same as Fig. 22, for range 6070-6310 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800U_3.ps}\end{figure}$ Figure 24: Same as Fig. 22, for range 6310-6550 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800U_4.ps}\end{figure}$ Figure 25: Same as Fig. 22, for range 6550-6790 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_1.ps}\end{figure}$ Figure 26: UVES night-sky spectrum, covering 6700-6940 Å. See the text of the Appendix for more general information about these plots. The vertical bars mark line measurements from this atlas. The sky spectrum is also plotted on a scale compressed by a factor of 10 to better show stronger lines. The full circles mark emission lines with identification in the Keck atlas (Osterbrock et al. 1996). The crosses mark the (air-corrected) positions of identified OH lines in the Rousselot et al. (2000) and Lidman et al. (2000) lists.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_2.ps}\end{figure}$ Figure 27: Same as Fig. 26, for range 6940-7180 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_3.ps}\end{figure}$ Figure 28: Same as Fig. 26, for range 7180-7420 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_4.ps}\end{figure}$ Figure 29: Same as Fig. 26, for range 7420-7660 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_5.ps}\end{figure}$ Figure 30: Same as Fig. 26, for range 7660-7900 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_6.ps}\end{figure}$ Figure 31: Same as Fig. 26, for range 7900-8140 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_7.ps}\end{figure}$ Figure 32: Same as Fig. 26, for range 8140-8380 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_8.ps}\end{figure}$ Figure 33: Same as Fig. 26, for range 8380-8560 Å.
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In the text

$\begin{figure} \par\includegraphics[width=14.7cm,clip]{VERSION_ELEC/8600U_1.ps}\end{figure}$ Figure 34: UVES night-sky spectrum, covering 8600-8840 Å. See the text of the Appendix for more general information about these plots. The vertical bars mark line measurements from this atlas. The sky spectrum is also plotted on a scale compressed by a factor 10 to better show stronger lines. The full circles mark emission lines with identification in the Keck atlas (Osterbrock et al. 1996). The crosses mark the (air-corrected) positions of identified OH lines in the Rousselot et al. (2000) and Lidman et al. (2000) lists. Artefacts due to a leaking column are marked by a squared plus.
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In the text

$\begin{figure} \par\includegraphics[width=14.7cm,clip]{VERSION_ELEC/8600U_2.ps}\end{figure}$ Figure 35: Same as Fig. 34, for range 8840-9080 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600U_3.ps}\end{figure}$ Figure 36: Same as Fig. 34, for range 9080-9320 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600U_4.ps}\end{figure}$ Figure 37: Same as Fig. 34, for range 9320-9560 Å.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600U_5.ps}\end{figure}$ Figure 38: Same as Fig. 34, for range 9560-9800 Å. There is a small gap near 9765 Å, due to incomplete spectral coverage by the CCD.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600U_6.ps}\end{figure}$ Figure 39: Same as Fig. 34, for range 9800-10 040 Å. There is a small gap near 9922 Å, due to incomplete spectral coverage by the CCD.
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In the text

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600U_7.ps}\end{figure}$ Figure 40: Same as Fig. 34, for range 10 040-10 280 Å. There are two gaps near 10086 Å and 10253 Å due to incomplete spectral coverage by the CCD.
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In the text

$\begin{figure} \par\includegraphics[width=16cm,clip]{VERSION_ELEC/8600U_8.ps}\end{figure}$ Figure 41: Same as Fig. 34, for range 10 280-10 430 Å.
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In the text

$\begin{figure} \par\includegraphics[width=17.75cm,clip]{extract.ps}\end{figure}$	Figure 2: 2D extracted (bottom) and 1D extracted spectrum (top). The central order marked in Fig. 1 has been selected here. Wavelength scale increases towards the right. The two sky windows are marked. The collapsed 1D sky spectrum has been constructed from these two windows. The features accepted and measured as sky emission lines are marked by open triangles.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=7.4cm,clip]{cross.ps}\end{figure}$	Figure 3: Cross-dispersion scans (setting 346_DI1_ $2\times 2$ ). One scan every 50 Å in slit direction is shown. The two areas defined by the broken lines define the two extraction windows for the sky spectrum (SKY1, SKY2). Their width is 4 binned pixels (2 $\hbox {$^{\prime \prime }$ }$ ) each, to be safe for the seeing wings of the object signal.
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$\begin{figure} \par\includegraphics[width=8.4cm,clip]{resp.ps}\end{figure}$	Figure 4: Master response curves selected for the flux calibration of the sky emission spectrum.
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$\begin{figure} \par\includegraphics[width=8.8cm,clip]{diff.ps}\end{figure}$	Figure 6: Residuals of wavelength determinations between the Keck atlas and the UVES atlas. 529 lines redwards of 5200 Å have been measured, with a mean difference of 8 mÅ and a standard deviation of 17 mÅ.
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/3460_1.ps}\end{figure}$	Figure 7: The night-sky spectrum as seen by UVES, covering the wavelength range $\lambda \lambda$ 3140-3300 Å. The vertical bars mark line measurements from this atlas.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/3460_2.ps}\end{figure}$	Figure 8: Same as Fig. 7, for range 3300-3460 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/3460_3.ps}\end{figure}$	Figure 9: Same as Fig. 7, for range 3460-3620 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/3460_4.ps}\end{figure}$	Figure 10: Same as Fig. 7, for range 3620-3760 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_1.ps}\end{figure}$	Figure 11: UVES night-sky spectrum, covering 3740-3900 Å. The vertical bars mark line measurements from this atlas. See the text of the Appendix for more general information about these plots.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_2.ps}\end{figure}$	Figure 12: Same as Fig. 11, for range 3900-4060 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_3.ps}\end{figure}$	Figure 13: Same as Fig. 11, for range 4060-4220 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_4.ps}\end{figure}$	Figure 14: Same as Fig. 11, for range 4220-4380 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_5.ps}\end{figure}$	Figure 15: Same as Fig. 11, for range 4380-4540 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_6.ps}\end{figure}$	Figure 16: Same as Fig. 11, for range 4540-4700 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/4370_7.ps}\end{figure}$	Figure 17: Same as Fig. 11, for range 4700-4860 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800L_1.ps}\end{figure}$	Figure 18: UVES night-sky spectrum, covering 4810-5050 Å. See the text of the Appendix for more general information about these plots. The vertical bars mark line measurements from this atlas. The sky spectrum is also plotted on a scale compressed by a factor 10 to better show stronger lines. The full circles mark emission lines with identification in the Keck atlas (Osterbrock et al. 1996).
Open with DEXTER

$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800L_2.ps}\end{figure}$	Figure 19: Same as Fig. 18, for range 5050-5290 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800L_3.ps}\end{figure}$	Figure 20: Same as Fig. 18, for range 5290-5530 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800L_4.ps}\end{figure}$	Figure 21: Same as Fig. 18, for range 5530-5770 Å.
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$\begin{figure} \par\includegraphics[width=14.7cm,clip]{VERSION_ELEC/5800U_2.ps}\end{figure}$	Figure 23: Same as Fig. 22, for range 6070-6310 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800U_3.ps}\end{figure}$	Figure 24: Same as Fig. 22, for range 6310-6550 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/5800U_4.ps}\end{figure}$	Figure 25: Same as Fig. 22, for range 6550-6790 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_2.ps}\end{figure}$	Figure 27: Same as Fig. 26, for range 6940-7180 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_3.ps}\end{figure}$	Figure 28: Same as Fig. 26, for range 7180-7420 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_4.ps}\end{figure}$	Figure 29: Same as Fig. 26, for range 7420-7660 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_5.ps}\end{figure}$	Figure 30: Same as Fig. 26, for range 7660-7900 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_6.ps}\end{figure}$	Figure 31: Same as Fig. 26, for range 7900-8140 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_7.ps}\end{figure}$	Figure 32: Same as Fig. 26, for range 8140-8380 Å.
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$\begin{figure} \par\includegraphics[width=15cm,clip]{VERSION_ELEC/8600L_8.ps}\end{figure}$	Figure 33: Same as Fig. 26, for range 8380-8560 Å.
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$\begin{figure} \par\includegraphics[width=14.7cm,clip]{VERSION_ELEC/8600U_2.ps}\end{figure}$	Figure 35: Same as Fig. 34, for range 8840-9080 Å.
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