Next: 7. SWS Calibration Up: 6. The RSRF and Previous: 6.6 Spurious Narrow Spectral

6.7 Overview of the RSRF curves

RSRF curves for all bands are plotted in this section. Note that the graphs are not noisy, but are affected by high frequency fringes.

**Figure 6.6:** The RSRF for band 1A based on a measurement of HR7001 (black) versus the RSRF as measured in the lab (grey). The fringes in the in-orbit-RSRF are real.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf1a.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.7:** The RSRF for band 1A based on a measurement of HR7001 (black) and the lab RSRF corrected to the overall shape of the in-orbit RSRF. Note that not every feature that was seen in the lab has been seen in orbit. Especially the differences in the 2.35 - 2.40 $\mu m$ region are relatively large. Similar features seen in SWS spectra might be not real.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf1afudged.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.8:** The RSRF for band 1b based on a measurement of HR7001 versus the lab RSRF (grey). The fringes in the in-orbit-RSRF are real.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf1b.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.9:** The RSRF for band 1d based on a measurement of HR7001 versus the lab RSRF (grey). The fringes in the in-orbit-RSRF are real.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf1d.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.10:** The RSRF for band 1e based on a measurement of HR7001 versus the lab RSRF (grey). The fringes in the in-orbit-RSRF are real.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf1e.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.11:** The RSRF for band 2a based on a measurement of HR7001 versus the lab RSRF (grey). The fringes in the in-orbit-RSRF are real.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf2a.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.12:** The RSRF for band 2A based on a measurement of HR7001 (black) and the lab RSRF corrected to the overall shape of the in-orbit RSRF.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf2afudged.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.13:** The RSRF for band 2b based on a measurement of HR7001 versus the lab RSRF (grey). Also in this band the lab measurements seem to show leakage. Attempts to correct the overall shape did not survive cross-checks with other calibration sources.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf2b.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.14:** The RSRF for band 2c based on an AOT 1 speed 4 measurement of HR5340 (black) versus the lab RSRF (grey). The small features between 7 and 8 microns and around 10 microns can introduce misleading features after incorrect dark. The increase in response beyond 12 microns has been seen in other sources.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf2c.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.15:** The RSRF for band 3a based on a measurement of NML-CYG versus the lab RSRF (grey). There is a good match, even at the fringe level. The fringes are a little ``sharper'' in the in-orbit RSRF because of the limited resolution of the lab measurements. Wrong dark subtraction will produce many spurious features.
$\begin{figure} \begin{tabular}{c} \centerline{\epsfig{file={rsrf3a.eps},width=15.0cm}}\\ \end{tabular}\end{figure}$

**Figure 6.16:** The RSRF for band 3c based on a measurement of NML-CYG versus the lab RSRF (grey). There is a good match, even at the fringe level. The fringes are a little 'sharper' in the in-orbit RSRF because of the limited resolution of the lab measurements. Wrong dark subtraction will produce many spurious features.
$\begin{figure} \begin{tabular}{c} {\epsfxsize =15cm \epsfbox{rsrf3c.eps}} \\ \end{tabular}\end{figure}$

**Figure 6.17:** The RSRF for band 3d based on a measurement of NML-CYG versus the lab RSRF (grey). There is a good match, even at the fringe level. The fringes are a little 'sharper' in the in-orbit RSRF because of the limited resolution of the lab measurements. Wrong dark subtraction will produce many spurious features.
$\begin{figure} \begin{tabular}{c} {\epsfxsize =15cm \epsfbox{rsrf3d.eps}} \\ \end{tabular}\end{figure}$

**Figure 6.18:** The RSRF for band 3e based on a measurement of NML-CYG versus the lab RSRF (grey). There is a good match, even at the fringe level. Wrong dark subtraction will produce many spurious features.
$\begin{figure} \begin{tabular}{c} {\epsfxsize =15cm \epsfbox{rsrf3e.eps}} \\ \end{tabular}\end{figure}$

**Figure 6.19:** The RSRF for band 4 based on a measurement of NML-CYG versus the lab RSRF (grey). Since the model of NML-CYG is only accurate to 30%, it is not clear if the in-orbit RSRF is actually different from the lab RSRF.
$\begin{figure} \begin{tabular}{c} {\epsfxsize =15cm \epsfbox{rsrf4nml.eps}} \\ \end{tabular}\end{figure}$

**Figure 6.20:** The RSRF for band 4 based on an AOT 1 speed 4 measurement of ETA-CAR versus the lab RSRF (grey).
$\begin{figure} \begin{tabular}{c} {\epsfxsize =15cm \epsfbox{rsrf4eta.eps}} \\ \end{tabular}\end{figure}$

Next: 7. SWS Calibration Up: 6. The RSRF and Previous: 6.6 Spurious Narrow Spectral

SWS Instrument & Data Manual, Issue 1.0, SAI/98-095/Dc