|Space Telescope Science Institute|
|Handbooks HTML Update Nov 2014|
The last in the series of supported long slits used with the first-order gratings and prism and is a good slit for spectrophotometric observations of point sources. The small dip seen at 2000Å is likely due to uncertainties in the numerical calculation, and will not affect the absolute flux calibration.Observations using this slit do not need to be preceded by a PEAKUP. Be aware of effects of OTA scatter on the line profiles when observing point sources in the wide slits (see Section 13.7). Targets not centered on the slit along the spatial direction can experience significant shifts in wavelength.Table 13.22: 52X2 Throughputs.
Figure 13.69: 52X2 Aperture Throughput as a Function of Wavelength