Comparison of G230LB and G230L

The trade-off between using the G230LB or the G230L (which uses the NUV-MAMA), depends sensitively on the science goals and your source properties.

• The CCD has read noise, whereas the MAMA does not.
• The CCD does not have bright object limits, whereas the MAMA does.
• The NUV-MAMA is solar insensitive whereas the CCD is not.
• The spatial sampling of the MAMA is better than that of the CCD.
• The CCD does not enable high time resolution (Dt<10 seconds),. whereas the MAMA does.
• For red objects, CCD data can suffer from scattered light problems. The detector PSF of the CCD is much cleaner than that of the NUV-MAMA.

Figure 13.22: Comparison of Limiting Magnitudes and Fluxes for G230LB and G230L. Plotted are the limiting source magnitudes and fluxes for G230LB and G230L to achieve a signal-to-noise ratio of 10 per 2-pixel spectral resolution element integrated across the PSF, in 1 hour.

Figure 13.23: Comparison of LSFs for G230LB and G230L