4.1. Example 2 - Datasets descriptions¶
4.1.1. Separate CCDs¶
This is a GMOS-N imaging observation of the galaxy Bootes V obtained in the r-band.
The calibratons we use in this example are:
- BPM. The bad pixel masks are now found in the Gemini Science Archive instead of being packaged with the software. They are associated like the other calibrations. Here we need the 2x2 binning GMOS-N Hamamatsu BPM valid for data taken in 2022. (The date in the name is the “valid from” date.)
- Biases for the science frames and the twilight flats. Note that the twilight flats were obtained several before after the science observations. We are going to use two set of biases, each contemporary to the science and the twilight frame, respectively.
- Twilight flats.
The Bad Pixel Masks (BPMs) are now found in the archive rather than packaged with the software. You must get the static BPM from the archive. See Getting Bad Pixel Masks from the archive in Tips and Tricks.
For accurate photometry, observations of photometric standard of various colors should be obtained and observed on each of the 3 CCDs.
350 s, i-band