![]() Each location within the survey will be observed with a total of 5-7 The typical exposure time in units of seconds. collecting_area The actual collecting area after accounting for obscuration, struts, etc. The linear obscuration of the telescope, expressed as a fraction of the diameter. Include effects like distortion, which are included in the WCS. The pixel scale in units of arcsec/pixel. Once the actual detectors exist and have beenĬharacterized, it might be updated to be a dict with entries for each SCA. Single value rather than a list of values. The gain for all SCAs (sensor chip assemblies) is expected to be the roughly the same,Īnd we currently have no information about how different they will be, so this is a To keep in mind that it is voltage that is sensed. To quantities measured in units of e-/pixel, but for some detector non-idealities, it is important To use a common language with that for CCDs, we will often refer ![]() Moreover, theĪctual quantity that is measured is technically not charge, but rather voltage. However, instead ofīeing read out along columns (as for CCDs), they are read directly from each pixel. In particular, the photon detection process begins with charge generation. The NIR detectors that will be used for Roman have a different photon detection process from CCDs. This isĬonsistent with diagrams and so on provided by the Roman project, which are 1-indexed. All SCA-related arrays are 1-indexed, i.e., theĮntry with index 0 is None and the entries from 1 to n_sca are the relevant ones. PSF and WCS, are specific to each SCA (Sensor Chip Assembly, the equivalent of a chip for an opticalĬCD) and therefore are indexed based on the SCA. Others, especially the return values of the functions to get the Some of these parameters relate to the entire Parameters related to the Roman geometry. There are a number of attributes of the galsim.roman module, which define some numerical
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