![]() But there are two problems if you take one spectrum after the other: At first, you lose time, and second, you don’t collect the data at the same time, which can a problem at fast-changing objects. You might say that you know in advance which part of the spectrum of a star you want to analyze. Taking an Echelle-spectrum is not more complicated than a guided deep-sky-image. Also, common high-res gratings are optimzed only for a part of the spectrum. This way, all relevant parts of the spectrum are covered AT THE SAME TIME. So, the biggest advantage of a BACHES Echelle spectrograph over a common Blaze Grating with a comparable resolution is obviously that you can cover the complete spectrum at the highest-possible resolution in just one image. With an Echelle spectrograph, you can take at once an image of the complete spectrum with one not-too-large CCD-sensor. ![]() In contrast to this, high-res gratings are optimzed for a rather small part of the spectrum you’d also need very long CCD-sensors (or a line of several sensors) to take an image of the complete first or second order spectrum at once. Echelle gratings are often used in astronomy for taking images of stellar spectras at high resolution, because this way a high-res spectrum covering a very large wavelength-range can be photographed in one single image.
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