![]() ![]() Plotting out different tungsten-halogen spectral data, there is evident a pattern of behavior, but there are slight differences. Indeed, the lower curve peaks higher, and the upper curve peaks lower. If you look closely at the SSF comparison chart in Post #2, you’ll notice that the lower and upper curves don’t quite match the reference data. Find a way to measure profile performance without prior reference data for the camera.Ī wonderful way to wile away the COVID-19 sequester… Power Measurement.Find out if the minimum lab-grad optical path alternative would significantly improve performance, and.Determine if simultaneous power measurement was required to produce good spectral data.Indeed, characterizing that camera is what got me going on this. Also, it concerned me that, once I finished figuring out how close I could come for a camera for which I had reference criteria, what would I do about my Z6, for which I had no such data. But there were still differences, and it ate at me that there might be an affordable level of device above the coarse light box that would close those gaps. ![]() Indeed, images I developed with this new profile looked fine, and it tamed the extreme blue situation that got me started chasing this. My measure of goodness was to compare the data I collected with a monochromator-based dataset for the same camera, and it surely looked close enough. This is in contrast to the widely accepted method of a succession of shots of single-wavelength presentations produced by a monochromator. In Post #2, I demonstrated a way to collect spectral data from a camera using what I’ll call the “single-shot spectrum” approach. ![]() I think the end result is satisfying, so let me describe the journey and the outcome. It’s been a bit of time since my last post on this, but I’ve been busy trying to put a bow on the whole thing. It’s amazing to me sometimes how pursuit of an endeavor can take you to places you hadn’t previously considered. How Close Can IT8 Come to SSF?" If you’re new to the series, you might want to read forward from the first post to understand what I’m doing here… Spectral Profiles "On The Cheap" and The Quest for Good Color - 3. Spectral Sensitivity Functions (SSFs) and Camera Profiles, The Quest for Good Color - 2. Zeitschrift für Instrumentenkunde, 22, 213–217.Note: This post is a follow-up to The Quest for Good Color - 1. Zeitschrift für Instrumentenkunde, 15, 362–370. Aplanatische und fehlerhafte Abbildung im Fernrohr. Teneriffe, an astronomer’s experiment: Or specialities of a residence above the clouds. The effect of condenser obstruction on the two-point resolution of a microscope. Formulas and theorems for the special functions of mathematical physics. Magnus, W., Oberheffinger, F., & Soni, R. Greenwood Village, Colorado, USA: Roberts & Company Publishers. Introduction to fourier optics (3rd ed.). Laser speckle and related phenomena (Vol. Optical and Quantum Electronics, 179–180.ĭainty, J. The effect of phase angle on the resolution of two coherently illuminated points. Journal of Optical Society of America, 56, 1001.Ĭook, D. Cambridge: Cambridge University Press.Ĭonsidine, P. Transactions of the Cambridge Philosophical Society, 5, 283.īorn, M., & Wolf, E. ![]() This process is experimental and the keywords may be updated as the learning algorithm improves.Ībramowitz, M., & Stegun, I. These keywords were added by machine and not by the authors. Linear superposition, convolution, isoplanaticity, and coherence are described, for use in dealing with extended objects. The amplitude and intensity point-spread functions of telescopes are defined. Ray terminologies are also introduced (e.g., principal ray, marginal ray). Optical system terminologies used to describe optical systems-telescopes in particular-are introduced (e.g., optical axis, telescope objective, central obstruction and telescope pupil function). The distribution of light energy in the Fraunhofer region describes the final image formed by the telescope. Solutions to the formula are given in three domains, all of which are used in the subsequent light propagation analysis: the geometrical optics region, the near-field Fresnel region and the far-field Fraunhofer region. The origin and basis of the Fresnel-Kirchhoff diffraction formula is described this formula derives directly from Maxwell’s equations. This chapter introduces the subject of diffraction-the key mechanism that determines how light propagates through the atmosphere and comes to a final focus in the telescope image plane. ![]()
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