poplasocialmedia.blogg.se - Zemax file for echelle spectrograph

#Zemax file for echelle spectrograph upgrade#
#Zemax file for echelle spectrograph full#

NACO (NAos-COnica) is an Adaptive Optics facility producing images as sharp as if taken in space.

ISAAC (Infrared Spectrometer And Array Camera) is an infrared imager and spectrograph, with an arm optimized for 1–2.5 μm and the other for 3–5 μm.AMBER is a near infrared Astronomical Multi-Beam combineR - an instrument for photometric and spectroscopic studies, which combines the light of three telescopes.4MOST has a high multiplex being able to simultaneously obtain spectra for ~2400 objects. 4MOST is a fibre-fed spectroscopic facility on the VISTA telescope with a large field-of-view to survey a significant fraction of the southern sky in a few years.X-shooter is a spectrograph covering a very wide range of wavelengths simultaneously.VISIR (VLT Imager and Spectrometer for mid-Infrared) studies the infrared light from celestial objects.UVES (UltraViolet and Visible Echelle Spectrograph) is the high-dispersion spectrograph of the VLT, observing from 300 nm to 1100 nm, with a maximum spectral resolution of 110 000.SPHERE (Spectro-Polarimetric High-contrast Exoplanet REsearch) is an extreme adaptive optics system with advanced coronographs, designed to observe exoplanets.

#Zemax file for echelle spectrograph full#

MUSE (Multi-Unit Spectroscopic Explorer) is a giant integral-field spectrograph, that can take spectra over its full field-of-view of about one square arcminute.KMOS (K-band Multi Object Spectrograph) is a near-infrared spectrograph equipped with 24 positionable integral-field units.HAWK-I (High Acuity Wide field K-band Imager) is a near-infrared imager with a relatively large field of view.FORS2 (FOcal Reducer and Spectrograph) is a multi-mode instrument that can be used for imaging in the visible and for low-resolution spectroscopy.It is also equipped for integral field spectroscopy. FLAMES (Fibre Large Array Multi-Element Spectrograph) offers the unique capability to study simultaneously and at high spectral resolution hundreds of individual stars in nearby galaxies.ESPRESSO (Echelle SPectrograph for Rocky Exoplanet and Stable Spectroscopic Observations) is a super-stable optical high-resolution spectrograph for the combined coudé focus of the VLT.ERIS (Enhanced Resolution Imager and Spectrograph) combines a general-use infrared imager and integral field spectrograph with the world-class adaptive optics installed on the VLT’s Unit Telescope 4 (Yepun).CRIRES (CRyogenic high-resolution InfraRed Echelle Spectrograph) provides a resolving power of up to 100 000 in the spectral range from 1 to 5 μm.

#Zemax file for echelle spectrograph upgrade#

AOF (Adaptive Optics Facility) is an upgrade of a 8-m Unit telescope of the Paranal Observatory with an Adaptive Secondary Mirror (DSM) to make this telescope an Adaptive Telescope providing turbulence corrected images at all focii, without the addition of adaptive modules and supplementary optics in front of the instruments.

4LGSF (4 Laser Guide Star Facility) sends four laser beams into the skies to produce four artificial stars by exciting sodium atoms located in the atmosphere.

If you need help with that let the community know. I’m guessing the people that told you to use it as a starting point meant that you could reprogram it to do what you exactly want it to do. Basically, it is how you specify which mirrors should be in which state ( A0, A1, or A2).Īs such, I don’t think you can use us_mems directly to solve your problem since it doesn’t apply a radius of curvature to the mirrors (to the best of my knowledge) and only has a fixed set of three different angles. P Flag and Rows 1-15 is a bit more complicated and is explained here. It is common for those devices to tilt at about 45 degrees so you would set Rot Angle = 45. The Rot Angle is the angle the micromirrors tilt about, when this value is zero, they seem to tilt about X. For example, you could set A0 = -12, A1 = 0, and A2 = +12, which would define three possible states for your micromirrors. The values A0, A1, and A2 from the us_mems dll are there to specify the available tilts for the micromirrors. Also note that the micromirrors generally tilt about the diagonal of the square surface they describe. Either the micromirror is tilted completely to one side or the other, and otherwise, it is considered to have a floating position (zero degree isn’t guaranteed), like when they are unpowered. It is an array of micromirrors, see image below from this document.Įach micromirror can tilt about a single axis and typically takes only two positions (plus or minus twelve degrees). As a side note, in the image above, the flat position adopted by many of the micromirrors isn’t typically achievable. I think what they call a MEMS in this DLL is actually a Digital Micromirror Device (DMD).