![zemax file echelle spectrograph zemax file echelle spectrograph](https://dpsablowski.files.wordpress.com/2015/12/li6104.png)
The motivation of the thesis is to study the limitations of the. Echelle++ can then be used independently, without access to commercial ray tracing software. The Echelle spectrograph operating at Vainu Bappu Telescope (VBT) is a general-purpose instrument designed for high-resolution spectroscopy. We chose to initially generate our own spectrograph model from the optical prescription in Zemax. John University Observatory since April 2001.HERCULES receives light from the f/13. of silicon immersion 6 DISTRIBUTION OF THIS DOCUMENT IS UNLIMIED.
![zemax file echelle spectrograph zemax file echelle spectrograph](https://www.spiedigitallibrary.org/ContentImages/Proceedings/9908/99086Z/FigureImages/00003_psisdg9908_99086z_page_4_1.jpg)
Echelle++ also works with low-resolution, low signal-to-noise, multi-object, IFU, or long-slit spectra, for simulating a wide array of spectrographs. The High Efficiency and Resolution Canterbury University Large Échelle Spectrograph (HERCULES) a fibre-fed échelle spectrograph that was designed and built at the University of Canterbury and has been in operation at Mt. of a Mid-IR Immersion Echelle Grating Spectrograph for Remote Sensing Norman L. The spectrograph is fiber fed, reaches a resolution of about 8,000, can be located in a gravity invariant and thermally controlled environment and can be used for the long term spectroscopic monitoring of bright objects.
![zemax file echelle spectrograph zemax file echelle spectrograph](https://img.yumpu.com/9379961/1/500x640/design-and-application-of-high-resolution-and-multiobject-.jpg)
It produces high-fidelity spectra fast, a very important feature when testing data reduction pipelines with a large set of different input spectra, when making critical choices about order spacing in the design phase of the instrument, or while aligning the spectrograph during construction. The basic idea is that any (fiber-fed) echelle spectrograph can be modelled with a set of wavelength-dependent transformation matrices and point spread functions which describe the spectrographs optics: First, wavelength-dependent affine transformation matrices are extracted from the ZEMAX model of the spectrograph. This instrument is an ideal solution to equip small telescopes with low cost but scientifically effective instrumentation. Echelle++ generates realistic spectra of astronomical and calibration sources, with accurate representation of optical aberrations, the shape of the point-spread function, detector characteristics, and photon noise.
ZEMAX FILE ECHELLE SPECTROGRAPH SOFTWARE
We present the software package, Echelle++, an open-source C++ code to simulate realistic raw spectra based on the Zemax model of any spectrograph, with a particular emphasis on cross-dispersed Échelle spectrographs.