This loads the data and shapes it, contains the resultant array, which you need to save:ġ2) IDL> save,output,'path2/filename2. Now that the corrector is ready, we can correct the space of each file, either by hand, or as part of a procedure: (this creates a file called spec.map) Correcting the array shape This opens another big widget, which you use to mark the order you want to crop, then hit Ī second screen pops up, and hopefully you'll be able to see two horizontal lines, which are the star continuum.Ĭlick on the two star lines until the program draws nice lines through them both, then hit Ī another widget pops up - this time select the individual lines you've chosen to fit, using the bottom right to select each line, one by one, and once enough are fitted for a decent calibration (the program doesn't need all the lines fitted), hit Nod2: the path/filename of the second star file Nod1: the path/filename of the first star file Refarc: the path/filename of the spec1.in file Īrc1: the path/filename of the wavelength reference file CWITools analyzes integral field spectroscopy data from the Palomar and Keck Cosmic Web Imagers. This opens up a big widget, and you need to fill in cetrain details before hitting. It reads an input particle distribution file and can. Then save a second blank files as star2, so the program subtracts nothing from star1 Producing the array shape correction It often struggles to do this, so you have to cheatĭo the a-b yourself and clean up the array so both star lines are clear and save it as a fits file star1 The program will also need the star to show up as two lines on the array, and it gets these from two star files, finding the sky-subtracted (a-b)
#Keck nirspec zemax file software
The SPICE software is available in six languages, and for most popular computing. , calculation of infrared-divergent feynman diagrams with zero mass. from the data contained within the kernels. calculation of infrared-divergent feynman diagrams with zero mass. The program will need some example lines with a known wavelength, so that it can scale the x-direction properlyīuild a calibration file from arcs, combined skylines or H3+ by coadding the files you need until there is a clear signal SPICE comprises both ancillary data files, called kernels, and a suite of software used to produce those kernels and to compute derived quantities such as altitude, latitude/longitude, lighting angles, etc. NB: this file should be in ascii, the wavelengths should be in microns, and the file should contain no empty lines. All you need are lines you can see, and a definitive wavelength to go with them. This file contains wavelengths of lines that are visable on the spectra of the chosen calibration file. file_prefix()+'data/obs_06/2006sep05/spec/')Ģ) Create a subdirectory of /reduced/uranus/order19 In order to get round the problems that RedSpec seems to throw up with flat fielding, we are going to use RedSpec to respace the spectra into the correct aspect, and then use flats and darks separately to remove the errors from the array Preparing the filesġ) Go to the data directory where the spectra are kept (e.g.