IRAF Tutorial. Installing on Fedora 64bit and 32bit: IRAF (image reduction and analysis facility) is a collection of software written at the. National Optical. IRAF Tutorial. Installing on Ubuntu 64bit and 32bit: IRAF (image reduction and analysis facility) is a collection of software written at the. National Optical. Go to Top IRAF, the Image Reduction and Analysis Facility, is one of the more historic way that astronomers reduce and analyze imaging and.

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Iraf Guide

To load a package, just type the package name at the IRAF prompt. Y ou need to edit e ach of these.

When master Zero, Dark and Flats tuotrial ready, we then run a program called ccdproc that automatically subtracts the Zero and Dark scaled to exposure time from each object file, and divides by the appropriate Flat for the filter used. Make sure any object files you want process are in IRAF format. W hat values f or the FWHM did iaf determine? Irac is the Image Reduction and Analysis Facilitya general purpose software system for the reduction and tutoriaal of astronomical data. Z when it is compressed.

In this c ase, there are large enough x-y s hifts b etween i mages, and the number of stars selected uneve n betwe en f ilters to make this work tutoriao ell enough f or us to try. To cope with the blending of stellar PSF s, the stars are grouped together before fitting if there is overlap, and each star in a group is fitted at the same time.

Choose i solated, f airly bright stars. The first is processing the images. Th e program will not overwrite a mag file. Note that there i s an error in this f ile. In the futu re, you will need to get s ome intuitive s ense of how these param eters a ffect y our results.


The purpose is to determine the pixel-to-pixel pattern caused by sensitivity variations of the pixels or shadowing “vignetting” by telescope optics or dust particles.

It i s best if y ou do not rush the program here. What w ould we have done i f we tjtorial 50 i mages instead! Having multiple versions of these files W ILL result in confusion and irregula r resul ts.

You need to learn how to set these parameters for your particular needs, using the epar edit parameters command. After y ou h ave f futorial out the table with your v alues, c ompare those values w ith an instructor’s cop y of the datapars listing to s ee y our values are reasonable.

There are other compression algorithms such as gzip that may be more effective, irwf which we have used from time to time. Rev iew these steps and consider wh ether or not they se em reasonable.


Irac are getting set up to determine param eter values for the task datapars. More time would have to b e spent e xamining the images. This is the standard procedure for exiting the editor. You can name the output zero file whatever you want, but make sure its the same name you set earlier in the ccdproc parameter file, or edit the ccdproc “zero level calibration image” parameter later to match this name.

ASTRO IRAF TUTORIAL Exercise 2 – Christopher Stubbs – Science de la nature

If only a few stars w ere selected, then perhaps s ome of the parameter v alues need to be a djusted. There i s probably more than one reason.

You can convert files one by one, itaf use lists as input and output. Bring up the help page for display. Compare your overall results w ith this diagram. Ea ch of the psf stars is scaled according to its aperture magnitude estimate, the weighted average is then fitted with a suitable analytic function, and a look- up table computed of the residuals interpolating between the remainder value for each pixel.


The computer then asks for an output name. Use imdelete on image files. The computer will the extract two files from the original FITS file, the image header, which will be named myimage. For observations of a globular cluster w ith expo sure times and bandwidths of the filters roughly equalw hy m tktorial w irar expect more stars in the v isual bandpass irraf the blue?

The analytic functions used are chosen from bivariate Gauss ian, Mof fat or Lorent z functions or you can set it to auto and it finds the best. Use rfits to make sure all your dark frames are in IRAF format. You may want to drag the icon for applications you use frequently like Terminal.

You should now have three windows. Since we w ill be graphing the visual magnitude against the B-V color, what we need to have is the same stars in both lists, and hope fully lots of them. Using the command is simple.

Once you h ave a CMD that y ou are satisfied with, print it and attach to this sheet. You can make two files, one containing the FITS file names and one containing the output names. You should, for deeper unde rstanding, try so me o f y our own values for data m in, datamax, etc. Here is a recently published CMD of M If you’re converting lots of files, which is usually the case, IRAF lets you take lists from a data file.