Some simple functions in IRAF. and how to flatten frames

Transcription

1 Some simple functions in IRAF and how to flatten frames

2 On the work stations in the computer lab we will set up the standard Image Reduction and Analysis Facility (IRAF) for each user by having each user type these commands in a Terminal window. (Here <cr> is a carriage return.) cd <cr> mkdir iraf <cr> cd iraf <cr> mkiraf <cr> Here you are prompted for a terminal type. You must type in the letters xgterm <cr>

3 We will want to edit one line of a file called login.cl which will now exist in your iraf subdirectory. The line should read set stdimage = imt2048 Once you save the new version of login.cl with an editor, you start up IRAF by typing the command runiraf <cr> This will pop up an xg-terminal window and after some delay an image display window (DS9/SAOImage). IRAF commands are entered at the > prompt in the xgterm window.

4 Typing the? At the IRAF prompt will give a list of packages that exist at that level of the system. If you type Ø noao Ø imred Ø ccdred You will be at the right place to flatten some frames. To back up one level the command is Ø bye

5 A number of useful linux commands work from the IRAF prompt such as pwd cd (print name of working directory) (change directory) If you ve created an astr320 subdirectory and put data files into a subdirectory of that called jan6, you can set your default directory within iraf by typing the following at this point in the xgterm window at the > prompt. Ø cd.. Ø cd astr320 Ø cd jan6

6 You could see all the files in that directory by typing Ø dir Try displaying one of the FITS files like this: Ø display ccd127 1 This should display the image ccd127.fits. The header information of that file can be displayed doing this: Ø imhead ccd127 l+ The last two characters are a lower case L and a plus sign.

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8 Note the parameters OBJECT, UTSTART, FILTER, EXPTIME (exposure time), and AIRMASS. You could make a text file containing the values of these parameters For all the FITS files in the directory by doing this. The output will be put into a text file called a.log Ø hselect *.fits $I,object,utstart,filter,exptime,airmass yes > a.log Such a log file may have been provided with the data files that you have in the directory. This is very useful for knowing which file(s) you are working on.

9 A CCD chip contains one to several million picture elements (pixels). They have different sensitivity. To flatten your data frames involves: 1) creating a master bias frame (using exposures of zero seconds) 2) creating a skyflat or a domeflat frame for each filter you observed with 3) applying the master bias frame and the appropriate flat frame to all the data frames, filter by filter

10 Say you took 10 exposures of zero seconds before observing for the night, and these are files ccd037.fits through ccd046.fits. One creates a little text file (named, for example, zlist, containing these names). This is done in a Terminal window with an editor. ccd037.fits ccd038.fits ccd039.fits ccd040.fits ccd042.fits ccd043.fits ccd044.fits ccd045.fits ccd046.fits

11 Two parameters relevant to the CCD camera used at the Las Campanas 1-m telescope in 2012 are the gain ( = 2.5 electrons per analog to digital unit) and the read noise of 6.5 electrons. We will need these soon enough. But first we must turn off some functionality in a program called ccdproc. After starting up IRAF Ø noao Ø imred Ø ccdred Ø epar ccdproc

12 epar and the name of some program allows you to inspect and change parameters. We want to set all but one of the yes/no switches from fixpix to scancor to no. This we do with the up/down arrow keys and by typing no a lot. When you re done changing these parameters in ccdproc, you exit by typing :q

13 > :q

14 Now we want to use the IRAF program zerocombine to combine the bias frames. We will create a file called Zero.fits by average-ing the 10 files specified in the file zlist. The FITS header parameter ccdtype for these images is set to the word zero.

15 Note that we have set the read noise to 6.5 and the gain to 2.5 electrons/adu. > :go

16 Next we want to create a V-band domeflat frame and a B-band domeflat frame. These images were obtained by shining a light on a bit white screen in the inside of the dome during the daytime with the dome closed. Say there is a file dv that contains the V-band domeflat images: ccd0023.fits ccd0024.fits ccd0025.fits ccd0026.fits ccd0027.fits ccd0028.fits ccd0029.fits

17 At this point we do want to subtract the master bias frame from the domeflat images, so we have to set couple switches in ccdproc. We set zerocor to yes and set the name of the master bias frame to Zero > epar ccdproc

18 > :q

19 Next we use the program flatcombine. > :go will produce V-band flat file domeflat_v.fits

20 We can investigate many things with the iraf program imexam. Individual options are: l c r e s make a plot that give a horizontal cut make a plot that gives a vertical cut radial profile of a star 2-D contour of a star 3-D looking contour of star/galaxy

21 Plots made with imexam using the c option (above) and the l option (below). The file is the V-band domeflat file make from 7 images taken on 6 Jan 2012.

22 Of course, we want to make a file containing the list of B-band domeflat images (db) and produce a B-band domeflat called something like domeflat_b.fits. Finally we are ready to flatten the V-band data frames and the B-band data frames. Say we have made a list of V-band data files and called it vlist. Then we would use ccdproc as shown on the following slide. We have set images flatcor to yes and flat to domeflat_v

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24 We need to create a skyflat or domeflat file for each of the filters we observed in (for which we are going to do subsequent analysis). So now we would something like blist and domeflat_b to process the B-band images. It is a good idea to keep a completely unprocessed set of files you are working on, as one can mess up the trimming, bias correction, and flattening.