IRAF V Tutorial/Exercise – Introduction to PSF Fitting and DAOphotName:_________________________________________ Due Date:__________Score ________ / 40IRAF V Tutorial/Exercise – Introduction to PSF Fitting and DAOphot1. <10 pts> Fill in the following table with the values for 5 stars from each of the B and V images for use later in the task daofind.V Filter (m920004)x y Sky mean Sky sigma FWHMpsf CountsAverages:B Filter (m920006)Averages:2. <5 pts> Edit datapars. Enter in this table both the values you got from your measurements and the values you will actually used after comparing your values to those on the instructor (on-line) list. Remember: We are working with m920004 first and will come back to this table when you get to m920006.V Filter B FilterYour initialvalueValue youusedYour initialvalueValue youusedfwhmpsf fwhmpsfsigma sigmadatamin datamindatamax datamax1/13/19 13. <3 pts> What values do you think are appropriate for: photpars.apertures: __________ fitskypars.annulus: __________ fitskypars.dannulus: __________4. <2 pts> What values for the FWHM did psf determine? V filter __________ B filter __________5. <5 pts> Compare the photometry in this exercise with those of IRAF IV for the following stars and comment on the results, giving explanations for any discrepancies (say, of 0.2 magnitudes or more).Star ID(IRAF IV)X(approx.)Y(approx.)V BIRAF IV IRAF V IRAV IV IRAF V681318206. <2 pts> Run the match program so that you have 2 lists of stars: a list of those stars in the V filter that have matches in the B filter, and a list of those stars in the B filter that have matches in the V filter.7. <3 pts> Create the color-magnitude diagram for your results using your favorite plotting program. Instructions are given on a separate sheet for using IDL and SuperMongo.Show your graph to your instructor before printing or before emailing. If your results are way off base, then you may have to go back, modify some of your parameters or check to make sure all parameters are set correctly (usually the problem), and redo the photometry. Once you have a CMD that you are satisfied with, print it and attach to this sheet (alternatively, your instructor or TA may just have you send the postscript file).2QuickTime™ and a decompressorare needed to see this picture.A. Ruelas-MayorgaandL. J. Sanchez Revista Mexicanade Astronomay Astrofisica, 41, 507–522(2005)8. Here is a recently published CMD of M 92, with the major regions identified. Compare your overall results with this diagram by answering the following questions:a. <1 pt> First, estimate on which part of the diagram the stars from this exercise lie. Indicate your guess clearly on this image. (It will help if you adjust the X- and Y-axis scales of your graph to match this figure.)b. <2 pts> Second, there is probably an offset in V and in B – V between your CMD and this one. Give 2 reasons why this may be.c. <2 pts> Why are there so many stars in this diagram that are scattered and do not lie on the main-sequence or the sub-giant, giant,or horizontal branches?(continued on the next page)39. <5 pts> Using good writing style, summarize in general terms the full process you experienced here.Perhaps describe the problems you had and what you learned from your errors. Also, maybe include suggestions for future students of DAOphot. Feel free to type your essay and attach to this