Deutsch IMG Library

The following is a listing of the entire contents of this library for IDL. Click on an individual procedure name to view its header and source code. This listing is a shortened form of the much longer entire library help file. This may be handy for text searchs, be beware that some of these are huge and may take a long time to load or even crash your browser.

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List of Routines

• A10READ Compare coordinates of stars in a GSC (gsclist) file and a USNO-A1.0 (a10list) file.
• BINARIES A sample program to fool around with binaries star systems
• BLACKSKY Changes current color table to white on black.
• BSCENTRD Compute "center of mass" centroid coordinates of a stellar object. This procedure is considerable slower than the Astronomy libraries' CNTRD procedure, but yields much better results for small "BAD STARS", i.e. small scruffy objects which don't necessarily have a good shape. It also avoids the CNTRD problem of ignoring a small star next to a much brighter one even if the exact coordinates are supplied. Results seem to be of comperable accuracy (based on comaprisons of residuals when transferring solutions to higher resolution images) on bright sources and can measure many sources CNTRD is not capable of. Careful study of results of this algorithm versus other popular ones still needs to be done. In general,
• CALC_A Returns the extinction of the supplied wavelength and E(B-V) using the Seaton Extinction curve through the UNRED procedure.
• CALC_ZDHA Calculate Zenith distance and Hour Angle and Azimuth given local standard time, latitude, longitude, ra, and dec.
• CLEANEXAMINE This procedure is designed to aid in the examination of the results of of a run of IMGclean, although there are other uses for the program. In addition to "examining" the difference between the two images, one can edit and replace to remove CR's that IMGclean missed and also fix mistakes where IMGclean damaged a star.
• DELAST Deletes all astrometric information from a header. Mainly useful for deleting screwy "astrometry" that IRAF delights in fouling up the header with (e.g., "PIXEL", "SYSTEM", etc. CTYPEs)
• DIAGFIND This procedures finds all (or first) star(s) within 0.1 magnitudes of a cursor click on the CM diagram output of diagram.pro and prints out relevant lines and draws arrow to object.
• DIAGMARK This procedures finds all stars within radius pixels of x,y and draws a line to it on the output window of diagram.pro
• DIAGRAM Generate a snazzy color-magnitude diagram with a variety of options and input formats. Everything is controlled via a self-documenting parameter file instead of keywords or parameters
• DOCIRCLE Read file
• DOFIND Procedure: DoFind,filename This procedure through the output of DoPHOT in the COMPLETE format only for an object of the specified coordinates dofind,filename,xc,yc,srchrad
• DOSTAT Procedure: DoStat,filename This procedure returns statistics of the output of DoPHOT in the COMPLETE format only! The number of different object types are counted up and the results are printed to the screen.
• EXTCAT_AC2000 Extract a region out of the AC 2000 CD-ROM.
• EXTRAC The EXTRAC function returns as its result any rectangular sub-matrix or portion of the parameter array. When parts of the specified subsection lie outside the bounds of the array, zeros are entered into these outlying elements.
• GSCA10COMP Compare coordinates of stars in a GSC (gsclist) file and a USNO-A1.0 (a10list) file.
• GSCTAB2LST convert a FITS table from IRAF 'regions' task into the ascii list like that outputted by the VAXes. -Deutsch 4/3/94 Call> gsctab2lst,inputtab,outlst e.g.> gsctab2lst,'47tuc.tab','47tuc.gsclst'
• GSC_READ This procedure reads a ST Guide Star format file and returns the stars in an array of structures with fields ID,StrID,RA,DEC,MAG.
• HLINES Print out some optical Hydrogren lines.
• IMGCLEAN[1] This procedure is designed to remove cosmic ray hits (CRs) from an image, especially WFPC images. The procedure's effectiveness varies from image to image. Often, it does an excellent job, but sometimes the operational parameters must be modified (via keywords) to tweak the performance of the software. It should not be assumed that this procedure will automatically do a good job! Keep a close eye on before and after images. Occaisionally, a faint star gets obliterated, especially if there is a cosmic ray around 3 pixels from it. Naturally, this procedure is only recommended when a CR split is not possible, as that will often yield better results.
• IMGCLEAN[2] This procedure is designed to remove cosmic ray hits (CRs) from a image, specifically WFPC images. The procedure was originally written with one image in mind and was made to work well with that image. Its effectiveness for other images varies. Often, it does an excellent job, but sometimes the operational parameters must be modified (via IDL2 kerwords) to tweak the performance of the software. Still in a somewhat primitive state, this procedure will be improved beginning June 1992. Suggestions welcome to SCIVAX::DEUTSCH.
• IMGMRG ***************************************************************************** ******* PROCEDURE: IMGMRG ***************************************************************************** *** DESCRIPTION: *** This procedure will combine two images (mainly designed for GSSS use) *** that individually do not produce a nice centered image. In other
• IMGMRG_CALL *************************************************************************** *** This procedure is designed to allow you to edit the variable inputs of *** the IMGMRG procedure more easily. The the IMGMRG program itself for a *** more detailed description of the variables. *************************************************************************** pro combine,dummy
• IMGPASTE This procedure takes a portion from SRCIMG and pastes it into DSTIMG. This is originally intended for replacing a star or other goof that IMGclean has made. DIAM should usually be odd for a symmetrical replacement. If DIAM is even, the extra pixels will spill over to the lower x,y pixels.
• IMGPUT Paste a small image into a larger one with edge-clipping handling
• IMGREAD Open an SDAS/GEIS file and read the image into a data array of appropriate type and read the header into a string array. This procedure was designed to be more versatile than the STRD procedure and to be specifically useful to WF/PC and FOC data, as well as all other GEIS images. IMGread supports multiple GROUPS (i.e. in STSDAS
• IMGTEXT This procedure writes text onto the current graphics window. Its purpose is to provide large, nice looking text with which to annotate images suitable for publication, since the Hershey Vector fonts often fall short of good publication quality at large sizes. The drawback is that, since they are bitmapped fonts, only certain fonts and sizes are available. However, by using the FONTCNVT utility, more can be
• IMGUNDER Display image in same area as last plot.
• IMSCL IMSCL is similar to BYTSCL except is uses a half-linear and half-logarithmic Call> imscl,img-min,0,max,linearmax,top= e.g.: imscl,img-300,0,10000,500,top=48 The example call produces a linear stretch of 300-500 for half of the dynamic range, and a logarithmic stretch from 500-10000 for the other half of the dynamic range. This allows fine detail visible at low levels
• OBJCENOM Compute "center of mass" in a box with the specified center and radius. This procedure is suited for irregular objects with multiple peaks that that would normall confuse a steller centroider.
• QAPER if (not silent) then print,'(inner,outer) radius=',vect(skyaper)
• QPHOT PCPsf=[0.151,0.189,0.227,0.253,0.276,0.302,0.324,0.344,0.357,0.370] ; derived from Tiny Tim B PC Psf
• QUICKSPLIT QuickSplit This program is supposed to be a real quick and dirty CR-split program IDL> quicksplit,image1,image2,[mindiff=,ignorelev=] image1 and image2 are the two images to be split mindiff= is a keyword for the minimum difference considered to be a CR ignorelev= is a keyword which specifies the level above which CR's are
• QUICKSPLIT2 QuickSplit2 This program is supposed to be a real quick and dirty CR-split program IDL> quicksplit,image1,image2,[mindiff=,ignorelev=] image1 and image2 are the two images to be split mindiff= is a keyword for the minimum difference considered to be a CR ignorelev= is a keyword which specifies the level above which CR's are
• RADPROF[1] Plot a radial profile of a (stellar) object and overplot a gaussian fit. Also prints out some fit parameters, e.g. Sky, FWHM, Max, Total.
• RADPROF[2] Plot a radial profile of a (stellar) object and overplot a gaussian fit. Also prints out some fit parameters, e.g. Sky, FWHM, Max, Total.
• SKYCALC print,vect([AX1*.1,AX1-AX1*.1,i*.01*(AX2*.9)+AX2*.05])
• SKYCHECK1 radec='06 01 47.287 +23 24 54.16' ; 0558+234 radec='05 11 32.621 +38 09 13.31' ; 0508+380 radec='11 19 00 +30 00 00' ; WD1 radec='14 00 00 +30 00 00' ; WD2 radec='15 13 22.8 -09 10 08' ; GRISM C star (and odd spec) radec='08 42 4.456 +33 42 58.83' ; KUV 08389+3354
• SKYHORIZ This program is designed to show how a given object (i.e. RA, DEC) tracks across the sky during a specified night. The program gives two forms of output: 1) a table listing Zenith Distance, Airmass, Hour Angle, UT, local time, and positions of the moon as well during a specified night; and 2) a plot of how the object and the moon track across the sky. Time interval is always 6pm to 6am local time.
• SKYLINE122 print,'Skyvalue=',strn(av1),', RMS=',strn(rms1)
• SKYPOS[1] This program is designed to show how a given object (i.e. RA, DEC) tracks across the sky during a specified night. The program gives two forms of output: 1) a table listing Zenith Distance, Airmass, Hour Angle, UT, local time, and positions of the moon as well during a specified night; and 2) a plot of how the object and the moon track across the sky. Alternately, the data can be printed for a single specified UT.
• SKYPOS[2] This program is designed to show how a given object (i.e. RA, DEC) tracks across the sky during a specified night. The program gives two forms of output: 1) a table listing Zenith Distance, Airmass, Hour Angle, UT, local time, and positions of the moon as well during a specified night; and 2) a plot of how the object and the moon track across the sky. Alternately, the data can be printed for a single specified UT.
• SKY_VALUE p - your image bitpix - number of bits/pixel percent - percent of borders to ignore in the computation sky - estimate sky value maxval - estimated upper value Modified May 2, 1991 DJL added percent parameter (which used to be hard
• STARCHCK print,'Center of ',vect([xc,yc]),' found after ',strn(i),' tries..'
• STARCHCK122 print,total(tst),n_elements(tst) print,tst
• STARFIT Routine to fit a 2D gaussian to a stellar object
• STRNSIGNIF Convert a number to a string with a fixed number of significant digits. Similar to strn(), this function converts a number to a string, but, unlike strn(), with a fixed number of significant digits.
• SUNRISESET ct2lst,lst,-1.0*longitude,timezone,jul_date-0.5d + UTs(j)/24.0d
• UJCHART UJCHART - an example reading/plotting program for use with the UJ 1.0 astrometric catalog. -Deutsch
• UNRED Correct a flux vector for interstellar extinction based on the the results of Cardelli, Clayton, & Mathis 1989, ApJ, 345, 245
• WAVG quicky weighted average results=wavg(array,weights,/weights) results=wavg(array,errors,/errors)
• WFPC2LIST No formal header yet. See the documentation in http//www.astro.washington.edu/deutsch/apoinfo.html
• WFPCMRG This procedure is designed to load all four chips of a WF or a PC and combining them into one 16 bit INTEGER image. The chips may be trimmed or left whole. Sky subtraction options are available. This is desgined for WFPC I images only!
• WHITESKY Changes current color table to black on white.