Regim Stacking Software

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Regim user handbook state 17.12.2011________________________________________________________________________

USERS MANUAL


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INDEX

1 What is Regim?

2 Supported file formats3 Installation prerequisites

4 Installation and start

4.1 Starting under Windows Xp, Vista, Windows 7

4.2 Starting under Linux

4.3 Starting under Mac OS X

4.4 More processor systems

5 Menu descriptions

5.1 The File menu

5.2 The Edit menu

5.3 The View menu

5.4 The Combine menu

5.5 The Color menu

5.6 The Preprocessing menu

5.7 The Tool menu

6 Presettings

7 Calibrations of raw pictures and Preprocessing

7.1 Preprocessing

7.2 Calibration

7.3 Generate Masterdark

7.4 Generate Masterflat

7.5 Defect list8 Deblooming

8.1 Removing of Blooming in opened pictures

8.2 Removing of Blooming in several pictures

9 Aligning of pictures

9.1 To align opened Deep Sky pictures

9.2 Aligning of many Deep Sky pictures

9.3 Aligning of opened sun pictures or moon pictures

9.4 Aligning of many sun pictures or moon pictures

10 Adjusting background

10.1 Adjusting of background of opened pictures

10.2 Adjusting background of several picture files11 Geometric Functions

11.1 Double picture size

11.2 To turn pictures around 90

12 Combination of single pictures

12.1 Average of opened pictures

12.2 Mean of many pictures

12.3 Median combination of opened pictures


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12.4 Median combination of many pictures

12.5 Sigma combination of opened pictures

12.6 Sigma combination of many pictures

12.7 SD-Mask combination of opened pictures

12.8 SD-Mask combination of many pictures12.9 Maximum combination of opened pictures

12.10 Maximum combination of many pictures

12.11 Subtracting of pictures

13 Gradient and Offset

13.1 Add Offset

13.2 Remove gradient

14 Color manipulations

14.1 RGB pictures put together to set

14.2 Manipulate Color canals

14.3 Monochrome changes14.4 Automatic Color calibration with star color

14.5 Manual Color calibration

14.6 Change RAW pictures in RGB

14.7 NoLiGCRA

15 Blink Comparator

15.1 Blinking of opened pictures

15.2 Blinking of many pictures

16 Visualization attitudes

16.1 To place black point and white point

16.2 Black point and white point for all pictures

16.3 Set Black- and White points automatically16.4 Picture Zoom

17 Editing Pixels

17.1 Notices

17.2 Changes

17.3 Navigating

18 Astrometrie (Plate Solving)

19 Indicate Histogramm

20 The status bar in the picture window

21 The status Window

22 Fit - Header indicate

23 General References for the procedure


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1 What is Regim?

Regim is a software tool that eases the processing of astronomical photos and recordingthat are taken with the digital single-lens reflex (DSLRs) or CCD cameras

Regim is not l like complex picture processing systems such as Adobe Photoshop rather,it a supplements the other processing systems .It simplifies steps that are used inastronomical receptions. These are especially the calibration of the raw pictures (Dark-and Flat field correction), as well as the aligning of the single pictures to each other andthe combination to a general view.

The successful installation use and results are at users risk.

Regim is freely available and may be used freely in unchanged form. However, a lot ofeffort is put in the program.The regular users of this program are encouraged to makesmall contributions towards development costs or contribute in the programming efforts.

Your questions are welcome. You can reach me through my e- mail.

2 Supported file formats

Regim supports the following file formats:

TIFF (uncompromised!) RGB/monochrome with 8 or 16 bits per canal

JPG files

FITITs files monochrome/RGB/Raw.

RAW files of different digital cameras (only reading)

Regim uses (Jrawio) for the reading-in of RAW data files. I sincerely thank FabrizioGiudici and all those who contributed to (Jrawio)


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3 Installation prerequisites

Regim is written completely in java and should therefore run on every platform, whereJava runtime environment (JRE) version 1.6.0 or higher versions are installed. It is testedfor Winxp, Windows 7, and Suse Linux 11.4 with JRE 1.6 and 1.7. The JRE pathattributes should be set like the path attributes of the runtime libraries.

For the processing of large pictures, Regim requires good memory. The main memoryshould not be measured therefore very concisely allocated. At least 512 MB should beavailable. 1 GB or more is to be recommended strongly

For processing larger pictures, Regim requires good allocation of memory. The main

memory allocation should not be too precise or short.

4 Installation and start

Download/ unzip the file regim.zip on your hard disk. In the directory Regim, you find afile Regim. jar, regim.properties as well as a file regim. cmd (for Win XP, Vista, Win 7)and a file regim. sh (for Linux and Mac OS X).

Reference: For Linux the flag export to file must bechecked/ set. (see the chmod command)

Reference: Java runtime environment must be installed

on your computer. One can download thisunder http://www.java.com (for the version1.6.0 of the runtime environment) if notinstalled. At present, I cannot yetrecommend the use of OpenJDK.Important for user of 64bit-Windowssystems: If you try to download the javaruntime environment of above-mentionedsite with Firefox one will apparently get the

32bit-Version automatically. Therefore inorder to download the 64bit-Version of thejavas runtime environment it is advisable touse the Internet explorer.

In the Standard moderate Regim st with upper storage limit of 1024MB and this is shownin the start. This appears in the batch file (regim. cmd, and/or regim. sh) over theparameter -Xmx1024m. If your computer has storage more than 1024MB, it is


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advantageous to set the storage allocation to the higher side. However it should be on thelower than the actual available storage. For systems with sufficient storage (> 4GB)Batch files are available in Regim to allocate 2GB memory. (regim2gb.cmd andregim2gb.sh).

4.1 Starting under Windows Xp, Vista, Windows 7

Change to the Windows explorer into the directory, in which you have Downloaded/unzipped Regim. Double click now on the file regim. cmd.

4.2 Starting under Linux

Open a terminal window and change into the directory, in which you have Downloaded/unzipped Regim. Now input regim. sh.

4.3 Starting under Mac OS X

Open a terminal window and change into the directory, in which you have Downloaded/unzipped Regim.. Now input sh regim. sh.

4.4 More processor systems

If your system controls several processors and/or processor kernels, please insist yourefer 6.

5 Menu descriptions

5.1 The File menu

Open Opens a picture file in that opens FIT, TIFF-, RAW- or JPG format. The pictureis represented subsequently in an own/particular window.

Save as Stores the picture as TIFF-, or jpg file in theuppermost picture window.

Save as FIT IT Stores the picture in the uppermost picturewindow as a FIT file. (Gradations)

Save as Splited FIT IT Stores the picture in the uppermost picturewindow as 3 separate FIT files depending onthe RGB factors.


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Close all Closes all open picture windows.

Preferences Opens the dialogue box for pre-settings.

Exit Exits the program.

5.2 The Edit menu

Register/ index Arranges several opened Deep Sky pictureson each other. Recommended only for afewer number of pictures that require largememory.

Register Files / Index Files Arranges several Deep Sky picture files on

each other. Recommended for a largenumber of pictures.

Register Sun / Index Sun Arranges several opened sun or moonpictures on each other. Sun and/or moonmust be complete in the picture.Recommended only for a slight number ofpictures, that require large memory.

Register Sun Files / Index Sun Files Arranges from several sun/moon picturefiles on each other. Sun and/or moon must

be complete in the picture. This isRecommended for a larger number ofpictures.

Remove Blooming Removes Blooming-spikes in bright stars ofan opened picture if the picture was receivedwith a CCD camera, that does not controlAnti-blooming.

Remove Blooming f. Files Removes Blooming-spikes in several picturefiles.

Normalize Background Adjusts the background of opened picturesto each other.

Normalize Background. in Files Adjusts the background in several picturefiles.


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Upsample 2x Doubles the width and the height of anopened picture.

Rotate Left 90 rotates the picture in the uppermost picture

window 90 anticlockwise.

Rotate Right 90 rotates the picture in the uppermost picturewindow 90 clockwise.

Add Offset Adds an Offset to the picture.

Remove Gradient Removes from the picture brightness orcolor gradient.

5.3 The View menu

Equalize visualization Adjusts the visualization attitudes (black-and-white points) for all open pictures to thecurrent (uppermost) picture.

Auto stretch Carry out an automatic adaptation of thevisualization attitudes (black-and-whitepoints) for the uppermost picture window.

Blink This causes blinking of just opened pictures mutually.

Blink Files It causes blinking of arbitrarily openedpicture files.

5.4 The Combine menu

Blend / aperture Arranges several opened pictures under theconsideration of weighting factors.

Blend Files / Aperture Files Arranges several picture files.Recommended for a larger number of

pictures.

Median CombineThe combine menu combines the openpictures files by means of median formationconsidering weight of important factors.


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Median Combine Files Combines several picture files by medianformation. This is recommended for a largernumber of pictures files.

Sigma Combine Combines several opened pictures by meansof Sigma- exclusion procedure.

Sigma Combine Files Combines several picture files by means ofSigma exclusion procedure.

SD-Combine Combines several opened pictures by meansof SD Mask- combination.

SD Combine Files Combines several picture files by means ofSD-Mask-combination.

Maximum Combine Combines several opened pictures by meansof maximum combination.

Maximum Combine Files Combines several picture files by means ofmaximum combination.

Subtract Files Subtracts the picture in the uppermostpicture window of several picture files.

5.5 The Color menu

Multiply Channels Multiplies the single color canals (RGB)with a value.

Combine Channels Combines three gradation pictures to a RGBcolor picture.

Split Channels Splits a RGB picture into three separatesingle color canals.

Monochrome This menu converts a RGB color pictureinto a black & white picture.

RAW Debayering this menu converts a camera-RAW-pictureinto a RGB color picture.


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Man. B V Color Calibration Enables the manual color calibration of apicture on the basis of the color index (B V)of a star.

Auto B V Color Calibration Enables the automatic color calibration of apicture on the basis of the color index (B V)of a star.

Non-linear g. c. retrieval Permits a linear contrast adaptation of a

RGB color pictures without the color ratios.

5.6 The Preprocessing menu

Setup defect list Open the dialogue for designing andchanging of defect lists (Split-/Pixel defect)of monochrome CCDs.

Setup darks A Master-dark file is generated out ofseveral single files. The files are combinedat the same time by means of mediandevelopment.

Setup flats A Master-flat file is generated out of severalsingle files under option consideration for

Dark-frames (for the Flats). The files arecombined at the same time by means ofmedian development.

Pre-processing. The complete data reduction (Dark- and Flatfield correction, repair of column defects,De-blooming, aligning and combination) iscarried out for several picture files.

5.7 The tool menu

Plate solve Carries out a Plate solving. It determines theexact coordinates, that standard and theorientation of the picture and in which fitheader is it written. That eases theAnalysis of the picture for example withAladin.


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6 Pre-settings

The preferences for pre-settings are in the file menu and the following dialogue boxappears for pre-settings.

Number of CPUS One can choose the number of the CPUsthat control the system. If, Regim is set fortwo or more processors this enables it forparallel processing of several threads. Thishelps to execute the written scripts faster.With this adjustment the system worksquicker. For a computer with 2 dual CoreCPU one should enter 2 in the dialogue box.If, your system has more processors and/orkernel, then select the correspondingnumber. (for Core 2 Quad for example 4).

It is recommended to enter the value 2 in theabove dialogue box for computers with onekernel processors


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Use proxy this adjustment is important if one isworking in large area networks (automatic

color calibration).If your computer requiresa proxy for the Internet connection,(frequently in larger company networks),select this option from the fields and fillboth the fields. In a home network, theywill require no proxies as a rule.

Proxy host Enter the name or the IP ADDRESS of theproxy in the field.

Proxy port Enter the number for proxy-port.

7 Calibrations of raw pictures and Preprocessing

7.1 PreprocessingPreprocessing function in the Preprocessing menu serves to calibrate around severalpictures and to carry out appropriate further basic preparation steps. This is a verypowerful function. One can write a single script for this.

Calibration of raw pictures (Dark- and Flat-field correction, correction of pixel

defects, De-bayering of RAW pictures)

De-blooming of pictures Align pictures on each other (registration)

Preview of the pictures.

Combine pictures for a general view.

Following dialogue appears:


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There are five check boxes, with which one can activate the scripts for:

1. Do Calibration Activates the calibration function

2. Do De-blooming Activates the De-blooming function

3. Do Register Activates the registration function (aligning)

4. Do Preview Activates the preview of the single pictures before thecombination. Single pictures can be sorted out here.

5. Do combination Activates the Combination function

To alternate between these functions one can name these function. The function can beactivated by a combination of capital keys. The dialogue-box allows data processing ofdata by dragging and dropping the four lists or choosing with the four buttons in the rightin the dialogue box.

Images:


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This list is for processing images. The datatopmost in the list is in the ggf. in the Masterfile registry. For this reason you see this datafirst in the list and all the other data after this

data.

Darks: The list for the Dark-frames. Here you can add several single Dark-frames or alsoalternatively an already existing Master-darkfile.

Flats: The list for the Flat-frames. Here you can add several single Flat-frames or also

alternatively an already existing Master-flatfile.

Flat Darks: The list for Dark frames like the Flat frames.

If you have made all the settings, press OK. The processing will start now and a newdialogue appears that indicates the progress. The results of the processing are stored inbetween respectively with corresponding file name. If you select the function docombination, the picture combined ready should be represented after conclusion of theprocessing. You can store this then.

7.2 Calibration

Choose the Preprocessing function for calibrating pictures. The selected raw pictures arecalibrated by means of the selected Darks and Flats at the same time. Additionaladjustments can be done on the main Calibration in the selectedPreprocessing dialoguebox:


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Repair defects Here you can determine whether pixels aresupposed to be repaired-/column defects ofthe CCD Sensors on the basis of a defectlist. This function can be used only for FITSmonochrome data. If the function isactivated, you can select an available defectlist.

Files are RAW: this menu tells how the color calibration ishandled by the program for the pictures inthe raw format. These can be RAW picturesof a DSLR, or RAW pictures of a colorCCD as RAW-FIT IT-files.

Standard DSLR : For DSLR RAWs. The pattern of the Bayermatrix for the Debayern of the pictures isdetermined automatically.


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Custom For color-CCD-pictures or DSLR RAWswhos Bayer matrix is not recognizedautomatically both check boxes to the rightbecome active.

First row contains red pixel Determines whether the first line contains aRAW picture red pixels.

First pixel of first row green Determines whether the first pixel of thefirst line is green. Both parameters mustcorrespond to Bayer matrix set for thecamera. The mistakes / values for the Ggf.

can be corrected by searching the attributesgiven in Annexure-A-for some of thecameras.

Stretch RAW to 16 bits: Calibration for pictures shot with mirrorreflex cameras normally is for 12 bit

but 14 bit is included in this function. Butdebyernig may be stretched

to 16 bits.In general, it is recommended to activate this function because otherwise the

pictures appear very dark. If you activate

the function, you yet should determinewhether the RAW pictures concerns 12 or14 bits files. 12 or 14 bits files.

Color correction scalingColor correction scaling The pictures that have dark color scaling can

be corrected using the color scale correctionchoosing a single color canal. The scalingcorrection is decided in percent.

Color correction offset This function indicates the Offset for the

color correction. The input values are addedto the respective color canals.

Auto scaling If, this function is selected the necessaryColor correction is scaled automatically.

Auto offset If, this function is selected the necessaryOffset mode is set automatically.


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7.3 Set-up Master-dark file

With the function SetupDarks in thePreprocessing menu one can generate Master-darkfile. All the files selected for processing appear in the file selection box. The finalMaster-dark is indicated subsequently appears in a new window and can be stored. Thiscan be used later during Preprocessing in place of the single Darks. Master-darksgenerated out of DSLR- Raw have a file extension.fit".

7.4 Set-up Master-flat file

With the function SetupFlats in thePreprocessing menu one can generate a Master-flat,All the file selected for processing appear in the file selection box. Another dialogue boxfor belongs to Flat dark pictures. The final Master-flat is indicated subsequently in a

new window and can be stored. This can be used then later during Preprocessing in placeof the single Flats and Flat Darks. Master-flats generated out of DSLR- Raws have thefile extension .fit"

7.5 Defect list set-up

The option Setupdefect list is in thePreprocessing menu. The defect list can be set-upto repair fissure defects on a monochrome CCD installed chip.


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One can create a fissure-defect list for the different cameras set-on. To locate the exactcoordinate of the defective pixels/columns one can use theEditpixels function.One can use the defect list later in pre-processing in the main calibration during thecalibration and reparing the defects one can decide which data to keep and which is to beleft-out.


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8 De-blooming function8.1 Removing of Blooming in an opened picture

Remove-blooming is in the edit menu or alternatively in the pre-processing menu.

This function is to remove the blooming from the pictures shot with a CCD camera (e.g.S Big ST10XME) that doesnt have anti-blooming set-up for shooting bright stars.A dialogue box appears with three parameters:

Bloom limits: With this function one can determine thebrightness value, to search Blooming. Allvalues that are higher may need Bloomingadjustment. One should test a series ofpictures to select how high the value shouldbe, to score good results. The value can varyaccording to installed equipment and

admissible standards.

Interpolation width with this value one can fix the brightness ofthe interpolations interval upper & lower -for Blooming-spikes. The upper & lowervalues for the Blooming-spikes can be usedto calculate the new pixel value for thatBlooming pixel. One can tweak the values.According to me, values of 2 or 3 gives thebest results.

Star limit this value helps to determine with certainty,which brightness value pixel would belongto a star. The program uses this value as abench-mark to recognize if the blooming iswithin the parameters of that of a star. Theinterpolated values are then to be setsomewhat higher in order to retain thecharacter of that of star. This is so becausethe set limit would be considered todetermine if the bright spots -the pixelvalue- are stars. This value certainly should

be set distinctly higher than the value of thesky-back-ground contrast usually has.However, it should be set as low as possible.This value allows suitable adjustment to thepictures. However, before setting of thisvalue one must test a series of pictures todetermine what value should be set. Thisvalue is also important because, the right


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value set-in, acts as a filter where there is alot of variation in the in the picture contrasti.e. the bright spots and the spots that have alower intensity.

If one has to remove blooming from single pictures please choose pictures that arealready calibrated (at least Dark Calibration, see 7.3 References not found) or else itwould not be processed further.

Reference: After the De-blooming, the center of thestars appears somewhat darker than theedge. However, in the further processing ifthe brightness level is raised then the effectdisappears from the pictures.

8.2 Removing of Blooming in several pictures

With the functionRemove Blooming from Files one can remove blooming from severalpicture files. In the file selection dialogue-box that appears one can first of all select thepicture files. Subsequently a dialogue-box with three input parameters appears asdescribed already in the previous section. The processed files are stored with the PrefixDbl_in the same index.

Reference: This function is also available underPreprocessing.


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9 Aligning of pictures

9.1 To align opened Deep Sky pictures

To edit /align two or more pictures/ opened picture files please select the Registerfunction from theEditmenu. The following dialogue box appears.

Master frame one can select picture to align and align itlike another picture defined in the Masterframe.

Images to register here one can select the pictures that aresupposed to be aligned. Only the picturesthat you explicitly select out of this list areprocessed.

Number of star with this function one can determine howmany stars the algorithm uses. A lownumber means faster processing time andless storage consumption in the seeking ofthe passport model/ pattern under the stars.If, the number for stars is low, the accuracyis lower or under circumstances even


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insufficient. Then one should increase thenumber for the stars.

Transform Mode: This function allows the mode oftransformation. Currently it is Linear.

Star min. brightness: One can determine the brightness a starshould have, to be recognized as a star whilesearching the passport muster. If the value isset to 0.2 means that a star must have at least20 percent of the maximal brightness. Formost pictures, this is a good value to startwith. If necessary, this value must be

corrected by either lowering or setting thevalue higher. If Regim does not findsufficient stars to align one should set alower value, depending on the number ofstars in the picture, field and depth of thereception. The status window shows thecount of the stars detected. If, there are lessthan 20 stars in a picture, alignmentbecomes difficult. If the value is low, itincreases the time for searching or seek timefor stars. The value should therefore be

higher than that of background picture.

Star max. brightness: With this parameter, the upper limit ofbrightness is determined for the star to berecognized. Bright stars, that are satiated orshow Blooming, are not well suited forfinding a passport pattern. By means of thisparameter, they can be excluded out of thesearch. If the value is set to 0.8 it means thata star possesses at most 80 percent of themaximal brightness in order to be used for

the search. 0.8 is a good guideline to beallowed for most applications.

Search radius with this menu one can define a radiuswithin which one wants to search for a starif one finds bright clusters in a picture. Oneagain has to define a value for this. Thesuitable value depends on the Sampling of


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the pictures (arch seconds per pixel).Thisvalue can be found iteratively. In mostcases, a good start value is 15.

2x upsample If, this function is turned on, the pictures inthe folder/ directory become double in size.

With this one can further combine the pictures to achieve a precise solution whensometimes the pictures slightly staggeredagainst one-another.(Drizzling & Dithering)

Same scale If, the pictures are of the samescale/quality/parameters one can book-markthem, as same scale. (This is normally thecase, when the same device combination is

used for the reception/ pictures).

Bi-cubic interpolation with this function the Interpolation can beturned on or off. The Interpolation givesbetter results, however requires morecomputation time. Pictures that are"oversampled" may be ignored in the setrules for Interpolation. (Small pixels in longfocal length)

Normalize background with this function one can adjust the

background of the single pictures at thesame level of brightness. This is important ifthe single pictures are to be combined laterwith the Sigma- or SD procedure.

ClickRegisterin order to start the alignment process. The process may take longer timedepending on the size of the pictures and amount of the stars. The correctly processedpictures are shown in a new window.

Reference: If you want to align a larger number ofpictures, better use the function Register

Files.

9.2 Aligning of many Deep Sky pictures

With the function in the Editmenu one can align a larger number of pictures suitably oneach other. In the file selection dialogue that appears, one can select all Pictures to bealigned. Subsequently a dialogue box as described in the previous section of registrationappears. The processed pictures are stored with the PrefixReg_in the same index.


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Reference: This function is also available underPreprocessing.

9.3 Aligning of sun or moon pictures files that are open

The Edit menu has the function Register Sun. One can align/ overlay two or severalopened Sun or Moon pictures files (e.g. for an animation) suitably on each other. Theprocedure is similar to that for Deep Sky pictures.

Reference: For the alignment, the entire Sun or Moonrespectively must be portrayed on allpictures. The alignment of cuts is notpossible. The accuracy of the alignment isthought for the creating animations, however

not as a method of several receptions.

9.4 Aligning of many sun pictures or moon pictures

One can use the functionRegisterSunFiles in theEditmenu to align a larger number ofmatching pictures. A dialog box will pop-up that will show all the pictures selected foralignment.

10 Adjusting Background

10.1 Adjusting of background of opened pictures

One can choose Normalize Background to adjust background of the sky in pictures.This is helps if pictures are supposed to be combined together later with the Sigma or SD-Mask-method. Then these combination procedures usually work more efficiently.Following dialogue appears:

One can set/fine-tune give specification- for the sky -background pictures and use it as aMaster picture to be used in other pictures. One can mark every picture right selection-that one wants to use and make Master-file folder.

10.2 Adjusting background of several picture files


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With the function Normalize Background in Files one can adjust the backgrounddescribed in previous section and carry out assimilation for a whole series of picture files,without the files being opened.

11 Geometric Functions

11.1 Double picture size

Use the Upsample 2x in the Editmenu to double the width of the pictures. It uses bi-cubic interpolation to do this.

11.2 Rotate Pictures around 90

Use the menu functions Rotate in the Editto turn around the picture in the uppermost

picture window by 90

12 Combinations of single pictures

Reference: The combination functions are also availablein preprocessing menu.

12.1 Average of opened pictures

That average of several pictures improves the signal-intoxication-ratio. The picturesmust be aligned on each other and/or possess exactly the same size. The functionBlend

in the Combine menu averages two or several opened pictures. Following dialogueappears:

Frame One can select here pictures to average from.


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Weight One can mention here a weight for factor.The information of the relevant picture ismultiplied before adding with the weightingfactor and the entire sum divides through the

sum of the weighting factors. It takes intoaccount different exposure times of thesingle pictures.

Ignore black border during alignment, the pictures often developa black edge. When this option is selected,black fringe areas are not included into theaperture process. For example the blackfringe area of a picture is the mean over anarea marked with information of anotherpicture. The black edge does not go into the

average, but rather only the information isused in this area out of the other picture.

12.2 Mean of many pictures

The functionBlend Files in the Combine menu can be set to average a large number ofpictures. A file selection dialogue appears, in which one can select the pictures to beaveraged. The pictures to be aligned on each other and/or must possess exactly the samesize. Subsequently a window appears which indicates the averaged picture.

12.3 Median combination of opened pictures

The operation corresponds to the average of opened pictures. One should select Medianhere instead of the average.

12.4 Median combination of many pictures

The operation corresponds to the mean of many pictures. One should select Median here

instead of the average.

12.5 Sigma combination of opened pictures

The operation corresponds to the mean of opened pictures. The Sigma Exclusionprocedure should be selected here instead of the average. With the Sigma Exclusionprocedure, one can get the advantages of both the average and median combination andavoid the disadvantages. During combination process, the empirical standard deviation of


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the relevant pixels of the single pictures is calculated simultaneously for every pixel andonly such pixels requisitioned for an average development, whose values lie in a certaininterval. The interval results from the medium value the calculated standard deviationonce the Sigma value is indicated. One can exclude Cosmics, satellite traces or airplane

traces, while the "good" values are requisitioned to the average and contribute to a bettersignal/distortion-ratio.

After the combination, a window with the statistics is displayed. One can verify theresults. The Sigma value should be selected so that the percentage of the rejected pixels(Rejected) is small and nevertheless no runaways such as airplane traces etc. are seen inthe picture.

12.6 Sigma combination of many pictures

The operation corresponds of to the mean of many pictures. The Sigma exclusionprocedure should be selected instead of the average. The selected files in the dialoguebox combines with Sigma combination method. The Sigma value can be changed asrequired. The standard value is 1.8.

12.7 SD-Mask-combination of opened pictures

The operation corresponds to the mean of opened pictures. SD-Mask-combinationprocedure is selected here instead of the average. One can render the benefits of both theaverage and median combination and avoid the disadvantages. During combinationprocess, the empirical standard deviation of the relevant pixels of the single picture iscalculated simultaneously for every pixel and average is undertaken only if the standarddeviation does not deviate too strongly by the average standard deviation. Otherwise the


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medium value is used. The permitted deviation which is indicated results from that of theaverage standard deviation multiplied with the Sigma value. Cosmics, satellite traces orairplane traces excluded, while the "good" values are requisitioned to the average andcontribute to a better signal/intoxication-ratio. This procedure usually delivers the best

results.The results depend very strongly on the input Sigma value. The standard value is about1.8. A window showing the statistical data is indicated after the combination.

12.8 SD-Mask-combination of many pictures

The operation corresponds to the mean of many pictures. SDMask- combinationprocedure is selected instead of the average. SD combination processes the selected fileswhich appear in the dialogue box. The Sigma value can be changed as required. Thestandard value is 1.8.

12.9 Maximum combination of opened pictures

The operation corresponds to the mean of opened pictures. The maximum combinationprocedure should be selected instead of the average. Herewith brightest value is selectedrespectively into the resultant picture. This is especially useful if one captured receptionsthrough different line filters (z. B. and OIII) and would like to combine this to a singleilluminant picture. A further application is the combining trail of reception.

12.10 Maximum combination of many pictures

The operation corresponds to the mean of many pictures. To be sure to use the maximum

combination procedure here instead of the average.

12.11 Subtracting of pictures

The function Subtract Files in the Combine menu serves around to subtract a picture ofseveral other pictures. At the same time the uppermost opened picture is subtracted ofthe picture files to be selected. All pictures must show the same dimensions and the sametype (FIT IT or TIFF).

13 Gradient and Offset

13.1 Add Offset

When this function in theEditmenu is set one can add or subtract any base sum per canalto a picture. Following dialogue appears:


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The input values are added to the respective canal. In order to subtract values, one shouldinput simply the negative values. The function avoids values that would burst the normalvalue area. If a value of 80000 arose for a pixel for example, this is limiting to thesystem with normal values to 65535. If a value of -200 is obtained this is set to 0.

The option Ignore Zero causes pixels, that remain unchanged to have the values 0.

13.2 Remove Gradient

Frequently pictures show brightness and/or colour gradient. These can be removed withthe function Remove Gradient in the Edit menu. This function is used mostly on aprocessed and ready picture. Simultaneous Regim generates a background profile of thepicture on the basis of random samples in the picture. This background profile issubtracted then to remove the Gradient. The problem exists therein, to distinguish thebackground of the picture from foreground (stars, galaxies, fog etc.). The randomsamples must be then be carefully selected. The dialogue offers following option:

Number samples with this one can determines how manyrandom samples are supposed to bedistributed over the width of the picture.The more the amount, the more detaileddistribution of the background model

Background Auto/manual Regim must determine the picturebackground of the random sample. This canresult automatically. In some pictures

especially with extensive objects, theautomatic mode may not succeed always. Insuch cases, the background must bedetermined manually. For this a value is tobe indicated for the background. Oneshould determine the value by trial anderror. One can undertake an approximateestimation of the value with the mouse


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placed over the picture background and readthe values in the status strip of the picture.

Generate with this function can generate random

samples. The positions of the randomsamples appear as small squares in thepicture. No squares should lie on the actualpicture object (z. B. galaxy). On the otherhand the background should be welluncovered. One can appropriately set ordelete additional points with the click of themouse.

Execute as soon as one is satisfied with thedistribution of the random samples, one can

execute the actual processing over thisbutton. It becomes the background modelwhen own picture open and calculatesdrawn-off of the actual picture.

Exit with this one exits the function.

Reference after conclusion of the function it can benecessary to correct the brightness of thepicture negligibly. The function removes


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the Gradient, however it does not take intoconsideration the general color assimilationof the background. If a picture in thebackground is generally to rot-lastig, this is

not corrected.

14 Color manipulations

14.1 RGB color pictures put together to set

The function Combine Channels in the Colormenu can be used to combine together aRGB color picture made out of separate three filtered white receptions. Open the threeSW pictures that your color canals represent and then select above-mentioned menu.Subsequently assign the correct color canals to the pictures.

14.2 Manipulate Color canals

The menu function Multiply Channels in the Colormenu can change the weight of thecolor canals in the current picture. Following dialogue appears:

Over the three slides and/or over the input fields, the three color canals withcorresponding values can be multiplied. One corresponds at the same time to the exitcondition. You can appraise the changes with the press button Preview. The changes

however become effective if one click the Ok. This function is applicable only for TIFF-RGB-pictures.

14.3 Monochrome changes

The function Monochrome in the Color menu can be used according to RGB colorpicture to produce a white picture. A dialogue appears for the attitude of the conversionoption. One has to select one of the four variants:


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Average when one chooses this function, all threecolor canals go in to similar parts.

Classic The selection causes the classic SW changewith stronger weight of the green canal.This is leaned on the human physiology ofseeing.

Luminance here the Luminant canal is extracted.

Custom One can customize the weight of the colorcanals with this function.

One can select the most favorable method.

14.4 Automatic Color calibration with star color

The color calibration of the astronomical reception is difficult. Usually a calibration isrecommended for G2-Stars. Unfortunately the spectral types of only few stars are


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determined and out of which relatively fewer stars are of spectral type G2. Theprobability of having G2-Stars in the received field is especially low. An exit offers thecalibration on the basis of the color index (B V) of stars. The color index is determinedfor many stars and therewith the probability to have a star with well known color index in

the picture is high. The idea, behind that the procedure sticks follows: Seek a star withwell known color index (B V) in its picture. For this color index, a certain color isindicated to the system. The system changes the color calibration so that the relevant starhas the color deposited for its color index. Furthermore the picture background isadapted so that it attains a neutral color. It would exceed the scope of this instruction todescribe the procedure in detail. It is based on the procedure that of P. Riepe and H.Tomsik in the VdS-Journal1 have described. The automatic color calibration works onthis principle. The manual selection of the stars, can be somewhat tiresome under certaincircumstances. Instead if one selects the automatic mode, it seeks the lost stars and leadsan adjustment (Plate Solving) against a star catalogue (NOMAD). At the same timerequisition up to 200 stars for the ascertainment of the color correction. The automatic

procedure is to be preferred therefore as a rule to the manual. Solely in individual cases,in which the automatic procedure can find no suitable coordination to the catalogue data,the manual application should be preferred. When one chooses the menu functionAutomatic B V Color Calibration in the Colormenu following dialogue appears:

___________________________1 P. Riepe, H. Tomsik, the colors of the stars, VdS journal no. 25 S. 53ff & VdS journalno. 26 S. 48ffH. Tomsik, P. Riepe, Farbkalibration of a CCD reception with the help of G stars, VdS

journal Nr. 25 S. 57ff & VdS journal no. 26 S. 50ff________________________________________________________________________


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Use object name To be able to carry out the adjustmentagainst the star catalogue the program mustknow from which fields it should select the

pictures. In the option Use object name, onecan initiate the labeling of the catalogue inthe field (z. B. M94 or NGC2403) toindicate the received object. The objectshould be at the same time half-way in thecenter of the picture. Smaller deviations arehowever undiscerning. The object name isdissolved then of the program by means of


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the Internet service Simbad. If it is notpossible to clearly coordinate to an objectname, one can select instead Usecoordinates and give further below the

equatorial coordinates of the picture center.

Object name if you selected Use object name, give herethe catalogue label of the object in thepicture at center (z. B. M94, NGC2403 orCollinder399).

Image center if you select Use coordinates; indicate herethe equatorial coordinates of the picturecenter.

Image FOV gives you here the size of the uncoveredpicture field in arch minutes. In arectangular picture format, you select thelong side. One should not to select the fieldsubstantially larger, than it is actually. Thiscan lead to longer running time and inaddition the star coordination may not becorrect.

Number of stars until Search radius. These five parametersdrive the search for stars in the picture. Its

meaning is described in the chapter on thealigning of pictures.

Auto background this option is dialed to try Regim todetermine the background automatically. Inmost cases, this option will function well

manual background this option, requests you to click with themouse on a region in the picture, that shouldcount as a background. This option is thenadvisable if the largest part of the picture or

quite the entire picture is taken in fog andtherefore the automatic determination of thesky background is impeded. Select then adark neutral area of the picture.

Reference: For this function, you require an Internetconnection. Also please read chapters 6.pre-settings


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If the program tries to adjust the stars in the picture against the stars out of the catalogue,an additional picture window appears to represent the stars out of the catalogue. Thiswindow appraises the selected passport patterns and is closed again after termination of

the calibration.

14.5 Manual Color calibration

This function works on the same principle on star color as the automatic color calibrationdescribed before. To be sure select the star results here manually.Open the RGB picture to be calibrated and identify one or several (up to 5) stars withwell known color index (z. B. by means of a star card program or Simbad/Aladin). Overthe Menu function Manual B V Color Calibration in the Color menu, the followingdialogue opens:


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Select in the dialogue box the color index which is the next to your star.


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Auto background this option is dialed by Regim to determinethe background automatically. In mostcases, this option will function well

manual background with this option, one can click on a region inthe picture, which is to be the backgroundThis option is then advisable if the largestpart of the picture or quite the entire pictureis taken in fog and therefore the automaticdetermination of the sky background isimpeded. Select then a dark neutral area ofthe picture.

Number of star here they can adjust how many stars youwant to use for the calibration.

Star search radius here the radius for the star recognition canbe selected. If one clicks on a star, Regimtries to grasp this exactly within theindicated radius. According to starbrightness, and Sampling (archseconds/pixel) different values can beuseful.

One can select the color index of a star subsequently in the picture, and click on theappropriate one. One can repeat these steps for up to five stars (attitude Number of star).

The selected stars are marked with a circle. Once the numbers of the stars are selected,one can click OKto start the color calibration. In case of manual background selection,one can to click a background region in the picture.

Reference: This function is applicable only for TIFF-RGB-pictures.

14.6 Change RAW pictures in RGB

This function carries out RAW Debayering in the Color menu. Following dialogueappears:


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One can find the description of the single parameters in the chapter 7.2.Calibration.

14.7 NoLiGCRA

This strange word stands for "Non linear gradation color retrieval algorithm". It is aprocedure developed by Harald Tomsik and Peter Riepe that permits it to stretch theHistogram of a color picture, without affecting the color ratios of the single pixels. Thebases of the procedure can be read in the corresponding article 2. First of all a whitepicture is generated out of the color picture. The Histogram of this white picture iscreated using a suitable program. Subsequently the stretched white picture with the


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original color picture in the NoLiGCRA procedure is reckoned. If a Luminant picture isalready available, this can also be used in place of the SW picture out of the RGB picture.This is how the procedure follows:

1 open the color picture and the stretched SW picture.2 select in the Colormenu the functionNon linearly gradation color retrieval.3 A dialogue with two selection boxes appears. Select the stretched SW picture andunder RGB image select the original color picture under Luminance frame.4 confirm with OK.

After short time the stretched RGB picture will appear.

_________________________2 H. Tomsik, P. Riepe, NOLIGCRA a trip through that all, around the color will, starsand space 04/2009 S. 86ff

________________________________________________________________________

15 Blink Comparator

15.1 Blinking of opened pictures

Select the functionBlink in the menu View to blink several opened pictures against eachother. Following dialogue appears:

To the left of the dialogue box one can select the left the pictures that you want to blink.Blinking can be set ON and OFF using the Startand Stop functions. One can also adjustthe blinking speed using the regulator button. The maximal blink speed depends naturallyon the size of the pictures and the efficiency of the computer. The blink function can beused for several purposes:


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1: For recognizing whether the pictures were aligned really to each other.2: For recognizing of moved objects (comet, small planets, etc.) in the pictures.

15.2 Blinking of many pictures

Many pictures blinking against each other, with the function Blink Files. In the fileselection dialogue appears, all pictures to blink are selected. Subsequently the dialoguedescribed in the prior section appears. The pictures are loaded in cyclic manner. It ispossible to blink practically unlimited number of pictures. The attainable blink speeddepends at the same time on the size of the pictures and the efficiency of the computer.

Reference: In the Blink Files function, the pictures inthe background are loaded cyclic into aninternal buffer in order to permit a fluidblinking. The standard buffer size is four.

I.e. up to four pictures are held in the buffer.The main memory could be suddenly full ifthe main memory is little for the pictures arelarge. In such cases, the buffer size can bereduced. In addition in the fileregim.properties the value for the parameterblinkFifoSize can be diminished. On theother hand Main memory is very muchavailable, or the pictures are rather small,you can increase the value also. Also seesection 4 regarding the storage upper limit.

16 Visualization attitudes

16.1 To place black point and white point

At the right window edge find two push regulators. Over these push regulators, you canadjust the black point as well as the white point for the uppermost picture window. Thisis helpful in order to make weak details visible especially in very dark pictures.

Important reference: These attitudes affect only the current screenvisualization. The picture data themselves

are not changed at the same time.

16.2 Black point and white point for all pictures

If you opened several pictures, it can receive the visualization attitudes of the currentpicture for all opened pictures. First of all adjust for the current picture the black pointand white point as described in the prior section. Select then the function Equalize


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Visualization out of the View menu. The black and white points are then set for allpictures.

16.3 Set black and white point automatically

You will find the function Auto Stretch in the menu View. This Function causes anautomatic adaptation of black point and white point around the any value of the picture.Those with especially CCD receptions can be judged very quickly. This function is alsoover the Pop-Up menu of a picture and the function key F4

16.4 Picture zoom

Regim represent always a loaded picture if possible completely in a window. In addition

the picture is represented under reduced circumstances. The current zoom step isindicated in the title strip of the picture window. If you want to change this, you canclick with the right mouse key into the picture window. Then a menu appears thatpermits it to change the zoom step between 1/1 and 1 /19. You can carry out thesefunctions also directly over the keyboard (keys +,- and 1).

Important reference: These attitudes affect only the current screenvisualization. The picture data themselvesare not changed at the same time.

17 Edit pixels

The functionEdit pixel is over the PopUp menu (right click into the picture). Followingdialogue appears:


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The single functions are clarified as follows.

17.1 The notices

With the right click of the mouse in the Edit pixel window represent the single pixels

around the position where they were. In the upper table, you find the brightness values,below to the left the actual representation of the pixels. With a mouse click into one ofboth tables you can select a pixel. The exact position in the general view and theaccompanying brightness values of the single canals are indicated to the right. Thevisualization attitudes (black- and white point) are the same like in the accompanyingpicture.


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17.2 Changes

After you selected a pixel, you can change the pixel data now on following types:

Through petition of values in the input fields on the right side. A petition into a

field must be locked with the Enter key in order to become effective.

Through petition of a brightness value into a field of the upper table. A petition

must be locked with the Enter key.

Through the Paint mode. Select in addition a pixel, that you would like to copy.

Subsequently you turn on the Paint mode through a click on the Paint button.After that you can click on with the mouse in the lower left table to dye all wantedpixels.

Reference: All changes are stored first of all in aninternal buffer and are not directly receivedinto the picture. The changes are receivedfirst then shifted into the picture if you pressthe button Apply changes, or leave thedialogue with OK.

17.3 Navigating

If one wants to change the selected picture area one can do this with the four navigationbuttons. You must confirm the changes withApply changes or they would be rejected.

Tip: Instead of the navigation buttons, they can also use the cursor keys in connectionwith the old key.

18 Astrometrie (Plate Solving)

The further analysis of a picture is often helpful if the picture information contains theshown sky cut. One can evaluate it then in suitable tools such as ALADIN3.

The determining of these information is named Plate Solving. At the same time the starsin the picture against data are adjusted out of star catalogues. If the adjustment was

successful, the determined data (coordinate of the picture midpoint, picture orientationetc.) in that are written with FIT IT Header. This FIT IT Header can then evaluate otherprograms (z. B. Aladin).

Reference: For this function, you require an Internetconnection. Also note chapters 6.Presettings


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You can reach the function over the menu Tools-> Plate Solve. Following dialogueappears:

The dialogue is extensively identical with the dialogue for the automatic color

calibration (see chapter 14.4.Automatische color calibration with star color).

__________________3 See http://aladin.u-strasbg.fr/ ________________________________________________________________________
http://aladin.u-strasbg.fr/http://aladin.u-strasbg.fr/


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After one undertakes the necessary petitions and pressed OK, a further dialogue appears,that indicates the progress. The success of the function is indicated in the dialogue-box.If the process is successful, Regim expand the FIT IT Header around the WCS4-

Parameter and store the picture now as IT file FIT.

How you regard FIT IT Header can be indicated in the chapter fit- Header indicator.

If you load a picture, which contains these WCS parameters in the Header, one get theequatorial coordinates for the position of the mouse pointer in the status strip of thepicture (see also chapter The status strip in the picture window). 4 WCS = worldCoordinate system. See http://fits.gsfc.nasa.gov/fits_wcs.html

19 Indicate Histogramm

To look at the Histogramm of a picture, click with the right mouse key into the picturewindow. One can select Histogramm from the menu. Thereupon a window with theHistogram opens itself.

In color pictures, you can select between the Gesamt histogramm and the single colorcanals.
http://fits.gsfc.nasa.gov/fits_wcs.htmlhttp://fits.gsfc.nasa.gov/fits_wcs.html


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20 The status strip in the picture window

The picture windows control a status strip, in which information to the picture isindicated. Individually these are:

W the width of the picture in pixel.

H of the height of the picture in pixel.

R the brightness sphere (of until), that occurs in the picture.

Avg the average brightness of the picture.

If you move the mouse over the picture, in addition following information is indicated:

X, Y the pixel coordinate over which the mouse pointer just is.

RGB and/or L the RGB values (in RGB pictures) and/orthe brightness values (in gradations pictures)at the current mouse pointer position.

If in the picture WCS data that contains FIT IT Header, in addition one gets theequatorial coordinates (Rektaszension and declension) are indicated for the position of

the mouse pointer.


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21 The status window

The status window serves in addition to issue certain status information of the process. Inthe present version, is useful to search for mistakes, in case if there are any. Interestinglythe editions are especially in the search for a passport pattern and the subsequenttransformation. During the transformation of the picture to be aligned, running points areissued. Furthermore a progress beam is indicated in most functions at the lower edge ofthe status window.

22 Fit - Header indicate


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By selecting fit Header one can look at fit -Header of one fit - picture, click with the rightmouse key into the picture window. Thereupon a window opens with the notice the fit-Headers.

23 General References for the procedure

The quality of the final result is primarily dependent on the quality of the available rawdata. Always try to receive as far as possible raw data. The careful preparing of suitabledark pictures (Darks) and Flat-fields is important. To this refer to the pertinent literature.The preparation with Regim should result in following sequence:

1 generate a Masterdark (menu Preprocessing-> Setup darks)2 generate a Masterflat (menu Preprocessing-> Setup flats)3 calibrate the raw pictures (menu Preprocessing-> Preprocessing)4 remove if required Blooming out of the calibrated single pictures (menu Edit-> Remove

Blooming from Files or directly under Preprocessing)5 arrange to guarantee the calibrated single pictures on each other out (menu Edit-> indexFiles or directly under Preprocessing)6 blink the pictures against each other, around, which all pictures were correctly aligned.7 combine the directed calibrated single pictures (menu Combinet-> aperture Files,Median combine Files, Sigma combine Files or SD combine files or directly underPreprocessing). The SD procedure is to be preferred as a rule.8 store the result.

For the further preparation, a standard picture preparation program such asPicture Window, Photoshop or Gimp is recommended.

Supplement A

Debayer attitudes for some cameras (without guarantee):

Regim Stacking Software

Documents

Transcript of Regim Stacking Software