-h, --help
Print the help message
-v, --verbose
Be more chatty. Repeat for even more verboseness
-D, --dirdirectory
Place all output files in the specified directory
-o, --outfile
Name the output files with this base name
-b, --backend-configfile
Use this config file for the "astrometry-engine" program
--configfile
Use this config file for the "astrometry-engine" program
--batch
Run astrometry-engine once, rather than once per input file
-f, --files-on-stdin
Read filenames to solve on stdin, one per line
-p, --no-plots
Don't create any plots of the results
--plot-scalescale
Scale the plots by this factor (eg, 0.25)
--plot-bgfile
Set the background image to use for plots (JPEG)
-G, --use-wget
Use wget instead of curl
-O, --overwrite
Overwrite output files if they already exist
-K, --continue
Don't overwrite output files if they already exist; continue a previous run
-J, --skip-solved
Skip input files for which the 'solved' output file already exists; NOTE: this assumes single-
field input files
--fits-image
assume the input files are FITS images
-N, --new-fitsfile
Output filename of the new FITS file containing the WCS header; "none" to not create this file
-Z, --kmzfile
Create KMZ file for Google Sky. (requires wcs2kml)
-i, --scampfile
Create image object catalog for SCAMP
-n, --scamp-configfile
Create SCAMP config file snippet
-U, --index-xylsfile
Output filename for xylist containing the image coordinate of stars from the index
--just-augment
Just write the augmented xylist files; don't run astrometry-engine.
--axyfile
Output filename for augment xy list (axy)
--temp-axy
Write 'augmented xy list' (axy) file to a temp file
--timestamp
Add timestamps to log messages
-7, --no-delete-temp
Don't delete temp files (for debugging)
-L, --scale-lowscale
Lower bound of image scale estimate
-H, --scale-highscale
Upper bound of image scale estimate
-u, --scale-unitsunits
In what units are the lower and upper bounds? Choices:
"degwidth", "degw", "dw"
width of the image, in degrees (default)
"arcminwidth", "amw", "aw"
width of the image, in arcminutes
"arcsecperpix", "app"
arcseconds per pixel
"focalmm"
35-mm (width-based) equivalent focal length
-8, --paritypos/neg
Only check for matches with positive/negative parity (default: try both)
-c, --code-tolerancedistance
Matching distance for quads (default: 0.01)
-E, --pixel-errorpixels
For verification, size of pixel positional error (default: 1)
-q, --quad-size-minfraction
Minimum size of quads to try, as a fraction of the smaller image dimension, default: 0.1
-Q, --quad-size-maxfraction
Maximum size of quads to try, as a fraction of the image hypotenuse, default 1.0
--odds-to-tune-upodds
Odds ratio at which to try tuning up a match that isn't good enough to solve (default: 1e6)
--odds-to-solveodds
Odds ratio at which to consider a field solved (default: 1e9)
--odds-to-rejectodds
Odds ratio at which to reject a hypothesis (default: 1e-100)
--odds-to-stop-lookingodds
Odds ratio at which to stop adding stars when evaluating a hypothesis (default: HUGE_VAL)
--use-source-extractor
Use Source Extractor rather than built-in image2xy to find sources
--source-extractor-configfile
Use the given Source Extractor config file. Note that CATALOG_NAME and CATALOG_TYPE values will be
over-ridden by command-line values. This option implies --use-source-extractor.
--source-extractor-pathfile
Use the given path to the Source Extractor executable. Default: just 'source-extractor', assumed
to be in your PATH. Note that you can give command line args here too (but put them in quotes),
eg:
--source-extractor-path 'source-extractor -DETECT_TYPE CCD'.
This option implies --use-source-extractor.
-3RA, --raRA
RA of field center for search, format: degrees or hh:mm:ss
-4DEC, --decDEC
DEC of field center for search, format: degrees or hh:mm:ss
-5degrees, --radiusdegrees
Only search in indexes within 'radius' of the field center given by --ra and --dec-d, --depthnumber or range
Number of field objects to look at, or range of numbers; 1 is the brightest star, so "-d 10" or
"-d 1-10" mean look at the top ten brightest stars only.
--objsint
Cut the source list to have this many items (after sorting, if applicable).
-l, --cpulimitseconds
Give up solving after the specified number of seconds of CPU time
-r, --resort
Sort the star brightnesses by background-subtracted flux; the default is to sort using acompromise
between background-subtracted and non-background-subtracted flux
-6, --extensionint
FITS extension to read image from.
--invert
Invert the image (for black-on-white images)
-z, --downsampleint
Downsample the image by factor int before running source extraction
--no-background-subtraction
Don't try to estimate a smoothly-varying sky background during source extraction.
--sigmafloat
Set the noise level in the image
-9, --no-remove-lines
Don't remove horizontal and vertical overdensities of sources.
--uniformizeint
Select sources uniformly using roughly this many boxes (0=disable; default 10)
--no-verify-uniformize
Don't uniformize the field stars during verification
--no-verify-dedup
Don't deduplicate the field stars during verification
-0, --no-fix-sdss
Don't try to fix SDSS idR files.
-C, --cancelfile
Filename whose creation signals the process to stop
-S, --solvedfile
Output file to mark that the solver succeeded
-I, --solved-infile
Input filename for solved file
-M, --matchfile
Output filename for match file
-R, --rdlsfile
Output filename for RDLS file
--sort-rdlscolumn
Sort the RDLS file by this column; default is ascending; use "-column" to sort "column" in
descending order instead.
--tagcolumn
Grab tag-along column from index into RDLS file
--tag-all
Grab all tag-along columns from index into RDLS file
-j, --scamp-reffile
Output filename for SCAMP reference catalog
-B, --corrfile
Output filename for correspondences
-W, --wcsfile
Output filename for WCS file
-P, --pnmfile
Save the PNM file as file-k, --keep-xylistfile
Save the (unaugmented) xylist to file-A, --dont-augment
Quit after writing the unaugmented xylist
-V, --verifyfile
Try to verify an existing WCS file
--verify-extextension
HDU from which to read WCS to verify; set this BEFORE --verify-y, --no-verify
Ignore existing WCS headers in FITS input images
-g, --guess-scale
Try to guess the image scale from the FITS headers
--crpix-center
Set the WCS reference point to the image center
--crpix-xpix
Set the WCS reference point to the given position
--crpix-ypix
Set the WCS reference point to the given position
-T, --no-tweak
Don't fine-tune WCS by computing a SIP polynomial
-t, --tweak-orderint
Polynomial order of SIP WCS corrections
-m, --temp-dirdir
Where to put temp files, default /tmpThefollowingoptionsarevalidforxylistinputsonly:-F, --fieldsnumberorrange
The FITS extension(s) to solve, inclusive
-w, --widthpixels
Specify the field width
-e, --heightpixels
Specify the field height
-X, --x-columncolumn-name
The FITS column containing the X coordinate of the sources
-Y, --y-columncolumn-name
The FITS column containing the Y coordinate of the sources
-s, --sort-columncolumn-name
The FITS column that should be used to sort the sources
-a, --sort-ascending
Sort in ascending order (smallest first); default is descending order
Note that most output files can be disabled by setting the filename to "none". (If you have a sick sense
of humour and you really want to name your output file "none", you can use "./none" instead.)
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