Provided by: astrometry.net_0.75+dfsg-1_amd64 bug

NAME

       solve-field - Main high-level command-line user interface.

SYNOPSIS

       solve-field [options] [image-file-1 image-file-2 ...]  [xyls-file-1 xyls-file-2 ...]

DESCRIPTION

       Main high-level command-line user interface for astrometry.net

       You can specify http:// or ftp:// URLs instead of filenames.  The "wget" or "curl" program
       will be used to retrieve the URL.

       The astrometry engine will take any image  and  return  the  astrometry  world  coordinate
       system  (WCS),  ie a standards-based description of the (usually nonlinear) transformation
       between image coordinates and sky coordinates with absolutely no  “false  positives”  (but
       maybe some “no answers”). It will do its best, even when the input image has no or totally
       incorrect meta data.

OPTIONS

       -h, --help
              Print the help message

       -v, --verbose
              Be more chatty. Repeat for even more verboseness

       -D, --dir directory
              Place all output files in the specified directory

       -o, --out file
              Name the output files with this base name

       -b, --backend-config file
              Use this config file for the "astrometry-engine" program

       --config file
              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-scale scale
              Scale the plots by this factor (eg, 0.25)

       --plot-bg file
              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-fits file
              Output  filename  of  the  new  FITS  file containing the WCS header; "none" to not
              create this file

       -Z, --kmz file
              Create KMZ file for Google Sky. (requires wcs2kml)

       -i, --scamp file
              Create image object catalog for SCAMP

       -n, --scamp-config file
              Create SCAMP config file snippet

       -U, --index-xyls file
              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.

       --axy file
              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-low scale
              Lower bound of image scale estimate

       -H, --scale-high scale
              Upper bound of image scale estimate

       -u, --scale-units units
              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, --parity pos/neg
              Only check for matches with positive/negative parity (default: try both)

       -c, --code-tolerance distance
              Matching distance for quads (default: 0.01)

       -E, --pixel-error pixels
              For verification, size of pixel positional error (default: 1)

       -q, --quad-size-min fraction
              Minimum size of quads to try,  as  a  fraction  of  the  smaller  image  dimension,
              default: 0.1

       -Q, --quad-size-max fraction
              Maximum size of quads to try, as a fraction of the image hypotenuse, default 1.0

       --odds-to-tune-up odds
              Odds  ratio  at  which  to  try  tuning  up a match that isn't good enough to solve
              (default: 1e6)

       --odds-to-solve odds
              Odds ratio at which to consider a field solved (default: 1e9)

       --odds-to-reject odds
              Odds ratio at which to reject a hypothesis (default: 1e-100)

       --odds-to-stop-looking odds
              Odds ratio at which to stop adding stars when  evaluating  a  hypothesis  (default:
              HUGE_VAL)

       --use-sextractor
              Use SExtractor rather than built-in image2xy to find sources

       --sextractor-config file
              Use  the  given  SExtractor  config  file.  Note that CATALOG_NAME and CATALOG_TYPE
              values  will  be  over-ridden  by  command-line  values.    This   option   implies
              --use-sextractor.

       --sextractor-path file
              Use  the  given  path  to  the  SExtractor  executable. Default: just 'sextractor',
              assumed to be in your PATH. Note that you can give command line args here too  (but
              put them in quotes), eg:

              --sextractor-path 'sextractor -DETECT_TYPE CCD'.

              This option implies --use-sextractor.

       -3 RA, --ra RA
              RA of field center for search, format: degrees or hh:mm:ss

       -4 DEC, --dec DEC
              DEC of field center for search, format: degrees or hh:mm:ss

       -5 degrees, --radius degrees
              Only search in indexes within 'radius' of the field center given by --ra and --dec

       -d, --depth number 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.

       --objs int
              Cut the source list to have this many items (after sorting, if applicable).

       -l, --cpulimit seconds
              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, --extension int
              FITS extension to read image from.

       --invert
              Invert the image (for black-on-white images)

       -z, --downsample int
              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.

       --sigma float
              Set the noise level in the image

       -9, --no-remove-lines
              Don't remove horizontal and vertical overdensities of sources.

       --uniformize int
              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, --cancel file
              Filename whose creation signals the process to stop

       -S, --solved file
              Output file to mark that the solver succeeded

       -I, --solved-in file
              Input filename for solved file

       -M, --match file
              Output filename for match file

       -R, --rdls file
              Output filename for RDLS file

       --sort-rdls column
              Sort  the  RDLS  file  by  this column; default is ascending; use "-column" to sort
              "column" in descending order instead.

       --tag column
              Grab tag-along column from index into RDLS file

       --tag-all
              Grab all tag-along columns from index into RDLS file

       -j, --scamp-ref file
              Output filename for SCAMP reference catalog

       -B, --corr file
              Output filename for correspondences

       -W, --wcs file
              Output filename for WCS file

       -P, --pnm file
              Save the PNM file as file

       -k, --keep-xylist file
              Save the (unaugmented) xylist to file

       -A, --dont-augment
              Quit after writing the unaugmented xylist

       -V, --verify file
              Try to verify an existing WCS file

       --verify-ext extension
              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-x pix
              Set the WCS reference point to the given position

       --crpix-y pix
              Set the WCS reference point to the given position

       -T, --no-tweak
              Don't fine-tune WCS by computing a SIP polynomial

       -t, --tweak-order int
              Polynomial order of SIP WCS corrections

       -m, --temp-dir dir
              Where to put temp files, default /tmp

   The following options are valid for xylist inputs only:
       -F, --fields number or range
              The FITS extension(s) to solve, inclusive

       -w, --width pixels
              Specify the field width

       -e, --height pixels
              Specify the field height

       -X, --x-column column-name
              The FITS column containing the X coordinate of the sources

       -Y, --y-column column-name
              The FITS column containing the Y coordinate of the sources

       -s, --sort-column column-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.)

AUTHOR

       The Astrometry.net team. Principal investigators are David W. Hogg (NYU) and  Dustin  Lang
       (CMU).

SEE ALSO

       http://astrometry.net