Skip site navigation (1)Skip section navigation (2)

FreeBSD Manual Pages

  
 
  

home | help
SOLVE-FIELD(1)			astrometry.net			SOLVE-FIELD(1)

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 afalse positivesa	(but  maybe  some  ano
       answersa). It will do its best, even when the input image has no	or to-
       tally 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 ex-
	      ists; 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-en-
	      gine.

       --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 hy-
	      potenuse,	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 hy-
	      pothesis (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-sub-
	      tracted and non-background-subtracted flux

       -6, --extension int
	      FITS extension to	read image from.

       -2, --no-fits2fits
	      Don't sanitize FITS files; assume	they're	already	valid

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

       -z, --downsample	int
	      Downsample the image by factor int before	running	source extrac-
	      tion

       --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=dis-
	      able; 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

0.56				   July	2015			SOLVE-FIELD(1)

NAME | SYNOPSIS | DESCRIPTION | OPTIONS | AUTHOR | SEE ALSO

Want to link to this manual page? Use this URL:
<https://www.freebsd.org/cgi/man.cgi?query=solve-field&sektion=1&manpath=FreeBSD+12.0-RELEASE+and+Ports>

home | help