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


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


Main high-level command-line user interface for

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.


Print the help message
Be more chatty. Repeat for even more verboseness
Place all output files in the specified directory
Name the output files with this base name
Use this config file for the "astrometry-engine" program
Use this config file for the "astrometry-engine" program
Run astrometry-engine once, rather than once per input file
Read filenames to solve on stdin, one per line
Don't create any plots of the results
Scale the plots by this factor (eg, 0.25)
Set the background image to use for plots (JPEG)
Use wget instead of curl
Overwrite output files if they already exist
Don't overwrite output files if they already exist; continue a previous run
Skip input files for which the 'solved' output file already exists; NOTE: this assumes single-field input files
assume the input files are FITS images
Output filename of the new FITS file containing the WCS header; "none" to not create this file
Create KMZ file for Google Sky. (requires wcs2kml)
Create image object catalog for SCAMP
Create SCAMP config file snippet
Output filename for xylist containing the image coordinate of stars from the index
Just write the augmented xylist files; don't run astrometry-engine.
Output filename for augment xy list (axy)
Write 'augmented xy list' (axy) file to a temp file
Add timestamps to log messages
-7, --no-delete-temp
Don't delete temp files (for debugging)
Lower bound of image scale estimate
Upper bound of image scale estimate
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
35-mm (width-based) equivalent focal length
-8, --parity pos/neg
Only check for matches with positive/negative parity (default: try both)
Matching distance for quads (default: 0.01)
For verification, size of pixel positional error (default: 1)
Minimum size of quads to try, as a fraction of the smaller image dimension, default: 0.1
Maximum size of quads to try, as a fraction of the image hypotenuse, default 1.0
Odds ratio at which to try tuning up a match that isn't good enough to solve (default: 1e6)
Odds ratio at which to consider a field solved (default: 1e9)
Odds ratio at which to reject a hypothesis (default: 1e-100)
Odds ratio at which to stop adding stars when evaluating a hypothesis (default: HUGE_VAL)
Use Source Extractor rather than built-in image2xy to find sources
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.
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.
-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
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.
Cut the source list to have this many items (after sorting, if applicable).
Give up solving after the specified number of seconds of CPU time
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 the image (for black-on-white images)
Downsample the image by factor int before running source extraction
Don't try to estimate a smoothly-varying sky background during source extraction.
Set the noise level in the image
-9, --no-remove-lines
Don't remove horizontal and vertical overdensities of sources.
Select sources uniformly using roughly this many boxes (0=disable; default 10)
Don't uniformize the field stars during verification
Don't deduplicate the field stars during verification
-0, --no-fix-sdss
Don't try to fix SDSS idR files.
Filename whose creation signals the process to stop
Output file to mark that the solver succeeded
Input filename for solved file
Output filename for match file
Output filename for RDLS file
Sort the RDLS file by this column; default is ascending; use "-column" to sort "column" in descending order instead.
Grab tag-along column from index into RDLS file
Grab all tag-along columns from index into RDLS file
Output filename for SCAMP reference catalog
Output filename for correspondences
Output filename for WCS file
Save the PNM file as file
Save the (unaugmented) xylist to file
Quit after writing the unaugmented xylist
Try to verify an existing WCS file
HDU from which to read WCS to verify; set this BEFORE --verify
Ignore existing WCS headers in FITS input images
Try to guess the image scale from the FITS headers
Set the WCS reference point to the image center
Set the WCS reference point to the given position
Set the WCS reference point to the given position
Don't fine-tune WCS by computing a SIP polynomial
Polynomial order of SIP WCS corrections
Where to put temp files, default /tmp

The following options are valid for xylist inputs only:

The FITS extension(s) to solve, inclusive
Specify the field width
Specify the field height
The FITS column containing the X coordinate of the sources
The FITS column containing the Y coordinate of the sources
The FITS column that should be used to sort the sources
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.)


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


July 2015 0.56