Upper bound of image scale estimate
Source: Ubuntu Manpage: solve-field – Main high-level command-line user interface.
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.
-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
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