1SOLVE-FIELD(1) astrometry.net SOLVE-FIELD(1)
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6 solve-field - Main high-level command-line user interface.
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9 solve-field [options] [image-file-1 image-file-2 ...] [xyls-file-1
10 xyls-file-2 ...]
11
13 Main high-level command-line user interface for astrometry.net
14 You can specify http:// or ftp:// URLs instead of filenames. The
16 "wget" or "curl" program will be used to retrieve the URL.
17 The astrometry engine will take any image and return the astrometry
19 world coordinate system (WCS), ie a standards-based description of the
20 (usually nonlinear) transformation between image coordinates and sky
21 coordinates with absolutely no “false positives” (but maybe some “no
22 answers”). It will do its best, even when the input image has no or
23 totally incorrect meta data.
24
26 -h, --help
27 Print the help message
28 -v, --verbose
30 Be more chatty. Repeat for even more verboseness
31 -D, --dir directory
33 Place all output files in the specified directory
34 -o, --out file
36 Name the output files with this base name
37 -b, --backend-config file
39 Use this config file for the "astrometry-engine" program
40 --config file
42 Use this config file for the "astrometry-engine" program
43 --batch
45 Run astrometry-engine once, rather than once per input file
46 -f, --files-on-stdin
48 Read filenames to solve on stdin, one per line
49 -p, --no-plots
51 Don't create any plots of the results
52 --plot-scale scale
54 Scale the plots by this factor (eg, 0.25)
55 --plot-bg file
57 Set the background image to use for plots (JPEG)
58 -G, --use-wget
60 Use wget instead of curl
61 -O, --overwrite
63 Overwrite output files if they already exist
64 -K, --continue
66 Don't overwrite output files if they already exist; continue a
67 previous run
68 -J, --skip-solved
70 Skip input files for which the 'solved' output file already
71 exists; NOTE: this assumes single-field input files
72 --fits-image
74 assume the input files are FITS images
75 -N, --new-fits file
77 Output filename of the new FITS file containing the WCS header;
78 "none" to not create this file
79 -Z, --kmz file
81 Create KMZ file for Google Sky. (requires wcs2kml)
82 -i, --scamp file
84 Create image object catalog for SCAMP
85 -n, --scamp-config file
87 Create SCAMP config file snippet
88 -U, --index-xyls file
90 Output filename for xylist containing the image coordinate of
91 stars from the index
92 --just-augment
94 Just write the augmented xylist files; don't run astrometry-
95 engine.
96 --axy file
98 Output filename for augment xy list (axy)
99 --temp-axy
101 Write 'augmented xy list' (axy) file to a temp file
102 --timestamp
104 Add timestamps to log messages
105 -7, --no-delete-temp
107 Don't delete temp files (for debugging)
108 -L, --scale-low scale
110 Lower bound of image scale estimate
111 -H, --scale-high scale
113 Upper bound of image scale estimate
114 -u, --scale-units units
116 In what units are the lower and upper bounds? Choices:
117 "degwidth", "degw", "dw"
119 width of the image, in degrees (default)
120 "arcminwidth", "amw", "aw"
122 width of the image, in arcminutes
123 "arcsecperpix", "app"
125 arcseconds per pixel
126 "focalmm"
128 35-mm (width-based) equivalent focal length
129 -8, --parity pos/neg
131 Only check for matches with positive/negative parity (default:
132 try both)
133 -c, --code-tolerance distance
135 Matching distance for quads (default: 0.01)
136 -E, --pixel-error pixels
138 For verification, size of pixel positional error (default: 1)
139 -q, --quad-size-min fraction
141 Minimum size of quads to try, as a fraction of the smaller image
142 dimension, default: 0.1
143 -Q, --quad-size-max fraction
145 Maximum size of quads to try, as a fraction of the image
146 hypotenuse, default 1.0
147 --odds-to-tune-up odds
149 Odds ratio at which to try tuning up a match that isn't good
150 enough to solve (default: 1e6)
151 --odds-to-solve odds
153 Odds ratio at which to consider a field solved (default: 1e9)
154 --odds-to-reject odds
156 Odds ratio at which to reject a hypothesis (default: 1e-100)
157 --odds-to-stop-looking odds
159 Odds ratio at which to stop adding stars when evaluating a
160 hypothesis (default: HUGE_VAL)
161 --use-sextractor
163 Use SExtractor rather than built-in image2xy to find sources
164 --sextractor-config file
166 Use the given SExtractor config file. Note that CATALOG_NAME and
167 CATALOG_TYPE values will be over-ridden by command-line values.
168 This option implies --use-sextractor.
169 --sextractor-path file
171 Use the given path to the SExtractor executable. Default: just
172 'sextractor', assumed to be in your PATH. Note that you can give
173 command line args here too (but put them in quotes), eg:
174 --sextractor-path 'sextractor -DETECT_TYPE CCD'.
176 This option implies --use-sextractor.
178 -3 RA, --ra RA
180 RA of field center for search, format: degrees or hh:mm:ss
181 -4 DEC, --dec DEC
183 DEC of field center for search, format: degrees or hh:mm:ss
184 -5 degrees, --radius degrees
186 Only search in indexes within 'radius' of the field center given
187 by --ra and --dec
188 -d, --depth number or range
190 Number of field objects to look at, or range of numbers; 1 is
191 the brightest star, so "-d 10" or "-d 1-10" mean look at the top
192 ten brightest stars only.
193 --objs int
195 Cut the source list to have this many items (after sorting, if
196 applicable).
197 -l, --cpulimit seconds
199 Give up solving after the specified number of seconds of CPU
200 time
201 -r, --resort
203 Sort the star brightnesses by background-subtracted flux; the
204 default is to sort using acompromise between background-sub‐
205 tracted and non-background-subtracted flux
206 -6, --extension int
208 FITS extension to read image from.
209 --invert
211 Invert the image (for black-on-white images)
212 -z, --downsample int
214 Downsample the image by factor int before running source extrac‐
215 tion
216 --no-background-subtraction
218 Don't try to estimate a smoothly-varying sky background during
219 source extraction.
220 --sigma float
222 Set the noise level in the image
223 -9, --no-remove-lines
225 Don't remove horizontal and vertical overdensities of sources.
226 --uniformize int
228 Select sources uniformly using roughly this many boxes (0=dis‐
229 able; default 10)
230 --no-verify-uniformize
232 Don't uniformize the field stars during verification
233 --no-verify-dedup
235 Don't deduplicate the field stars during verification
236 -0, --no-fix-sdss
238 Don't try to fix SDSS idR files.
239 -C, --cancel file
241 Filename whose creation signals the process to stop
242 -S, --solved file
244 Output file to mark that the solver succeeded
245 -I, --solved-in file
247 Input filename for solved file
248 -M, --match file
250 Output filename for match file
251 -R, --rdls file
253 Output filename for RDLS file
254 --sort-rdls column
256 Sort the RDLS file by this column; default is ascending; use
257 "-column" to sort "column" in descending order instead.
258 --tag column
260 Grab tag-along column from index into RDLS file
261 --tag-all
263 Grab all tag-along columns from index into RDLS file
264 -j, --scamp-ref file
266 Output filename for SCAMP reference catalog
267 -B, --corr file
269 Output filename for correspondences
270 -W, --wcs file
272 Output filename for WCS file
273 -P, --pnm file
275 Save the PNM file as file
276 -k, --keep-xylist file
278 Save the (unaugmented) xylist to file
279 -A, --dont-augment
281 Quit after writing the unaugmented xylist
282 -V, --verify file
284 Try to verify an existing WCS file
285 --verify-ext extension
287 HDU from which to read WCS to verify; set this BEFORE --verify
288 -y, --no-verify
290 Ignore existing WCS headers in FITS input images
291 -g, --guess-scale
293 Try to guess the image scale from the FITS headers
294 --crpix-center
296 Set the WCS reference point to the image center
297 --crpix-x pix
299 Set the WCS reference point to the given position
300 --crpix-y pix
302 Set the WCS reference point to the given position
303 -T, --no-tweak
305 Don't fine-tune WCS by computing a SIP polynomial
306 -t, --tweak-order int
308 Polynomial order of SIP WCS corrections
309 -m, --temp-dir dir
311 Where to put temp files, default /tmp
312 The following options are valid for xylist inputs only:
314 -F, --fields number or range
315 The FITS extension(s) to solve, inclusive
316 -w, --width pixels
318 Specify the field width
319 -e, --height pixels
321 Specify the field height
322 -X, --x-column column-name
324 The FITS column containing the X coordinate of the sources
325 -Y, --y-column column-name
327 The FITS column containing the Y coordinate of the sources
328 -s, --sort-column column-name
330 The FITS column that should be used to sort the sources
331 -a, --sort-ascending
333 Sort in ascending order (smallest first); default is descending
334 order
335 Note that most output files can be disabled by setting the filename to
337 "none". (If you have a sick sense of humour and you really want to
338 name your output file "none", you can use "./none" instead.)
339
341 The Astrometry.net team. Principal investigators are David W. Hogg
342 (NYU) and Dustin Lang (CMU).
343
345 http://astrometry.net
3460.56 July 2015 SOLVE-FIELD(1)