1SOLVE-FIELD(1)                  astrometry.net                  SOLVE-FIELD(1)
2
3
4

NAME

6       solve-field - Main high-level command-line user interface.
7

SYNOPSIS

9       solve-field  [options]  [image-file-1  image-file-2  ...]  [xyls-file-1
10       xyls-file-2 ...]
11

DESCRIPTION

13       Main high-level command-line user interface for astrometry.net
14
15       You can specify http:// or  ftp://  URLs  instead  of  filenames.   The
16       "wget" or "curl" program will be used to retrieve the URL.
17
18       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

OPTIONS

26       -h, --help
27              Print the help message
28
29       -v, --verbose
30              Be more chatty. Repeat for even more verboseness
31
32       -D, --dir directory
33              Place all output files in the specified directory
34
35       -o, --out file
36              Name the output files with this base name
37
38       -b, --backend-config file
39              Use this config file for the "astrometry-engine" program
40
41       --config file
42              Use this config file for the "astrometry-engine" program
43
44       --batch
45              Run astrometry-engine once, rather than once per input file
46
47       -f, --files-on-stdin
48              Read filenames to solve on stdin, one per line
49
50       -p, --no-plots
51              Don't create any plots of the results
52
53       --plot-scale scale
54              Scale the plots by this factor (eg, 0.25)
55
56       --plot-bg file
57              Set the background image to use for plots (JPEG)
58
59       -G, --use-wget
60              Use wget instead of curl
61
62       -O, --overwrite
63              Overwrite output files if they already exist
64
65       -K, --continue
66              Don't overwrite output files if they already exist;  continue  a
67              previous run
68
69       -J, --skip-solved
70              Skip  input  files  for  which  the 'solved' output file already
71              exists; NOTE: this assumes single-field input files
72
73       --fits-image
74              assume the input files are FITS images
75
76       -N, --new-fits file
77              Output filename of the new FITS file containing the WCS  header;
78              "none" to not create this file
79
80       -Z, --kmz file
81              Create KMZ file for Google Sky. (requires wcs2kml)
82
83       -i, --scamp file
84              Create image object catalog for SCAMP
85
86       -n, --scamp-config file
87              Create SCAMP config file snippet
88
89       -U, --index-xyls file
90              Output  filename  for  xylist containing the image coordinate of
91              stars from the index
92
93       --just-augment
94              Just write the augmented xylist  files;  don't  run  astrometry-
95              engine.
96
97       --axy file
98              Output filename for augment xy list (axy)
99
100       --temp-axy
101              Write 'augmented xy list' (axy) file to a temp file
102
103       --timestamp
104              Add timestamps to log messages
105
106       -7, --no-delete-temp
107              Don't delete temp files (for debugging)
108
109       -L, --scale-low scale
110              Lower bound of image scale estimate
111
112       -H, --scale-high scale
113              Upper bound of image scale estimate
114
115       -u, --scale-units units
116              In what units are the lower and upper bounds? Choices:
117
118              "degwidth", "degw", "dw"
119                     width of the image, in degrees (default)
120
121              "arcminwidth", "amw", "aw"
122                     width of the image, in arcminutes
123
124              "arcsecperpix", "app"
125                     arcseconds per pixel
126
127              "focalmm"
128                     35-mm (width-based) equivalent focal length
129
130       -8, --parity pos/neg
131              Only  check  for matches with positive/negative parity (default:
132              try both)
133
134       -c, --code-tolerance distance
135              Matching distance for quads (default: 0.01)
136
137       -E, --pixel-error pixels
138              For verification, size of pixel positional error (default: 1)
139
140       -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
144       -Q, --quad-size-max fraction
145              Maximum  size  of  quads  to  try,  as  a  fraction of the image
146              hypotenuse, default 1.0
147
148       --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
152       --odds-to-solve odds
153              Odds ratio at which to consider a field solved (default: 1e9)
154
155       --odds-to-reject odds
156              Odds ratio at which to reject a hypothesis (default: 1e-100)
157
158       --odds-to-stop-looking odds
159              Odds  ratio  at  which  to  stop  adding stars when evaluating a
160              hypothesis (default: HUGE_VAL)
161
162       --use-sextractor
163              Use SExtractor rather than built-in image2xy to find sources
164
165       --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
170       --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
175              --sextractor-path 'sextractor -DETECT_TYPE CCD'.
176
177              This option implies --use-sextractor.
178
179       -3 RA, --ra RA
180              RA of field center for search, format: degrees or hh:mm:ss
181
182       -4 DEC, --dec DEC
183              DEC of field center for search, format: degrees or hh:mm:ss
184
185       -5 degrees, --radius degrees
186              Only search in indexes within 'radius' of the field center given
187              by --ra and --dec
188
189       -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
194       --objs int
195              Cut  the  source list to have this many items (after sorting, if
196              applicable).
197
198       -l, --cpulimit seconds
199              Give up solving after the specified number  of  seconds  of  CPU
200              time
201
202       -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
207       -6, --extension int
208              FITS extension to read image from.
209
210       --invert
211              Invert the image (for black-on-white images)
212
213       -z, --downsample int
214              Downsample the image by factor int before running source extrac‐
215              tion
216
217       --no-background-subtraction
218              Don't try to estimate a smoothly-varying sky  background  during
219              source extraction.
220
221       --sigma float
222              Set the noise level in the image
223
224       -9, --no-remove-lines
225              Don't remove horizontal and vertical overdensities of sources.
226
227       --uniformize int
228              Select  sources  uniformly using roughly this many boxes (0=dis‐
229              able; default 10)
230
231       --no-verify-uniformize
232              Don't uniformize the field stars during verification
233
234       --no-verify-dedup
235              Don't deduplicate the field stars during verification
236
237       -0, --no-fix-sdss
238              Don't try to fix SDSS idR files.
239
240       -C, --cancel file
241              Filename whose creation signals the process to stop
242
243       -S, --solved file
244              Output file to mark that the solver succeeded
245
246       -I, --solved-in file
247              Input filename for solved file
248
249       -M, --match file
250              Output filename for match file
251
252       -R, --rdls file
253              Output filename for RDLS file
254
255       --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
259       --tag column
260              Grab tag-along column from index into RDLS file
261
262       --tag-all
263              Grab all tag-along columns from index into RDLS file
264
265       -j, --scamp-ref file
266              Output filename for SCAMP reference catalog
267
268       -B, --corr file
269              Output filename for correspondences
270
271       -W, --wcs file
272              Output filename for WCS file
273
274       -P, --pnm file
275              Save the PNM file as file
276
277       -k, --keep-xylist file
278              Save the (unaugmented) xylist to file
279
280       -A, --dont-augment
281              Quit after writing the unaugmented xylist
282
283       -V, --verify file
284              Try to verify an existing WCS file
285
286       --verify-ext extension
287              HDU from which to read WCS to verify; set this BEFORE --verify
288
289       -y, --no-verify
290              Ignore existing WCS headers in FITS input images
291
292       -g, --guess-scale
293              Try to guess the image scale from the FITS headers
294
295       --crpix-center
296              Set the WCS reference point to the image center
297
298       --crpix-x pix
299              Set the WCS reference point to the given position
300
301       --crpix-y pix
302              Set the WCS reference point to the given position
303
304       -T, --no-tweak
305              Don't fine-tune WCS by computing a SIP polynomial
306
307       -t, --tweak-order int
308              Polynomial order of SIP WCS corrections
309
310       -m, --temp-dir dir
311              Where to put temp files, default /tmp
312
313   The following options are valid for xylist inputs only:
314       -F, --fields number or range
315              The FITS extension(s) to solve, inclusive
316
317       -w, --width pixels
318              Specify the field width
319
320       -e, --height pixels
321              Specify the field height
322
323       -X, --x-column column-name
324              The FITS column containing the X coordinate of the sources
325
326       -Y, --y-column column-name
327              The FITS column containing the Y coordinate of the sources
328
329       -s, --sort-column column-name
330              The FITS column that should be used to sort the sources
331
332       -a, --sort-ascending
333              Sort  in ascending order (smallest first); default is descending
334              order
335
336       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

AUTHOR

341       The Astrometry.net team. Principal  investigators  are  David  W.  Hogg
342       (NYU) and Dustin Lang (CMU).
343

SEE ALSO

345       http://astrometry.net
346
347
348
3490.56                               July 2015                    SOLVE-FIELD(1)
Impressum