SINFONI Pipeline Reference Manual  2.5.2
sinfo_new_slit_pos.h
1 #ifndef SINFO_NEW_SLIT_POS_H
2 #define SINFO_NEW_SLIT_POS_H
3 /*
4  * This file is part of the ESO SINFONI Pipeline
5  * Copyright (C) 2004,2005 European Southern Observatory
6  *
7  * This program is free software; you can redistribute it and/or modify
8  * it under the terms of the GNU General Public License as published by
9  * the Free Software Foundation; either version 2 of the License, or
10  * (at your option) any later version.
11  *
12  * This program is distributed in the hope that it will be useful,
13  * but WITHOUT ANY WARRANTY; without even the implied warranty of
14  * MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the
15  * GNU General Public License for more details.
16  *
17  * You should have received a copy of the GNU General Public License
18  * along with this program; if not, write to the Free Software
19  * Foundation, 51 Franklin St, Fifth Floor, Boston, MA 02111-1307 USA
20  */
21 /*****************************************************************************
22 * E.S.O. - VLT project
23 *
24 * "@(#) $Id: sinfo_new_slit_pos.h,v 1.5 2007-06-06 07:10:45 amodigli Exp $"
25 *
26 * who when what
27 * -------- -------- ----------------------------------------------
28 * amodigli 17/09/03 created
29 */
30 
31 /************************************************************************
32  * sinfo_new_slit_pos.h
33 
34  Normal method:
35 
36  does the wavelength calibration and the fitting of the slitlet sinfo_edge
37  positions (ASCII file 32 x 2 values) if wished
38  produces an array of the bcoefs and of the fit parameters if wished and a
39  wavelength calibration map input is an emission line frame and a line list
40 
41  o searching for lines by cross sinfo_correlation with a line list
42  o Gaussian fitting of emission lines in each column->positions of the lines->
43  resulting fit parameters can be stored in an ASCII file
44  o Fitting of a polynomial to the line positions for each column
45  o Smoothing: fitting of each polynomial coefficient by another polynomial
46  across the whole frame -> resulting polynomial coefficients can be stored
47  in an ASCII file.
48  o Wavelength calibration map (micron value for each frame pixel) can be
49  produced by using these coefficients and a cross sinfo_correlation to the
50  original frame
51 
52  o The slitlet sinfo_edge positions can be fitted:
53  1) Automatically (not really stable) or by using guess sinfo_edge positions
54  2) By using a Boltzmann or a linear slope function
55 
56 
57  Slit method:
58 
59  does the wavelength calibration and the fitting of the slitlet sinfo_edge
60  positions (ASCII file 32 x 2 values) if wished produces a list of the fit
61  parameters and of the smoothed coefficients if wished and a wavelength
62  calibration map input is an emission line frame and a line list
63 
64  o Does the same as other method but smoothes the found polynomial
65  coefficients within each slitlet and not over the whole frame.
66 
67  o Produces always a wavelength calibration map and does not crosscorrelate.
68 
69  *----------------------------------------------------------------------
70  */
71 
72 /*
73  * header files
74  */
75 #include <cpl.h>
76 #include "sinfo_msg.h"
77 
78 
79 /*----------------------------------------------------------------------------
80  * Function ANSI C prototypes
81  *--------------------------------------------------------------------------*/
82 
83 /*----------------------------------------------------------------------------
84  Function : sinfo_new_slit_pos()
85  In : ini_file: file name of according .ini file
86  Out : integer (0 if it worked, -1 if it doesn't)
87  Job :
88 
89 
90  Normal method:
91 
92  does the wavelength calibration and the fitting of the slitlet sinfo_edge
93  positions (ASCII file 32 x 2 values) if wished
94  produces an array of the bcoefs and of the fit parameters if wished and a
95  wavelength calibration map input is an emission line frame and a line list
96 
97 
98  o searching for lines by cross sinfo_correlation with a line list
99  o Gaussian fitting of emission lines in each column->positions of the lines->
100  resulting fit parameters can be stored in an ASCII file
101  o Fitting of a polynomial to the line positions for each column
102  o Smoothing: fitting of each polynomial coefficient by another polynomial
103  across the whole frame -> resulting polynomial coefficients can be stored
104  in an ASCII file.
105  o Wavelength calibration map (micron value for each frame pixel) can be
106  produced by using these coefficients and a cross sinfo_correlation to the
107  original frame
108 
109  o The slitlet sinfo_edge positions can be fitted:
110  1) Automatically (not really stable) or by using guess sinfo_edge positions
111  2) By using a Boltzmann or a linear slope function
112 
113  Slit method:
114 
115  does the wavelength calibration and the fitting of the slitlet sinfo_edge
116  positions (ASCII file 32 x 2 values) if wished produces a list of the fit
117  parameters and of the smoothed coefficients if wished and a wavelength
118  calibration map input is an emission line frame and a line list
119 
120  o Does the same as other method but smoothes the found polynomial
121  coefficients within each slitlet and not over the whole frame.
122 
123  o Produces always a wavelength calibration map and does not crosscorrelate.
124  ---------------------------------------------------------------------------*/
125 int sinfo_new_slit_pos (cpl_parameterlist* config, cpl_frameset* sof) ;
126 
127 
128 #endif
129 
130 /*--------------------------------------------------------------------------*/