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#ifndef SINFO_NEW_CUBES_COADD_H
#define SINFO_NEW_CUBES_COADD_H
/*
* This file is part of the ESO SINFONI Pipeline
* Copyright (C) 2004,2005 European Southern Observatory
*
* This program is free software; you can redistribute it and/or modify
* it under the terms of the GNU General Public License as published by
* the Free Software Foundation; either version 2 of the License, or
* (at your option) any later version.
*
* This program is distributed in the hope that it will be useful,
* but WITHOUT ANY WARRANTY; without even the implied warranty of
* MERCHANTABILITY or FITNESS FOR A PARTICULAR PURPOSE. See the
* GNU General Public License for more details.
*
* You should have received a copy of the GNU General Public License
* along with this program; if not, write to the Free Software
* Foundation, 51 Franklin St, Fifth Floor, Boston, MA 02111-1307 USA
*/
/*******************************************************************************
* E.S.O. - VLT project
*
* "@(#) $Id: sinfo_new_cubes_coadd.h,v 1.10 2007-06-06 07:10:45 amodigli Exp $"
*
* who when what
* -------- -------- ----------------------------------------------
* schreib 06/05/03 created
*/
/************************************************************************
* sinfo_new_cubes_coadd.h
* routines to create a data cube
*----------------------------------------------------------------------
*/
/*
* header files
*/
#include <math.h>
#include <cpl.h>
#include "sinfo_msg.h"
/*----------------------------------------------------------------------------
* Function ANSI C prototypes
*--------------------------------------------------------------------------*/
/*----------------------------------------------------------------------------
@name sinfo_new_cubes_coadd()
@param ini_file: file name of according .ini file
@param integer (0 if it worked, -1 if it doesn't)
@doc this routine does the resampling of an offset-corrected,
flatfielded, bad pixel corrected and
eventually interleaved data frame. Additionally, an intensity
calibration is carried through by using
a standard star or a black body measurement.
The spectral features of the flatfield halogen lamp are corrected.
Afterwards a data cube is created out of the resampled image.
It is the users choice to use either
the fitted sinfo_edge positions of the slitlets or the distances
of the slitlets gained from a north-south-test.
---------------------------------------------------------------------------*/
int
sinfo_new_cubes_coadd (const char* plugin_id,
cpl_parameterlist* config,
cpl_frameset* sof,
const char* procatg) ;
#endif /*!SINFO_CUBES_COADD2_H*/
/*--------------------------------------------------------------------------*/
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