MUSE Pipeline Reference Manual
1.0.2
|
Variables | |
const muse_cpltable_def | muse_euro3dcube_e3d_data_def [] |
const muse_cpltable_def | muse_euro3dcube_e3d_grp_def [] |
const muse_cpltable_def | muse_dataspectrum_def [] |
const muse_cpltable_def | muse_sky_lines_lines_def [] |
const muse_cpltable_def | muse_sky_lines_oh_transitions_def [] |
const muse_cpltable_def | muse_line_catalog_def [] |
const muse_cpltable_def | muse_badpix_table_def [] |
The MUSE pipeline uses and produces a number of FITS tables in different formats, which are described in this section.
const muse_cpltable_def muse_badpix_table_def[] |
This is a FITS table with 24 extensions. This is used in the low-level recipes working on raw data. Each extension lists known bad pixels of one CCD.
Columns:
xpos
': X position of a bad pixel (on untrimmed raw data) [int]ypos
': Y position of a bad pixel (on untrimmed raw data) [int]status
': 32bit bad pixel mask as defined by Euro3D [int]value
': Extra value, e.g. depth for traps [float] Definition at line 753 of file muse_data_format_z.c.
Referenced by muse_quality_convert_dq().
const muse_cpltable_def muse_dataspectrum_def[] |
Spectral data from a datacube
Columns:
lambda
': Wavelength [double]data
': Data values [double]stat
': Data variance [double]dq
': Quality flag of data values [int] Definition at line 164 of file muse_data_format_z.c.
Referenced by muse_resampling_spectrum(), and muse_sky_spectrum_from_cube().
const muse_cpltable_def muse_euro3dcube_e3d_data_def[] |
Euro3D format. See Format Definition Document, Kissler-Patig et al., Issue 1.2, May 2003, for a description.
Contrary to the examples in the Euro3D specs we use floats instead of doubles for the entries in the group table. This is because the E3D tool is otherwise not able to read the values correctly.
This data format may be written alternatively to the common DATACUBE format, if the parameter &format& is set to &Euro3D& or &xEuro3D&.
Columns:
SPEC_ID
': Spectrum identifier [int]SELECTED
': Selection flag [int]NSPAX
': Number of instrument spaxels composing the spectrum [int]SPEC_LEN
': Useful number of spectral elements [int]SPEC_STA
': Starting wavelength of spectrum [int]XPOS
': Horizontal position [double]YPOS
': Vertical position [double]GROUP_N
': Group number [int]SPAX_ID
': Spaxel identifier [string]DATA_SPE
': Data spectrum [float array]QUAL_SPE
': Data quality spectrum [int array]STAT_SPE
': Associated statistical error spectrum [float array] Definition at line 66 of file muse_data_format_z.c.
Referenced by muse_resampling_euro3d().
const muse_cpltable_def muse_euro3dcube_e3d_grp_def[] |
Euro3D format. See Format Definition Document, Kissler-Patig et al., Issue 1.2, May 2003, for a description.
Contrary to the examples in the Euro3D specs we use floats instead of doubles for the entries in the group table. This is because the E3D tool is otherwise not able to read the values correctly.
This data format may be written alternatively to the common DATACUBE format, if the parameter &format& is set to &Euro3D& or &xEuro3D&.
Columns:
GROUP_N
': Group number [int]G_SHAPE
': Spaxel shape keyword [string]G_SIZE1
': Horizontal size per spaxel [float]G_ANGLE
': Angle of spaxel on the sky [float]G_SIZE2
': Vertical size per spaxel [float]G_POSWAV
': Wavelength for which the WCS is valid [float]G_AIRMAS
': Airmass [float]G_PARANG
': Parallactic angle [float]G_PRESSU
': Pressure [float]G_TEMPER
': Temperature [float]G_HUMID
': Humidity [float] Definition at line 124 of file muse_data_format_z.c.
Referenced by muse_resampling_euro3d().
const muse_cpltable_def muse_line_catalog_def[] |
This is a list of arc lines to be used for wavelength calibration. It is a FITS table, with one row for each line, which contains central wavelength of the line in question and a relative strength of the line, if known. The line fluxes may be used in the data reduction software as a first guess to the expected flux, the actual fluxes will be determined using line fitting. Additionally, to identify the lines and associate them with an arc lamp, a column ion (with element and ionization status) and a quality flag are needed. Optionally, a comment column might be useful.
Columns:
lambda
': Wavelength [float]flux
': Relative flux [float]ion
': Ion from which the line originates [string]quality
': Quality flag (0: undetected line, 1: line used for pattern matching, 2: line that is part of a multiplet, 3: good line, fully used, 5: bright and isolated line, use as FWHM reference [int]comment
': Optional comment [string] Definition at line 723 of file muse_data_format_z.c.
Referenced by muse_wave_lines_check().
const muse_cpltable_def muse_sky_lines_lines_def[] |
This type of file contains one or more binary tables with the relative fluxes on the sky emission lines. If both tables are present, they are merged, so that lines should not appear in both tables.
Columns:
name
': Line name [string]group
': Line group id [int]lambda
': Air wavelength [double]flux
': Line flux [double]dq
': Quality of the entry (>0: dont use) [int] Definition at line 469 of file muse_data_format_z.c.
Referenced by muse_sky_lines_load(), muse_sky_lines_save(), and muse_sky_master_load().
const muse_cpltable_def muse_sky_lines_oh_transitions_def[] |
This type of file contains one or more binary tables with the relative fluxes on the sky emission lines. If both tables are present, they are merged, so that lines should not appear in both tables.
Columns:
name
': Transition name; like "OH 8-3 P1e(22.5) 2" [string]lambda
': Air wavelength [double]v_u
': Upper transition level [int]v_l
': Lower transition level [int]nu
': Vibrational momentum [int]E_u
': Upper energy [double]J_u
': Upper momentum [double]A
': Transition probability [double] Definition at line 504 of file muse_data_format_z.c.