1
2
3
4
5
6
7
8
9
10
11
12
13
14
15
16
17
18
19
20
21
22
23
24
25
26
27
28
29
30
31
32
33
34
35
36
37
38
39
40
41
42
43
44
45
46
47
48
49
50
51
52
53
54
55
56
57
58
59
60
61
62
63
64
65
66
67
68
69
70
71
72
73
74
75
76
77
78
79
80
81
82
83
84
85
86
87
88
89
90
91
92
93
94
95
96
97
98
99
100
101
102
103
104
105
106
107
108
109
110
111
112
113
114
115
116
117
118
119
120
121
122
123
124
125
126
127
128
129
130
131
132
133
134
135
136
137
138
139
140
141
142
143
144
145
146
147
148
149
150
151
152
153
154
155
156
157
158
159
160
161
162
163
164
165
166
167
168
169
170
171
172
173
174
175
176
177
178
179
180
181
182
183
184
185
186
187
188
189
190
191
192
193
194
195
|
.help calibrate Mar93 noao.onedspec
.ih
NAME
calibrate -- Apply extinction corrections and flux calibrations
.ih
USAGE
calibrate input output [records]
.ih
PARAMETERS
.ls input
List of input spectra to be calibrated. When using record format
extensions the root names are specified, otherwise full image names
are used.
.le
.ls output
List of calibrated spectra. If no output list is specified or if the
output name is the same as the input name then the calibrated spectra
replace the input spectra. When using record format extensions the output
names consist of root names to which the appropriate record number
extension is added. The record number extension will be the same as the
input record number extension. The output spectra are coerced to have
real datatype pixels regardless of the pixel type.
.le
.ls records (imred.irs and imred.iids only)
The set of record number extensions to be applied to each input and output
root name when using record number extension format. The syntax consists
of comma separated numbers or ranges of numbers. A range consists of
two numbers separated by a hyphen. This parameter is not queried
when record number formats are not used.
.le
.ls extinct = yes
Apply extinction correction if a spectrum has not been previously
corrected? When applying an extinction correction, an extinction file
is required.
.le
.ls flux = yes
Apply a flux calibration if a spectrum has not been previously calibrated?
When applying a flux calibration, sensitivity spectra are required.
.le
.ls extinction = <no default>
Extinction file for the observation. Standard extinction files
are available in the "onedstds$" directory.
.le
.ls observatory = ")_.observatory"
Observatory at which the spectra were obtained if not specified in the
image header by the keyword OBSERVAT. The default is a redirection to the
package parameter of the same name. The observatory may be one of the
observatories in the observatory database, "observatory" to select the
observatory defined by the environment variable "observatory" or the
parameter \fBobservatory.observatory\fR, or "obspars" to select the current
parameters in the \fBobservatory\fR task. See \fBobservatory\fR for
additional information.
.le
.ls ignoreaps = no
Ignore aperture numbers and apply a single flux calibration to all
apertures? Normally multiaperture instruments have separate sensitivity
functions for each aperture while long slit or Fabry-Perot data use a
single sensitivity function where the apertures are to be ignored. The
sensitivity spectra are obtained by adding the aperture number as an
extension to the sensitivity spectrum root name. When apertures are
ignored the specified sensitivity spectrum name is used without adding an
extension and applied to all input apertures.
.le
.ls sensitivity = "sens"
The root name for the sensitivity spectra produced by \fBsensfunc\fR.
Normally with multiaperture instruments, \fBsensfunc\fR will produce a
spectrum appropriate to each aperture with an aperture number extension.
If the apertures are ignored (\fIignoreaps\fR = yes) then the sensitivity
spectrum specified is used for all apertures and no aperture number is
appended automatically.
.le
.ls fnu = no
The default calibration is into units of flux per unit wavelength (F-lambda).
If \fIfnu\fR = yes then the calibrated spectrum will be in units of
flux per unit frequency (F-nu).
.le
.ls airmass, exptime
If the airmass and exposure time are not in the header nor can they be
determined from other keywords in the header then these query parameters
are used to request the airmass and exposure time. The values are updated
in the input and output images.
.le
.ih
DESCRIPTION
The input spectra are corrected for extinction and calibrated to a flux
scale using sensitivity spectra produced by the task \fBsensfunc\fR.
One or both calibrations may be performed by selecting the appropriate
parameter flags. It is an error if no calibration is specified. Normally
the spectra should be extinction corrected if also flux calibrating.
The image header keywords DC-FLAG (or the dispersion type field in the
"multispec" world coordinate system), EX-FLAG, and CA-FLAG are checked for
dispersion solution (required), previous extinction correction, and
previous flux calibration. If previously calibrated the spectrum is
skipped and a new output image is not created.
The input spectra are specified by a list of root names (when using record
extension format) or full image names. The output calibrated spectra may
replace the input spectra if no output spectra list is specified or if the
output name is the same as the input name. When using record number
extensions the output spectra will have the same extensions applied to the
root names as those used for the input spectra.
When applying an extinction correction the AIRMASS keyword is sought.
If the keyword is not present then the airmass at the time defined
by the other header keywords is computed using the
latitude of the observatory and observation parameters in the image
header. The observatory is first determined from the image under the
keyword OBSERVAT. If absent the observatory specified by the task
parameter "observatory" is used. See \fBobservatory\fR for further
details of the observatory database. If the air mass cannot be
determined an error results. Currently a single airmass is used
and no correction for changing extinction during the observation is
made and adjustment to the middle of the exposure. The task
\fBsetairmass\fR provides a correction for the exposure time to compute
an effective air mass. Running this task before calibration is
recommended.
If the airmass is not in the header and cannot be computed then
the user is queried for a value. The value entered is then
recorded in both the input and output image headers. Also if
the exposure time is not found then it is also queried and
recorded in the image headers.
The extinction correction is given by the factor
10. ** (0.4 * airmass * extinction)
where the extinction is the value interpolated from the specified
extinction file for the wavelength of each pixel. After extinction
correction the EX-FLAG is set to 0.
When applying a flux calibration the spectra are divided by the
aperture sensitivity which is represented by a spectrum produced by
the task \fBsensfunc\fR. The sensitivity spectrum is in units of:
2.5 * Log10 [counts/sec/Ang / ergs/cm2/sec/Ang].
A new spectrum is created in "F-lambda" units - ergs/cm2/sec/Angstrom
or "F-nu" units - ergs/cm2/sec/Hz. The sensitivity must span the range of
wavelengths in the spectrum and interpolation is used if the wavelength
coordinates are not identical. If some pixels in the spectrum being
calibrated fall outside the wavelength range of the sensitivity function
spectrum a warning message giving the number of pixels outside the
range. In this case the sensitivity value for the nearest wavelength
in the sensitivity function is used.
Multiaperture instruments typically have
a separate aperture sensitivity function for each aperture. The appropriate
sensitivity function for each input spectrum is selected based on the
spectrum's aperture by appending this number to the root sensitivity function
spectrum name. If the \fIignoreaps\fR flag is set, however, the aperture
number relation is ignored and the single sensitivity spectrum (without
extension) is applied.
.ih
EXAMPLES
1. To flux calibrates a series of spectra replacing the input spectra by
the calibrated spectra:
cl> calibrate nite1 ""
2. To only extinction correct echelle spectra:
cl> calibrate ccd*.ec.imh new//ccd*.ec.imh flux-
3. To flux calibrate a long slit spectrum:
.nf
cl> dispaxis = 2
cl> calibrate obj.imh fcobj.imh
.fi
.ih
REVISIONS
.ls CALIBRATE V2.10.3
This task was revised to operate on 2D and 3D spatial spectra; i.e. long
slit and Fabry-Perot data cubes. This task now includes the functionality
previously found in \fBlongslit.extinction\fR and \fBlongslit.fluxcalib\fR.
A query for the airmass and exposure time is now made if the information
is not in the header and cannot be computed from other header keywords.
.le
.ls CALIBRATE V2.10
This task was revised to operate on nonlinear dispersion corrected spectra
and 3D images (the \fBapextract\fR "extras"). The aperture selection
parameter was eliminated (since the header structure does not allow mixing
calibrated and uncalibrated spectra) and the latitude parameter was
replaced by the observatory parameter. The observatory mechanism insures
that if the observatory latitude is needed for computing an airmass and the
observatory is specified in the image header the correct calibration will
be applied. The record format syntax is available in the \fBirs/iids\fR
packages. The output spectra are coerced to have real pixel datatype.
.le
.ih
SEE ALSO
setairmass, standard, sensfunc, observatory, continuum
.endhelp
|
