| System | Command | Arguments | Description | Type |
|---|
| alfosc |
alfosc-calibs |
[-e] [-skip] <date-string> |
Script to do biases and spectral calibs for all setups and windows used in a particular night.
Of course, this script should not be used for previous nights in case optical elements have been changed since.
The wheel setups are checked for inconsistencies in current vs stored wheel position content.
Any such inconsistent setup will be skipped, with a warning on the talker.
Command-line arguments:
[-e] echo mode: only show what will have be done in case started without the -e flag
<datestr> for expample 'ALwb13'
Spectroscopic and window setups are collected from the FITSheader database.
For all different window setups bias frames will be taken.
For all different setups with a grism in the beam, spectroscopic flats and arc-lamp spectra will be taken.
For flat/arc exposure times, alfosc.callampstimes is used.
Setups that are yet non-supported by alfosc.callampstimes will automatically be skipped, with a warning on the talker
When the flag -skip is given, the user is asked to specify interactively
from which GRISM or WINDOW setup to (re-)start alfosc-calibs.
Is supposed to work also for spectropolarimetry.
|
DATA |
| alfosc |
clearobject |
[-d] |
Clears the value of the FITS keyword OBJECT. |
DATA |
| alfosc |
clearobserver |
[-d] |
Clears the value of the FITS keyword OBSERVER. |
DATA |
| alfosc |
comment |
[-d] <text> |
Sets the FITS keyword COMMENT to <text>. Will be cleared after each image. FEB 13, 2013: This command is currently unavailable. |
DATA |
| alfosc |
filename |
[-d] <nn> |
Sets the default file name to <nn> (four characters). |
DATA |
| alfosc |
filenamestd |
[-d] |
Sets the filename back to the default file name. |
DATA |
| alfosc |
focuspyr |
|
Interactively examine a focus pyramid image to determine the focus offset required to bring the telescope in focus. The estimated best focus offset determined by the focuspyr-auto script will be presented on screen for comparison. |
DATA |
| alfosc |
focuspyr-auto |
[<file>] |
Computes the required telescope focus offset from a Focus Pyramid image <file>. If no input file is given (full path), the last image in the data directory will be used. |
DATA |
| alfosc |
imexam |
|
Initiates an IRAF imexam session on the image currently loaded into the ALFOSC DS9. While active in the imexam session, no further commands can be issued from the sequencer window. To kill the imexam session type q on the image in the postprocessing display.
CURSOR KEY COMMANDS:
? Print help
a Aperture radial photometry measurement (see above for output)
c Column plot
e Contour plot
f Redraw the last graph
j Fit 1D gaussian to image lines
k Fit 1D gaussian to image columns
l Line plot
m Statistics
image[section] npixels mean median stddev min max
q Quit
r Radial profile plot (see above for output)
s Surface plot
x Print coordinates
col line pixval [xorign yorigin dx dy r theta]
|
DATA |
| alfosc |
impath |
[-d] <text> |
Sets the path of the image saving to <text>. |
DATA |
| alfosc |
imtype |
[-d] <text> |
Sets the FITS keyword IMTYPE to <text>. |
DATA |
| alfosc |
log-comment |
"Comment in quotes" [file1 file2 ...] |
When invoked with just the comment, it will be applied to the latest available image with a prefix for the current night (which starts at noon) and the sequencer's instrument.
If image names are provided, the program will test the existence of ALL them before applying the change.
Eg.
$ alfosc.log-comment "This is a comment"
$ alfosc.log-comment "Comment for two" ALug170154 ALug170155
Notice that there's no need to add the ".fits" after each image's name
If no arguments are provided, a usage message is displayed |
DATA |
| alfosc |
object |
[-d] <text> |
Sets the FITS keyword OBJECT to <text>. |
DATA |
| alfosc |
observer |
[-d] <text> |
Sets the FITS keyword OBSERVER to <text>. |
DATA |
| alfosc |
photstd |
[-e] [-a mode] [-f filterIDs] |
Automatic exposure of standard stars.
Goes to nearest standard field and does exposures in filters UBVRi as default - or filters specified by the user.
Currently supports UBVRi and
in the future sdss ugriz. Other filters can be done, but will have the same exposure times, set by the variable default_time.
Instead of going to the nearest field, aquisition mode can be set to a specific target. The TCS name must be used, see http://www.not.iac.es/instruments/alfosc/photstd/.
Usage example:
alfosc.photstd -a A_PG1633+099 -f "74 75 120 110"
|
DATA |
| alfosc |
piname |
text |
Sets the value of the FITS keyword PINAME to "text". |
DATA |
| alfosc |
propid |
text |
Sets the value of the FITS keyword PROPID to "text". |
DATA |
| alfosc |
proptitl |
text |
Sets the value of the FITS keyword PROPTITL to "text". |
DATA |
| alfosc |
qicpol |
[<2ndfile>] |
Circular polarimetry quick-look tool (FAPOL+ calcite) which calculates the circular polarization from a set of two images (retarder plate positions 0 and 90.0 degrees). The flux of each image is measured with fixed aperture using iraf/apphot from raw images. See more detailed description of the script from here |
DATA |
| alfosc |
qilpol |
[<4thfile>] |
Linear polarimetry quick-look tool (FAPOL+ calcite) which calculates the linear polarization from a set of four images (retarder plate positions 0, 22.5 45 and 67.5 degrees). The flux of each image is measured with fixed aperture using iraf/apphot from raw images. See more detailed description of the script from here. |
DATA |
| alfosc |
quickspec |
[<file>] |
Extracts spectra and applies an approximate wavelength calibration on an ALFOSC spectroscopic image using the iraf tasks apall and dispcor. If no file is specified, spectral extraction from the last image written to disk will be attempted. Extracted spectra are kept in the directory /data/reduced/alfosc/ on the instrument computer. Existing spectra will be overwritten if the task is re-run on the same file. The wavelength calibration is done using standard wavelength settings for the standard horizontally oriented central slits. The wavelength calibration is only approximate, and is most likely based on a slit that you are not currently using. Note that the slits have different Y-positions and hence different wavelength zeropoints, and that hence zeropoint offsets of for instance 200 Ångström are normal. The quickspec will leave the user in an IRAF splot session. To kill the session type q in the postprocessing graphics window. There are 2 ways of initiating quickspec. Automatic (see command quickspec-config auto=yes below), and from the sequencer command line. * When called from the sequencer command line, all input and output will go through that sequencer terminal. * When automatic, the input and output goes through the BIAS 'command' window. |
DATA |
| alfosc |
quickspec-config |
[<options>] |
Use this command to set the IRAF apall task parameters used in the quickspec script.
auto=[yes|no] : Automatically run quickspec on incoming images
kill=[yes|no] : Automatically remove previous quickspec windows
default : loads default values.
Below parameters are specific for the apal iraf task:
background=[none|average|median|minimum|fit]
weights=[none|variance]
clean=[yes|no]
edit=[yes|no]
nfind=[1-10] (useful for Echelle spectra, MOS spectra, spectropolarimetry, and longslit spectra with more than one object on the slit) If the command is issued without any options, current parameter settings will be listed. |
DATA |
| alfosc |
rempath |
[-d] <nn> |
Sets the remote saving path to <nn>. |
DATA |
| alfosc |
remsave_off |
[-d] |
Turns off remote saving. |
DATA |
| alfosc |
remsave_on |
[-d] |
Turns on remote saving. |
DATA |
| alfosc |
remsystem |
[-d] <nn> |
Sets the remote host computer to <nn>. |
DATA |
| alfosc |
reset-log |
|
The script will use infosys.kill to reset the monitoring system, then it will wait for a set number of seconds, and at last it will instruct the obslog to show the listing for alfosc, all the while informing the user about what is happening
If there's any error, the script will notify the user and suggest further actions. |
DATA |
| alfosc |
restore-uparm |
|
Populates the iraf uparm directory, used by the pyraf based sequencer scripts, with some known working parameter files.
|
DATA |
| alfosc |
runselector |
<date> |
A command line frontend to set the PROPID,PROPTITL & PINAME fits keywords for the current observations. Choose the program being observed from a drop-down menu. The optional date argument displays programs for that date. |
DATA |
| alfosc |
runselectorUIF |
[alfosc|fies] <date> |
A GUI frontend to set the PROPID,PROPTITL & PINAME fits keywords for the current observations. Choose the program being observed from a drop-down menu. The optional date argument displays programs for that date. This GUI is started automatically when starting the observing system |
DATA |
| alfosc |
save |
[-d] |
Saves a read-out image to disk. |
DATA |
| alfosc |
slitrot |
|
Uses the currently loaded DS9 image to compute the TCS field rotation angle required to align two objects along a slit. The targets are identified interactively by the user through an imexam session. |
DATA |
| alfosc |
tweakmos |
[-e] <MASKfile.fits> <FIELDfile.fits> |
The routine will first display the mask image, and the user has to identify the fiducial holes one by one, using the pointer (please follow the on-line instructions in the Sequencer terminal).
Position the cursor over a fiducial hole and press 'a' (for centroiding) or 'x' (for cursor coordinates). This can be done multiple times until satisfied. When ready to go to the next hole press 'n'. Repeat until all fiducial holes are identified, and then press 'q'.
When all useful fiducial holes are marked, the object field is displayed and the position of the first alignment hole will be marked with a blue circle. Now try to identify the corresponding star on the image.
Position the cursor over the star corresponding to the blue circle and press 'a' (for centroiding) or 'x' (for cursor coordinates). This can be done multiple times until satisfied. When ready to go to the next star-hole pair press 'n'. Repeat until all fiducial stars are identified.
For further information:
http://www.not.iac.es/instruments/alfosc/mos-mode/tgt-aqu-new.html
|
DATA |
