Tips for Visiting Astronomers

For a quick look to the data, IRAF can be used in combination with the pipeline products and/or eclipse. IRAF is started in wgsoff1 typing "cl". To open the ds9 display type "ds9" within the IRAF terminal.

Imaging

Reduced images will be available for the modes supported by the pipeline in the directory /data-ut1/reduced/YYYY-MM-DD. They can be loaded and inspected with GASGANO.

The Zero Points obtained by the pipeline from the observed standard stars are stored in the header of the reduced images: /data-ut1/reduced/YYYY-MM-DD/r.ISAAC*_tpl_0000.fits

type

> dfits r.ISAAC*_tpl_0000.fits |fitsort QC.FILTER.OBS QC.ZPOINT

to view the zero point.

Photometry can be performed on the reduced images using the task "phot" in IRAF after updating the parameters "datapar", "photpar", "fitskypar" and "centerpar".

Spectroscopy

Two-D reduced spectra will be available for the modes supported by the pipeline in the directory /data-ut1/reduced/YYYY-MM-DD. One-D spectra are extracted by the pipeline and stored in tfits tables. These tables can be converted into fits files using the IRAF scripts "readtf_one" and/or "readtf_many". They take in input one single tfits file and a list of them, respectively. Two spectra are generated as output, one containing the extracted spectrum of the source, the other containing the spectrum of the sky that can be used for wavelenght calibration purposes. The 1-D fits files can be displayed using "splot" in IRAF.

Alternatively 1-D spectra can be extracted using "apall" in IRAF. Apall expects the dispersion direction to be vertical so the 2-D ISAAC spectra must be either rotated by 90 deg or the keyword "DISPAXIS" must be add to the header and set to 1. To edit the header use "hedit".

Arithmetic operations between spectra can be executed with "sarith" or "imarith".

To use the pipeline's recipes in an independent form:

> isaacp

gives a list of the recipes available

> isaacp man recipe_name

provides the help of the particular recipe.