Joint Astronomy Centre
Show document only
JAC Home
JCMT
UKIRT
Contact info
JAC Divisions
OMP
Outreach
Seminars
Staff-only Wiki
Weather
Web Cameras
____________________

Observing at UKIRT
Service Observing
UKIDSS Survey Operations
Target of Opportunity
Calibration & Utilities
UKIRT Archive
Public wiki
Accessing Flexed Data
Accessing UKIDSS Data
Reduction Cookbooks
Telescope
Site Quality
Instruments
Newsletter/Publications
UKIRT Faults
JAC Safety Manual
USG: CGS4 sloping spectra
JACH | JCMT | UKIRT | Computer Services | USG

Previous: Curved Spectra | Up: USG Main Page | Next: Figaro Cookbook

Correcting sloping CGS4 spectra.

Most CGS4 users in semester 95A were affected by a mechanical problem that developed with the new rotating slit mechanism which was installed as part of the CGS4 upgrade. The result of this is most clearly visible in arc observations, where the arc lines are clearly tilted with respect to the direction perpendicular to the dispersion. OH lines will also be obviously tilted, and you will have to correct for the tilt before combining the two beams if you nodded along the slit, and before trying to fit to and remove any residual atmospheric lines.

Here are some suggestions for dealing with the above during data reduction with various software packages.

CGS4DR

It is not possible to corrrect the entire detector within CGS4DR. However for point sources you can calibrate the detector using the arc line at the row of your source. This will ensure your wavelength calibration is correct for your object. If you are nodding on the detector, repeat the process separately for the row with the nodded object.

Figaro

Use the ARC command to fit to a single spectrum which has been extracted from a row close to the centre of the image. Then use the IARC command to derive the fit across the detector, working from the centre outwards. It is important to answer yes to the IARC prompt "cross correlate to find shifts". Then use the ISCRUNCH command to apply the fit to straighten out the arc lines and your data frames (RO's or RG's).

IRAF

If you have been using IRAF to reduce your data, you have to use the tasks noao.twodspec.longslit.identify and reidentify as usual along some dispersion line. A 2-D fit of wavelength as a function of pixel co-ordinate can then be performed with the task fitcoords (also in the longslit package). Finally the transform task will perform the geometrical correction. For more information please see the User's Guide to Reducing Slit Spectra with IRAF (Massey, Valdes & Barnes, 1992).

Previous: Curved Spectra | Up: USG Main Page | Next: Figaro Cookbook

JACH | JCMT | UKIRT | Computer Services | USG

Last Modification Date 1995/09/13 - Last Modification Author: gsw
UKIRT Software Group ( uksg@jach.hawaii.edu)
Contact: Tom Kerr. Updated: Wed Oct 6 12:07:27 HST 2004

Return to top ^