UKIRT
Show document only
UKIRT Home
Contact Info
OMP
UKIRT Staff wiki
Weather
Web Cameras
____________________

Survey Observing
Other Observing
Observing Tool Manual
Schedule
Applying For Time
Get UKIDSS Data
Get non-UKIDSS Data
Data Reduction
Acknowledge Us
Telescope
WFCAM
Cassegrain
Technical Reference
UKIRT Publications
Graphical Weather Server
EAO Safety Manual
UKIRT Waiver Form
TSS Priority Page
Continuing Observations

Continuing Observations

Once you have completed a pair of main and offset beam observations, the pipeline forms a group file, into which it subtracts the main and offset images. This image is then displayed in a seperate GAIA window, the spectrum extracted from both rows in it is displayed in the top half of a second KAPPA window and the y-profile is displayed on the lower left of the first KAPPA window and mentioned above. Examples:

If this object has been flagged as a standard star (in the OT), then the pipeline will consult the BS catalogue or SIMBAD to determine the spectral type (and hence temperature) and V magnitude of the star (which are displayed in the extracted spectrum title). It will use these to create a black body model of the star (nb. no interpolation over stellar features currently takes place), which will be used to flux calibrate subsequent data.

As soon as you have observed a non standard star tagret in the main and offset beam positions, a group file will be created and displayed and spectra will be extracted and displayed as before. An additional KAPPA window is created to show you the extracted spectrum (_sp) and flux calibrated (fc) spectra. These are obviously all updated as more data is observed and signal to noise ratio is accumulated. Examples follow:

/

Contact: Tom Kerr. Updated: Wed Oct 6 11:54:13 HST 2004

Return to top ^