One stage in the analysis of your spectrum may be the comparison of your data against standard spectra. Comparisons may be made with blackbody curves, camera artifacts, Kurucz (both the latest, unpublished models and those published in 1979, Ap. J. Suppl. Ser. 40,1) model atmosphere calculations, and with representative standard stars.
Long exposures may contain camera artifacts that look like features. Spectra showing these artifacts have been generated that you may wish to compare with your data. You can fetch these spectra by executing the following procedure:
You will be prompted for the camera name (LWP, LWR, or SWP), and processing type (point source or extended source) or order number (for high dispersion artifacts). The available spectra are averages of numerous sky background images (processed with IUESIPS) with exposure times of at least three hours.
You may generate a black body curve and scale it to match your data. The program BBDRAW will plot your data and allow you to select temperatures and see the resulting curves until you tell it to quit.
|WPICK||Wavelength of the point used to scale the black body curve.|
|TEMP||Temperature of black body curve last chosen by you.|
|DILUTION||Scale factor used to scale the black body curve to your data.|
|WBB||Wavelengths of black body curve.|
|FBB||Fluxes of black body curve.|
|q||Data quality flags ( or ), if you wish to see them displayed.|
|sigma||The NEWSIPS vector (or other fitting error, e.g., from GEX), if the user wishes to display it.|
You will be offered the chance to create a PS file containing a plot of your data with the final fitted curve.