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Analysis and Interpretation of Astronomical Spectra 38

8.15 Summary – Which Method Fits to Which Task
The following table provides an overview of which calibration-, normalisation- or radiomet-
ric correction methods are appropriate, or even required for the following tasks.

Legend: R = Requirement B = Best option, P = possible option

Methods of Cali- Relative λ-Calibration with
bration, Normali- known Lines
sation or Radio- Absolute λ- Calibration with
metric correction calibration-light-source
Pseudo-continuum of the raw
Task profile
Rectified continuum,
normalised to
Relative Flux calibration with
synthetic model star
Relative Flux calibration with
recorded standard star
Scaling of emission-intensities
to theor. Balmer Decrement
Absolute Flux calibration

Calibration of the profile to the rest R
wavelength λ0

Absolute calibration of the profile to R
the measured wavelength λ

Measurement of the relative RPPBPP P
difference Δλ P
P
Absolute Measurement of the RPBPP
Doppler shift

Measurement of FWHM PPPBPP

Measurement of EW PP R

Determination of the spectral class B P P B B B

Optical intensity comparison of the P P R
absorption lines B P R

Measurement of the reddened P P BP P
Balmer -Decrement
Estimation of the original IE- and IA- P P BP P
values in the unreddened original P P
profile P P R
Comparison of the absorbed fluxes P P
at different absorption lines R R

Evaluation of the emission intensi- R
ties (eg for plasma diagnostics)
R
Estimation of the effective tempera-
ture Teff based on continuum slope

Fluctuations of the continuum
radiation

Profile processing for certain, scien-
tific databases

Flux measurement in physical units P P E