Up: Modeling echelle spectrographs

# 5. Wavelength calibration of echelle spectra

In the following we take a closer look onto the practical use in wavelength calibration of the formalism developed so far and validated against two specific spectrographs. It is important to recall that we have started from text book physical principles, derived analytical equations and their simplifications for practical purposes with the primary goal to obtain robust procedures for improved calibration and data analysis.

## 5.1. Generating initial solutions

The model represents adequately all effects for off-plane spectrographs including line curvature with an accuracy close to one pixel. Because it is mostly based on linear algebra (see Appendix A), it is straight forward to produce high performance code. Such code can be used to generate accurate initial solutions of the dispersion relation using the grating positions as provided by encoders. This allows to implement fully automatic wavelength calibration procedures.

In cases where no grating positions are available, or where the zero points of such readings are unstable, one has to resort to interactive line identifications. Clearly, for these cases one will want to derive simple procedures and code. An important question therefore is how to make use of the special properties of the echelle relation in order to minimize the amount of such line identifications required to bootstrap a semi-automatic wavelength calibration procedure. In order to remain of any practical use, the simplified formalism still has to provide a local accuracy of a few resolution elements.

## 5.2. Simplified forms of the echelle relation

Using the set of equations presented in Appendix A, here with the approximation , and defining the intermediate quantities and as:

one derives for an in-plane spectrograph (s=0, ):

Because of the approximation this form for does not depend on the characteristics of the cross-disperser. In the absence of detector rotation (see also Hall et al. 1994) the product is constant for a given , i.e. a fixed column on the detector.

One can solve Eq. (26) for as

with the coefficients ai, i=0,..,4 involving the engineering parameters. If in addition the order curvature is negligible one can simplify further to a first order polynomial.

Usually in real instruments the alignment of the detector with the dispersion direction is not perfect. A misalignment by only 1 degree on a 1 K pixel detector amounts to an error of about 10 pixels at the edges. Hence, it is necessary to correct either the positions or the linear echelle relation for detector rotation.

In this case only three parameters will be needed to describe the initial relation. The value of this rotation angle may be determined geometrically, for example by comparing the difference in y position for a given wavelength in two adjacent orders.

This naive approximation would state that y-positions depend only on the characteristics of the cross-disperser. However, it can readily be seen that even under the assumptions from the start of this section, this is an over-simplification, because the expression of the position as it can be derived from the formalism in Appendix A involves both, and respectively. It is obvious that the y positions have to depend also on the dispersion relation of the echelle grating as well, because the combination of the two gratings produces the well known order curvature in echellograms. Therefore one cannot expect a sufficiently accurate determination of the rotation angle by simply comparing y-positions for fixed wavelengths. If the order curvature is significant one will need more identifications, and a least-square minimization of equation 28 (click here) as presented in Appendix B. Still this model based bootstrapping of the wavelength calibration requires less initial idenfications than 2d-polynomial methods as presented by e.g. Goodrich & Veilleux (1988) or Verschueren et al. (1997).

Up: Modeling echelle spectrographs

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