To perform GPI’s exoplanet characterization science goals requires a wavelength precision of ~1%. However, the uniformity of the datacube is greatly increased with a better quality calibration. Performing a robust, high-accuracy wavelength calibration with GPI has been on of the primary challenges of the pipeline development. Similar to other near-IR spectrographs, GPI uses the well calibrated emission lines of a Xenon lamp (Argon also works for Y-band). The current accuracy of the wavelength calibration is below 0.5% for all bands. A new calibration based on forward modeling is also being developed. This routine is expected to both increase the robustness and precision of the calibration
Most data reduction recipes for raw GPI data will begin by loading a wavelength calibration using the pipeline primitive Load Wavelength Calibration. Typically the calibration is obtained automatically from the Calibration Database based on the closest-in-time wavelength calibration file. There are no significant user-selectable options for this step to be concerned with.
Calibration DB File Type: Wavelength Solution Cal File
File Suffix: wavecal
Generate with Recipe: “Wavelength Solution”
Take a series of arc lamp exposures (multiple exposures to increase S/N). Reduce these using the ‘Wavelength Solution’ recipe. This will create a references datacube that provides the starting x and y positions, the wavelength at those positions, the wavelength dispersion, and the tilt angle for each lenslet spectrum. This data cube may then be used to extract full spectral data cubes from science data.
The Xenon arc lamp spectrum has more cleanly separated emission lines, but with our updated algorithms we now believe the pipeline can derive good wavelength calibrations from either Xe or Ar. The GCAL Ar lamp is 3-10x brighter depending on wavelength so the integration times are favorable. In general, Gemini instrument scientists will ensure proper calibration data are taken for wavecals.
This recipe is computationally intensive, and will take tens of minutes to run on typical machines.
Performing the wavelength calibrations are quite simple but ensuring that the determination was successful does require examination of the solution in GPItv (see the Displaying GPI Wavelength Calibration feature documentation). As the Gaussian fitting routines that determine the locations of the of spots are sensitive to bad pixels, it is recommended that a recent badpixel mask is used. The following figure shows the successful completion of a wavelength calibration.
The following figure demonstrates an unsuccessful calibration due to a bad pixel. The image shows the full detector, where the grid and dispersion lines appear uniform, only a small variation is seen in the lower right hand corner.
The following image shows a zoom on this region. The user should note that is an example of failure which is very difficult to see.
A successful determination of the calibration will show a clean grid of centroids (intersection of the red lines) with identical length dispersion axes (shown as green lines).
If you do experience a failed wavelength calibration, first check to make sure the correct dark and badpixel mask were used. If so, then one may modify the maxpos and maxtilt parameters. One may also change the interpolation type of the bad-pixel interpolation. In extreme cases, the bad pixel could be added to the mask manually, although this has never been necessary.
Schuyler Wolff, Zack Draper, Marshall Perrin