Astronomical Spectroscopy - Physics - University of Cincinnati
Astronomical Spectroscopy - Physics - University of Cincinnati
Astronomical Spectroscopy - Physics - University of Cincinnati
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– 78 –<br />
as needed between sets. Finally, always check, as the data is coming in, that when you do<br />
subtract one slit (or sky <strong>of</strong>fset) position from another that you do get zero counts outside<br />
<strong>of</strong> the star. What can go wrong here, as was mentioned in § 2.5.2, is that the strengths<br />
<strong>of</strong> the OH bands vary with time. This is particularly true if clouds move in or the seeing<br />
changes between slit positions, with the result that the OH lines will not cancel entirely and<br />
reduction will be much more difficult. If this occurs, one is forced to use a shorter integration<br />
per step to find a time frame over which the sky emission is sufficiently stable.<br />
Note that even if one does have “perfect” sky subtraction <strong>of</strong> the OH spectra, the large<br />
signal in the OH lines invariably adds noise to the final reduced spectra. This is unavoidable,<br />
and makes the entire concept <strong>of</strong> defining the signal-to-noise-ratio in the NIR tricky to define,<br />
as it is bound to vary depending upon the OH spectra within a particular region.<br />
What could possibly go wrong A lot. The second author has never worked on an<br />
infrared spectrometer that didn’t <strong>of</strong>fer additional challenges which fell outside the standard<br />
operation as listed above. To keep this brief, four <strong>of</strong> the most common problems that occur<br />
will now be discussed. They include: flexure, fringing, wavelength calibration problems,<br />
and poor telluric matching. Each <strong>of</strong> these can lead to greatly reduced signal-to-noise in the<br />
spectra, far below what would be predicted by counts alone.<br />
• Flexure. No spectrograph is absolutely rigid! Flexure can be a larger issue for infrared<br />
spectrographs because the optics must be cooled to reduce the thermal background, and<br />
it is challenging to minimize the thermal conduction to the internal spectrograph bench<br />
while also minimizing the mechanical flexure between the bench and outer structure <strong>of</strong><br />
the instrument. Depending on how the instrument is mounted, when observing to the<br />
east, versus looking to the west, for instance, or as the telescope passes meridian, the<br />
internal light path will shift due to structure shifts. The amount <strong>of</strong> flexure depends<br />
on the instrument and telescope set up. Previous users or the support astronomer for<br />
the instrument can help the new user decide if this needs to be considered and how<br />
to mitigate the effects. This is best addressed during the observing, keeping telluric<br />
standards, lamps and objects on the same side <strong>of</strong> the meridian for instance.<br />
• Fringing. Optical CCDs fringe in the red wavelength regions due to interference<br />
within the surface layers <strong>of</strong> the detector; for IR spectrographs, fringing can occur due<br />
to parallel optical surfaces, such as blocking filters, in the optical path. While in<br />
principle, this should cancel out with the dome flats, due to flexure in the system and<br />
light path differences, they typically do not cancel well. Common remedies include<br />
obtaining quartz lamps at the exact same sky location as the observations. This might<br />
work and should be included in the observing plan. However, the fringes are <strong>of</strong>ten not