This page (revision-57) was last changed on 07-Dec-2016 14:14 by David R Williams

This page was created on 09-Jul-2008 07:16 by David R Williams

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[{ALLOW edit EISMainUsers}]
[{ALLOW view Anonymous}]
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The most critical part of the raster description that ''isn't'' summarised in the ''Raster Title'' is the Line List. This is because the line list is too variable to easily summarised. So, it gets its own panel in the raster description.\\
The most critical part of the raster description that __isn't__ summarised in the ''Raster Title'' is the Line List. This is because the line list is too variable to easily summarised. So, it gets its own panel in the raster description.
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Note that, like studies and rasters, line lists have and ID and acronym.
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You'll see that, like the raster, a Lin
You'll see that, like the raster, a Line List has a one-line so-called ''Title'' string associated with it. Since this is truncated, it doesn't serve much purpose, and we'll skip it here.
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Again, fairly self-explanatory\\
:-)
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One point to perhaps reiterate, though, is that you can use a line list created by anyone else in your study. All line lists, rasters, and studies in the OSDB are there to be re-used and cannibalised by anyone wanting to propose an observation.
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There can be up to 25 spectral windows in a line list, but the minimum is normally three: the core lines. The core lines are
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||Ion||Wavelength (Å)
|Fe XII |195.12
|Ca XVII|192.82
|He II |256.32
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Each spectral window can have a width that is an integer multiple of 8, from 8 to 1024 (half a CCD width), and there can be up to 25 windows, each with independent widths. In the example image above, you can see that most windows have a width of 24 pixels (a little over 0.5 Å), which is usually adequate. But a few windows,
Each spectral window can have a width that is an integer multiple of 8, from 8 to 1024 (half a CCD width), and there can be up to 25 windows, each with independent widths. In the example image above, you can see that most windows have a width of 24 pixels (a little over 0.5 Å), which is usually adequate. But a few windows are wider (32, 40 or 48 pixels). Wider windows often (but don't necessarily) indicate that the line list author was trying to capture other lines by using a wider spectral window.
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This also helps to explain why the core lines of {{Fe XII}} (195.12 Å) and {{Ca XVII}} (192.82 Å) aren't explicitly included in this line list: they are already covered by the {{Fe XII}} window at 194.91 Å and the {{O V}} window at 192.84 Å, respectively.
This page (revision-57) was last changed on 07-Dec-2016 14:14 by David R WilliamsTop