Astronomical Spectroscopy - Physics - University of Cincinnati
Astronomical Spectroscopy - Physics - University of Cincinnati
Astronomical Spectroscopy - Physics - University of Cincinnati
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– 69 –<br />
red (including at least 7770-8700Å) but also in the blue to obtain some <strong>of</strong> the classical luminosity<br />
indicators used for Galactic yellow supergiants. To observe each fiber configuration<br />
twice, on “blue nights” and “red nights” would require twice as many observing nights, given<br />
the large overhead in each fiber configuration.<br />
The fibers feed a bench spectrograph mounted in a dark room a floor below the telescope.<br />
Changing the grating tilt might require refocusing the spectrograph (a manual operation,<br />
impractical at night) but simply changing blocking filters could be done remotely. If the<br />
filters were <strong>of</strong> similar thickness, and if the camera’s focus was fairly achromatic (which<br />
would be expected <strong>of</strong> a Schmidt camera) then one could configure the fibers, observe in the<br />
red, and simply by changing blocking filters, observe in the blue. No one was quite sure if<br />
this would work, as no one could remember the spectrograph having been used this way, but<br />
it would be easy enough to check on the first afternoon <strong>of</strong> the run. A 790 line/mm grating<br />
blazed at 8500Å in first order was available, and would yield 2.6Å resolution in the red in<br />
first order, and 1.3Å resolution in the blue in second order, providing wavelength coverage<br />
<strong>of</strong> 7300-9050Å in the red and 3650-4525Å in the blue. Obviously the red observations would<br />
require a blocking filter that removed light 7300Å. Among the available filters, an OG515<br />
did an excellent job in the first case, and a BG39 did a good job in the second case while<br />
still transmitting well over the region <strong>of</strong> interest (see Figure 3). (The same argument was<br />
presented above in § 2.2.1.)<br />
Prior to the observing run, thirty fiber configuration fields had been designed in order<br />
to obtain as many <strong>of</strong> the target stars as possible. Since bad weather is always a possibility<br />
(even at Cerro Tololo) the fields were designed in a particular order, with field centers chosen<br />
to include the maximum number <strong>of</strong> stars that had not been previously assigned. Although<br />
the fiber configuration program is flexible in providing various weighting schemes for targets,<br />
it was found necessary to slightly rewrite the code to allow for stars that had been previously<br />
assigned to be added “for free”, i.e., without displacing any not-yet assigned star. (It helped<br />
that the first author had written the original version <strong>of</strong> the code some years back.) The<br />
process took a week or more to refine the code, but the assignments themselves then were<br />
straightforward.<br />
The first afternoon at the telescope, the astronomers arrived to find that everything<br />
appeared to be in good shape. Instrument support personnel had inserted the grating and<br />
blocking filter, checked the grating tilt, and had focused the spectrograph, substantiating the<br />
fact that the focus was unchanged between the red and the blue setups. A comparison arc<br />
had been used to focus the spectrograph, and examination confirmed the expectation that<br />
at the best focus the spectral resolution covered about seven pixels. The observers decided