Astronomical Spectroscopy - Physics - University of Cincinnati
Astronomical Spectroscopy - Physics - University of Cincinnati
Astronomical Spectroscopy - Physics - University of Cincinnati
Create successful ePaper yourself
Turn your PDF publications into a flip-book with our unique Google optimized e-Paper software.
– 17 –<br />
each order (Equation 9). This is apparent from Figure 5, as the shorter wavelengths (higher<br />
orders) span less <strong>of</strong> the chip. At lower orders the wavelength coverage actually exceeds the<br />
length <strong>of</strong> the chip. Note that the same spectral feature may be found on adjacent orders,<br />
but usually the blaze function is so steep that good signal is obtained for a feature in one<br />
particular order. This can be seen for the very strong H and K Ca II lines apparent near the<br />
center <strong>of</strong> order 16 and to the far right in order 15 in Figure 5.<br />
If a grating is used as the cross disperser, then the separation between orders should<br />
increase for lower order numbers (larger wavelengths) as gratings provide fairly linear dispersion<br />
and the free spectral range is larger for lower order numbers. (There is more <strong>of</strong> a<br />
difference in the wavelengths between adjacent orders and hence the orders will be more<br />
spread out by a cross-dispersing grating.) However, Figure 5 shows that just the opposite<br />
is true for MagE: the separation between adjacent orders actually decreases towards lower<br />
order numbers. Why MagE uses prisms for cross-dispersing, and (unlike a grating) the<br />
dispersion <strong>of</strong> a prism is greater in the blue than in the red. In the case <strong>of</strong> MagE the decrease<br />
in dispersion towards larger wavelength (lower orders) for the cross-dispersing prisms more<br />
than compensates for the increasing separation in wavelength between adjacent orders at<br />
longer wavelengths.<br />
Some echelle spectrographs are listed in Table 3. HIRES, UVES, and the KPNO 4-m<br />
echelle have a variety <strong>of</strong> gratings and cross-dispersers available; most <strong>of</strong> the others provide<br />
a fixed format but give nearly full wavelength coverage in the optical in a single exposure.<br />
Table 3. Some Echelle Spectrographs<br />
Instrument Telescope R (1 arcsec slit) Coverage(Å) Comments<br />
HIRES Keck I 39,000 Variable<br />
ESI Keck II 4,000 3900-11000 Fixed format<br />
UVES VLT-UT2 40,000 Variable Two arms<br />
MAESTRO MMT 28,000 3185-9850 Fixed format<br />
MIKE Magellan II 25,000 3350-9500 Two arms<br />
MagE Magellan II 4,100