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Astronomical Spectroscopy - Physics - University of Cincinnati

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– 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

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