====OBSERVING THE SUN.====
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For solar observations the WLS has a dedicated portable telescope which shows the sun in Hα light (656.28 nm). The bandpass is very small: with the basic set-up "single stack" less than 0.075 nm (0.75 Å), and about half of this (0.055 nm) with the second "double stack" filter added in front of the objective.
Appropriate 1¼" eyepieces have focal lenghths of 25 mm and 12 mm. Take care: the tuning system regulation air pressure uses a piston at the bottom side of the telescope. The knob hase a range of about 3 cm. // Do not use more than the first 2 cm of this range.// The knob is not secured and can come loose. This is not harmfull but it is very difficult to reattach it. If that happens do not use force and expect it to take an hour or so
 to find the reconnection...\\ The telescope tube is mounted on a parallactic mount with an electric drive requiring a 6V power source.\\ 
The telescope is easy to assemble, and use, but very sensitive. Before using it personal instruction is required.\\ 
Solar Lunt instruction(dutch):{{:telescopes:lunt_ls60tha_instructie.pdf|Lunt LS60 handleiding}}\\
Vixen Great Polaris (GP)-DX mount:{{:telescopes:great_polaris_mount_vixen_northamerica.pdf|Vixen GP Manual}}\\ 
Solar Lunt telescope: {{:telescopes:ls60tha_manual.pdf|Lunt LS60 manual}}

===Specification LS60THα Solar Telescope===  
  * Ultra-Narrow Band Hydrogen-alpha (656.28nm) Dedicated System
  * Double-Stacked with Pressure Tuner
  * A 60mm refractor basic system with additional 50mm aperture secondary removable filter.
  * Dual etalons with “Pressure Tuner” allowing for <0.5 Angstrom bandpass.
  * Type: Dual Interference Etalon{{ :telescopes:lunt_ls60tha_dmk_11_04_2016_30s_stack.jpg?300|}}
  * Tuning: Internal “Pressure Tune” and front tilt
  * Aperture: 60mm (Scope), 50mm (Filter)
  * Focal Length: 500mm
  * F-ratio: 8.3
  * Bandpass: <0.5 Angstroms @ 656nm
  * Focuser: 10:1 fine adjustment
  * Diagonal: B600 or B1200 Blocking Filter
  * Vixen GP-DX equatorial mount, with motor drive on both axes, and micro-computer control

**An etalon Hα narrow band filter.**\\ 
A Fabry–Pérot interferometer or etalon is typically made of a transparent plate with two reflecting surfaces, or two parallel highly reflecting mirrors. The heart of the Fabry–Pérot interferometer is a pair of partially reflective glass optical flats spaced millimeters to centimeters apart, with the reflective surfaces facing each other.

**The „Pressure Tuner“ system.**\\ 
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Lunt uses a proprietary wavelength adjustment system which compensates for the variation in the air pressure of the atmosphere depending on height and weather. The sensitive etalon filter systems respond to these air pressure variations. The wavelength range that is allowed through the filters, shifts as a function of the air pressure. This shifting is indeed minimal, but at bandwidths of less than one Angstrom it is already clearly visible. If the filter is not adjusted precisely to the H-alpha wavelength, the image of the sun through the telescope degrades, prominences and surface details are no longer visible. This adjustment is typically done by a mechanical tilting of the filter. The new air-pressure system “Pressure Tuner” by Lunt Solar Systems adapts the air pressure in the filter system by 100 percent to the real external air pressure. Thereafter the air surrounding the Etalon can simply be compressed or decompressed by the tuning system in order to change the air pressure between the surfaces. This allows the Etalon surfaces to always remain at the same perfect angle to the light waves but changes the diffractive index of the air in the chamber and thus accomplishes the same tuning expect that it goes around + or - 0.4 Å on either side of the centerline. The “Pressure Tuner” system from Lunt Solar Systems shifts the passband. Hydrogen gas on the sun with differnt speeds is thus selected. This is called "doppler tuning".