INTERNATIONAL. Member Observatory. The Boquete Optical SETI Observatory. (11/5/15)

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1 INTERNATIONAL Member Observatory The Boquete Optical SETI Observatory. (11/5/15) Boquete, Panama is located about 25 miles south of the Panama/Costa Rica Border on the slopes of Vulcan Baru, the tallest mountain in Panama. Our home is at 4400 feet elevation with daytime temperatures in the mid to upper 70s and night time in the mid to upper 60s Fahrenheit. We have just two seasons, rainy and dry. The rainy season is for doing projects and the dry for observing. Construction of the observatory was begun in 2008 at the same time the house was being built. All of the structural elements were made on site. A modified English yoke telescope mounting was designed and built such that heavy instrument loads could be easily balanced out. A 14 Cassegrain and 5 refractor were then installed. Machine shops are almost non-existent in the area and everything had to be fabricated in the garage. If it couldn't be cut, filed, drilled or welded, it didn't happen. The original observatory and setup with the 5 refractor piggy-backed on the 14 Cassegrain telescope. This served well for over 4 years.

2 The observatory upgrade. In May of this 2015, a 20 f4.2 Newtonian primary mirror and secondary were ordered with Hubble Optics. Then, in June, modification of the building and construction of the 20 telescope assembly was begun. Again, a modified English yoke mounting was planned and the same construction constraints persisted. A new telescope room roof had to be built to provide more overhead room. In early September of 2015, the 20 telescope assembly was installed in the observatory building. The design constraints were so tight that only 1 inch of extra clearance was available both overhead and in the north-south directions. The right ascension bearings had to be mounted in the concrete walls to allow room for the RA yoke. Advantageously, the primary mirror was determined to be f4.1 (not f4.2) which allowed a bit more focusing range for the photometer and video camera. More next page

3 Above. Various stages in the construction of the weldments. A concrete mirror mockup was used for the initial rough balancing. Below left. Yet another photometer (~15 lbs.) had to be built to accommodate the highly convergent rays as a result of the short focal length. It also includes several wish-list improvements such as motorized focusing. Below right. Mirror cell provided by Bruce Howard (Owl Observatory) mounted in the weldment.

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5 The larger telescope assembly continues to use stepping motors and friction drives. For targeting, encoders (2000 pulse/rev.) mounted on the secondary drive wheels aid in tracking the positions. New micro stepper drives were also installed to provide better resolution. Bruce Howard also provided an excellent motor driven secondary focuser for the 14 Cassegrain telescope.

6 During the cool evenings and with all the equipment running the control room stays nice and cozy. Note the wireless pendant (with string) for positioning of the telescope, shutter and two focusing adjustments.

7 An auto-guiding system was made using a sensitive video camera (10-6 lux) mounted on the 14 Cassegrain (above left). A video monitor along with position detection scheme (above right) permits on/off axis guiding on stars down to 14 th magnitude while holding position within ~1-2 arc seconds. The telescope control I/O electronics are of 1990s vintage Opto-22 origin and a compiled Quick Basic program performs all of the telescope control functions. The software has evolved to cover an extensive wish-list.

8 Above. The telescope control computer display. Upper right graph, a high speed log amplifier takes the raw total count pulses and converts them to a DC level for input to an Opto I/O module. Level shifting in the software permits a wide dynamic range. The Group Hits and Coincidence Hits graphs show detection of a 0.6 Hz LED test pulse. The Quick Basic display looks pretty old fashioned, but hey... Above. Photo of the data crunching computer monitor. On the left and right respectively are the Stellarium star chart and the Spectrum Lab fast Fourier transform analyzer display. Note the LED test signal (peaks and white vertical lines) on the display. Bottom center is the StepVoice Recorder.

9 The new setup has only recently been put into service and with minor adjustments is improving daily. The structure has proven to be very stable and yet easily positioned either manually or electronically. It was planned and hoped that the 20 installation would be complete before the beginning of the dry season and good observing weather. It is gratifying that the work is done and the dry season, beginning around the first of December, is still about a month away. I look forward to using the greatly improved capabilities and broader search strategy.

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