Gateway to the Universe

Hartung–Boothroyd Observatory is a leading educational facility, aiding in the study of astrophysics, tracking asteroids, and fostering diverse academic collaborations.

Perched on Mount Pleasant in the town of Dryden, New York, the Hartung-Boothroyd Observatory (HBO) stands as a testament to the celestial curiosity that Cornell University has nurtured for decades. It is a gateway to the stars, a place where the heavens unfold in wondrous detail to the eyes of astrophiles and the lenses of powerful telescopes.

The observatory is home to a reflecting telescope, one of the largest in New York State dedicated to both education and research. This remarkable instrument, housed under a retractable dome, has provided students and researchers with direct experience in astronomical observations since its establishment in 1974.

HBO isn’t just an observatory; it is a bridge between the terrestrial and the cosmic. It represents an educational philosophy that values direct engagement with the subject of study. Undergraduates, graduates, and faculty members flock to the facility to engage in projects that range from studying variable stars and exoplanets to tracking asteroids. Here, theoretical astrophysics meets the tactile world, allowing for an integrated understanding of the universe’s complexities.

It is used mainly as a Cornell University (Ithaca, New York) teaching facility for upper-level astronomy classes. The observatory is named financial contributions of M. John Hartung ’08 (chemical industrialist and donor) and in honor of the labor of Samuel L. Boothroyd (founding professor and chairman of astronomy 1921–1942). The telescope construction began in the 1930s and the observatory was dedicated in 1974. It contains the James R. Houck 60 centimeter telescope and various instruments.

The James R. Houck telescope at HBO was a project initiated by its namesake in 1972, using optics and a lightweight tube which had been fabricated in the late 1930s by Samuel T. Boothroyd, Cornell’s first astronomer, and a mounting constructed by George Gull ’72 as his senior design thesis in Mechanical Engineering.

The telescope, control electronics and instruments are largely the result of work done by undergraduates since 1970. It was manufactured by the students at the Tompkins, Tioga and Seneca BOCES and by Therm, Inc., with mirror coatings by Evaporated Metal Films corporation, all in Ithaca. The latter corporation was founded by members of Boothroyd’s scientific team, as he pioneered the use of evaporated metal coatings in astronomical optics. The telescope and observatory were dedicated in 1974.

The primary mirror is made of Pyrex from the Corning Glass Works and is in fact from a 1/8-scale test pour by the Corning company in preparation for the making of the 200″ Palomar mirror. It is 0.635 m (25 inches) in size, but the outer half inch is masked. The focal length of the mirror is 2.5m (100″) or f/4.

The Cassegrain design of the James R. Houck telescope is a combination of a primary concave mirror and a secondary convex mirror, often used in optical telescopes, the main characteristic being that the optical path folds back onto itself, relative to the optical system’s primary mirror entrance aperture. This design puts the focal point at a convenient location behind the primary mirror and the convex secondary adds a telephoto effect creating a much longer focal length in a mechanically short system.

View south

The secondary is an 8″ mirror made of Cervit (a low thermal coefficient material). In combination with the primary, it yields a final f/13.5 beam to the nominal focus, which lies 18.5″ behind the primary mirror’s vertex. At nominal focus, the plate scale is about 24 arcsec/mm, with an effective focal length of 8.57 m.

View southwest toward Ithaca College

The telescope, control electronics and instruments are largely the result of work done by undergraduates since 1970. It was manufactured by the students at the Tompkins, Tioga and Seneca BOCES and by Therm, Inc., with mirror coatings by Evaporated Metal Films corporation, all in Ithaca. The latter corporation was founded by members of Boothroyd’s scientific team, as he pioneered the use of evaporated metal coatings in astronomical optics.

The dome itself, like all professional observatories, is unheated. The telescope and instrumentation can be controlled from a neighboring control room which is heated and offers standard amenities plus several computers for simultaneous data reduction.

The observatory was founded by James Houck and managed by him through 2006. The principal contact is Don Barry, who managed the facility from 2006-2015, and taught Experimental Astronomy using the facility.

“Graduates” of the HBO project are now senior engineers and technical managers as well as graduate students, research associates and faculty at major universities.

Moreover, the observatory is a beacon for interdisciplinary collaboration. It’s not uncommon to find astronomers working alongside computer scientists, engineers, and educators. This cross-pollination of ideas enhances the potential for innovation, fostering new techniques in data analysis, instrument design, and educational methods. The observatory’s role extends beyond its primary function; it is a hub of convergence for diverse academic disciplines, all under the umbrella of exploring the unknown.

HBO also contributes to the global astronomical community through its research. The data collected here feed into larger networks of observation and analysis, aiding in the collective endeavor of mapping and understanding the universe. Its strategic location in upstate New York, away from the light pollution of large urban centers, grants it relatively clear night skies, making it an invaluable resource for both optical astronomy and astrophotography.

In an era where space exploration has captured the public imagination like never before, observatories such as the Hartung-Boothroyd are more crucial than ever. They serve as terrestrial launchpads, propelling minds into the realm of scientific inquiry. Here, the vastness of space becomes approachable, the mechanics of the cosmos decipherable, and the mysteries of the universe a little less mysterious.

As the night falls and the stars emerge, the Hartung-Boothroyd Observatory continues its silent vigil over the heavens. It stands as a beacon of knowledge and discovery, an educational catalyst, and a gateway to the stars. For the students and astronomers who work from this dome on Mount Pleasant, HBO is more than an observatory—it is a vessel navigating the infinite ocean of the night sky, a journey that begins in the heart of Cornell University and extends to the edges of the observable universe.

Copyright 2023 Michael Stephen Wills All Rights Reserved http://www.MichaelStephenWills.com

McMath-Pierce Solar Telescope – 3

Adaptive optics

These views within the McMath–Pierce solar telescope enclosure were captured during a guided tour of the instrument, April 20, 2005. By way of orientation, the observation room we visited is near the location labeled “4” on the model of the following photograph or the “Observation Room” of the drawing.

We learned each of the sets of mirrors is considered a separate telescope. The first step in designing the new solar telescope was to determine the optimal image scale. Working on the spectra of the solar granules, on the physical structure of the sunspots and their associated magnetic fields, requires a considerable image size. Past experience has shown that the optimal image of the sun should be approximately 0.91 meters. The highlight of our visit to the Main Observation room was meeting with the technician operating the recently developed low-cost adaptive optics system.

Tip-tilt correction and low order wavefront correction is available with a number of portable optical benches.  These are primarily used with the Main spectrograph and the Solar Stellar spectrograph on the Main telescope, but due to their compact mounting they could be used with other telescopes and instruments in the facility.

This configuration uses a rapidly deformable mirror to correct distortions introduced by the turbulent atmosphere. Using sensors to measure the degree of image distortion, the adaptive optics system adjusts the shape of the mirror accordingly and converts a blurred image into a clear one. The following image demonstrates the correction. “Low-cost” = $25,000 in 2003 US dollars. Under references is a link to a full description of the device by the creator.

A main area of ​​study in the observatory is the structure of sunspots, which are relatively cold, dark spots on the surface of the Sun created by intense magnetic activity.

Some of the most important discoveries made at McMath-Pierce include the detection of water vapor in the Sun, the measurement of kilogauss magnetic fields (thousands of times stronger than those on Earth) outside sunspots and the detection of a natural maser (like a laser, but with a microwave instead of visible light) in the Martian atmosphere.

Over the years and technological advances, the National Solar Observatory has moved its headquarters from Tucson to Boulder, Colorado. The organization abandoned its solar telescopes at Kitt Peak and in New Mexico for a larger instrument in Hawaii, the Daniel K. Inouye Solar Telescope on the island of Maui, which began operating in 1919.

References:
Wikipedia “McMath–Pierce solar telescope”

“Low Cost Adaptive Solar Optics” by Christopoher Kellar

Insights into the architectural design.

National Solar Observatory website..

Copyright 2022 Michael Stephen Wills All Rights Reserved

McMath-Pierce Solar Telescope – 2

The Mirrors

These views within the McMath–Pierce solar telescope enclosure were captured during a guided tour of the instrument, April 20, 2005. By way of orientation, think of yourself at the location labeled “4” on this model. This is the only large telescope where humans can view the interior and visually experience the light paths “bouncing” between the mirrors.

McMath–Pierce solar telescope has three heliostats mounted on a 110-foot tower adjacent to a slanted enclosure. The 2.03-meter heliostat feeds a 1.61-meter primary mirror, there are 1.07-meter and 0.91-meter primary mirrors fed by a pair of 0.81-meter heliostats. Here we are inside the slanted enclosure, looking up the shaft to the tower mounted heliostats, readily identified as the three circles, the largest at center (3.51 feet in diameter). The smaller (2.66 feet) heliostats named “East” (on left) and “West.”

Built in 1962, the building was designed by American architect Myron Goldsmith and Bangladeshi-American structural engineer Fazlur Rahman Khan. It was the largest solar telescope and the largest unobstructed aperture telescope in the world. It is named after the astronomers Robert Raynolds McMath and Keith Pierce. Painted white to reflect sunlight to reduce heat accumulation, the enclosure is water cooled to prevent convection currents through the column of air within the slanted enclosure, keeping the air as still as possible along the light path between the mirrors.

In the three photographs following, we face the underground portion of the slanted shaft and (what looks to be) the 0.91 meter (2.99 feet) primary concave mirror. I say that because in some of the photographs a beam of light, to the left of the mirror, can be seen travelling further underground, presumably to the largest primary mirror. As there is only one such light beam, I conclude the west heliostat is inactive.

Here we looking up the slanted enclosure. Look carefully at the first photograph, below, to see reflections on the glass partition. The observation platform was separated from the light paths to maintain the stillness of the air column. The two mirrors of the first photograph are the third mirror, reflecting concentrated sunlight from the 0.91 and 1.61-meter primary mirrors into the observatory rooms. The mirror for the 1.07-meter primary is out of sight in foreground, I believe this set of three mirrors (West heliostats, primary and third) was out of service.

The second photograph, on right, is a close up of the third mirror for the largest primary. A foreshortened, perfectly round light disk is clearly visible.

Here we are inside the slanted enclosure, facing the underground portion of the slanted shaft and (what looks to be) the 0.91-meter primary concave mirror. In the lower right corner is the reverse side of the third mirror for the largest primary mirror, the 1.61-meter.

Reference: Wikipedia “McMath–Pierce solar telescope”
Copyright 2022 Michael Stephen Wills All Rights Reserved