Download PARI Newsletter Spring

VIEW
Volume 16
Number 2
Spring/Summer 2016
New website:
a transformation
Sneak Peak
In this issue . . .
Science in the Stars . . . . . . 2
3D Planets . . . . . . . . . . . . . . 2,3
Biogen Grant . . . . . . . . . . . . 3
Observing Opportunities
3
Summer Programs . . . . . .
4
Research Update . . . . . . . .
5
Coming soon to computer, tablet or smart phone near you! PARI’s
new website is currently being beta-tested and will soon be made
available to the public.
Keep an eye on www.pari.edu.
PARI in Pictures . . . . . . . . . 9
Space Day . . . . . . . . . . . . . . . 10
Volunteering . . . . . . . . . . . . 11
Brad McCall . . . . . . . . . . . . . 12
In Memoriam . . . . . . . . . . . . 12
Chamber Award . . . . . . . . . 13
Astronomer’s Corner 14-18
PARI Calendar
June 10 July 8
August 11
August 12
Sept. 9
Sept. 16
Evening at PARI
Evening at PARI
Perseid Meteor Shower Observing Session
Evening at PARI
Evening at PARI
Friends of PARI Annual Meeting
Pisgah Astronomical Research Institute, a public not-for-profit 501(c)(3) foundation
Science in the Stars at
the Western Regional
Science Fair
PARI continued its active support of
the Western Regional Science Fair at
Western Carolina University in Cullowhee. This year’s theme was Science in
the Stars, and PARI’s Bob Hayward and
Christi Whitworth were invited to make
the featured presentation to the 400+
attendees, a program on the electromagnetic spectrum.
PARI also sponsored a booth, sharing
information about Smiley and SCOPE
Star Classification. Each year, PARI also
supports an award in astronomy. The
photo here shows Bob and Christi presenting the Elementary Division award
to Dasgididi Denili Brody Hill from
New Kituah Academy for his project on
counting stars. Junior Division winners
were Whitley Sumpter, Amanda Gibson
and Madison Logan from Hayesville
Middle School for their rocketry project.
Dasgididi Denili Brody Hill receives the
Elementary Division award
A busy spring for PARI’s 3D Planets
PARI’s 3D Planets program continues its
series of week-long workshops for middle-school girls at local science museums
throughout North Carolina. So far this
year the program has been hosted at the
Museum of Life and Science in Durham,
Hands On! A Child’s Gallery in Hendersonville, Horizons Unlimited in Salisbury
and Port Discover in Elizabeth City.
Page 2
Sponsored by the Burroughs Wellcome
Fund and Red Hat, 3D Planets provides
girls ages 9-13 the opportunity to learn
about lunar and planetary altimeter data,
3D design and 3D printing. The girls then
use their knowledge to design and produce new tools for educators to use at the
3D Planets (continued)
local science museums for people with visual impairments. The
workshops this spring involved a
total of 60 girls and they produced
30 models of the Moon and Mars.
Photos shown here are from the
workshop at the Museum of Life
and Science in Durham.
PARI to host
Rosman Middle
School students
PARI has been awarded a $2,500
grant to facilitate a field trip to
PARI by students from Rosman
Middle School. The grant is from
the Biogen Foundation’s Ignite
the Power of STEM program, administered by the North Carolina
Community Foundation.
The grant will allow PARI to bring
about 140 middle school students
to the campus and engage in a
full day of learning opportunities
with our astronomers and educators. The objective is to host the
students in an active laboratory
environment so they will better
understand science careers, the
need for STEM skills and the importance of cultivating their own
future opportunities. Tentatively
targeted for August, the field trip
will allow students to learn from
the researchers about their education, background interests and
career paths.
PARI schedules public night-sky
observing opportunities throughout
the year.
The night-sky observing sessions included as part of our monthly
Evening at PARI programs have proven to be so popular that PARI has
scheduled additional opportunities throughout the year. To date in
2016, we’ve hosted three well-attended sessions and three more are
scheduled. The next event is planned for August 11, to coincide with
the Perseid meteor shower. Check the website, www.pari.edu, for details and other opportunities to gaze skyward with PARI astronomers.
Page 3
Student programs
highlight a busy
summer at PARI
Students are involved throughout the year
at PARI but the summer months are primetime for intensive on-campus experiences,
including:
• Duke TIP (Talent Identification Program) is returning to PARI for the 15th
consecutive year. This year will again
feature two sessions. In each session,
27 students from across the country will
spend a full two weeks on campus exploring astrophysics, stellar and galactic
astronomy, astrobiology and astronomical instrumentation. The program includes research studies using PARI radio
and optical telescopes as well as some
formal class sessions. Students engage
in original research under the direction
of PARI astronomers and Duke TIP staff,
then write and present a summary of
their work.
• Undergraduate Interns. PARI will also
host five undergraduate interns. The J.
Donald Cline Scholar will work on instrumentation for the 2017 solar eclipse.
The Jo Cline Intern will help redesign and
plan the PARI Exhibit Gallery. The 12m
radio telescope will receive upgrades
from the Chip Parks Intern and the Janet Parks Intern will embark on an Earth
Science project involving stream quality.
An IT Intern will work direction with CIO
Lamar Owens on upgrades for PARI’s IT
infrastructure. All interns will live on
the PARI campus and serve as mentors
during the Duke TIP sessions.
• Southwestern Community College is
planning to bring its middle school camp
to PARI in June and is also planning a visit for its undergraduate astronomy students.
Page 4
In addition to the student activities, PARI’s
regular programs continue throughout the
summer, including Evening at PARI, scheduled public observing opportunities, and
much more. Check the website Event Calendar for details.
Ten Years of Research with the
PARI West Optical Telescope
In early 2006 a clamshell dome
and a DFM Engineering 0.4m
(16-inch) optical telescope were
installed on the Optical Ridge at
PARI. The clamshell was carefully mounted on the observatory building (Figure 1), and the
pier for the telescope mount
was poured (Figure 2). After the
DFM staff installed the telescope
mount and telescope tube and optics (Figure 3), the telescope was
ready for viewing through the
eyepiece (Figure 4). The next step
was installation of a camera
RESEARCH UPDATE
M. Castelaz,
Lead Scientist
The clamshell is carried to the rooftop of the observatory building.
In Fall 2006 the telescope was equipped with astronomical filters and a new research grade Apogee CCD camera. And, on December 9, 2006 both the telescope and
camera were ready and first light images were taken.
Figure 5 shows an image of the Dumbbell Nebula – the
first light image. The characteristics of the telescope
and camera are given in Box 1.
Thad McCall inspects the mold for the pier
before pouring.
ology at PARI, undergraduates, and PARI summer interns. We estimate that about 210 TIP
students and scores of undergraduates and
astronomers from a dozen colleges and universities have done their research with this
telescope, acquiring more than 50,000 images
during the 10 years. Because hundreds of sky
scientists have used the telescope, we can’t
present every project done with the telescope.
Instead, we have selected a representative
sample of work that has been done with WOT.
Since 2006 the West Optical Telescope (WOT), as it is
known, continues to be used by astronomers, young
scholars in the Duke TIP (Talent Identification Program)
Summer Field Study in Astronomy, Physics, and Astrobi-
The telescope fork mount is set in place.
Page 5
PARI West Optical
Telescope (continued)
Projects conducted by high school
students in Duke TIP Program
cover a broad range of topics from
planetary science to quasars.
The projects are typically a team
effort consisting of three students. Box 2 on the next page lists
many of the titles of projects that
used the West Optical Telescope.
Those projects that involved nebulae relied heavily on images for
morphology studies, while those
that involved stars were photometric data measuring the brightnesses of individual stars.
The telescope peering out of the clamshell dome.
Figure 6.
Figure 5. First light image – M27 the
Dumbbell Nebula
Page 6
Figure 7. A light curve of an exoplanet transit of
Tres 1B
Duke TIP Student Research Projects
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
•
The Search for Extra-Solar Planets
Supernovae
HII Regions and Supernova Remnants: A Comparative Study: The HII Regions
Aspect
HII Regions and Supernova Remnants: A Comparative Study: The Supernova
Remnant Aspect
Elemental Distribution of Reflection and Emission Nebulae
Stellar Astronomy and Radio Emissions
Comparing masses and Ages of Binary Systems and Observing U Scorpii,
The Effects of Supernova Remnants verses The Effects of Planetary Nebulae
on Star Formation,
Neptune: The Mystic Planet
Supernovae
Pulsations of Phoenix Variable Star XX Cygnus
Searching for Tres-1B
Spectroscopic Binary Stars
Determining the Rotation of Saturn and Its Rings
A Study of Particle Sizes and Distributions in NGC 7023
Brightness of Potential Stars that will Become Supernovae
Supernovae: Past and Present
Planets around Binary Stars
Observing Beta Lyrae: A Binary Star System
Dust Reddening in Spiral galaxies
Bizzare Blazars
Determining the Temperature of Clouds Near Sagittarius A*
Analysis of the Eclipsing Binary U Corona Borealis
Do Star in the Same Cluster Have Similar Chemical Compositions (Focusing
on M39, NGC6756, and IC 4665)?”
Emission, Reflection, and Dark Nebulae
Observing the Transit of Exoplanet WASP-14b
Studies of the ‘Green’ Stars (Beta Libra)
Observed Correlation in Binary Star Systems
Figure 8. A 1 second exposure of the Moon
PARI West Optical
Telescope (continued)
As an example of an image taken
for morphological purposes,
Figure 6 shows a 10 second
exposure of the Orion Nebula
taken with a red filter. This
particular image came from the
study “Emission, Reflection, and
Dark Nebulae” where the students
were comparing the natures of
different types of gas and dust
clouds in the interstellar medium.
As an example of photometry,
Figure 7 shows a light curve of
an exoplanet transit – part of the
project “Searching for Tres-1B.”
The light curve shows the change
in stellar brightness (y-axis) as
a function of time (Julian Date
x-axis). The dip that occurs is
the result of a planet orbiting the
star Tres 1 and slightly obscuring
some light from that star.
Undergraduates
in
upper
level astronomy courses have
conducted observing sessions
with their astronomy professor
at PARI with the West Optical
telescope. These sessions also
include imaging and photometry.
So, for example, images of the
Moon were taken to study lunar
features. Figure 8 is one such
image. The field of view of WOT is
about 30 arcminutes, so an image
will contain nearly all of the full
Moon. Figure 9 is an image of the
spiral galaxy M33. Note the detail
in the structure of the spiral arms.
Students used images like these
to study different types of galaxies
like spiral, barred-spirals, and
ellipticals.
Page 7
PARI West Optical Telescope
(continued)
Astronomers usually use the West Optical
Telescope for photometry. Figure 10 shows light
curves taken in Visual, Red, and Infrared filters
of the eclipsing binary V523 Cassiopeia. This
binary consists of two solar type stars orbiting
each other in 5.5 hours! The light curves shown
in Figure 10 are the result of 7 nights of observing,
accumulating more than 1,200 images per filter.
The light curves were used to compare the period
of revolution with historical measurements. The
comparison shows that there must be a third
companion orbiting the pair about once every
100 years.
We continue to use the West Optical Telescope,
and look forward to new discoveries and
research projects. Figures 11 and 12 show the
telescope when configured with a low resolution
spectrometer – ready for the next observer.
Figure 12. The West Optical Telescope
Observatory
Page 8
Figure 9. The galaxy M33
Figure 10. The light curve of V523 Cas. The curves
show one star orbiting the other in about 5.5 hours.
PARI in Pictures
Friends of PARI Volunteer Alex Armstrong is a professional photographer who graciously
provides stunning photos for PARI literature and public outreach. Here are a few of his
recent works.
Page 9
Space Day Draws a Crowd
From the first public open house
in our history (in the year 2000),
the first Saturday in May has
been a highlight on the PARI
calendar, a special day when PARI
welcomes visitors drawn to our
annual Space Day festivities. This
year was no exception--- a full
day of fun-filled and educational
family activities.
Page 10
Volunteer at PARI
Since its inception, PARI has relied heavily on volunteers to accomplish many of the tasks associated with operating a large
science education and research
center.
Volunteers serve our mission in
two ways. First, by involving volunteers we extend our outreach
to the public beyond the realm of
researchers and educational institutions. Secondly, volunteers
help get the work done.
Currently, PARI is seeking volunteers to:
• Conduct tours—greet visitors
and guide tours of the PARI
campus.
• Facilitate special events- night
sky observing, education programs, Evening at PARI, and
many more.
• Assist with astronomy research- work with the archive
of rare, historic photographic
plates in PARI’s APDA.
High school students are invited
to participate in college prep experiences.
If you want to help, or simply learn more about what you can do, contact Sarah Chappell at
[email protected] or call 828-862-5554.
Page 11
Thad McCall
in Memoriam
Thad McCall’s life and the
history of the PARI campus are
so intertwined they are virtually
inseparable. As a teenager, Thad
helped clear the roadway to what
was to become NASA’s Rosman
Tracking Station in 1962. He
then embarked on a remarkable
53-year career at the site: first
with NASA, then the Department
of Defense, then the U.S. Forest
Service, and finally PARI.
Thad’s knowledge of the site was
so impressive that PARI Founder
Don Cline has often remarked
The McCall family is shown at last fall’s Friends of PARI annual meeting, when Brad that he would not have acquired
was presented the President’s Award. Thad was honored with the same award at the the site if Thad did not come with
Friends of PARI meeting in 2007 and again in 2013. Shown here, left to right, are: Thad,
it.
Mary, Don and Brad.
He knew every nut and bolt, what was behind every door and how everything worked.
Thad served as facilities director during his PARI years and there is quite likely not a piece of functioning
infrastructure that does not carry on it one of Thad’s fingerprints.
A native of Transylvania County, Thad served in Vietnam with the U.S. Army, then returned home to settle
in the Silversteen Community with Mary, his wife of 53 years. His son, Brad, carries on the family tradition
at PARI, currently serving as site security officer.
Thad loved NASCAR, bluegrass music, his community, his family--- and PARI.
He will be long remembered.
Brad McCall
PARI security officer receives certification
Brad McCall, PARI security officer, has completed
extensive training by the Security Guard Exchange
in Charlotte and has been certified by the NC Private
Protective Service Board.
Brad’s training included emergency response,
communication, patrol procedures, health and
safety hazards, deportment and defense tactics. At
PARI, his responsibilities include site security, site
safety procedures and surveillance, including the
installation, maintenance and monitoring of PARI’s
extensive network of security monitoring equipment.
Page 12
PARI wins “Nonprofit of the Year”
At its annual gala, the Brevard/Transylvania Chamber of Commerce announced a new award: Nonprofit of
the Year. PARI was honored as the first recipient.
In presenting the award, Brevard Mayor Jimmy Harris acknowledged PARI’s rich history and current efforts to involve the public in science, saying “this once top-secret location is now more accessible than
ever.”
CIO Lamar Owen, a lifelong Transylvania Country resident, represented PARI at the event and is shown here
receiving the award from Chamber President Kevin Howell.
(Photo courtesy of The Transylvania Times.)
Page 13
Radio and Optical Astronomy:
Two Windows on the Universe
astronomer’s corner
Dr. Bob Hayward,
Astronomer/Educator
How can we see stars at night? Well, you could answer that question by giving me an explanation of the
physiology of the eye, i.e., starlight enters through the pupil, is focused on the retina, etc. But, what I am
getting at is that, with all the air between us and the celestial heavens, how does that light we see with our
eyes even get to the surface of the earth?
There must be some sort of “window” through the atmosphere for visible light to reach the surface of the
earth from the heavens above. Obviously, for some reason or reasons, our atmosphere is transparent to
visible light in exactly the wavelengths to which our eyes are sensitive. That is no coincidence. Our eyes
evolved to take advantage of the type of energy that is available to us. It would do us no evolutionary good
to have evolved eyes that were sensitive only to radiations that did not efficiently illuminate the world we
live in. Thus, whether we are trying to fell a mastodon with a spear of are looking for the International
Space Station on a clear night, we make use of visible light.
Unfortunately, for astronomers this does
not always hold true. I had an office mate in
my University of Arizona graduate school
days whose PhD dissertation completion
was delayed a full year because many of
the nights on which he had obtained telescope time on the big telescopes at Kitt
Peak National Observatory were clouded
out and he was delayed in obtaining the
observational data he needed to complete
his PhD research.
The Nature of Visible Light: Light is an electromagnetic wave. Or, it’s a particle called a photon.
Or, it’s both a wave and a particle. Actually, light
consists of electromagnetic energy that behaves
sometimes like a wave and sometimes like a particle. Physicists and astronomers have to take
both of these characteristics into account to fully
understand how light works.
Page 14
To understand light as a wave of energy, we have
to consider it to be a wave that is passing by our
point of observation. The frequency is given as
how many of these waves pass by our point in a
given interval of time. Normally, we give that frequency in the number of waves per second.
Now, the number of waves that pass by our point will depend on how fast the wave is moving. In the case
of light, this is an easy answer – light travels at the speed of light. That seems very logical but it has profound implications. Albert Einstein showed that the speed of light in a vacuum is constant; it is (rounded
off) 300,000 km/sec or 186,000 mi/sec. From basic physics we realize that the relationship among the
frequency, wavelength and the speed of an electromagnetic wave such as light is given by
Light is an electromagnetic wave with a wavelength between 400 and 700 nanometers. A nanometer is a
very small distance, at least by everyday standards; it is one billionth of a meter. So, light has a wavelength
of 400 to 700 billionths of a meter. Thus, when we are talking about visible light, a wavelength range of 400
to 700 nanometers gives us frequencies of about 1014 i.e., 100,000,000,000,000 waves per second passing
by a given point. In other words, the frequency of the wave is 1014 waves per second. Internationally, one
wave per second is known as a Hertz, abbreviated Hz. So the frequency of visible light is somewhere on
the order of 1014 Hz. This term is most used to measure frequencies in millions of Hertz, i.e., megahertz
or MHz.
We now know that visible light is not the only type of energy inherent in what we now call the electromagnetic spectrum. The full spectrum ranges from very small wavelength radiation such as  (gamma) rays
and x-rays all the way to very long radio waves. Visible light is actually a very small part of the total electromagnetic spectrum.
The nature of Radio Waves: Up until the 1920’s that was all there was to astronomy. Astronomers had
to depend on how much light they could gather in from the skies above. They built telescopes with lenses
or mirrors as large as technology and budgets permitted. And they designed auxiliary equipment such as
cameras, spectographs, photometers, etc., to place on these telescopes and squeeze out as much information as they could from the tiny bits of light that came from these faraway object they were so interested in.
Many of these photographs and spectra recoded on glass plates are being preserved and digitized in PARI’s
Page 15
Two Windows on the Universe (Continued)
Astronomical Photographic Plate Archive (APDA).
Then, along came, as they often do, a rather serendipitous discovery. In 1928 Bell Labs in Holmdel,
NJ was investigating the possibility of using radio
waves in the 10-20 meter wavelength range to carry
transatlantic telephone traffic. But, they kept getting interference on their receivers in that range.
They gave the job of determining the source of this
interference to Karl Jansky a physics graduate of the
University of Wisconsin. Jansky built a receiving
antenna array designed to receive radio signals at
about 14.5 meters wavelength, frequency 20.5 MHz.
As Jansky studied the radio waves he was receiving on his antenna array, he realized he was receiving radio
“noise” from thunderstorms. But, there was still a mysterious signal that was coming from an unknown
source. One thing he did notice was that this signal was being received about four minutes earlier each
night. In other words it had a periodicity of 23 hours 56 minutes. Bingo! Any astronomer knows that this
is the sidereal rotation period of good ol’ planet earth.
What is the sidereal period? We all know that the earth rotates on its axis in 24 hours. But, that is only if
you measure it with respect to the sun as we do when we plan our daily lives. But, due to the earth’s revolution around the sun, the sun appears to move roughly one degree eastward per day in front of the zodiac
constellations. This is due to the earth’s motion of 360 degrees of orbit around the sun which it completes
in roughly 365¼ days, i.e., 360°/365.25 days  1°/day. Thus, the source of Jansky’s mysterious interference must have been coming from something on the celestial sphere of the sky! Jansky had inadvertently
built the first radio telescope; he had invented radio astronomy! Further measurements and investigation
determined that what he was picking up was a radio signal from a source in the constellation of Sagittarius;
he had discovered that the center of our Milky Way galaxy is a source of radio waves.
Page 16
Two Windows on the Universe (Continued)
Radio Astronomy Today: So, let’s rephrase my opening question but in the light (pun intended) of the
radio spectrum. How can a radio telescope see the center of the Milky Way, now known as radio source
Sagittarius A, at night…or during the day for that matter? It’s because not only is there a window in the
sky that lets visible light reach the surface of the earth so we can enjoy watching the gods play among the
constellations at night, but there is also a window through the earth’s ionosphere, that layer of charged
particles or ions, that lets radio waves reach the surface of the earth. This window stretches from about
0.3 millimeters (A millimeter is 1/1000 of a meter.) at the edge of the far infrared to about 30 meters above
which the earth’s ionosphere is opaque to radio waves.
Over the years astronomers have realized that not only is the sky full of optical sources like the stars, it is
also full of radio sources. Some of these are stars but, in general, stars are not strong radio sources. We
can “see” the sun with a radio telescope, during the day, of course, because it is so close to us. Radio waves
typically result from charged particles of matter moving very quickly in a magnetic field. You cell phone
transmits a signal when electrons from the battery are caused to move in a calculated manner, thus giving
off radio signals that can be received by another device and turned into sound waves in a speaker or an
image on a screen. Radio sources in the sky are typically nebulae of hot gases, galaxies with active cores, or
even planets such as Jupiter whose strong magnetic field is disturbed by the motion of its satellite Io.
While some radio telescopes today do consist of antenna wires
strung between poles similar to the one Jansky used, most consist
of dish shaped antennae like the ones at PARI. (Basically, if you
have DIRECTV or DISH Network satellite television, you have a radio telescope, a small dish that receives radio waves from an object
in the sky, a satellite.) Just as your eye receives light waves and
gathers them in to a focus on a receiver, called a retina, at the back
of your eyeball, radio telescope dishes focus radio waves on a receiver that is generally held in place at the focus of the telescope.
Courtesy of the National
Astronomy and Ionosphere Center,
Arecibo Observatory, a facility of
the National Science Foundation
Since radio signals from astronomical sources are very weak, the
larger the telescope one uses, the more success there will be to detecting and analyzing a signal. PARI’s two main radio telescopes are
both 26 meters (85 feet) in diameter. PARI’s signature telescope
“Smiley” is a 4.6 meter (15 feet) dish. It is used primarily for an instructional program that allows students to access to control it over
the internet. Typically, they view the sun or Sagittarius A during the
daytime since radio waves are not washed out by full sunlight. (Otherwise, you couldn’t use your cellphone or listen to a radio during
the day.) The largest radio telescope in the world is the 1000-foot
Arecibo telescope in Puerto Rico. This magnificent instrument is
built into a circular depression in the land. It cannot be steered
physically. However, it can observe objects in a limited area of the
sky by moving the receiver suspended of the dish. Thus, in this case
the receiver is not held at a single focus above the dish. Currently some radio telescopes event consist of multiple antennae spaced
across a large area of land such as the Very Large Array in New Mexico. How does a radio telescope “see”? In visible light our eyes focus
Page 17
Two Windows on the Universe (Continued)
a complete image onto the retina of our eyes to create an image that is interpreted by our brains. Our eyes
detect light throughout that 400 to 700 nanometer range of the electromagnetic spectrum. A radio telescope receives a single signal from a single point in the sky and at a single wavelength in the 0.3 millimeter
to 30 meter radio range of the spectrum. If more than one receiver at differing wavelengths is installed, a
radio telescope could receive multiple signals at the same time.
To produce an image, the telescope has
to be moved back and forth over the
source to detect signals from a multitude of point across the object of interest. Many times these signals are
displayed in visible light in what are
termed “false color images. (We cannot
view radio waves directly. If they could,
our eyes would have to be as big as at
least a small radio telescope.)
False color 13 mm radio image of Jupiter.
The “wings” on the side are the orbit of Io.
Summary: So we find that there are two “windows” to the sky. One stretches from 300 to 700 nanometers
and allows visible light to reach the surface of the earth. The other stretches from 0.3 millimeters to 30 meters and lets radio emissions from celestial objects reach our earthbound radio telescopes. What about the
other wavelengths listed in the graphic earlier in this article? We are now aware that celestial objects emit
radiations virtually across the entire electromagnetic spectrum. The problem for earthbound observers is
that at those wavelengths, the windows are shut tight; those radiations do not get through our atmosphere
and ionosphere. To study objects in those wavelengths we have to rely on satellites that can be placed high
above where there are not even any “windows” to be closed.
References:
“Arecibo Observatory,” Wikipedia. https://en.wikipedia.org/wiki/Arecibo_Observatory
Astronoblog, Haverford Astronomy department blog. Haverford College, 370 Lancaster Avenue. Haverford, PA 19041, http://blogs.haverford.edu/astronoblog/
“How To Hear Radio Signals from Jupiter,” Space Today Online. http://www.spacetoday.org/SolSys/Jupiter/JupiterRadio.html
“Karl Jansky and the Discovery of Cosmic Radio Waves,” National Radio Astronomy Observatory,
http://www.nrao.edu/whatisra/hist_jansky.shtml
“Electromagnetic Spectrum,” TutorVista.com. http://physics.tutorvista.com/waves/electromagnetic-spectrum.html
Page 18
Please support the PARI mission!
PARI is a public not-for-profit organization. Financially, we are dependent upon contributions and grants for our educational and research
programs, and for the many operating expenses associated with maintaining the campus and our facilities.
If you have recently contributed, we thank you for your support. If not, please support PARI and our mission with a contribution. PARI is a
public not-for-profit 501 (c)(3) and all donations are tax deductible to the full amount allowed by law.
To make a contribution now, please click below. If you prefer to mail a contribution, please send it to: PARI, Attn: Director of Finance, One
PARI Drive, Rosman, NC 28772.
Your generosity in supporting PARI and our mission is appreciated and valued. Your gift will allow PARI to advance STEM learning, empower
people of all ages to become more scientifically literate and encourage young learners to consider STEM careers.
Thank you for helping make all of this possible.
Pisgah Astronomical Research Institute
One PARI Drive, Rosman, NC 28772
Phone: (828) 862-5554 Fax: (828) 862-5877 Web: www.pari.edu
Don Cline
Stephen Saucier
Michael Castelaz, PhD
Christi Whitworth
Bob Hayward, PhD
Lamar Owen
Mark Krochmal
Ben Goldsmith
Thurburn Barker
John Avant
Ann Daves
Alex Armstrong
Sarah Chappell
Tim DeLisle
Donnie Curto
Brad McCall
John Sinclair
Chris Daves
Ken Steiner
President
Executive Director
Lead Scientist
Director of Learning Experiences
Astronomer/Educator
Chief Information Officer
IT Support Manager
Research Director
Director of APDA
Communications Director
Director of Finance, HR & Development
Special Projects
Visitor Support/Volunteers
Software Engineering Manager
Facilities Coordinator
Facilities/Security
Curator of Meteorites and Minerals
Facilities
Special Projects Consultant
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
[email protected]
The Pisgah Astronomical Research Institute (PARI) is a public not-for-profit 501 (c)(3) foundation established in 1998. Located in the
Pisgah Forest 30 miles southwest of Asheville, NC, the PARI campus is a dark sky location for astronomy and was selected in 1962 by NASA
as the site for one of the first U.S. satellite tracking facilities. Today, the 200 acre campus houses radio and optical telescopes, earth science
instruments, 30 buildings, a fulltime staff and all the infrastructure necessary to support STEM (science, technology, engineering and math)
education and research. PARI offers educational programs at all levels, from K-12 through post-graduate research. PARI is home to the Astronomical Photographic Data Archive and a member of the NC Grassroots Science Museums Collaborative.
PARI’s Exhibit Gallery displays a collection of rare meteorites as well as NASA Space Shuttle artifacts, many of which have flown in space.
For more information about PARI and its programs, visit www.pari.edu. Follow PARI on Twitter at http://twitter.com/Astronomy_PARI.
“Like” PARI on Facebook at www.facebook.com/Pisgah.Astronomical.Research.Institute.
Page 19