1. The Solar C Observatory

The Solar C Observatory is a 0.5m off-axis Gregorian system coronagraphic reflecting telescope which is located on Haleakala adjacent to the Mees Solar Observatory with a .45 meter diameter primary mirror. The telescope housed within the Observatory is designed to allow coronal observations which have not been realized, even from space, develop technology which we believe will be used for future satellite observations, support several long-term coronal observing platforms which extend intermittent coronal space observations, and provide a model environment for the future ATST project

2. Multicolor Active Galactic Nuclei Monitoring (MAGNUM) Telescope:

Multicolor Active Galactic Nuclei Monitoring started on 1995. The telescope was designed to monitor the distance of the active galaxies through the Multi colors variances that the galaxies emitted. This telescope was constructed on the North Dome of the University of Hawaii’s LURE facility, on top of the Haleakala. The operations started on September, 2000. The MAGNUM project will: explore the new method of distance detection, detect distances to AGNs and quasars (QSOs) at red shifts of 1-2, increase the sample size of monitored galaxies by 2 orders of magnitude enabling statistical determination of properties, use multi-color monitoring observations to learn about the internal structure and origin of AGNs and QSOs, measure the delay time from multiple images of the QSOs, so the Hubble constant can be measured, and discover distant galaxy clusters in deep images of the monitored fields produced by adding the individual monitor images.

3. The Maui Space Surveillance System (MSSS)

The Maui Space Surveillance System (MSSS) is a state-of-the-art electro-optical facility combining operational satellite, the only of its kind in the world. The MSSS houses the 3.67-meter Advanced Electro Optical System (AEOS) and the other telescopes with ranging sizes of 0.4 to 1.6 meters.

4. The Faulkes Telescope

The Faulkes Telescope Project is the education arm of Las Cumbres Observatory Global Telescope Network (LCOGTN). This telescope is housed within a dome shaped structures where a shutter is required to be opened to expose the lens to the open sky. This telescope is a quick response telescope where this is used for rapid response when needed. This telescope can move at two degrees per second. This telescope has two modes, the real time and the offline mode; the offline mode is where an observer will input the coordinates to select the target and then filters the selection. While in the offline mode, the coordinates will be uploaded to the system for targeting, then there will be a flexible schedule made.

I. Optical/Infrared Observatories:

1. You can Study here in the Hawaii University’s Institute for Astronomy: The University of Hawaii (UH)-Hilo 24 Telescope and The University of Hawaii (UH)-2.2 Telescope: http://www.uhh.hawaii.edu and http://www.ifa.hawaii.edu/gradprog/introduction.htm respectively

2. As for the NASA Infrared Telescope Facility (IRTF), you can schedule your visit here through this link: http://irtfweb.ifa.hawaii.edu/observing/schedule.php. You can also do a remote observation through this manual offered by the site: http://irtfweb.ifa.hawaii.edu/observing/remote_obs/

3. The Canada-France-Hawaii Telescope is available for observation with this information given to interested observers: http://www.cfht.hawaii.edu/observing.php

4. For the United Kingdom Infrared Telescope, an observing schedule is provided, alongside with the application to the observation within the observatory. Scheduling, booking and preparations are also made available within the site: http://www.jach.hawaii.edu/UKIRT/observe.html

5. At the Keck Observatory, an application can be achieved by visiting this site: http://www2.keck.hawaii.edu/observing/obswmkap.html

6. Subaru Telescope (Schedule): http://www.naoj.org/cgi-bin/opecenter/schedule.cgi

7. Gemini Northern Telescope (Schedule): http://www.gemini.edu/sciops/schedules/schedCurrClassIndex.html

II. Submillimeter Observatories:

1. Caltech Submillimeter Observatory (Schedule): http://www.submm.caltech.edu/cso/schedule/

2. For the James Clerk Maxwell observatory, an observing schedule is provided, alongside with the application to the observation within the observatory. Scheduling, booking and preparations are also made available within the site: http://www.jach.hawaii.edu/JCMT/observing/

3. The Submillimeter Array site will require some proposal procedures prior to observing in the Site: http://sma1.sma.hawaii.edu/proposing.html

III. Radio Observatories:

1. The Very Long Baseline Array provides support and encourages scientists to visit the National Radio Astronomy Observatory (NRAO) observatories: http://www.nrao.edu/astrores/visitors.shtml

The primary source of the detection of the Submillimeter Array is the cold interstellar material, which is consisted of gas, dust, and small rock like bodies. These are the substances that makes the stars and the planets. Throught the scanning of the detected radiations that were emmited by these materials, the study of the formation and the deaths of the interstellar bodies can be made through the use of the Submillimeter Array. One great feature of the SMA is that it can seethrough the dust clouds in space, thus witnessing the birth of a star where opical telescopes of the human eyes cannot see.

The SMA is the world’s first imagin interometric telescope at the submillimeter wavelengths, it is consisted of 8 movable antennas that can be moved along the sides of a Releaux triangle to provide optimal imaging quality. Each of the antennas is composed of a smooth parabolic reflector 6 meters (19 and 2/3 feet) in diameter. The signals from the antennas are amplified and combined electronically to give the resolution equivalent to an antenna of 0.5 km (0.3 miles) across.

The SMA is located on the summit of Mauna Kea, which is above the 40% of the earths atmosphere. The submillimeter radiation that the astronomical objects emit is partially absorbed by the Earth’s atmosphere, and at sea level, the little submillimeter that enters the Earth will be impossible to detect, by having the SMA on a high and dry site, the radiation can be detected and studied.

A silver coating was applied to the telescope to enhance the mirror’s unprecedented performance. Other incorporated technologies include the laser guide stars, Adaptive Optics and the multi-object spectroscopy will enable observers to access the latest tools in exploring the universe.

The Gemini was built in cooperation of 7 countries naming, the United States, United Kingdom, Canada, Chile, Australia, Brazil and Argentina. A network was built to provide remote assistance and access to the observatory with the flexibility of “Queue Scheduling” and remote participation, researcher can access anywhere within the Gemini Partnership will be assured the best possible match between observation, instrument and observing conditions.

The Telescopic glass is housed within an enclosure, which has a cylindrical enclosure with the height of 43 meters. The enclosure has a base diameter of 40 meters, with a total weight of 2000 tons.

The Keck Observatory was made possible through the grants of more than $140 from the W. M. Keck Foundation, at which the observatory was operated by the California Association for Research in Astronomy (CARA). Its Board of Directors includes representatives from the California Institute of Technology and the University of California.