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| The CoMP instrument has begun to provide quantitative measurements of the coronal magnetic field using a specially designed camera and Lyot filter to measure the polarization of infrared light from the corona.
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| A Fabry-Perot interferometer is deployed at the Polar Cap Observatory (PCO) near Resolute, Canada (75 N), the site of the National Science Foundation Advanced Modular Incoherent Scatter Radar (AMISR).It measures mesospheric and lower thermospheric tidal waves and the upper thermosphere polar cap convection pattern using hydroxyl and atomic oxygen emissions.
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| A network of two instruments which observe solar
oscillations as seen in the radial velocity of the solar surface.
Analysis of these oscillations yields information on the internal
structure and rotational characteristics of the Sun.
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| The Precision Solar Photometric Telescope Project (PSPT) is
funded by the National Science Foundation Atmospheric Science
(ATM) and Astronomy (AST) divisions to provide high-resolution
and high photometric precision full-disk solar data for the solar
research community.
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| Uses precise time-series photometry to search for extrasolar
giant planets transiting their parent stars. An important
byproduct of this search will be an unusually complete survey of
variable stars within its selected fields-of-view. STARE is a
member of TrES, a network of three small-aperture telescopes
searching the sky for transiting planets.
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| The Mark-IV K-Coronameter (Mk4) is a 23 cm objective
coronameter-polarimeter located on Mauna Loa, in Hawaii. It is
used to observe the solar corona in polarized optical light.
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| CHIP is a differential device using properties of the
Helium-I line at 1083 nm as an indicator of both chromospheric
and coronal structures. CHIP records images of the sun at 1083
nm, as well as at a number of other nearby wavelengths (for
calibration purposes). It is basically composed of a liquid
crystal variable retarder Lyot filter connected to an IR CCD.
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| A telescope with a removable occulting disk used to make
observations of the limb or disk in Hydrogen-alpha (wavelength
656.3nm) light.
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| The ASP is perhaps the one single instrument that spurred development of the array of new solar spectro-polarimetric instrumentation. Observations from this instrument provided the first highly quantitative measurements of the full field vector with spatial resolution adequate to isolate, if not fully resolve, some solar structures.
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| There is a large potential scientific pay-off for observations combining simultaneous visible and IR spectro-polarimetry. These issues, along with increasing demand for flexible spectro-polarimetry and the need to ultimately replace ASP, have led this year to the development of the new SPINOR facility instrument.
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| The DLSP is intended to expand the capabilities of ASP in another direction -- toward very high angular resolution. Much of the demand for ASP observing time is for observations of photospheric vector magnetic fields. The DLSP is optimized to provide the highest angular resolution spectro-polarimetry for the photospheric Zeeman-sensitive neutral iron absorption lines at 630 nm.
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| POLIS is a ground-based prototype of the spectro-polarimeter to be flown on the Sunrise high altitude balloon platform. Stationed at Tenerife, Canary Islands, Spain, it is a collaborative program between the Kiepenheuer-Institut für Sonnenphysik (KIS), Freiburg, Germany and HAO.
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| The ATST is a project for a large-aperture solar telescope. With its 4 meter diameter primary mirror, the ATST will have a collecting area 16 times larger than the largest existing solar telescope and will be able to operate at the diffraction limit thanks to an advanced adaptive optics system. This project has been ranked by the Decadal Survey of Astronomy and Astrophysics as the most important ground-based initiative for the next decade.
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