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Transcript
Future Telescopes Areas of Telescope Advancement • Gather more light – Larger mirrors (or many smaller ones) • Sharper images – Larger mirrors or arrays of mirrors – Correct for blurring of atmosphere (adaptive optics) – Space satellites (e.g., Hubble) • Images of larger areas – Specially-designed telescope optics – Cameras with large detector arrays • More sophisticated instruments – High spectral resolution – Multi-object spectroscopy – Adaptive optics Day Night The largest single mirrors are currently 8 m in diameter. Rather than use larger mirrors, future telescopes will contain arrays of mirrors. Smaller mirrors are easier and cheaper to build, so larger telescopes often use segmented mirrors The largest optical/IR telescopes currently have mirror diameters of 10 m. The next generation of telescopes should reach 30-100 m QuickTime™ and a Motion JPEG A decompressor are needed to see this picture. Improvement in resolution from 1 to 100 m Large Synoptic Survey Telescope (LSST) LSST is a 8.4 telescope that will use a wide-field camera to image 2/3 of the sky 1000 times at optical wavelengths from 2016-2026. The primary goals are the discovery of all large near-Earth asteroids (>100 m) and measurements of dark energy. QuickTime™ and a Microsoft Video 1 decompressor are needed to see this picture. LSST camera Searching for Asteroids with LSST Imaging through a perfect telescope FWHM ~l/D in units of l/D Point Spread Function (PSF): intensity profile from point source With no turbulence, FWHM is diffraction limit of telescope, ~ l/D Example: l / D = 0.02” for l = 1 mm, D = 10 m With turbulence, image size gets much larger (typically 0.5 2”) How does adaptive optics work? Measure details of blurring from “guide star” near the object you want to observe Calculate (on a Light from both guide computer) the star and astronomical shape to apply to object is reflected from deformable mirror deformable mirror; to correct blurring distortions are removed QuickTime™ and a Cinepak decompressor are needed to see this picture. Comparison of normal seeing and AO QuickTime™ and a YUV420 codec decompressor are needed to see this picture. Neptune with AO on Keck (10 m) Keck AO 2.3 arc sec normal seeing Neptune with Hubble and Keck AO HST Keck AO Limitations of AO • most AO systems are restricted to IR; very difficult in optical • AO correction applies to only a very small patch of sky • need bright star near target for wavefront correction, although lasers can be used to create artificial stars Stratospheric Observatory for IR Astronomy (SOFIA) SOFIA is a 2.5 m IR telescope that will soon be deployed on a modified 747. QuickTime™ and a YUV420 codec decompressor are needed to see this picture. SOFIA will observe at wavelengths that are blocked by the atmosphere for telescopes on the ground Example of a SOFIA flight path Example of a SOFIA flight path James Webb Space Telescope (JWST) JWST is a 6.5 m IR telescope that will be launched in 2014. Because of its large mirror, it will over much better sensitivity and spatial resolution than any previous IR telescope. It will focus on the first stars and galaxies, as well as planets around other stars. Spitzer JWST Orbit of JWST QuickTime™ and a H.264 decompressor are needed to see this picture. QuickTime™ and a Sorenson Video decompressor are needed to see this picture. Atacama Large Millimeter/submillimeter Array (ALMA) ALMA will be an array of 54m and 12m millimeter-wave dishes on a high plain (5000 m) in Chile. It will provide 0.02” resolution at 1mm, which is comparable to JWST. Like JWST, ALMA will focus on the first galaxies and the formation of planets. The ALMA site QuickTime™ and a Sorenson Video decompressor are needed to see this picture. ALMA science disk gap created by 5 AU gas giant at 100 pc ALMA science Hubble Nearby galaxies QuickTime™ and a decompressor are needed to see this picture. Distant galaxies QuickTime™ and a decompressor are needed to see this picture. ALMA science ALMA Nearby galaxies QuickTime™ and a decompressor are needed to see this picture. Distant galaxies Square Kilometer Array (SKA) SKA will be an array of thousands of radio dishes with a total collecting area of 1 km2 and a baseline of 3000 km. It will be built in either Australia or Africa and should begin operations in 2020. SKA will offer both sharp images (<0.1”) and a huge field of view (1 deg), as well as 100x the sensitivity of VLA. SKA will study interstellar gas from soon after the Big Bang and the formation of planets. SKA design QuickTime™ and a YUV420 codec decompressor are needed to see this picture.