Astronomy and Astrophysics – Astrophysics
Scientific paper
Dec 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009agufmsh53b..10r&link_type=abstract
American Geophysical Union, Fall Meeting 2009, abstract #SH53B-10
Astronomy and Astrophysics
Astrophysics
[7500] Solar Physics, Astrophysics, And Astronomy, [7524] Solar Physics, Astrophysics, And Astronomy / Magnetic Fields
Scientific paper
The 4m Advance Technology Solar Telescope (ATST) on Haleakala will be the most powerful solar telescope and the world’s leading resource for studying solar magnetism that controls the solar wind, flares, coronal mass ejections and variability in the Sun’s output. The project is about to enter the construction phase and is expected to be fully commissioned in 2017. A brief overview of the science goals and observational requirements of the ATST will be given followed by a summary of the design status of the telescope and its instrumentation will during which the technical and engineering challenges the ATST project faces will be discussed. ATST will provide high resolution and high sensitivity observations of the dynamic solar magnetic fields throughout the solar atmosphere, including the corona. With its 4 m aperture, ATST will resolve features at 0.”03 (20km on the sun) at visible wavelengths. The science requirement for polarimetric sensitivity (10-5 relative to intensity) and accuracy (5x10-4 relative to intensity) place strong constraints on the polarization analysis and calibration units. A high order adaptive optics system delivers a corrected beam to the initial set of state-of-the-art, facility class instrumentation located in the Coude lab facility. A few examples of the many unique science capabilities of the 4m ATST will be discussed. The initial set of first generation instruments includes: 1: the Visible Broadband Imager will provide images at the highest possible spatial and temporal resolution at a number of specified wavelengths in the range from 390 nm to 860 nm. 2: the Visible Spectro-Polarimeter will provide precision vector field measurements simultaneously at diverse wavelengths in the visible spectrum and thus deliver quantitative diagnostics of the magnetic field vector as a function of height in the solar atmosphere, along with the associated variation of the thermodynamic properties. 3: the Diffraction-Limited Near-Infrared Spectro-Polarimeter will record with high temporal cadence the full polarization state of spectral lines in the near infrared wavelength regime from 900 nm to 2300 nm. 4: the Cryogenic Near Infrared-Spectro-Polarimeter will measure solar magnetic fields over a large field-of-view at infrared wavelengths from 1000 nm to 5000 nm in the solar corona. 5: the Visible Tunable Filter will provide two-dimensional spectroscopy and polarimetry by recording diffraction-limited narrow-bandpass images with high temporal resolution.
Keil Stephen L.
Rimmele Th.
Wagner Jakub
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