Site testing for the Advanced Technology Solar Telescope

Hill, F.; Beckers, J. M.; Brandt, Peter; Briggs, John W.; Brown, Thomas M.; Brown, William J.; Collados, M.; Denker, C.; Fletcher, Stephen; Hegwer, S.; Horst, T. W.; Komsa, M.; Kuhn, J. R.; Lecinski, A.; Lin, Haosheng; Oncley, S.; Penn, Matthew; Radick, R. R.; Rimmelé, Thomas; Socas‐Navarro, H.; Streander, K. V.

doi:10.1117/12.673677

Cited by 24 publications

(15 citation statements)

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“…The ATST project has been carrying an extensive site survey to identify the location of its future 4 m solar telescope [1]. We discuss here some of their results from the La Palma site survey.…”

Section: Seeing At Izaña and La Palmamentioning

confidence: 99%

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Design and implementation of an image stabilization device at the THEMIS solar telescope

et al. 2008

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An image stabilizer has been inserted into the optical path of the THEMIS solar telescope. THEMIS is a Ritchey-Chretien reflector telescope using an altazimuthal mount and closely tied to its spectrograph. The optical and mechanical design, implementation and system tests are described, and emphasis is put on the complexity of situations that this stabilizer must accept, including the scanning of the solar surface while stabilizing. The current closed-loop crossover frequency of the device is 65 Hz at −3 dB on all typical solar scenes.

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Section: Seeing At Izaña and La Palmamentioning

confidence: 99%

“…Ref. [1] shows for one summer season the evolution of the median seeing with the time of the day. Seeing in La Palma is clearly better in the morning than at any other moment of the day.…”

Section: Seeing At Izaña and La Palmamentioning

confidence: 99%

Design and implementation of an image stabilization device at the THEMIS solar telescope

et al. 2008

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“…The Site Survey Working Group (SSWG) delivered its final report in August 2004. The report was evaluated by the Science Working Group (ASWG), which issued its site recommendation for Haleakalā to the project director in October 2004 6 . Taking into account cost and feasibility issues summarized by the project, the ATST director accepted the ASWG's recommendation for Haleakalā as the proposed ATST site.…”

Section: Site Selection and Preparation Processmentioning

confidence: 99%

Advanced Technology Solar Telescope project management

et al. 2010

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The Advanced Technology Solar Telescope (ATST) has recently received National Science Foundation (NSF) approval to begin the construction process. ATST 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. This paper gives an overview of the project, and describes the project management principles and practices that have been developed to optimize both the project's success as well as meeting requirements of the project's funding agency.

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“…An extensive site survey was conducted between 2000 and 2005 (Hill et al, 2004(Hill et al, , 2006. The ATST Site Survey Working Group oversaw the development and construction of instrumentation to measure daytime solar seeing (Beckers, 2002), sky brightness (Lin and Penn, 2004), clear time fraction, dust levels, and water-vapor content.…”

Section: Introductionmentioning

confidence: 99%

The Daniel K. Inouye Solar Telescope – Observatory Overview

et al. 2020

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We present an overview of the National Science Foundation’s Daniel K. Inouye Solar Telescope (DKIST), its instruments, and support facilities. The 4 m aperture DKIST provides the highest-resolution observations of the Sun ever achieved. The large aperture of DKIST combined with state-of-the-art instrumentation provide the sensitivity to measure the vector magnetic field in the chromosphere and in the faint corona, i.e. for the first time with DKIST we will be able to measure and study the most important free-energy source in the outer solar atmosphere – the coronal magnetic field. Over its operational lifetime DKIST will advance our knowledge of fundamental astronomical processes, including highly dynamic solar eruptions that are at the source of space-weather events that impact our technological society. Design and construction of DKIST took over two decades. DKIST implements a fast (f/2), off-axis Gregorian optical design. The maximum available field-of-view is 5 arcmin. A complex thermal-control system was implemented in order to remove at prime focus the majority of the 13 kW collected by the primary mirror and to keep optical surfaces and structures at ambient temperature, thus avoiding self-induced local seeing. A high-order adaptive-optics system with 1600 actuators corrects atmospheric seeing enabling diffraction limited imaging and spectroscopy. Five instruments, four of which are polarimeters, provide powerful diagnostic capability over a broad wavelength range covering the visible, near-infrared, and mid-infrared spectrum. New polarization-calibration strategies were developed to achieve the stringent polarization accuracy requirement of 5×10−4. Instruments can be combined and operated simultaneously in order to obtain a maximum of observational information. Observing time on DKIST is allocated through an open, merit-based proposal process. DKIST will be operated primarily in “service mode” and is expected to on average produce 3 PB of raw data per year. A newly developed data center located at the NSO Headquarters in Boulder will initially serve fully calibrated data to the international users community. Higher-level data products, such as physical parameters obtained from inversions of spectro-polarimetric data will be added as resources allow.

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Site testing for the Advanced Technology Solar Telescope

Cited by 24 publications

References 0 publications

Design and implementation of an image stabilization device at the THEMIS solar telescope

Design and implementation of an image stabilization device at the THEMIS solar telescope

Advanced Technology Solar Telescope project management

The Daniel K. Inouye Solar Telescope – Observatory Overview

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