The Daniel K. Inouye Solar Telescope – Observatory Overview
Abstract 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...
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Englisch |
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2020 |
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Enthalten in: Solar physics - Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967, 295(2020), 12 vom: Dez. |
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| Übergeordnetes Werk: |
volume:295 ; year:2020 ; number:12 ; month:12 |
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| DOI / URN: |
10.1007/s11207-020-01736-7 |
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| Katalog-ID: |
SPR042272602 |
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| 100 | 1 | |a Rimmele, Thomas R. |e verfasserin |4 aut | |
| 245 | 1 | 4 | |a The Daniel K. Inouye Solar Telescope – Observatory Overview |
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| 520 | |a Abstract 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. | ||
| 650 | 4 | |a Telescopes |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Instrumentation |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Sun |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Magnetic fields |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Photosphere |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Chromosphere |7 (dpeaa)DE-He213 | |
| 650 | 4 | |a Corona |7 (dpeaa)DE-He213 | |
| 700 | 1 | |a Warner, Mark |e verfasserin |4 aut | |
| 700 | 1 | |a Keil, Stephen L. |e verfasserin |4 aut | |
| 700 | 1 | |a Goode, Philip R. |e verfasserin |4 aut | |
| 700 | 1 | |a Knölker, Michael |e verfasserin |4 aut | |
| 700 | 1 | |a Kuhn, Jeffrey R. |e verfasserin |4 aut | |
| 700 | 1 | |a Rosner, Robert R. |e verfasserin |4 aut | |
| 700 | 1 | |a McMullin, Joseph P. |e verfasserin |4 aut | |
| 700 | 1 | |a Casini, Roberto |e verfasserin |4 aut | |
| 700 | 1 | |a Lin, Haosheng |e verfasserin |4 aut | |
| 700 | 1 | |a Wöger, Friedrich |e verfasserin |4 aut | |
| 700 | 1 | |a von der Lühe, Oskar |e verfasserin |4 aut | |
| 700 | 1 | |a Tritschler, Alexandra |e verfasserin |4 aut | |
| 700 | 1 | |a Davey, Alisdair |e verfasserin |4 aut | |
| 700 | 1 | |a de Wijn, Alfred |e verfasserin |4 aut | |
| 700 | 1 | |a Elmore, David F. |e verfasserin |4 aut | |
| 700 | 1 | |a Fehlmann, André |e verfasserin |4 aut | |
| 700 | 1 | |a Harrington, David M. |e verfasserin |4 aut | |
| 700 | 1 | |a Jaeggli, Sarah A. |e verfasserin |4 aut | |
| 700 | 1 | |a Rast, Mark P. |e verfasserin |4 aut | |
| 700 | 1 | |a Schad, Thomas A. |e verfasserin |4 aut | |
| 700 | 1 | |a Schmidt, Wolfgang |e verfasserin |4 aut | |
| 700 | 1 | |a Mathioudakis, Mihalis |e verfasserin |4 aut | |
| 700 | 1 | |a Mickey, Donald L. |e verfasserin |4 aut | |
| 700 | 1 | |a Anan, Tetsu |e verfasserin |4 aut | |
| 700 | 1 | |a Beck, Christian |e verfasserin |4 aut | |
| 700 | 1 | |a Marshall, Heather K. |e verfasserin |4 aut | |
| 700 | 1 | |a Jeffers, Paul F. |e verfasserin |4 aut | |
| 700 | 1 | |a Oschmann, Jacobus M. |e verfasserin |4 aut | |
| 700 | 1 | |a Beard, Andrew |e verfasserin |4 aut | |
| 700 | 1 | |a Berst, David C. |e verfasserin |4 aut | |
| 700 | 1 | |a Cowan, Bruce A. |e verfasserin |4 aut | |
| 700 | 1 | |a Craig, Simon C. |e verfasserin |4 aut | |
| 700 | 1 | |a Cross, Eric |e verfasserin |4 aut | |
| 700 | 1 | |a Cummings, Bryan K. |e verfasserin |4 aut | |
| 700 | 1 | |a Donnelly, Colleen |e verfasserin |4 aut | |
| 700 | 1 | |a de Vanssay, Jean-Benoit |e verfasserin |4 aut | |
| 700 | 1 | |a Eigenbrot, Arthur D. |e verfasserin |4 aut | |
| 700 | 1 | |a Ferayorni, Andrew |e verfasserin |4 aut | |
| 700 | 1 | |a Foster, Christopher |e verfasserin |4 aut | |
| 700 | 1 | |a Galapon, Chriselle Ann |e verfasserin |4 aut | |
| 700 | 1 | |a Gedrites, Christopher |e verfasserin |4 aut | |
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| 700 | 1 | |a Goodrich, Bret D. |e verfasserin |4 aut | |
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| 700 | 1 | |a Guzman, Stephanie S. |e verfasserin |4 aut | |
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| 700 | 1 | |a Hegwer, Steve |e verfasserin |4 aut | |
| 700 | 1 | |a Hubbard, Robert P. |e verfasserin |4 aut | |
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| 700 | 1 | |a Johansson, Erik M. |e verfasserin |4 aut | |
| 700 | 1 | |a Johnson, Luke C. |e verfasserin |4 aut | |
| 700 | 1 | |a Liang, Chen |e verfasserin |4 aut | |
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| 700 | 1 | |a McQuillen, Isaac |e verfasserin |4 aut | |
| 700 | 1 | |a Mayer, Christopher |e verfasserin |4 aut | |
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| 700 | 1 | |a Sekulic, Predrag |e verfasserin |4 aut | |
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10.1007/s11207-020-01736-7 doi (DE-627)SPR042272602 (DE-599)SPRs11207-020-01736-7-e (SPR)s11207-020-01736-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Rimmele, Thomas R. verfasserin aut The Daniel K. Inouye Solar Telescope – Observatory Overview 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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. Telescopes (dpeaa)DE-He213 Instrumentation (dpeaa)DE-He213 Sun (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Photosphere (dpeaa)DE-He213 Chromosphere (dpeaa)DE-He213 Corona (dpeaa)DE-He213 Warner, Mark verfasserin aut Keil, Stephen L. verfasserin aut Goode, Philip R. verfasserin aut Knölker, Michael verfasserin aut Kuhn, Jeffrey R. verfasserin aut Rosner, Robert R. verfasserin aut McMullin, Joseph P. verfasserin aut Casini, Roberto verfasserin aut Lin, Haosheng verfasserin aut Wöger, Friedrich verfasserin aut von der Lühe, Oskar verfasserin aut Tritschler, Alexandra verfasserin aut Davey, Alisdair verfasserin aut de Wijn, Alfred verfasserin aut Elmore, David F. verfasserin aut Fehlmann, André verfasserin aut Harrington, David M. verfasserin aut Jaeggli, Sarah A. verfasserin aut Rast, Mark P. verfasserin aut Schad, Thomas A. verfasserin aut Schmidt, Wolfgang verfasserin aut Mathioudakis, Mihalis verfasserin aut Mickey, Donald L. verfasserin aut Anan, Tetsu verfasserin aut Beck, Christian verfasserin aut Marshall, Heather K. verfasserin aut Jeffers, Paul F. verfasserin aut Oschmann, Jacobus M. verfasserin aut Beard, Andrew verfasserin aut Berst, David C. verfasserin aut Cowan, Bruce A. verfasserin aut Craig, Simon C. verfasserin aut Cross, Eric verfasserin aut Cummings, Bryan K. verfasserin aut Donnelly, Colleen verfasserin aut de Vanssay, Jean-Benoit verfasserin aut Eigenbrot, Arthur D. verfasserin aut Ferayorni, Andrew verfasserin aut Foster, Christopher verfasserin aut Galapon, Chriselle Ann verfasserin aut Gedrites, Christopher verfasserin aut Gonzales, Kerry verfasserin aut Goodrich, Bret D. verfasserin aut Gregory, Brian S. verfasserin aut Guzman, Stephanie S. verfasserin aut Guzzo, Stephen verfasserin aut Hegwer, Steve verfasserin aut Hubbard, Robert P. verfasserin aut Hubbard, John R. verfasserin aut Johansson, Erik M. verfasserin aut Johnson, Luke C. verfasserin aut Liang, Chen verfasserin aut Liang, Mary verfasserin aut McQuillen, Isaac verfasserin aut Mayer, Christopher verfasserin aut Newman, Karl verfasserin aut Onodera, Brialyn verfasserin aut Phelps, LeEllen verfasserin aut Puentes, Myles M. verfasserin aut Richards, Christopher verfasserin aut Rimmele, Lukas M. verfasserin aut Sekulic, Predrag verfasserin aut Shimko, Stephan R. verfasserin aut Simison, Brett E. verfasserin aut Smith, Brett verfasserin aut Starman, Erik verfasserin aut Sueoka, Stacey R. verfasserin aut Summers, Richard T. verfasserin aut Szabo, Aimee verfasserin aut Szabo, Louis verfasserin aut Wampler, Stephen B. verfasserin aut Williams, Timothy R. verfasserin aut White, Charles verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 295(2020), 12 vom: Dez. (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:295 year:2020 number:12 month:12 https://dx.doi.org/10.1007/s11207-020-01736-7 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 295 2020 12 12 |
| spelling |
10.1007/s11207-020-01736-7 doi (DE-627)SPR042272602 (DE-599)SPRs11207-020-01736-7-e (SPR)s11207-020-01736-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Rimmele, Thomas R. verfasserin aut The Daniel K. Inouye Solar Telescope – Observatory Overview 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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. Telescopes (dpeaa)DE-He213 Instrumentation (dpeaa)DE-He213 Sun (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Photosphere (dpeaa)DE-He213 Chromosphere (dpeaa)DE-He213 Corona (dpeaa)DE-He213 Warner, Mark verfasserin aut Keil, Stephen L. verfasserin aut Goode, Philip R. verfasserin aut Knölker, Michael verfasserin aut Kuhn, Jeffrey R. verfasserin aut Rosner, Robert R. verfasserin aut McMullin, Joseph P. verfasserin aut Casini, Roberto verfasserin aut Lin, Haosheng verfasserin aut Wöger, Friedrich verfasserin aut von der Lühe, Oskar verfasserin aut Tritschler, Alexandra verfasserin aut Davey, Alisdair verfasserin aut de Wijn, Alfred verfasserin aut Elmore, David F. verfasserin aut Fehlmann, André verfasserin aut Harrington, David M. verfasserin aut Jaeggli, Sarah A. verfasserin aut Rast, Mark P. verfasserin aut Schad, Thomas A. verfasserin aut Schmidt, Wolfgang verfasserin aut Mathioudakis, Mihalis verfasserin aut Mickey, Donald L. verfasserin aut Anan, Tetsu verfasserin aut Beck, Christian verfasserin aut Marshall, Heather K. verfasserin aut Jeffers, Paul F. verfasserin aut Oschmann, Jacobus M. verfasserin aut Beard, Andrew verfasserin aut Berst, David C. verfasserin aut Cowan, Bruce A. verfasserin aut Craig, Simon C. verfasserin aut Cross, Eric verfasserin aut Cummings, Bryan K. verfasserin aut Donnelly, Colleen verfasserin aut de Vanssay, Jean-Benoit verfasserin aut Eigenbrot, Arthur D. verfasserin aut Ferayorni, Andrew verfasserin aut Foster, Christopher verfasserin aut Galapon, Chriselle Ann verfasserin aut Gedrites, Christopher verfasserin aut Gonzales, Kerry verfasserin aut Goodrich, Bret D. verfasserin aut Gregory, Brian S. verfasserin aut Guzman, Stephanie S. verfasserin aut Guzzo, Stephen verfasserin aut Hegwer, Steve verfasserin aut Hubbard, Robert P. verfasserin aut Hubbard, John R. verfasserin aut Johansson, Erik M. verfasserin aut Johnson, Luke C. verfasserin aut Liang, Chen verfasserin aut Liang, Mary verfasserin aut McQuillen, Isaac verfasserin aut Mayer, Christopher verfasserin aut Newman, Karl verfasserin aut Onodera, Brialyn verfasserin aut Phelps, LeEllen verfasserin aut Puentes, Myles M. verfasserin aut Richards, Christopher verfasserin aut Rimmele, Lukas M. verfasserin aut Sekulic, Predrag verfasserin aut Shimko, Stephan R. verfasserin aut Simison, Brett E. verfasserin aut Smith, Brett verfasserin aut Starman, Erik verfasserin aut Sueoka, Stacey R. verfasserin aut Summers, Richard T. verfasserin aut Szabo, Aimee verfasserin aut Szabo, Louis verfasserin aut Wampler, Stephen B. verfasserin aut Williams, Timothy R. verfasserin aut White, Charles verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 295(2020), 12 vom: Dez. (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:295 year:2020 number:12 month:12 https://dx.doi.org/10.1007/s11207-020-01736-7 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 295 2020 12 12 |
| allfields_unstemmed |
10.1007/s11207-020-01736-7 doi (DE-627)SPR042272602 (DE-599)SPRs11207-020-01736-7-e (SPR)s11207-020-01736-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Rimmele, Thomas R. verfasserin aut The Daniel K. Inouye Solar Telescope – Observatory Overview 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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. Telescopes (dpeaa)DE-He213 Instrumentation (dpeaa)DE-He213 Sun (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Photosphere (dpeaa)DE-He213 Chromosphere (dpeaa)DE-He213 Corona (dpeaa)DE-He213 Warner, Mark verfasserin aut Keil, Stephen L. verfasserin aut Goode, Philip R. verfasserin aut Knölker, Michael verfasserin aut Kuhn, Jeffrey R. verfasserin aut Rosner, Robert R. verfasserin aut McMullin, Joseph P. verfasserin aut Casini, Roberto verfasserin aut Lin, Haosheng verfasserin aut Wöger, Friedrich verfasserin aut von der Lühe, Oskar verfasserin aut Tritschler, Alexandra verfasserin aut Davey, Alisdair verfasserin aut de Wijn, Alfred verfasserin aut Elmore, David F. verfasserin aut Fehlmann, André verfasserin aut Harrington, David M. verfasserin aut Jaeggli, Sarah A. verfasserin aut Rast, Mark P. verfasserin aut Schad, Thomas A. verfasserin aut Schmidt, Wolfgang verfasserin aut Mathioudakis, Mihalis verfasserin aut Mickey, Donald L. verfasserin aut Anan, Tetsu verfasserin aut Beck, Christian verfasserin aut Marshall, Heather K. verfasserin aut Jeffers, Paul F. verfasserin aut Oschmann, Jacobus M. verfasserin aut Beard, Andrew verfasserin aut Berst, David C. verfasserin aut Cowan, Bruce A. verfasserin aut Craig, Simon C. verfasserin aut Cross, Eric verfasserin aut Cummings, Bryan K. verfasserin aut Donnelly, Colleen verfasserin aut de Vanssay, Jean-Benoit verfasserin aut Eigenbrot, Arthur D. verfasserin aut Ferayorni, Andrew verfasserin aut Foster, Christopher verfasserin aut Galapon, Chriselle Ann verfasserin aut Gedrites, Christopher verfasserin aut Gonzales, Kerry verfasserin aut Goodrich, Bret D. verfasserin aut Gregory, Brian S. verfasserin aut Guzman, Stephanie S. verfasserin aut Guzzo, Stephen verfasserin aut Hegwer, Steve verfasserin aut Hubbard, Robert P. verfasserin aut Hubbard, John R. verfasserin aut Johansson, Erik M. verfasserin aut Johnson, Luke C. verfasserin aut Liang, Chen verfasserin aut Liang, Mary verfasserin aut McQuillen, Isaac verfasserin aut Mayer, Christopher verfasserin aut Newman, Karl verfasserin aut Onodera, Brialyn verfasserin aut Phelps, LeEllen verfasserin aut Puentes, Myles M. verfasserin aut Richards, Christopher verfasserin aut Rimmele, Lukas M. verfasserin aut Sekulic, Predrag verfasserin aut Shimko, Stephan R. verfasserin aut Simison, Brett E. verfasserin aut Smith, Brett verfasserin aut Starman, Erik verfasserin aut Sueoka, Stacey R. verfasserin aut Summers, Richard T. verfasserin aut Szabo, Aimee verfasserin aut Szabo, Louis verfasserin aut Wampler, Stephen B. verfasserin aut Williams, Timothy R. verfasserin aut White, Charles verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 295(2020), 12 vom: Dez. (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:295 year:2020 number:12 month:12 https://dx.doi.org/10.1007/s11207-020-01736-7 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 295 2020 12 12 |
| allfieldsGer |
10.1007/s11207-020-01736-7 doi (DE-627)SPR042272602 (DE-599)SPRs11207-020-01736-7-e (SPR)s11207-020-01736-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Rimmele, Thomas R. verfasserin aut The Daniel K. Inouye Solar Telescope – Observatory Overview 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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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10.1007/s11207-020-01736-7 doi (DE-627)SPR042272602 (DE-599)SPRs11207-020-01736-7-e (SPR)s11207-020-01736-7-e DE-627 ger DE-627 rakwb eng 530 ASE 39.51 bkl Rimmele, Thomas R. verfasserin aut The Daniel K. Inouye Solar Telescope – Observatory Overview 2020 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier Abstract 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. Telescopes (dpeaa)DE-He213 Instrumentation (dpeaa)DE-He213 Sun (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Photosphere (dpeaa)DE-He213 Chromosphere (dpeaa)DE-He213 Corona (dpeaa)DE-He213 Warner, Mark verfasserin aut Keil, Stephen L. verfasserin aut Goode, Philip R. verfasserin aut Knölker, Michael verfasserin aut Kuhn, Jeffrey R. verfasserin aut Rosner, Robert R. verfasserin aut McMullin, Joseph P. verfasserin aut Casini, Roberto verfasserin aut Lin, Haosheng verfasserin aut Wöger, Friedrich verfasserin aut von der Lühe, Oskar verfasserin aut Tritschler, Alexandra verfasserin aut Davey, Alisdair verfasserin aut de Wijn, Alfred verfasserin aut Elmore, David F. verfasserin aut Fehlmann, André verfasserin aut Harrington, David M. verfasserin aut Jaeggli, Sarah A. verfasserin aut Rast, Mark P. verfasserin aut Schad, Thomas A. verfasserin aut Schmidt, Wolfgang verfasserin aut Mathioudakis, Mihalis verfasserin aut Mickey, Donald L. verfasserin aut Anan, Tetsu verfasserin aut Beck, Christian verfasserin aut Marshall, Heather K. verfasserin aut Jeffers, Paul F. verfasserin aut Oschmann, Jacobus M. verfasserin aut Beard, Andrew verfasserin aut Berst, David C. verfasserin aut Cowan, Bruce A. verfasserin aut Craig, Simon C. verfasserin aut Cross, Eric verfasserin aut Cummings, Bryan K. verfasserin aut Donnelly, Colleen verfasserin aut de Vanssay, Jean-Benoit verfasserin aut Eigenbrot, Arthur D. verfasserin aut Ferayorni, Andrew verfasserin aut Foster, Christopher verfasserin aut Galapon, Chriselle Ann verfasserin aut Gedrites, Christopher verfasserin aut Gonzales, Kerry verfasserin aut Goodrich, Bret D. verfasserin aut Gregory, Brian S. verfasserin aut Guzman, Stephanie S. verfasserin aut Guzzo, Stephen verfasserin aut Hegwer, Steve verfasserin aut Hubbard, Robert P. verfasserin aut Hubbard, John R. verfasserin aut Johansson, Erik M. verfasserin aut Johnson, Luke C. verfasserin aut Liang, Chen verfasserin aut Liang, Mary verfasserin aut McQuillen, Isaac verfasserin aut Mayer, Christopher verfasserin aut Newman, Karl verfasserin aut Onodera, Brialyn verfasserin aut Phelps, LeEllen verfasserin aut Puentes, Myles M. verfasserin aut Richards, Christopher verfasserin aut Rimmele, Lukas M. verfasserin aut Sekulic, Predrag verfasserin aut Shimko, Stephan R. verfasserin aut Simison, Brett E. verfasserin aut Smith, Brett verfasserin aut Starman, Erik verfasserin aut Sueoka, Stacey R. verfasserin aut Summers, Richard T. verfasserin aut Szabo, Aimee verfasserin aut Szabo, Louis verfasserin aut Wampler, Stephen B. verfasserin aut Williams, Timothy R. verfasserin aut White, Charles verfasserin aut Enthalten in Solar physics Dordrecht [u.a.] : Springer Science + Business Media B.V, 1967 295(2020), 12 vom: Dez. (DE-627)269019162 (DE-600)1473830-2 1573-093X nnns volume:295 year:2020 number:12 month:12 https://dx.doi.org/10.1007/s11207-020-01736-7 kostenfrei Volltext GBV_USEFLAG_A SYSFLAG_A GBV_SPRINGER SSG-OPC-AST SSG-OPC-ASE GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_32 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_74 GBV_ILN_90 GBV_ILN_95 GBV_ILN_100 GBV_ILN_101 GBV_ILN_105 GBV_ILN_110 GBV_ILN_120 GBV_ILN_138 GBV_ILN_150 GBV_ILN_151 GBV_ILN_152 GBV_ILN_161 GBV_ILN_170 GBV_ILN_171 GBV_ILN_187 GBV_ILN_206 GBV_ILN_213 GBV_ILN_224 GBV_ILN_230 GBV_ILN_250 GBV_ILN_281 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_636 GBV_ILN_702 GBV_ILN_2001 GBV_ILN_2003 GBV_ILN_2004 GBV_ILN_2005 GBV_ILN_2006 GBV_ILN_2007 GBV_ILN_2008 GBV_ILN_2009 GBV_ILN_2010 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2015 GBV_ILN_2020 GBV_ILN_2021 GBV_ILN_2025 GBV_ILN_2026 GBV_ILN_2027 GBV_ILN_2031 GBV_ILN_2034 GBV_ILN_2037 GBV_ILN_2038 GBV_ILN_2039 GBV_ILN_2044 GBV_ILN_2048 GBV_ILN_2049 GBV_ILN_2050 GBV_ILN_2055 GBV_ILN_2056 GBV_ILN_2057 GBV_ILN_2059 GBV_ILN_2061 GBV_ILN_2064 GBV_ILN_2065 GBV_ILN_2068 GBV_ILN_2088 GBV_ILN_2093 GBV_ILN_2106 GBV_ILN_2107 GBV_ILN_2108 GBV_ILN_2110 GBV_ILN_2111 GBV_ILN_2112 GBV_ILN_2113 GBV_ILN_2118 GBV_ILN_2122 GBV_ILN_2129 GBV_ILN_2143 GBV_ILN_2144 GBV_ILN_2147 GBV_ILN_2148 GBV_ILN_2152 GBV_ILN_2153 GBV_ILN_2188 GBV_ILN_2190 GBV_ILN_2232 GBV_ILN_2336 GBV_ILN_2446 GBV_ILN_2470 GBV_ILN_2472 GBV_ILN_2507 GBV_ILN_2522 GBV_ILN_2548 GBV_ILN_4035 GBV_ILN_4037 GBV_ILN_4046 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4242 GBV_ILN_4246 GBV_ILN_4249 GBV_ILN_4251 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4326 GBV_ILN_4328 GBV_ILN_4333 GBV_ILN_4334 GBV_ILN_4335 GBV_ILN_4336 GBV_ILN_4338 GBV_ILN_4393 GBV_ILN_4700 39.51 ASE AR 295 2020 12 12 |
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Rimmele, Thomas R. @@aut@@ Warner, Mark @@aut@@ Keil, Stephen L. @@aut@@ Goode, Philip R. @@aut@@ Knölker, Michael @@aut@@ Kuhn, Jeffrey R. @@aut@@ Rosner, Robert R. @@aut@@ McMullin, Joseph P. @@aut@@ Casini, Roberto @@aut@@ Lin, Haosheng @@aut@@ Wöger, Friedrich @@aut@@ von der Lühe, Oskar @@aut@@ Tritschler, Alexandra @@aut@@ Davey, Alisdair @@aut@@ de Wijn, Alfred @@aut@@ Elmore, David F. @@aut@@ Fehlmann, André @@aut@@ Harrington, David M. @@aut@@ Jaeggli, Sarah A. @@aut@@ Rast, Mark P. @@aut@@ Schad, Thomas A. @@aut@@ Schmidt, Wolfgang @@aut@@ Mathioudakis, Mihalis @@aut@@ Mickey, Donald L. @@aut@@ Anan, Tetsu @@aut@@ Beck, Christian @@aut@@ Marshall, Heather K. @@aut@@ Jeffers, Paul F. @@aut@@ Oschmann, Jacobus M. @@aut@@ Beard, Andrew @@aut@@ Berst, David C. @@aut@@ Cowan, Bruce A. @@aut@@ Craig, Simon C. @@aut@@ Cross, Eric @@aut@@ Cummings, Bryan K. @@aut@@ Donnelly, Colleen @@aut@@ de Vanssay, Jean-Benoit @@aut@@ Eigenbrot, Arthur D. @@aut@@ Ferayorni, Andrew @@aut@@ Foster, Christopher @@aut@@ Galapon, Chriselle Ann @@aut@@ Gedrites, Christopher @@aut@@ Gonzales, Kerry @@aut@@ Goodrich, Bret D. @@aut@@ Gregory, Brian S. @@aut@@ Guzman, Stephanie S. @@aut@@ Guzzo, Stephen @@aut@@ Hegwer, Steve @@aut@@ Hubbard, Robert P. @@aut@@ Hubbard, John R. @@aut@@ Johansson, Erik M. @@aut@@ Johnson, Luke C. @@aut@@ Liang, Chen @@aut@@ Liang, Mary @@aut@@ McQuillen, Isaac @@aut@@ Mayer, Christopher @@aut@@ Newman, Karl @@aut@@ Onodera, Brialyn @@aut@@ Phelps, LeEllen @@aut@@ Puentes, Myles M. @@aut@@ Richards, Christopher @@aut@@ Rimmele, Lukas M. @@aut@@ Sekulic, Predrag @@aut@@ Shimko, Stephan R. @@aut@@ Simison, Brett E. @@aut@@ Smith, Brett @@aut@@ Starman, Erik @@aut@@ Sueoka, Stacey R. @@aut@@ Summers, Richard T. @@aut@@ Szabo, Aimee @@aut@@ Szabo, Louis @@aut@@ Wampler, Stephen B. @@aut@@ Williams, Timothy R. @@aut@@ White, Charles @@aut@@ |
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530 ASE 39.51 bkl The Daniel K. Inouye Solar Telescope – Observatory Overview Telescopes (dpeaa)DE-He213 Instrumentation (dpeaa)DE-He213 Sun (dpeaa)DE-He213 Magnetic fields (dpeaa)DE-He213 Photosphere (dpeaa)DE-He213 Chromosphere (dpeaa)DE-He213 Corona (dpeaa)DE-He213 |
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Rimmele, Thomas R. Warner, Mark Keil, Stephen L. Goode, Philip R. Knölker, Michael Kuhn, Jeffrey R. Rosner, Robert R. McMullin, Joseph P. Casini, Roberto Lin, Haosheng Wöger, Friedrich von der Lühe, Oskar Tritschler, Alexandra Davey, Alisdair de Wijn, Alfred Elmore, David F. Fehlmann, André Harrington, David M. Jaeggli, Sarah A. Rast, Mark P. Schad, Thomas A. Schmidt, Wolfgang Mathioudakis, Mihalis Mickey, Donald L. Anan, Tetsu Beck, Christian Marshall, Heather K. Jeffers, Paul F. Oschmann, Jacobus M. Beard, Andrew Berst, David C. Cowan, Bruce A. Craig, Simon C. Cross, Eric Cummings, Bryan K. Donnelly, Colleen de Vanssay, Jean-Benoit Eigenbrot, Arthur D. Ferayorni, Andrew Foster, Christopher Galapon, Chriselle Ann Gedrites, Christopher Gonzales, Kerry Goodrich, Bret D. Gregory, Brian S. Guzman, Stephanie S. Guzzo, Stephen Hegwer, Steve Hubbard, Robert P. Hubbard, John R. Johansson, Erik M. Johnson, Luke C. Liang, Chen Liang, Mary McQuillen, Isaac Mayer, Christopher Newman, Karl Onodera, Brialyn Phelps, LeEllen Puentes, Myles M. Richards, Christopher Rimmele, Lukas M. Sekulic, Predrag Shimko, Stephan R. Simison, Brett E. Smith, Brett Starman, Erik Sueoka, Stacey R. Summers, Richard T. Szabo, Aimee Szabo, Louis Wampler, Stephen B. Williams, Timothy R. White, Charles |
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The Daniel K. Inouye Solar Telescope – Observatory Overview |
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Abstract 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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Abstract 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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Abstract 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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Inouye Solar Telescope – Observatory Overview</subfield></datafield><datafield tag="264" ind1=" " ind2="1"><subfield code="c">2020</subfield></datafield><datafield tag="336" ind1=" " ind2=" "><subfield code="a">Text</subfield><subfield code="b">txt</subfield><subfield code="2">rdacontent</subfield></datafield><datafield tag="337" ind1=" " ind2=" "><subfield code="a">Computermedien</subfield><subfield code="b">c</subfield><subfield code="2">rdamedia</subfield></datafield><datafield tag="338" ind1=" " ind2=" "><subfield code="a">Online-Ressource</subfield><subfield code="b">cr</subfield><subfield code="2">rdacarrier</subfield></datafield><datafield tag="520" ind1=" " ind2=" "><subfield code="a">Abstract 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. 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| score |
7.4008837 |