List of astronomical interferometers at visible and infrared wavelengths
August 21, 2023
Here is a list of currently existing astronomical optical interferometers (i.e. operating from visible to mid-infrared wavelengths), and some parameters describing their performance.
Current performance of ground-based interferometers
Columns 2-5 determine the range of targets that can be observed and the range of science which can be done. Higher limiting magnitude means that the array can observe fainter sources. The limiting magnitude is determined by the atmospheric seeing, the diameters of the telescopes and the light lost in the system. A larger range of baselines means that a wider variety of science can be done and on a wider range of sources.
Columns 6-10 indicate the approximate quality and total amount of science data the array is expected to obtain. This is per year, to account for the average number of cloud-free nights on which each array is operated.
Current Performance of Existing Astronomical Interferometers
^T.A. ten Brummelaar; et al. (2005). "First Results from the CHARA Array. II. A Description of the Instrument". Astrophysical Journal. 628 (1): 453–465. arXiv:astro-ph/0504082. Bibcode:2005ApJ...628..453T. doi:10.1086/430729. S2CID 987223.
^M.M. Colavita; et al. (1999). "The Palomar Testbed Interferometer". Astrophysical Journal. 510 (1): 505–521. arXiv:astro-ph/9810262. Bibcode:1999ApJ...510..505C. doi:10.1086/306579. S2CID 15986684.
Further reading
Fujinobu Takahashi (2000). Very long baseline interferometer. IOS Press. ISBN4-274-90378-8.
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Here is a list of currently existing astronomical optical interferometers i e operating from visible to mid infrared wavelengths and some parameters describing their performance Contents 1 Current performance of ground based interferometers 2 New interferometers and improvements to existing interferometers 3 See also 4 References 5 Further readingCurrent performance of ground based interferometers EditColumns 2 5 determine the range of targets that can be observed and the range of science which can be done Higher limiting magnitude means that the array can observe fainter sources The limiting magnitude is determined by the atmospheric seeing the diameters of the telescopes and the light lost in the system A larger range of baselines means that a wider variety of science can be done and on a wider range of sources Columns 6 10 indicate the approximate quality and total amount of science data the array is expected to obtain This is per year to account for the average number of cloud free nights on which each array is operated Current Performance of Existing Astronomical Interferometers Interferometer and observing mode Waveband Limiting magnitude Minimum baseline m un projected Maximum baseline m Approx no visibility measurements per year measurements per night x nights used per year Max ratio of no phase no amplitude measurements measure of imaging performance 0 none Accuracy of amplitude2 measurements Accuracy of phase measurements milli radians Number of spectral channels max in use simultaneously Operational CommentsCHARA Array 1 V R I J H K 8 34 330 7500 0 7 1 10 30000 Yes 30000 in the visible band maximum baseline 330 mCOAST visible R I 7 4 60 2000 0 5 4 10 4 Closed 300 cloudy nights per year maximum baseline 100 mCOAST infrared J H 3 4 60 100 0 5 20 10 1 Closed 300 cloudy nights per year maximum baseline 100 mGI2T visible R I 5 10 65 2000 0 10 400 Closed CLOSED in 2006IOTA J H K L 7 6 30 10000 0 3 2 10 1 Closed Integrated optics beam combiner CLOSED ISI N 0 10 50 5000 0 3 1 1 1000 Closed Maximum baseline 70 mKeck Interferometer H K L N 10 3 85 85 1000 0 4 1 330 Closed Nulling Key Science Underway No imaging on a single baseline instrument maximum baseline 11 m CLOSED Keck Aperture Masking J H K L 2 0 5 9 20000 0 9 20 10 1 CLOSED MIRA 1 2 R I 3 30 30 500 0 10 1 Closed Mid InfraredNavy Precision Optical Interferometer NPOI V R I 6 5 97 operational 432 not yet commissioned 50000 0 7 4 10 16 Yes at Lowell Observatory 12cm siderostats operational3 x 1 0m apertures being addedWorld s largest optical baseline 437m6 phasedPalomar Testbed Interferometer 2 J H K 7 86 110 50000 0 2 0 1 5 10 Closed dual star capable No imaging on a single baseline instrument CLOSED 2009 SUSI B V R I 5 5 160 operated 640 never commissioned 5000 0 4 10 21 Closed No imaging on a single baseline instrument Maximum baseline 160mVLTI UTs AMBER J H K simultaneously 7 46 130 400 0 3 1 10 2000 Yes Used for a few weeks per year Longest overall VLTI Baseline 130mVLTI ATs AMBER J H K simultaneously 4 46 130 400 0 3 1 10 2000 Yes Longest overall VLTI Baseline 130mVLTI UTs VINCI K 11 46 130 400 0 gt 1 1 Yes Integrated optics beam combiner Longest overall VLTI Baseline 130mVLTI ATs VINCI K Never checked 12 200 400 0 gt 1 1 Yes Longest overall VLTI Baseline 130m VLTI UTs MIDI N 4 5 46 130 200 0 10 250 Yes Used for a few weeks per year Longest overall VLTI Baseline 130m Dismantled Apr 2015VLTI ATs MIDI N 4 5 200 200 0 10 250 Yes VLTI inldes World s largest unfilled apertures siderostats 1 8 m 8 m Longest overall VLTI Baseline 130m Dismantled Apr 2015New interferometers and improvements to existing interferometers EditExpected Future Performance of Astronomical Interferometers Interferometer and observing mode Waveband Limiting magnitude Minimum baseline m un projected Maximum baseline m Approx no visibility measurements per year measurements per night x nights used per year Max ratio of no phase no amplitude measurements measure of imaging performance 0 none Accuracy of amplitude2 measurements Accuracy of phase measurements milli radians Number of spectral channels max in use simultaneously CommentsLBTI near infrared J H K gt 20 0 22 10000000 1 30 100 100 2006 MRO R I J H K 14 7 400 100000 0 6 1 10 1000 Under ConstructionVLTI near infrared using 4 ATs and PRIMA J H K 12 8 200 10000 1 1 0 1 4000 decommissioned 2014VLTI near infrared using 3 UTs and PRIMA J H K 14 46 130 500 1 1 0 3 4000 decommissioned 2014VLTI near infrared using 4 UTs and MATISSE J H K N Q commissioning 2017 See also EditLists of telescopes Photometric system has a key for waveband letters References Edit T A ten Brummelaar et al 2005 First Results from the CHARA Array II A Description of the Instrument Astrophysical Journal 628 1 453 465 arXiv astro ph 0504082 Bibcode 2005ApJ 628 453T doi 10 1086 430729 S2CID 987223 M M Colavita et al 1999 The Palomar Testbed Interferometer Astrophysical Journal 510 1 505 521 arXiv astro ph 9810262 Bibcode 1999ApJ 510 505C doi 10 1086 306579 S2CID 15986684 Further reading EditFujinobu Takahashi 2000 Very long baseline interferometer IOS Press ISBN 4 274 90378 8 Portals Astronomy Stars Spaceflight Outer space Solar System Retrieved from https en wikipedia org w index php title List of astronomical interferometers at visible and infrared wavelengths amp oldid 1117788910, wikipedia, wiki, book, books, library,
