List of astronomical interferometers at visible and infrared wavelengths

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
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)
Comments
CHARA Array[1]V, R, I, J, H, K83433075000.71%103000030000 in the visible band; maximum baseline 330-m
COAST visibleR, I746020000.54%104?300 cloudy nights per year, maximum baseline 100-m
COAST infraredJ, H34601000.520%101300 cloudy nights per year, maximum baseline 100-m
GI2T visibleR, I510652000010%-400?CLOSED in 2006
IOTAJ, H, K, L'7630100000.32%101?Integrated optics beam combiner. CLOSED.
ISIN0105050000.31%11000Maximum baseline 70-m
Keck InterferometerH, K, L, N10.38585100004%1330Nulling Key Science Underway - No imaging on a single baseline instrument; maximum baseline 11-m. CLOSED.
Keck Aperture MaskingJ, H, K, L20.59200000.920%101CLOSED.
MIRA 1.2R, I33030500010%-1Mid-Infrared
Navy Precision Optical Interferometer(NPOI) visibleV, R, I55300500000.74%1016at NOFS; siderstats operational 4 x 1.8m added apertures in FY13. World's largest optical baseline-437m, 6-phased
Palomar Testbed Interferometer[2]J,H,K7861105000002%0.15,10"dual-star" capable , No imaging on a single baseline instrument. CLOSED 2009.
SUSIB, V, R, I55640500004%1021No imaging on a single baseline instrument; Maximum baseline 160m
VLTI
+UTs AMBER
J, H, K simultaneously7461304000.31%102000Used for a few weeks per year. Longest overall VLTI Baseline 130m
VLTI
+ATs AMBER
J, H, K simultaneously4461304000.31%102000Longest overall VLTI Baseline 130m
VLTI
+UTs VINCI
K11461304000>1%-1Integrated optics beam combiner. Longest overall VLTI Baseline 130m
VLTI
+ATs VINCI
KNever checked122004000>1%-1Longest overall VLTI Baseline 130m.
VLTI
+UTs MIDI
N4.546130200010%-250Used for a few weeks per year. Longest overall VLTI Baseline 130m. Dismantled Apr 2015
VLTI
+ATs MIDI
N4.5?200200010%-250VLTI inldes World's largest unfilled apertures (siderostats, 1.8-m, 8-m). Longest overall VLTI Baseline 130m. Dismantled Apr 2015

New interferometers and improvements to existing interferometers

Expected 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)
Comments
LBTI
(near infrared)
J, H, K>2002210000000130%100100?2006?
MROR, I, J, H, K1474001000000.61%101000?Under Construction
VLTI
(near infrared using 4 ATs and PRIMA)
J, H, K1282001000011%0.14000?decommissioned 2014
VLTI
(near infrared using 3 UTs and PRIMA)
J, H, K144613050011%0.34000?decommissioned 2014
VLTI
(near infrared using 4 UTs and MATISSE)
J, H, K, N, Qcommissioning 2017?

See also

References

  1. T.A. ten Brummelaar; et al. (2005). "First Results from the CHARA Array. II. A Description of the Instrument". Astrophysical Journal. 628 (1): 453. arXiv:astro-ph/0504082. Bibcode:2005ApJ...628..453T. doi:10.1086/430729.
  2. M.M. Colavita; et al. (1999). "The Palomar Testbed Interferometer". Astrophysical Journal. 510 (1): 505. arXiv:astro-ph/9810262. Bibcode:1999ApJ...510..505C. doi:10.1086/306579.

Further reading

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