가시광선 및 적외선 파장 천문간섭계 목록
지상 간섭계의 현재 성능

2-5열은 관찰할 수 있는 표적의 범위와 수행할 수 있는 과학의 영역을  결정한다. 더 높은 한계 등급은 어레이가 더 희미한 소스를 관찰할 수 있음을 의미한다. 한계 등급은 대기 관측, 망원경의 직경 및 시스템에서 손실된 빛에 의해 결정된다.  더 넓은 범위의 기준선은 더 넓은 범위의 광원에 대하여 더 다양한 영역의 과학에서 수행할 수 있음을 의미한다.
열 6-10은 어레이에 의하여 얻을 수 있을 것으로 예상되는 과학 데이터의 대략적인 품질과 총량을 나타낸다. 이는 연간 데이터로 각 어레이가 운영되는 구름 없는 야간 일수의 평균 값을 설명한다.
| 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? | Comments |
| --- | --- | --- | --- | --- | --- | --- | --- | --- | --- | --- | --- |
| CHARA Array | V, R, I, J, H, K | 8 | 34 | 330 | 7500 | 0.7 | 1% | 10 | 30000 | Yes | 30000 in the visible band; maximum baseline 330-m |
| COAST visible | R, I | 7 | 4 | 60 | 2000 | 0.5 | 4% | 10 | 4? | Closed | 300 cloudy nights per year, maximum baseline 100-m |
| COAST infrared | J, H | 3 | 4 | 60 | 100 | 0.5 | 20% | 10 | 1 | Closed | 300 cloudy nights per year, maximum baseline 100-m |
| GI2T visible | R, I | 5 | 10 | 65 | 2000 | 0 | 10% | - | 400? | Closed | CLOSED in 2006 |
| IOTA | 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-m |
| Keck 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-Infrared |
| Navy 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 operational 3 x 1.0m apertures being added World's largest optical baseline-437m 6-phased |
| Palomar Testbed Interferometer | 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 160m |
| VLTI  +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 130m |
| VLTI  +ATs AMBER | J, H, K simultaneously | 4 | 46 | 130 | 400 | 0.3 | 1% | 10 | 2000 | Yes | Longest overall VLTI Baseline 130m |
| VLTI  +UTs VINCI | K | 11 | 46 | 130 | 400 | 0 | >1% | - | 1 | Yes | Integrated optics beam combiner. Longest overall VLTI Baseline 130m |
| VLTI  +ATs VINCI | K | Never checked | 12 | 200 | 400 | 0 | >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 2015 |
| VLTI  +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 2015 |