가시광선 및 적외선 파장 천문간섭계 목록

다음은 현재 존재하는 천문학적 광학 간섭계 (즉, 가시광선에서 중적외선 파장까지 작동)의 목록 및 그 성능에 관한 매개변수 일부이다.
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. 
+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?
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
+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
>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 Construction
VLTI(near infrared using 4 ATs and PRIMA)
J, H, K
12
8
200
10000
1
1%
0.1
4000?
decommissioned 2014
VLTI(near infrared using 3 UTs and PRIMA)
J, H, K
14
46
130
500
1
1%
0.3
4000?
decommissioned 2014
VLTI(near infrared using 4 UTs and MATISSE)
J, H, K, N, Q
commissioning 2017?
* 망원경 목록
* 파장 대역을 나타내는 문자 키는 측광 시스템에 있다.
* 
분류:우주에 관한 목록