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| [[ http://www.stsci.edu/jwst/instruments/miri/sensitivity | This table ]] gives the sensitivity and the $ \lambda $ but not the $ \Delta\lambda $, so I will guess: || λ || sensitivity || Δλ || c Δλ/λ^2^ || || μm || μJy || μm (guess) || Hz (guess) || || 5.6 || 0.2 || 2.0 || 1.9e13 || || 7.7 || 0.28 || 2.0 || 1.2e13 || || 10 || 0.7 || 2.0 || 6.0e12 || || 11.3 || 1.7 || 2.0 || 4.7e12 || || 12.8 || 1.4 || 2.0 || 3.6e12 || || 15 || 1.8 || 2.5 || 3.3e12 || || 18 || 4.3 || 3.0 || 2.8e12 || || 21 || 8.6 || 4.0 || 2.7e12 || || 25.5 || 28 || 5.0 || 2.3e12 || |
* [[ http://ircamera.as.arizona.edu/MIRI/performance.htm | This table ]] gives the sensitivity, recomputed here: * (detection limit, 10 sigma, 10,000 seconds) || || λ || λ/ || sensitivity || Jy-Hz || λ,,0,, || λ,,1,, || || || μm || /Δλ || μJy || W/m^2^ || μm || μm || || F560W || 5.6 || 5 || 0.16 || 1.7e-20 || 6.19 || 5.07 || || F770W || 7.7 || 3.5 || 0.25 || 2.8e-20 || 8.88 || 6.68 || || F1000W || 10 || 5 || 0.54 || 3.2e-20 || 11.05 || 9.05 || || F1130W || 11.3 || 16 || 1.35 || 2.2e-20 || 11.66 || 10.95 || || F1280W || 12.8 || 5 || 0.84 || 3.9e-20 || 14.14 || 11.58 || || F1500W || 15 || 5 || 1.39 || 5.6e-20 || 16.57 || 13.57 || || F1800W || 18 || 6 || 3.46 || 9.6e-20 || 19.56 || 16.56 || || F2100W || 21 || 4 || 7.09 || 2.5e-19 || 23.79 || 18.54 || || F2550W || 25.5 || 6 || 26.2 || 5.1e-19 || 27.71 || 23.46 || |
Infrared Telescopes
Jansky Units and Infrared Radio Telescopes
1 Jansky is 1e-26 W/m2-Hz. Hz implies bandwidth. The bandwidth of a radio telescope is obvious - the bandwidth in Hertz, probably after a chilled reflector into a chilled low noise amplifier, then through a filter. A wider filter picks up more power, and more thermal noise. So the power in Janksy units for a source is Jy = 1e26 * Power~Received / ( Area * ( f_2 - f_1 ) with power in watts, Area of the receiving surface in square meters, and frequencies in Hertz.
Infrared telescopes have much wider bandwidth, and infrared is typically characterized with wavelength (usually micrometers) rather than Hertz. We can recast the formula as
Jy~=~1e26*(P/A)*c*(1/\lambda_2-1/\lambda_1)~=~1e26*(P/A)*c(\lambda_1-\lambda_2)/(\lambda_1\lambda_2)
where c is the speed of light. Defining \Delta\lambda~=~\lambda_1-\lambda_2 and center wavelength \lambda = \sqrt{\lambda_1\lambda_2}, this simplifies to:
Jy ~=~ 1e26*(P/A)*c~\Delta\lambda/\lambda^2
So, how much is that? A parsec is 3.26 light years or 3.0857e16 meters, like a star that appears to move one arcsecond in the sky as the earth moves 1 AU across its orbit. So, a sphere 1 AU in diameter would appear one arc-second across from 1 parsec away. From 200 parsecs away ( 6.1714e18 meters ), a sphere 100 AU in radius or 200 AU in diameter, and heated by the entire sun's output (3.86e26 W), would be about 60K, and deposit all that power on a 200 parsec diameter sphere with an area of 4.786e38 square meters, a power density of 8.07e-13W/m2. We still don't know enough to compute the Jansky units, because we don't know the bandwidth. That is a function of the filtering and imager on our telescope - and if the telescope is not in orbit, the passband and emissions of the atmosphere.
Kuiper Server Sky
A shell 100 AU in diameter at 60K enclosing the sun. Peak emissions at 48μm and a power flux of 0.1366 W/m2. Here is a table of wavelengths (in micrometers) at the 1st, 2nd, etc. to the 99th percentile.
% |
+00 |
+01 |
+02 |
+03 |
+04 |
+05 |
+06 |
+07 |
+08 |
+09 |
00 |
0.00 |
24.13 |
26.72 |
28.58 |
30.09 |
31.41 |
32.59 |
33.68 |
34.70 |
35.66 |
10 |
36.59 |
37.48 |
38.33 |
39.17 |
39.98 |
40.78 |
41.56 |
42.34 |
43.10 |
43.85 |
20 |
44.60 |
45.35 |
46.09 |
46.82 |
47.56 |
48.29 |
49.03 |
49.76 |
50.50 |
51.24 |
30 |
51.98 |
52.73 |
53.48 |
54.23 |
54.99 |
55.76 |
56.53 |
57.32 |
58.10 |
58.90 |
40 |
59.71 |
60.53 |
61.35 |
62.19 |
63.05 |
63.91 |
64.79 |
65.68 |
66.59 |
67.51 |
50 |
68.46 |
69.42 |
70.40 |
71.40 |
72.42 |
73.46 |
74.53 |
75.63 |
76.75 |
77.90 |
60 |
79.09 |
80.30 |
81.55 |
82.84 |
84.17 |
85.54 |
86.96 |
88.43 |
89.95 |
91.52 |
70 |
93.16 |
94.86 |
96.64 |
98.49 |
100.43 |
102.47 |
104.60 |
106.85 |
109.22 |
111.73 |
80 |
114.39 |
117.22 |
120.25 |
123.50 |
127.00 |
130.79 |
134.92 |
139.44 |
144.44 |
150.00 |
90 |
156.26 |
163.39 |
171.63 |
181.33 |
193.05 |
207.65 |
226.70 |
253.35 |
295.35 |
381.33 |
James Webb Space Telescope
NASA's JWST Mid Infrared Instrument (MIRI), scheduled to deploy in 2018, will be the most powerful long distance infrared imager available, with a 6.5 meter mirror. The imager is a 1024x1024 pixel Raytheon Si:As sensor chip assembly (SCA) with 25 µm pixels. The pixels are 0.11 arcseconds.
This table gives the sensitivity, recomputed here:
- (detection limit, 10 sigma, 10,000 seconds)
|
λ |
λ/ |
sensitivity |
Jy-Hz |
λ0 |
λ1 |
|
μm |
/Δλ |
μJy |
W/m2 |
μm |
μm |
F560W |
5.6 |
5 |
0.16 |
1.7e-20 |
6.19 |
5.07 |
F770W |
7.7 |
3.5 |
0.25 |
2.8e-20 |
8.88 |
6.68 |
F1000W |
10 |
5 |
0.54 |
3.2e-20 |
11.05 |
9.05 |
F1130W |
11.3 |
16 |
1.35 |
2.2e-20 |
11.66 |
10.95 |
F1280W |
12.8 |
5 |
0.84 |
3.9e-20 |
14.14 |
11.58 |
F1500W |
15 |
5 |
1.39 |
5.6e-20 |
16.57 |
13.57 |
F1800W |
18 |
6 |
3.46 |
9.6e-20 |
19.56 |
16.56 |
F2100W |
21 |
4 |
7.09 |
2.5e-19 |
23.79 |
18.54 |
F2550W |
25.5 |
6 |
26.2 |
5.1e-19 |
27.71 |
23.46 |
Herschel
ESA's Herschel Space Telescope, active from 2009 to 2013, has a 3.5 meter mirror and a wavelength range of 55 to 672 μm. The Photodetector Array Camera and Spectrometer (PACS) uses two low resolution arrays of bolometers:
Red |
16x32 |
6.4as |
Blue |
32x64 |
3.2as |
These measure in 3 bands, either 70 alone or 100 and 160 together:
70 |
60 to 85 μm |
5 mJy (5σ, 1h) |
100 |
85 to 130 μm |
5 mJy (5σ, 1h) |
160 |
130 to 210 μm |
10 mJy (5σ, 1h) |