Table 1
Radiative background and photon noise from instrument, atmosphere, and astrophysical background in several sub-bands suitable for SZE measurements.
| Ground | ||
|
|
||
| Band | Background | Noise in 1s |
| (GHz) | (pW) | (fW/GHz) |
|
|
||
| 85−110 | 40 | 55 |
| 125−175 | 110 | 110 |
|
|
||
| Stratospheric balloon | ||
|
|
||
| Band | Background | Noise in 1s |
| (GHz) | (pW) | (fW/GHz) |
|
|
||
| 125−175 | 80 | 90 |
| 190−260 | 110 | 130 |
| 280−360 | 110 | 160 |
| 390−420 | 40 | 100 |
|
|
||
| Satellite | ||
|
|
||
| Band | Background | Noise in 1s |
| (GHz) | (pW) | (fW/GHz) |
|
|
||
| 100−180 | 7 | 30 |
| 180−350 | 10 | 50 |
| 350−700 | 16 | 80 |
| 700−1000 | 7 | 70 |
Notes. Photon noise per spectral bin is computed assuming that noise from all the frequencies within the sub-band is contributing to the measurement of the considered bin. Top: room-temperature spectrometer on a ground-based telescope (1 mm PWV). Middle: room-temperature spectrometer on a stratospheric balloon. Bottom: cold (2 K) spectrometer on a satellite. All instruments are diffraction limited at the lowest end of each sub-band. Turbulence and atmospheric fluctuations, which can be relevant in the groud-based case, are not included.
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