Receiver Noise

Noise, Receiver


the electrical fluctuations that occur mainly in the input circuits (for example, amplifiers and filters) of radio-receiving apparatus (seeFLUCTUATIONS, ELECTRICAL).

When combined with noises from external sources, such as atmospheric noise, terrestrial noise, and cosmic noise, a total noise is produced that acts as a natural threshold of the sensitivity of the radio receiver. The quantitative characteristic of receiver-noise intensity is its noise temperature. For example, until the 1950’s, the input devices used in superhigh-frequency radio receivers had noise temperatures of more than 2000°K, which was many times higher than the noise temperatures of the external sources. Subsequently, low-noise, superhigh-frequency amplifying devices were invented, such as tunnel diodes, parametric amplifiers, and quantum mechanical amplifiers, which made it possible to lower the receiver-noise temperatures, respectively, to values of the order of 300°, 30°, and 3 K, thereby improving the sensitivity of superhigh-frequency radio receivers by about 10 to 50 times.


Ainbinder, 1. M. Shumy radiopriemnikov. Moscow, 1974.


References in periodicals archive ?
The transmit power test value is 20dBm and the receiver noise level is 90dBm, requiring a total cancellation of the 110dBm interference for proper operation of a full duplex system.
7 antenna pattern Antenna downtilt 3[degrees] Receiver noise figure NF = 5 dB Cell size/radius 8 km Sectorization 3 sectors Antenna polarization [+ or -] 45[degrees] Reference sensitivity -101.
Fully symmetric receiver thresholds ensure the devices maintain good duty cycle symmetry at low signal levels and boost receiver noise immunity, while supporting full failsafe operation.
For a baseline, receiver noise figure was first measured with a noise source and a spectrum analyzer as discussed in reference 1.
By providing high-efficiency operation and low dynamic EVM over temperature and low receiver noise figure, this new FEM can extend the range of a 5 GHz ultra high data rate 802.
Dependence of an error probability for a BPSK modulation scheme on free space path loss: dots - without coding, circles - with convolutional coding (rate 3/4, constraint length K = 7); receiver noise temperature is 20 K (dashed lines) and 290 K (solid lines); HPA back-off level is 7 dB; phase and frequency offsets are equal to zero; antennas gain G = 1; satellite phase noise is negligible
1] HPA back-off level BER (Satellite and Ground Receiver Noise (Aircraft and Temperatures T = 290 K) Satellite) Free Space Path Loss 110 dB 112 dB 115 dB 1.
Others include details of practical low noise amplifiers, logarithmic amplifiers and the measurement of receiver noise performance.
B] the Boltzmann's constant, T the receiver noise temperature, and [R.
4 [4] doesn't include the interferer's state, so the assumed distribution of receiver noise power for LR-WPAN is shown in Fig.
5 dB of antenna gain and a receiver noise figure of 5 dB.
The gain block between the front-end and the back-end is necessary to meet the overall receiver noise figure (< 9 dB) specification.

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