. "Appendix H Use of 0 dBi for Sidelobe Gain in Calculations of Interference in Radio Astronomy Bands." Handbook of Frequency Allocations and Spectrum Protection for Scientific Uses . Washington, DC: The National Academies Press, 2007.
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Handbook of Frequency Allocations and Spectrum Protection for Scientific Uses
TABLE H.1 Characteristics of Antenna Sidelobe Models
Φ0 (G = 0 dBi)
SA.509 (32-25 log Φ)
S.580 (29-25 log Φ)
RA.1631 and S.1428 (34-30 log Φ)
An examination of the choice of 0 dBi, rather than some other constant gain figure, can be made with the aid of the more detailed reference models of sidelobe levels that have subsequently been developed. An early reference model for a large antenna is found in Recommendation ITU-R RS.509. The sidelobe gain as a function of boresight angle Φ is equal to (32-25 log Φ) dBi for 1°<Φ<48°, and is a constant value of −10 dBi for Φ >48°. With this model the 0 dBi sidelobe level occurs at a boresight angle of Φ0 = 19°. However, radio astronomy antennas are commonly used over a range of elevation angles down to ~10° when tracking a source under study across the sky. As a result, sidelobes of a level several decibels greater that 0 dBi are sometimes presented toward the horizon, which is the direction of incidence for signals from terrestrial transmitters. Hence, for sidelobes represented by Recommendation ITU-R RS.509, the 0 dBi figure does not guarantee freedom from interference.
The average percentage of data loss when the detrimental threshold is determined using the 0 dBi figure can be estimated using the models for antenna sidelobe levels, as follows. Included here are more recent models based on improved antenna design, which are found in Recommendations ITU-R S.580, S.1248, and RA.1631. For each of the models, the boresight angle Φ0 for which the gain is 0 dBi is given in column 2 of Table H.1. The solid angle of the antenna response for which the gain exceeds 0 dBi is Ω = 2π (1-cos Φ0) steradian. This is given for each model in column 3 of the table, expressed as a fraction of the hemisphere (from the horizon to the zenith) from which interference can arrive. Thus, if it is assumed that the angles of pointing of the radio astronomy antenna are uniformly distributed over the sky (which is only approximately the case) and that one interfering transmitter is active, the values in column 3 provide an estimate of the fraction of time that the interference received exceeds the detrimental level.2 For the more recent sidelobe models in the table these values are ~3 percent, and to reduce this result to 2 percent (the maximum tolerable value, as noted above), one would need to use a detrimental threshold based on a sidelobe gain slightly higher than 0 dBi. However, the 0 dBi value has the advantage of simplicity, and within the uncertainties of the pointing distribution, it results in detrimental thresholds in reasonable accord with the acceptable loss of observing time.
When the elevation angle of the main beam of the radio astronomy antenna is less than Φ0, some of the sidelobes with a gain higher than 0 dBi are pointing toward the ground and thus are not susceptible to interference. In practice, this effect is reduced by the fact that radio astronomy antennas rarely point below ~7°, and it is neglected in the present approximate analysis.