ITU-R REPORT RA 2188-2010 Power flux-density and e i r p levels potentially damaging to radio astronomy receivers《功率通量密度和等效全向辐射功率(e i r p )等级对无线电天文接收器的潜在危害》.pdf

《ITU-R REPORT RA 2188-2010 Power flux-density and e i r p levels potentially damaging to radio astronomy receivers《功率通量密度和等效全向辐射功率(e i r p )等级对无线电天文接收器的潜在危害》.pdf》由会员分享，可在线阅读，更多相关《ITU-R REPORT RA 2188-2010 Power flux-density and e i r p levels potentially damaging to radio astronomy receivers《功率通量密度和等效全向辐射功率(e i r p )等级对无线电天文接收器的潜在危害》.pdf（8页珍藏版）》请在麦多课文档分享上搜索。

1、 Report ITU-R RA.2188(10/2010)Power flux-density and e.i.r.p.levels potentially damaging toradio astronomy receiversRA SeriesRadio astronomyii Rep. ITU-R RA.2188 Foreword The role of the Radiocommunication Sector is to ensure the rational, equitable, efficient and economical use of the radio-frequen

2、cy spectrum by all radiocommunication services, including satellite services, and carry out studies without limit of frequency range on the basis of which Recommendations are adopted. The regulatory and policy functions of the Radiocommunication Sector are performed by World and Regional Radiocommun

3、ication Conferences and Radiocommunication Assemblies supported by Study Groups. Policy on Intellectual Property Right (IPR) ITU-R policy on IPR is described in the Common Patent Policy for ITU-T/ITU-R/ISO/IEC referenced in Annex 1 of Resolution ITU-R 1. Forms to be used for the submission of patent

4、 statements and licensing declarations by patent holders are available from http:/www.itu.int/ITU-R/go/patents/en where the Guidelines for Implementation of the Common Patent Policy for ITU-T/ITU-R/ISO/IEC and the ITU-R patent information database can also be found. Series of ITU-R Reports (Also ava

5、ilable online at http:/www.itu.int/publ/R-REP/en) Series Title BO Satellite delivery BR Recording for production, archival and play-out; film for television BS Broadcasting service (sound) BT Broadcasting service (television) F Fixed service M Mobile, radiodetermination, amateur and related satellit

6、e services P Radiowave propagation RA Radio astronomy RS Remote sensing systems S Fixed-satellite service SA Space applications and meteorology SF Frequency sharing and coordination between fixed-satellite and fixed service systems SM Spectrum management Note: This ITU-R Report was approved in Engli

7、sh by the Study Group under the procedure detailed in Resolution ITU-R 1. Electronic Publication Geneva, 2010 ITU 2010 All rights reserved. No part of this publication may be reproduced, by any means whatsoever, without written permission of ITU. Rep. ITU-R RA.2188 1 REPORT ITU-R RA.2188 Power flux-

8、density and e.i.r.p. levels potentially damaging to radio astronomy receivers (Question ITU-R 145/7) (2010) TABLE OF CONTENTS Page 1 General explanation of concerns 2 2 Conversion from empirically-determined, device-specific damaging power input levels to corresponding incident pfd and e.i.r.p. . 2

9、3 Values of the damaging input power levels Pdand corresponding incident pfd Fd. 3 A Frequencies up to 90 GHz: HFET amplifiers . 3 B Frequencies above 90 GHz: SIS mixer input stages 3 4 Summary: Threshold levels of the incident power flux-density. 4 Annex 1 Operational concerns relevant to avoidance

10、 of damage . 5 2 Rep. ITU-R RA.2188 1 General explanation of concerns Telescopes of the radio astronomy service (RAS) are designed to achieve strong isolation from ambient radiation and have been placed in remote locations whenever possible, to enable detection of cosmic phenomena wherever they may

11、occur on the sky (although typically above about 5 elevation). However, both cosmic and man-made signals which cross the main beam are received with very high gain, owing to the large apertures needed to detect weak cosmic signals. For man-made signals the combination of high receiving gain and high

12、 incident signal strength could suffice to permanently degrade the performance of a RAS receiver, or perhaps even destroy it. This Report describes the means by which the corresponding incident power flux-density (pfd) may be ascertained. The nature of the possible damage of concern to the RAS is no

13、t necessarily complete burnout of the receiver input stages. Because the RAS has large investments in antenna collecting area it is necessary to use this most efficiently, so a long-term degradation of even 10% in the noise figure of a receiver input would be sufficient to warrant replacement. Servi

14、cing of input stages is time-consuming and expensive since cycling of cryogenic systems is involved and recent RAS instruments employ arrays of antennas and/or receiving elements numbering anywhere from tens to hundreds. Receivers used by the RAS are designed to provide the lowest possible receiver

15、noise temperatures to allow study of the widest possible range of astronomical signal levels. Receiver input stages are coupled directly to the antenna outputs without input filters or other components, since even very small losses can introduce significant levels of thermal noise. The amplifiers an

16、d mixers used in the input stages for high frequency observations necessarily require components with very small physical dimensions which limit their power-handling capacity. Because the amplifier or mixer in RAS receivers is usually fed directly from the output of the antenna feed, damage can occu

17、r even if the transmitter frequency does not fall within the receiver passband. On the low-frequency side the damage is generally confined by waveguide cutoff at the throat of the horn to frequencies no less than 0.6 times the centre frequency of the feed horn. On the high side the power delivered t

18、o the receiver by a horn feed will decrease by approximately 6 dB per octave as the beamwidth of the feed decreases, and by a further factor depending on the response of the coupling circuitry from the feed to the amplifier or mixer input. This second factor will depend upon the particular design of

19、 the coupling. Two main types of low-noise input stages are presently used by the RAS, corresponding approximately to observations at frequencies below or above 90 GHz, and these are discussed separately below. The HFET low-noise transistor amplifiers which are used up to 90 GHz (and which are the o

20、nly kind used below 70 GHz) are somewhat more susceptible to damage than the superconducting SIS mixers which are mainly employed above 90 GHz. 2 Conversion from empirically-determined, device-specific damaging power input levels to corresponding incident pfd and e.i.r.p. Let Pd(W) be the empiricall

21、y-determined power level that will cause damage at the receiver input and assume that this results from a pfd Fd(W/m2) incident on an RAS antenna. If the direction of the transmitter falls on the axis of the RAS main beam and the effective collecting area of the antenna is Ae(m2), then Pd= AeFd and:

22、 Fd= Pd/ Ae(1) Rep. ITU-R RA.2188 3 Tables 1 and 2 give values of the empirically-determined Pdand derived Fdfor various frequencies with RAS antennas of circular aperture and an assumed aperture efficiency of 0.7. The sizes of RAS antennas shown are those widely used for arrays (12 and 25 m) or for

23、 large single dishes (100 m). Also given in the last column of either table is an example of the radiated e.i.r.p. which will produce the specified Fd at a distance D = 400 km corresponding to a satellite in low Earth orbit and assuming free space propagation, calculated as: e.i.r.p.d=4 D2Pd(2) 3 Va

24、lues of the damaging input power levels Pdand corresponding incident pfd FdA Frequencies up to 90 GHz: HFET amplifiers HFET amplifiers are used as low-noise input stages for frequencies up to approximately 90 GHz and the maximum safe input power levels for such devices lie in the range Pd= 5-15 mW.

25、It is difficult to give more precise figures for the maximum levels because the damage depends not only upon the characteristics of the transistors but also on the impedances presented by the circuits in which they are used. Such impedances can vary by factors of two or more over the bandwidth of an

26、 individual amplifier. The damage which has been observed during testing is believed to be largely due to voltage breakdown between the gate and the source or drain and thus should not be a function of gate width, as it would be for damage by thermal effects. However, it is expected that amplifiers

27、used at higher frequencies would be more easily damaged than those at lower frequencies. Here we use Pd= 15 mW (18 dBW) as a maximum safe input level for the frequency range 1-20 GHz, Pd= 10 mW (20 dBW) for 20-50 GHz and Pd= 5 mW (23 dBW) for 50 to 90 GHz. Table 1 gives derived values of the corresp

28、onding incident power flux-density Fdfor frequencies up to 90 GHz. B Frequencies above 90 GHz: SIS mixer input stages In RAS receivers for frequencies greater than about 90 GHz, SIS mixers are almost universally used. Unlike HFET transistor amplifiers, SIS mixers are not available commercially and a

29、re produced in small quantities to the specifications of individual observatories. As a result, the characteristics of SIS mixers in use in radio astronomy, including the damage levels, vary more widely than those for HFETs. Damage levels for SIS mixers result mainly from thermal effects, and are in

30、versely proportional to the total junction area within the mixer and the thermal resistance for the transmission of heat generated within the junction to the outside. Tests made on two niobium SIS junctions have been used to estimate the corresponding levels for other junctions from calculations of

31、the thermal resistance. Table 2 shows the damaging input power levels for a number of SIS mixers currently in use at several observatories. A single SIS mixer can consist of up to six junctions in series, and in sideband-separating mixers the input signal is divided between two mixer elements. There

32、fore Table 2 shows the area for each junction and the number of junctions within the mixer, which are the quantities from which the damage power is calculated. The diameter of the antennas used at the particular observatories is also shown, and from this the corresponding potentially-damaging incide

33、nt pfd levels Fdat the antennas have been determined using equation (1). As in Table 1, these pfd levels and equation (2) are used to calculate the corresponding e.i.r.p. at a separation distance of 400 km assuming free-space propagation. 4 Rep. ITU-R RA.2188 4 Summary: Threshold levels of the incid

34、ent power flux-density The entries in Tables 1 and 2 show that incident pfd above 60 dB(W/m2) are potentially damaging at frequencies up to 90 GHz, while incident power flux-densities above 45 dB(W/m2) are potentially damaging at frequencies above 90 GHz. Threshold power levels are lower at the high

35、er frequencies in part due to the use of smaller antennas and in part because the SiS receivers used at higher frequencies are expected to be more robust. Note that, to order of magnitude, the input power levels capable of damaging radio astronomy receivers correspond to a voltage drop of approximat

36、ely 1 V across 50 , i.e. 20 mW. TABLE 1 Representative antenna diameters and values of Fd, the potentially damaging pfd for HFET input stages from 1-90 GHz Frequency (GHz) RA antenna diameter (m) RA antenna effective area (m2) Pd(mW) Fd(dB(W/m2) e.i.r.p.dat 400 km (dBW) 1-20 25 344 15 43 801-20 100

37、5 500 15 55 68 20-50 25 344 10 45 7820-50 100 5 500 10 57 66 50-90 25 344 5 48 7550-90 100 5 500 5 60 63 TABLE 2 Representative values of Fd, the potentially damaging pfd for SIS mixer receivers at 90-275 GHz, for representative radio astronomy sites Observatory(1)Junction area (m)2Number of junctio

38、ns Antennadiameter (m) Antenna effective area (m2) Pd(mW) Fd(dB(W/m2) e.i.r.p.dat 400 km(dBW) ALMA 3.8 8 12 79.2 55 32 91 CARMA 6 m 1.21 1 6 19.8 4 37 86 CARMA 6 m 2.24 1 6 19.8 5 36 87 CARMA 10 m 1.44 2 10 55.0 9 38 85 CARMA 10 m 3.8 4 10 55.0 27 33 90 IRAM Bure 4.0 2 15 124 14 40 83 IRAM Veleta 2.

39、25 6 30 495 32 42 81 IRAM Veleta 1.44 4 30 495 17 45 78 Kitt Peak 8.55 6 12 79.2 62 31 92 Onsala 4.01 2 20.1 222 14 42 81 (1)Observatory locations are: ALMA, Atacama desert, Chile; CARMA, Cedar Flat, California, United States of America; IRAM, Plateau de Bure, France and Pico Veleta, Spain; Kitt Pea

40、k, Arizona, United States of America; Onsala, Sweden. For more information on these and other radiotelescope sites(http:/www.iucaf.org or http:/ Rep. ITU-R RA.2188 5 Annex 1 Operational concerns relevant to avoidance of damage RAS operators will always program or otherwise protect their instruments

41、so as to avoid possibly-damaging situations, if they are aware that such situations could occur. The need to protect an instrument may influence its basic design as well as its future operations. To prevent damage to an RAS receiver it is necessary to avoid any situation in which the RAS antenna poi

42、nts toward a transmitter that is producing a pfd at the RAS antenna equal to, or greater than, the corresponding value of Fdin Tables 1 and 2. In practice this requires either that the transmitting service avoids pointing the transmitting antenna in a direction such that an RAS observatory falls wit

43、hin its main beam, or that the RAS operator avoids pointing near the transmitter. In general the latter option is possible if the RAS operator is given forewarning of any such event, including the location and operational properties of the transmitter. Approximate beamwidths for antennas in Tables 1

44、 and 2 are shown in Table 3. These range from just under one degree down to one quarter of an arcminute, so the probability of a main-beam encounter by chance is not large. However, in the case of a large antenna array such as ALMA which contains approximately 60 dual-polarization receivers, the dam

45、age resulting from a main beam encounter could be very costly. The Cloudsat cloud profiling radar of the Earth exploration-satellite service (EESS), operating in a shared RAS-EESS band at 94-94.1 GHz in accordance with RR Nos. 5.562 and 5.562A and described in Annex 2 of Recommendation ITU-R RA.1750

46、, provides an example of potentially_damaging transmissions whose effect upon RAS receivers has been successfully mitigated by ongoing provision of orbital elements and exchange of other information between the RAS and the EESS. The peak transmitter power is 1 kW, the peak transmitting antenna gain

47、is 63 dBi, and the orbital height is 705 km, resulting in a peak pfd of 35 dB(W/m2), 10 dB above the threshold levels of the incident pfd given in Table 2. For Cloudsat the transmitting antenna points toward the nadir, so main-beam to main-beam coupling may occur only if the RAS antenna is pointing

48、toward the zenith, which simplifies the avoidance problem. However, implementations of similarly high-powered 94 GHz radar are presently being flown on aircraft and driven on trucks in the vicinity of several mm-wave telescopes. Other high power satellite radars, in operation or proposed, include sy

49、nthetic aperture radars (SARs) in the EESS near 5 GHz and 9.6 GHz such as RISAT and TerraSar-X. For these, the orientation of the transmitting antenna beam can fall within a large range of angle with respect to the nadir, greatly complicating the problem of avoidance on the part of the RAS operator. 6 Rep. ITU-R RA.2188 TABLE 3 Approximate half power beamwidths for some frequencies and antenna diameters used in Tables 1 and 2 Frequency (GHz) RAS antenna diameter (m) Half-power beamwidth (arcmin) 1 25 50100 12 10 25 5 100 1.250 12 2.1 25