Noto User Manual THE RADIOTELESCOPE
Contents
1. PRIMARY FOCUS CASSEGRAIN FDCUS CONTROL ROOM Fig 4 2 Signal distribution between the foci 24 4 3 Control Room The backend systems are installed in the control room located at the antenna s base It is connected to the foci through the links shown in the following red line and green line are fiber optic links PRIMARY FOCUS ROSSO F O PUNTO PUNTO BLU DOPPINO TWISTED PAIR VERDE LAN FO CASSEGRAIN FOCUS CONTROL ROOM Fig 4 3 Control links From the control room receivers antenna and sub reflector movement can be controlled Moreover the new metrology system temperature sensors and a little antenna used for the olographic measurement of the surface can be operated 25 5 Efficiency and System Temperature The antenna gain is defined as G 1075 14 B k Jy B m 0 5 non polarized radiation Ag geometric area B Boltzmann s constant Na antenna efficiency For the Noto antenna the constants are 1075 s 9 292 DK B nais the overall efficiency estimated assembling all the signal degradation factors The antenna gain varies according to the elevation and it reaches a maximum at 45 A good interpolation is obtained with a second degree polynomial such as ax bx c The coefficients of the normalized polynomials at each frequency are listed in the following Fre n oo c 0 327 0 0 1 0 5 1 0 0 1 1 6 6 8310687 10 7 285044 10 8 0577027 12. 43 GHZ 3x12 A ne ee Pen ee Ga he Sands dae SY nad AR eas Re 22 A 2 DIStFIDUTIOMNS a Em 23 4 3 Control oOIms ie a as 24 5 EFFICIENCY AND SYSTEM TEMPERATURE sesssese mmm emen 25 Em 48 1 EE 27 7 OBSERVING MODEG cccccceceeece eens eee nun Hann nun nn nen nun nun nn nn nun neuen sean rna nnn 29 7 1 ON OFF techniq es oie ere a a REND e UA be 29 7 2 Mapping techniques rv cease ia 29 8 BACK END oet tas codon deed OA A RO Rt a eR E UR EUR YR ee RV ERRARE eR TRA a 33 8 1 SpectrolTie ters uoce ere RR EE a MEC ERO 34 Gl T AECOS reseaux ot GER x MR ER UD RACER URN ae MoE ewes cua Bence ane eae Races A CRUS 34 8 2 CONTINUUM Ai RER Oa ERA DIO ee NOD A AR EDDA ELDER TS 35 iv TS Mark AVERTI 35 SiS NEBL ich nr 37 8 3 1 MA eee CU ATE RR 37 1 Introduction The Noto 32 m antenna is a Cassegrain radiotelescope operated since 1989 by the Istituto di Radioastronomia until 2004 part of the CNR Consiglio Nazionale delle Ricerche and now part of the INAF Istituto Nazionale di AstroFisica Fig 1 1 The Noto antenna The main features of this instrument are the following e Active surface e Secondary reflector wobbling shifting time x 1 sec at v 20 GHz e Complete automation and remote control of the observing settings Position Noto Italy Coordinates Lat 36 52 33 78 N Long 14 59 20 51 E Alt 30 m f s l Optics Cassegrain Frequency coverage 1 4 86 GHz Primary r
3. central frequency user defined maximum total bandwidth 400 MHz IF DISTRIBUTOR 3 500 900 100 500 IF DISTRIBUTOR 1 amp 2 14 VIDEOCONVERTER Attenuators 1002 900 100 220 sae 220 500 100 900 100 220 9 100 500 220 500 28x16 MHz TOTAL POWER DETECTOR A D 16 bit Fig 8 2 Maximum bandwidths MHz processed by the Mark IV example at 22 GHz 0 125 MHz and 1 MHz band are available only with external filters please ask if available at the site B Processing of the whole input 2x400 MHz centered at 300 MHz and 1x400 MHz centered at 700 MHz 36 IF DISTRIBUTOR 3 500 900 100 500 14 VIDEOCONVERTER IF DISTRIBUTOR 1 amp 2 mT 4 T b b LI LI LJ LI LI b b LI LJ LJ iE LR a OS o www eee eee Attenuators 100 500 100 500 100 900 a 5 m E m ea c Im o a zi XL ke o E PC A D 16 bit Fig 8 3 Maximum total bandwidths MHz example at 22 GHz At 1 4 1 6 2 3 GHz effective bandwidths may be considered smaller because of RFI 37 8 3 VLBI 8 3 1 Mark V The VLBI observations are handled with the Mark IV base conversion bands splitting A D conversion and the Mark V data storage terminals The Mark V is made of 2 blocks of 8x400 Gbyte hard disks
4. IF standard band inside the RF band of Av the LO frequency must be changed within the range listed in the table according to the following 42 5 Av 10 5 0 271 oL 2 v 23 4 2 Distribution The connections between the radiotelescope foci involve three different kinds of signal Local Oscillator in order to cut down the expenses related to the construction of a high number of independent superheterodyne receivers a common solution is to share some local oscillators at least for one conversion A single local oscillator therefore can serve more receivers through a signal distribution system IF the RF signals once received and converted by the Front End are sent to the Back End installed in the Control Room at the antenna base Reference 5 MHz H maser signal necessary for the local oscillator stability All the signals are distributed via coaxial cable The distribution scheme is simplified by the fact that there are only two double conversion receivers 6 GHz at the Cassegrain focus and 22 GHz at the primary focus Both use the same local oscillator for the second conversion Besides the two receiver channels cannot be tuned at different positions inside the RF bandwidth The LO signal is distributed by an LO distributor OLD The reference distributor REFD and the IF distributor IFD are also installed in the Cassegrain focus The receiver can be chosen from the Control Room using the selector
5. Noise temperature K 120 Useful RF band GHz 1 40 1 72 RF filter width MHz 320 IF filter width MHz 35 Instantaneous RF band GHz 1 366 1 446 LO frequency GHz 1 279 LO range GHz 1 020 1 305 Single USB Conversion GHz a Standard parameters of the 1 5 GHz parameters The maximum bandwidth is 80 MHz tunable only within the two RF ranges listed in the above table To shift the IF standard band inside the RF band of Av the LO frequency must be changed within the range listed in the table according to the following RF 1 4 41 72 gt vg 1 2719 1 Av 19 2 3 8 3 GHz Type Hot Coaxial Channels 2 Polarization LHC RHC LHC RHC Central frequency GHz 2 28 8 58 Noise temperature 120 110 Useful RF band GHz 2 20 2 36 8 18 8 58 RF filter width MHz 160 400 IF filter width MHz 160 400 Instantaneous RF band GHz 2 20 2 36 8 18 8 58 LO frequency GHz 2 020 8 080 LO range GHz 0 0 Single USB Single USB Conversion GHz 0 18 0 34 0 1 0 5 Standard parameters of the 2 3 8 3 GHz coaxial receiver It is possible to use the receivers both together coaxial 2 IF outputs one per each frequency and separately 2 IF outputs For the VLBI coaxial observation one channel only for each receiver is used typically the right hand circular polarized one this because the Mark IV can handle only 2 IF inputs 20 5 GHz Type Cooled Channels 2 Polarization LHC RHC Central frequency GHz 4 875 Noise temperature 30
6. Useful RF band GHz 4 65 5 15 RF filter width MHz 500 IF filter width MHz 350 Instantaneous RF band GHz 4 700 5 050 LO frequency GHz 1 150x4 LO range GHz 1 138 1 175 Conversion GHz A RAD Standard parameters of the 5 GHz receiver To shift the IF standard band inside the RF band of Av the LO frequency must be changed within the range listed in the table according to the following 4 600 Av OL 4 21 22 GHz Type Cooled Channels 2 Polarization LHC RHC Central frequency GHz 22 150 Noise temperature K 90 Useful RF band GHz 21 90 22 40 RF filter width MHz 500 IF filter width MHz 400 Instantaneous RF band GHz 21 95 22 35 LO1 frequency GHz 1 150 x18 LO2 frequency GHz 1 150 LO1 range GHz 20 668 20 778 Double USB Conversion GHz 1 147 1 153 0 1 0 5 Standard parameters of the 22 GHz receiver To shift the IF standard band inside the RF band of Av the LO frequency must be changed within the range listed in the table according to the following 22 15 Av 0 3 Ma 19 22 43 GHz Type Cooled Channels 2 Polarization LHC RHC Central frequency GHz 42 5 Noise temperature K 40 Useful RF band GHz 37 48 RF filter width MHz 11000 IF filter width MHz 400 Instantaneous RF band GHz 42 3 42 7 LO1 frequency GHz 15 86 LO1 range GHz 13 21 18 51 LO2 frequency GHz 10 500 Double USB Conversion 10 5 11 5 0 1 0 5 Standard parameters of the 43 GHz receiver To shift the
7. correlator 28 29 7 Observing Modes 7 1 ON OFF Techniques In order to reduce as much as possible the atmospheric contribution during an observation it is possible to apply some techniques based on at least a couple of exposures one on source and one on an adjacent area OFF source reference position sufficiently free from emission At high frequencies short scale and strong atmospheric fluctuations affect the observation hence the need of quick antenna shifts between the two positions which have to be reasonably close to each other or the usage of other techniques which do not involve the movement of the entire structure The Noto antenna offers the following ON OFF techniques Position Switching The antenna shifts between two different positions The time needed to cover some beams is nearly 5 seconds at all frequencies Wobbling The shifting of the beam is obtained moving the secondary mirror only This technique requires always a shorter time than the Position Switching In both cases the algorithm used is of the type ON OFF ON OFF 7 2 Mapping Techniques If the radio emission is extended over an area larger than the antenna beam several pointings might be necessary in order to cover the entire area of interest The Nyquist theorem states that the correct source sampling along a direction requires an angular distance between the pointings of iga 2D The Nyquist sampling is commonly expressed
8. 0 2 3 5 8197959 10 9 4270958 10 6 1824204 10 5 1 4396956 10 1 9594323 10 9 3333009 10 8 3 6 2013643 10 6 9932510 10 8 0284355 10 12 1 1407653 10 1 1413276 107 7 1452747 10 22 2 0746800 10 1 7584500 10 2 0928100 107 Tab 5 1 Normalized gain curves coefficients 26 The sensitivity can be estimated as follows aT ys AS GyAvt nN a receiver constant 1 Tsys system temperature G gain K Jy Av bandwidth T integration time n integration number Nr available channels 1 2 In the following table the system temperatures and the sensitivities of the Medicina antenna are listed Vo T receive Tsys Ma G SEFD Bandwidth AS GHz K K 969 K Jy Jy MHz Guiya 0 327 150 170 34 0 1 1700 2x15 310 0 5 1 E y 34 0 1 16 120 130 41 0 12 1083 2x35 129 2 3 120 140 58 0 17 823 2x160 46 5 30 48 51 0 15 320 2x350 12 8 3 110 130 51 0 15 867 2x400 31 12 2x1050 22 90 110 44 0 13 846 2x400 30 43 70 80 28 01 800 2x400 21 Tab 5 2 Sensitivity of the antenna assuming T 1 sec n 1 N 2 Primary Focus Cassegrain Focus Usually at these frequencies a narrower bandwidth is used because of RFI 27 6 VLBI Regarding the VLBI observations the Noto antenna is part of the EVN European VLBI Network since 1984 Some observations have been conducted using only the two Italian antennas Noto and Medicina and the Bonn
9. Noto User Manual 32 m Antenna Version 1 Elena Cenacchi Alessandro Orfei Francesco Schillir Karl Heinz Mack e cenacchi ira inaf it THE RADIOTELESCOPE Last update 11 September 2006 Index 1 INTRODUCTION 82 2 nen 5 2 ANTENNA STRUCTURE sssssssssesseenn nennen menn nnns amena annnm 7 2 3 Primary reflectors o rere y a Ep vn ii ei nenn 7 2 2 Quadrupod and secondary reflector sess emen 8 DL WODDIIAG A en ee RE da 9 2 3 Polnting ertOrS cocer e ex ex a ner ini 10 2 4 Specification summary rdece maianen ndina aae nennen nena sena sean ESSERE anna sean 11 2 4 1 Observation conditions seenenunenunnnennnenne nen nnennnnnnnnnnnn nhe nnn nennen nnn 11 2 4 2 Surface acctFacy xus ere veu A er S D e eR E 11 243 PONING CFI ONS PARERE 12 cu olguie ome c EL aan real 13 Sel Primary TOCUS ceci pesa ui fece Frutex EET ortu eas FRE een lene Fa dA Due Sx Era o al exe Ta Tie Pa erre 13 3 2 Cassegrain fOCUS ie e ea t enixe e e Oa care EE NA a ada ERI EAE LR amen RE 14 3 3 Servosystems specifications srs eea ie ainda a nennen nnne 15 4 FRONT END 2 2 2 ent cv ce a ee x YA nn a RUE 17 4 1 Feeds nd receivers ree En RI GA GO PE RR ER 17 DOS GAZ vein one 18 2 3 8 3 GAZE ais ee aba u Exe as eva edad cain de ERE SEX EAR EVER ola ea de eed vee debian eee EVA 19 Lac La P 20 22 GAZ i sieve En ovals NEE bah corset EEE ie 21
10. a hyperbolic reflector 3 2 m diameter made of a single aluminium panel rms 0 35 mm On the backup structure 3 mechanical actuators are installed and allow the mirror to tilt around the 3 axes In addition the whole system can translate along the x and y axis 1 Gmsaora 2 Tecno a conto 3 Tara husana 4 Scamnsrroae 5 Ammon Z Fig 2 4 Hyperbolic mirror The mirror must completely be retracted along the y axis when the primary focus is used E H seria au re Fig 2 5 Configuration for Cassegrain focus usage plain line and primary focus usage dotted line The mirror and the quadrupod induce an obstruction on the primary reflector of nearly 4 Sub reflector 2 Quadrupod 2 Total 4 Cause Obstruction Tab 2 2 Primary reflector obstruction 2 2 1 Wobbling The system that rotates the secondary mirror has been optimized in order to enhance the number of receivers that can be installed at the Cassegrain focus but actually it is used only to realize the Wobbling technique using one receiver at once Typical shifting times shorter then those used in Position Switching are listed in the following table Mirror rotation Mirror rotation Frequency Beam HPBW Required time Required time GHz a sec 3 n sec 5 450 2 56 1 16 5 12 2 12 6 390 2 22 1 03 4 44 1 86 22 120 0 68 0 45 1 37 0 71 Tab 2 3 Wobbling time for 2 5 beam and 5 beam throws 2 3 Po
11. ar travel mm 420 Kinematics Linear velocity mm sec 7 2 Linear acceleration mm sec 24 Tab 3 3 Primary focus feed positioner transverse axis Primary focus feed positioner z axis Unity Value Linear travel mm 350 Kinematics Linear velocity mm sec 7 2 Linear acceleration mm sec 24 Tab 3 4 Primary focus feed positioner z axis Sub reflector Unity Value Linear travel x axis mm 160 Linear travel y axis mm 160 Linear travel y axis out of focus mm 2240 Linear travel z axis mm 250 Angular travel x axis 9 4 2 Kinematics nm Angular travel y axis 4 2 Linear velocity x axis mm sec 55 5 Linear velocity y axis mm sec 17 1 Linear velocity z axis mm sec 48 3 Angular velocity 9 sec 1 9 Tab 3 5 Sub reflector kinematics 16 17 4 Front End 4 1 Feeds and Receivers The Noto antenna covers the range 1 35 48 GHz The following receivers are available Band Vo Channels tsy VHsky Gain inc ae Bandwidth pBW Hemt Cooled Label GHz cm GHz GHz K Jy a WU LEN E EA OE E LESA E A d E FOA TA TE Tab 4 2 Receivers parameters Primary Focus Cassegrain Focus Visky VHsky receiver maximum bandwidth The receiver labels have been assigned only for identification purpose At UHF P L S bands the effective bandwidths can be smaller due to RFI 18 1 6 GHz Type Hot Channels 2 Polarization LHC RHC Central frequency GHz 1 56
12. as fraction of the beam ag 1 x 0 43HPBW 2D 30 The Noto antenna mainly offers two mapping techniques Raster Scan The map is obtained through discrete adjacent pointings point and shoot mode At every step the antenna stops and acquires data for the exposure time required The time necessary to cover an area A considering the on source time only with a monofeed system can be roughly estimated as N HPew y N number of pointings tesp single exposure time depending on the sensitivity required The Nyquist sampling is approximated with a half beam shift in both directions vertical and horizontal Usually this mapping technique is associated with an ON OFF technique therefore the total time necessary to complete a survey is given by Crop Coy Cop E Lor N Es z t sh ON ts antenna shifting time Position Swiching or secondary mirror shifting time Wobbling The scan can be conducted in several user defined ways the most common is along two perpendicular directions cross scan On The Fly In the On The Fly mode the antenna is moved along one direction usually with a raws and columns path at constant speed The data are continously acquired and downloaded by the backend every few seconds OTF dumps corresponding to angular excursions of few arcseconds depending on the antenna speed To reach the required sensitivity it is necessary to scan the same area several tim
13. ce Accuracy Structural Elements Primary reflector panels Secondary reflector panels Gravitational deformation Total surface accuracy 0 38 RSS mm RSS mm 90 El 60 El 0 1 0 38 0 0 2 Tab 2 6 Surface accuracy at 90 and 60 elevation To estimate the phase error e from the surface accuracy the following can be used surface accuracy A observation wavelength _ 416 a rad 11 Usually a maximum tolerable phase error is assumed as e 36 0 63 rad so that the minimum observable wavelength is Ain 3 206 25 This means for the Noto antenna Ann E AMM gt v 75 GHz 2 4 3 Pointing accuracy Pointing accuracy Observation condition rms arcmin Normal Precision 0 13 Tab 2 7 Pointing accuracy 12 3 Optics The Noto antenna has 2 focal positions e Primary focus F1 e Cassegrain focus F2 6240 Fig 3 1 Optics of Noto antenna dimensions mm 3 1 Primary Focus With the Cassegrain optics the primary reflector focus is usable only if the secondary reflector is completely retracted Behind the mirror a movable positioner is installed equipped with 3 receiver bays Fig 3 2 Primary focus feed positioner 13 The primary mirrror focal length is nearly 10 3 m therefore the focal ratio is F D amp 0 32 Fig 3 3 Primary focus dimensions mm 3 2 Cassegrain Focus The secondary mirror 9 m from the primary mirror allows t
14. eflector diameter 32 m Secondary reflector diameter 3 2 m Primary f D 0 32 las Cassegrain f D 3 04 Elevation range 0 90 Azimut range 270 Slew rates wind speed lt 60 km h on an Surface accuracy rms specified 0 1 mm Pointing accuracy rms specified 8 arcsec FWHM Beamwidth 38 7 arcmin f GHz Gain 0 10 0 16 K Jy First secondary lobes circa 20 dB under the main lobe Primary Focus movable positioner 2 receiver bays Cassegrain Focus fixed 1 receiver bay Parabolic reflector correction system Active surface Look up table Tab 1 1 Characteristics of the Noto antenna Receivers mounts Fig 1 2 The Noto antenna side 2 Antenna Structure 2 1 Primary Reflector The primary reflector diameter 32 m is made of 240 aluminium panels RMS 0 4 mm substained by a backup reticular truss The housing of the Cassegrain focus feeds is at the mirror vertex Fig 2 3 Primary reflector front D2 4 he Di gt C1 D1 D2 mm mm mm Raw B 2617 8 437 62 1113 96 RawC 2604 15 1113 96 1770 4 Raw D 2617 24 887 1 1206 06 Raw E 2648 38 1206 1515 Raw F 2659 33 1515 04 1810 74 Raw G 2718 1810 74 2098 14 Tab 2 1 Geometry of the panels 2 2 Quadrupod and Secondary Reflector The primary reflector backup structure substains the secondary mirror placed at a distance of 9 m through 4x45 inclined beams quadrupod The secondary mirror is
15. es preferably along different directions The ON source time is t acquisition time Ng number of dumps depending on the required sensitivity The Nyquist sampling is obtained if the acquisition time for each dump corresponds to an angular antenna shift equal or shorter than the ideal Nyquist distance Also the distance between raws and columns must be coherent with the Nyquist sampling 3l The On The Fly technique is characterized by very short scanning times so it is the best one in order to reduce the atmospheric contribution anyway it is necessary to use an ON OFF technique For a squared spectroscopic map the total observing time can be estimated with the following Eon Coy Core torr N Eon The Noto antenna offers the On The Fly Mapping on a user defined RA Dec map with a maximum scan speed of 200 s 32 33 8 Back End The Noto antenna is equipped with the following processing systems e ARCOS Autocorrelator Input 2 Maximum bandwidth per input 16 MHz Minimum bandwidth per input 0 125 MHz Channels 2048 A D Conversion 2 bit Available software ADLB4 Tab 8 1 Can be further reduced on request e Total Power Input 3 Maximum bandwidth per input 400 MHz A D Conversion 16 bit Available software ON OFF Tab 8 2 e VLBI Mark IV Mark V Input 2 Maximum bandwidth per input 400 MHz Output 28 x0 125 16 MHz A D Conversion 1 2 bit Data transfer 1 Gbit s Hard D
16. he usage of the Cassegrain focus at nearly 20 cm above the reflector vertex This focus has been designed to offer several adjacent focal positions which can be obtained through the angular movement of the secondary mirror see fig 3 4 Fig 3 4 Cassegrain focal plane Unlike the Medicina antenna the focal positions do not host different receivers and the frequency change requires the installation of the necessary receiver into the central bay The 14 Wobbling technique is used only to realize the Beam Switching e g On Source Off Source and to carry faster radiometric measurements The secondary hyperbolic reflector yelds a magnification iz which depends on the ratio between the focal length and the distance from the prime focus nearly 9 m and 1 m respectively The total focal length can be estimated as follows 9 074 2 0 956 i F 97 36 m z 9 49 F 2 The focal ratio is therefore F2 D x 3 04 3 3 Servosystems Specifications Azimuth drive Unity Value Angular travel 9 540 Kinematics Angular velocity sec 0 8 Angular acceleration sec 0 82 Number of wheels 4 Configuration Driving wheels 2 Drives per wheel 1 Track Diameter m 18 3 Tab 3 1 Azimuth drive Elevation drive Unity Value Angular travel 90 Kinematics Angular velocity sec 0 5 Angular acceleration sec 0 31 Tab 3 2 Elevation Drive Primary focus feed positioner Unity Value Line
17. inting Errors The accuracy of the pointing correction increases with the observing frequency i e as the antenna beam width decreases Commonly the following is assumed _ HPBW d 10 Op pointing accuracy HPBW 3 dB beam width main lobe For the Noto antenna the values are listed in the following Frequency HPBW Error GHZ 0 1 5 29 lt 2 9 22 2 lt 0 2 Tab 2 4 Beam and pointing errors The systematic errors are usually quite high Some arcminute Anyway they have been determined according to the antenna position Az El after apposite astronomical observations reference radio sources and a correction model has been derived Once the model has been applied the residual error is 0 1 both in azimuth and elevation exactly as required 10 2 4 Specification Summary 2 4 1 Observation conditions Precision Normal Survival Parameters Wind continuous Wind gusts Sun Precipitation Temperature Humidity Wind continuous Wind gusts Precipitation Temperature Humidity Wind Precipitation Seismic Specifications 25 km h 20 30 km h Absent Absent 25 30 C 90 lt 65 km h 50 80 km h Absent 30 50 C lt 100 200 km h lt 5 cm h snow 0 3 g horizontal Tab 2 5 Observation conditions In survival conditions and when not in use the antenna must be settled at 90 elevation and 206 151 azimuth stow position 2 4 2 Surfa
18. isk 2 x 8 x 400 Gbyte Tab 8 3 At 1 4 1 6 2 3 GHz the effective bandwidths may be smaller because of RFI 34 8 1 Spectrometers 8 1 1 Arcos Arcos ARcetri COrrelation Spectrometer is a digital spectrometer developed by the Osservatorio di Arcetri It is connected to the Mark IV and receives 2x16 MHz input from the videoconverters of the terminal The system could handle 2x20 MHz bands anyway the Mark IV imposes 2x0 125 16 MHz bands 2 steps The main constituents are 2 correlation boards 2048 channels in total 2 A D sampler 4 channel sampler boards 2 bit 4 levels IF DISTRIBUTOR 3 500 900 100 500 IF DISTRIBUTOR 1 amp 2 14 VIDEOCONVERTER Attenuators 1002900 100 220 220 500 100 900 100 220 100 500 220 500 28x16 MHz TOTAL POWER DETECTOR A D 16 bit Fig 8 1 ARCOS correlator scheme example at 22 GHz bands in MHz 0 125 MHz and 1 MHz band are available only with external filters please ask if available at the site 35 8 2 Continuum 8 2 1 Mark IV The Total Power observations use the Mark IV terminal and the Field System software The terminal is made of two parts IF distributor receives the input from the Front End and splits them in sub bands Videoconverters 14 units that operate the base band conversion and the integration It is possible to choose between two outputs A 28 narrow bands minimum width 0 125 MHz maximum 16 MHZz
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