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A 324-Element Vivaldi Antenna Array for Radio Astronomy Instrumentation

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A 324-Element Vivaldi Antenna Array for Radio Astronomy Instrumentation IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT, VOL. 61, NO. 1, JANUARY 2012 241 A 324-Element Vivaldi Antenna Array for Radio Astronomy Instrumentation Edwin Walter Reid, Laura Ortiz-Balbuena, Aliakbar Ghadiri, Student Member, IEEE,and Kambiz Moez, Member, IEEE Abstract—This paper presents a 324-element 2-D broadside the laws of sampling theory over the entire bandwidth. Hence, array for radio astronomy instrumentation which is sensitive to the array elements must be spaced close enough (less than one two mutually orthogonal polarizations. The array is composed of wavelength (λ) apart at the shortest wavelength in the receiving cruciform units consisting of a group of four Vivaldi antennas arranged in a cross-shaped structure. The Vivaldi antenna used band) to avoid undersampling. Undersampling manifests itself in this array exhibits a radiation intensity characteristic with a as the appearance of grating lobes in addition to the main lobe. symmetrical main beam of 87.5◦ at 3 GHz and 44.2◦ at 6 GHz. The On the other hand, placing the array elements very close to measured maximum side/backlobe level is 10.3 dB below the main each other causes distortion in the received signal because of beam level. The array can operate at a high frequency of 5.4 GHz the mutual coupling of the neighboring array elements [7]. without the formation of grating lobes. One way of reducing the mutual coupling is to use a large Index Terms—Radio astronomy instrumentation, ultra- number of low-gain small array elements instead of a few large wideband (UWB) antenna, Vivaldi antenna. elements as they exhibit less mutual coupling with each other because of their smaller physical area of influence. Also, the I. INTRODUCTION placement of elements over a ground plane tends to reduce the coupling even further because of the canceling effect of the out- BSERVATIONAL radio astronomy is concerned with of-phase images. A conservative approach is to limit the longest the measurement of electromagnetic radiation emitted by O wavelength of the received signal to λ/2 so that the effect cosmic radio sources, where the radiation is a rapidly and irreg- of interelement coupling is small. There are many references ularly varying function of time. During the past decade, plans supporting the claim that Vivaldi antenna elements can be for significantly improving the observing capability in radio spaced more closely than λ/2 apart without suffering excessive astronomy at meter and centimeter wavelengths have received mutual coupling at the longest wavelength in the band [8]–[13]. increasingly prominent consideration [1]–[4]. This results from This paper is organized as follows. In Section II, we present the need for superior sensitivity and high survey speed, required the theory on radiation from Vivaldi antennas and provide for the study of many astronomical and cosmological phenom- a closed-form method for computing its radiation pattern. ena [5]. The instrument used for the measurement of the cosmic Section III explains the details on the construction of the an- radio waves consists of three basic components operating in tenna. In Section IV, we describe the design of the experimental tandem: a receiving antenna, a sensitive receiver, and a data array using modular cruciform units and address the interele- recorder. The antenna–receiver combination, called a radio ment coupling effects. Finally, in Section V, the simulation and telescope, acts like a bolometer in which the antenna’s radiation measurement results of one Vivaldi antenna element and the resistance measures the equivalent temperature of distant parts entire array are presented. of the space. This antenna is a critical element in building a sen- sitive radio astronomy instrument. The objective of this paper is to develop a highly sensitive phased array antenna that is to be II. VIVALDI ANTENNA used as the feed system for the large adaptive reflector (LAR) radio telescopes [6]. The phased array can be viewed as a way The Vivaldi antenna has been utilized in many radio fre- of discretely sampling an aperture, and it must therefore obey quency (RF) applications such as radio astronomy, ground pen- etrating radar, ultra-wideband (UWB) communication systems, and UWB imaging system because of its simple structure, light Manuscript received February 10, 2011; revised May 3, 2011; accepted May 5, 2011. Date of publication August 4, 2011; date of current version weight, wideband characteristics, low cross polarization, and December 8, 2011. This work was supported by the Natural Sciences and highly directive patterns [14]–[17]. The Vivaldi antenna con- Engineering Research Council of Canada. The Associate Editor coordinating sists of an exponentially tapered slot cut in a metal film (with or the review process for this paper was Dr. Matteo Pastorino. E. W. Reid is with Radio Frequency Works, St. Albert, AB T8N 7J1, Canada. without a thin substrate) on one side of the material. The narrow L. Ortiz-Balbuena is with the Universidad Autonoma Metropolitana, Mexico slot toward one end is coupled to a transmission line, usually City D.F. C.P. 09340, Mexico. A. Ghadiri and K. Moez are with the Department of Electrical and Computer using a balun. Away from this region, the slot is exponentially Engineering, University of Alberta, Edmonton, AB 26G 2V4, Canada (e-mail: tapered, and a travelling wave, propagating along the slot, [email protected]; [email protected]). radiates in the end-fire direction. Vivaldi antennas are two to Color versions of one or more of the figures in this paper are available online at http://ieeexplore.ieee.org. six wavelengths in length, and therefore, they have a very wide Digital Object Identifier 10.1109/TIM.2011.2159414 pattern bandwidth and high directivity with low sidelobes and 0018-9456/$26.00 © 2011 IEEE 242 IEEE TRANSACTIONS ON INSTRUMENTATION AND MEASUREMENT, VOL. 61, NO. 1, JANUARY 2012 on a conducting half-plane is given by [19] G(θ, φ; x, z)=| sin φ|ejπ/4F (v)ejβ0(x sin θ cos φ+z cos θ) φ −jβ0(x sin θ−z cos θ) sin 2 e + e−jπ/4 √ (5) πk0x sin θ where F (ν) is the complex Fresnel integral [20], β0 is the freespace wavenumber, and v = β0x sin θ(1 + cos φ).Thera- diation pattern for the ith section of the stepped slot-line approximation is expressed as i i Eθ(θ, φ)= G(θ, φ; x, z)EAP (x, z) dxdz. (6) Section i By adding up the contributions from all sections of the slot- line, we obtain N i Eθ(θ, φ)= Eθ(θ, φ). (7) Fig. 1. Stepped approximation of a Vivaldi antenna. i=1 can be designed to produce an axis-symmetrical main beam [8]. The E-plane radiation pattern was extracted by specializing They are well suited for microwave frequencies (above 1 GHz) the Green’s function at φ = π. Therefore for which a long electrical length yields a practical geometric e−jπ/4 β W i cos θ 2 length, and they can potentially have low dissipative losses. In Ei (θ, π)= Zi J 0 θ β g 0 2 sin θ this section, we develop a theoretical model for the radiation 0 characteristic of a general tapered slot antenna. The theoretical ∗ i − ∗ i i − i − i F uh F ul i F u¯h F u¯l model provides insight on the radiation mechanism of Vivaldi × e jβ0c L √ +Γ ejβ0c L √ ci−sin θ ci +sinθ antenna and a method to compute its pattern. A Vivaldi antenna can be constructed from a cascade of interconnected slot-line (8) segments i =(1, 2, 3,...) centered along the x-axis with gap where ui = β (ci − sin θ)xi, u¯i = β (ci +sinθ)xi, ui = width W i corresponding to the segment i, shown in Fig. 1. The l 0 l l 0 l h β (ci − sin θ)xi , u¯i = β (ci +sinθ)xi , ci = λ /λi , and Γ is model is based on Itoh’s analysis [18]. The transversal aperture 0 h h 0 h 0 g field within the slot-line Ei (x, z) is given by the reflection coefficient due to a backward travelling wave on A the aperture. Now, the H-plane radiation pattern is obtained by i − Ei (x, z)=a ejβg (x L) f (z) (1) specializing the Green’s function at θ = π/2. Thus A 1 1 π i i i Ei ,φ where βg =2π/λg, λg is the guide wavelength of the slot-line θ 2 at segment i, and −jπ/4 e − i = e jβ0c L Zi β g 2 1 0 f1(z)= . (2) i 2 | | πW − 2z sin φ i jvi i jvi 1 W i × · F p e h − F p e l (ci +cosφ) h l In the derivation of the E- and H-plane radiation patterns, ˜ | sin φ| 1 + cos φ ∗ ∗ the Fourier transform of f1(z), denoted as f1(α), is required, − · F qi − F qi i i − h l which is (c +cosφ) (c 1) i φ 2 ∗ ∗ ˜ αW +sin F qi − F qi f1(α)=J0 (3) i − h l 2 2 c 1 −jπ/4 e i where α is the transform variable and J (αW i/2) is the Bessel +Γ ejβ0c L Zi 0 β g function of the first kind of zero order. Enforcing the conser- 0 vation of energy principle for power flowing along the entire | sin φ| − i − i × · i jv¯h − i jv¯l F ph e F pl e i (ci − cos φ) tapered slot-line results in a1 = Zg. Therefore i | | i − αW sin φ 1 + cos φ i i E˜i (x, α)=ejβg (x L) Zi J .
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