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Design of (2+1+2)D FFT for Interferometric Pulsar Survey

Published online by Cambridge University Press:  12 April 2016

T. Daishido ,
N. Tanaka ,
S. Sudo ,
M. Suzuki ,
Y. Saito ,
R. Agehama ,
M. Adachi  and
N. Watanabe
T. Daishido
Affiliation:
Astrophysics Group, School of Education, Waseda University, Shinjuku-ku, Tokyo 169-50, Japan
N. Tanaka
Affiliation:
Astrophysics Group, School of Education, Waseda University, Shinjuku-ku, Tokyo 169-50, Japan
S. Sudo
Affiliation:
Astrophysics Group, School of Education, Waseda University, Shinjuku-ku, Tokyo 169-50, Japan
M. Suzuki
Affiliation:
Astrophysics Group, School of Education, Waseda University, Shinjuku-ku, Tokyo 169-50, Japan
Y. Saito
Affiliation:
Astrophysics Group, School of Education, Waseda University, Shinjuku-ku, Tokyo 169-50, Japan
R. Agehama
Affiliation:
Astrophysics Group, School of Education, Waseda University, Shinjuku-ku, Tokyo 169-50, Japan
M. Adachi
Affiliation:
Astrophysics Group, School of Education, Waseda University, Shinjuku-ku, Tokyo 169-50, Japan
N. Watanabe
Affiliation:
Astrophysics Group, School of Education, Waseda University, Shinjuku-ku, Tokyo 169-50, Japan

Abstract

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The Following design of a Pulsar Survey System with a Huge Interferometric Array is discussed. (1) A Huge Array of 320m × 320m with 256(= 16 × 16) spherical dishes of 20m in diameter, (2) RF is 1.4 GHz, (3) Receivers are frequency modified GPS(1.57542, 1.2276GHz) ones, (4) Phase and Delay Tracking, (5) Phase Calibration using Differential GPS(GPS signal × 2 → CW), (6) (2+1+2)D FFT /256 pixel Imaging + 256 ch Filtering + Dispersion Removal and Period finding(17M point floating 2DFFT by DSP), (8) Observing time required for the same sensitivity to Arecibo τ/τA: 0.88(Timing), 0.003(Survey).

Type
Part 1 The Pulsar Population
Information
International Astronomical Union Colloquium , Volume 160: Pulsars: Problems and Progress , 1996 , pp. 19 - 20
Copyright
Copyright © Astronomical Society of the Pacific 1996

References

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