TY - GEN
T1 - Estimation of polarization effects on sky visibilities for FARSIDE
AU - Mahesh, Nivedita
AU - Gehlot, Bharat
AU - Bowman, Judd
AU - Jacobs, Daniel
N1 - Funding Information:
This work is directly supported by the NASA Solar System Exploration Research Virtual Institute cooperative agreement number 80ARC017M0006. N.M. was supported by the Future Investigators in NASA Earth and Space Science and Technology (FINESST) cooperative agreement 80NSSC19K1413.
Publisher Copyright:
© 2022 URSI.
PY - 2022
Y1 - 2022
N2 - The Farside Array for Radio Science Investigations of the Dark ages and Exoplanets (FARSIDE) is a NASA funded probe-class mission concept to place a radio array (100 kHz-40 MHz) on the far side of the Moon. The nominal array design consists of 128 non co-spatial orthogonal pairs of antenna and receiver nodes distributed over a 10 km×10 km area in a four arm spiral configuration. In this work we quantify the polarization leakages, due to dipole offsets, in terms of the stokes I, Q, U, and V beams as a function of sky position. We find that the offset leads to additional mixing and leakages of all Stokes components of the sky into the U and V polarizations of the instrument. We develop a custom interferometer pipeline for FARSIDE incorporating the co-spatial and non co-spatial Stokes beams and the uv-coverage of the array. We calculate the sky visibilities and produce the dirty images of point sources of the GLEAM catalog. Using the results, we estimate the effects of spatially non co-located antennas on the imaging performance of the array.
AB - The Farside Array for Radio Science Investigations of the Dark ages and Exoplanets (FARSIDE) is a NASA funded probe-class mission concept to place a radio array (100 kHz-40 MHz) on the far side of the Moon. The nominal array design consists of 128 non co-spatial orthogonal pairs of antenna and receiver nodes distributed over a 10 km×10 km area in a four arm spiral configuration. In this work we quantify the polarization leakages, due to dipole offsets, in terms of the stokes I, Q, U, and V beams as a function of sky position. We find that the offset leads to additional mixing and leakages of all Stokes components of the sky into the U and V polarizations of the instrument. We develop a custom interferometer pipeline for FARSIDE incorporating the co-spatial and non co-spatial Stokes beams and the uv-coverage of the array. We calculate the sky visibilities and produce the dirty images of point sources of the GLEAM catalog. Using the results, we estimate the effects of spatially non co-located antennas on the imaging performance of the array.
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U2 - 10.23919/AT-AP-RASC54737.2022.9814437
DO - 10.23919/AT-AP-RASC54737.2022.9814437
M3 - Conference contribution
AN - SCOPUS:85134877240
T3 - 2022 3rd URSI Atlantic and Asia Pacific Radio Science Meeting, AT-AP-RASC 2022
BT - 2022 3rd URSI Atlantic and Asia Pacific Radio Science Meeting, AT-AP-RASC 2022
PB - Institute of Electrical and Electronics Engineers Inc.
T2 - 3rd URSI Atlantic and Asia Pacific Radio Science Meeting, AT-AP-RASC 2022
Y2 - 30 May 2022 through 4 June 2022
ER -