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26 April 2024 |
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A 189 MHz, 2400 square degree polarization survey with the Murchison Widefield Array 32-element prototype | | G. Bernardi
; L.J. Greenhill
; D.A. Mitchell
; S.M. Ord
; B.J. Hazelton
; B.M. Gaensler
; A. de Oliveira-Costa
; M.F. Morales
; R. Udaya Shankar
; R. Subrahmanyan
; R.B. Wayth
; E. Lenc
; C.L. Williams
; W. Arcus
; S.A. Balwinder
; D.G. Barnes
; J.D. Bowman
; F.H. Briggs
; J.D. Bunton
; R.J. Cappallo
; B.E. Corey
; A. Deshpande
; L. deSouza
; D. Emrich
; R. Goeke
; D. Herne
; J.N. Hewitt
; M. Johnston-Hollitt1
; D. Kaplan
; J.C. Kasper
; B.B. Kincaid
; R. Koenig
; E. Kratzenberg
; C.J. Lonsdale
; M.J. Lynch
; S.R. McWhirter
; E. Morgan
; D. Oberoi
; J. Pathikulangara
; T. Prabu
; R.A. Remillard
; A.E.E. Rogers
; A. Roshi
; J.E. Salah
; R.J. Sault
; K.S. Srivani
; J. Stevens
; S.J. Tingay
; M. Waterson11
; R.L. Webster
; A.R. Whitney
; A. Williams
; J.S.B. Wyithe
; | | Date: |
26 May 2013 | | Abstract: | We present a Stokes I, Q and U survey at 189 MHz with the Murchison Widefield
Array 32-element prototype covering 2400 square degrees. The survey has a 15.6
arcmin angular resolution and achieves a noise level of 15 mJy/beam. We
demonstrate a novel interferometric data analysis that involves calibration of
drift scan data, integration through the co-addition of warped snapshot images
and deconvolution of the point spread function through forward modeling. We
present a point source catalogue down to a flux limit of 4 Jy. We detect
polarization from only one of the sources, PMN J0351-2744, at a level of 1.8
pm 0.4%, whereas the remaining sources have a polarization fraction below 2%.
Compared to a reported average value of 7% at 1.4 GHz, the polarization
fraction of compact sources significantly decreases at low frequencies. We find
a wealth of diffuse polarized emission across a large area of the survey with a
maximum peak of ~13 K, primarily with positive rotation measure values smaller
than +10 rad/m^2. The small values observed indicate that the emission is
likely to have a local origin (closer than a few hundred parsecs). There is a
large sky area at 2^h30^m where the diffuse polarized emission rms is fainter
than 1 K. Within this area of low Galactic polarization we characterize the
foreground properties in a cold sky patch at $(alpha,delta) =
(4^h,-27^circ.6)$ in terms of three dimensional power spectra | | Source: | arXiv, 1305.6047 | | Services: | Forum | Review | PDF | Favorites | |
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