For interested parties, here's the arxiv link and password for the paper (submitted to ApJ).
Saul ---------- Forwarded message ---------- From: <[email protected]> Date: Tue, Feb 9, 2016 at 6:56 AM Subject: arXiv New submission -> 1602.02635 in astro-ph.IM from [email protected] To: [email protected] Your submission submit/1476266 has been assigned the permanent arXiv identifier 1602.02635 and is available at: http://arxiv.org/abs/1602.02635 The paper password for this article is: 2gcfp Please share this with your co-authors. They may use it to claim ownership. Abstract will appear in today's mailing as: ------------------------------------------------------------------------------ \\ arXiv:1602.02635 From: Saul Kohn <[email protected]> Date: Mon, 8 Feb 2016 16:28:38 GMT (1891kb,D) Title: Constraining Polarized Foregrounds for EoR Experiments I: 2D Power Spectra from the PAPER-32 Imaging Array Authors: S. A. Kohn, J. Aguirre, C. Nunhokee, G. Bernardi, J. Pober, Z. Ali, R. Bradley, C. Carilli, D. DeBoer, N. Gugliucci, D. Jacobs, P. Klima, D. MacMahon, J. Manley, D. Moore, A. Parsons, I. Stefan, W. Walbrugh Categories: astro-ph.IM astro-ph.CO Comments: 13 pages, 7 figures, submitted to ApJ License: http://arxiv.org/licenses/nonexclusive-distrib/1.0/ \\ Current-generation low frequency interferometers constructed with the objective of detecting the high-redshift 21 cm background, aim to generate power spectra of the brightness-temperature contrast of neutral hydrogen in primordial intergalactic medium. Two-dimensional power spectra (power in Fourier modes parallel and perpendicular to the line of sight) formed from interferometric visibilities have been shown to delineate a boundary between spectrally-smooth foregrounds (known as the wedge) and spectrally-structured 21 cm background emission (the EoR-window). However, polarized foregrounds are known to possess spectral structure due to Faraday rotation, which can leak into the EoR window. In this work, we create and analyze 2D power spectra from the PAPER-32 imaging array in Stokes I, Q, U and V. These allow us to observe and diagnose systematic effects in our calibration at high signal-to-noise within the Fourier space most relevant to EoR experiments. We observe well-defined windows in the Stokes visibilities, with Stokes Q, U and V power spectra sharing a similar wedge shape to that seen in Stokes I. With modest polarization calibration, we see no evidence that polarization calibration errors move power outside the wedge in any Stokes visibility, to the noise levels attained. Deeper integrations will be required to confirm that this behavior persists to the depth required for EoR detection. \\ Contains: delayfalls_wedgeres.pdf: 255979 bytes emulateapj.cls: 56203 bytes high_kperp_with_imshow_errorbars_title.pdf: 113663 bytes ionosphere4casacal_morelines.pdf: 30989 bytes natbib.bst: 24934 bytes new_antenna_config.pdf: 10177 bytes newcal_forks_lines.pdf: 125754 bytes oldcal_forks_lines.pdf: 126311 bytes uv_coverage_exclbad_overlaid.png: 259255 bytes wedgepaper.bbl: 46284 bytes wedgepaper.out: 639 bytes wedgepaper.synctex: 911477 bytes wedgepaper.tex: 42511 bytes wedges_final_vmin9_greybg.pdf: 139786 bytes zen_2455819_50285-I-image.pdf: 106235 bytes zen_2455819_50285-Q-image.pdf: 108233 bytes zen_2455819_50285-U-image.pdf: 102016 bytes zen_2455819_50285-V-image.pdf: 105054 bytes zen_2455819_50285_orig-I-image.pdf: 96242 bytes zen_2455819_50285_orig-Q-image.pdf: 99338 bytes zen_2455819_50285_orig-U-image.pdf: 107981 bytes zen_2455819_50285_orig-V-image.pdf: 110207 bytes
