Sent from my iPad
Begin forwarded message: From: <[email protected]<mailto:[email protected]>> Date: February 10, 2016 at 8:13:54 PM EST To: <[email protected]<mailto:[email protected]>> Subject: arXiv Replacement -> 1502.05072 in astro-ph.CO from [email protected]<mailto:[email protected]> Reply-To: <[email protected]<mailto:[email protected]>> Your replacement of 1502.05072 by submission submit/1477823 has been published and is available at: http://arxiv.org/abs/1502.05072 The paper password for this article is: nnd6n Please share this with your co-authors. They may use it to claim ownership. Abstract will appear in today's mailing as: ------------------------------------------------------------------------------ \\ arXiv:1502.05072 From: James Aguirre <[email protected]<mailto:[email protected]>> Date: Tue, 17 Feb 2015 21:53:01 GMT (477kb) Date (revised v2): Wed, 10 Feb 2016 04:09:22 GMT (488kb,D) Title: New Limits on Polarized Power Spectra at 126 and 164 MHz: Relevance to Epoch of Reionization Measurements Authors: David Moore, James E. Aguirre, Saul Kohn, Aaron Parsons, Zaki Ali, Richard Bradley, Chris Carilli, David DeBoer, Matthew Dexter, Nicole Gugliucci, Daniel Jacobs, Pat Klima, Adrian Liu, David MacMahon, Jason Manley, Jonathan Pober, Irina Stefan, and William Walbrugh Categories: astro-ph.CO astro-ph.IM Comments: Submitted to ApJ License: http://arxiv.org/licenses/nonexclusive-distrib/1.0/ \\ Polarized foreground emission is a potential contaminant of attempts to measure the fluctuation power spectrum of highly redshifted 21 cm HI emission from the epoch of reionization. Using the Donald C. Backer Precision Array for Probing the Epoch of Reionization (PAPER), we present limits on the observed power spectra of all four Stokes parameters in two frequency bands, centered at 126 MHz ($z=10.3$) and 164 MHz ($z=7.66$) for a three-month observing campaign of a 32-antenna deployment, for which unpolarized power spectrum results have been reported at $z=7.7$ (Parsons et al 2014) and $7.5 < z < 10.5$ (Jacobs et al 2014). The power spectra in this paper are processed in the same way as in those works, and show no definitive detection of polarized power. This non-detection appears to be largely due to the suppression of polarized power by ionospheric rotation measure fluctuations, which strongly affect Stokes Q and U. We are able to show that the net effect of polarized leakage is a negligible contribution at the levels of of the limits reported in Parsons et al 2014 and Jacobs et al 2014. \\ Contains: FOV-eps-converted-to.pdf: 70102 bytes PQ_vs_t-eps-converted-to.pdf: 81043 bytes Pspec_2x2_110_149-eps-converted-to.pdf: 32216 bytes Pspec_2x2_37_70-eps-converted-to.pdf: 32170 bytes RM_dist_per_LST.pdf: 16905 bytes Tsys_all-eps-converted-to.pdf: 176843 bytes Tsys_lst-eps-converted-to.pdf: 41724 bytes apj_w_etal.bst: 30706 bytes emulateapj.cls: 62658 bytes ms.bbl: 14352 bytes ms.tex: 48630 bytes widefield_RM_snap.pdf: 106626 bytes
