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|Title: ||Imaging the epoch of reionization: Limitations from foreground confusion and imaging Algorithms|
|Authors: ||Vedantham, Harish|
Udaya Shankar, N.
|Issue Date: ||Feb-2012 |
|Publisher: ||The American Astronomical Society|
|Citation: ||The Astrophysical Journal, 2012, Vol. 745, p176|
|Abstract: ||Tomography of redshifted 21 cm transition from neutral hydrogen using Fourier synthesis telescopes is a promising tool to study the Epoch of Reionization (EoR). Limiting the confusion from Galactic and extragalactic foregrounds is critical to the success of these telescopes. The instrumental response or the point-spread function (PSF) of such telescopes is inherently three dimensional with frequency mapping to the line-of-sight (LOS) distance. EoR signals will necessarily have to be detected in data where continuum confusion persists; therefore, it is important that the PSF has acceptable frequency structure so that the residual foreground does not confuse the EoR signature. This paper aims to understand the three-dimensional PSF and foreground contamination in the same framework. We develop a formalism to estimate the foreground contamination along frequency, or equivalently LOS dimension, and establish a relationship between foreground contamination in the image plane and visibility weights on the Fourier plane. We identify two dominant sources of LOS foreground contamination—"PSF contamination" and "gridding contamination." We show that PSF contamination is localized in LOS wavenumber space, beyond which there potentially exists an "EoR window" with negligible foreground contamination where we may focus our efforts to detect EoR. PSF contamination in this window may be substantially reduced by judicious choice of a frequency window function. Gridding and imaging algorithms create additional gridding contamination and we propose a new imaging algorithm using the Chirp Z Transform that significantly reduces this contamination. Finally, we demonstrate the analytical relationships and the merit of the new imaging algorithm for the case of imaging with the Murchison Widefield Array.|
|Description: ||Restricted Access. An open-access version is available at arXiv.org (one of the alternative locations)|
|Alternative Location: ||http://adsabs.harvard.edu/abs/2012ApJ...745..176V|
|Copyright: ||2012, The American Astronomical Society|
|Appears in Collections:||Research Papers (A&A)|
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