Twenty-one centimeter tomography with foregrounds

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dc.creatorWang, Xiaomin
dc.creatorTegmark, Max
dc.creatorSantos, Mario
dc.creatorKnox, Lloyd
dc.date2005-01-06
dc.date2006-06-09
dc.date.accessioned2026-07-07T10:47:57Z
dc.date.available2026-07-07T10:47:57Z
dc.descriptionTwenty-one centimeter tomography is emerging as a powerful tool to explore the end of the cosmic dark ages and the reionization epoch, but it will only be as good as our ability to accurately model and remove astrophysical foreground contamination. Previous treatments of this problem have focused on the angular structure of the signal and foregrounds and what can be achieved with limited spectral resolution (bandwidths in the 1 MHz range). In this paper we introduce and evaluate a ``blind'' method to extract the multifrequency 21cm signal by taking advantage of the smooth frequency structure of the Galactic and extragalactic foregrounds. We find that 21 cm tomography is typically limited by foregrounds on scales $k\ll 1h/$Mpc and limited by noise on scales $k\gg 1h/$Mpc, provided that the experimental bandwidth can be made substantially smaller than 0.1 MHz. Our results show that this approach is quite promising even for scenarios with rather extreme contamination from point sources and diffuse Galactic emission, which bodes well for upcoming experiments such as LOFAR, MWA, PAST, and SKA.
dc.description10 pages, 6 figures. Revised version including various cases with high noise level. Major conclusions unchanged. Accepted for publication in ApJ
dc.identifierhttps://arxiv.org/abs/astro-ph/0501081
dc.identifierhttp://arxiv.org/abs/astro-ph/0501081
dc.identifierAstrophys.J.650:529-537,2006
dc.identifierdoi:10.1086/506597
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/183714
dc.subjectAstrophysics
dc.titleTwenty-one centimeter tomography with foregrounds
dc.typetext

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