The birth of the first luminous sources and the ensuing epoch of reionization are best studied via the redshifted 21-cm emission line, the signature of the first two imprinting the last. In this work, we present a fully Bayesian method, HIBAYES, for extracting the faint, global (skyaveraged) 21-cm signal from the much brighter foreground emission.We showthat a simplified (but plausible) Gaussian model of the 21-cm emission from the Cosmic Dawn epoch (15 ≲ z ≲ 30), parametrized by an amplitude AHI, a frequency peak νHI and a width σHI, can be extracted even in the presence of a structured foreground frequency spectrum (parametrized as a seventh-order polynomial), provided sufficient signal-to-noise (400 h of observation with a single dipole). We apply our method to an early, 19-min-long observation from the Large aperture Experiment to detect the Dark Ages, constraining the 21-cm signal amplitude and width to be -890 < AHI < 0 mK and σHI > 6.5 MHz (corresponding to Δz > 1.9 at redshift z ≃ 20) respectively at the 95-per cent confidence level in the range 13.2 < z <27.4 (100 > ν >50 MHz).

Bayesian constraints on the global 21-cm signal from the Cosmic Dawn

Bernardi, G.;PRICE, David;Mesinger, A.;
2016-01-01

Abstract

The birth of the first luminous sources and the ensuing epoch of reionization are best studied via the redshifted 21-cm emission line, the signature of the first two imprinting the last. In this work, we present a fully Bayesian method, HIBAYES, for extracting the faint, global (skyaveraged) 21-cm signal from the much brighter foreground emission.We showthat a simplified (but plausible) Gaussian model of the 21-cm emission from the Cosmic Dawn epoch (15 ≲ z ≲ 30), parametrized by an amplitude AHI, a frequency peak νHI and a width σHI, can be extracted even in the presence of a structured foreground frequency spectrum (parametrized as a seventh-order polynomial), provided sufficient signal-to-noise (400 h of observation with a single dipole). We apply our method to an early, 19-min-long observation from the Large aperture Experiment to detect the Dark Ages, constraining the 21-cm signal amplitude and width to be -890 < AHI < 0 mK and σHI > 6.5 MHz (corresponding to Δz > 1.9 at redshift z ≃ 20) respectively at the 95-per cent confidence level in the range 13.2 < z <27.4 (100 > ν >50 MHz).
Settore FIS/05 - Astronomia e Astrofisica
Cosmology: observations; Dark ages, reionization, first stars; Diffuse radiation; Methods: data analysis; Methods: statistical;
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/11384/69365
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