Statistical 21-cm signal separation via Gaussian Process Regression analysis

F. G. Mertens*, A. Ghosh, L. V. E. Koopmans

*Bijbehorende auteur voor dit werk

OnderzoeksoutputAcademicpeer review

39 Citaten (Scopus)
208 Downloads (Pure)

Samenvatting

Detecting and characterizing the Epoch of Reionization (EoR) and Cosmic Dawn via the redshifted 21-cm hyperfine line of neutral hydrogen will revolutionize the study of the formation of the first stars, galaxies, black holes, and intergalactic gas in the infant Universe. The wealth of information encoded in this signal is, however, buried under foregrounds that are many orders of magnitude brighter. These must be removed accurately and precisely in order to reveal the feeble 21-cm signal. This requires not only the modelling of the Galactic and extragalactic emission, but also of the often stochastic residuals due to imperfect calibration of the data caused by ionospheric and instrumental distortions. To stochastically model these effects, we introduce a new method based on ` Gaussian Process Regression' (GPR) which is able to statistically separate the 21-cm signal from most of the foregrounds and other contaminants. Using simulated LOFAR-EoR data that include strong instrumental mode mixing, we show that this method is capable of recovering the 21-cm signal power spectrum across the entire range k = 0.07 - 0.3 h cMpc (1). The GPR method is most optimal, having minimal and controllable impact on the 21-cm signal, when the foregrounds are correlated on frequency scales greater than or similar to 3 MHz and the rms of the signal has sigma(21cm) greater than or similar to 0.1 sigma(noise). This signal separation improves the 21-cm power-spectrum sensitivity by a factor greater than or similar to 3 compared to foreground avoidance strategies and enables the sensitivity of current and future 21-cm instruments such as the Square Kilometre Array to be fully exploited.

Originele taal-2English
Pagina's (van-tot)3640-3652
Aantal pagina's13
TijdschriftMonthly Notices of the Royal Astronomical Society
Volume478
Nummer van het tijdschrift3
DOI's
StatusPublished - aug-2018

Citeer dit