2020MNRAS.495.2813G

Query : 2020MNRAS.495.2813G

2020MNRAS.495.2813G - Mon. Not. R. Astron. Soc., 495, 2813-2826 (2020/July-1)

Foreground modelling via Gaussian process regression: an application to HERA data.

GHOSH A., MERTENS F., BERNARDI G., SANTOS M.G., KERN N.S., CARILLI C.L., GROBLER T.L., KOOPMANS L.V.E., JACOBS D.C., LIU A., PARSONS A.R., MORALES M.F., AGUIRRE J.E., DILLON J.S., HAZELTON B.J., SMIRNOV O.M., GEHLOT B.K., MATIKA S., ALEXANDER P., ALI Z.S., BEARDSLEY A.P., BENEFO R.K., BILLINGS T.S., BOWMAN J.D., BRADLEY R.F., CHENG C., CHICHURA P.M., DEBOER D.R., DE LERA ACEDO E., EWALL-WICE A., FADANA G., FAGNONI N., FORTINO A.F., FRITZ R., FURLANETTO S.R., GALLARDO S., GLENDENNING B., GORTHI D., GREIG B., GROBBELAAR J., HICKISH J., JOSAITIS A., JULIUS A., IGARASHI A.S., KARISEB M., KOHN S.A., KOLOPANIS M., LEKALAKE T., LOOTS A., MacMAHON D., MALAN L., MALGAS C., MAREE M., MARTINOT Z.E., MATHISON N., MATSETELA E., MESINGER A., NEBEN A.R., NIKOLIC B., NUNHOKEE C.D., PATRA N., PIETERSE S., RAZAVI-GHODS N., RINGUETTE J., ROBNETT J., ROSIE K., SELL R., SMITH C., SYCE A., TEGMARK M., THYAGARAJAN N., WILLIAMS P.K.G. and ZHENG H.

Abstract (from CDS):

The key challenge in the observation of the redshifted 21-cm signal from cosmic reionization is its separation from the much brighter foreground emission. Such separation relies on the different spectral properties of the two components, although, in real life, the foreground intrinsic spectrum is often corrupted by the instrumental response, inducing systematic effects that can further jeopardize the measurement of the 21-cm signal. In this paper, we use Gaussian Process Regression to model both foreground emission and instrumental systematics in ∼2 h of data from the Hydrogen Epoch of Reionization Array. We find that a simple co-variance model with three components matches the data well, giving a residual power spectrum with white noise properties. These consist of an 'intrinsic' and instrumentally corrupted component with a coherence scale of 20 and 2.4 MHz, respectively (dominating the line-of-sight power spectrum over scales k|| <= 0.2 h cMpc–1) and a baseline-dependent periodic signal with a period of ∼1 MHz (dominating over k|| ∼ 0.4-0.8 h cMpc–1), which should be distinguishable from the 21-cm Epoch of Reionization signal whose typical coherence scale is ∼0.8 MHz.

Abstract Copyright: © 2020 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): instrumentation: interferometers - methods: statistical - dark ages, reionization, first stars - diffuse radiation - large-scale structure of Universe - cosmology: observations

Simbad objects: 8

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Number of rows : 8
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2026 		#notes
1 NGC 1316 rG 03 22 41.789 -37 12 29.52 9.81 9.15 8.53 7.66   ~ 1491 1
2 ESO 252-18A Sy1 05 19 49.7229323856 -45 46 43.852662732   15.73 15.77 14.85   ~ 714 0
3 MCG+07-41-003 Bla 19 59 28.35656837 +40 44 02.0972325   16.22 15.10     ~ 2537 2
4 PMN J2100-2828 rG 21 00 12.447 -28 29 07.44           ~ 12 1
5 GLEAM J210138-280019 Rad 21 01 38.3 -28 00 19           ~ 1 0
6 NVSS J210139-280320 Rad 21 01 40.54 -28 03 19.7           ~ 2 1
7 GLEAM J210722-252556 Rad 21 07 22.3 -25 25 56           ~ 1 0
8 GLEAM J210724-252953 Rad 21 07 24.5 -25 29 53           ~ 1 0

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