000169396 001__ 169396
000169396 005__ 20260225153354.0
000169396 0247_ $$2doi$$a10.1093/mnras/staa1191
000169396 0248_ $$2sideral$$a142900
000169396 037__ $$aART-2020-142900
000169396 041__ $$aeng
000169396 100__ $$0(orcid)0000-0002-6211-499X$$aAsorey, Jacobo
000169396 245__ $$aHIR4: cosmology from a simulated neutral hydrogen full sky using Horizon Run 4
000169396 260__ $$c2020
000169396 5203_ $$aThe distribution of cosmological neutral hydrogen will provide a new window into the large-scale structure of the Universe with the next generation of radio telescopes and surveys. The observation of this material, through 21 cm line emission, will be confused by foreground emission in the same frequencies. Even after these foregrounds are removed, the reconstructed map may not exactly match the original cosmological signal, which will introduce systematic errors and offset into the measured correlations. In this paper, we simulate future surveys of neutral hydrogen using the Horizon Run 4 (HR4) cosmological N-body simulation. We generate H i intensity maps from the HR4 halo catalogue, and combine with foreground radio emission maps from the Global Sky Model, to create accurate simulations over the entire sky. We simulate the H i sky for the frequency range 700–800 MHz, matching the sensitivity of the Tianlai pathfinder. We test the accuracy of the fastICA, PCA, and log-polynomial fitting foreground removal methods to recover the input cosmological angular power spectrum and measure the parameters. We show the effect of survey noise levels and beam sizes on the recovered the cosmological constraints. We find that while the reconstruction removes power from the cosmological 21 cm distribution on large scales, we can correct for this and recover the input parameters in the noise-free case. However, the effect of noise and beam size of the Tianlai pathfinder prevents accurate recovery of the cosmological parameters when using only intensity mapping information.
000169396 540__ $$9info:eu-repo/semantics/closedAccess$$aAll rights reserved$$uhttp://www.europeana.eu/rights/rr-f/
000169396 590__ $$a5.287$$b2020
000169396 591__ $$aASTRONOMY & ASTROPHYSICS$$b16 / 68 = 0.235$$c2020$$dQ1$$eT1
000169396 592__ $$a2.057$$b2020
000169396 593__ $$aSpace and Planetary Science$$c2020$$dQ1
000169396 593__ $$aAstronomy and Astrophysics$$c2020$$dQ1
000169396 655_4 $$ainfo:eu-repo/semantics/article$$vinfo:eu-repo/semantics/publishedVersion
000169396 700__ $$aParkinson, David
000169396 700__ $$aShi, Feng
000169396 700__ $$aSong, Yong-Seon
000169396 700__ $$aAhn, Kyungjin
000169396 700__ $$aKim, Juhan
000169396 700__ $$aYao, Jian
000169396 700__ $$aZhang, Le
000169396 700__ $$aZuo, Shifan
000169396 773__ $$g495, 2 (2020), 1788-1806$$pMon. not. R. Astron. Soc.$$tMonthly notices of the Royal Astronomical Society$$x0035-8711
000169396 8564_ $$s5045631$$uhttps://zaguan.unizar.es/record/169396/files/texto_completo.pdf$$yVersión publicada
000169396 8564_ $$s2750954$$uhttps://zaguan.unizar.es/record/169396/files/texto_completo.jpg?subformat=icon$$xicon$$yVersión publicada
000169396 909CO $$ooai:zaguan.unizar.es:169396$$particulos$$pdriver
000169396 951__ $$a2026-02-25-14:58:31
000169396 980__ $$aARTICLE