Journal article
Direct Optimal Mapping Image Power Spectrum and its Window Functions
Z Xu, H Kim, JN Hewitt, KF Chen, NS Kern, E Rath, R Byrne, A Gorce, R Pascua, ZE Martinot, JS Dillon, BJ Hazelton, A Liu, MF Morales, Z Abdurashidova, T Adams, JE Aguirre, P Alexander, ZS Ali, R Baartman Show all
Astrophysical Journal | IOP Publishing Ltd | Published : 2024
Abstract
The key to detecting neutral hydrogen during the epoch of reionization (EoR) is to separate the cosmological signal from the dominating foreground radiation. We developed direct optimal mapping (DOM) to map interferometric visibilities; it contains only linear operations, with full knowledge of point spread functions from visibilities to images. Here, we demonstrate a fast Fourier transform-based image power spectrum and its window functions computed from the DOM images. We use noiseless simulation, based on the Hydrogen Epoch of Reionization Array Phase I configuration, to study the image power spectrum properties. The window functions show <10−11 of the integrated power leaks from the fore..
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Grants
Awarded by National Aeronautics and Space Administration
Funding Acknowledgements
This material is based upon work supported by the National Science Foundation under grants Nos. 1636646 and 1836019 and institutional support from the HERA collaboration partners. This research is funded in part by the Gordon and Betty Moore Foundation through grant GBMF5215 to the Massachusetts Institute of Technology. HERA is hosted by the South African Radio Astronomy Observatory, which is a facility of the National Research Foundation, an agency of the Department of Science and Innovation. The authors wish to thank the anonymous referee for their insightful feedback.We acknowledge the use of the Ilifu cloud computing facility and the support from the Inter-University Institute for Data Intensive Astronomy (IDIA). J.S.D. gratefully acknowledges the support of the NSF AAPF award No. 1701536. N.K. acknowledges support from NASA through the NASA Hubble Fellowship grant No. HST-HF2-51533.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. R.B. is supported by National Science Foundation Award No. 2303952. P.K. acknowledges support from the South African Radio Astronomy Observatory (SARAO) and the NationalResearch Foundation(grant No. 84156). This result is part of aproject that has received funding from the European ResearchCouncil(ERC)under the European Union's Horizon 2020research and innovation program(grant agreement No. 948764;P.B. and M.J.W.). P.B. acknowledges support from STFC grantST/T000341/1. Parts of this research were supported by theAustralian Research Council Centre of Excellence for All SkyAstrophysics in 3 Dimensions(ASTRO 3D), through projectNo. CE170100013. G.B. acknowledges funding from the INAFPRIN-SKA 2017 project 1.05.01.88.04(FORECaST), supportfrom the Ministero degli Affari Esteri della CooperazioneInternazionale-Direzione Generale per la Promozione delSistema Paese Progetto di Grande Rilevanza ZA18GR02 andthe National Research Foundation of South Africa(grant No.113121)as part of the ISARP RADIOSKY2020 Joint ResearchScheme, from the Royal Society and the Newton Fund undergrant NA150184 and from the National Research Foundation of South Africa(grant No. 103424). E.d.L.A. acknowledges thefunding support of the UKRI Science and TechnologyFacilities Council SKA grant. A.L. acknowledges supportfrom the New Frontiers in Research Fund Exploration grantprogram, the Canadian Institute for Advanced Research(CIFAR)Azrieli Global Scholars program, a Natural Sciencesand Engineering Research Council of Canada(NSERC)Discovery Grant and a Discovery Launch Supplement, the Sloan Research Fellowship, and the William Dawson Scholar-ship at McGill.