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http://hdl.handle.net/2289/7800Full metadata record
| DC Field | Value | Language |
|---|---|---|
| dc.contributor.author | Patwa, Akash K | - |
| dc.contributor.author | Sethi, S | - |
| dc.contributor.author | Dwarakanath, K S | - |
| dc.date.accessioned | 2021-07-23T04:49:32Z | - |
| dc.date.available | 2021-07-23T04:49:32Z | - |
| dc.date.issued | 2021-06 | - |
| dc.identifier.citation | Monthly Notices of the Royal Astronomical Society, 2021, Vol. 504, p2062-2072 | en_US |
| dc.identifier.issn | 0035-8711 | - |
| dc.identifier.issn | 1365-2966 (Online) | - |
| dc.identifier.uri | http://hdl.handle.net/2289/7800 | - |
| dc.description | Restricted Access. An open-access version is available at arXiv.org (one of the alternative locations) | en_US |
| dc.description.abstract | The detection of redshifted hyperfine line of neutral hydrogen (H i) is the most promising probe of the epoch of reionization (EoR). We report an analysis of 55 h of Murchison Widefield Array (MWA) phase II drift scan EoR data. The data correspond to a central frequency ν0=154.24MHz (z ≃ 8.2 for the redshifted H i hyperfine line) and bandwidth B=10.24MHz. As one expects greater system stability in a drift scan, we test the system stability by comparing the extracted power spectra from data with noise simulations and show that the power spectra for the cleanest data behave as thermal noise. We compute the H i power spectrum as a function of time in one and two dimensions. The best upper limit on the 1D power spectrum are: Δ2(k)≃(1000 mK)2 at k ≃ 0.2h Mpc−1 and at k ≃ 1h Mpc−1. The cleanest modes, which might be the most suited for obtaining the optimal signal to noise, correspond to k ≳ 1h Mpc−1. We also study the time-dependence of the foreground-dominated modes in a drift scan and compare with the expected behaviour. | en_US |
| dc.language.iso | en | en_US |
| dc.publisher | Oxford University Press on behalf of the Royal Astronomical Society | en_US |
| dc.relation.uri | https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.2062P/abstract | en_US |
| dc.relation.uri | https://arxiv.org/abs/2104.03321 | en_US |
| dc.relation.uri | https://doi.org/10.1093/mnras/stab989 | en_US |
| dc.rights | 2021 The Author(s) | en_US |
| dc.subject | methods: data analysis | en_US |
| dc.subject | methods: observational | en_US |
| dc.subject | techniques: interferometric | en_US |
| dc.subject | dark ages | en_US |
| dc.subject | reionization | en_US |
| dc.subject | first stars | en_US |
| dc.subject | early Universe | en_US |
| dc.subject | cosmology | en_US |
| dc.title | Extracting the 21cm EoR signal using MWA drift scan data | en_US |
| dc.type | Article | en_US |
| Appears in Collections: | Research Papers (A&A) | |
Files in This Item:
| File | Description | Size | Format | |
|---|---|---|---|---|
| 2021_MNRAS_Vol.504_p2062.pdf Restricted Access | Restricted Access | 2.77 MB | Adobe PDF | View/Open Request a copy |
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