The Tianlai dish pathfinder array: design, operation, and performance of a prototype transit radio interferometer

Wu, Fengquan; Li, Jixia; Zuo, Shifan; Chen, Xuelei; Das, Santanu; Marriner, J.; Oxholm, Trevor M.; Phan, Anh Huy; Stebbins, Albert; Timbie, Peter; Ansari, R.; Campagne, Jean-Eric; Chen, Zhiping; Cong, Yanping; Huang, Qizhi; Kwak, Juhun; Li, Yichao; Liu, Tao; Lei, Yingfeng; Niu, Chenhui; Calvin, Osinga; Perdereau, O.; Peterson, Jeffrey B.; Podczerwinski, John; Shi, Huli; Siebert, Gage; Sun, Shijie; Tian, Huajun; Tucker, Gregory S.; Wang, Qun-Xiong; Wang, Rongli; Wang, Yougang; Wu, Yanlin; Xu, Yuelong; Yu, Kaifeng; Yu, Zijie; Zhang, Jiao; Zhang, Jie; Zhu, Jialu

doi:10.1093/mnras/stab1802

Cited by 35 publications

(23 citation statements)

References 38 publications

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“…This is a small flux, but within the reach of current and planned radio surveys. In terms of raw signal-to-noise, this signal is within the reach of a large number of existing and near-future experiments, including CHIME (CHIME/Pulsar Collaboration et al 2021), ASKAP (Hotan et al 2021), MeerKAT (Jonas & MeerKAT Team 2016), Tianlei (Wu et al 2021), and GBT (Wolz et al 2021).…”

Section: Detectability Of the Signalmentioning

confidence: 94%

The radio SZ effect as a probe of the cosmological radio background

Holder,

Chluba

2021

Preprint

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If there is a substantial cosmological radio background, there should be a radio Sunyaev-Zeldovich (SZ) effect that goes along with it. The radio background Comptonization leads to a slight photon excess at all wavelengths, while Comptonization of the CMB at low frequencies leads to a decrement. For levels of the radio background consistent with observations, these effects cancel each other around ν 735 MHz, with an excess at lower frequencies and a decrement at higher frequencies. Assuming a purely cosmological origin of the observed ARCADE radio excess, at ν 20 GHz the signal scales as ∆T /T CMB 2 y (ν/735 MHz) −2.59 − 1 with frequency and the Compton-y parameter of the cluster. For a typical cluster, the total radio SZ signal is at the level of ∆T 1 mK around the null, with a steep scaling towards radio frequencies. This is above current raw sensitivity limits for many radio facilities at these wavelengths, providing a unique way to confirm the cosmological origin of the ARCADE excess and probe its properties (e.g., redshift dependence and isotropy). We also give an expression to compute the radio-analogue of the kinematic SZ effect, highlighting that this might provide a new tool to probe large-scale velocity fields and the cosmic evolution of the radio background.

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Section: Detectability Of the Signalmentioning

confidence: 94%

The radio SZ effect as a probe of the cosmological radio background

Holder,

Chluba

2021

Preprint

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“…More broadly, many of the methods developed for this analysis are not specific to CHIME, but could also be applied to other low-redshift interferometric 21 cm surveys, such as CHORD (Vanderlinde et al 2019), Tianlai (Li et al 2020;Wu et al 2021), HIRAX (Crichton et al 2021), uGMRT (Chakraborty et al 2021), and the Ooty Wide Field Array (Subrahmanya et al 2017), as well as higher-redshift surveys like HERA (DeBoer et al 2017) and potential future projects (Cosmic Visions 21 cm Collaboration et al 2018).…”

Section: Atomic Hydrogen Content Of Galaxies and Quasarsmentioning

confidence: 99%

Detection of Cosmological 21 cm Emission with the Canadian Hydrogen Intensity Mapping Experiment

Collaboration¹,

Amiri²,

Bandura³

et al. 2022

Preprint

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We present a detection of 21 cm emission from large-scale structure (LSS) between redshift 0.78 and 1.43 made with the Canadian Hydrogen Intensity Mapping Experiment (CHIME). Radio observations acquired over 102 nights are used to construct maps which are foreground filtered and stacked on the angular and spectral locations of luminous red galaxies (LRG), emission line galaxies (ELG), and quasars (QSO) from the eBOSS clustering catalogs. We find decisive evidence for a detection when stacking on all three tracers of LSS, with the logarithm of the Bayes Factor equal to 18.9 (LRG), 10.8 (ELG), and 56.3 (QSO). An alternative frequentist interpretation, based on the likelihood-ratio test, yields a detection significance of 7.1σ (LRG), 5.7σ (ELG), and 11.1σ (QSO). These are the first 21 cm intensity mapping measurements made with an interferometer. We constrain the effective clustering amplitude of neutral hydrogen (HI), defined as A HI ≡ 10 3 Ω HI b HI + f µ 2 , where Ω HI is the cosmic abundance of HI, b HI is the linear bias of HI, and f µ 2 = 0.552 encodes the effect of redshift-space distortions at linear order. We find A HI = 1.51 +3.60 −0.97 for LRGs (z = 0.84), A HI = 6.76 +9.04 −3.79for ELGs (z = 0.96), and A HI = 1.68 +1.10 −0.67 for QSOs (z = 1.20), with constraints limited by modeling uncertainties at nonlinear scales. We are also sensitive to bias in the spectroscopic redshifts of each tracer, and find a non-zero bias ∆ v = −66 ± 20 km/s for the QSOs. We split the QSO catalog into three redshift bins and have a decisive detection in each, with the upper bin at z = 1.30 producing the highest redshift 21 cm intensity mapping measurement thus far.

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“…A number of ongoing and upcoming interferometric 21 cm experiments have redundancy in their array configurations and, thus, can take advantage of the B C approach we demonstrate here. These include the Canadian Hydrogen Intensity Mapping Experiment (CHIME; Newburgh, et al 2014), the Hydrogen Epoch of Reionization Array (HERA;DeBoer et al 2017), the Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX; Newburgh et al 2016), Phase II of the Murchison Widefield Array (MWA; Wayth et al 2018) and Tianlai (Li et al 2020;Wu et al 2021). For the simulated observations calibrated in this paper we use a HERA-like hexagonal close-packed redundant array.…”

Section: The Bmentioning

confidence: 99%

A Bayesian approach to high fidelity interferometric calibration − II: demonstration with simulated data

Sims

Pober

Sievers

2022

Monthly Notices of the Royal Astronomical Society

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In a companion paper, we presented BayesCal, a mathematical formalism for mitigating sky-model incompleteness in interferometric calibration. In this paper, we demonstrate the use of BayesCal to calibrate the degenerate gain parameters of full-Stokes simulated observations with a HERA-like hexagonal close-packed redundant array, for three assumed levels of completeness of the a priori known component of the calibration sky model. We compare the BayesCal calibration solutions to those recovered by calibrating the degenerate gain parameters with only the a priori known component of the calibration sky model both with and without imposing physically motivated priors on the gain amplitude solutions and for two choices of baseline length range over which to calibrate. We find that BayesCal provides calibration solutions with up to four orders of magnitude lower power in spurious gain amplitude fluctuations than the calibration solutions derived for the same data set with the alternate approaches, and between ∼107 and ∼1010 times smaller than in the mean degenerate gain amplitude, on the full range of spectral scales accessible in the data. Additionally, we find that in the scenarios modelled only BayesCal has sufficiently high fidelity calibration solutions for unbiased recovery of the 21 cm power spectrum on large spectral scales (k∥ ≲ 0.15 hMpc−1). In all other cases, in the completeness regimes studied, those scales are contaminated.

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The Tianlai dish pathfinder array: design, operation, and performance of a prototype transit radio interferometer

Cited by 35 publications

References 38 publications

The radio SZ effect as a probe of the cosmological radio background

The radio SZ effect as a probe of the cosmological radio background

Detection of Cosmological 21 cm Emission with the Canadian Hydrogen Intensity Mapping Experiment

A Bayesian approach to high fidelity interferometric calibration − II: demonstration with simulated data

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