The Tianlai Cylinder Pathfinder array: System functions and basic performance analysis

Li, JiXia; Zuo, Shifan; Wu, Fengquan; Wang, Yougang; Zhang, JuYong; Sun, Shijie; Xu, Yuelong; Yu, Zijie; Ansari, R.; Li, Yichao; Stebbins, Albert; Timbie, Peter; Cong, Yanping; Geng, Jin-Jun; Hao, Jie; Huang, Qizhi; Li, Jianbin; Li, Rui; Liu, Donghao; Liu, YingFeng; Liu, Tao; Marriner, J.; Niu, Chenhui; Pen, Ue-Li; Peterson, Jeffrey B.; Shi, Huli; Shu, Lin; Song, Yafang; Tian, Huajun; Wang, Guisong; Wang, Qun-Xiong; Wang, RongLi; Wang, WeiXia; Wang, Xin; Yu, Kaifeng; Zhang, Jiao; Zhu, Bowen; Zhu, Jialu; Chen, XueLei

doi:10.1007/s11433-020-1594-8

Cited by 41 publications

(31 citation statements)

References 28 publications

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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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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

Self Cite

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“…So far, there are many current and future HI IM experiments comprised of wide-field and high-sensitivity radio telescopes or interferometers. Here we consider several typical examples, namely, the Baryon acoustic oscillations In Neutral Gas Observations (BINGO) [6,[32][33][34], the Five-hundred-meter Aperture Spherical radio Telescope (FAST) [35][36][37][38][39][40], the Square Kilometre Array (SKA) [24,[41][42][43], and the Tianlai cylinder array [18,[44][45][46][47][48]. This work aims to forecast how future HI IM experiments, including BINGO, FAST, SKA Phase I midfrequency array (SKA1-MID), and Tianlai, can constrain the interacting dark energy (IDE) model.…”

Section: Introductionmentioning

confidence: 99%

Prospects for Constraining Interacting Dark Energy Models with 21 cm Intensity Mapping Experiments

Zhang,

Wang,

et al. 2021

Preprint

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We forecast the constraints on cosmological parameters in the interacting dark energy model using the mock data generated for neutral hydrogen intensity mapping (IM) experiments. In this work, we consider only the interacting dark energy model with the energy transfer rate Q = βHρc, and take BINGO, FAST, SKA1-MID, and Tianlai as typical examples of the 21 cm IM experiments. We find that the Tianlai cylinder array will play an important role in constraining the interacting dark energy model. Assuming perfect foreground removal and calibration, and using the Tianlaialone data, we obtain σ(H0) = 0.10 km s −1 Mpc −1 , σ(Ωm) = 0.0013, and σ(σ8) = 0.0015 in the IΛCDM model, which are much better than the results of Planck+optical BAO (i.e. optical galaxy surveys). However, the Tianlai-alone data cannot provide very tight constraint on the coupling parameter β, compared with Planck+optical BAO, while the Planck+Tianlai data can give a rather tight constraint of σ(β) = 0.00052, due to the parameter degeneracies being well broken by the data combination. In the IwCDM model, we obtain σ(β) = 0.00058 and σ(w) = 0.006 from Planck+Tianlai. In addition, we also make a detailed comparison among BINGO, FAST, SKA1-MID, and Tianlai in constraining the interacting dark energy model. We show that the future 21 cm IM experiments will provide a useful tool for exploring the nature of dark energy, and will play a significant role in measuring the coupling between dark energy and dark matter.

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“…It has also been proposed that the large scale structure can be more efficiently mapped at low angular resolution by applying the intensity mapping (IM) method (Chang et al 2008). A number of such experiments are underway, such as Tianlai (Chen 2012;Xu et al 2015;Li et al 2020b;Wu et al 2020), CHIME (Bandura et al 2014;Newburgh et al 2014) and HIRAX (Newburgh et al 2016), as well as the specially designed single dish experiment BINGO (Battye et al 2012(Battye et al , 2016. This technique may also be applied to the new generation of general purpose radio telescopes, such as the MeerKAT (Santos et al 2017) and the Square Kilometer Array (SKA) (Santos et al 2015) in the southern hemisphere, and the Fivehundred-meter Aperture Spherical Telescope (FAST) (Nan et al 2011) in the northern hemisphere.…”

Section: Introductionmentioning

confidence: 99%

1/f Noise Analysis for FAST HI Intensity Mapping Drift-Scan Experiment

Hu,

Li,

Wang

et al. 2021

Preprint

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We investigate the 1/f noise of the Five-hundred-meter Aperture Spherical Telescope (FAST) receiver system using drift-scan data from an intensity mapping pilot survey. All the 19 beams have 1/f fluctuations with similar structures. Both the temporal and the 2D power spectrum densities are estimated. The correlations directly seen in the time series data at low frequency are associated with the sky signal, perhaps due to a coupling between the foreground and the system response. We use Singular Value Decomposition (SVD) to subtract the foreground. By removing the strongest components, the measured 1/f noise power can be reduced significantly. With 20 modes subtraction, the knee frequency of the 1/f noise in a 10 MHz band is reduced to 1.8 × 10 −3 Hz, well below the thermal noise over 500-seconds time scale. The 2D power spectra show that the 1/f-type variations are restricted to a small region in the time-frequency space and the correlations in frequency can be suppressed with SVD modes subtraction. The residual 1/f noise after the SVD mode subtraction is uncorrelated in frequency, and a simple noise diode frequency-independent calibration of the receiver gain at 8s interval does not affect the results. The 1/f noise can be important for HI intensity mapping, we estimate that the 1/f noise has a knee frequency ( ) ∼ 6 × 10 −4 Hz, and time and frequency correlation spectral indices ( ) ∼ 0.65, ( ) ∼ 0.8 after the SVD subtraction of 30 modes. This can bias the H power spectrum measurement by 10 percent.

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The Tianlai Cylinder Pathfinder array: System functions and basic performance analysis

Cited by 41 publications

References 28 publications

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

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

Prospects for Constraining Interacting Dark Energy Models with 21 cm Intensity Mapping Experiments

1/f Noise Analysis for FAST HI Intensity Mapping Drift-Scan Experiment

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