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, John P.; Oxholm, Trevor M.; Phan, Anh; Stebbins, Albert; Timbie, Peter T.; Ansari, Reza; Campagne, Jean-Eric; Chen, Zhiping; Cong, Yanping; Huang, Qizhi; Li, Yichao; Liu, Tao; Liu, Yingfeng; Niu, Chenhui; Osinga, Calvin; Perdereau, Olivier; Peterson, Jeffrey B.; Shi, Huli; Siebert, Gage; Sun, Shijie; Tian, Haijun; Tucker, Gregory S.; Wang, Qunxiong; Wang, Rongli; Wang, Yougang; Wu, Yanlin; Xu, Yidong; Yu, Kaifeng; Yu, Zijie; Zhang, Jiao; Zhang, Juyong; Zhu, Jialu

doi:10.48550/arxiv.2011.05946

Cited by 3 publications

(3 citation statements)

References 32 publications

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“…The next few years will see data from a number of H intensity mapping experiments, for example the proposed MeerKLASS survey at the Square Kilometre Array (SKA) precursor MeerKAT (Santos et al 2017;Wang et al 2020), an H survey at the 500m dish telescope FAST (Hu et al 2020), and multiple surveys with the SKA using the single-dish mode of operation (Battye et al 2013;Bull et al 2015;Santos et al 2017;SKA Cosmology SWG et al 2020). Other international experiments include the CHIME project (Bandura et al 2014), HIRAX (Newburgh et al 2016), and Tianlai (Li et al 2020b;Wu et al 2020).…”

Section: Introductionmentioning

confidence: 99%

HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

Wolz,

Pourtsidou,

Masui

et al. 2021

Preprint

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We present the joint analysis of Neutral Hydrogen (H ) Intensity Mapping observations with three galaxy samples: the Luminous Red Galaxy (LRG) and Emission Line Galaxy (ELG) samples from the eBOSS survey, and the WiggleZ Dark Energy Survey sample. The H intensity maps are Green Bank Telescope observations of the redshifted 21cm emission on 100 deg 2 covering the redshift range 0.6 < 𝑧 < 1.0. We process the data by separating and removing the foregrounds present in the radio frequencies with F ICA. We verify the quality of the foreground separation with mock realisations, and construct a transfer function to correct for the effects of foreground removal on the H signal. We cross-correlate the cleaned H data with the galaxy samples and study the overall amplitude as well as the scale-dependence of the power spectrum. We also qualitatively compare our findings with the predictions by a semi-analytic galaxy evolution simulation. The cross-correlations constrain the quantity Ω H 𝑏 H 𝑟 H ,opt at an effective scale 𝑘 eff , where Ω H is the H density fraction, 𝑏 H is the H bias, and 𝑟 H ,opt the galaxyhydrogen correlation coefficient, which is dependent on the H content of the optical galaxy sample. At 𝑘 eff = 0.31 ℎ/Mpc we find Ω H 𝑏 H 𝑟 H ,Wig = [0.58 ± 0.09 (stat) ± 0.05 (sys)] × 10 −3 for GBT-WiggleZ, Ω H 𝑏 H 𝑟 H ,ELG = [0.40 ± 0.09 (stat) ± 0.04 (sys)] × 10 −3 for GBT-ELG, and Ω H 𝑏 H 𝑟 H ,LRG = [0.35 ± 0.08 (stat) ± 0.03 (sys)] × 10 −3 for GBT-LRG, at 𝑧 0.8. We also report results at 𝑘 eff = 0.24 ℎ/Mpc and 𝑘 eff = 0.48 ℎ/Mpc. With little information on H parameters beyond our local Universe, these are amongst the most precise constraints on neutral hydrogen density fluctuations in an underexplored redshift range.

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Section: Introductionmentioning

confidence: 99%

HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

Wolz,

Pourtsidou,

Masui

et al. 2021

Preprint

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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

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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

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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 Dish Pathfinder Array: design, operation and performance of a prototype transit radio interferometer

Cited by 3 publications

References 32 publications

HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

HI constraints from the cross-correlation of eBOSS galaxies and Green Bank Telescope intensity maps

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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