The Hydrogen Intensity and Real-time Analysis eXperiment: 256-Element Array Status and Overview

Crichton, Devin; Aich, Moumita; Amara, Adam; Bandura, Kevin; Bassett, Bruce A.; Bengaly, Carlos; Berner, Pascale; Bhatporia, Shruti; Bucher, Martin; Chang, Tzu-Ching; Chiang, H. Cynthia; Cliche, Jean-Francois; Crichton, Carolyn; Dave, Romeel; de Villiers, Dirk I. L.; Dobbs, Matt A.; Ewall-Wice, Aaron M.; Eyono, Scott; Finlay, Christopher; Gaddam, Sindhu; Ganga, Ken; Gayley, Kevin G.; Gerodias, Kit; Gibbon, Tim; Gumba, Austin; Gupta, Neeraj; Harris, Maile; Heilgendorf, Heiko; Hilton, Matt; Hincks, Adam D.; Hitz, Pascal; Jalilvand, Mona; Julie, Roufurd; Kader, Zahra; Kania, Joseph; Karagiannis, Dionysios; Karastergiou, Aris; Kesebonye, Kabelo; Kittiwisit, Piyanat; Kneib, Jean-Paul; Knowles, Kenda; Kuhn, Emily R.; Kunz, Martin; Maartens, Roy; MacKay, Vincent; MacPherson, Stuart; Monstein, Christian; Moodley, Kavilan; Mugundhan, V.; Naidoo, Warren; Naidu, Arun; Newburgh, Laura B.; Nistane, Viraj; Di Nitto, Amanda; Ölçek, Deniz; Pan, Xinyu; Paul, Sourabh; Peterson, Jeffrey B.; Pieters, Elizabeth; Pieterse, Carla; Pillay, Aritha; Polish, Anna R.; Randrianjanahary, Liantsoa; Refregier, Alexandre; Renard, Andre; Retana-Montenegro, Edwin; Rout, Ian H.; Russeeawon, Cyndie; Sadr, Alireza Vafaei; Saliwanchik, Benjamin R. B.; Sampath, Ajith; Sanghavi, Pranav; Santos, Mario G.; Sengate, Onkabetse; Shaw, J. Richard; Sievers, Jonathan L.; Smirnov, Oleg M.; Smith, Kendrick M.; Sob, Ulrich Armel Mbou; Srianand, Raghunathan; Stronkhorst, Pieter; Sunder, Dhaneshwar D.; Tartakovsky, Simon; Taylor, Russ; Timbie, Peter; Tolley, Emma E.; Townsend, Junaid; Tyndall, Will; Ungerer, Cornelius; van Dyk, Jacques; van Vuuren, Gary; Vanderlinde, Keith; Viant, Thierry; Walters, Anthony; Wang, Jingying; Weltman, Amanda; Woudt, Patrick; Wulf, Dallas; Zavyalov, Anatoly; Zhang, Zheng

doi:10.48550/arxiv.2109.13755

Cited by 6 publications

(8 citation statements)

References 51 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

View full text Add to dashboard Cite

show abstract

“…While shot noise is the dominant noise for number counts, thermal noise is the most relevant noise source for intensity mapping. In Appendix C we briefly discuss thermal noise for intensity mapping and give the relevant ingredients for the Hydrogen Intensity and Real-Time Analysis eXperiment (HIRAX) experiment [29]. In Fig.…”

Section: Comparison With Intensity Mappingmentioning

confidence: 99%

An Estimator for the lensing potential from galaxy number counts

Nistane,

Jalilvand,

Carron

et al. 2022

Preprint

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We derive an estimator for the lensing potential from galaxy number counts which contains a linear and a quadratic term. We show that this estimator has a much larger signal-to-noise ratio than the corresponding estimator from intensity mapping. We show that this is due to the additional lensing term in the number count angular power spectrum which is present already at linear order. We estimate the signal-to-noise ratio for future photometric surveys. We find that particularly at high redshifts, z Á 1.5, the signal to noise ratio can become of order 30. We therefore claim that number counts in photometric surveys are an excellent means to measure tomographic lensing spectra.

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“…[31,64,65] for recent reviews). These correlations have been successfully detected using galaxies, quasars and the Lyman-↵ forest [69][70][71][72][73]. In fact, due to the large scales involved and the differential nature of the measurement (one or more peaks on top of a smooth background signal), BAOs are among the most robust measurements in cosmology.…”

Section: Instrumental Concepts and Challengesmentioning

confidence: 99%

Current status and future of cosmology with 21cm Intensity Mapping

Ansari¹

2022

Preprint

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21cm Intensity Mapping (IM) has been proposed about 15 years ago as a cost effective method to carry out cosmological surveys and to map the 3D distribution of matter in the universe, over a large range of post EoR redshifts, from z=0 to z=6. Since then a number of pathfinder instruments have been built, such as CHIME or Tianlai. Several other ones will be commissioned in the next few years (HIRAX, CHORD, BINGO), while even larger arrays, with several thousand antennae are being considered for the next generation experiments. We will briefly review the 21cm cosmology of the Epoch of Reionisation (EoR), and we will then focus on IM for late time cosmology. After presenting some of the promises of this technique to constrain the cosmological model, dark energy and inflation, we will review some of the instrumental and scientific challenges of IM surveys. The second part of the paper presents an overview of the ongoing and future experiments, as well as recent results by GBT, CHIME and Tianlai.

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The Hydrogen Intensity and Real-time Analysis eXperiment: 256-Element Array Status and Overview

Cited by 6 publications

References 51 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

An Estimator for the lensing potential from galaxy number counts

Current status and future of cosmology with 21cm Intensity Mapping

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