The hyperfine transition of 3He+ as a probe of the intergalactic medium

Bagla, J. S.; Loeb, Abraham

doi:10.48550/arxiv.0905.1698

Cited by 9 publications

(14 citation statements)

References 40 publications

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“…Intensity mapping was originally developed for 21 cm radiation (Hogan & Rees 1979;Scott & Rees 1990;Madau et al 1997), but has been studied for several other lines (in increasing frequency): deuterium (Sigurdson & Furlanetto 2006), 3 He+ (McQuinn & Switzer 2009;Bagla & Loeb 2009), CO (Righi et al 2008;Carilli 2011;Lidz et al 2011;Breysse et al 2014;Li et al 2015), C II (Gong et al 2012;Silva et al 2014;Uzgil et al 2014;Yue et al 2015), Lyα ance amount to different forms of dimensionality reduction. Liu & Tegmark (2011) show that most of the covariance that distinguishes foregrounds is in the ν, ν ′ directions rather than combinations involving angular separations.…”

Section: Introductionmentioning

confidence: 99%

Interpreting the Unresolved Intensity of Cosmologically Redshifted Line Radiation

Switzer

Chang

Masui

et al. 2015

ApJ

107

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Intensity mapping experiments survey the spectrum of diffuse line radiation rather than detect individual objects at high signal-to-noise ratio. Spectral maps of unresolved atomic and molecular line radiation contain threedimensional information about the density and environments of emitting gasand efficiently probe cosmological volumes out to high redshift. Intensity mapping survey volumes also contain all other sources of radiation at the frequencies of interest. Continuum foregrounds are typically~10 2 -10 3 times brighter than the cosmological signal. The instrumental response to bright foregrounds will produce new spectral degrees of freedom that are not known in advance, nor necessarily spectrally smooth. The intrinsic spectra of foregrounds may also not be wellknown in advance. We describe a general class of quadratic estimators to analyze data from single-dish intensity mapping experimentsand determine contaminated spectral modes from the data themselves. The key attribute of foregrounds is not that they are spectrally smooth, but instead that they have fewer bright spectral degrees of freedom than the cosmological signal. Spurious correlations between the signal and foregrounds produce additional bias. Compensation for signal attenuation must estimate and correct this bias. A successful intensity mapping experiment will control instrumental systematics that spread variance into new modes, and it must observe a large enough volume that contaminant modes can be determined independently from the signal on scales of interest.

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Section: Introductionmentioning

confidence: 99%

Interpreting the Unresolved Intensity of Cosmologically Redshifted Line Radiation

Switzer

Chang

Masui

et al. 2015

ApJ

107

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“…The spin temperature of 3 He + is determined by the collisional process and HeII Lyα radiative transfer via the HeII analog of the Wouthuysen-Field effect (Bagla & Loeb 2009;McQuinn & Switzer 2009;Takeuchi et al 2014):…”

Section: Data Availabilitymentioning

confidence: 99%

“…Among these, the LOw Frequency ARray 1 (LOFAR), the Murchison Widefield Array 2 (MWA), the Hydrogen Epoch of Reionization Array 3 (HERA), the Precision Array for Probing the Epoch of Reionization 4 (PAPER) and the upcoming Square Kilometer Array 5 (SKA). While efforts to probe the high-z IGM have focused extensively on the 21 cm line, the hyperfine transition of 3 He + at 8.66 GHz (3.5 cm) also offers a unique insight into some astrophysical phenomena prevalent in the early universe (Furlanetto et al 2006;Bagla & Loeb 2009;McQuinn & Switzer 2009;Takeuchi et al 2014;Vasiliev et al 2019). In addition to being a probe of the high-z evolution of the helium component of gas, Bagla & Loeb (2009) suggested that this feature could also in principle be used to obtain independent constraints on the 21 cm signal, because the evolution of both HII and HeII are driven by stellar type sources during the epoch of (hydrogen) reionization, and thus the 21 cm and 3.5 cm signals are expected to be anti-correlated at these redshifts.…”

Section: Introductionmentioning

confidence: 99%

“…Although Bagla & Loeb (2009) have evaluated the expected signal with a semi-analytic approach, a more rigorous modeling has yet to be done which accounts for the evolution of HeII (the thorough analysis of Takeuchi et al 2014 was concentrated at lower redshift and still lacked a full radiative transfer). Here we revisit this problem employing the simulations of reionization described in Eide et al (2018, hereafter E18) and Eide et al (submitted;hereafter E20), which model both H and He reionization as driven by stellar type sources, accreting nuclear black holes, X-ray binaries and shock heated interstellar medium.…”

Section: Introductionmentioning

confidence: 99%

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Probing the high-z IGM with the hyperfine transition of 3He+

Khullar

Busch

et al. 2020

Monthly Notices of the Royal Astronomical Society

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Abstract The hyperfine transition of 3He+ at 3.5 cm has been thought as a probe of the high-z IGM since it offers a unique insight into the evolution of the helium component of the gas, as well as potentially give an independent constraint on the 21 cm signal from neutral hydrogen. In this paper, we use radiative transfer simulations of reionization driven by sources such as stars, X-ray binaries, accreting black holes and shock heated interstellar medium, and simulations of a high-z quasar to characterize the signal and analyze its prospects of detection. We find that the peak of the signal lies in the range ∼1 − 50 μK for both environments, but while around the quasar it is always in emission, in the case of cosmic reionization a brief period of absorption is expected. As the evolution of HeII is determined by stars, we find that it is not possible to distinguish reionization histories driven by more energetic sources. On the other hand, while a bright QSO produces a signal in 21 cm that is very similar to the one from a large collection of galaxies, its signature in 3.5 cm is very peculiar and could be a powerful probe to identify the presence of the QSO. We analyze the prospects of the signal’s detectability using SKA1-mid as our reference telescope. We find that the noise power spectrum dominates over the power spectrum of the signal, although a modest S/N ratio can be obtained when the wavenumber bin width and the survey volume are sufficiently large.

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“…Sigurdson & Furlanetto (2006) have suggested a challenging possibility of determination of D/H abundance ratio by looking at hyperfine structure line at high redshift of both the H and D. Signals from IGMs and dense objects at high redshifts through the 3 He hyperfine transition has been studied. Detailed physics and suggested observational plans were presented (McQuinn & Switzer 2009), and the anticorrelation of H i 21 cm maps and 3 He ii 3 cm maps was suggested (Bagla & Loeb 2009).…”

Section: Introductionmentioning

confidence: 99%

Signals of the cosmological reionization in the radio sky through C and O fine structure lines

Kusakabe

Kawasaki

2011

Monthly Notices of the Royal Astronomical Society

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We study the excitation of the fine structure levels of C I, C II and O I by ultraviolet (UV) photons around strong UV sources which are also ionizing sources of the cosmological reionization at a redshift of ∼10. The evolutions of ionized regions around a point source are calculated by solving rate equations for non-equilibrium chemistry. Signals of UV photons through the fine structure lines are considered to be stronger at locations of more abundant chemical species of C I, C II and O I. Such environments would be realized at locations where strong fluxes of non-ionizing UV line photons available for the pumping up of fine structure levels exist, and simultaneously ionizing UV photons are effectively shielded by dense H I regions. Signals from H I regions of moderately large densities induced by redshifted UV photons emitted at the point sources are found to be dominantly large over those of others. We discuss the detectability of the signals, and show that signals from idealized environments will be possibly detected by radio observations with next-generation arrays to come after the Atacama Large Millimeter/submillimeter Array (ALMA).

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The hyperfine transition of 3He+ as a probe of the intergalactic medium

Cited by 9 publications

References 40 publications

Interpreting the Unresolved Intensity of Cosmologically Redshifted Line Radiation

Interpreting the Unresolved Intensity of Cosmologically Redshifted Line Radiation

Probing the high-z IGM with the hyperfine transition of 3He+

Signals of the cosmological reionization in the radio sky through C and O fine structure lines

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