Microwave Radiation of Singly Charged Helium 3 from H II Regions

Goldwire, H. C.; Goss, W. M.

doi:10.1086/149225

Cited by 12 publications

(17 citation statements)

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“…† The values of A 10 for some of the materials which is interesting on radio astronomy can be found in(Townes 1957;Gould 1994;Sunyaev 1966;Goldwire & Goss 1967).…”

mentioning

confidence: 99%

Probing large-scale filaments with H I and 3He II

Takeuchi

Zaroubi

Sugiyama

2014

Monthly Notices of the Royal Astronomical Society

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We explore the observability of the neutral hydrogen (H i) and the singly-ionized isotope helium-3 ( 3 He ii) in the intergalactic medium (IGM) from the Epoch of Reionization down to the local Universe. The hyperfine transition of 3 He ii, which is not as well known as the H i transition, has energy splitting corresponding to 8 cm. It also has a larger spontaneous decay rate than that of neutral hydrogen, whereas its primordial abundance is much smaller. Although both species are mostly ionized in the IGM, the balance between ionization and recombination in moderately high density regions renders them abundant enough to be observed. We estimate the emission signal of both hyperfine transitions from large scale filamentary structures and discuss the prospects for observing them with current and future radio telescopes. We conclude that H i in filaments is possibly observable even with current telescopes after 100 hours of observation. On the other hand, 3 He ii is only detectable with future telescopes, such as SKA, after the same amount of time.

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“…† The values of A 10 for some of the materials which is interesting on radio astronomy can be found in(Townes 1957;Gould 1994;Sunyaev 1966;Goldwire & Goss 1967).…”

mentioning

confidence: 99%

Probing large-scale filaments with H I and 3He II

Takeuchi

Zaroubi

Sugiyama

2014

Monthly Notices of the Royal Astronomical Society

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“…As a result of the ground state being the triplet, emission is suppressed. The Einstein coefficient for the spontaneous decay of this transition is A10 = 1.96 × 10 −12 s −1 (Sunyaev 1966;Goldwire & Goss 1967), which is ∼ 700 times larger than the corresponding coefficient for the hyperfine transition of hydrogen. The effective gain is reduced by a factor of 3 due to the excited state being the singlet.…”

Section: Hyperfine Transition Of 3 He IImentioning

confidence: 89%

“…The astrophysical relevance of this transition was first pointed out by Townes (1957). Early studies focused on observing the transition from the interstellar medium, specifically from emission line nebulae (Sunyaev 1966;Goldwire & Goss 1967;Goldwire 1967). Several papers (Doroshkevich, Zel'Dovich, & Novikov 1967;Sunyaev & Zeldovich 1975;Furlanetto, Oh, & Briggs 2006) pointed out that this transition may potentially be used to probe early stages of galaxy formation.…”

Section: Introductionmentioning

confidence: 99%

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

Bagla,

Loeb

2009

Preprint

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“…This would require using future optical and near-infrared observational facilities of 30m class telescopes (Cooke 2015). An alternative option to measure the BBN abundance of 3 He is to detect the absorption owing to the hyperfine 3 HeII line (Townes 1957;Sunyaev 1966;Goldwire & Goss 1967;Rood et al 1979) in the quasar spectra at z > ∼ 3 (McQuinn & Switzer 2009). The 3 HeII hyperfine line has been detected from local HII regions and planetary nebulae using both single-dish radio telescopes (e.g.…”

Section: Introductionmentioning

confidence: 99%

Probing primordial 3He from hyperfine line afterglows around supercritical black holes

Vasiliev

Sethi

Shchekinov

2019

Monthly Notices of the Royal Astronomical Society

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We consider the possibility of the detection of 3 HeII hyperfine line (rest frequency, 8.67 GHz) emission from ionized zones around accreting black holes (BHs) formed at high redshifts, z = 15-30. We show that the brightness temperature in 8.67GHz line increases and reaches a peak value after the accretion onto the BH exhausts and HeIII recombines into HeII. This period of brightening last up to 40 million years. We find that during this period the maximum brightness temperature reaches ≃ 0.2-0.5µK, depending on the epoch when such a black hole starts growing. The maximum angular size of the region emitting in the hyperfine line is around 0.5 ′ . The flux from such a region (≃ 0.3 nJy) is too small to be detected by SKA1-MID. The RMS of the collective flux from many emitting regions from a volume bounded by the synthesized beam and the band-width of SKA1-MID might reach 100 nJy, which is potentially detectable by SKA1-MID.

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Microwave Radiation of Singly Charged Helium 3 from H II Regions

Cited by 12 publications

References 0 publications

Probing large-scale filaments with H I and 3He II

Probing large-scale filaments with H I and 3He II

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

Probing primordial 3He from hyperfine line afterglows around supercritical black holes

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