Exploring delaying and heating effects on the 21-cm signature of fuzzy dark matter

Sarkar, Debanjan; Flitter, Jordan; Kovetz, Ely D.

doi:10.1103/physrevd.105.103529

Cited by 14 publications

(8 citation statements)

References 95 publications

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“…For weak X-ray efficiency, Ref. [72] showed that Lyman-α heating dominates most of the EoH, and our results largely do not depend on the CMB heating. In our fiducial simulations, we consider log 10 (L X /SFR) = 39.…”

Section: Simulationsupporting

confidence: 64%

“…However, previous studies (like Ref. [72]) showed that for a fixed z, LW feedback suppresses the amplitude of the power spectrum significantly. On the other hand, the difference ∆z half ∼ 0.3 − 0.5 between with and without Lyman-α heating scenarios is small, and we can directly compare the heating effects here.…”

Section: A Effect Of Lyman-α Heatingmentioning

confidence: 86%

“…Based on this, we set log 10 (L X /SFR) = 39 to compensate for the extra heating caused by Lyman-α photons. Note that, for high X-ray efficiency, the Lyman-α heating is subdominant [72].…”

Section: Simulationmentioning

confidence: 99%

“…For details, the reader is referred to Ref. [72]. We consider a total of 540 days of observation per redshift with 6 hours of observation per day.…”

Section: Sensitivity Calculation For Heramentioning

confidence: 99%

“…1 In Ref. [72], we showed that Lyman-α heating suppresses the 21-cm power spectrum amplitude and this will likely affect the detectability of the VAOs.…”

Section: Introductionmentioning

confidence: 98%

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Measuring the cosmic expansion rate using 21-cm velocity acoustic oscillations

Sarkar¹,

Kovetz²

2022

Preprint

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The fluctuations in the dark matter-baryon relative velocity field are imprinted as acoustic oscillations in the 21-cm power spectrum during cosmic dawn (CD). These velocity acoustic oscillations (VAOs) keep the imprints of the comoving sound horizon scale. In a previous work by Muñoz, it has been demonstrated that these VAOs can be treated as standard rulers to measure the cosmic expansion rate at high redshifts by considering a variety of Lyman-Werner feedback strengths and foreground contamination scenarios. Here we extend that analysis by using a modified version of the public code 21cmFAST. We use this code to simulate the VAOs in 21-cm power spectrum and forecast the potential to constrain H(z) with the HERA radio telescope, taking into account the effects of Lyman-α heating, Lyman-Werner feedback and foregrounds, the dependence on various astrophysical parameters, and the degeneracy with cosmological parameters. We find that H(z) can be measured with HERA at ∼ 0.3 − 6% relative accuracy in the range 11 < z < 20, under different astrophysical and foreground scenarios, with uncertainties in the Planck cosmological parameters setting a ∼ 0.08 − 0.2% relative-error floor in the measurement. This accuracy is on par with most low-redshift measurements and can be helpful in testing various cosmological scenarios motivated by the ongoing "Hubble Tension".

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Section: Simulationsupporting

confidence: 64%

Section: A Effect Of Lyman-α Heatingmentioning

confidence: 86%

Section: Simulationmentioning

confidence: 99%

“…For details, the reader is referred to Ref. [72]. We consider a total of 540 days of observation per redshift with 6 hours of observation per day.…”

Section: Sensitivity Calculation For Heramentioning

confidence: 99%

“…1 In Ref. [72], we showed that Lyman-α heating suppresses the 21-cm power spectrum amplitude and this will likely affect the detectability of the VAOs.…”

Section: Introductionmentioning

confidence: 98%

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Measuring the cosmic expansion rate using 21-cm velocity acoustic oscillations

Sarkar¹,

Kovetz²

2022

Preprint

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Dark ages, a window on the dark sector. Hunting for ultra-light axions

Vanzan,

Raccanelli,

Bartolo

2024

J. Cosmol. Astropart. Phys.

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Measurements of 21 cm intensity mapping (IM) during the dark ages can potentially provide us with an unprecedented window on high redshifts and small scales. One of the main advantages this can bring involves the possibility to probe the nature of dark matter. Tests of dark matter models with the large-scale structure of the Universe are limited by non-linearities and astrophysical effects, which are not present for IM measurements during the dark ages. In this paper we focus on constraining the model in which dark matter is comprised, totally or in part, by ultra-light axion-like particles around the 10-18– 10-22 eV mass scale. For this model, the angular power spectrum of 21 cm brightness temperature fluctuations will exhibit a small-scale suppression. However, this effect is intertwined with the imprint of baryon-dark matter relative velocity at recombination, causing at the same time an enhancement at large-scales, which is affected by the mass and abundance of axion dark matter. In this work we forecast how future radio arrays will be able to constrain ultra-light axion mass through both these effects on the angular power spectrum.

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Effects of feedback-free starburst galaxies on the 21-cm signal and reionization history

Libanore,

Flitter,

Kovetz

et al. 2024

Monthly Notices of the Royal Astronomical Society

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Different star formation models at Cosmic Dawn produce detectable signatures in the observables of upcoming 21-cm experiments. In this work, we consider the physical scenario of feedback-free starbursts (FFB), according to which the star formation efficiency (SFE) is enhanced in sufficiently massive haloes at early enough times, thus explaining the indication from the JWST for an excess of bright galaxies at $z \ge 10$. We model the contribution of FFBs to popII SFE and compute the impact these have on the 21-cm global signal and power spectrum. We show that FFBs affect the evolution of the brightness temperature and the 21-cm power spectrum, but they only have a limited effect on the neutral hydrogen fraction. We investigate how the observables are affected by changes in the underlying star formation model and by contribution from popIII stars. Finally, we forecast the capability of next-generation Hydrogen Epoch of Reionization Array (HERA) to detect the existence of FFB galaxies via power spectrum measurements. Our results show the possibility of a significant detection, provided that popII stars are the main drivers of lowering the spin temperature. Efficient popIII star formation will make the detection more challenging.

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Exploring delaying and heating effects on the 21-cm signature of fuzzy dark matter

Cited by 14 publications

References 95 publications

Measuring the cosmic expansion rate using 21-cm velocity acoustic oscillations

Measuring the cosmic expansion rate using 21-cm velocity acoustic oscillations

Dark ages, a window on the dark sector. Hunting for ultra-light axions

Effects of feedback-free starburst galaxies on the 21-cm signal and reionization history

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