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Bursty star formation, now observed in distant galaxies, adds a positive shot-noise-like term to the Cosmic Dawn 21-cm power spectrum, filling in the predicted absorption trough and boosting high-redshift small-scale power by up to an order

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2026-08-01 09:43 UTC pith:PTN3R7BC

load-bearing objection A clean analytic extension of Zeus21 adding a bursty shot-noise term; the deterministic-shot baseline is a keeper, but both headline boosts—WF trough and high redshift—are more contingent than the abstract suggests, especially given the unquantified stellar-lifetime response. the 3 major comments →

arxiv 2607.20651 v1 pith:PTN3R7BC submitted 2026-07-22 astro-ph.CO astro-ph.GA

When galaxies burst II. Implications of enhanced burstiness for the 21-cm Cosmic Dawn signal

Hovav Lazare , Sarah Libanore , Eleonora Vanzan , Julian B. Mu\~noz , Ely D. Kovetz This is my paper
classification astro-ph.CO astro-ph.GA
keywords 21-cm cosmologyCosmic Dawnbursty star formationshot noise21-cm power spectrumLyman-alpha backgroundX-ray heatingunequal-time correlations
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

Recent observations of very distant galaxies suggest star formation was bursty, with episodes lasting tens of millions of years. This paper asks what such burstiness does to the 21-cm signal of neutral hydrogen during Cosmic Dawn and argues that the effect is not a small correction. Modeling each galaxy's star formation as a stochastic, time-correlated process, the authors show that burstiness injects a shot-noise-like boost into the Lyman-alpha and X-ray backgrounds that drive the 21-cm signal, filling in the predicted absorption trough by a factor of a few and boosting high-redshift small-scale power by up to an order of magnitude. The sky-averaged signal is unchanged, so the effect appears purely in the fluctuation statistics. If correct, forthcoming low-frequency radio arrays could observe this signature, turning the 21-cm power spectrum into a probe of how stochastically the faintest galaxies formed stars.

Core claim

This paper claims that bursty star formation—the observed tendency of early galaxies to form stars in episodes lasting tens of millions of years—materially changes the predicted 21-cm power spectrum of Cosmic Dawn, even though it leaves the sky-averaged signal unchanged. The burstiness induces a positive, shot-noise-like term in the fluctuations of the Lyman-alpha and X-ray backgrounds, sourced by unequal-time correlations within each galaxy's star-formation history. This term fills in the near-cancellation that creates the absorption trough, boosting the power there by a factor of a few, and dominates small scales at z greater than about 20, where the faintest halos are the most bursty. The

What carries the argument

The central object is an unequal-time, same-halo autocorrelation of the star-formation rate density. Each galaxy's star-formation rate is treated as a stochastic process with a correlation function that decays exponentially with the time separation between two emission epochs, governed by a burst amplitude and a coherence time. Because Lyman-alpha and X-ray photons reaching an observer were emitted from concentric shells at different retarded times, this correlator is convolved with the shells' radiative kernels. The result is a positive, roughly white shot-noise contribution to the power spectrum that is largest when the shell-pair light-travel time is shorter than the burst coherence time—

Load-bearing premise

The burst-strength relation is extrapolated to halos far smaller than those used to calibrate it, and a saturation cap on the burst amplitude is unconstrained; the high-redshift enhancement changes by up to a factor of about 3.5 when the cap is relaxed.

What would settle it

Measure the 21-cm power spectrum at the absorption-trough epoch (z ~ 15–16) at k ~ 0.1 cMpc^-1 with sensitivity near a few mK^2: the bursty model predicts a floor several times above the no-shot baseline, so a clean non-detection of that floor would rule out the mechanism. A less direct falsifier is a measurement of the burst-strength scatter for halos below about 5 × 10^9 solar masses; if those halos are not strongly bursty, the high-redshift boost disappears.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • At the absorption trough near z ~ 15–16, the bursty shot noise lifts the 21-cm power spectrum from about 2 mK^2 to about 9 mK^2 at k = 0.1 cMpc^-1 in the fiducial model, turning a near-null into a measurable signal.
  • Across a broad region of the (z, k) plane the bursty model exceeds the no-shot baseline by factors of 2–5, reaching roughly an order of magnitude at small scales and z greater than about 22.
  • The effect becomes negligible at z less than about 12, where clustering from more massive halos dominates, so burstiness does not disturb inferences from lower-redshift 21-cm upper limits.
  • The sky-averaged 21-cm signal is unchanged by construction, so global-signal experiments are not affected; only fluctuation statistics carry the signature.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the extrapolated burstiness applies to the faintest atomic-cooling halos, the 21-cm power spectrum would effectively see a galaxy population invisible to deep imaging surveys, making it a unique census of sub-detection-threshold galaxies.
  • The same unequal-time formalism should extend to the ionizing continuum: mean ionizing photon production would be unchanged, but burstiness would make reionization patchier, with ionized bubbles growing during bursts and partially recombining between them—a signature the paper leaves for future work.
  • Because the high-redshift boost depends so strongly on the unconstrained saturation cap, a joint analysis of 21-cm and galaxy data could turn the boost amplitude itself into a measurement of small-halo burstiness.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

3 major / 4 minor

Summary. The paper extends the public analytic 21-cm code Zeus21 to include bursty star formation modeled as an Ornstein–Uhlenbeck process calibrated by the M26 analysis of JWST/HST data. The central technical contribution is an unequal-time, same-halo SFR correlator that is propagated through the non-local Lyα and X-ray kernels that drive the Cosmic Dawn 21-cm signal. The authors also add a deterministic shot-noise term arising from halo discreteness. They find that burstiness leaves the global 21-cm signal unchanged by construction but boosts the 21-cm power spectrum by factors of several over the no-shot baseline, especially near the Wouthuysen–Field trough (z~15–16) and at high redshift/small scales (z≳20), while the deterministic shot noise alone gives a smaller and more localized correction. The paper includes extensive parameter-sensitivity tests and a comparison with 21cmFAST and earlier shot-noise studies.

Significance. If the central result holds, this is a valuable and timely result: it shows that bursty star formation, inferred from JWST, can qualitatively change the predicted 21-cm power spectrum at Cosmic Dawn and provides a fast O(1 s) analytic route to survey forecasts. The introduction of deterministic shot noise into Zeus21 is itself a useful extension, and the authors are explicit about what is and is not changed by construction. The paper also gives credit to, and engages with, competing semi-numerical implementations. However, the quantitative headline — a factor-of-few boost at the WF trough and order-of-magnitude enhancement at high z — depends on two modeling steps that are acknowledged but not quantitatively assessed: the unconstrained extrapolation of σ_PS to low-mass halos, and the assumption that Lyα/X-ray luminosities respond instantaneously to the bursty SFR. Because these assumptions directly control the two headline regimes, the paper in its current form does not yet fully establish the advertised predictions.

major comments (3)
  1. [Sec. VI.A, Fig. 7] The high-redshift (z≳20) enhancement is driven by halos below the M26 calibration regime (M_h ≲ 5×10^9 M_sun). The parameter σ_max^PS, which caps σ_PS there, is unconstrained by data, and Fig. 7 shows that changing it from 2.3 to 3.5 changes the total 21-cm power by up to a factor ~3.5 at z=21. This is a load-bearing uncertainty because Fig. 5 reports order-of-magnitude boosts at z=22–25 and the abstract emphasizes enhancement at the beginning of Cosmic Dawn where low-mass halos dominate. The paper states this limitation clearly but the central claim of a large high-z boost is therefore not robust without a more defensible cap or a propagated uncertainty band. I ask the authors to present the high-z predictions as a range across σ_max^PS, or to identify a physically motivated prior for the cap, and to state which conclusions survive the conservative choice.
  2. [Sec. IV.A, Eqs. (16)–(19), and Sec. VI.E] The Lyα and X-ray shot-noise terms assume that the instantaneous SFR is directly proportional to the emitted luminosity. Physically, Lyα emission from a burst lasts only ~10 Myr (the UV-bright phase), and X-ray binaries produce delayed and extended emission. The unequal-time SFR correlator in Eq. (11) should be convolved with finite stellar-population response functions before insertion into Eqs. (17) and (19). The authors acknowledge this in Sec. VI.E and predict a reduction of the large-scale burstiness signal toward the deterministic-shot case, but they do not provide a quantitative estimate. Since the WF-trough boost at k≈0.1 cMpc⁻¹ (Fig. 4, left) is one of the paper's two headline results, and Sec. VI.C identifies z~15–16 at k=0.1 as the primary observational target, this missing calculation is not a peripheral caveat. I request a quantitative test, e.g., a simple convolution with a
  3. [Sec. II, Table I; Sec. V, Figs. 4–5] The paper uses fiducial values for σ_PS and τ_PS without propagating their quoted uncertainties into the 21-cm predictions. The M26 constraints are σ_PS=2.1^{+0.11}_{-0.08} and τ_PS=25^{+27}_{-11} Myr; the latter is broad and highly asymmetric. The right panel of Fig. 4 shows that τ_PS=1 Myr essentially removes the bursty enhancement, while τ_PS=100 Myr shifts and further boosts the features. Because the central claim is a factor-of-few enhancement, it should be accompanied by at least an error band or a sensitivity scan over the 68% range of the M26 parameters, rather than a single fiducial curve. This is particularly important for the WF transition where the shot-noise contribution partially fills a cancellation.
minor comments (4)
  1. [Abstract and Sec. V, Fig. 5] The abstract and conclusions describe a boost by 'a factor of a few,' but Fig. 5 shows order-of-magnitude enhancements at z≳22 and small scales. Please harmonize the wording with the actual range and clearly distinguish the observationally accessible WF regime from the more uncertain high-z regime.
  2. [Sec. IV.C, Eq. (21)] The cross term is written P^shot_{TX,xα} in Eq. (21) but elsewhere referred to as P^shot_{Lyα,TX}; unify the notation to avoid confusion.
  3. [Sec. III.A, Eq. (10)] The ensemble average on the right side of Eq. (10) is written without an explicit bracket around the product of y_i and the phase; adding the expectation symbol would improve clarity for the reader.
  4. [Sec. VI.E] The discussion of finite stellar lifetimes is well placed but too brief; a short estimate of the effective coherence time for Lyα relative to τ_PS would make the caveat more actionable and connect it directly to Eqs. (17) and (19).

Circularity Check

0 steps flagged

No significant circularity: burstiness parameters are externally calibrated and the 21-cm calculation is a forward propagation, not a fit to the target.

full rationale

The paper's derivation chain is not circular. The burstiness parameters (sigma_PS, tau_PS, and mass slopes) are adopted from M26, which is calibrated to JWST/HST UV luminosity functions, Halpha/UV ratios, and clustering data (Sec. II, Table I; Refs. [16,17]); these are external observables unrelated to the 21-cm power spectrum. The central calculation, Eqs. (7), (11), (17), (19), and (21), propagates the resulting per-halo unequal-time SFR autocorrelation through Ly-alpha and X-ray light-cone kernels into Delta^2_T21. None of those equations is fitted to the 21-cm power spectrum or to the WF-trough boost; the enhancement is an emergent output of the shell-convolution integrals. The statement that the global signal is unchanged is explicitly a convention choice ('The mean signal remains unchanged given the conventions chosen in this work,' Sec. I; see also the Sec. II footnote), not a validated prediction, and it is not used as evidence for the central claim. Self-citations exist (M26 and the companion paper [18]), but M26 is anchored to independent data, and Zeus21 [59] is an independently developed code base; no load-bearing argument reduces to an unverified self-citation or to a uniqueness claim. The acknowledged limitations, namely extrapolation of sigma_PS below M_h ~ 5e9 M_sun with the unconstrained cap sigma_max^PS (Sec. VI.A, Fig. 7) and the neglect of finite stellar-lifetime response for Ly-alpha and X-ray emission (Sec. VI.E), are modeling uncertainties and physical approximations, not reductions of the result to its inputs by construction. I therefore find no significant circularity.

Axiom & Free-Parameter Ledger

6 free parameters · 8 axioms · 0 invented entities

The central calculation takes the M26 OU burstiness model and the Zeus21 SFR/astrophysical background as inputs; no new physical entities are introduced. The principal free parameters are the M26-fitted burstiness values plus the unconstrained cap σ_max^PS, which governs the high-z prediction.

free parameters (6)
  • σ_PS = 2.1 (+0.11/-0.08)
    Burst amplitude at pivot mass 10^10 M_sun, fitted by M26 to JWST UVLF, Hα/UV scatter and clustering; sets the exponential boost factor.
  • τ_PS = 25 Myr (+27/-11)
    OU coherence time, weakly fitted by M26; controls how far apart in time/radius the burst enhancement reaches.
  • dσ_PS/dlog10 M_h = -0.50 ± 0.13
    Mass slope makes smaller halos burstier; drives the high-redshift enhancement.
  • σ_max^PS = 2.3 (baseline; 3.5 tested)
    Hand-chosen cap on σ_PS for halos below the M26 calibration range; unconstrained; directly controls high-z boost amplitude (Fig. 7).
  • dlog10 τ_PS/dlog10 M_h = 0 (fiducial; -1 to +1 varied)
    Unconstrained by M26; varying it changes the X-ray shot noise by factors up to 5 (Fig. 8).
  • Zeus21 astrophysical parameters (f_*, M_p, α_*, β_*, f_duty) = Default Zeus21 values (fitted to UVLFs)
    SFR efficiency and duty-cycle parameters inherited from Zeus21 (Appendix B); they set which halo masses dominate and thus how much burstiness matters.
axioms (8)
  • domain assumption SFR of each halo is a lognormal Ornstein-Uhlenbeck process with mass-dependent σ_PS and τ_PS
    Eqs. (1)-(4); adopted from M26, not derived here; central to the unequal-time correlation.
  • domain assumption Per-halo bursty fluctuations are independent of environment and of the large-scale density field
    Sec. III; implies zero burst-shot-noise cross-correlation with density (Eq. 20); ignores coherent environmental bursts.
  • domain assumption Lyα and X-ray luminosities are instantaneously proportional to the SFR at emission time
    Sec. IV; neglects finite stellar lifetimes and X-ray delays; authors note this would suppress large-scale burstiness (Sec. VI.E).
  • domain assumption No halo mergers or displacement over the burst timescale; HMF anchored at z_ref = max(z1,z2)
    Sec. III.A; authors state the formulation is an upper bound on cross-redshift correlation strength.
  • domain assumption M26 burstiness parameters apply at z ~ 10-25 and to halos below the calibrated mass range
    Sec. II; flagged by the authors as a 'key and potentially vulnerable assumption'.
  • domain assumption Only PopII stars in atomic-cooling galaxies contribute; MCGs/PopIII are excluded
    Secs. I and VI.E; if MCGs are bursty, the results could differ substantially.
  • domain assumption Mean-anchored lognormal convention (subtract σ_x²/2 in Eq. 1)
    This convention makes the mean SFRD, and hence the global T_21(z), unchanged by burstiness; a different anchoring would change the global signal.
  • standard math Lognormal moment-generating identity and OU covariance formula
    Appendix A, Eqs. (A2)-(A4); standard Gaussian statistics.

pith-pipeline@v1.3.0-alltime-deepseek · 31249 in / 18654 out tokens · 150547 ms · 2026-08-01T09:43:53.671416+00:00 · methodology

0 comments
read the original abstract

Recent JWST observations suggest that star formation in the early universe was substantially burstier than assumed in standard models. Such burstiness can be described as a stochastic process characterized by the burst amplitude and the coherence time of star formation epochs. In this paper, we investigate how bursty star formation modifies the 21-cm power spectrum during Cosmic Dawn through its impact on the non-local radiation fields that govern its evolution, namely Lyman-$\alpha$ and X-ray backgrounds. To do so, we introduce an unequal-time correlation in the star-formation-rate density sourcing the two fields and we compute its impact using the analytical framework implemented in the public code Zeus21. We find that the burstiness-induced time correlation produces a shot-noise-like contribution in the Lyman-$\alpha$ and X-ray fields, enhancing both their auto- and cross-power spectra while leaving the global 21-cm signal, $T_{21}(z)$, unchanged. As a result, the 21-cm power spectrum is strongly modified by a shot-noise-like contribution at the beginning of the Cosmic Dawn, where the signal is dominated by lower-mass halos ($M_h\lesssim10^{10}\,M_\odot$), and is boosted by a factor of a few near the Wouthuysen-Field absorption trough. Elsewhere at low redshift, where the clustering signal dominates and larger halos drive the signal, the burstiness component is negligible.

Figures

Figures reproduced from arXiv: 2607.20651 by Eleonora Vanzan, Ely D. Kovetz, Hovav Lazare, Julian B. Mu\~noz, Sarah Libanore.

Figure 1
Figure 1. Figure 1: FIG. 1. Halo-mass dependence of the burstiness amplitude [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Illustration of the unequal-time correlation in our [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3 [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p009_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Impact of burstiness on the 21-cm power spectrum across Cosmic Dawn. The [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6 [PITH_FULL_IMAGE:figures/full_fig_p012_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. The ratio of the total 21-cm power-spectrum with [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8 [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗

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Reference graph

Works this paper leans on

99 extracted references · 75 linked inside Pith

  1. [1]

    The brightest galaxies at cosmic dawn,

    C. A. Mason, M. Trenti and T. Treu, “The brightest galaxies at cosmic dawn,” Mon. Not. Roy. Astron. Soc. 521(2023) no.1, 497-503 [arXiv:2207.14808]

    Pith/arXiv arXiv 2023

  2. [2]

    and shell radii (R 1, R2). Summing over past red- shifts and shells, we obtain that the X-ray power spec- trum reads as P shot TX (z, k) = X z′ 1,z′ 2≥z c1,X (z′ 1)c1,X (z′ 2) X R1,R2 ∆R2 ×c 2,X (R1, z′ 1)c 2,X (R2, z′

  3. [3]

    (17), but with two emission red- shifts per shell-pair rather than one

    ˆWR1 (k) ˆWR2 (k) ×P shot ˙ρ∗ (k;t(z ′ 1, R1), t(z′ 2, R2)).(19) The previous equation contains the same shell-pair as the Lyαkernel of Eq. (17), but with two emission red- shifts per shell-pair rather than one. In this way, the 4D-correlated kernel allows us to account for coherent contributions to the heating rate of the same halo at fixed comoving posi...

    2018

  4. [4]

    A Comprehensive Study of Galaxies at z∼9–16 Found in the Early JWST Data: Ultraviolet Luminosity Func- tions and Cosmic Star Formation History at the Pre- reionization Epoch,

    Y. Harikane, M. Ouchi, M. Oguri, Y. Ono, K. Naka- jima, Y. Isobe, H. Umeda, K. Mawatari and Y. Zhang, “A Comprehensive Study of Galaxies at z∼9–16 Found in the Early JWST Data: Ultraviolet Luminosity Func- tions and Cosmic Star Formation History at the Pre- reionization Epoch,” Astrophys. J. Suppl.265(2023) no.1, 5 [arXiv:2208.01612]

    Pith/arXiv arXiv 2023

  5. [5]

    The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies atz∼8.5–14.5

    S.L. Finkelstein, et al., “The Complete CEERS Early Universe Galaxy Sample: A Surprisingly Slow Evolution of the Space Density of Bright Galaxies atz∼8.5–14.5”, The Astrophysical Journal Letters969(2024) no.1, L2 [arXiv:2311.04279]

    Pith/arXiv arXiv 2024

  6. [6]

    C. T. Donnan, et al., Mon. Not. Roy. Astron. Soc.533 (2024) no.3, 3222-3237 [arXiv:2403.03171] 17

    Pith/arXiv arXiv 2024

  7. [7]

    Earliest Galax- ies in the JADES Origins Field: Luminosity Function and Cosmic Star Formation Rate Density 300 Myr af- ter the Big Bang,

    B. Robertson, B. D. Johnson, S. Tacchella, D. J. Eisen- stein, K. Hainline, S. Arribas, W. M. Baker, A. J. Bunker, S. Carniani and P. A. Cargile,et al.“Earliest Galax- ies in the JADES Origins Field: Luminosity Function and Cosmic Star Formation Rate Density 300 Myr af- ter the Big Bang,” Astrophys. J.970(2024) no.1, 31 [arXiv:2312.10033]

    arXiv 2024

  8. [8]

    Bursty Star Formation Naturally Explains the Abundance of Bright Galaxies at Cosmic Dawn,

    G. Sun, C. A. Faucher-Gigu` ere, C. C. Hayward, X. Shen, A. Wetzel and R. K. Cochrane, “Bursty Star Formation Naturally Explains the Abundance of Bright Galaxies at Cosmic Dawn,” Astrophys. J. Lett.955(2023) no.2, L35 [arXiv:2307.15305]

    Pith/arXiv arXiv 2023

  9. [9]

    Identification and properties of intense star-forming galaxies at red- shifts z>10,

    B. E. Robertson, S. Tacchella, B. D. Johnson, K. Hain- line, L. Whitler, D. J. Eisenstein, R. Endsley, M. Rieke, D. P. Stark and S. Alberts,et al.“Identification and properties of intense star-forming galaxies at red- shifts z>10,” Nature Astron.7(2023) no.5, 611-621 [arXiv:2212.04480]

    arXiv 2023

  10. [10]

    Stochastic star forma- tion in early galaxies: Implications for the James Webb Space Telescope,

    A. Pallottini and A. Ferrara, “Stochastic star forma- tion in early galaxies: Implications for the James Webb Space Telescope,” Astron. Astrophys.677(2023), L4 [arXiv:2307.03219]

    Pith/arXiv arXiv 2023

  11. [11]

    Balancing the ef- ficiency and stochasticity of star formation with dust extinction inz≳10 galaxies observed by JWST,

    J. Mirocha and S. R. Furlanetto, “Balancing the ef- ficiency and stochasticity of star formation with dust extinction inz≳10 galaxies observed by JWST,” Mon. Not. Roy. Astron. Soc.519(2022) no.1, 843-853 [arXiv:2208.12826]

    Pith/arXiv arXiv 2022

  12. [12]

    (Star)bursts of FIRE: observa- tional signatures of bursty star formation in galaxies

    M. Sparre, et al. “(Star)bursts of FIRE: observa- tional signatures of bursty star formation in galaxies”, Mon. Not. Roy. Astron. Soc.466(2017) no.1, 88-104 [arXiv:1510.03869]

    Pith/arXiv arXiv 2017

  13. [13]

    A Model for the Origin of Bursty Star Formation in Galaxies,

    C. A. Faucher-Giguere, “A Model for the Origin of Bursty Star Formation in Galaxies,” Mon. Not. Roy. Astron. Soc.473(2018) no.3, 3717-3731 [arXiv:1701.04824]

    Pith/arXiv arXiv 2018

  14. [14]

    Bursty star formation during the Cosmic Dawn driven by delayed stellar feedback Free

    “Bursty star formation during the Cosmic Dawn driven by delayed stellar feedback Free”, Mon. Not. Roy. Astron. Soc.511(2022) no.3, 3895–3909 [arXiv:2109.04488]

    Pith/arXiv arXiv 2022

  15. [15]

    Seen and unseen: bursty star for- mation and its implications for observations of high- redshift galaxies with JWST,

    G. Sun, et al., “Seen and unseen: bursty star for- mation and its implications for observations of high- redshift galaxies with JWST,” arXiv:2305.02713 (2023) [arXiv:2305.02713]

    Pith/arXiv arXiv 2023

  16. [16]

    The Star-forming Main Sequence in JADES and CEERS atz >1.4: Investigating the Bursti- ness of Star Formation

    L. Clarke, et al. “The Star-forming Main Sequence in JADES and CEERS atz >1.4: Investigating the Bursti- ness of Star Formation”, The Astrophysical Journal,977 (2024), n.1, 133 [arXiv:2406.05178]

    Pith/arXiv arXiv 2024

  17. [17]

    The star-forming and ionizing prop- erties of dwarf z 6-9 galaxies in JADES: insights on bursty star formation and ionized bubble growth

    R. Endsley, et al. “The star-forming and ionizing prop- erties of dwarf z 6-9 galaxies in JADES: insights on bursty star formation and ionized bubble growth”, Mon. Not. Roy. Astron. Soc.533(2024) no.1, 1111-1142 [arXiv:2306.05295]

    Pith/arXiv arXiv 2024

  18. [18]

    Constraining bursty star formation histories with galaxy UV and Hαluminosity functions and clus- tering,

    G. Sun, J. B. Mu˜ noz, J. Mirocha and C. A. Faucher- Gigu` ere, “Constraining bursty star formation histories with galaxy UV and Hαluminosity functions and clus- tering,” JCAP04(2025), 034

    2025

  19. [19]

    Relatively Fast and Reasonably Furious: Evidence for Increased Burstiness in Smaller Halos at Cosmic Dawn,

    J. B. Mu˜ noz, J. Chisholm, G. Sun, J. Samuel, J. Mirocha, E. Bregou, A. Venditti, M. Qezlou, C. Simmonds and R. Endsley, “Relatively Fast and Reasonably Furious: Evidence for Increased Burstiness in Smaller Halos at Cosmic Dawn,” [arXiv:2601.07912]

    Pith/arXiv arXiv

  20. [20]

    When galaxies burst: enhanced shot- noise for line-intensity mapping in the JWST era,

    E. D. Kovetz, H. Lazare, S. Libanore, J. B. Mu˜ noz and E. Vanzan, “When galaxies burst: enhanced shot- noise for line-intensity mapping in the JWST era,” [arXiv:2605.13967]

    Pith/arXiv arXiv

  21. [21]

    Line-Intensity Mapping: 2017 Status Report,

    E. D. Kovetz, M. P. Viero, A. Lidz, L. Newburgh, M. Rahman, E. Switzer, M. Kamionkowski, J. Aguirre, M. Alvarez and J. Bock,et al.“Line-Intensity Mapping: 2017 Status Report,” [arXiv:1709.09066]

    Pith/arXiv arXiv 2017

  22. [22]

    Line-intensity map- ping: theory review with a focus on star-formation lines,

    J. L. Bernal and E. D. Kovetz, “Line-intensity map- ping: theory review with a focus on star-formation lines,” Astron. Astrophys. Rev.30(2022) no.1, 5 [arXiv:2206.15377]

    Pith/arXiv arXiv 2022

  23. [23]

    Line-Intensity Mapping,

    T. C. Chang and A. Lidz, “Line-Intensity Mapping,” [arXiv:2602.03011]

    arXiv

  24. [24]

    Effects of Bursty Star Formation on [C ii] Line Intensity Mapping of High-redshift Galaxies,

    L. J. Liu, G. Sun, T. C. Chang, S. R. Furlanetto and C. M. Bradford, “Effects of Bursty Star Formation on [C ii] Line Intensity Mapping of High-redshift Galaxies,” Astrophys. J.974(2024) no.2, 175 [arXiv:2401.04204]

    Pith/arXiv arXiv 2024

  25. [25]

    The First Galaxies in the Universe

    A. Loeb and S. R. Furlanetto, “The First Galaxies in the Universe”, Princeton University Press, Princeton, NJ (2013)

    2013

  26. [26]

    21-cm cosmology,

    J. R. Pritchard and A. Loeb, “21-cm cosmology,” Rept. Prog. Phys.75(2012), 086901 [arXiv:1109.6012]

    Pith/arXiv arXiv 2012

  27. [27]

    21-CM tomogra- phy of the intergalactic medium at high redshift,

    P. Madau, A. Meiksin and M. J. Rees, “21-CM tomogra- phy of the intergalactic medium at high redshift,” Astro- phys. J.475, 429 (1997) [arXiv:astro-ph/9608010 [astro- ph]]

    Pith/arXiv arXiv 1997

  28. [28]

    Measuring the small - scale power spectrum of cosmic density fluctuations through 21 cm tomography prior to the epoch of structure forma- tion,

    A. Loeb and M. Zaldarriaga, “Measuring the small - scale power spectrum of cosmic density fluctuations through 21 cm tomography prior to the epoch of structure forma- tion,” Phys. Rev. Lett.92, 211301 (2004) [arXiv:astro- ph/0312134 [astro-ph]]

    arXiv 2004

  29. [29]

    What Next-Generation 21 cm Power Spectrum Measurements Can Teach Us About the Epoch of Reionization,

    J. C. Pober, A. Liu, J. S. Dillon, J. E. Aguirre, J. D. Bow- man, R. F. Bradley, C. L. Carilli, D. R. DeBoer, J. N. He- witt and D. C. Jacobs,et al.“What Next-Generation 21 cm Power Spectrum Measurements Can Teach Us About the Epoch of Reionization,” Astrophys. J.782, 66 (2014) [arXiv:1310.7031]

    Pith/arXiv arXiv 2014

  30. [30]

    Snowmass2021 Cosmic Frontier White Paper: 21cm Radiation as a Probe of Physics Across Cosmic Ages,

    A. Liuet al.[Snowmass 2021 Cosmic Frontier 5 Topical Group], “Snowmass2021 Cosmic Frontier White Paper: 21cm Radiation as a Probe of Physics Across Cosmic Ages,” [arXiv:2203.07864]

    Pith/arXiv arXiv 2021

  31. [31]

    Cosmology at Low Frequencies: The 21 cm Transition and the High-Redshift Universe,

    S. Furlanetto, S. P. Oh and F. Briggs, “Cosmology at Low Frequencies: The 21 cm Transition and the High-Redshift Universe,” Phys. Rept.433(2006), 181-301 [arXiv:astro- ph/0608032 [astro-ph]]

    arXiv 2006

  32. [32]

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

    S. Libanore, J. Flitter, E. D. Kovetz, Z. Li and A. Dekel, “Effects of feedback-free starburst galaxies on the 21-cm signal and reionization history,” Mon. Not. Roy. Astron. Soc.532, no.1, 149-163 (2024) [erratum: Mon. Not. Roy. Astron. Soc.543, no.1, 772 (2025)] [arXiv:2310.03021]

    Pith/arXiv arXiv 2024

  33. [33]

    JWST Con- straints on the UV Luminosity Density at Cosmic Dawn: Implications for 21 cm Cosmology,

    S. Hassan, C. C. Lovell, P. Madau, M. Huertas-Company, R. S. Somerville, B. Burkhart, K. L. Dixon, R. Feldmann, T. K. Starkenburg and J. F. Wu,et al.“JWST Con- straints on the UV Luminosity Density at Cosmic Dawn: Implications for 21 cm Cosmology,” Astrophys. J. Lett. 958, no.1, L3 (2023) [arXiv:2305.02703]

    Pith/arXiv arXiv 2023

  34. [34]

    Exploiting synergies between JWST and cosmic 21-cm observations to uncover star formation in the early Universe,

    J. Dhandha, A. Fialkov, T. Gessey-Jones, H. T. J. Bevins, S. Tacchella, S. Pochinda, E. d. Acedo, S. Singh and R. Barkana, “Exploiting synergies between JWST and cosmic 21-cm observations to uncover star formation in the early Universe,” Mon. Not. Roy. Astron. Soc.542, no.3, 2292-2322 (2025) [arXiv:2503.21687]

    Pith/arXiv arXiv 2025

  35. [35]

    On the excitation mechanism of the 21-cm (radio-frequency) interstellar hydrogen emission line.,

    S. A. Wouthuysen, “On the excitation mechanism of the 21-cm (radio-frequency) interstellar hydrogen emission line.,” Astronomical Journal57, 31-32 (1952)

    1952

  36. [36]

    The Spin Temperature of Intergalactic Neu- tral Hydrogen.,

    G. B. Field, “The Spin Temperature of Intergalactic Neu- tral Hydrogen.,” Astrophysical Journal129, 536 (1959)

    1959

  37. [37]

    Wouthuysen-Field coupling strength and 18 application to high-redshift 21 cm radiation,

    C. M. Hirata, “Wouthuysen-Field coupling strength and 18 application to high-redshift 21 cm radiation,” Mon. Not. Roy. Astron. Soc.367, 259–274 (2006) [arXiv:astro- ph/0507102]

    arXiv 2006

  38. [38]

    Descending from on high: lyman series cascades and spin-kinetic temperature coupling in the 21 cm line,

    J. R. Pritchard and S. R. Furlanetto, “Descending from on high: lyman series cascades and spin-kinetic temperature coupling in the 21 cm line,” Mon. Not. Roy. Astron. Soc.367, 1057-1066 (2006) [arXiv:astro- ph/0508381 [astro-ph]]

    arXiv 2006

  39. [39]

    Radiation Backgrounds at Cosmic Dawn: X-Rays from Compact Binaries,

    P. Madau and T. Fragos, “Radiation Backgrounds at Cosmic Dawn: X-Rays from Compact Binaries,” Astro- phys. J.840(2017) no.1, 39 [arXiv:1606.07887]

    Pith/arXiv arXiv 2017

  40. [40]

    21 cm fluctua- tions from inhomogeneous X-ray heating before reion- ization,

    J. R. Pritchard and S. R. Furlanetto, “21 cm fluctua- tions from inhomogeneous X-ray heating before reion- ization,” Mon. Not. Roy. Astron. Soc.376, 1680–1694 (2007) [arXiv:astro-ph/0607234]

    Pith/arXiv arXiv 2007

  41. [41]

    Signatures of X-rays in the early Universe,

    A. Mesinger, A. Ferrara and D. S. Spiegel, “Signatures of X-rays in the early Universe,” Mon. Not. Roy. Astron. Soc.431(2013), 621 [arXiv:1210.7319]

    Pith/arXiv arXiv 2013

  42. [42]

    The X-ray spectra of the first galaxies: 21 cm signatures,

    F. Pacucci, A. Mesinger, S. Mineo and A. Ferrara, “The X-ray spectra of the first galaxies: 21 cm signatures,” Mon. Not. Roy. Astron. Soc.443(2014) no.1, 678-686 [arXiv:1403.6125]

    Pith/arXiv arXiv 2014

  43. [43]

    The observable signature of late heating of the Universe during cosmic reionization,

    A. Fialkov, R. Barkana and E. Visbal, “The observable signature of late heating of the Universe during cosmic reionization,” Nature506(2014), 197 [arXiv:1402.0940]

    Pith/arXiv arXiv 2014

  44. [44]

    Unequal-Time Cor- relators for Cosmology,

    T. D. Kitching and A. F. Heavens, “Unequal-Time Cor- relators for Cosmology,” Phys. Rev. D95, no.6, 063522 (2017) [arXiv:1612.00770]

    Pith/arXiv arXiv 2017

  45. [45]

    Power spectrum in the cave,

    A. Raccanelli and Z. Vlah, “Power spectrum in the cave,” [arXiv:2305.16278]

    Pith/arXiv arXiv

  46. [46]

    Observed unequal-time power spec- trum,

    F. Spezzati, E. Vanzan, A. Raccanelli, Z. Vlah and D. Bertacca, “Observed unequal-time power spec- trum,” Phys. Rev. D112, no.2, 023530 (2025) [arXiv:2503.09759]

    Pith/arXiv arXiv 2025

  47. [47]

    The unequal- time matter power spectrum: impact on weak lensing observables,

    L. F. de la Bella, N. Tessore and S. Bridle, “The unequal- time matter power spectrum: impact on weak lensing observables,” JCAP08, 001 (2021) [arXiv:2011.06185]

    Pith/arXiv arXiv 2021

  48. [48]

    Unequal time correlators and the Zel’dovich approximation,

    N. E. Chisari and A. Pontzen, “Unequal time correlators and the Zel’dovich approximation,” Phys. Rev. D100, no.2, 023543 (2019) [arXiv:1905.02078]

    Pith/arXiv arXiv 2019

  49. [49]

    The multi-frequency angular power spectrum of the epoch of reionization 21 cm signal,

    K. K. Datta, T. R. Choudhury and S. Bharadwaj, “The multi-frequency angular power spectrum of the epoch of reionization 21 cm signal,” Mon. Not. Roy. Astron. Soc. 378, 119-128 (2007) [arXiv:astro-ph/0605546 [astro-ph]]

    Pith/arXiv arXiv 2007

  50. [50]

    The Evolving Power Spectrum for the Light Cone Epoch of Reionization 21 cm Signal,

    S. Pramanick, S. Bharadwaj, K. M. A. Elahi and R. Mon- dal, “The Evolving Power Spectrum for the Light Cone Epoch of Reionization 21 cm Signal,” Astrophys. J.984, no.2, 105 (2025) [arXiv:2503.21499]

    Pith/arXiv arXiv 2025

  51. [51]

    Beyond the power spectrum: A new framework for nonstationary fields with appli- cations to light-cone effects in line intensity mapping,

    M. Blamart and A. Liu, “Beyond the power spectrum: A new framework for nonstationary fields with appli- cations to light-cone effects in line intensity mapping,” Phys. Rev. D113, no.6, 6 (2026) [arXiv:2505.09674]

    Pith/arXiv arXiv 2026

  52. [52]

    Time-dependent fluctu- ations in the metagalactic photoionization background,

    A. Meiksin and M. McQuinn, “Time-dependent fluctu- ations in the metagalactic photoionization background,” Mon. Not. Roy. Astron. Soc.482, no.4, 4777-4797 (2019) [arXiv:1809.08645]

    Pith/arXiv arXiv 2019

  53. [53]

    Shot noise and scat- ter in the star formation efficiency as a source of 21-cm fluctuations,

    I. Reis, R. Barkana and A. Fialkov, “Shot noise and scat- ter in the star formation efficiency as a source of 21-cm fluctuations,” Mon. Not. Roy. Astron. Soc.511, no.4, 5265-5273 (2022) [arXiv:2106.13111]

    Pith/arXiv arXiv 2022

  54. [54]

    Efficient simulation of discrete galaxy populations and associated radiation fields over the first billion years,

    J. E. Davies, A. Mesinger and S. G. Murray, “Efficient simulation of discrete galaxy populations and associated radiation fields over the first billion years,” Astron. As- trophys.701, A236 (2025) [arXiv:2504.17254]

    arXiv 2025

  55. [55]

    21cmF AST: A Fast, Semi-Numerical Simulation of the High-Redshift 21-cm Signal,

    A. Mesinger, S. Furlanetto and R. Cen, “21cmF AST: A Fast, Semi-Numerical Simulation of the High-Redshift 21-cm Signal,” Mon. Not. Roy. Astron. Soc.411, 955 (2011) [arXiv:1003.3878]

    Pith/arXiv arXiv 2011

  56. [56]

    21cmF AST v3: A Python-integrated C code for generating 3D realiza- tions of the cosmic 21cm signal,

    S. G. Murray, B. Greig, A. Mesinger, J. B. Mu˜ noz, Y. Qin, J. Park and C. A. Watkinson, “21cmF AST v3: A Python-integrated C code for generating 3D realiza- tions of the cosmic 21cm signal,” J. Open Source Softw. 5, no.54, 2582 (2020) [arXiv:2010.15121]

    Pith/arXiv arXiv 2020

  57. [57]

    The impact of the first galaxies on cos- mic dawn and reionization,

    J. B. Mu˜ noz, Y. Qin, A. Mesinger, S. G. Murray, B. Greig and C. Mason, “The impact of the first galaxies on cos- mic dawn and reionization,” Mon. Not. Roy. Astron. Soc. 511, no.3, 3657-3681 (2022) [arXiv:2110.13919]

    Pith/arXiv arXiv 2022

  58. [58]

    Dark-ages Reionization and Galaxy formation simula- tion – I. The dynamical lives of high-redshift galaxies,

    G. B. Poole, P. W. Angel, S. J. Mutch, C. Power, A. R. Duffy, P. M. Geil, A. Mesinger and S. B. Wyithe, “Dark-ages Reionization and Galaxy formation simula- tion – I. The dynamical lives of high-redshift galaxies,” Mon. Not. Roy. Astron. Soc.459, no.3, 3025-3039 (2016) [arXiv:1512.00559]

    Pith/arXiv arXiv 2016

  59. [59]

    Dark- ages reionization and galaxy formation simulation – III. Modelling galaxy formation and the epoch of reioniza- tion,

    S. J. Mutch, P. M. Geil, G. B. Poole, P. W. Angel, A. R. Duffy, A. Mesinger and J. S. B. Wyithe, “Dark- ages reionization and galaxy formation simulation – III. Modelling galaxy formation and the epoch of reioniza- tion,” Mon. Not. Roy. Astron. Soc.462, no.1, 250-276 (2016) [arXiv:1603.04848]

    Pith/arXiv arXiv 2016

  60. [60]

    Thermal and reionization his- tory within a large-volume semi-analytic galaxy forma- tion simulation,

    S. Balu, B. Greig, Y. Qiu, C. Power, Y. Qin, S. Mutch and J. S. B. Wyithe, “Thermal and reionization his- tory within a large-volume semi-analytic galaxy forma- tion simulation,” Mon. Not. Roy. Astron. Soc.520, no.3, 3368-3382 (2023) [arXiv:2210.08910]

    Pith/arXiv arXiv 2023

  61. [61]

    An effective model for the cosmic-dawn 21-cm signal,

    J. B. Mu˜ noz, “An effective model for the cosmic-dawn 21-cm signal,” Mon. Not. Roy. Astron. Soc.523, no.2, 2587–2607 (2023) [arXiv:2302.08506]

    Pith/arXiv arXiv 2023

  62. [62]

    Effective model for the 21-cm sig- nal with population III stars,

    H. A. G. Cruz, J. B. Munoz, N. Sabti and M. Kamionkowski, “Effective model for the 21-cm sig- nal with population III stars,” Phys. Rev. D111(2025) no.8, 8 [arXiv:2407.18294]

    Pith/arXiv arXiv 2025

  63. [63]

    Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era,

    A. Venditti, J. B. Munoz, V. Bromm, S. Fujimoto, S. L. Finkelstein and J. Chisholm, “Bursty or Heavy? The Surprise of Bright Population III Systems in the Reionization Era,” Astrophys. J.994, no.1, 32 (2025) [arXiv:2505.20263 [astro-ph.GA]]

    arXiv 2025

  64. [64]

    Hydrogen Epoch of Reionization Array (HERA),

    D. R. DeBoer, A. R. Parsons, J. E. Aguirre, P. Alexander, Z. S. Ali, A. P. Beardsley, G. Bernardi, J. D. Bowman, R. F. Bradley and C. L. Carilli,et al.“Hydrogen Epoch of Reionization Array (HERA),” Publ. Astron. Soc. Pac. 129, no.974, 045001 (2017) [arXiv:1606.07473]

    Pith/arXiv arXiv 2017

  65. [65]

    First Results from HERA Phase I: Upper Limits on the Epoch of Reioniza- tion 21 cm Power Spectrum,

    Z. Abdurashidovaet al.[HERA], “First Results from HERA Phase I: Upper Limits on the Epoch of Reioniza- tion 21 cm Power Spectrum,” Astrophys. J.925, no.2, 221 (2022) [arXiv:2108.02263]

    Pith/arXiv arXiv 2022

  66. [66]

    Improved Constraints on the 21 cm EoR Power Spectrum and the X-Ray Heat- ing of the IGM with HERA Phase I Observations,

    Z. Abdurashidovaet al.[HERA], “Improved Constraints on the 21 cm EoR Power Spectrum and the X-Ray Heat- ing of the IGM with HERA Phase I Observations,” As- trophys. J.945, no.2, 124 (2023) [arXiv:2210.04912]

    Pith/arXiv arXiv 2023

  67. [67]

    LOF AR: The LOw- Frequency ARray,

    M. P. van Haarlemet al.[LOF AR], “LOF AR: The LOw- Frequency ARray,” Astron. Astrophys.556, A2 (2013) [arXiv:1305.3550]

    Pith/arXiv arXiv 2013

  68. [68]

    Im- proved upper limits on the 21-cm signal power spec- trum of neutral hydrogen atz≈9.1from LOF AR,

    F. G. Mertens, M. Mevius, L. V. E. Koopmans, A. R. Of- fringa, G. Mellema, S. Zaroubi, M. A. Brentjens, H. Gan, B. K. Gehlot and V. N. Pandey,et al.“Im- proved upper limits on the 21-cm signal power spec- trum of neutral hydrogen atz≈9.1from LOF AR,” Mon. Not. Roy. Astron. Soc.493, no.2, 1662-1685 (2020) 19 [arXiv:2002.07196]

    Pith/arXiv arXiv 2020

  69. [69]

    First upper limits on the 21-cm signal power spectrum of neutral hydrogen atz= 9.16 from the LOF AR 3C196 field,

    E. Ceccotti, A. R. Offringa, F. G. Mertens, L. V. E. Koopmans, S. Munshi, J. K. Chege, A. Acharya, S. A. Brackenhoff, E. Chapman and B. Ciardi,et al. “First upper limits on the 21-cm signal power spectrum of neutral hydrogen atz= 9.16 from the LOF AR 3C196 field,” [arXiv:2504.18534]

    arXiv

  70. [70]

    An absorption profile centred at 78 megahertz in the sky-averaged spectrum,

    J. D. Bowman, A. E. E. Rogers, R. A. Monsalve, T. J. Mozdzen and N. Mahesh, “An absorption profile centred at 78 megahertz in the sky-averaged spectrum,” Nature555, no.7694, 67–70 (2018) [arXiv:1810.05912]

    Pith/arXiv arXiv 2018

  71. [71]

    On the detection of a cosmic dawn signal in the radio back- ground,

    S. Singh, J. Nambissan T., R. Subrahmanyan, N. Udaya Shankar, B. S. Girish, A. Raghunathan, R. Somashekar, K. S. Srivani and M. Sathyanarayana Rao, “On the detection of a cosmic dawn signal in the radio back- ground,” Nature Astron.6, no.5, 607–617 (2022) [arXiv:2112.06778]

    Pith/arXiv arXiv 2022

  72. [72]

    On the Theory of the Brownian Motion,

    G. E. Uhlenbeck and L. S. Ornstein, “On the Theory of the Brownian Motion,” Phys. Rev.36, 823–841 (1930)

    1930

  73. [73]

    Stochastic modelling of star- formation histories I: the scatter of the star-forming main sequence,

    N. Caplar and S. Tacchella, “Stochastic modelling of star- formation histories I: the scatter of the star-forming main sequence,” Monthly Notices of the Royal Astronomical Society487, no.3, 3845-3869 (2019)

    2019

  74. [74]

    The Impact of cold gas accretion above a mass floor on galaxy scaling relations,

    N. Bouche, A. Dekel, R. Genzel, S. Genel, G. Cresci, N. M. Forster Schreiber, K. L. Shapiro, R. I. Davies and L. Tacconi, “The Impact of cold gas accretion above a mass floor on galaxy scaling relations,” Astrophys. J. 718, no.2, 1001–1018 (2010) [arXiv:0912.1858]

    Pith/arXiv arXiv 2010

  75. [75]

    An analytic model for the evolution of the stellar, gas and metal content of galaxies,

    R. Dav´ e, K. Finlator and B. D. Oppenheimer, “An analytic model for the evolution of the stellar, gas and metal content of galaxies,” Monthly Notices of the Royal Astronomical Society421, no.1, 98-107 (2012) [arXiv:1108.0426]

    Pith/arXiv arXiv 2012

  76. [76]

    Halo Models of Large Scale Structure,

    A. Cooray and R. K. Sheth, “Halo Models of Large Scale Structure,” Phys. Rept.372, 1-129 (2002) [arXiv:astro- ph/0206508 [astro-ph]]

    arXiv 2002

  77. [77]

    Multi-tracer intensity map- ping: Cross-correlations, Line noise & Decorrelation,

    E. Schaan and M. White, “Multi-tracer intensity map- ping: Cross-correlations, Line noise & Decorrelation,” JCAP05, 068 (2021) [arXiv:2103.01964]

    Pith/arXiv arXiv 2021

  78. [78]

    Halo model approach for the 21-cm power spectrum at cos- mic dawn,

    A. Schneider, S. K. Giri and J. Mirocha, “Halo model approach for the 21-cm power spectrum at cos- mic dawn,” Phys. Rev. D103, no.8, 083025 (2021) [arXiv:2011.12308]

    Pith/arXiv arXiv 2021

  79. [79]

    Toy Models for Galaxy For- mation versus Simulations,

    A. Dekel, A. Zolotov, D. Tweed, M. Cacciato, D. Cev- erino and J. R. Primack, “Toy Models for Galaxy For- mation versus Simulations,” Mon. Not. Roy. Astron. Soc. 435, 999 (2013) [arXiv:1303.3009]

    Pith/arXiv arXiv 2013

  80. [80]

    Detecting the earliest galaxies through two new sources of 21cm fluctuations,

    R. Barkana and A. Loeb, “Detecting the earliest galaxies through two new sources of 21cm fluctuations,” Astro- phys. J.626, 1-11 (2005) [arXiv:astro-ph/0410129 [astro- ph]]

    Pith/arXiv arXiv 2005

Showing first 80 references.