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Towards a multi-tracer neutrino mass measurement with line-intensity mapping

T0 review · 3 major / 4 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read A multi-tracer forecast combining [CII] line-intensity maps with CMB-S4 and DESI-BAO reaches 18 meV sensitivity on the summed neutrino mass, and with a 21-cm reionization prior it crosses the 5σ threshold for the 60 meV normal-hierarchy…

desk verdict A clean, well-documented Fisher forecast for neutrino masses with LIM; the headline 5-sigma claim leans on a self-cited 21-cm tau prior, but the no-prior 18 meV result is the solid core. read the letter →

arxiv 2412.04071 v1 pith:HLABSFXD submitted 2024-12-05 astro-ph.CO

Gali Shmueli , Sarah Libanore , Ely D. Kovetz This is my paper · ORCID
classification astro-ph.CO PACS 98.80.Es14.60.Pq
keywords neutrinomasssumline-intensitymapping[CII]158micronlineFisherforecastvelocitytomographykineticSunyaev-Zeldovicheffectmovinglensopticaldepthtoreionization
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper asks whether line-intensity mapping — collecting the total spectral-line glow of unresolved galaxies instead of cataloguing individual ones — can move cosmology toward a measurement of the absolute neutrino-mass scale. Its central claim is a forecasted sensitivity ladder: the future AtLAST [CII] survey alone reaches $\sigma(\sum m_\nu) \approx 50$ meV from its clustering power spectrum, and combining that signal with velocity tomography, CMB-S4, and DESI-BAO forecasts yields $\sigma(\sum m_\nu) \approx 18$ meV without any external prior on the reionization optical depth $\tau$. Adding a $\tau$ prior derived from forecasted 21-cm observations tightens the sensitivity to $\sim 11.5$ meV, which would be a $\gtrsim 5\sigma$ detection of the 60 meV mass sum that is the minimum of the normal neutrino hierarchy. If the forecast holds, line-intensity mapping becomes a standalone route to the neutrino-mass measurement at redshifts ($z \approx 1$–$8$) largely beyond the reach of galaxy surveys, while a secondary result is that kinetic Sunyaev–Zel'dovich and moving-lens velocity reconstruction improves the LIM-only number by only a few percent and adds almost nothing once CMB and BAO data are included.

What carries the argument

The argument runs on a Fisher-matrix forecast (Eq. 37) whose signal covariance couples three observables: the [CII] intensity power spectrum built from a halo model with a luminosity–mass relation (Eqs. 8–15), and the radial and transverse components of a reconstructed three-dimensional velocity field. The radial velocity comes from kinetic Sunyaev–Zel'dovich tomography — the CMB temperature shift from photons scattering off the bulk motion of free electrons — whose reconstruction noise follows from a squeezed-bispectrum estimator, a three-point statistic dominated by one long-wavelength mode (Eq. 27). The transverse velocity comes from the moving-lens effect, the temperature pattern imprinted by time-varying gravitational potentials of moving structures, with noise propagated from a reconstructed gravitational-potential field (Eq. 31). Massive neutrinos enter through the scale-dependent growth rate $f(k,z)$ in the linear velocity–density relation $v(k) \propto (f a H/k)\,\delta(k)$ and through free-streaming suppression of the matter power spectrum on small scales. The degeneracy that blocks a CMB-only measurement — between $\tau$, the amplitude $A_s$, and $\sum m_\nu$ — is broken in the combination by the LIM auto-power spectrum and, for the strongest claim, by the external $\tau$ prior drawn from forecasted 21-cm observations.

What would settle it

Re-run the same Fisher pipeline with $\tau$ assigned its current measured level — Planck-era $\sigma(\tau)$ near 0.007–0.02, or the Planck low-$\ell$ EE-polarization covariance the paper says behaves like a 0.0075 prior — instead of the forecasted 21-cm prior; if $\sigma(\sum m_\nu)$ then lands above roughly 12 meV, the claimed $\gtrsim 5\sigma$ measurement of $\sum m_\nu = 60$ meV does not follow. A complementary check is to add a foreground-residual noise term to the CMB-S4 forecast on multipoles $\ell \lesssim 30$, where the current model is foreground-free.

Watch

Extended reading notes

Core claim

On its own terms the paper establishes a sensitivity ladder for [CII] line-intensity mapping. Current-generation instruments of the CCAT-prime type cannot meaningfully constrain the mass sum ($\sigma \approx 8$ eV); an intermediate reduced-AtLAST configuration forecasts $\sigma \approx 166$ meV, comparable to a ten-year VRO10 photometric survey; and the full AtLAST design reaches $\sigma \approx 50$ meV from the [CII] auto-power spectrum alone, improving by about 4% when the three-dimensional velocity field reconstructed from kSZ and moving-lens cross-correlations with CMB-S4 is added. Summing the Fisher matrices of AtLAST, CMB-S4, and DESI-BAO gives the paper's headline numbers: $\sigma(\sum m_\nu) \approx 18$ meV with no $\tau$ prior, and $\sigma \approx 11.5$ meV once the 21-cm-forecast $\tau$ prior is imposed — the configuration the authors associate with a $\gtrsim 5\sigma$ measurement of $\sum m_\nu = 60$ meV under the normal hierarchy. The paper further shows that velocity tomography inherits the CMB's $\tau$–$\sum m_\nu$ degeneracy: it helps the LIM-only forecast (up to about 11% with a 1% prior on the radial velocity bias $b_\parallel$) but contributes negligibly once CMB-S4 and BAO are combined in.

Load-bearing premise

The $\gtrsim 5\sigma$ claim rests on a $\tau$ prior that is itself a forecast from future 21-cm observations rather than a measurement (the analysis relies on it in Sec. IV C), and the CMB forecast in the analysis is computed without foregrounds, which the paper itself notes would act conservatively.

Editorial extensions

If this is right

  • An AtLAST-like [CII] survey alone constrains $\sum m_\nu$ at $\sigma \approx 50$ meV, enough to reject the inverted hierarchy at more than $2\sigma$ from LIM maps alone, while probing redshifts beyond the range of optical galaxy surveys.
  • The combined forecast reaches $\sigma(\sum m_\nu) \approx 18$ meV with no $\tau$ prior, well below the 0.072 eV 95% CL upper bound that the paper cites from Planck, ACT lensing, and DESI.
  • A $\tau$ prior from 21-cm observations converts the 18 meV constraint into an 11.5 meV one, crossing the $\gtrsim 5\sigma$ threshold on $\sum m_\nu = 60$ meV and making reionization-era 21-cm cosmology a necessary partner for the strongest neutrino-mass claim.
  • Velocity tomography is a small correction rather than the engine: about 4% at full AtLAST and up to about 11% at reduced-AtLAST with a 1% prior on $b_\parallel$, and nearly zero once CMB-S4 and BAO are included, so the kSZ and moving-lens channels mainly serve as cross-checks on the LIM auto-spectrum.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The same machinery transfers to other star-formation lines such as CO and [OIII]; because the constraining power rides on clustering and redshift coverage more than on the line's specific astrophysics, a multi-line Fisher combination is a natural extension that could push below the single-line 50 meV number — a step this paper does not take.
  • The $\gtrsim 5\sigma$ outcome may not need 21-cm cosmology: the paper notes that low-$\ell$ EE polarization gives constraints comparable to a 0.0075 prior on $\tau$, so whether an all-CMB route reaches the 11 meV regime depends on how tight a genuinely measured EE-based prior turns out to be.
  • The forecast restricts large-scale modes to $k \le 0.1\,\mathrm{Mpc}^{-1}$ and the velocity channel weakens if pixel noise grows, so a testable stress case is to push $k$ beyond 0.1 and lengthen observing time per voxel; this would reveal whether velocity tomography can ever become the leading term rather than a few-percent accessory.
  • The [CII] luminosity–halo mass relation is held fixed apart from its per-bin normalization, so varying its slope and scatter, or folding in line-formation uncertainties, is the most direct stress test of the 18 meV and 11.5 meV figures.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper presents Fisher-matrix forecasts for the sum of neutrino masses, Σmν, using [CII] line-intensity mapping, alone and combined with kinetic Sunyaev-Zel'dovich and moving-lens velocity tomography, CMB-S4, and DESI BAO forecasts. The authors report that AtLAST-like [CII] LIM alone reaches σΣmν ≈ 50 meV, that velocity tomography improves this by a few percent, and that the combination of AtLAST + CMB-S4 + DESI-BAO reaches σΣmν ≈ 18 meV without a τ prior. With a τ prior derived from forecasted 21-cm observations (Ref. [50]), they report σΣmν ≈ 11.5 meV, which they translate into a ≳5σ detection of the normal-hierarchy minimum Σmν = 60 meV. The analysis is clearly specified, the code is public, and the parameter set, noise models, and window functions are described in detail.

Significance. If the forecasts are robust, the paper makes a useful and timely contribution by showing that a next-generation [CII] LIM experiment can match or exceed current galaxy-survey forecasts for neutrino mass constraints, and by quantifying the marginal role of velocity tomography. The strengths include a clear Fisher framework with a public code, explicit treatment of the velocity-reconstruction noise from kSZ and moving-lens effects, and an honest presentation of the no-τ-prior result of 18 meV. The main caveat is that the headline 5σ statement depends on an external, projected τ prior rather than on the LIM data themselves, so the significance of the paper's central claim is sensitive to how that prior is framed and validated.

major comments (3)
  1. [Sec. IV C, Fig. 8, Abstract] The advertised ≳5σ sensitivity is not a LIM+CMB+BAO result but a LIM+CMB+BAO+τ(21-cm forecast) result. Without the τ prior the same combination gives σΣmν ≈ 18 meV, which for Σmν = 60 meV is only ≈3.3σ. The difference between this 3σ bound and the claimed 5σ detection is supplied almost entirely by a projected prior from Ref. [50], a forecast by the same first and last authors rather than a measured value. The paper should present the no-prior 18 meV constraint as the primary LIM-based forecast, clearly separate the 'with forecast τ prior' scenario in the abstract and conclusions, and show how σΣmν depends on the assumed prior width (e.g., a curve over σ(τ) ≈ 0.001–0.02) so the robustness of the 5σ claim can be judged.
  2. [Sec. II B and Sec. IV C] The CMB-S4 noise model in Eq. (2) omits foregrounds, and the paper states only that including them 'will amount to a more conservative approach, as shown in Ref. [94].' Because the combined constraints in Fig. 8 rely on CMB-S4's large-scale sensitivity to break the τ–Σmν degeneracy, the forecast should include a quantitative foreground treatment or at least a demonstration that a reasonable foreground-residual model does not shift the 18 meV and 11.5 meV numbers substantially. Citing Ref. [94] for this point is not a substitute for showing the sensitivity in the present analysis.
  3. [Sec. III C, Eq. (41), footnote 7] The parameter bRSD, which multiplies the f μ² term in c_X, is fixed to 1, whereas the companion galaxy-survey analysis in Ref. [94] marginalizes over it. Since the RSD term carries part of the neutrino-mass information, fixing bRSD can artificially tighten the forecasted constraints. The authors should marginalize over bRSD with a broad prior, or demonstrate explicitly that the quoted values (σΣmν ≈ 50 meV, 18 meV, and 11.5 meV) are insensitive to this choice.
minor comments (4)
  1. [References, Ref. [94]] Reference [94] is cited with the incomplete arXiv identifier 'arXiv:24xx.xxxx'; this placeholder must be replaced with a full reference or a preprint number before publication.
  2. [Abstract and Table III] The abstract says velocity tomography improves the AtLAST constraint by 4%, but Table III shows 51.0 meV → 50.0 meV with velocities alone (≈2%) and 51.0 meV → 49.0 meV with the additional 1% b∥ prior. The stated percentage should be reconciled with the table.
  3. [Sec. III B 1, Eq. (24)] The text refers to the 'Thompson cross-section'; the correct name is Thomson cross-section.
  4. [Sec. III A, Eq. (3)] The phrase 'kB the Boltzmann constant' lacks a space and a verb; it should read 'k_B is the Boltzmann constant' for clarity.

Circularity Check

1 steps flagged · score 4.0 of 10

Headline >5σ neutrino-mass sensitivity is prior-dominated by a self-cited 21-cm τ forecast; the no-prior 18 meV LIM+CMB+BAO result is independent.

  1. self citation load bearing [Sec. IV C (Combined results), Fig. 8; Abstract]
    "The right vertical line in the plot matches the conservative prior choice in Ref. [68], while the left vertical line indicates the prior computed in Ref. [50], using 21-cm forecasts to get a direct measurement of this parameter. We see that in this regime, LIM lowers the constraints from CMB+BAO all the way to σP mν ∼ 11 meV, which would yield a larger than 5 σ measurement of P mν, enabling a robust determination of the neutrino mass hierarchy problem."

    The paper's advertised >5σ detection of Σmν=60 meV is obtained by adding a τ prior taken from Ref. [50], whose authors are G. Shmueli, D. Sarkar and E. D. Kovetz — the same first and last authors as the present paper. That prior is not a measured quantity but a forecasted projection from 21-cm observations. The paper's own no-τ-prior combined result is σΣmν∼18 meV, which corresponds to 60/18≈3.3σ. Therefore the difference between a ~3σ bound and the claimed ≳5σ detection is supplied almost entirely by a self-cited projected prior, making the headline sensitivity load-bearing on the authors' own forecast rather than on the LIM analysis itself. The 18 meV result remains self-contained, so this is a partial, not full, circularity.

full rationale

The Fisher-forecast machinery itself is not circular: σΣmν is obtained from the inverse Fisher matrix with derivatives of the modeled signal spectra; no neutrino-mass parameter is fitted to target data; the 1% b∥ prior is motivated by the external FRB forecast of Ref. [126]; the LIM specs and noise treatment are standard; and the code is public. The combined LIM+CMB-S4+DESI-BAO constraint without a τ prior, σΣmν∼18 meV, is independent of the authors' own prior work. The single load-bearing self-citation is the τ prior from Ref. [50], a forecast by the same first and last authors, which converts the ~3.3σ no-prior result into the advertised >5σ statement. Because the paper transparently reports both numbers and the no-prior forecast stands on its own, the circularity is moderate rather than complete. Score 4 reflects one load-bearing self-citation with an otherwise independent central forecast.

Assumptions & free parameters 4 free parameters · 6 assumptions · 0 invented entities

The forecast rests on standard cosmological parameters plus four astrophysical amplitude parameters (B_X per redshift bin), two velocity bias parameters, and an external tau prior from a self-cited 21-cm forecast. The astrophysical models and experiment noise assumptions carry most of the burden that the reader must accept.

free parameters (4)
  • b_parallel (radial velocity reconstruction bias) = 1 fiducial; 1% prior used in main results
    Absorbs uncertainty in the small-scale electron distribution in kSZ reconstruction (Eq. 25); marginalized in the Fisher analysis, which weakens velocity constraints unless a prior is applied.
  • b_perp (transverse velocity reconstruction bias) = 1 fiducial
    Absorbs uncertainty in the small-scale gravitational potential model for the moving lens effect (Eq. 33); marginalized.
  • B_X(z) = I_X b_X per redshift bin = Set from the Silva et al. [CII] model; four independent bins
    The line intensity-bias amplitude is treated as a free nuisance parameter per redshift bin (Sec. III C); fiducial values come from an astrophysical model, not from data used here.
  • Tau prior width = Taken from Ref. [50] 21-cm forecast; not stated numerically in the paper
    The 5-sigma claim uses a tau prior derived from 21-cm forecasted observations; its width is an input from a self-cited projection rather than an external measurement.
assumptions (6)
  • domain assumption The linear continuity equation v = k-hat f a H / k delta holds on the large scales used for velocity reconstruction (Eq. 19).
    Invoked in Sec. III B to write the velocity field as an unbiased tracer of density; breaks down on small scales where non-linearities matter.
  • domain assumption The [CII] luminosity-halo mass relation of Silva et al. (2015) and the halo model describe the LIM signal.
    Used in Eqs. (4)-(12) in Sec. III A; a different luminosity model changes the fiducial B_X and the forecast sensitivity.
  • domain assumption The electron density profile follows Battaglia (2016), with electron bias set equal to halo bias.
    Used in Eq. (26) in Sec. III B 1; this sets P_Xe and the kSZ reconstruction noise, with residual uncertainty partly absorbed by b_parallel.
  • domain assumption The CMB-S4 noise model excludes foregrounds and uses Gaussian lensed covariance for ell > 30 plus Planck TT for ell < 30.
    Sec. II B and Sec. IV C; foregrounds would increase the noise and degrade the constraints, as the authors acknowledge.
  • domain assumption Redshift-space distortions are modeled at Kaiser level only, with Fingers-of-God and GR effects neglected and bRSD fixed to 1.
    Sec. III A after Eq. (7) and Sec. III C; unmodeled small-scale RSD could bias the clustering Fisher information.
  • domain assumption The 21-cm based tau prior from Ref. [50] has the forecasted width and is uncorrelated with the LIM data.
    Sec. IV C and Fig. 8; the 5-sigma result depends on this prior, which is a forecast from a paper by the same first and last authors.

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Cite this review

Pith. "Pith review of Towards a multi-tracer neutrino mass measurement with line-intensity mapping." pith.science (2026). https://pith.science/paper/HLABSFXD

@misc{pith2026241204071,
  author       = {Pith},
  title        = {Pith review of: Towards a multi-tracer neutrino mass measurement with line-intensity mapping},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/HLABSFXD}},
  note         = {Machine review of arXiv:2412.04071}
}
abstract

Accurately determining neutrino masses is a main objective of contemporary cosmology. Since massive neutrinos affect structure formation and evolution, probes of large scale structure are sensitive to the sum of their masses. In this work, we explore future constraints on $\sum m_\nu$ utilizing line-intensity mapping (LIM) as a promising emerging probe of the density of our Universe, focusing on the fine-structure [CII] line as an example, and compare these constraints with those derived from traditional galaxy surveys. Additionally, we perform a multi-tracer analysis using velocity tomography via the kinetic Sunyaev-Zeldovich and moving lens effects to reconstruct the three-dimensional velocity field. Our forecasts indicate that the next-generation AtLAST detector by itself can achieve $\sigma_{\Sigma m_\nu} \sim 50$ meV sensitivity. Velocity tomography will further improve these constraints by 4%. Incorporating forecasts for CMB-S4 and DESI-BAO in a comprehensive multi-tracer analysis, while setting a prior on the optical depth to reionization $\tau$ derived using 21-cm forecasted observations, to break degeneracies, we find that a $\gtrsim5\sigma$ detection of $\sum m_\nu\!\sim\! 60$ meV, under the normal hierarchy, is within reach with LIM. Even without a $\tau$ prior, our combined forecast reaches $\sigma_{\Sigma m_\nu} \!\sim\! 18$ meV.

Figures

Figures reproduced from arXiv: 2412.04071 by the authors.

Figure 1
Figure 1. FIG. 1. CMB power spectrum from primary CMB, gravita [PITH_FULL_IMAGE:figures/full_fig_p006_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Velocity auto-power spectrum (in black) compared [PITH_FULL_IMAGE:figures/full_fig_p007_2.png] view at source ↗
Figure 4
Figure 4. FIG. 4. Velocity power spectrum (black) and reconstruction [PITH_FULL_IMAGE:figures/full_fig_p008_4.png] view at source ↗
Figures from the paper (4 more)
Figure 5
Figure 5. Figure 5: FIG. 5. Ratio between the growth factor in the case of massive [PITH_FULL_IMAGE:figures/full_fig_p010_5.png]
Figure 6
Figure 6. Figure 6: FIG. 6. Constraints of the summed neutrino masses as func [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. Left: Constraints on the summed neutrino masses as function of the survey area Ω [PITH_FULL_IMAGE:figures/full_fig_p012_7.png]
Figure 8
Figure 8. Figure 8: FIG. 8. Constraints of the summed neutrino masses as func [PITH_FULL_IMAGE:figures/full_fig_p012_8.png]

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Reference graph

Works this paper leans on

133 extracted references · 18 canonical work pages · cited by 1 Pith paper

  1. [50]

    Optical depth to reionization from perturbative 21cm clustering

    N. Sailer, S. F. Chen and M. White, “Optical depth to reionization from perturbative 21 cm clustering,” JCAP 10, 007 (2022) [arXiv:2205.11504]

    work page Pith review arXiv 2022

  2. [94]

    Transverse velocities and matter gradient correlations: A new signal and a new challenge to moving-lens analyses,

    S. C. Hotinli, E. Pierpaoli, S. Ferraro and K. Smith, “Transverse velocities and matter gradient correlations: A new signal and a new challenge to moving-lens analyses,” Phys. Rev. D 108, no.8, 083508 (2023) [arXiv:2305.15462 [astro-ph.CO]]

    arXiv 2023

  3. [1]

    kSZ optical depth degener- acy

    kSZ effect To model the kSZ effect [51–53], we follow Ref. [70]. The temperature anisotropy induced by kSZ is given by the LoS integral: TkSZ(θ) = K∗ Z L 0 dr qr(χ∗θ + rˆr), (23) where ˆr is the unit vector in the radial direction, χ∗ the comoving distance associated with z∗, θ is the angular direction on the sky and qr(x) = δe(x)vr(x) is the elec- tron m...

  4. [2]

    ML effect When galaxy clusters, or other potential-well sources (which we refer to as lenses), move in the plane orthogo- nal to the LoS, they can source peculiar velocities in the transverse direction. This produces in the CMB a typical dipole pattern, which is referred to as the ML effect [85– 88]; estimators for such quantity have been built in the con...

  5. [3]

    A Measurement of atmospheric neutrino oscillation parameters by SUPER- KAMIOKANDE I,

    Y. Ashie et al. [Super-Kamiokande], “A Measurement of atmospheric neutrino oscillation parameters by SUPER- KAMIOKANDE I,” Phys. Rev. D 71, 112005 (2005) [arXiv:hep-ex/0501064]

    arXiv 2005

  6. [4]

    Review of neutrino oscllations ex- periments,

    M. D. Messier, “Review of neutrino oscllations ex- periments,” eConf C060409, 018 (2006) [arXiv:hep- ex/0606013]

    arXiv 2006

  7. [5]

    Evidence for os- cillation of atmospheric neutrinos,

    Y. Fukuda et al. [Super-Kamiokande], “Evidence for os- cillation of atmospheric neutrinos,” Phys. Rev. Lett.81, 1562-1567 (1998) [arXiv:hep-ex/9807003]

    arXiv 1998

  8. [6]

    Constraints on neutrino oscillations using 1258 days of Super- Kamiokande solar neutrino data,

    S. Fukuda et al. [Super-Kamiokande], “Constraints on neutrino oscillations using 1258 days of Super- Kamiokande solar neutrino data,” Phys. Rev. Lett. 86, 5656-5660 (2001) [arXiv:hep-ex/0103033]

    arXiv 2001

Show all 133 references
  1. [7]

    Determination of solar neutrino oscillation parameters using 1496 days of Super-Kamiokande I data,

    S. Fukuda et al. [Super-Kamiokande], “Determination of solar neutrino oscillation parameters using 1496 days of Super-Kamiokande I data,” Phys. Lett. B 539, 179- 187 (2002) [arXiv:hep-ex/0205075]

    2002 arXiv

  2. [8]

    Measurement of the L/E distributions of atmospheric neutrinos in Soudan 2 and their interpretation as neutrino oscillations,

    M. C. Sanchez et al. [Soudan 2], “Measurement of the L/E distributions of atmospheric neutrinos in Soudan 2 and their interpretation as neutrino oscillations,” Phys. Rev. D 68, 113004 (2003) [arXiv:hep-ex/0307069]

    2003 arXiv

  3. [9]

    Final neutrino oscillation results from LSND and KARMEN,

    G. Drexlin, “Final neutrino oscillation results from LSND and KARMEN,” Nucl. Phys. B Proc. Suppl.118, 146-153 (2003)

    2003

  4. [10]

    Measurement of neutrino oscillation with KamLAND: Evidence of spectral distor- tion,

    T. Araki et al. [KamLAND], “Measurement of neutrino oscillation with KamLAND: Evidence of spectral distor- tion,” Phys. Rev. Lett. 94, 081801 (2005) [arXiv:hep- ex/0406035]

    2005

  5. [11]

    Power spectra for cold dark matter and its variants,

    D. J. Eisenstein and W. Hu, “Power spectra for cold dark matter and its variants,” Astrophys. J. 511, 5 (1997) [arXiv:astro-ph/9710252]

    1997 arXiv

  6. [12]

    Massive neutrinos and cosmology,

    J. Lesgourgues and S. Pastor, “Massive neutrinos and cosmology,” Phys. Rept. 429, 307-379 (2006) [arXiv:astro-ph/0603494]

    2006 arXiv

  7. [13]

    Neutrinos in Non-linear Structure For- mation - The Effect on Halo Properties,

    J. Brandbyge, S. Hannestad, T. Haugbølle and Y. Y. Y. Wong, “Neutrinos in Non-linear Structure For- mation - The Effect on Halo Properties,” JCAP 09, 014 (2010) [arXiv:1004.4105]

    2010 arXiv

  8. [14]

    Effects of Massive Neutrinos on the Large- Scale Structure of the Universe,

    F. Marulli, C. Carbone, M. Viel, L. Moscardini and A. Cimatti, “Effects of Massive Neutrinos on the Large- Scale Structure of the Universe,” Mon. Not. Roy. As- tron. Soc. 418, 346 (2011) [arXiv:1103.0278]

    2011 arXiv

  9. [15]

    DEMNUni: The clustering of large-scale structures in the presence of massive neutrinos,

    E. Castorina, C. Carbone, J. Bel, E. Sefusatti and K. Dolag, “DEMNUni: The clustering of large-scale structures in the presence of massive neutrinos,” JCAP 07, 043 (2015) doi:10.1088/1475-7516/2015/07/043 [arXiv:1505.07148 [astro-ph.CO]]

    2015 arXiv

  10. [16]

    The Cosmic microwave back- ground radiation,

    E. Gawiser and J. Silk, “The Cosmic microwave back- ground radiation,” Phys. Rept. 333, 245-267 (2000) [arXiv:astro-ph/0002044]

    2000 arXiv

  11. [17]

    Planck 2018 results. I. Overview and the cosmological legacy of Planck,

    N. Aghanim et al. [Planck], “Planck 2018 results. I. Overview and the cosmological legacy of Planck,” As- tron. Astrophys. 641, A1 (2020) [arXiv:1807.06205]

    2020 arXiv

  12. [18]

    Planck 2018 results. VI. Cosmological parameters,

    N. Aghanim et al. [Planck], “Planck 2018 results. VI. Cosmological parameters,” Astron. Astrophys. 641, A6 (2020) [erratum: Astron. Astrophys. 652, C4 (2021)] [arXiv:1807.06209]

    2020 arXiv

  13. [19]

    DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations,

    A. G. Adame et al. [DESI], “DESI 2024 VI: Cosmological Constraints from the Measurements of Baryon Acoustic Oscillations,” [arXiv:2404.03002 [astro-ph.CO]]

    2024 arXiv

  14. [20]

    Neutrino mass bounds from DESI 2024 are relaxed by Planck PR4 and cosmological supernovae,

    I. J. Allali and A. Notari, “Neutrino mass bounds from DESI 2024 are relaxed by Planck PR4 and cosmological supernovae,” [arXiv:2406.14554 [astro-ph.CO]]

    2024 arXiv

  15. [21]

    CMB lensing from Planck PR4 maps,

    J. Carron et al., “CMB lensing from Planck PR4 maps,” JCAP 09, 039 (2022)

    2022

  16. [22]

    The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Pa- rameters,

    J. Carron et al., “The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Pa- rameters,” The astrophysical journal, 962, 2 (2023)

    2023

  17. [23]

    DESI 2024 III: Baryon Acous- tic Oscillations from Galaxies and Quasars,

    A. G. Adame et al., “DESI 2024 III: Baryon Acous- tic Oscillations from Galaxies and Quasars,” (2024) [arXiv:2404.03000]

    2024 arXiv

  18. [24]

    DESI 2024 IV: Baryon Acous- tic Oscillations from the Lyman Alpha Forest,

    A. G. Adame et al., “DESI 2024 IV: Baryon Acous- tic Oscillations from the Lyman Alpha Forest,” (2024) [arXiv:2404.03001]

    2024 arXiv

  19. [25]

    Living at the Edge: A Crit- ical Look at the Cosmological Neutrino Mass Bound,

    D. Naredo-Tuero et al., “Living at the Edge: A Crit- ical Look at the Cosmological Neutrino Mass Bound,” (2024) [arXiv:2407.13831]

    2024 arXiv

  20. [26]

    No νs is Good News,

    N. Craig, D. Green, J. Meyers and S. Rajendran, “No νs is Good News,” [arXiv:2405.00836 [astro-ph.CO]]

    arXiv

  21. [27]

    The Cosmological Preference for Negative Neutrino Mass,

    D. Green and J. Meyers, “The Cosmological Preference for Negative Neutrino Mass,” [arXiv:2407.07878 [astro- ph.CO]]

    arXiv

  22. [28]

    Negative neutrino masses as a mirage of dark energy,

    W. Elbers, C. S. Frenk, A. Jenkins, B. Li and S. Pascoli, “Negative neutrino masses as a mirage of dark energy,” [arXiv:2407.10965 [astro-ph.CO]]

    arXiv

  23. [29]

    Constraining neutrino prop- erties with a Euclid-like galaxy cluster survey,

    M. C. A. Cerbolini, B. Sartoris, J. Q. Xia, A. Biviano, S. Borgani and M. Viel, “Constraining neutrino prop- erties with a Euclid-like galaxy cluster survey,” JCAP 06, 020 (2013) doi:10.1088/1475-7516/2013/06/020 [arXiv:1303.4550 [astro-ph.CO]]

    2013 arXiv

  24. [30]

    Neu- trino Masses from Clustering of Red and Blue Galaxies: A Test of Astrophysical Uncertainties,

    M. E. C. Swanson, W. J. Percival and O. Lahav, “Neu- trino Masses from Clustering of Red and Blue Galaxies: A Test of Astrophysical Uncertainties,” Mon. Not. Roy. Astron. Soc. 409, 1100-1112 (2010) doi:10.1111/j.1365- 2966.2010.17371.x [arXiv:1006.2825 [astro-ph.CO]]

    2010

  25. [31]

    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. [arXiv:1709.09066 [astro- ph.CO]]

    arXiv

  26. [32]

    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, no.1, 5 (2022) doi:10.1007/s00159-022-00143-0 [arXiv:2206.15377 [astro-ph.CO]]

    2022 arXiv

  27. [33]

    Astrophysics & Cosmology from Line Intensity Mapping vs Galaxy Surveys,

    E. Schaan and M. White, “Astrophysics & Cosmology from Line Intensity Mapping vs Galaxy Surveys,” JCAP 16 05, 067 (2021) [arXiv:2103.01971 [astro-ph.CO]]

    2021 arXiv

  28. [34]

    Strategies to Detect Dark-Matter Decays with Line- Intensity Mapping,

    J. L. Bernal, A. Caputo and M. Kamionkowski, “Strategies to Detect Dark-Matter Decays with Line- Intensity Mapping,” Phys. Rev. D 103, no.6, 063523 (2021) [erratum: Phys. Rev. D 105, no.8, 089901 (2022)] doi:10.1103/PhysRevD.103.063523 [arXiv:2012.00771 [astro-ph.CO]]

    2021 arXiv

  29. [35]

    Cosmic Optical Background Excess, Dark Matter, and Line-Intensity Mapping,

    J. L. Bernal, G. Sato-Polito and M. Kamionkowski, “Cosmic Optical Background Excess, Dark Matter, and Line-Intensity Mapping,” Phys. Rev. Lett. 129, no.23, 231301 (2022) [arXiv:2203.11236 [astro-ph.CO]]

    2022 arXiv

  30. [36]

    Un- veiling cosmological information on small scales with line intensity mapping,

    S. Libanore, C. Unal, D. Sarkar and E. D. Kovetz, “Un- veiling cosmological information on small scales with line intensity mapping,” Phys. Rev. D 106, no.12, 123512 (2022) [arXiv:2208.01658]

    2022 arXiv

  31. [37]

    Constraining primordial magnetic fields with line-intensity mapping,

    T. Adi, S. Libanore, H. A. G. Cruz and E. D. Kovetz, “Constraining primordial magnetic fields with line-intensity mapping,” JCAP 09, 035 (2023) [arXiv:2305.06440 [astro-ph.CO]]

    2023 arXiv

  32. [38]

    Constraining cosmology with the CMB ×line inten- sity mapping-nulling convergence,

    H. Fronenberg, A. S. Maniyar, A. R. Pullen and A. Liu, “Constraining cosmology with the CMB ×line inten- sity mapping-nulling convergence,” Phys. Rev. D 109, no.12, 123518 (2024) [arXiv:2309.06477 [astro-ph.CO]]

    2024 arXiv

  33. [39]

    COMAP Pathfinder – Season 2 results II. Up- dated constraints on the CO(1-0) power spectrum,

    N. O. Stutzer, J. G. S. Lunde, P. C. Breysse, D. T. Chung, K. A. Cleary, D. A. Dunne, H. K. Erik- sen, H. T. Ihle, H. Padmanabhan and D. Tolgay, et al. “COMAP Pathfinder – Season 2 results II. Up- dated constraints on the CO(1-0) power spectrum,” [arXiv:2406.07511 [astro-ph.CO]]

    arXiv

  34. [40]

    A wide field-of-view low- resolution spectrometer at APEX: Instrument design and scientific forecast,

    P. Ade et al. [CONCERTO], “A wide field-of-view low- resolution spectrometer at APEX: Instrument design and scientific forecast,” Astron. Astrophys. 642, A60 (2020) [arXiv:2007.14246 [astro-ph.IM]]

    2020 arXiv

  35. [41]

    COMAP Early Science: I. Overview,

    K. A. Cleary, J. Borowska, P. C. Breysse, M. Catha, D. T. Chung, S. E. Church, C. Dickinson, H. K. Erik- sen, M. K. Foss and J. O. Gundersen, et al. “COMAP Early Science: I. Overview,” [arXiv:2111.05927 [astro- ph.CO]]

    arXiv

  36. [42]

    CCAT-prime Collab- oration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope,

    M. Aravena et al. [CCAT-Prime], “CCAT-prime Collab- oration: Science Goals and Forecasts with Prime-Cam on the Fred Young Submillimeter Telescope,” Astro- phys. J. Suppl. 264, no.1, 7 (2023) [arXiv:2107.10364 [astro-ph.CO]]

    2023 arXiv

  37. [43]

    Cosmology with the SPHEREX All-Sky Spectral Survey,

    O. Dor´ e et al. [SPHEREx], “Cosmology with the SPHEREX All-Sky Spectral Survey,” [arXiv:1412.4872 [astro-ph.CO]]

    arXiv

  38. [44]

    Neutrino Properties with Ground-based Millimeter-wavelength Line Inten- sity Mapping,

    A. Moradinezhad Dizgah, G. K. Keating, K. S. Karkare, A. Crites and S. R. Choudhury, “Neutrino Properties with Ground-based Millimeter-wavelength Line Inten- sity Mapping,” Astrophys. J. 926, no.2, 137 (2022) [arXiv:2110.00014 [astro-ph.CO]]

    2022 arXiv

  39. [45]

    Snowmass 2021 Cosmic Frontier White Paper: Cosmology with Millimeter-Wave Line Intensity Mapping,

    K. S. Karkare et al. [Snowmass Cosmic Frontier 5 Top- ical Group], “Snowmass 2021 Cosmic Frontier White Paper: Cosmology with Millimeter-Wave Line Intensity Mapping,” [arXiv:2203.07258 [astro-ph.CO]]

    2021 arXiv

  40. [46]

    Hydrogen Epoch of Reionization Array (HERA),

    D. R. DeBoer, A. R. Parsons, J. E. Aguirre, P. Alexan- der, Z. S. Ali, A. P. Beardsley, G. Bernardi, J. D. Bow- man, 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 [ast...

    2017 arXiv

  41. [47]

    Imaging the redshifted 21-cm pattern around the first sources during the cosmic dawn using the SKA,

    R. Ghara, T. R. Choudhury, K. K. Datta and S. Choud- huri, “Imaging the redshifted 21-cm pattern around the first sources during the cosmic dawn using the SKA,” Mon. Not. Roy. Astron. Soc. 464, no.2, 2234- 2248 (2017) [arXiv:1607.02779 [astro-ph.CO]]

    2017 arXiv

  42. [48]

    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, 181-301 (2006) [arXiv:astro-ph/0608032 [astro-ph]]

    2006 arXiv

  43. [49]

    21-cm cosmology,

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

    2012 arXiv

  44. [51]

    Eliminating the optical depth nuisance from the CMB with 21 cm cosmology,

    A. Liu, J. R. Pritchard, R. Allison, A. R. Par- sons, U. Seljak and B. D. Sherwin, “Eliminating the optical depth nuisance from the CMB with 21 cm cosmology,” Phys. Rev. D 93, no.4, 043013 (2016) [arXiv:1509.08463]

    2016 arXiv

  45. [52]

    Mitigating the optical depth degeneracy in the cosmological measurement of neutrino masses using 21-cm ob- servations,

    G. Shmueli, D. Sarkar and E. D. Kovetz, “Mitigating the optical depth degeneracy in the cosmological measurement of neutrino masses using 21-cm ob- servations,” Phys. Rev. D 108, no.8, 083531 (2023) doi:10.1103/PhysRevD.108.083531 [arXiv:2305.07056 [astro-ph.CO]]

    2023 arXiv

  46. [53]

    The Interaction of Matter and Radiation in a Hot-Model Universe,

    Y. B. Zeldovich and R. A. Sunyaev, “The Interaction of Matter and Radiation in a Hot-Model Universe,” As- trophys. Space Sci. 4, 301-316 (1969)

    1969

  47. [54]

    The Observations of relic radiation as a test of the nature of X-Ray radi- ation from the clusters of galaxies,

    R. A. Sunyaev and Y. B. Zeldovich, “The Observations of relic radiation as a test of the nature of X-Ray radi- ation from the clusters of galaxies,” Comments Astro- phys. Space Phys. 4, 173-178 (1972)

    1972

  48. [55]

    The Sunyaev-Zeldovich effect towards three clusters of galaxies,

    M. Birkinshaw, M. and S. F. Gull and H. Hardebeck, “The Sunyaev-Zeldovich effect towards three clusters of galaxies,” Nature 309, 34 (1984)

    1984

  49. [56]

    Cosmology from the thermal Sunyaev-Zel’dovich power spectrum: Primordial non- Gaussianity and massive neutrinos,

    J. C. Hill and E. Pajer, “Cosmology from the thermal Sunyaev-Zel’dovich power spectrum: Primordial non- Gaussianity and massive neutrinos,” Phys. Rev. D 88, no.6, 063526 (2013) [arXiv:1303.4726 [astro-ph.CO]]

    2013 arXiv

  50. [57]

    Roncarelli, C

    M. Roncarelli, C. Carbone and L. Moscardini, Mon. Not. Roy. Astron. Soc. 447, no.2, 1761-1773 (2015) doi:10.1093/mnras/stu2546 [arXiv:1409.4285 [astro- ph.CO]]

    2015 arXiv

  51. [58]

    The BAHAMAS project: the CMB–large-scale structure tension and the roles of massive neutrinos and galaxy formation,

    I. G. Mccarthy, S. Bird, J. Schaye, J. Harnois-Deraps, A. S. Font and L. Van Waerbeke, “The BAHAMAS project: the CMB–large-scale structure tension and the roles of massive neutrinos and galaxy formation,” Mon. Not. Roy. Astron. Soc. 476, no.3, 2999-3030 (2018) [arXiv:1712.0241...

    2018 arXiv

  52. [59]

    Bolliet, T

    B. Bolliet, T. Brinckmann, J. Chluba and J. Lesgour- gues, Mon. Not. Roy. Astron. Soc. 497, no.2, 1332-1347 (2020) doi:10.1093/mnras/staa1835 [arXiv:1906.10359 [astro-ph.CO]]

    2020 arXiv

  53. [60]

    Gravitational instability: An Approx- imate theory for large density perturbations,

    Y. B. Zeldovich, “Gravitational instability: An Approx- imate theory for large density perturbations,” Astron. Astrophys. 5, 84-89 (1970)

    1970

  54. [61]

    The Interaction of matter and radiation in the hot model of the universe,

    R. A. Sunyaev and Y. B. Zeldovich, “The Interaction of matter and radiation in the hot model of the universe,” Astrophys. Space Sci. 7, 20-30 (1970)

    1970

  55. [62]

    Microwave back- ground radiation as a probe of the contemporary struc- ture and history of the universe,

    R. A. Sunyaev and Y. B. Zeldovich, “Microwave back- ground radiation as a probe of the contemporary struc- ture and history of the universe,” Ann. Rev. Astron. Astrophys. 18, 537-560 (1980)

    1980

  56. [63]

    Microwave polar- ization in the direction of galaxy clusters induced by the CMB quadrupole anisotropy,

    S. Y. Sazonov and R. A. Sunyaev, “Microwave polar- ization in the direction of galaxy clusters induced by the CMB quadrupole anisotropy,” Mon. Not. Roy. As- 17 tron. Soc. 310, 765-772 (1999) [arXiv:astro-ph/9903287 [astro-ph]]

    1999 arXiv

  57. [64]

    Evidence of Galaxy Cluster Motions with the Kinematic Sunyaev- Zel’dovich Effect,

    N. Hand, G. E. Addison, E. Aubourg, N. Battaglia, E. S. Battistelli, D. Bizyaev, J. R. Bond, H. Brewing- ton, J. Brinkmann and B. R. Brown, et al. “Evidence of Galaxy Cluster Motions with the Kinematic Sunyaev- Zel’dovich Effect,” Phys. Rev. Lett. 109, 041101 (2012) [arXiv:120...

    2012 arXiv

  58. [65]

    Planck intermediate results. XXXVII. Evidence of unbound gas from the kinetic Sunyaev-Zeldovich effect,

    P. A. R. Ade et al. [Planck], “Planck intermediate results. XXXVII. Evidence of unbound gas from the kinetic Sunyaev-Zeldovich effect,” Astron. Astrophys. 586, A140 (2016) [arXiv:1504.03339 [astro-ph.CO]]

    2016 arXiv

  59. [66]

    Evidence for the kinematic Sunyaev-Zel’dovich effect with the Atacama Cosmology Telescope and velocity reconstruction from the Baryon Oscillation Spectroscopic Survey,

    E. Schaan et al. [ACTPol], “Evidence for the kinematic Sunyaev-Zel’dovich effect with the Atacama Cosmology Telescope and velocity reconstruction from the Baryon Oscillation Spectroscopic Survey,” Phys. Rev. D 93, no.8, 082002 (2016) [arXiv:1510.06442 [astro-ph.CO]]

    2016 arXiv

  60. [67]

    Detection of the kine- matic Sunyaev–Zel’dovich effect with DES Year 1 and SPT,

    B. Soergel et al. [DES and SPT], “Detection of the kine- matic Sunyaev–Zel’dovich effect with DES Year 1 and SPT,” Mon. Not. Roy. Astron. Soc. 461, no.3, 3172- 3193 (2016) [arXiv:1603.03904 [astro-ph.CO]]

    2016 arXiv

  61. [68]

    Kinematic Sunyaev-Zel’dovich Ef- fect with Projected Fields: A Novel Probe of the Baryon Distribution with Planck, WMAP, and WISE Data,

    J. C. Hill, S. Ferraro, N. Battaglia, J. Liu and D. N. Spergel, “Kinematic Sunyaev-Zel’dovich Ef- fect with Projected Fields: A Novel Probe of the Baryon Distribution with Planck, WMAP, and WISE Data,” Phys. Rev. Lett. 117, no.5, 051301 (2016) doi:10.1103/PhysRevLett.117.05130...

    2016 arXiv

  62. [69]

    Detection of the pairwise kinematic Sunyaev-Zel’dovich effect with BOSS DR11 and the Atacama Cosmology Telescope,

    F. De Bernardis, S. Aiola, E. M. Vavagiakis, M. D. Niemack, N. Battaglia, J. Beall, D. T. Becker, J. R. Bond, E. Calabrese and H. Cho, et al. “Detection of the pairwise kinematic Sunyaev-Zel’dovich effect with BOSS DR11 and the Atacama Cosmology Telescope,” JCAP 03, 008 (2017)...

    2017 arXiv

  63. [70]

    CMB-S4 Science Book, First Edition,

    K. N. Abazajian et al. [CMB-S4], “CMB-S4 Science Book, First Edition,” [arXiv:1610.02743 [astro-ph.CO]]

    arXiv

  64. [71]

    The Simons Ob- servatory: Science goals and forecasts,

    P. Ade et al. [Simons Observatory], “The Simons Ob- servatory: Science goals and forecasts,” JCAP 02, 056 (2019) [arXiv:1808.07445 [astro-ph.CO]]

    2019 arXiv

  65. [72]

    KSZ tomog- raphy and the bispectrum,

    K. M. Smith, M. S. Madhavacheril, M. M¨ unchmeyer, S. Ferraro, U. Giri and M. C. Johnson, “KSZ tomog- raphy and the bispectrum,” [arXiv:1810.13423 [astro- ph.CO]]

    arXiv

  66. [73]

    Constraining local non-Gaussianities with kinetic Sunyaev-Zel’dovich tomography,

    M. M¨ unchmeyer, M. S. Madhavacheril, S. Ferraro, M. C. Johnson and K. M. Smith, “Constraining local non-Gaussianities with kinetic Sunyaev-Zel’dovich tomography,” Phys. Rev. D 100, no.8, 083508 (2019) doi:10.1103/PhysRevD.100.083508 [arXiv:1810.13424 [astro-ph.CO]]

    2019 arXiv

  67. [74]

    Cosmological Con- straints from Galaxy Cluster Velocity Statistics,

    S. Bhattacharya and A. Kosowsky, “Cosmological Con- straints from Galaxy Cluster Velocity Statistics,” As- trophys. J. Lett. 659, L83-L86 (2007) [arXiv:astro- ph/0612555 [astro-ph]]

    2007

  68. [75]

    Constraints on massive neutrinos from the pairwise kinematic Sunyaev-Zel’dovich effect,

    E. M. Mueller, F. de Bernardis, R. Bean and M. D. Niemack, “Constraints on massive neutrinos from the pairwise kinematic Sunyaev-Zel’dovich effect,” Phys. Rev. D 92, no.6, 063501 (2015) [arXiv:1412.0592 [astro-ph.CO]]

    2015 arXiv

  69. [76]

    Dark Energy Con- straints from Galaxy Cluster Peculiar Velocities,

    S. Bhattacharya and A. Kosowsky, “Dark Energy Con- straints from Galaxy Cluster Peculiar Velocities,” Phys. Rev. D 77, 083004 (2008) [arXiv:0712.0034 [astro-ph]]

    2008 arXiv

  70. [77]

    Dark energy imprints on the kinematic Sunyaev–Zel’dovich signal,

    Y. Z. Ma and G. B. Zhao, “Dark energy imprints on the kinematic Sunyaev–Zel’dovich signal,” Phys. Lett. B 735, 402-411 (2014) [arXiv:1309.1163 [astro-ph.CO]]

    2014 arXiv

  71. [78]

    Constraints on gravity and dark energy from the pairwise kinematic Sunyaev- Zeldovich effect,

    E. M. Mueller, F. de Bernardis, R. Bean and M. D. Niemack, “Constraints on gravity and dark energy from the pairwise kinematic Sunyaev- Zeldovich effect,” Astrophys. J. 808, no.1, 47 (2015) [arXiv:1408.6248 [astro-ph.CO]]

    2015 arXiv

  72. [79]

    Phe- nomenology of a vector-field-induced (and possibly par- ity breaking) compensated isocurvature perturbation,

    E. Vanzan, M. Kamionkowski and S. C. Hotinli, “Phe- nomenology of a vector-field-induced (and possibly par- ity breaking) compensated isocurvature perturbation,” [arXiv:2311.18121 [astro-ph.CO]]

    arXiv

  73. [80]

    Kinetic Sunyaev- Zel’dovich effect in modified gravity,

    F. Bianchini and A. Silvestri, “Kinetic Sunyaev- Zel’dovich effect in modified gravity,” Phys. Rev. D 93, no.6, 064026 (2016) [arXiv:1510.08844 [astro-ph.CO]]

    2016 arXiv

  74. [81]

    Constraints on cosmology beyond ΛCDM with ki- netic Sunyaev Zel’dovich velocity reconstruction,

    J. Krywonos, S. C. Hotinli and M. C. Johnson, “Constraints on cosmology beyond ΛCDM with ki- netic Sunyaev Zel’dovich velocity reconstruction,” [arXiv:2408.05264 [astro-ph.CO]]

    arXiv

  75. [82]

    Evidence of the Missing Baryons from the Kinematic Sunyaev-Zeldovich Effect in Planck Data,

    C. Hern´ andez-Monteagudo, Y. Z. Ma, F. S. Kitaura, W. Wang, R. G´ enova-Santos, J. Mac ´ ıas-P´ erez and D. Herranz, “Evidence of the Missing Baryons from the Kinematic Sunyaev-Zeldovich Effect in Planck Data,” Phys. Rev. Lett. 115, no.19, 191301 (2015) [arXiv:1504.04011 [ast...

    2015 arXiv

  76. [83]

    The halo by halo missing baryon problem,

    S. S. McGaugh, “The halo by halo missing baryon problem,” IAU Symp. 244, 136-145 (2008) doi:10.1017/S1743921307013920 [arXiv:0707.3795 [astro-ph]]

    2008 arXiv

  77. [84]

    Using the kinematic Sunyaev-Zeldovich effect to determine the peculiar ve- locities of clusters of galaxies,

    M. G. Haehnelt and M. Tegmark, “Using the kinematic Sunyaev-Zeldovich effect to determine the peculiar ve- locities of clusters of galaxies,” Mon. Not. Roy. As- tron. Soc. 279, 545-556 (1996) [arXiv:astro-ph/9507077 [astro-ph]]

    1996 arXiv

  78. [85]

    Measuring cluster peculiar velocities with the sunyaev-zeldovich effects: scaling relations and sys- tematics,

    A. Diaferio, S. Borgani, L. Moscardini, G. Murante, K. Dolag, V. Springel, G. Tormen, L. Tornatore and P. Tozzi, “Measuring cluster peculiar velocities with the sunyaev-zeldovich effects: scaling relations and sys- tematics,” Mon. Not. Roy. Astron. Soc. 356, 1477-1488 (2005) [...

    2005 arXiv

  79. [86]

    Reconstructing patchy helium reionization using the cosmic microwave background and large-scale structure,

    M. C ¸ alı¸ skan, N. Anil Kumar, S. C. Hotinli and M. Kamionkowski, “Reconstructing patchy helium reionization using the cosmic microwave background and large-scale structure,” [arXiv:2312.00118 [astro- ph.CO]]

    arXiv

  80. [87]

    A test for transverse mo- tions of clusters of galaxies,

    M. Birkinshaw and S. Gull, “A test for transverse mo- tions of clusters of galaxies,” Nature 302, 315–317 (1983) doi:10.1038/302315a0

    1983 doi

  81. [88]

    Cosmic mi- crowave background anisotropies from the Rees-Sciama effect in Omega(0) <= 1 universes,

    R. Tuluie, P. Laguna and P. Anninos, “Cosmic mi- crowave background anisotropies from the Rees-Sciama effect in Omega(0) <= 1 universes,” Astrophys. J. 463, 15 (1996) [arXiv:astro-ph/9510019 [astro-ph]]

    1996 arXiv

  82. [89]

    Moving gravitational lenses: Imprints on the CMB,

    N. Aghanim, S. Prunet, O. Forni and F. R. Bouchet, “Moving gravitational lenses: Imprints on the CMB,” Astron. Astrophys. 334, 409 (1998) [arXiv:astro- ph/9803040 [astro-ph]]

    1998

  83. [90]

    Nonlinear integrated Sachs-Wolfe ef- fect,

    A. Cooray, “Nonlinear integrated Sachs-Wolfe ef- fect,” Phys. Rev. D 65, 083518 (2002) [arXiv:astro- ph/0109162 [astro-ph]]

    2002

  84. [91]

    Perturbations of a cosmological model and angular variations of the mi- crowave background,

    R. K. Sachs and A. M. Wolfe, “Perturbations of a cosmological model and angular variations of the mi- crowave background,” Astrophys. J. 147, 73-90 (1967)

    1967

  85. [92]

    Transverse Veloci- ties with the Moving Lens Effect,

    S. C. Hotinli, J. Meyers, N. Dalal, A. H. Jaffe, M. C. Johnson, J. B. Mertens, M. M¨ unchmeyer, K. M. Smith and A. van Engelen, “Transverse Veloci- ties with the Moving Lens Effect,” Phys. Rev. Lett.123, no.6, 061301 (2019) [arXiv:1812.03167 [astro-ph.CO]]. 18

    2019 arXiv

  86. [93]

    The imprint of proper mo- tion of nonlinear structures on the cosmic microwave background,

    R. Tuluie and P. Laguna, “The imprint of proper mo- tion of nonlinear structures on the cosmic microwave background,” Astrophys. J. Lett. 445, L73-L76 (1995) [arXiv:astro-ph/9501059 [astro-ph]]

    1995 arXiv

  87. [95]

    Cosmology with the moving lens effect,

    S. C. Hotinli, K. M. Smith, M. S. Madhavacheril and M. Kamionkowski, “Cosmology with the moving lens effect,” Phys. Rev. D 104, no.8, 083529 (2021) [arXiv:2108.02207 [astro-ph.CO]]

    2021 arXiv

  88. [96]

    Probing neutrino masses with velocity to- mography,

    A. J. Tishue, S. C. Hotinli, E. D. Kovetz, M. S. Mad- havacheril, “Probing neutrino masses with velocity to- mography,” [arXiv:24xx.xxxx]

  89. [97]

    Kinetic Sunyaev-Zel’dovich tomog- raphy with line-intensity mapping,

    G. Sato-Polito, J. L. Bernal, K. K. Boddy and M. Kamionkowski, “Kinetic Sunyaev-Zel’dovich tomog- raphy with line-intensity mapping,” Phys. Rev. D 103, no.8, 083519 (2021) [arXiv:2011.08193 [astro-ph.CO]]

    2021 arXiv

  90. [98]

    A 158 Micron [CII] Line Survey of Galaxies at z ˜ 1 to 2: An Indicator of Star Forma- tion in the Early Universe,

    G. J. Stacey, S. Hailey-Dunsheath, C. Ferkinhoff, T. Nikola, S. C. Parshley, D. J. Benford, J. G. Staguhn and N. Fiolet, “A 158 Micron [CII] Line Survey of Galaxies at z ˜ 1 to 2: An Indicator of Star Forma- tion in the Early Universe,” Astrophys. J. 724, 957-974 (2010) [arXiv...

    2010 arXiv

  91. [99]

    De- tecting Z > 10 objects through carbon, nitrogen and oxygen emission lines,

    M. Suginohara, T. Suginohara and D. N. Spergel, “De- tecting Z > 10 objects through carbon, nitrogen and oxygen emission lines,” Astrophys. J. 512, 547 (1999) [arXiv:astro-ph/9803236 [astro-ph]]

    1999 arXiv

  92. [100]

    The reliability of [CII] as a star formation rate indicator,

    I. De Looze, M. Baes, G. J. Bendo, L. Cortese and J. Fritz, “The reliability of [CII] as a star formation rate indicator,” Mon. Not. Roy. Astron. Soc. 416, 2712 (2011) [arXiv:1106.1643 [astro-ph.CO]]

    2011 arXiv

  93. [101]

    [CII] 158 µm Emission as a Star Formation Tracer,

    R. Herrera-Camus, A. D. Bolatto, M. G. Wolfire, J. D. Smith, K. V. Croxall, R. C. Kennicutt, D. Calzetti, G. Helou, F. Walter and A. K. Leroy, et al. “[CII] 158 µm Emission as a Star Formation Tracer,” Astrophys. J. 800, no.1, 1 (2015) [arXiv:1409.7123 [astro-ph.GA]]

    2015 arXiv

  94. [102]

    The Experiment for Cryogenic Large-aperture In- tensity Mapping (EXCLAIM),

    P. A. R. Ade, C. J. Anderson, E. M. Barrentine, N. G. Bellis, A. D. Bolatto, P. C. Breysse, B. T. Bulcha, G. Cataldo, J. A. Connors and P. W. Cursey, et al. “The Experiment for Cryogenic Large-aperture In- tensity Mapping (EXCLAIM),” J. Low Temp. Phys. 199, no.3-4, 1027-1037 (...

    2020 arXiv

  95. [103]

    The Terahertz Intensity Mapper (TIM): a Next-Generation Experiment for Galaxy Evolution Studies

    J. Vieira, J. Aguirre, C. M. Bradford, et al. “The Terahertz Intensity Mapper (TIM): a Next-Generation Experiment for Galaxy Evolution Studies” (2020) [arXiv:2009.14340]

    2020 arXiv

  96. [104]

    Sensitiv- ity of the Prime-Cam Instrument on the CCAT- prime Telescope,

    S. K. Choi, J. Austermann, K. Basu, N. Battaglia, F. Bertoldi, D. T. Chung, N. F. Cothard, S. Duff, C. J. Duell and P. A. Gallardo, et al. “Sensitiv- ity of the Prime-Cam Instrument on the CCAT- prime Telescope,” J. Low Temp. Phys. 199, no.3- 4, 1089-1097 (2020) doi:10.1007/s1...

    2020 arXiv

  97. [105]

    Probing Cosmic Reionization and Molecular Gas Growth with TIME,

    G. Sun, T. C. Chang, B. D. Uzgil, J. Bock, C. M. Brad- ford, V. Butler, T. Caze-Cortes, Y. T. Cheng, A. Cooray and A. T. Crites, et al. “Probing Cosmic Reionization and Molecular Gas Growth with TIME,” Astrophys. J. 915, no.1, 33 (2021) [arXiv:2012.09160 [astro-ph.GA]]

    2021 arXiv

  98. [106]

    The Atacama Large Aperture Sub- millimeter Telescope (AtLAST),

    P. Klaassen, et al. “The Atacama Large Aperture Sub- millimeter Telescope (AtLAST),” [arXiv:1907.04756]

    1907 arXiv

  99. [107]

    The key sci- ence drivers for the Atacama Large Aperture Submil- limeter Telescope (AtLAST),

    M. Booth, P. Klaassen, C. Cicone, T. Mroczkowski, S. Wedemeyer, K. Akiyama, G. Bower, M. A. Cordiner, L. Di Mascolo and D. Johnstone, et al. “The key sci- ence drivers for the Atacama Large Aperture Submil- limeter Telescope (AtLAST),” [arXiv:2405.20140 [astro- ph.IM]]

    arXiv

  100. [108]

    AtLAST Science Overview Report,

    M. Booth, P. Klaassen, C. Cicone, T. Mroczkowski, M. A. Cordiner, L. Di Mascolo, D. Johnstone, E. van Kampen, M. M. Lee and D. Liu, et al. “AtLAST Science Overview Report,” [arXiv:2407.01413 [astro-ph.IM]]

    arXiv

  101. [109]

    Validation of the Scientific Program for the Dark Energy Spectro- scopic Instrument,

    A. G. Adame et al. [DESI], “Validation of the Scientific Program for the Dark Energy Spectro- scopic Instrument,” Astron. J. 167, no.2, 62 (2024) [arXiv:2306.06307 [astro-ph.CO]]

    2024 arXiv

  102. [110]

    The DESI Experi- ment Part I: Science,Targeting, and Survey Design,

    A. Aghamousa et al. [DESI], “The DESI Experi- ment Part I: Science,Targeting, and Survey Design,” [arXiv:1611.00036 [astro-ph.IM]]

    arXiv

  103. [111]

    LSST Science Book, Version 2.0,

    P. A. Abell et al. [LSST Science and LSST Project], “LSST Science Book, Version 2.0,” [arXiv:0912.0201 [astro-ph.IM]]

    arXiv

  104. [112]

    User’s guide to extracting cosmologi- cal information from line-intensity maps,

    J. L. Bernal, P. C. Breysse, H. Gil-Mar ´ ın and E. D. Kovetz, “User’s guide to extracting cosmologi- cal information from line-intensity maps,” Phys. Rev. D 100, no.12, 123522 (2019) [arXiv:1907.10067 [astro- ph.CO]]

    2019

  105. [113]

    Toward a halo mass function for precision cosmology: The Limits of universality,

    J. L. Tinker, A. V. Kravtsov, A. Klypin, K. Abazajian, M. S. Warren, G. Yepes, S. Gottlober and D. E. Holz, “Toward a halo mass function for precision cosmology: The Limits of universality,” Astrophys. J. 688, 709-728 (2008) [arXiv:0803.2706 [astro-ph]]

    2008 arXiv

  106. [114]

    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]]

    2002

  107. [115]

    The Large Scale Bias of Dark Matter Halos: Numer- ical Calibration and Model Tests,

    J. L. Tinker, B. E. Robertson, A. V. Kravtsov, A. Klypin, M. S. Warren, G. Yepes and S. Gottlober, “The Large Scale Bias of Dark Matter Halos: Numer- ical Calibration and Model Tests,” Astrophys. J. 724, 878-886 (2010) [arXiv:1001.3162 [astro-ph.CO]]

    2010 arXiv

  108. [116]

    The linear power spectrum of observed source number counts,

    A. Challinor and A. Lewis, “The linear power spectrum of observed source number counts,” Phys. Rev. D 84, 043516 (2011) [arXiv:1105.5292 [astro-ph.CO]]

    2011 arXiv

  109. [117]

    Fingers of God: A critique of Rees’ theory of primoridal gravitational radiation,

    J. C. Jackson, “Fingers of God: A critique of Rees’ theory of primoridal gravitational radiation,” Mon. Not. Roy. Astron. Soc. 156, 1P-5P (1972) [arXiv:0810.3908 [astro-ph]]

    1972 arXiv

  110. [118]

    Clustering in real space and in redshift space,

    N. Kaiser, “Clustering in real space and in redshift space,” Mon. Not. Roy. Astron. Soc. 227, 1-27 (1987)

    1987

  111. [119]

    Prospects for Detecting C II Emission Dur- ing the Epoch of Reionization,

    M. B. Silva, M. G. Santos, A. Cooray and Y. Gong, “Prospects for Detecting C II Emission Dur- ing the Epoch of Reionization,” Astrophys. J. 806, no.2, 209 (2015) doi:10.1088/0004-637X/806/2/209 [arXiv:1410.4808 [astro-ph.GA]]

    2015 arXiv

  112. [120]

    A Universal density profile from hierarchical cluster- ing,

    J. F. Navarro, C. S. Frenk and S. D. M. White, “A Universal density profile from hierarchical cluster- ing,” Astrophys. J. 490, 493-508 (1997) [arXiv:astro- ph/9611107 [astro-ph]]

    1997

  113. [121]

    The Kinetic Sunyaev-Zel’dovich effect from reionization,

    M. McQuinn, S. R. Furlanetto, L. Hernquist, O. Zahn and M. Zaldarriaga, “The Kinetic Sunyaev-Zel’dovich effect from reionization,” Astrophys. J. 630, 643-656 (2005) [arXiv:astro-ph/0504189 [astro-ph]]

    2005 arXiv

  114. [122]

    The Kinetic Sunyaev-Zel’dovich effect as a probe of the physics of cosmic reionization: the effect of self-regulated reionization,

    H. Park, P. R. Shapiro, E. Komatsu, I. T. Iliev, K. Ahn and G. Mellema, “The Kinetic Sunyaev-Zel’dovich effect as a probe of the physics of cosmic reionization: the effect of self-regulated reionization,” Astrophys. J. 769, 19 93 (2013) [arXiv:1301.3607 [astro-ph.CO]]

    2013 arXiv

  115. [123]

    The Tau of Galaxy Clusters,

    N. Battaglia, “The Tau of Galaxy Clusters,” JCAP 08, 058 (2016) [arXiv:1607.02442 [astro-ph.CO]]

    2016 arXiv

  116. [124]

    Mass reconstruction with cmb polarization,

    W. Hu and T. Okamoto, “Mass reconstruction with cmb polarization,” Astrophys. J. 574, 566-574 (2002) [arXiv:astro-ph/0111606 [astro-ph]]

    2002 arXiv

  117. [125]

    Velocity reconstruction with the cosmic microwave background and galaxy surveys,

    J. Cayuso, R. Bloch, S. C. Hotinli, M. C. Johnson and F. McCarthy, “Velocity reconstruction with the cosmic microwave background and galaxy surveys,” JCAP 02, 051 (2023) [arXiv:2111.11526 [astro-ph.CO]]

    2023 arXiv

  118. [126]

    Massive Neu- trinos and the Large Scale Structure of the Universe,

    J. R. Bond, G. Efstathiou and J. Silk, “Massive Neu- trinos and the Large Scale Structure of the Universe,” Phys. Rev. Lett. 45, 1980-1984 (1980)

    1980

  119. [127]

    The Cosmic Linear Anisotropy Solving System (CLASS) I: Overview,

    J. Lesgourgues, “The Cosmic Linear Anisotropy Solving System (CLASS) I: Overview,” [arXiv:1104.2932 [astro- ph.IM]]

    arXiv

  120. [128]

    Cosmology with the kinematic Sunyaev- Zeldovich effect: Breaking the optical depth degeneracy with fast radio bursts,

    M. S. Madhavacheril, N. Battaglia, K. M. Smith and J. L. Sievers, “Cosmology with the kinematic Sunyaev- Zeldovich effect: Breaking the optical depth degeneracy with fast radio bursts,” Phys. Rev. D100, no.10, 103532 (2019) [arXiv:1901.02418 [astro-ph.CO]]

    2019 arXiv

  121. [129]

    The benefits of CMB delens- ing,

    S. C. Hotinli, J. Meyers, C. Trendafilova, D. Green and A. van Engelen, “The benefits of CMB delens- ing,” JCAP 04, no.04, 020 (2022) doi:10.1088/1475- 7516/2022/04/020 [arXiv:2111.15036 [astro-ph.CO]]

    2022 arXiv

  122. [130]

    Cosmic Expansion History from Line-Intensity Mapping,

    J. L. Bernal, P. C. Breysse and E. D. Kovetz, “Cosmic Expansion History from Line-Intensity Mapping,” Phys. Rev. Lett. 123, no.25, 251301 (2019) doi:10.1103/PhysRevLett.123.251301 [arXiv:1907.10065 [astro-ph.CO]]

    2019

  123. [131]

    CMB optical depth mea- surements: Past, present, future,

    B. G. Keating and N. Miller, “CMB optical depth mea- surements: Past, present, future,” New Astron. Rev. 50, 184-190 (2006) [arXiv:astro-ph/0508269]

    2006 arXiv

  124. [132]

    Observing the Epoch of Reion- ization with the Cosmic Microwave Background,

    C. L. Reichardt, “Observing the Epoch of Reion- ization with the Cosmic Microwave Background,” [arXiv:1511.01117]

    arXiv

  125. [133]

    Neutrino Mass from Cosmology: Probing Physics Beyond the Standard Model,

    C. Dvorkin, M. Gerbino, D. Alonso, N. Battaglia, S. Bird, A. Diaz Rivero, A. Font-Ribera, G. Fuller, M. Lattanzi and M. Loverde, et al. “Neutrino Mass from Cosmology: Probing Physics Beyond the Standard Model,” [arXiv:1903.03689 [astro-ph.CO]]

    1903 arXiv

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