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arxiv: 1907.05323 · v1 · pith:XH4UPO2Pnew · submitted 2019-07-11 · 🌌 astro-ph.GA · astro-ph.CO

Extragalactic astrophysics with next-generation CMB experiments

G. de Zotti , M. Bonato , M. Negrello , T. Trombetti , C. Burigana , D. Herranz , M. L\'opez-Caniego , Z.-Y. Cai
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L. Bonavera J. Gonz\'alez-Nuevo
This is my paper

Pith reviewed 2026-05-24 22:57 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.CO
keywords CMB surveysgravitational lensingproto-clustershigh-redshift galaxiesdusty star-forming galaxiesradio sourcespolarized emission
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The pith

Next-generation CMB experiments will detect thousands of strongly lensed galaxies out to redshift 6 and proto-clusters in their main star-forming phase.

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

Current CMB surveys from Planck, SPT and ACT have already shown that these instruments can contribute to extragalactic astronomy by finding lensed high-redshift galaxies and dusty star-forming systems. The paper argues that planned space and ground-based experiments with greater sensitivity and resolution will scale up these detections dramatically. This would enable detailed studies of galaxy structure at early times thanks to lensing magnification and stretching, and catch galaxy clusters while their stars are still forming in bulk. A sympathetic reader would care because these observations probe the peak epoch of star formation in the universe and test models of galaxy assembly.

Core claim

The central claim is that instruments such as PICO, CORE, CMB-Bharat, Simons Observatory and CMB-S4 will discover several thousands of strongly lensed galaxies out to z~6 or more, along with galaxy proto-clusters at the epoch when their member galaxies formed most of their stars. They will also detect tens of thousands of local dusty galaxies and thousands of radio sources up to z~5, and measure polarized emission from thousands of sources at mm/sub-mm wavelengths.

What carries the argument

Strong gravitational lensing by foreground galaxies that boosts flux and stretches images, combined with the high sensitivity of next-generation CMB surveys to mm/sub-mm emission from dusty galaxies.

If this is right

  • Investigation of galaxy internal structure at z~3 with ~60 pc resolution becomes routine for many objects.
  • Proto-clusters can be identified before they develop detectable hot gas via X-rays or SZ effect.
  • Large samples of polarized radio sources and dusty galaxies will be available for statistical studies.
  • Number counts of high-z sources can be measured to much fainter levels than today.

Where Pith is reading between the lines

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

  • These detections could tighten constraints on the star formation rate density at z>3 by providing large, uniformly selected samples.
  • Cross-correlations with optical or near-IR surveys might reveal the dark matter halos hosting these proto-clusters.
  • Failure to find the predicted numbers would indicate either lower lensing optical depths or different evolution in the sub-mm luminosity function than assumed.

Load-bearing premise

That the number counts of dusty galaxies and the statistics of strong lensing at faint flux levels and high redshifts can be reliably extrapolated from existing shallower surveys.

What would settle it

Running the next-generation surveys and counting far fewer than several thousand strongly lensed galaxies or proto-clusters would falsify the yield predictions.

Figures

Figures reproduced from arXiv: 1907.05323 by C. Burigana, D. Herranz, G. de Zotti, J. Gonz\'alez-Nuevo, L. Bonavera, M. Bonato, M. L\'opez-Caniego, M. Negrello, T. Trombetti, Z.-Y. Cai.

Figure 1
Figure 1. Figure 1: Effect of angular resolution on the confusion limit. The filled blue circles show the differential counts of sources on SPT maps degraded to the PICO resolution at 150 GHz (FWHM = 6.2 0 ; left panel) and 220 GHz (FWHM = 3.6 0 ; right panel) compared with the SPT counts of Mocanu et al. [5, orange stars]. The vertical dot-dashed lines correspond, from left to right, to the 90% completeness limits at the ful… view at source ↗
Figure 2
Figure 2. Figure 2: Spectral energy distributions of extragalactic sources in the frequency range of CMB experiments, compared with the estimated detection limits of the PICO project and with the completeness limits of the SPT surveys extrapolated to 40 and to 270 GHz, to cover the range of the CMB-S4 project. The PCCS2 90% completeness limits in the “extragalactic zone” are also shown for comparison (in the left panel only).… view at source ↗
Figure 3
Figure 3. Figure 3: Upper left panel. Integral counts of strongly lensed galaxies from Herschel surveys at 500 µm [600 GHz; green and magenta data points from ref. 24], compared with the predictions of the Cai et al. [25] model (solid orange line). The yellow square on the bottom-right corner is our own estimate of the counts of strongly lensed galaxies detected by Planck. The counts of unlensed proto-spheroidal galaxies (dat… view at source ↗
Figure 4
Figure 4. Figure 4: 3D colour-colour plot showing the colours of strongly-lensed galaxies detected by Planck (purple stars) compared to those of local galaxies (light blue symbols) and of radio sources (green symbols). The distribution of local galaxies extends to the blue far beyond the chosen boundaries of the figure. Strongly lensed galaxies populate a region intermediate between those of local galaxies and radio sources a… view at source ↗
Figure 5
Figure 5. Figure 5: SEDs of the strongly lensed galaxy SDP 81 at 3.042 detected by the Herschel Astrophysical Terahertz Large Area Survey [H-ATLAS; 36] and imaged with the Sub-Millimeter Array (SMA) at 880 µm [15] and of the foreground lens at z = 0.299 imaged with the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope [HST; 37]. As is generally the case, the lens is a spheroidal galaxy in passive evolution, hence very … view at source ↗
Figure 6
Figure 6. Figure 6: SEDs of spectroscopically confirmed sub-mm bright high-z proto-clusters detected by Ivison et al. [70], Wang et al. [71], Miller et al. [72] and Oteo et al. [73], compared with (from top to bottom) the detection limits of diffraction limited space-borne telescopes of 1, 1.5 and 2 m size, and with the SPT completeness limit. The flux densities by Ivison et al. [70] and Wang et al. [71] are shown as lower li… view at source ↗
Figure 7
Figure 7. Figure 7: Integral counts and redshift distributions of proto-clusters at 220 GHz and 600 GHz (1.4 mm and 500 µm, respectively) predicted by Negrello et al. [74]. The vertical lines in the upper left panel show, from left to right, the 5 σ confusion limit for a 6 m telescope, the SPT completeness limit and the 5 σ detection limits for 2, 1.5 and 1 m telescopes operating at the diffraction limit. Only the three latte… view at source ↗
Figure 8
Figure 8. Figure 8: Expected flux density at 220 GHz due to the integrated dust emission from member galaxies of a cluster with M = 1014.5 M as a function of the cluster redshift (solid thick black curve). The cluster luminosity includes contributions from normal late-type and starburst galaxies (warm and cold SFGs, respectively) and from proto-spheroidal galaxies (spheroids), computed using the model by Cai et al. [25]. The … view at source ↗
Figure 9
Figure 9. Figure 9: Integral number counts of radio sources at 220 and 600 GHz. The vertical dashed lines show the 5 σ confusion limits for a space-borne experiment with a 1 m, 1.5 m and a 2 m telescope (from right to left) operating at the diffraction limit. The dot-dashed and dotted vertical lines on the left panel show the completeness limit of the SPT survey and the 5 σ confusion limit for the SPT telescope, respectively.… view at source ↗
Figure 10
Figure 10. Figure 10: Estimated integral number counts in polarized intensity of radio sources and of dusty galaxies (IR) at 60, 145, 220 and 800 GHz. The contribution of dusty galaxies is completely negligible at 60 GHz. The vertical dashed black lines show the 5 σ detection limits for a space-borne instrument with a 1.5 m telescope and state-of-the-art sensitivity derived from simulations similar to those described in De Zot… view at source ↗
read the original abstract

Planck, SPT and ACT surveys have clearly demonstrated that Cosmic Microwave Background (CMB) experiments, while optimised for cosmological measurements, have made important contributions to the field of extragalactic astrophysics in the last decade. Future CMB experiments have the potential to make even greater contributions. One example is the detection of high-z galaxies with extreme gravitational amplifications. The combination of flux boosting and of stretching of the images has allowed the investigation of the structure of galaxies at z ~3 with the astounding spatial resolution of about 60 pc. Another example is the detection of proto-clusters of dusty galaxies at high z when they may not yet possess the hot intergalactic medium allowing their detection in X-rays or via the Sunyaev-Zeldovich effect. Next generation CMB experiments, like PICO, CORE, CMB-Bharat from space and Simons Observatory and CMB-S4 from the ground, will discover several thousands of strongly lensed galaxies out to z~6 or more and of galaxy proto-clusters caught in the phase when their member galaxies where forming the bulk of their {stars. They will also detect tens of thousands of local dusty galaxies and thousands of radio sources at least up to z~5. Moreover they will measure the polarized emission of thousands of radio sources and of dusty galaxies at mm/sub-mm wavelengths.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript reviews the extragalactic science potential of next-generation CMB experiments (PICO, CORE, CMB-Bharat from space; Simons Observatory and CMB-S4 from the ground). Building on results from Planck, SPT and ACT, it argues that these instruments will detect several thousand strongly lensed galaxies out to z ≳ 6, proto-clusters of dusty galaxies during their peak star-formation epoch, tens of thousands of local dusty galaxies, and thousands of radio sources to z ~ 5, while also measuring polarized emission from thousands of sources at mm/sub-mm wavelengths.

Significance. If the yield forecasts are robust, the work correctly identifies a high-impact, multi-purpose science case for future CMB facilities: the combination of wide area, high sensitivity and multi-frequency coverage will enable statistical samples of strongly lensed high-z galaxies (with ~60 pc resolution) and proto-clusters that are difficult to obtain at other wavelengths. The emphasis on the complementarity with X-ray and SZ searches is a useful framing.

major comments (2)
  1. [Abstract] Abstract: the quantitative forecasts ('several thousands of strongly lensed galaxies out to z~6 or more' and 'galaxy proto-clusters') are presented as firm expectations without any error budget, explicit sensitivity analysis, or reference to the specific number-count models and lensing optical-depth calculations on which they rest. Because these numbers constitute the central claim of the paper, the absence of even a brief derivation or citation to the underlying extrapolation assumptions is a load-bearing omission.
  2. [Abstract] Abstract (and implied main-text discussion of yields): the extrapolation implicitly assumes that the Euclidean-normalized differential counts dN/dS and the lensing probability continue with the same faint-end slope and redshift distribution below the current ~10–30 mJy limits and beyond z ~ 4. No test of the stability of these assumptions against plausible changes in the high-z population or magnification bias is provided; if either assumption fails, the predicted yields shift by factors of several, directly affecting the claimed discovery potential.
minor comments (2)
  1. [Abstract] Abstract: typographical error 'where' should read 'were' ('when their member galaxies where forming').
  2. [Abstract] Abstract: stray '{' character before 'stars'.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the constructive comments and for recognizing the potential impact of the science case. We address each major comment below.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the quantitative forecasts ('several thousands of strongly lensed galaxies out to z~6 or more' and 'galaxy proto-clusters') are presented as firm expectations without any error budget, explicit sensitivity analysis, or reference to the specific number-count models and lensing optical-depth calculations on which they rest. Because these numbers constitute the central claim of the paper, the absence of even a brief derivation or citation to the underlying extrapolation assumptions is a load-bearing omission.

    Authors: We agree that the abstract would be strengthened by explicit references to the underlying models. The quoted yields are extrapolations from the number counts and lensing optical depths already presented in the main text (drawing on Planck, SPT and ACT results). We will revise the abstract to include citations to the relevant number-count models and lensing calculations, together with a short parenthetical note on the extrapolation assumptions. revision: yes

  2. Referee: [Abstract] Abstract (and implied main-text discussion of yields): the extrapolation implicitly assumes that the Euclidean-normalized differential counts dN/dS and the lensing probability continue with the same faint-end slope and redshift distribution below the current ~10–30 mJy limits and beyond z ~ 4. No test of the stability of these assumptions against plausible changes in the high-z population or magnification bias is provided; if either assumption fails, the predicted yields shift by factors of several, directly affecting the claimed discovery potential.

    Authors: We acknowledge that a quantitative test of the stability of the faint-end slope and redshift distribution would be valuable. The main text already notes the reliance on current survey results, but we will add a brief sensitivity discussion (or reference to existing robustness checks in the cited literature) to address possible variations in the high-z population and magnification bias. revision: yes

Circularity Check

0 steps flagged

No circularity in forward-looking yield forecasts

full rationale

The paper presents observational forecasts for next-generation CMB experiments based on scaling existing Planck/SPT/ACT number counts and lensing optical depths. No derivations, equations, fitted parameters, or self-citations are shown that reduce any claimed yield to quantities defined by the authors' own prior work. The central claims are extrapolations relying on external literature, making the analysis self-contained against benchmarks outside the present manuscript.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The paper is a review of projected capabilities and contains no free parameters, axioms, or invented entities of its own; all quantitative statements rest on extrapolations from prior literature.

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