The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ~1 Gyr old I. Survey overview and case studies

A. D. Bolatto; A. Ferrara; A. Posses; A. Sternberg; D. Fisher; D. Liu; D. Lutz; D. Narayanan; E. da Cunha; G. Calistro Rivera

REVIEW 3 major objections 5 minor 4 cited by

The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ~1 Gyr old I. Survey overview and case studies

T0 review · 3 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read The paper claims that kiloparsec-resolution ALMA imaging of 39 star-forming galaxies at z≈4–6 shows [C II] gas extending beyond starlight, an Arp 220-like deficit in one region, and a [C II]/FIR deficit trend shifted toward higher…

desk verdict A well-executed, data-rich survey overview that delivers a valuable public kiloparsec-resolved [CII] sample at z~4-6; the global [CII]/FIR results are plausible but carry an unquantified dust-temperature dependence that should be addressed before publication. read the letter →

arxiv 2505.06340 v1 pith:OXQXGVNR submitted 2025-05-09 astro-ph.GA

R. Herrera-Camus , J. González-López , N. Förster Schreiber , M. Aravena , I. de Looze , J. Spilker , K. Tadaki , L. Barcos-Muñoz

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R. J. Assef J. E. Birkin A. D. Bolatto R. Bouwens S. Bovino R. A. A. Bowler G. Calistro Rivera E. da Cunha R. I. Davies R. L. Davies T. Díaz-Santos A. Ferrara D. Fisher R. Genzel J. Hodge R. Ikeda M. Killi L. Lee Y. Li J. Li D. Liu D. Lutz I. Mitsuhashi D. Narayanan T. Naab M. Palla S. H. Price A. Posses M. Relaño R. Smit M. Solimano A. Sternberg L. Tacconi K. Telikova H. Übler S. A. van der Giessen S. Veilleux V. Villanueva M. Baeza-Garay

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classification astro-ph.GA

keywords high-redshiftgalaxiesinterstellarmedium[CII]158μmemissionmain-sequencestar-forminggalaxykinematicsmergersdustcontinuumALMAsurvey

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 CRISTAL survey maps the 158 μm [C II] line and dust continuum at roughly kiloparsec resolution in 39 main-sequence star-forming galaxies that lived when the Universe was about 1 billion years old, and combines those ALMA data with HST and JWST imaging of the same systems. The paper's central claim is that the cold interstellar medium of these early galaxies is not a simple mirror of their stars: [C II] emission commonly extends well beyond the stellar light, and the resolved morphologies range from rotating disks to mergers, tidal tails, and clumpy complexes. It further claims that the global [C II]/FIR ratio declines with FIR luminosity as it does locally, but the whole trend sits at higher luminosities, consistent with larger molecular gas reservoirs. Two case studies anchor the argument: a kiloparsec-scale dusty region in CRISTAL-10 has a [C II]/FIR ratio as low as the extreme local system Arp 220, and the young stellar clumps of CRISTAL-13 are spatially offset from the [C II] emission, interpreted as feedback dispersing or evaporating the gas. If these claims hold, the survey establishes a kiloparsec-resolution benchmark for interpreting gas, dust, and star formation in the first billion years of cosmic history.

What carries the argument

The argument is carried by the [C II]-to-far-infrared luminosity ratio, L[CII]/LFIR, a standard proxy for the photoelectric heating efficiency of neutral interstellar gas; the paper's central comparison is the well-known ‘[C II] deficit’, the decline of this ratio with increasing FIR luminosity or FIR surface brightness. The observational machinery is the combination of ALMA Band 7 observations with synthesized beams of roughly 0.1 to 0.7 arcseconds, HST/WFC3 and JWST/NIRCam imaging, and SED fitting from companion papers that supplies stellar masses, star formation rates, FIR luminosities, and dust continuum sizes. For the case studies, the FIR luminosity is derived from a single Band 7 continuum measurement assuming a dust temperature of 50 K for CRISTAL-10 and 40 K for CRISTAL-13, and the paper shows how the [C II]/FIR ratios move under a ±10 K temperature change.

What would settle it

Measure the dust spectral energy distribution of CRISTAL-10's Region 1 with a longer-wavelength ALMA band (for instance Band 9) or with JWST/MIRI to obtain a direct dust temperature; if the temperature is about 60–70 K rather than 50 K, the inferred far-infrared luminosity rises enough that [C II]/FIR climbs out of the Arp 220 regime and the extreme-deficit case fails. For the global relation, re-fitting the CRISTAL SEDs with additional submillimeter photometry or different dust templates would settle whether the shift of the [C II]/FIR–LFIR trend relative to local galaxies is real.

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Extended reading notes

Core claim

On its own terms, the paper establishes that typical star-forming galaxies at z ≈ 4–6 contain a cold gas reservoir that is systematically more extended and more disturbed than the rest-frame UV and optical starlight suggests. In many CRISTAL systems the [C II] emission reaches two to three times the extent of the stellar light, and roughly half the sample is classified as disk-dominated while at least a third shows clear interaction or merger signatures. The paper also reports a global trend: the [C II]/FIR ratio declines with FIR luminosity as in local galaxies but shifted to higher luminosities, which it attributes to higher molecular gas content. At FIR surface brightnesses of about $10^{9}$ to $10^{11}$ Lsun/$kpc^{2}$, a range previously unexplored at high redshift, CRISTAL galaxies show elevated [C II]/FIR ratios relative to z ≈ 0 galaxies at the same surface brightness, with lower metallicity, extraplanar gas, and shock excitation offered as likely contributors. The two case studies are CRISTAL-10, where a ~3 kpc dusty region reaches L[CII]/LFIR = 2.5 × $10^{-4}$, comparable to Arp 220, and CRISTAL-13, where six young stellar clumps are anti-correlated with [C II] peaks, consistent with feedback clearing the surrounding gas.

Load-bearing premise

The load-bearing premise is that the far-infrared luminosities and surface brightnesses entering the [C II]/FIR ratios are accurate: the global values come from SED fits, while the CRISTAL-10 and CRISTAL-13 case studies convert a single ALMA Band 7 continuum measurement into a far-infrared luminosity by assuming dust temperatures of 50 K and 40 K, so if the true dust temperatures or SED assumptions differ, the extreme-deficit claims and the position of the high-redshift trend move.

Editorial extensions

If this is right

Low-resolution [C II] measurements at z ≈ 4–6 misclassify a substantial fraction of galaxies: once seen at kiloparsec resolution, about half of the CRISTAL systems are disk-dominated and at least a third show interaction or merger signatures.
Source-integrated [C II]/FIR ratios can hide localized extreme deficits, since CRISTAL-10's global ratio is about ten times higher than its most obscured region; resolved measurements are therefore needed to diagnose the ISM conditions in high-redshift starbursts.
If the shifted [C II]/FIR–LFIR trend is caused by higher molecular gas content, direct CO or [C I] observations of CRISTAL galaxies should find gas fractions well above local values at comparable stellar mass and star formation rate.
At fixed FIR surface brightness, high-redshift galaxies with log Σ_FIR between about 11.5 and 13.5 (in Lsun/kpc^2) have [C II]/FIR ratios three to ten times higher than local galaxies, implying elevated photoelectric heating efficiency or extra diffuse and shocked [C II] emission.
Extended [C II] envelopes around many CRISTAL galaxies mean that [C II] sizes should not be used as proxies for stellar or disk sizes in early-Universe galaxies, because they overestimate the spatial extent of star formation.

Reading between the lines

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

A direct test of the gas-fraction explanation: CO(2–1) or [C I] observations of a subset of CRISTAL galaxies should recover molecular gas fractions roughly ten times higher than local main-sequence galaxies at matched specific star formation rate; if they do not, the shifted [C II]/FIR–LFIR relation needs another driver.
The metallicity explanation predicts a spatial correlation within galaxies: regions with the highest [C II]/FIR ratios should also have the lowest gas-phase metallicities when mapped with JWST/NIRSpec, an internal test the current data cannot yet make.
The CRISTAL-13 feedback interpretation implies an age ordering: the six western clumps should be younger than the roughly 10 Myr photoevaporation timescale, while older clumps should sit closer to [C II] peaks; resolved stellar-age maps can falsify this ordering.
Extending the same method to fainter FIR surface brightness or to z > 6 would test whether the elevated [C II]/FIR branch continues or turns over as CMB effects on diffuse gas grow, sharpening the boundary between local and early-Universe ISM physics.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

The CRISTAL survey paper does exactly what a good survey overview should: it puts a large, homogeneous, public dataset on the table. The 39 galaxies with kiloparsec-scale [CII] and dust continuum, plus HST and JWST ancillary imaging, are a genuine step forward for studying normal star-forming galaxies at z~4-6. The data reduction is documented in detail, fluxes from three independent methods agree within 10% for most sources, and the cross-checks against ALPINE and visibility-plane measurements give me confidence in the measurements themselves. That part is solid.

The science highlights are also reasonable. CRISTAL-10's spatially resolved [CII] deficit is interesting, and CRISTAL-13's offset between young stellar clumps and [CII] peaks is a nice, concrete example of feedback at work. The paper is honest about the assumptions: the case studies state their adopted dust temperatures and show the sensitivity to ±10 K. That is good practice.

Where I part ways with the paper's framing is the global [CII]/FIR analysis in Section 9. The FIR luminosities come from a single ALMA Band 7 continuum point and SED fits, and the dust-temperature degeneracy is not propagated into the z~0 comparison shown in Figure 14. Equation (2) is a new empirical relation with no fit uncertainties. A factor of 2-3 shift in LFIR - well within plausible SED systematics - would move the CRISTAL points diagonally and could weaken the claimed 'previously unexplored ΣFIR range' and the 3-10× offset from local galaxies. The stress-test note about this is fair. It is not a fatal flaw, but it is a real gap in the quantitative argument, and it is easily fixable with error bars and a caveat.

A second soft spot: several interpretive claims cite in-prep companion papers as support (Lee et al., Birkin et al., Herrera-Camus et al., etc.). That is normal for a survey paper, but it makes it hard to evaluate some conclusions independently without digging into the companion papers. The core data release stands on its own, though.

Who is this for? Anyone working on high-redshift ISM, galaxy structure, or ALMA surveys. The sample and data products will be used for years. It deserves peer review, but the referee should ask for quantified uncertainties on Eq. (2) and an explicit statement about the SED assumptions in the global comparison. I would take the paper with those revisions.

Referee Report

3 major / 5 minor

Summary. This paper presents the CRISTAL survey overview, an ALMA Cycle 8 Large Program targeting 39 main-sequence star-forming galaxies at 4≲z≲6 with Band 7 [CII] 158 μm and dust continuum observations at ~kpc resolution, combined with HST/WFC3 and JWST/NIRCam imaging. The authors describe the sample selection, ALMA calibration and imaging, and the final data products, and report global line fluxes and continuum fluxes measured with three complementary methods (aperture photometry, 2D Gaussian fits, and S/N-threshold integration) that agree within ~10% except for four interacting systems. The science highlights include: (i) diverse morphologies and kinematics, with [CII] often more extended than the stellar light; (ii) CRISTAL-10, where a dust-bright region lacking a UV counterpart has [CII]/FIR ≈ 2.5×10⁻⁴, comparable to Arp 220; (iii) CRISTAL-13, where six young stellar clumps are spatially anti-correlated with the [CII] emission; and (iv) a global analysis showing that CRISTAL galaxies follow a [CII]/FIR versus FIR luminosity deficit trend shifted to higher luminosities, and occupy a Σ_FIR range of roughly 10⁹–10¹¹ L☉ kpc⁻² with higher [CII]/FIR at fixed Σ_FIR than local galaxies.

Significance. The paper delivers a valuable public dataset and a well-documented reduction, with multiple cross-checks: three independent flux measurement methods agree, and the fluxes are consistent with ALPINE and with visibility-plane measurements from Mitsuhashi et al. (2024). The resolved [CII]-to-stellar-light comparisons, the kinematic/morphological census, and the identification of extended [CII] beyond stellar light are important contributions to high-redshift ISM studies. However, the quantitative ISM claims—the Arp 220-like deficit in CRISTAL-10, the PDR/feedback interpretation in CRISTAL-13, and the global offset in the [CII]/FIR–Σ_FIR plane—depend on FIR luminosities that are not fully characterized: most global values come from SED fits with a single Band 7 continuum constraint, and the case-study values rely on assumed dust temperatures. The claims are plausible and interesting, but the lack of propagated uncertainties currently makes the quantitative conclusions stronger than the underlying evidence.

major comments (3)

[Section 9, Eqs. (1)–(2) and Fig. 14] The manuscript does not state the wavelength range used to define L_FIR for the CRISTAL and Spilker et al. high-redshift samples, while the local comparison sample (Lutz et al. 2016; Herrera-Camus et al. 2018a) is, by standard usage, the 42.5–122.5 μm FIR band. If the high-z L_FIR values are total 8–1000 μm luminosities (as typically output by SED fitting codes such as CIGALE or MAGPHYS), the [CII]/L_FIR ratios and Σ_FIR values in Fig. 14 are systematically biased relative to the z≈0 sample. Please state the adopted passband definitions explicitly for all samples and, if they differ, recompute the comparison with matched definitions.
[Section 9, Eq. (2) and Fig. 14] Equation (2) is presented with fixed numerical coefficients and no quoted uncertainties, and the CRISTAL points in Fig. 14 have no error bars reflecting SED systematics. For most CRISTAL galaxies the only far-IR constraint is a single ALMA Band 7 continuum point (Mitsuhashi et al. 2024), so L_FIR is controlled by assumed dust temperature and emissivity index; a factor of ~2–3 change in L_FIR is plausible. Such variations shift points diagonally in both panels of Fig. 14 and can alter the claimed 3–10× offset and the 'previously unexplored' Σ_FIR range. I request that the authors quote the uncertainties on the coefficients of Eq. (2) and provide a sensitivity band for the CRISTAL sample, for example for ±10 K in T_dust or for a plausible range of β.
[Sections 8.1 and 8.2, Figs. 12–13] The quantitative case-study results rely on L_FIR derived from the Band 7 continuum assuming T_dust = 50 K (CRISTAL-10) and 40 K (CRISTAL-13). The ±10 K sensitivity bar is shown only for CRISTAL-10 in Fig. 12, and the text acknowledges that 'the dust temperature could potentially be higher'; no such sensitivity is shown for CRISTAL-13. The qualitative interpretations—Region 1 as Arp 220-like and the eastern component as a dense PDR—would be better supported by reporting the full range of [CII]/F_IR for a plausible range of (T_dust, β) and by clearly stating how the conclusions would change if the adopted temperatures are incorrect.

minor comments (5)

[Section 3.1] Typo: 'the initial CRISTAL sample consist of 19 galaxies' should read 'consists of 19 galaxies'.
[Section 7.1] The sentence 'The [C II] and continuum fluxes in Table 2 agree on average within a ~10% and ~20% with the fluxes measured in Ikeda et al. (2025) and Mitsuhashi et al. (2024)' is ambiguous: it is not clear which quantity agrees to 10% and which to 20%, or with which reference.
[Figure 14 caption] The caption for the right panel states 'best fit to the data at z≈0 and z≈3–6 (this work; Eq. 2)', but the fit includes both CRISTAL galaxies and Spilker et al. (2016) systems; please specify the exact sample and Σ_FIR range used for the fit.
[Section 2.5] Typo: 'There results are further supported' should be 'These results are further supported'.
[Section 5.2] The paper notes that the JvM effect is not corrected, but the released data products would benefit from an explicit statement in the data-release documentation telling users whether the correction should be applied; a sentence in Section 5.2 or the repository documentation would suffice.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the paper's claims are observational measurements and empirical fits, not derivations from their own inputs; self-citations to companion papers are data sources, not unverified premises that force the conclusions.

full rationale

The derivation chain is observational. [CII] fluxes and Band 7 continuum are measured in Section 7 and Table 2; FIR luminosities are taken from SED fits in Mitsuhashi et al. (2024) or, in the case studies, from the Band 7 continuum under explicitly stated dust-temperature assumptions (Section 8.1 with T_dust = 50 K; Section 8.2 with T_dust = 40 K). The [CII]/FIR ratios and Sigma_FIR values are then formed from these measured or assumed quantities and compared against external z approximately 0 samples (Lutz et al. 2016; Herrera-Camus et al. 2018a) and high-z samples (Spilker et al. 2016). Equation (2) is an empirical fit to the plotted data, not a prediction claimed from a held-out subset. The case-study comparisons to Arp 220 and Orion are external benchmarks, not consequences of the assumed dust temperatures. The paper cites companion papers by the same team for data products, but those citations supply independent measurements and analyses rather than an unverified theorem that forces the stated conclusions. The main caveat is systematic: LFIR for most CRISTAL galaxies rests on single-band continuum plus SED assumptions, with dust-temperature uncertainties not propagated into the global Figure 14 points; this affects accuracy and significance, not logical circularity. No step reduces, by construction, to its own input.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

The central claims rest on standard cosmology and IMF assumptions, SED-derived stellar and FIR properties from companion papers, and two adopted dust temperatures for the case-study regions. The main empirical result is a fitted quadratic relation with three free coefficients and no quoted uncertainties. No new physical entities are introduced.

free parameters (3)

Coefficients of the z~3-6 [CII]/FIR vs log10(Sigma_FIR) quadratic (Eq. 2) = intercept -8.4163, linear 1.3245, quadratic -0.0731
Empirical fit to CRISTAL and Spilker et al. (2016) data; no uncertainties or scatter are quoted.
Assumed dust temperature for CRISTAL-10 regions 1 and 2 = T_dust = 50 K
Converts Band 7 continuum to FIR luminosity for the [CII]/FIR measurements; the paper shows the effect of a 40-60 K range.
Assumed dust temperature for the CRISTAL-13 eastern component = T_dust = 40 K
Used for the [CII]/FIR ratio quoted in Section 8.2; from Faisst et al. (2020a) and Villanueva et al. (2024).

assumptions (6)

domain assumption A flat Lambda-CDM cosmology (Omega_M=0.3, Omega_Lambda=0.7, H0=70 km/s/Mpc) is assumed.
Stated in Section 1; all luminosities and physical scales depend on this cosmology.
domain assumption Stellar masses and star formation rates are normalized to a Chabrier (2003) IMF.
Stated in Section 1; SED-derived quantities from companion papers follow this normalization.
domain assumption SED fitting codes (CIGALE, MAGPHYS) give reliable stellar masses, SFRs, and FIR luminosities.
Adopted from Mitsuhashi et al. (2024), Li et al. (2024), and Lines et al. (2024); these quantities feed the [CII]/FIR analysis and sample properties.
domain assumption The [CII]/FIR ratio can be used as a tracer of photoelectric heating efficiency.
Section 9; standard PDR assumption, with acknowledged caveats about other coolants and non-PDR contributions.
ad hoc to paper A dust temperature of 50 K for CRISTAL-10 and 40 K for CRISTAL-13 regions is representative.
Assumed for FIR luminosity from single-band continuum in the case studies; sensitivity is shown for ±10 K but not propagated globally.
domain assumption The JvM effect is negligible for these images because cleaning was deep (nsigma=1).
Section 5.2; the paper argues the effect is minimal, with a more detailed assessment deferred to a companion paper.

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Cite this review

Pith. "Pith review of The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ~1 Gyr old I. Survey overview and case studies." pith.science (2026). https://pith.science/paper/OXQXGVNR

@misc{pith2026250506340,
  author       = {Pith},
  title        = {Pith review of: The ALMA-CRISTAL survey: Gas, dust, and stars in star-forming galaxies when the Universe was ~1 Gyr old I. Survey overview and case studies},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OXQXGVNR}},
  note         = {Machine review of arXiv:2505.06340}
}

abstract

We present the ALMA-CRISTAL survey, an ALMA Cycle 8 Large Program designed to investigate the physical properties of star-forming galaxies at $4 \lesssim z \lesssim 6$ through spatially resolved, multi-wavelength observations. This survey targets 19 star-forming main-sequence galaxies selected from the ALPINE survey, using ALMA Band 7 observations to study [CII] 158 $\mu$m line emission and dust continuum, complemented by JWST/NIRCam and HST imaging to map stellar and UV emission. The CRISTAL sample expanded to 39 after including newly detected galaxies in the CRISTAL fields, archival data, and pilot study targets. The resulting dataset provides a detailed view of gas, dust, and stellar structures on kiloparsec scales at the end of the era of reionization. The survey reveals diverse morphologies and kinematics, including rotating disks, merging systems, [CII] emission tails from potential interactions, and clumpy star formation. Notably, the [CII] emission in many cases extends beyond the stellar light seen in HST and JWST imaging. Scientific highlights include CRISTAL-10, exhibiting an extreme [CII] deficit similar to Arp 220; and CRISTAL-13, where feedback from young star-forming clumps likely causes an offset between the stellar clumps and the peaks of [CII] emission. CRISTAL galaxies exhibit global [CII]/FIR ratios that decrease with increasing FIR luminosity, similar to trends seen in local galaxies but shifted to higher luminosities, likely due to their higher molecular gas content. CRISTAL galaxies also span a previously unexplored range of global FIR surface brightness at high-redshift, showing that high-redshift galaxies can have elevated [CII]/FIR ratios. These elevated ratios are likely influenced by factors such as lower metallicity gas, the presence of significant extraplanar gas, and contributions from shock-excited gas.

Figures

Figures reproduced from arXiv: 2505.06340 by the authors.

**Figure 1.** Histograms showing the distribution of redshift (left), stellar mass (center), and star formation rate (right) for the CRISTAL (green), ALPINE (gray; Le Fèvre et al. 2020; Béthermin et al. 2020; Faisst et al. 2020b), and REBELS samples (gold; Bouwens et al. 2022) [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗

**Figure 2.** The CRISTAL sample consists of 39 star-forming galaxies between 4 ≲ z ≲ 6 that are representative of the population of massive (M⋆ ≳ 109 M⊙) galaxies at this redshift range. The figure shows the stellar mass-star formation rate plane for galaxies between 4 ≲ z ≲ 6. CRISTAL galaxies are shown as green circles, color-coded according to their redshift. The main-sequence of star-forming galaxies at z = 5 is shown follo… view at source ↗

**Figure 3.** Histogram showing the distribution of observing time (first panel), synthesized beam size (second panel), noise measured in the cubes for 20 km s−1 channels (third panel) and Band 7 continuum (fourth panel). The average values for ALPINE galaxies (Le Fèvre et al. 2020; Béthermin et al. 2020; Faisst et al. 2020b) are indicated by a gray line. criteria of stellar mass (Mstar ≥ 109.5 M⊙), observability, and the availab… view at source ↗

Figures from the paper (11 more)

**Figure 4.** Figure 4: Comparison between the ALPINE and CRISTAL [Cii] observations of the CRISTAL-05 galaxy at z = 5.5 (Posses et al. 2024). (Top) [Cii] integrated intensity map based on the ALPINE Natural weighting observations (left), and the CRISTAL higher-angular observations using the …

**Figure 5.** Figure 5: [Cii] 158 µm line surveys of typical or main-sequence star-forming galaxies as a function of redshift. The surveys included are: Herschel Space Observatory-based KINGFISH (Kennicutt et al. 2011) and SHINING (Graciá-Carpio et al. 2011; Herrera-Camus et al. 2018a,b), as …

**Figure 7.** Figure 7: [Cii] integrated flux measured from the CRISTAL and ALPINE data. The colorscale represents the S/N of the integrated line detection in the ALPINE data (Béthermin et al. 2020). In general there is good agreement between the CRISTAL and ALPINE fluxes, except for four sys…

**Figure 6.** Figure 6: [Cii] 158 µm line spectra for all the star-forming galaxies in the CRISTAL sample listed in [PITH_FULL_IMAGE:figures/full_fig_p011_6.png]

**Figure 8.** Figure 8: Position in the sky of the CRISTAL galaxies including the JWST pointings footprints from programs COSMOS-Web, PRIMER, JADES, and FRESCO, and HST pointings footprints from programs COSMOS-DASH, CANDELS, and 3D-HST. CRISTAL galaxies from the original sample, pilot progra…

**Figure 9.** Figure 9: [Cii] integrated line emission maps for the CRISTAL galaxies, constructed from the naturally weighted cubes. All maps have been scaled to the same physical size, indicated by a white line on the left side representing 6 kpc. The colorscale represents the integrated flu…

**Figure 10.** Figure 10: JWST composite images of CRISTAL galaxies, overlaid with [C ii] line emission (white contours) and dust continuum emission (pink contours). Contour levels correspond to [3, 5, 10]σ, except for CRISTAL-01, where the emission intensity is shown on a logarithmic scale, a…

**Figure 11.** Figure 11: Multi-wavelength view of the CRISTAL galaxies including from left to right: integrated [C ii] line emission, [C ii]-based velocity field, dust continuum emission, [Cii] and dust continuum emission overlaid on a composite image based on HST/WFC3 and JWST/NIRCam observa…

**Figure 12.** Figure 12: (Left) Multi-wavelength view of CRISTAL-10, a main-sequence star-forming galaxy at z = 5.67. The background image is a composite of three HST/WFC3 filters, highlighting the rest-frame UV stellar light emitted by young, massive stars. Overlaid on this image are white c…

**Figure 13.** Figure 13: (Left) Composite image based on three JWST/NIRCam blue filters (F090W, F115W, F150W) that show the stellar light from multiple young stellar clumps in CRISTAL-13, a main-sequence star-forming galaxy at z = 4.58. Overlaid are the integrated [C ii] line emission (white …

**Figure 14.** Figure 14: (Left) [Cii]/FIR luminosity ratio as a function of the FIR luminosity observed in nearby star-forming galaxies and starbursts (beige points; Lutz et al. 2016; Herrera-Camus et al. 2018a) and high-z star-forming galaxies (gray points; Spilker et al. 2016, and reference…

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Forward citations

Cited by 4 Pith papers

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