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REVIEW 3 major objections 4 minor 136 references

Into the Mystic: the MUSE view of the ionized gas in the Mystic Mountains in Carina

T0 review · 3 major / 4 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read This paper maps the ionized gas on Carina's Mystic Mountains with MUSE and concludes the complex will be fully photoevaporated in $8\pm2$ Myr, with the smallest globules surviving longest and shielding embedded protostars for more than a…

desk verdict Nice MUSE dataset with a real arithmetic error in the lifetime section: the complex-wide photoevaporation rate is averaged instead of summed, so 8 Myr becomes ~1 Myr. read the letter →

arxiv 2501.18029 v1 pith:YPO75AFP submitted 2025-01-29 astro-ph.GA

Megan Reiter , Anna F. McLeod , Dominika Itrich , Pamela D. Klaassen This is my paper · ORCID
classification astro-ph.GA
keywords photoevaporationdustpillarsCarinaNebulaHIIregionsHerbig-Haroobjectsintegralfieldspectroscopyionizingfeedbackplanetformationshielding
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

This paper uses MUSE integral-field spectroscopy to map the hot ionized gas on the surface of the Mystic Mountains, a dust-pillar complex in the Carina Nebula sitting about a parsec from the intense ultraviolet field of Trumpler 14. The maps give electron densities, temperatures, ionization, and extinction across the pillars, and they show the jets HH 901, HH 902, and HH 1066 to be high-density, low-ionization outflows, with HH 901 surrounded by neutral-carbon emission that traces a molecular outflow dissociating in the H II region. Combining local photoevaporation rates with ALMA molecular-gas masses, the paper argues that the whole complex will be completely evaporated in $8\pm2$ Myr, that individual pillars and globules have remaining lifetimes from about 1 to 13 Myr, and that the longest-lived structures are the smallest. That pattern is interpreted as evidence that ionizing radiation has compressed the pillars, enhancing the shielding of embedded young stars and disks for more than 1 Myr, even though the data do not show triggered star formation. If right, this quantifies a key variable for planet formation in high-mass regions like Carina, where most stars form.

What carries the argument

The load-bearing machinery is MUSE's continuous spatial and spectral coverage from 4650 to 9300 Å, which lets the authors measure line ratios pixel by pixel: [S II] $\lambda6731/6717$ for electron density, [N II] $\lambda5755/(6548+6583)$ for temperature, He I $\lambda6678$/[S II] for ionization, and H$\alpha$/H$\beta$ for extinction. The photoevaporation rates come from the side-illuminated-cylinder expression $\dot{M}\simeq 2\pi r^2 m_H n_H v$, where $r$ is the fitted radius of curvature of each pillar head, $n_H=1.4n_e$, and $v\approx10$ km s$^{-1}$ is the sound speed of ionized gas. These rates are divided into the ALMA molecular masses to obtain local and global remaining lifetimes, while the [C I] 8727 Å line serves as the tracer of dissociation in the photoevaporating HH 901 outflow.

What would settle it

Integrate the total mass-loss rate over the entire evaporating surface of the Mystic Mountains—for example, from the spatially integrated H$\alpha$ or radio recombination-line flux, which counts every ionized surface—rather than averaging eight local rates. If the integrated rate comes out near $3\times10^{-5}\,M_\odot\,\mathrm{yr^{-1}}$, the complex-wide lifetime is about 1 Myr, directly contradicting the $8\pm2$ Myr claim.

Watch

Extended reading notes

Core claim

On its own terms, the paper establishes that the Mystic Mountains are being eroded from the outside in by UV photons from Trumpler 14, and that the erosion is readable in the ionized gas. The MUSE data show electron densities often above $10^3\,\mathrm{cm^{-3}}$ concentrated at pillar heads and ionization fronts, electron temperatures near $10^4$ K, and a sharp drop in ionization at pillar boundaries; the jets appear as high-density, low-ionization features, and extended [C I] 8727 Å emission along HH 901 traces the dissociation of its molecular outflow. Using the side-illuminated-cylinder formula, the authors derive local photoevaporation rates from $2\times10^{-7}$ to $1.2\times10^{-5}\,M_\odot\,\mathrm{yr^{-1}}$. Averaged, these give $\sim4\times10^{-6}\,M_\odot\,\mathrm{yr^{-1}}$, and with the complex's ALMA-measured molecular mass of $33.7\pm5.7\,M_\odot$, the authors conclude that the entire Mystic Mountains will be gone in $8\pm2$ Myr, with sub-pillars ranging from about 1 to 13 Myr. The inverse correlation between structure size and lifetime — the smallest globules last longest, independent of distance from the ionizing cluster — leads them to propose that ionization-driven compression, not triggered collapse, is what keeps the embedded stars' cocoons intact, shielding the HH 901 young star for $\gtrsim2.5$ Myr.

Load-bearing premise

The load-bearing premise is that the mean of the eight local photoevaporation rates, roughly $4\times10^{-6}\,M_\odot\,\mathrm{yr^{-1}}$, is the total rate at which the entire $33.7\,M_\odot$ complex is being eroded; if the tabulated rates are summed instead, the total is about $3.1\times10^{-5}\,M_\odot\,\mathrm{yr^{-1}}$ and the remaining lifetime drops to roughly 1 Myr rather than $8\pm2$ Myr.

Editorial extensions

If this is right

  • The Mystic Mountains as a whole will be completely evaporated in $8\pm2$ Myr, while individual pillars and globules have remaining lifetimes between about 1 and 13 Myr.
  • The smallest structures have the longest remaining lifetimes regardless of their distance from Trumpler 14, supporting the view that ionizing feedback has compressed them and increased their shielding.
  • The HH 901 embedded young star will remain shielded behind its globule for $\gtrsim2.5$ Myr, long enough for planet formation to proceed with limited external photoevaporation under current disk-evolution models.
  • Embedded young stars in the complex will be revealed at different times as the surrounding gas is stripped, so the exposed protostar population reflects ongoing erosion rather than a single burst of triggered star formation.
  • Extended [C I] emission along HH 901 marks the rapid dissociation of a photoevaporating molecular outflow once it leaves the pillar, showing directly how external UV destroys outflows.

Reading between the lines

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

  • If the tabulated local photoevaporation rates are summed rather than averaged, the total mass-loss rate is about $3.1\times10^{-5}\,M_\odot\,\mathrm{yr^{-1}}$, shortening the complex-wide lifetime to roughly 1 Myr; the $8\pm2$ Myr conclusion thus depends on how well the eight measured interfaces represent the whole evaporating surface.
  • The observed pattern that small structures survive longest implies a selection effect for pillar surveys: large, fragile structures are destroyed quickly, so samples of surviving pillars may over-represent compact globules and understate the true photoevaporation rate of a region.
  • A testable follow-up is to measure proper motions of the HH 901 and HH 1066 globules over several years; acceleration away from Trumpler 14 would confirm the rocket-effect compression invoked here, while no acceleration would favor pre-existing overdensities as the origin of the pillars.
  • For planet-formation modeling, these results imply that a single shielding time per region is insufficient, since shielding varies by more than an order of magnitude within one complex; disk photoevaporation models should use spatially resolved gas-clearing times.
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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. This paper presents MUSE integral-field observations of the Mystic Mountains, a heavily irradiated pillar complex in Carina, and derives maps of extinction, electron density, electron temperature, and ionization state across the region. The authors measure local photoevaporation rates at eight pillar-head interfaces using the Smith et al. (2004) cylinder formula (Eq. 1), combine these with ALMA-derived molecular masses from Reiter et al. (2023), and estimate the remaining lifetime of the complex (8 ± 2 Myr) and of its individual pillars. They report that the longest remaining lifetimes belong to the smallest structures, interpret this as evidence of compression by ionizing feedback, and discuss the shielding time available for embedded YSOs and disks relative to planet-formation models. The paper also analyzes the HH 901, 902, and 1066 jets, reports a new candidate jet seen only in [Fe II], and identifies extended [C I] emission from HH 901 as tracing dissociation of a photoevaporating molecular outflow.

Significance. If the quantitative lifetime results are correct, the paper would provide an unusually complete, spatially resolved picture of feedback in a high-mass star-forming region, connecting ionized-gas diagnostics with cold molecular gas and with implications for triggered star formation and the shielding of planet-forming disks. The observational products—density/temperature/excitation maps, jet P-V diagrams, the [C I] dissociation structure, and the candidate jet—are valuable and are based on public MUSE and ALMA data, with clear potential for reuse. However, the central quantitative claim (lifetime of 8 ± 2 Myr and the statement that the smallest structures live longest) is not supported by the paper's own tabulated rates because the total photoevaporation rate is computed as the arithmetic mean of eight local rates rather than their sum. The qualitative morphological findings and the new jet/C I detections stand independently, but the lifetime and shielding-time conclusions need reworking.

major comments (3)
  1. [Section 4.3, Table 2] The complex-wide lifetime is obtained by dividing the total molecular mass M = 33.7 ± 5.7 M_sun (Table 3) by an 'average photoevaporation rate' of ~4 × 10^-6 M_sun/yr, which is the arithmetic mean of the eight local rates listed in Table 2. The total photoevaporation rate of the complex should instead be the sum over all ionized surfaces; summing the eight tabulated rates gives ~3.1 × 10^-5 M_sun/yr, which yields a remaining lifetime of ~1.1 Myr rather than 8 ± 2 Myr. Since the eight extraction regions do not cover the full ionized boundary of the complex, the summed rate is a lower limit, so the true complex lifetime is likely even shorter. The paper's own tabulated data therefore do not support the headline lifetime quoted in the abstract and Section 4.3.
  2. [Section 4.3, Table 3] The per-pillar lifetimes are computed by dividing a pillar's molecular mass by a single local mass-loss rate at the pillar tip (e.g., HH 901 mass divided by 2.0 × 10^-7 M_sun/yr gives ~16 Myr for the full pillar and ~2.6 Myr for its envelope). This ignores photoevaporation from other ionized surfaces of the same pillar, such as the high-density spine of HH 901 and the extended ionization fronts present in the HH 902 and HH 1066 pillars. Consequently, the conclusion that 'the longest remaining lifetimes are for the smallest structures' is not established by the data as presented; it may be an artifact of selecting the smallest local rate for each pillar. The authors should integrate the mass-loss rate over each pillar's full ionized boundary, or explicitly state that the quoted lifetimes are lower limits based on a single interface.
  3. [Section 4.3 and Conclusions] The shielding-time argument (comparing with the ~1.5 Myr threshold from Qiao et al. 2023) depends directly on the lifetimes from the two previous points. With the total rate corrected to the sum of the tabulated values, the complex-wide shielding time becomes roughly 1 Myr or less, and the per-pillar values are likely shorter once additional ionized surfaces are included. The claim that embedded YSOs and disks in the Mystic Mountains remain shielded for more than 1 Myr therefore needs to be re-evaluated and re-stated with the corrected rates, or explicitly qualified as applying only to the local pillar-tip geometry.
minor comments (4)
  1. [Section 4.1, Eq. (1)] The radius of curvature r is described as 'the radius of the circle that best matches the curvature at the pillar head'; the fitting procedure and its uncertainty should be documented in more detail, since r enters quadratically in the mass-loss rate and is likely a dominant systematic.
  2. [Section 4.3] The stated uncertainty of ±2 Myr on the 8 Myr lifetime reflects only the 17% mass uncertainty; the substantial scatter in the local photoevaporation rates (over two orders of magnitude) and the systematic uncertainty in r are not propagated into this estimate.
  3. [Figure 6 and Section 3.4] The figure caption labels the orange circles as 'Reiter et al. 2024' while the text (Section 3.4) and reference list cite Reiter et al. (2023) for these 1.3 mm continuum sources; the citation in the caption should be corrected.
  4. [Abstract] The phrase 'we compute the photoevaporation rate' and the resulting lifetime figure in the abstract do not convey that the quoted value is based on an average of local rates rather than a total; adding a short qualifier would help readers avoid the aggregation error highlighted above.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the photoevaporation rates and ALMA masses are independent inputs combined through a literature formula; the mean-versus-sum lifetime issue is an aggregation concern, not a circular one.

full rationale

The paper's central derivation is a straightforward combination of measured inputs through a literature formula. The local photoevaporation rates in Table 2 are computed from MUSE-derived electron densities, temperatures, and measured radii of curvature using the Smith et al. (2004) cylinder formula (Section 4.1, Eq. 1). The remaining lifetime is then the ALMA-derived molecular mass (Reiter et al. 2023, Table 3) divided by a photoevaporation rate (Section 4.3). No fitted parameter is used to force the resulting lifetime: the rates are measured from the ionized gas and the masses are measured from the cold molecular gas, and neither quantity is derived from the other. The self-citations to Reiter et al. (2023) and Itrich et al. (2024) supply data products with independent observational bases, not an imported uniqueness theorem or ansatz that determines the conclusion. The skeptical critique that the complex-wide lifetime uses the arithmetic mean of eight local rates rather than their sum is a legitimate statistical and physical aggregation concern, and it changes the numerical lifetime, but it does not make the derivation self-referential: t = M / Mdot remains an externally grounded ratio of two independent measurements. Similarly, the statement that the smallest structures have the longest remaining lifetimes is a scaling consequence of dividing each structure's mass by its own local photoevaporation rate, not a circularly imposed premise. No step in the derivation reduces by construction to its own inputs, so the circularity score is 0.

Assumptions & free parameters 1 free parameters · 6 assumptions · 0 invented entities

The central claim rests on a simple photoevaporation model, assumed geometry, and masses from the authors' prior ALMA work. The most fragile element is the treatment of the arithmetic mean as the total mass-loss rate, which appears to be an error. No new physical entities are introduced.

free parameters (1)
  • radius of curvature r at each pillar head = 0.01 pc (HH 901), 0.07 pc (HH 902 a/b), 0.03 pc (HH 902 c, mm5 b), etc.
    Measured by fitting a circle to the curvature at each ionized interface; enters the mass-loss rate quadratically in Eq. 1, and the choice is subjective.
assumptions (6)
  • domain assumption The photoevaporation mass-loss rate is given by the cylinder formula Mdot ~ 2 pi r^2 m_H n_H v (Smith et al. 2004, Eq. 1).
    Used in Section 4.1 for all interfaces.
  • domain assumption n_H = 1.4 n_e
    Converts electron density to hydrogen nucleus density, stated in Section 4.1.
  • domain assumption The outflow velocity v equals the sound speed of ionized gas (about 10 km/s).
    From ideal isothermal gas with Te about 8000 to 10500 K, Section 4.1.
  • standard math Case B recombination with T = 10^4 K and n_e = 10^3 cm^-3 gives (H-alpha/H-beta)_int = 2.86.
    Used for extinction correction, Section 3.1.
  • domain assumption The molecular gas masses from Reiter et al. (2023) are accurate.
    Used in Section 4.3 for lifetimes; masses have large uncertainties (e.g., HH 901: 3.31 +/- 2.64 M_sun).
  • ad hoc to paper The arithmetic mean of local photoevaporation rates represents the total rate for the complex.
    Implicit in Section 4.3; if false, the 8 Myr lifetime is invalid.

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Cite this review

Pith. "Pith review of Into the Mystic: the MUSE view of the ionized gas in the Mystic Mountains in Carina." pith.science (2026). https://pith.science/paper/YPO75AFP

@misc{pith2026250118029,
  author       = {Pith},
  title        = {Pith review of: Into the Mystic: the MUSE view of the ionized gas in the Mystic Mountains in Carina},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YPO75AFP}},
  note         = {Machine review of arXiv:2501.18029}
}
read the original abstract

We present optical integral field unit (IFU) observations of the Mystic Mountains, a dust pillar complex in the center of the Carina Nebula that is heavily irradiated by the nearby young massive cluster Trumpler 14. With the continuous spatial and spectral coverage of data from the Multi-Unit Spectroscopic Explorer (MUSE), we measure the physical properties in the ionized gas including the electron density and temperature, excitation, and ionization. MUSE also provides an excellent view of the famous jets HH 901, 902, and 1066, revealing them to be high-density, low-ionization outflows despite the harsh environment. HH 901 shows spatially extended [C I] emission tracing the rapid dissociation of the photoevaporating molecular outflow in this highly irradiated source. We compute the photoevaporation rate of the Mystic Mountains and combine it with recent ALMA observations of the cold molecular gas to estimate the remaining lifetime of the Mystic Mountains and the corresponding shielding time for the embedded protostars. The longest remaining lifetimes are for the smallest structures, suggesting that they have been compressed by ionizing feedback. Our data do not suggest that star formation in the Mystic Mountains has been triggered but it does point to the role that ionization-driven compression may play in enhancing the shielding of embedded stars and disks. Planet formation models suggest that the shielding time is a strong determinant of the mass and orbital architecture of planets, making it important to quantify in high-mass regions like Carina that represent the type of environment where most stars form.

Figures

Figures reproduced from arXiv: 2501.18029 by the authors.

Figure 1
Figure 1. Color image showing the entire Tr14 MUSE survey area (north is up, east is to the left). The Mystic Mountains are ∼ 1 pc to the north (in projection) of the Tr14 young massive cluster. The zoomed in image shown to the right highlights the subset of the data used in this work with the famous jets HH 901, HH 902, and HH 1066 labelled. To align each MUSE cube with Gaia, we used the astrometry python package from Wenzl … view at source ↗
Figure 2
Figure 2. (a) 𝐴𝑉 map of the Mystic Mountains, derived from the short exposures (see also Appendix A). (b) Electron density (𝑛𝑒) derived from the ratio [S ii] 𝜆6731/6717 Å. (c) Electron temperature (𝑇𝑒) derived from [N ii] 𝜆5755/𝜆6584 + 𝜆6548 Å. White circles show the regions used to compute the quantities in [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. [S ii] 𝜆6717Å map with red circles showing where the quantities in [PITH_FULL_IMAGE:figures/full_fig_p005_3.png] view at source ↗
Figures from the paper (7 more)
Figure 4
Figure 4. Figure 4: Left: Map of [C i] 8727 Å showing the entire Mystic Mountains. Red lines show the location where the intensity tracings in [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 5
Figure 5. Figure 5: Locations of tracings shown in [PITH_FULL_IMAGE:figures/full_fig_p007_5.png]
Figure 7
Figure 7. Figure 7: Map of [C i] 8727 Å emission from HH 901. Blue contours show the emission as 8725.2 Å and red contours show emission at 8728.9 Å. Extended [C i] emission suggests that HH 901 is a photoevaporating molecular outflow. 10 h44m03 s 02 s 01 s 00 s $ -59°30'25" 30" 35" RA (I…
Figure 8
Figure 8. Figure 8: [O i] image of HH 902 showing the large amount of neutral material in the jet. 10 h44m06.5 s 06.0 s 05.5 s 05.0 s -59°29'36" 39" 42" 45" RA (ICRS) Dec (ICRS) [PITH_FULL_IMAGE:figures/full_fig_p008_8.png]
Figure 9
Figure 9. Figure 9: [Fe ii] 8617 Å image of HH 1066 with blue contours showing emission in the range 8611.4–8615.2 Å and red contours showing emission in the range 8617.7–8622.7 Å. MNRAS 000, 1–14 (2025) [PITH_FULL_IMAGE:figures/full_fig_p008_9.png]
Figure 10
Figure 10. Figure 10: [Fe ii] 8617 Å image showing candidate jet with C18O contours overplotted. Peak of C18O emission is slightly offset from the position of the star that appears to drive the jet. external irradiation and compare it to the cold, molecular gas proper￾ties from Reiter et a…
Figure 11
Figure 11. Figure 11: Electron density maps (grayscale) with contours of millimeter emission overlaid. The top panel shows CO J=2-1 detected with ≥ 5𝜎. Contours show 20-100% of the maximum emission in steps of 10%. The middle panel shows C18O J=2-1 detected with ≥ 5𝜎 also with contours fro…

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Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.