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The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): V. Protoplanetary gas disk masses

T0 review · 4 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read A homogeneous ALMA sample of 30 low-mass stars shows the median protoplanetary gas disk mass drops by roughly an order of magnitude between <1 Myr and 1–3 Myr, then roughly plateaus among surviving disks.

desk verdict A solid, transparent gas mass census; the direction of the decline is robust but the headline Ophiuchus median may be 2–3x too high. read the letter →

arxiv 2506.10738 v1 pith:L2YGAE5J submitted 2025-06-12 astro-ph.EP astro-ph.GAastro-ph.SR

Leon Trapman , Ke Zhang , Giovanni P. Rosotti , Paola Pinilla , Benoît Tabone , Ilaria Pascucci , Carolina Agurto-Gangas , Rossella Anania
show 14 more authors
John Carpenter Lucas A. Cieza Dingshan Deng Camilo González-Ruilova Michiel R. Hogerheijde Nicolás T. Kurtovic Aleksandra Kuznetsova James Miley Laura M. Pérez Dary A. Ruíz-Rodríguez Kamber Schwarz Anibal Sierra Estephani TorresVillanueva Miguel Vioque
This is my paper
classification astro-ph.EPastro-ph.GAastro-ph.SR
keywords protoplanetarydisksgasdiskmassCOisotopologuesN2H+thermochemicalmodelsevolutionALMAsurveystar-formingregions
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 tries to establish how the gas reservoir available for planet formation evolves over the first ten million years of a disk's life, using a homogeneous ALMA sample of thirty low-mass stars in three star-forming regions. Fitting a large thermochemical model grid to CO isotopologue and N2H+ observations, it reports that the median gas disk mass falls by roughly an order of magnitude, from about $7.0\times10^{-3}\,M_\odot$ in Ophiuchus (under 1 Myr) to about $9.4\times10^{-4}\,M_\odot$ in Lupus (1–3 Myr), and stays near $6.8\times10^{-4}\,M_\odot$ in Upper Sco (2–6 Myr), with roughly one dex of scatter in each region. Most of the decline therefore happens before about 1 Myr, after which the surviving disks change little in median mass, possibly because dispersal preferentially removes the lower-mass disks. The same fits imply that the CO abundance in the line-emitting layer is about ten times below the interstellar value and does not change between Lupus and Upper Sco, and that the gas-to-dust ratio rises by a factor of roughly three over that interval.

What carries the argument

The machinery is a grid of 2232 thermochemical disk models computed with the DALI code, spanning gas masses $10^{-6}$ to $0.5\,M_\odot$, characteristic radii 1–300 au, gas-to-dust ratios 10–1000, two vertical structures, two dust populations, four stellar spectra, six CO abundances, and three cosmic-ray ionization rates. Synthetic 13CO, C18O, N2H+, and continuum observables are interpolated piecewise-linearly and fit to the AGE-PRO fluxes with an MCMC sampler, with the 12CO 90% radius used to break mass–size degeneracies. The key lever is N2H+: because its abundance rises when CO freezes out or is depleted, the C18O/N2H+ pair simultaneously constrains gas mass and CO abundance. The ten Ophiuchus disks are fit separately using only C17O and continuum, under priors of near-ISM CO abundance and a luminosity-only (cold) temperature structure.

What would settle it

Measure gas masses independently of CO, for example with HD (1-0) far-infrared observations, for a matched sample of Ophiuchus and Lupus disks; if HD-based masses do not show a roughly tenfold drop between regions under 1 Myr and regions at 1–3 Myr, then the decline is an artifact of the CO/temperature assumptions rather than a true evolution of the gas reservoir.

Watch

Extended reading notes

Core claim

The central claim is that protoplanetary gas disk masses decline with stellar population age in a specific pattern: $7.0^{+4.4}_{-2.6}\times10^{-3}\,M_\odot$ in Ophiuchus (<1 Myr), $9.4^{+5.4}_{-3.4}\times10^{-4}\,M_\odot$ in Lupus (~1–3 Myr), and $6.8^{+5.1}_{-2.8}\times10^{-4}\,M_\odot$ in Upper Sco (~2–6 Myr), with ~1 dex scatter. The paper argues that almost all of this evolution occurs between Ophiuchus and Lupus, and that the similar Lupus and Upper Sco distributions are consistent with survivorship bias. It also claims the bulk CO abundance in the 13CO/C18O emitting layer is about $10^{-5}$, roughly ten times below the ISM, with no significant change from Lupus to Upper Sco, and that the median gas-to-dust mass ratio increases from ~40 in Lupus to ~120 in Upper Sco, implying dust is removed faster than gas at later ages.

Load-bearing premise

The claim rests on assuming Ophiuchus disks have near-ISM CO abundance and cold, luminosity-only temperatures, since warmer or already-depleted disks would give 2–3 times lower masses and shrink the tenfold decline to a factor of about 3–5.

Editorial extensions

If this is right

  • If the medians are right, the largest gas supply for giant-planet formation is present before 1 Myr; by 1–3 Myr the median reservoir is about a tenth of the early value and stays near that level among surviving disks to 5 Myr.
  • The constant, depleted CO abundance from Lupus to Upper Sco means CO is removed from the warm molecular layer within about the first Myr and then reaches a steady state.
  • The rising gas-to-dust ratio between Lupus and Upper Sco points to dust being removed by inward drift or planetesimal formation while gas remains.
  • Gas mass correlates strongly with observed CO and dust disk radii, so more massive disks are physically larger and can host substructures farther out.
  • Several compact disks have observed lifetimes $M_{\rm gas}/\dot{M}_{\rm acc}$ about ten times shorter than their region age, implying their accretion is episodic, their gas masses are underestimated, or they will disperse soon.

Reading between the lines

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

  • If the early drop is a real evolutionary feature, planet formation models that require a massive gas disk after 1 Myr need to build their cores faster than the inferred median timescale would allow.
  • A targeted test of the Ophiuchus calibration would be deep C17O observations of Class I disks with independent temperature constraints; warmer temperatures would lower derived masses by 2–3x and shrink the order-of-magnitude decline.
  • Applying the same CO+N2H+ fit to clusters older than 5 Myr would show whether the Lupus–Upper Sco plateau persists or is a survivorship-bias artifact.
  • A future far-infrared HD survey across ages would give CO-independent gas masses and directly test whether the tenfold CO abundance reduction is real or a model assumption.
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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

4 major / 5 minor

Summary. The paper presents a large grid of DALI thermochemical models and uses an MCMC forward-modeling approach to measure protoplanetary gas disk masses for 30 disks in the AGE-PRO survey, spanning Ophiuchus, Lupus, and Upper Sco. The authors simultaneously fit CO isotopologue fluxes, N2H+ fluxes, millimeter continuum fluxes, and measured CO disk sizes, and report median gas masses declining from 7.0e-3 Msun in Ophiuchus (<1 Myr) to 9.4e-4 Msun in Lupus and 6.8e-4 Msun in Upper Sco, with roughly one order of magnitude scatter. They also derive bulk CO abundances about a factor of ten below the ISM value and an increase in the median gas-to-dust mass ratio from Lupus to Upper Sco. Secondary results include correlations between gas mass and disk size and a discussion of disk lifetimes.

Significance. If the result holds, this is an important observational constraint on the early evolution of protoplanetary gas reservoirs, and it is one of the largest homogeneous samples in which gas masses are derived from CO isotopologues together with an N2H+ abundance constraint. The paper has several genuine strengths: the model grid and fitting code are made available; the priors are explicit in Table 5; the interpolation assumption is tested in Appendix D (5-20% flux underestimation); and the MCMC pipeline is benchmarked against HD-based masses for DM Tau, GM Aur, and TW Hya, with good agreement for the first two and a noted bimodality for TW Hya. The gas masses, CO abundances, and gas-to-dust ratios are honestly reported as outputs of a forward model rather than assumed constants, so there is no circularity in the central derivation. The main correctness risk is the calibration of the Ophiuchus sample, which rests on a specific 'cold' temperature model and on two sources whose cold-model posteriors peak at the edge of the model grid.

major comments (4)
  1. [Section 3.5 and Figure 7] The absolute Ophiuchus median is only as secure as the cold-model assumption. The warm models, with L* increased by a factor of ten, reduce individual Ophiuchus gas masses by factors of 2-3, and the paper itself states that the cold model is an upper limit and the warm model a lower limit on the mass. Because the headline claim is the factor of roughly 7-10 decline from Ophiuchus to Lupus, adopting warm-model values would shrink that contrast to roughly a factor of 2-3. The manuscript acknowledges this caveat but then proceeds with the cold-model values in Section 3.6. The authors should marginalize over the temperature ambiguity or present both medians side by side and qualify the 'order-of-magnitude' phrasing accordingly.
  2. [Section 3.5, Section 3.6, Table 2] For Oph 1 and Oph 7, the cold-model gas mass posteriors peak at the upper edge of the model grid, as the text states, so their reported values are upper limits rather than detections. In the Monte Carlo calculation of the region median, these sources are drawn as point masses from the posterior, which biases the Ophiuchus median upward. The median is also heavily influenced by the three most massive sources (Oph 1, 6, and 7). The region median should be recomputed treating Oph 1 and Oph 7 as censored data, for example with a Kaplan-Meier estimator or by explicitly marginalizing over masses beyond the grid edge, and the sensitivity of the median to this choice should be reported.
  3. [Section 3.5 and Figure 8] The gas-to-dust ratios derived for Oph 1, Oph 6, and Oph 7 are close to 10^3, which is difficult to reconcile with the assumption of ISM-like gas and the 'young' dust population adopted for these sources. The authors caution that the dust masses may be underestimated because of optical depth or opacity effects, but they still include these extreme ratios when quoting the Ophiuchus gas-to-dust distribution and when discussing the evolution of the gas-to-dust ratio. A quantitative robustness check, for example recomputing the Ophiuchus median after applying a conservative dust-mass correction or after removing the three high-ratio sources, is needed to see whether the 'increase by a factor of 3 from Lupus to Upper Sco' conclusion survives.
  4. [Section 3.6 and Figure 9] The quoted uncertainties on the region medians include only the measurement uncertainties on individual gas masses and not the statistical uncertainty due to the limited sample size of ten disks per region. The paper notes this in the text, but the central comparison of the three medians is still presented without a sampling uncertainty. A bootstrap or hierarchical calculation should be added to show whether the Ophiuchus-Lupus contrast remains statistically significant under the cold-model assumption; this does not affect the direction of the result, but it is load-bearing for the strength of the 'order-of-magnitude decline' claim.
minor comments (5)
  1. [Section 3.6] The text contains a typo: 'Kaplar-Meier' should be 'Kaplan-Meier'.
  2. [Throughout] There are small spacing/formatting issues in the text, such as 'DALImodels' and 'It is is not unsurprising'; these should be corrected during editing.
  3. [Section 3.5] The phrase '(see, e.g. 20)' should be '(see, e.g., Figure 20)' or 'see Appendix H' for clarity.
  4. [Section 3.4 and Table 5] In the description of the MCMC priors, the Gaussian prior on stellar luminosity is said to have a 30% uncertainty, but Table 5 lists per-source values with different standard deviations; a brief note explaining how these were derived would be helpful.
  5. [Appendix B] The HD benchmark section reports that TW Hya's posterior is bimodal and correlated with the cosmic-ray ionization rate; the text should state explicitly whether this bimodality is considered a limitation of the N2H+ method or a consequence of the prior range, as the current wording leaves this open.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: gas masses are forward-model fits benchmarked against independent HD data.

full rationale

The paper derives gas disk masses by inverting a large thermochemical model grid against CO isotopologue and N2H+ fluxes with an MCMC sampler. The headline quantities (median gas masses per region, bulk CO abundances, gas-to-dust ratios) are posterior estimates from those fits, not constants recovered by construction. The Ophiuchus masses use an explicitly stated prior of near-ISM CO abundance and a cold temperature model, but this is a model assumption, not a fitted parameter renamed as a prediction; the paper quantifies the effect of warmer models (2-3x lower masses) and explicitly labels Oph 1 and Oph 7 as upper limits because their cold-model posteriors peak at the grid edge. The method is benchmarked against independent HD-based gas masses for TW Hya, DM Tau, and GM Aur in Appendix B, and the N2H+-based CO abundance constraint is independently supported by the thermochemical code of Anderson et al. (2019, 2022). Citations to Trapman et al. provide methodological benchmarks and analytical formulas, but the load-bearing validation relies on external Herschel HD data and independent codes, so no self-citation chain forces the results. The reported correlations (e.g., Mgas vs R_CO,90%) are post-hoc and do not define the gas masses. While the Ophiuchus median is sensitive to temperature and envelope assumptions, that is a robustness/caveat, not circularity; the paper states these caveats explicitly. No step in the derivation reduces to its own input by definition or by fitted-constant construction.

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

The central measurement rests on a large model grid with several chosen, unconstrained inputs and one post-hoc assumption. The fitted quantities (Mgas, xCO, zeta_CR) are honest outputs, but the claims depend on the following free parameters or priors: the peak CO abundance grid and its log-uniform prior; the cosmic ray ionization rate grid; the fixed 20 K dust temperature used to convert continuum flux to dust mass, which directly sets the gas-to-dust ratio claim; and the Ophiuchus-specific near-ISM CO prior. The key axioms are the faithfulness of the DALI code, the validity of global CO scaling as a proxy for chemical processing, the N2-as-main-nitrogen-carrier assumption, the linear interpolation between grid points, and the cold-model and near-ISM treatment of Ophiuchus. No new physical entities are introduced.

free parameters (4)
  • Peak CO gas-phase abundance (xCO) = Median ~1.4e-5 (Lupus) and ~2.0e-5 (Upper Sco); grid values 3e-7 to 1e-4
    Free grid parameter fitted to C18O and N2H+ fluxes; the claim that bulk CO is ~10x below ISM is this fitted value (Table 1, Section 3.4).
  • Cosmic ray ionization rate (zeta_CR) = Grid values 1e-19, 1e-18, 1e-17 s-1 with log-uniform prior; low-zeta_CR posteriors favored for compact disks
    Fitted through the N2H+ flux; N2H+ emission varies roughly 3x per dex of zeta_CR, directly shifting the derived gas masses (Section 2.1.2, Figure 2).
  • Dust temperature for continuum-derived dust masses = 20 K
    All dust masses and hence gas-to-dust ratios assume a single 20 K optically thin conversion; the paper accepts order-of-magnitude uncertainty on dust masses (Table 2 note, Section 3.6).
  • Ophiuchus CO abundance prior = xCO restricted to [3e-5, 1e-4], near ISM
    Adopted for the ten Class I disks instead of fitting the full xCO range; if CO is already depleted in Ophiuchus the derived masses would be lower (Section 3.5).
assumptions (6)
  • domain assumption DALI thermochemical code correctly computes dust/gas temperatures, chemistry, excitation, and ray-traced line fluxes for the modeled disk structures
    All synthetic observables come from DALI (Bruderer et al. 2012; Section 2); no independent verification of the code's accuracy is given in this paper.
  • ad hoc to paper Global scaling of the CO abundance structure reproduces the line fluxes of a disk with genuinely depleted CO
    Post-processing scaling makes the model 'no longer fully self-consistent' (Section 2); Appendix A validates it within 30% for the AGE-PRO flux range but finds C18O offsets of factor 1 to 4 for xCO=1e-6 in compact disks.
  • domain assumption N2 is the main nitrogen carrier with ISM-like abundance
    The van 't Hoff et al. (2017) N2H+ network assumes this; Section 4.3 states that N2 depletion would lower N2H+ emission and thus underestimate gas masses, and that the observational support is limited to a few disks.
  • ad hoc to paper Piece-wise linear interpolation between grid points is accurate
    Required for the MCMC (Section 3.4); Appendix D finds the interpolation underestimates 13CO/C18O/N2H+ fluxes by 5 to 20%, which the authors note could slightly overestimate masses.
  • ad hoc to paper Ophiuchus Class I disks have near-ISM CO and are not substantially envelope-heated ('cold model')
    Section 3.5: adopted for the ten youngest disks; warm models (10x luminosity proxy) give 2 to 3x lower masses, and the paper adopts the cold model 'with the explicit caveat that the gas masses could be lower'.
  • standard math The tapered powerlaw surface density with gamma=1 describes the gas distribution of all sample disks
    Standard self-similar viscous disk solution (Lynden-Bell and Pringle 1974), Eq. 1; the paper notes Upper Sco 1 has a gas gap that violates this assumption.

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Cite this review

Pith. "Pith review of The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): V. Protoplanetary gas disk masses." pith.science (2026). https://pith.science/paper/L2YGAE5J

@misc{pith2026250610738,
  author       = {Pith},
  title        = {Pith review of: The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO): V. Protoplanetary gas disk masses},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/L2YGAE5J}},
  note         = {Machine review of arXiv:2506.10738}
}
read the original abstract

The evolution of the gas mass of planet-forming disks around young stars is crucial for our understanding of planet formation, yet it has proven hard to constrain observationally, due both to the difficulties of measuring gas masses and the lack of a homogeneous sample. Here we present a large grid of thermochemical models which we use to measure protoplanetary gas disk masses of AGE-PRO, the ALMA survey of Gas Evolution in PROtoplanetary disks. AGE-PRO covers a sample of 30 disks around similar spectral type (M3-K6) stars with ages between 0.1 and 10 Myr. Our approach is to simultaneously fit observations of CO isotopologues and N2H+, a complementary molecule produced when CO freezes out. We find that the median gas mass of the three regions decreases over time, from 7.0(+4.4,-2.6)x10^-3 Msun in Ophiuchus (<1 Myr) to 9.4(+5.4,-3.4)x10^-4 Msun for Lupus (~1-3 Myr) and 6.8(+5.1,-2.8)x10^-4 Msun for Upper Sco (~2-6 Myr), with ~1 dex scatter in gas mass in each region. We note that the gas mass distributions for Lupus and Upper Sco look very similar, which could be due to survivorship bias for the latter. The median bulk CO abundance in the CO emitting layer is found to be a factor ~10 lower than the ISM value but does not significantly change between Lupus and Upper Sco. From Lupus to Upper Sco the median gas-to-dust mass ratio increases by a factor ~3 from ~40 to ~120, suggesting efficient inward pebble drift and/or the formation of planetesimals.

Figures

Figures reproduced from arXiv: 2506.10738 by the authors.

Figure 1
Figure 1. Flow chart of processes to generate the AGE-PRO model grid. The square boxes show actions and ellipses show outputs after each action step. Gas disk mass: The gas disk mass (Mdisk) is covered by seven values from Mdisk = 10−6 M⊙ up to 0.5M⊙. The range of masses in the grid grew dynamically over the course of this work in order to cover all AGE-PRO sources. Disk size: Similarly, the range for disk size (Rc), seven va… view at source ↗
Figure 2
Figure 2. Top panels: 13CO and C18O 2-1 line luminosities (i = 0 ◦ ) for models with a gas mass of Mgas = 10−3 M⊙. The same models are shown in each panel, with colors highlighting the effect of different disk parameters on the line luminosity (see [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. 13CO and C18O J = 2−1 line luminosities for the AGE-PRO sources in Lupus and Upper Sco compared to our grid of thermochemical disk models with xCO = 10−4 . The rightmost panels zoom in on the part of the main figure that contains the bulk of the AGE-PRO observations. One source, Lupus 10 (V1094 Sco) lies outside this region. A diagonal shaded region show the absolute flux uncertainty expected for ALMA Band 6. The co… view at source ↗
Figures from the paper (25 more)
Figure 4
Figure 4. Figure 4: N2H + 3-2 and C18O 2-1 line luminosities for our models and the AGE-PRO sources. Observations for Lupus and Upper Sco are shown in black and purple, respectively. Circles denote detections in both lines and diamonds denote 1σ for non-detections in both lines. In case o…
Figure 5
Figure 5. Figure 5: Example posterior distributions of Mgas and xCO for Lupus 2 (Sz 71/GW Lup), using constraints from fluxes of the 13CO, C 18O, N2H + lines, and 1.3 mm continuum. Shown at the top of each panel and by the vertical dashed line are the 16th, 50th, and 84th quantile of each…
Figure 6
Figure 6. Figure 6: Posterior probability distribution of Mgas obtained from fitting either the observed integrated 13CO 2-1, C18O 2-1, N2H +3-2, and 1300µm continuum fluxes (Lupus and Upper Sco) or the C17O 2-1 and 1.300 µm continuum fluxes (Ophiuchus) using the MCMC routine outline in S…
Figure 7
Figure 7. Figure 7: Comparison of the Ophiuchus gas disk masses derived using cold (L∗ = L∗, obs) and hot (L∗ = 10 × L∗, obs) models. A comparison of the posterior distributions is presented in [PITH_FULL_IMAGE:figures/full_fig_p014_7.png]
Figure 8
Figure 8. Figure 8: From top to bottom, left panels show the gas disk masses, gas-to-dust mass ratios and bulk CO gas abundance for sources in Ophiuchus (gray pentagons), Lupus (brown circles), and Upper Sco (green diamonds), all set against their dust disk mass. The markers show the medi…
Figure 10
Figure 10. Figure 10: Gas disk mass versus stellar age for individual disks is within the uncertainties of the median gas masses. Con￾tributing to the overlap in the median gas masses is the large spread of individual disks, including a few relatively old (>4 Myr) Upper Sco disks with high…
Figure 11
Figure 11. Figure 11: Top left: The correlation between Mgas and RCO, 90%, the latter being obtained from the best fit Nuker profile of the 12CO 2-1 emission (see Trapman et al. 2025, in press. for details). Black circles and purple diamonds represent sources in Lupus and Upper Sco, respec…
Figure 12
Figure 12. Figure 12: Disk mass versus stellar mass accretion rate for disks in Lupus (black) and Upper Sco (purple). The gray errorbar shows typical uncertainty of the accretion rate (see Alcala et al. ´ 2017; Ma￾nara et al. 2020). Dotted gray lines show different disk lifetimes, defined …
Figure 13
Figure 13. Figure 13: Lupus and Upper Sco gas masses derived using either ζCR ∈ [10−19 , 10−17] s−1 (clear markers) or ζCR ∈ [10−20 , 10−19] s−1 (solid markers) as a prior for the cosmic ray ionization rate (see Section 3.4 for details). Note that in most cases decreasing ζCR in￾creases Mg…
Figure 14
Figure 14. Figure 14: Top row: line fluxes of models with low C/H and O/H elemental ratios. The grey dash line indicates the 3σ detection level of AGE￾PRO observations. Bottom row: line flux ratios between the models with initial low elemental ratios with models with scaled CO abundance st…
Figure 15
Figure 15. Figure 15: Posterior distribution of Mgas, Rc , xCO, ζcr, and L∗ for TW Hya (top), DM Tau (middle), and GM Aur (bottom). Black vertical dashed lines show the 16th, 50th, and 84th quantile of the distribution. Shown in orange are the HD-based gas mass and the corresponding xCO fr…
Figure 16
Figure 16. Figure 16: Comparison of the accuracy of gas mass constraints without (left) and with (right) N2H + for the Lupus 3 source [PITH_FULL_IMAGE:figures/full_fig_p030_16.png]
Figure 17
Figure 17. Figure 17: left panels: 13CO 2-1, C18O 2-1, and N2H + 3-2 line fluxes as a function of “flaring”-ness (i.e. (ψx%, h100,x%)) for an example disk with Mgas = 10−3 M⊙ and Rc = 60 au. Black crosses denote “flat” and “flared” models that are in the model grid, with the dashed gray li…
Figure 18
Figure 18. Figure 18: As [PITH_FULL_IMAGE:figures/full_fig_p033_18.png]
Figure 19
Figure 19. Figure 19: Joint posterior probability distribution of Mgas and xCO obtained from fitting the observed integrated 13CO 2-1, C18O 2-1, N2H +3-2, and 1300µm continuum fluxes using MCMC. Orange dashed lines show the best fit Mgas and xCO for each disk. Oph 1 Oph 2 Oph 3 Oph 4 Oph 5…
Figure 20
Figure 20. Figure 20 [PITH_FULL_IMAGE:figures/full_fig_p034_20.png]
Figure 21
Figure 21. Figure 21: Left: distribution of derived Rc for Lupus 3 based its RCO, 90%, Mgas, and L∗. Middle: Difference between the best fitting disk size (RCO, 90%,est) and the observed value (RCO, 90%,obs). Right: Comparison of the full posterior distribution of Mgas and the portion samp…
Figure 22
Figure 22. Figure 22: Comparison of the characteristic radii (Rc) obtained from the MCMC fit described in Section 3.4 to the analytically computed Rc discussed in Appendix I. J. EXTRA FIGURES OF THE CORRELATIONS BETWEEN DISK AND STELLAR PROPERTIES K. CORNER PLOTS OF THE MCMC Fig. Set 26. C…
Figure 23
Figure 23. Figure 23: Gas mass versus effective temperature (Teff), stellar mass (M∗), stellar luminosity (L∗), gas disk outer radius (RCO, 90%), dust disk outer radius (Rdust, 90%), and the characteristic radius Rc for the twenty disks in Lupus (black) and Upper Sco (purple). See Appendix…
Figure 24
Figure 24. Figure 24: Results of the Monte Carlo Spearman rank tests, quantified by ρ, between Mgas and various stellar and disk parameters. Left panels show the distribution of ρ and right panels show the associated p-value. Orange vertical lines in each panel show the 16th, 50th, and 84t…
Figure 25
Figure 25. Figure 25: As [PITH_FULL_IMAGE:figures/full_fig_p040_25.png]
Figure 26
Figure 26. Figure 26: As [PITH_FULL_IMAGE:figures/full_fig_p041_26.png]
Figure 27
Figure 27. Figure 27: As [PITH_FULL_IMAGE:figures/full_fig_p042_27.png]
Figure 28
Figure 28. Figure 28: As [PITH_FULL_IMAGE:figures/full_fig_p043_28.png]
Figure 26
Figure 26. Figure 26: Posterior probability distributions of the model parameters obtained from fitting the observed integrated 13CO 2-1, C18O 2-1, N2H +3-2, and 1300µm continuum fluxes and the gas disk size (RCO, 90%) of Lupus 1 (Sz 65) using MCMC. Vertical dashed lines show the 16th , 50…

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Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.