Pith. sign in

REVIEW 3 major objections 4 minor 300 references

By decomposing the 10–400 GHz radio spectra of 20 protostars into dust and ionised-gas emission, this paper finds circumstellar disks tens to hundreds of times more massive than millimeter-only estimates, with grains already grown to millim

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-01 23:14 UTC pith:YZYBHLLI

load-bearing objection Valuable new dataset and outflow connections, but the headline dust-mass factors rest on a thermal-only radio model that the paper's own spectral indices undermine. the 3 major comments →

arxiv 2607.15468 v1 pith:YZYBHLLI submitted 2026-07-16 astro-ph.GA astro-ph.SR

A JWST, ALMA and VLA survey of the Ophiuchus-A star-forming region: Unveiling hidden dust mass and connecting infrared outflows to their radio origins

Isaac C. Radley , John D. Ilee , Gemma Busquet , Hauyu Baobab Liu , Klaus M. Pontoppidan , Alvaro Ribas , Marc Audard , Eleonora Bianchi
show 13 more authors
Tyler L. Bourke Claudio Codella Audrey Coutens Josep M. Girart Melvin G. Hoare Izaskun Jim\'enez-Serra Doug Johnstone Laurent Loinard Olja Pani\'c Jaime E. Pineda Linda Podio John J. Tobin David J. Wilner
This is my paper
classification astro-ph.GA astro-ph.SR
keywords star formationprotoplanetary disksdust growthdust massradio spectral energy distributionmissing disk mass problemprotostellar jetsOphiuchus L1688
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

This paper tries to show that the standard way of weighing protoplanetary disks—using a single millimeter flux measurement—misses most of the dust, because the millimeter emission is often optically thick and because the grains have grown to sizes that radiate efficiently only at longer wavelengths. Combining high-resolution VLA radio images with JWST infrared images and archival ALMA data, the authors decompose each source's full radio spectrum into a dust component and an ionised-gas component. Their models imply dust masses on average 150 times larger than 1.3 mm estimates with one widely used opacity law, and 34 times larger with another. If correct, this largely dissolves the long-standing 'missing disk mass' problem, because even the most evolved Class II disks would contain enough solid material to build multiple gas-giant cores. The same observations also align 10 GHz radio emission with outflow cavities seen by JWST, tying protostellar jets to their launching regions.

Core claim

The central claim is that single-wavelength millimeter flux densities severely underestimate the mass of dust in young circumstellar disks. Fitting a physical model to each object's 10–400 GHz SED—dust emission with a size distribution, self-scattering, and DSHARP opacities, plus a thermal free-free component from ionised gas—the authors find disk-integrated dust masses that are, on average, 150 times (DSHARP opacities) and 34 times (Beckwith power-law opacities) the mass derived from a 1.3 mm flux density alone, with a minimum increase of 11 times. They also infer maximum grain sizes of order a millimeter even at the Class 0 stage, and attribute the large mass difference to high optical dep

What carries the argument

The load-bearing tool is the millimetre–centimetre radio spectral energy distribution (SED) decomposition. Each source's observed flux densities from 10 GHz to 400 GHz are fitted with a two-component model: (1) dust emission assuming an MRN grain-size power law, uniform temperature and maximum grain size, DSHARP dust opacities, and the inclusion of dust self-scattering; and (2) ionised gas as a modified blackbody free-free source with a fixed electron temperature of 8000 K. The fit yields dust column density, solid angle, maximum grain size, temperature, and an emission measure. These SED-derived masses are then compared with the standard single-wavelength mass formula using a 1.3 mm flux de

Load-bearing premise

The load-bearing assumption is that all emission below roughly 45 GHz that is not accounted for by a single thermal free-free component with an electron temperature of 8000 K is optically thin dust emission with uniform temperature, one maximum grain size, and DSHARP opacities—if some of that cm-wave emission is non-thermal gyrosynchrotron radiation, or if the opacity model is wrong, the 'tens to hundreds of times' mass inflation collapses.

What would settle it

Measure the 10–45 GHz spectral index, circular polarisation, and short-timescale variability of a few of these sources (for example GSS30-IRS3 or VLA 1623 W) with VLA A-configuration. A negative spectral index, high degree of circular polarisation, or minute-to-hour variability would indicate gyrosynchrotron emission contaminating the cm-wave band, invalidating the thermal free-free plus dust decomposition. Alternatively, if a next-generation interferometer resolves the 44 GHz continuum of a Class 0 disk and finds it compact and optically thick rather than extended and optically thin, the infe

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Millimeter-only disk mass surveys are biased low by large factors, so the apparent deficit of solid material in protoplanetary disks is partly an observational artifact rather than a real shortage.
  • Even Class II disks in this sample retain 10s–100s of Earth masses of dust, enough to assemble multiple gas-giant cores without requiring near-100% planet formation efficiency.
  • Dust growth to millimeter sizes occurs already in Class 0 and Class I stages, not just in older disks, constraining when the growth barriers of bouncing, fragmentation, and radial drift must be overcome.
  • At 10 GHz, ionised gas dominates most of the sample (more than 70% of the flux), so cm-wave data cannot be interpreted as dust without a spectral decomposition.
  • The sharp drop in flux density between 40 and 100 GHz seen in roughly half the sample is explained by a transition from optically thick to optically thin dust emission, not by an ionised-gas excess.
  • Future high-resolution, low-frequency observations with facilities like SKA and ngVLA should spatially resolve the optically thin dust and confirm the launching radii of the jets the authors identify.

Where Pith is reading between the lines

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

  • If the mass-inflation factors are correct, then disk evolution models and exoplanet demographics should be re-calibrated: the same observed millimeter fluxes imply much larger initial mass reservoirs, softening the tension between measured disk masses and the masses of observed exoplanets.
  • A direct testable extension would be to spatially resolve 7–10 mm continuum of a Class 0 disk with next-generation interferometers; the model predicts extended, optically thin dust emission that traces the millimeter disk, whereas compact, variable, or polarised emission would betray a non-thermal origin.
  • The same SED decomposition could be applied to other nearby star-forming regions to test whether Ophiuchus is typical; if similar mass inflation appears everywhere, the 'missing disk mass' problem may be largely a wavelength-coverage bias.
  • The fixed 8000 K electron temperature and the single-zone dust model are simplifications; a radially stratified dust model with a temperature gradient could alter the derived masses, though the broadband spectral shape would need to remain consistent with the observed SED.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper presents a multi-wavelength survey of 20 Class 0–III YSOs in Ophiuchus A, combining new VLA 10/22/44 GHz continuum imaging with JWST/NIRCam images and archival ALMA fluxes. The authors fit power-law and physical two-component SED models to derive dust and ionised-gas properties, infer maximum grain sizes and dust masses, and connect 10 GHz extensions to jet/outflow cavities seen by JWST. The headline claim is that SED-derived dust masses are tens to hundreds of times larger than standard 1.3 mm-only estimates, with mm-sized grains present even at Class 0, offering a partial solution to the 'missing disk mass' problem.

Significance. The observational dataset itself is valuable: homogeneous VLA A-configuration continuum at 7–25 au resolution, careful variability screening, and a rich morphological connection between 10 GHz emission and NIRCam outflow cavities. If the mass-enhancement claim survived model-selection scrutiny, it would be important for early grain growth and the planet-formation mass budget. However, the central claim is conditional on an assumption that all ionised gas emission is thermal free-free and on a specific DSHARP opacity model; the paper does not propagate model-selection or opacity-systematic uncertainties into the headline factors. The survey and outflow-origin results are solid and publishable, but the mass claim needs substantial additional testing or reframing.

major comments (3)
  1. [§3.4.1 / §3.4.2 / Table 2] The physical SED model in §3.4.2 includes only one ionised-gas component: thermal free-free with Te fixed at 8000 K. Yet §3.4.1 finds α_ionised ≈ −0.2 ± 0.2 for Class II objects, states that these are 'more dominated by non-thermal gyro-emission', and explicitly notes for GSS30-IRS2 that its α_ionised is 'consistent with non-thermal gyro-emission... which is not captured in our thermal free-free model'. Table 2 shows f_ion > 70% at 10 GHz for most sources, so the low-frequency dust component is a small residual. If gyrosynchrotron emission contributes at 22–44 GHz, the thermal-only fit will tend to absorb its steep negative spectral index into the dust component, directly inflating the fitted Mdust and the 11–380x enhancement factors. No polarization or spectral-index test is offered to rule out this contamination. The abstract's opacity caveat does not cover this model-selection uncerta
  2. [§4.2 / Eq. (5) / Table 3] The mass-enhancement ratios are not an independent validation. Equation (5) is evaluated using 1.3 mm flux densities and T_dust, α_dust, and κ taken from the same SED model that produced Table 3. For κ_ν,DSHARP, the comparison is essentially between the integrated SED-model mass and a single-frequency projection of that model; for κ_ν,β, the opacity is derived from the model's α_dust. The reported 'minimum increase of 11 times' and the averages of 150 and 34 times are therefore conditional on the assumed opacity law and on the dust/ionised-gas decomposition. The text acknowledges opacity sensitivity in general terms, but no systematic uncertainty from opacity composition, porosity, or non-thermal contamination is propagated into the headline factors. The central claim should either be quoted with a range that includes these systematics or explicitly restricted to a sub-sample where the t
  3. [§3.4.2 / DoAr24, DoAr24Eb / Table 3] The imposed EM upper limit for DoAr24 and DoAr24Eb is justified only as providing 'solutions in line with the rest of the sample'. This is a per-object prior adjustment made after inspecting the data, and it directly affects the inferred dust component. DoAr24Eb then receives amax = 239 mm and Mdust = 211 M⊕, and it is included in the sample-level claims. No independent constraint on EM is given, and no sensitivity test shows that the headline mass-enhancement factors are robust to this choice. This needs either external justification or an explicit statement of how the results change if the cap is relaxed.
minor comments (4)
  1. [§3.4.2] A paragraph discussing optically thick emission at >200 GHz, dust self-scattering, and DSHARP opacities appears twice nearly verbatim. Please remove the duplication.
  2. [§2] Typo: 'Table 1 gives they key information' should read 'the key information'.
  3. [§3.4.1] The prior description says the ionised gas spectral index may vary 'between 1.5, the lower limit expected from dust self scattering, and –2'. This mixes dust and ionised-gas regimes; presumably the intended upper limit is 1.5 for the ionised component, and the parenthetical should be corrected.
  4. [Figure 7 / §3.4.2] VSSG27 is absent from Figure 7 because 'no valid solution was found', but the caption and discussion do not explain this. Please note in the caption that VSSG27 is excluded and state how its exclusion affects any sample averages.

Circularity Check

0 steps flagged

No circular reduction; SED-derived masses are model inferences, not identities; self-citations are methodological and non-load-bearing; gyrosynchrotron caveat is a correctness risk, not circularity.

full rationale

The central claim (Section 4.2, 'a minimum increase of 11 times the mass derived from a 1.3mm flux density measurement') arises from comparing two quantities derived from the same observational data: the full radio-SED model mass (Section 3.4.2) and the single-band Hildebrand mass (Eq. 5). This is an internal model comparison, not a prediction from withheld data. The SED model mass is not defined in terms of the 1.3mm mass; it is fit from free parameters (T_dust, a_max, Sigma_dust, Omega_dust, EM, Omega_ionised) across 10-400 GHz. The ratio M_SED/M_1.3mm is a function of the fitted optical depth and scattering treatment, not an algebraic identity; in the optically thin limit the two coincide, but the large ratios are reported precisely when the model departs from that limit. The paper transparently acknowledges the opacity sensitivity in the abstract and Section 3.4.2. Self-citations to I. C. Radley et al. (2025) are used for variability methodology, ALMA beam parameters, and outflow context, but none is load-bearing for the mass-enhancement inference. The DSHARP opacity prescription is externally sourced from Birnstiel et al. (2018). The genuine limitation, flagged explicitly in Section 3.4.2, is that GSS30-IRS2 has 'an ionised gas spectral index consistent with non-thermal gyro-emission... which is not captured in our thermal free-free model'; this and the fixed Te=8000K are modeling/robustness risks to the low-frequency dust residual, not evidence of circular derivation. The score of 2 reflects only the presence of minor, non-load-bearing self-citations; no circular step was found.

Axiom & Free-Parameter Ledger

7 free parameters · 9 axioms · 0 invented entities

The central claim rests on a six-parameter dust+ionised-gas model with adopted DSHARP opacities and uniform physical conditions. The headline mass increase over mm-only estimates is not an external benchmark; it is the model's interpretation of the same SED. Several priors were adjusted per object (EM cap, Sigma_dust cap, Omega_ionised <= Omega_dust), and the paper is transparent about opacity sensitivity but does not propagate it into the mass ratios.

free parameters (7)
  • T_dust = 20–151 K (Table 3)
    Free parameter in the SED model; drives the dust-mass scaling through the Planck function.
  • a_max = 0.3–239 mm (Table 3; DoAr24Eb excluded from averages)
    Free parameter describing maximum grain size; central to the grain-growth and hidden-mass claims.
  • Sigma_dust = 7.7e-4 to 27.7 g/cm2 (Table 3)
    Free parameter controlling optical depth and dust mass; prior capped at 50 g/cm2.
  • Omega_dust = Fixed from ALMA for most objects; free for DoAr24, DoAr24Eb, S2, GSS29
    Solid angle of dust emission; where unresolved it is a free parameter, adding degeneracy.
  • EM (emission measure) = 10^6–10^12 cm^-6 pc; capped at 10^10 for DoAr24/Eb
    Free parameter for the ionised-gas component; the cap is an explicit prior adjustment.
  • Omega_ionised = Free, with upper limit Omega_ionised <= Omega_dust
    Free parameter for the ionised-gas geometry.
  • Power-law amplitudes and indices (A_dust, A_ionised, alpha_dust, alpha_ionised) = Table 2
    Fitted in the empirical SED models of Section 3.4.1; used for model selection and f_ion, and to set some priors.
axioms (9)
  • domain assumption MRN grain size distribution with q = -3.5
    Standard assumption in dust modelling; affects opacity and mass scaling.
  • domain assumption DSHARP dust compositions and opacities
    Adopted for the physical model; the paper acknowledges that other opacity laws change dust masses by large factors.
  • domain assumption Uniform T_dust, a_max, and electron temperature within each source
    Simplifies the model but ignores radial gradients; the paper notes T_dust is a disk-averaged value.
  • domain assumption No mutual obscuration between dust and ionised gas emission sources
    Assumed in the SED decomposition; could bias the relative contributions.
  • domain assumption Free-free opacity follows Mezger & Henderson (1967), and applies equally to jets, winds, and HII regions
    Used for the ionised-gas component; non-thermal gyrosynchrotron is not included in the model.
  • domain assumption Electron temperature fixed to Te = 8000 K for all objects
    Chosen from literature range; affects the free-free spectrum, though weakly in the optically thin limit.
  • standard math Distance to Ophiuchus L1688 = 138.4 pc
    Taken from Ortiz-León et al. (2018); scales all physical sizes and masses.
  • domain assumption Hildebrand (1983) mass formula is used for mm-only mass comparison, despite being valid only in the optically thin limit
    The paper explicitly notes the formula 'is only valid in the optically thin limit' but uses it as a comparison baseline.
  • ad hoc to paper The 45 GHz break in the broken power law model is fixed a priori
    The choice of 45 GHz divides the 'millimetre' and 'centimetre' regimes; results depend on this choice.

pith-pipeline@v1.3.0-alltime-deepseek · 52522 in / 13108 out tokens · 135981 ms · 2026-08-01T23:14:29.935482+00:00 · methodology

0 comments
read the original abstract

We present an infrared, millimetre, and radio survey of 20 Class 0-III young stellar objects in the Ophiuchus A L1688 star-forming cluster, combining high-resolution (7-25 au) VLA and JWST observations with archival ALMA data. We implement physically motivated models to derive dust and ionised gas properties, spectral behaviour and their relative contributions through the millimetre-centimetre radio spectral energy distribution. Our models reveal circumstellar dust disks that are, on average, tens to hundreds of times more massive than millimetre-only estimates (subject to uncertainties arising from the choice of dust opacity) and contain millimetre-sized grains even at the Class 0 stage. Owing to the VLA's high resolution we are able to connect outflows to their origins, detecting protostellar jet emission on scales of 10s-1000s au. Our results represent a homogeneous characterisation of the dust and ionised gas properties in Ophiuchus and present a potential solution to the long-standing 'missing disk mass' problem. However, our understanding is still limited by resolution and sensitivity at frequencies <40 GHz. Future facilities like the SKA and ngVLA are needed to provide the necessary capabilities to fully spatially resolve this emission (<0.18") even in one of the closest star-forming regions.

Figures

Figures reproduced from arXiv: 2607.15468 by Alvaro Ribas, Audrey Coutens, Claudio Codella, David J. Wilner, Doug Johnstone, Eleonora Bianchi, Gemma Busquet, Hauyu Baobab Liu, Isaac C. Radley, Izaskun Jim\'enez-Serra, Jaime E. Pineda, John D. Ilee, John J. Tobin, Josep M. Girart, Klaus M. Pontoppidan, Laurent Loinard, Linda Podio, Marc Audard, Melvin G. Hoare, Olja Pani\'c, Tyler L. Bourke.

Figure 1
Figure 1. Figure 1: (a) NIRCam first anniversary image of the Ophiuchus L1688 core (NASA/ESA/CSA/STScI) overlaid with white crosses representing the positions of a subset of objects in our sample. Image colours correspond to emission from the following filters: F187N (blue), F200W (light blue) F335W (cyan), F444W (yellow) and F470N (Red). Inset panels (b)–(g) show zoomed in 2 µm , 4.4 µm and 4.7 µm images corresponding to the… view at source ↗
Figure 2
Figure 2. Figure 2: VLA 44 GHz (left), 22 GHz (middle) and 10 GHz (right) continuum images for GSS30-IRS3 centred on the position shown in [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Zoomed 4.4 µm NIRCam image with ALMA 217-219 GHz continuum (white contours) tracing the disk morphology and VLA 10 GHz continuum (blue contours) revealing extended emission along outflow cavities. Contours correspond to 5-, 10-, 20-, and 100-σ (ALMA) and 3-, 5-, 10-, and 20-σ (VLA), with σ as defined in [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Large-scale NIRCam images reveal extended outflows, protostellar jets and knot-like features on 100s–1000s au scales with each panel showing one of three filters: 2 µm (continuum, scattered light), 4 µm (continuum, scattered light) and, 4.7 µm (H2S(9) rotational line). Overlaid ALMA continuum emission (white contours) traces the disk morphology while VLA 10 GHz continuum (blue contours) traces ionised gas … view at source ↗
Figure 5
Figure 5. Figure 5: Radio spectral energy distributions and their derived spectral indices for all objects in our sample, annotated in the top left alongside their Class. Flux densities taken from this work are presented with filled circles and flux densities from the literature are shown as open circles. Posterior realisations are shown as the grey shaded region with the posterior median indicated as the black dashed line. F… view at source ↗
Figure 6
Figure 6. Figure 6: SED models for each object as presented in [PITH_FULL_IMAGE:figures/full_fig_p019_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Dust masses derived for each object employing three methods, ordered by Class and increasing SED dust mass. Filled circles show masses derived using the multiwavelength radio SED analysis described in Section 3.4.2 with errors as shown in [PITH_FULL_IMAGE:figures/full_fig_p023_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Theoretical radio SEDs (bottom) and their local spectral indices (top) which emulate different optical depth scenarios by assuming a range of Σdust values. The spectral index, α∆5 GHz, is calculated at 5 GHz intervals along the radio SED and plotted against the midpoint of the frequency range. We annotate τ ∼ 1 in each model with a dashed line, showing the optically thick to optically thin transition. Each… view at source ↗
Figure 9
Figure 9. Figure 9: SED model of GSS30-IRS1 considering dust only emission (black solid line), compared to observed flux densi￾ties from this work (closed circles) and the literature (open circles). Derived parameters are annotated in the bottom right alongside the 16th and 84th percentile uncertainties in addition to 1000 draws from the posterior as the orange shaded region. Note that even with extreme dust disk prop￾erties,… view at source ↗
Figure 10
Figure 10. Figure 10: VLA Continuum images for Q (44 GHz), K (22 GHz) and X band (10 GHz) and respective 3- and 5-σ contours broken into two blocks. RMS values in mJy beam−1 are shown in the top right of each panel. For the non-detection (ND) in SM1 we indicate the expected position with a white cross. Image beam sizes and position angles are shown as the hatched ellipse in the bottom left of each panel. We include a 50 au sca… view at source ↗
Figure 11
Figure 11. Figure 11: Continued from [PITH_FULL_IMAGE:figures/full_fig_p037_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Continued from [PITH_FULL_IMAGE:figures/full_fig_p038_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: 4.4 µm (left) and 4.7 µm (right) colour maps focused on GSS30-IRS1. We have applied a lognormal stretch with a minimum of 20 MJy sr−1 in order to accentuate potential structures in the image. We show VLA 10 GHz contours in blue where contours are 3-, 5-, 10-, 20- and 100-σ with σ ∼ 4 µJy. Beam sizes are shown as open ellipses in the bottom left and a 200 au scale bar is shown in the bottom right of each p… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

300 extracted references · 8 canonical work pages · 3 internal anchors

  1. [1]

    Asymmetric dust disk driving a multicomponent molecular outflow in the young Class 0 protostar GSS30 IRS3

    Early Planet Formation in Embedded Disks (eDisk): XVI. Asymmetric dust disk driving a multicomponent molecular outflow in the young Class 0 protostar GSS30 IRS3. , keywords =. doi:10.1051/0004-6361/202449981 , archivePrefix =. 2407.20885 , primaryClass =

    Pith/arXiv arXiv

  2. [2]

    , keywords =

    A systematic survey of millimetre-wavelength flaring variability of young stellar objects in the Orion Nebula Cluster. , keywords =. doi:10.1093/mnras/stad926 , archivePrefix =. 2303.15516 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    The Disk Substructures at High Angular Resolution Project (DSHARP). IX. A High-definition Study of the HD 163296 Planet-forming Disk. , keywords =. doi:10.3847/2041-8213/aaf747 , archivePrefix =. 1812.04047 , primaryClass =

    Pith/arXiv arXiv 2041

  4. [4]

    , keywords =

    Multi-frequency analysis of the ALMA and VLA high resolution continuum observations of the substructured disc around CI Tau: Preference for submillimetre-sized low-porosity amorphous carbon grains. , keywords =. doi:10.1051/0004-6361/202452986 , archivePrefix =. 2507.08797 , primaryClass =

    arXiv

  5. [5]

    Simulation of clustering by a modified continuous distribution of ellipsoids

    Optical constants of cosmic carbon analogue grains - I. Simulation of clustering by a modified continuous distribution of ellipsoids. , keywords =. doi:10.1093/mnras/282.4.1321 , adsurl =

    doi:10.1093/mnras/282.4.1321

  6. [6]

    , keywords =

    Time Monitoring of Radio Jets and Magnetospheres in the Nearby Young Stellar Cluster R Coronae Australis. , keywords =. doi:10.1088/0004-637X/780/2/155 , archivePrefix =. 1311.4761 , primaryClass =

    Pith/arXiv arXiv

  7. [7]

    , keywords =

    One Solution to the Mass Budget Problem for Planet Formation: Optically Thick Disks with Dust Scattering. , keywords =. doi:10.3847/2041-8213/ab1f8c , archivePrefix =. 1904.02127 , primaryClass =

    Pith/arXiv arXiv 2041

  8. [8]

    , keywords =

    SMA 200 400 GHz Survey for Dust Properties in the Icy Class II Disks in the Taurus Molecular Cloud. , keywords =. doi:10.3847/1538-4365/ad528b , archivePrefix =. 2405.19867 , primaryClass =

    Pith/arXiv arXiv

  9. [9]

    , keywords =

    On the Effects of Self-obscuration in the (Sub)Millimeter Spectral Indices and the Appearance of Protostellar Disks. , keywords =. doi:10.3847/1538-4357/aae779 , archivePrefix =. 1810.00904 , primaryClass =

    Pith/arXiv arXiv

  10. [10]

    , keywords =

    An ALMA Survey of Protoplanetary Disks in the Orionis Cluster. , keywords =. doi:10.3847/1538-3881/aa69c0 , archivePrefix =. 1703.08546 , primaryClass =

    Pith/arXiv arXiv

  11. [11]

    , keywords =

    On the excitation of the infrared knots along protostellar jets. , keywords =. doi:10.1051/0004-6361:20040087 , archivePrefix =. astro-ph/0402395 , primaryClass =

    Pith/arXiv arXiv

  12. [12]

    The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). II. Dust and Gas Disk Properties in the Ophiuchus Star-forming Region. , keywords =. doi:10.3847/1538-4357/add2ec , archivePrefix =. 2506.10731 , primaryClass =

    Pith/arXiv arXiv

  13. [13]

    , keywords =

    The Ophiuchus DIsk Survey Employing ALMA (ODISEA): Disk Dust Mass Distributions across Protostellar Evolutionary Classes. , keywords =. doi:10.3847/2041-8213/ab1338 , archivePrefix =. 1904.06471 , primaryClass =

    Pith/arXiv arXiv 2041

  14. [14]

    , archivePrefix = "arXiv", eprint =

    emcee: The MCMC Hammer. , archivePrefix = "arXiv", eprint =. doi:10.1086/670067 , adsurl =

    doi:10.1086/670067

  15. [15]

    Protostars and Planets VI , year = 2014, editor =

    Dust Evolution in Protoplanetary Disks. Protostars and Planets VI , year = 2014, editor =. doi:10.2458/azu_uapress_9780816531240-ch015 , archivePrefix =. 1402.1354 , primaryClass =

    Pith/arXiv arXiv 2014

  16. [16]

    , keywords =

    A Ballistic Bow Shock Model for Jet-driven Protostellar Outflow Shells. , keywords =. doi:10.1086/321649 , archivePrefix =. astro-ph/0104374 , primaryClass =

    Pith/arXiv arXiv

  17. [17]

    arXiv e-prints , keywords =

    UV-irradiated outflows from low-mass protostars in Ophiuchus with JWST/MIRI. arXiv e-prints , keywords =. doi:10.48550/arXiv.2509.10256 , archivePrefix =. 2509.10256 , primaryClass =

    work page doi:10.48550/arxiv.2509.10256

  18. [18]

    Progress of Theoretical Physics , year = 1980, month = aug, volume =

    Formation of the Giant Planets. Progress of Theoretical Physics , year = 1980, month = aug, volume =. doi:10.1143/PTP.64.544 , adsurl =

    doi:10.1143/ptp.64.544 1980

  19. [19]

    The protostellar disc of VLA 1623-2417W and its streamers imaged by ALMA

    FAUST - VIII. The protostellar disc of VLA 1623-2417W and its streamers imaged by ALMA. , keywords =. doi:10.1093/mnras/stad964 , archivePrefix =. 2303.16257 , primaryClass =

    Pith/arXiv arXiv

  20. [20]

    The VLA Nascent Disk and Multiplicity Survey of Perseus Protostars (VANDAM). IV. Free-Free Emission from Protostars: Links to Infrared Properties, Outflow Tracers, and Protostellar Disk Masses. , keywords =. doi:10.3847/1538-4365/aaceae , archivePrefix =. 1806.02434 , primaryClass =

    Pith/arXiv arXiv

  21. [21]

    The VLA Nascent Disk And Multiplicity Survey of Perseus Protostars (VANDAM). III. Extended Radio Emission from Protostars in Perseus. , keywords =. doi:10.3847/1538-4357/aa9980 , archivePrefix =. 1711.03035 , primaryClass =

    Pith/arXiv arXiv

  22. [22]

    , keywords =

    Experimental Investigations on Aggregate-Aggregate Collisions in the Early Solar Nebula. , keywords =. doi:10.1006/icar.1993.1163 , adsurl =

    arXiv 1993

  23. [23]

    Experimental Studies on the Aggregation Properties of Ice and Dust in Planet-Forming Regions. Proc. 58th Int. Astronautical Congress 2007 (Paris: Int. Astronautical Federation) , year = 2007, month = sep, pages =. doi:10.48550/arXiv.1106.4760 , archivePrefix =. 1106.4760 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1106.4760 2007

  24. [24]

    , year = 2008, month = sep, volume =

    The growth mechanisms of macroscopic bodies in protoplanetary disks. , year = 2008, month = sep, volume =. doi:10.1146/annurev.astro.46.060407.145152 , adsurl =

    arXiv 2008

  25. [25]

    , keywords =

    Breaking through: The effects of a velocity distribution on barriers to dust growth. , keywords =. doi:10.1051/0004-6361/201220004 , archivePrefix =. 1208.0304 , primaryClass =

    Pith/arXiv arXiv

  26. [26]

    , keywords =

    Characterizing the Multiple Protostellar System VLA 1623-2417 with JWST, ALMA, and VLA: Outflow Origins, Dust Growth, and an Unsettled Disk. , keywords =. doi:10.3847/1538-4357/adb0b9 , archivePrefix =. 2501.18348 , primaryClass =

    Pith/arXiv arXiv

  27. [27]

    , keywords =

    Distribution of solids in the rings of the HD 163296 disk: a multiwavelength study. , keywords =. doi:10.1051/0004-6361/202142303 , archivePrefix =. 2207.01496 , primaryClass =

    Pith/arXiv arXiv

  28. [28]

    A pathfinder for Square Kilometre Array studies

    VLA cm-wave survey of young stellar objects in the Oph A cluster: constraining extreme UV- and X-ray-driven disk photoevaporation. A pathfinder for Square Kilometre Array studies. , keywords =. doi:10.1051/0004-6361/201935340 , archivePrefix =. 1909.03515 , primaryClass =

    Pith/arXiv arXiv 1909

  29. [29]

    Misaligned Rotations of the Envelope, Outflow, and Disks in the Multiple Protostellar System of VLA 1623-2417: FAUST. III. , keywords =. doi:10.3847/1538-4357/ac4cae , archivePrefix =. 2201.07334 , primaryClass =

    Pith/arXiv arXiv

  30. [30]

    , keywords =

    Effects of Scattering, Temperature Gradients, and Settling on the Derived Dust Properties of Observed Protoplanetary Disks. , keywords =. doi:10.3847/1538-4357/ab7d32 , archivePrefix =. 2003.02982 , primaryClass =

    Pith/arXiv arXiv 2003

  31. [31]

    , keywords =

    ``Ashfall'' Induced by Molecular Outflow in Protostar Evolution. , keywords =. doi:10.3847/2041-8213/ac2b2f , archivePrefix =. 2109.12779 , primaryClass =

    Pith/arXiv arXiv 2041

  32. [32]

    The X-shooter view

    Connection between jets, winds and accretion in T Tauri stars. The X-shooter view. , keywords =. doi:10.1051/0004-6361/201730834 , archivePrefix =. 1710.05587 , primaryClass =

    Pith/arXiv arXiv

  33. [33]

    , keywords =

    The JWST Early Release Observations. , keywords =. doi:10.3847/2041-8213/ac8a4e , archivePrefix =. 2207.13067 , primaryClass =

    Pith/arXiv arXiv 2041

  34. [34]

    , keywords =

    Molecular outflows entrained by jet bowshocks. , keywords =

  35. [35]

    , keywords =

    Towards a population synthesis model of objects formed by self-gravitating disc fragmentation and tidal downsizing. , keywords =. doi:10.1093/mnras/stt672 , archivePrefix =. 1304.4978 , primaryClass =

    Pith/arXiv arXiv

  36. [36]

    , keywords =

    Hydraulic/Shock Jumps in Protoplanetary Disks. , keywords =. doi:10.1086/500396 , archivePrefix =. astro-ph/0510305 , primaryClass =

    Pith/arXiv arXiv

  37. [37]

    Gravitoviscous protoplanetary disks with a dust component. III. Evolution of gas, dust, and pebbles. , keywords =. doi:10.1051/0004-6361/201937198 , archivePrefix =. 2004.00126 , primaryClass =

    Pith/arXiv arXiv 2004

  38. [38]

    Protostars and Planets VII , year = 2023, editor =

    Planet-Disk Interactions and Orbital Evolution. Protostars and Planets VII , year = 2023, editor =. doi:10.48550/arXiv.2203.09595 , archivePrefix =. 2203.09595 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.2203.09595 2023

  39. [39]

    , keywords =

    Snow lines can be thermally unstable. , keywords =. doi:10.1093/mnras/staa1309 , archivePrefix =. 2005.03665 , primaryClass =

    Pith/arXiv arXiv 2005

  40. [40]

    Early Planet Formation in Embedded Disks (eDisk). I. Overview of the Program and First Results. , keywords =. doi:10.3847/1538-4357/acd384 , archivePrefix =. 2306.15406 , primaryClass =

    Pith/arXiv arXiv

  41. [41]

    arXiv e-prints , keywords =

    Anticipated Performance of the Square Kilometre Array -- Phase 1 (SKA1). arXiv e-prints , keywords =. doi:10.48550/arXiv.1912.12699 , archivePrefix =. 1912.12699 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1912.12699 1912

  42. [42]

    Science with a Next Generation Very Large Array , year = 2018, editor =

    The ngVLA Reference Design. Science with a Next Generation Very Large Array , year = 2018, editor =. doi:10.48550/arXiv.1810.08197 , archivePrefix =. 1810.08197 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1810.08197 2018

  43. [43]

    , keywords =

    Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA. , keywords =. doi:10.3847/1538-4357/ae1588 , archivePrefix =. 2511.20817 , primaryClass =

    arXiv

  44. [44]

    , keywords =

    870 m Dust Continuum of the Youngest Protostars in Ophiuchus. , keywords =. doi:10.3847/1538-4357/abf4fd , archivePrefix =. 2105.00514 , primaryClass =

    Pith/arXiv arXiv

  45. [45]

    , keywords =

    Extremely Dense Cores Associated with Chandra Sources in Ophiuchus A: Forming Brown Dwarfs Unveiled?. , keywords =. doi:10.3847/1538-4357/aae153 , archivePrefix =. 1810.00573 , primaryClass =

    Pith/arXiv arXiv

  46. [46]

    , keywords =

    Super-resolution Imaging of the Protoplanetary Disk HD 142527 Using Sparse Modeling. , keywords =. doi:10.3847/1538-4357/ab899f , archivePrefix =. 2004.10989 , primaryClass =

    arXiv 2004

  47. [47]

    , keywords =

    Towards a population synthesis model of self-gravitating disc fragmentation and tidal downsizing II: the effect of fragment-fragment interactions. , keywords =. doi:10.1093/mnras/stx2870 , archivePrefix =. 1711.01133 , primaryClass =

    Pith/arXiv arXiv

  48. [48]

    , keywords =

    The effect of cooling on the global stability of self-gravitating protoplanetary discs. , keywords =. doi:10.1046/j.1365-8711.2003.06253.x , archivePrefix =. astro-ph/0211088 , primaryClass =

    arXiv 2003

  49. [49]

    , keywords =

    The Eccentric Cavity, Triple Rings, Two-armed Spirals, and Double Clumps of the MWC 758 Disk. , keywords =. doi:10.3847/1538-4357/aac6cb , archivePrefix =. 1805.12141 , primaryClass =

    Pith/arXiv arXiv

  50. [50]

    , keywords =

    Gravitational instability in a planet-forming disk. , keywords =. doi:10.1038/s41586-024-07877-0 , archivePrefix =. 2409.02196 , primaryClass =

    Pith/arXiv arXiv

  51. [51]

    , keywords =

    Asymmetric features in the protoplanetary disk MWC 758. , keywords =. doi:10.1051/0004-6361/201526011 , archivePrefix =. 1505.05325 , primaryClass =

    Pith/arXiv arXiv

  52. [52]

    , keywords =

    Continuum Spectra of Collimated, Ionized Stellar Winds. , keywords =. doi:10.1086/164209 , adsurl =

    doi:10.1086/164209

  53. [53]

    The Gould's Belt Very Large Array Survey. IV. The Taurus-Auriga Complex. , keywords =. doi:10.1088/0004-637X/801/2/91 , archivePrefix =. 1412.6445 , primaryClass =

    Pith/arXiv arXiv

  54. [54]

    , keywords =

    Massive discs around low-mass stars. , keywords =. doi:10.1093/mnras/staa883 , archivePrefix =. 2001.06225 , primaryClass =

    Pith/arXiv arXiv 2001

  55. [55]

    Generation of radiative knots in a randomly pulsed protostellar jet. I. Dynamics and energetics. , keywords =. doi:10.1051/0004-6361/200913595 , archivePrefix =. 0912.2757 , primaryClass =

    Pith/arXiv arXiv

  56. [56]

    , keywords =

    Protostellar outflows: a window to the past. , keywords =. doi:10.1093/mnras/stab3572 , archivePrefix =. 2201.02999 , primaryClass =

    Pith/arXiv arXiv

  57. [57]

    , keywords =

    Discovery of a remarkable bipolar flow and exciting source in the rho Ophiuchi cloud core. , keywords =

  58. [58]

    , keywords =

    Radio emission from the sun and stars. , keywords =. doi:10.1146/annurev.aa.23.090185.001125 , adsurl =

    arXiv

  59. [59]

    Essential Radio Astronomy

  60. [60]

    , keywords =

    Imaging the Photoevaporating Disk and Radio Jet of GM Aur. , keywords =. doi:10.3847/0004-637X/829/1/1 , archivePrefix =. 1607.04225 , primaryClass =

    Pith/arXiv arXiv

  61. [61]

    , keywords =

    Dust characterization of protoplanetary disks: A guide to multi-wavelength analyses and accurate dust mass measurements. , keywords =. doi:10.1051/0004-6361/202452935 , archivePrefix =. 2501.13877 , primaryClass =

    Pith/arXiv arXiv

  62. [62]

    , keywords =

    The Radial Distribution of Dust Particles in the HL Tau Disk from ALMA and VLA Observations. , keywords =. doi:10.3847/1538-4357/ab3d33 , archivePrefix =. 1908.07140 , primaryClass =

    Pith/arXiv arXiv 1908

  63. [63]

    , keywords =

    Radio survey of the stellar population in the infrared dark cloud G14.225-0.506. , keywords =. doi:10.1051/0004-6361/202348085 , archivePrefix =. 2311.12542 , primaryClass =

    Pith/arXiv arXiv

  64. [64]

    , keywords =

    Protostellar Jets Enclosed by Low-velocity Outflows. , keywords =. doi:10.1088/2041-8205/796/1/L17 , archivePrefix =. 1411.7124 , primaryClass =

    Pith/arXiv arXiv 2041

  65. [65]

    ALMA chemical survey of disk-outflow sources in Taurus (ALMA-DOT). VI. Accretion shocks in the disk of DG Tau and HL Tau. , keywords =. doi:10.1051/0004-6361/202141264 , archivePrefix =. 2110.13820 , primaryClass =

    Pith/arXiv arXiv

  66. [66]

    , keywords =

    Performance of NIRCam on JWST in Flight. , keywords =. doi:10.1088/1538-3873/acac53 , archivePrefix =. 2212.12069 , primaryClass =

    Pith/arXiv arXiv

  67. [67]

    Disks around T Tauri Stars with SPHERE (DARTTS-S). I. SPHERE/IRDIS Polarimetric Imaging of Eight Prominent T Tauri Disks. , keywords =. doi:10.3847/1538-4357/aab846 , archivePrefix =. 1803.10882 , primaryClass =

    Pith/arXiv arXiv

  68. [68]

    , keywords =

    Investigating Protostellar Accretion-driven Outflows across the Mass Spectrum: JWST NIRSpec Integral Field Unit 3 5 m Spectral Mapping of Five Young Protostars. , keywords =. doi:10.3847/1538-4357/ad2fa0 , archivePrefix =. 2310.03803 , primaryClass =

    Pith/arXiv arXiv

  69. [69]

    , keywords =

    Morphological Evolution of Bipolar Outflows from Young Stellar Objects. , keywords =. doi:10.1086/526766 , adsurl =

    work page doi:10.1086/526766

  70. [70]

    , keywords =

    Submillimeter Continuum Observations of rho Ophiuchi A: The Candidate Protostar VLA 1623 and Prestellar Clumps. , keywords =. doi:10.1086/172425 , adsurl =

    doi:10.1086/172425

  71. [71]

    , keywords =

    A 2 au Resolution View by ALMA of the Planet-hosting WISPIT 2 Disk. , keywords =. doi:10.3847/2041-8213/ae3c0a , archivePrefix =. 2601.15948 , primaryClass =

    arXiv 2041

  72. [72]

    , keywords =

    On the theory of disc photoevaporation. , keywords =. doi:10.1111/j.1365-2966.2011.20337.x , archivePrefix =. 1112.1087 , primaryClass =

    arXiv 2011

  73. [73]

    , keywords =

    IRAS4A1: Multiwavelength continuum analysis of a very flared Class 0 disk. , keywords =. doi:10.1051/0004-6361/202347685 , archivePrefix =. 2310.11999 , primaryClass =

    Pith/arXiv arXiv

  74. [74]

    , keywords =

    Temperature Structures of Embedded Disks: Young Disks in Taurus Are Warm. , keywords =. doi:10.3847/1538-4357/abb1a2 , archivePrefix =. 2008.08106 , primaryClass =

    Pith/arXiv arXiv 2008

  75. [75]

    The Open Journal of Astrophysics , keywords =

    Detailed Microwave Continuum Spectra from Bright Protoplanetary Disks in Taurus. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.144268 , archivePrefix =. 2507.21268 , primaryClass =

    Pith/arXiv arXiv

  76. [76]

    , keywords =

    Into the thick of it: ALMA 0.45 mm observations of HL Tau at a resolution of 2 au. , keywords =. doi:10.1051/0004-6361/202349046 , archivePrefix =. 2404.04164 , primaryClass =

    Pith/arXiv arXiv

  77. [77]

    Observations of edge-on protoplanetary disks with ALMA. I. Results from continuum data. , keywords =. doi:10.1051/0004-6361/202038087 , archivePrefix =. 2008.06518 , primaryClass =

    Pith/arXiv arXiv 2008

  78. [78]

    , keywords =

    Determining Dust Properties in Protoplanetary Disks: SED-derived Masses and Settling with ALMA. , keywords =. doi:10.3847/1538-4357/aca905 , archivePrefix =. 2211.16732 , primaryClass =

    Pith/arXiv arXiv

  79. [79]

    , keywords =

    The Metallicity Electron Temperature Relationship in H II Regions. , keywords =. doi:10.3847/1538-4357/ad2458 , archivePrefix =. 2401.17969 , primaryClass =

    Pith/arXiv arXiv

  80. [80]

    , keywords =

    The Electron Temperature Gradient in the Galactic Disk. , keywords =. doi:10.1086/508803 , archivePrefix =. astro-ph/0609006 , primaryClass =

    Pith/arXiv arXiv

Showing first 80 references.