Pith. sign in

REVIEW 2 major objections 5 minor 1 cited by

Characterizing magnetic field morphologies in three Serpens protostellar cores with ALMA

T0 review · 2 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

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

Pith's one-line read This paper argues that millimeter polarization along protostellar outflow cavity walls cannot be explained by radiative alignment of 0.1-micron interstellar dust; the aligned grains must have grown beyond 10 microns.

desk verdict New 40–50 au ALMA polarization maps are a solid, citable dataset, but the >10 µm grain-growth claim in cavity walls is not nailed down until the projection geometry is quantified. read the letter →

arxiv 1909.00046 v1 pith:MAAHCFBB submitted 2019-08-30 astro-ph.GA astro-ph.SR

Valentin J. M. Le Gouellec , Charles L. H. Hull , Anaëlle J. Maury , Josep M. Girart , {L}ukasz Tychoniec , Lars E. Kristensen , Zhi-Yun Li , Fabien Louvet
show 2 more authors
Paulo C. Cortes Ramprasad Rao
This is my paper · ORCID
classification astro-ph.GAastro-ph.SR
keywords dustpolarizationClass0protostarsmagneticfieldsradiativealignmenttorquesgraingrowthoutflowcavitywallssubmillimeterobservations
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 presents ALMA 870-micron dust polarization maps of three Class 0 protostars, the youngest stellar objects, at resolutions of 40 to 150 au. Its central claim is that the unusually high polarization fractions along outflow cavity walls in Serpens Emb 8(N), up to 36 percent, can be explained by radiative alignment torques only if the aligned grains are larger than 10 micrometers, far above the 0.1-micron interstellar dust standard. It also reports that the magnetic fields in the inner cores of SMM1-a and Emb 8(N) are poloidal, aligned with the bipolar outflows, rather than toroidally wrapped by rotation. If correct, the paper shows that dust grows to at least 10 microns at hundreds of au from the protostar, and that outflows shape both the magnetic field and the grain population in young envelopes.

What carries the argument

The machinery is the radiative alignment torque (RAT) mechanism, in which an anisotropic radiation field spins up dust grains that then precess into alignment with the magnetic field; the polarization angle is rotated by 90 degrees to infer the field. The load-bearing step is the penetration-depth calculation: using published dust opacities, the authors compute how far photons of each wavelength can travel into the wall before optical depth reaches unity. Because RATs are most efficient for photons whose wavelength is comparable to the grain size, the observed 200 au polarized layer can only be explained if grains as large as 10 microns exist to be spun by mid- and far-infrared photons. They also use spectral-index and brightness-temperature measurements to rule out self-scattering and k-RAT alignment, where grains align with the radiation field rather than the magnetic field, as the dominant polarization mechanism in the inner cores.

What would settle it

Measure the true thickness of the polarized wall in a nearly edge-on Class 0 outflow: if the wall is a projection and the physical penetration depth is under roughly 10 au, then 0.1-micron grains suffice and the >10 micron claim fails; if the wall remains about 200 au thick after correcting for projection, the large-grain scenario is confirmed.

Watch

Extended reading notes

Core claim

On its own terms, the paper's discovery is that the observed polarized millimeter emission from the walls of the outflow cavities of Serpens Emb 8(N) requires a population of aligned dust grains larger than 10 micrometers at 500 to 1000 au scales in Class 0 envelopes. Using standard dust opacities, the authors estimate that UV and short-wavelength photons between 1 and 10 micrometers can penetrate only 1 to 35 au into the cavity walls, yet the polarized layer is observed to be roughly 200 au thick. Since radiative torques spin grains most efficiently when the photon wavelength is comparable to the grain size, such deep alignment requires grains of order 10 micrometers or larger. In addition, the polarization maps toward SMM1-a show a poloidal magnetic field at the base of the bipolar outflow, with the highly polarized emission aligned with the extremely high-velocity redshifted jet; two polarized filaments to the south are interpreted as an outflow cavity wall and a possible accretion streamer.

Load-bearing premise

The argument rests on the assumption that the 200 to 300 au polarized layer seen along the cavity wall is a physically thick slab of dust; if it is instead a thin curved wall projected on the sky, ultraviolet photons could reach all the grains and ordinary 0.1-micron interstellar dust would explain the polarization without invoking grain growth.

Editorial extensions

If this is right

  • The inner roughly 200 au magnetic fields of SMM1-a and Emb 8(N) are poloidal and aligned with the bipolar outflow axis, with no toroidal component detected.
  • The molecular tracers anticorrelate with polarization: C18O and 13CS appear where dust is polarized, while DCO+ appears where it is not, identifying cold dense gas as a poor-alignment zone.
  • If the thick-wall interpretation stands, Class 0 envelopes at 500 to 1000 au must contain grains above 10 micrometers, which is far larger than the 0.1-micron interstellar dust population.
  • The polarization asymmetry at the base of the redshifted jet in SMM1-a indicates that mechanical alignment torques may augment radiative torques near fast jets.

Reading between the lines

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

  • If outflow activity transports large grains outward, as proposed in the paper's discussion, the same process could seed the outer envelope with material processed near the protostar, linking cavity walls to the composition of future planet-forming disks.
  • A direct observational extension would be to re-observe the same cavity walls at longer millimeter wavelengths: if grains larger than 10 micrometers are responsible, the polarization fraction should remain high, whereas self-scattering or k-RAT alignment would produce a different wavelength dependence.
  • Quantifying the projection effect the authors flag would settle the large-grain claim; a nearly edge-on outflow cavity or a kinematic measure of the wall's true depth would show whether the 200 au thickness is real or inflated.
  • The same RAT penetration-depth logic applied to the similar polarized walls of BHR 71 and B335 would indicate whether the large-grain requirement is a general feature of Class 0 outflows or specific to Serpens.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. This paper presents ALMA 870 μm dust polarization observations of three Class 0 protostars in Serpens Main (SMM1, Emb 8(N), Emb 8) at spatial resolutions of roughly 40–150 au, together with CO and dense-gas tracer maps. The main observational results are: (i) Emb 8(N) shows high polarization fractions, up to ~36%, along the outflow cavity walls with the inferred magnetic field running along the walls; (ii) SMM1-a shows a poloidal magnetic field in its inner ~200 au and two polarized filaments to the south, one interpreted as a redshifted cavity wall and one as a possible accretion streamer; and (iii) Emb 8 shows less outflow-correlated polarization. Based on a penetration-depth calculation in Section 4.4, the authors propose that RAT alignment in the Emb 8(N) cavity walls requires grains larger than 10 μm at ~500–1000 au scales, because UV and 10 μm photons penetrate only ~1–35 au into the walls while the polarized layer appears 200–300 au thick.

Significance. The observational material is valuable and generally carefully reduced: self-calibration, polarized-intensity debiasing, noise thresholds, and beam matching across dataset combinations are clearly described, and the maps are made available. The poloidal-field detection, the depolarization zones, and the molecular-line correlations are interesting observational results that stand independently of the grain-growth interpretation. If the >10 μm grain-growth claim were established, it would be an important constraint on early dust evolution in Class 0 envelopes. However, the claim is not yet established, because the conversion from the observed apparent width of the polarized layer to a physical penetration depth is not justified, as detailed below.

major comments (2)
  1. [§4.4, Eqs. (5)–(7)] The central claim that grains in the Emb 8(N) cavity walls must be larger than 10 μm is not established because the observed 200–300 au width of the polarized layer is used as if it were the physical thickness of the wall. The authors acknowledge in the same section that projection of a curved cavity wall will inflate the apparent thickness, but they do not quantify the inflation. For a paraboloidal shell of true thickness δ, the projected width can be hundreds of au while the line-of-sight path through the wall is much longer than δ; the column density from Eq. (6) is an average over that path and does not constrain the column density along the wall normal. If δ is only a few au, the normal-direction column could fall below the A_V ≈ 1 threshold (10^21–10^22 cm^-2) that the authors adopt, and ordinary 0.1 μm grains could be aligned by UV photons. The relevant comparison is between the computed penetration depth and the true physical thickness, not the projected width; the projection caveat therefore cuts against the paper's main conclusion and must be quantified before the >10 μm grain-growth claim can be accepted.
  2. [§4.4, footnote 6 and Eq. (7)] The gas densities used in Eq. (7) appear to be derived by dividing the aperture-averaged column density from Eq. (6) by a path length comparable to the 200 au aperture diameter; if so, the penetration-depth calculation presupposes the thick-wall geometry it is meant to test. The manuscript does not state the assumed path length or the resulting uncertainty. An independent estimate of the wall density, or a radiative-transfer model that includes the cavity geometry, is needed to break the degeneracy between physical thickness, line-of-sight path length, and density.
minor comments (5)
  1. [Figure 7 caption] The caption states 'The peak polarized intensity is 203 mJy beam^-1', but Figure 5 gives the peak polarized intensity as 6.28 mJy beam^-1 and the peak total intensity as 203 mJy beam^-1; this appears to be a typographical error.
  2. [§4.1] There is a duplicated word in 'the high (∼20%) polarization fractions observed observed by Planck'; please correct.
  3. [§4.1.2] The phrase 'the self-scattering effect is expecting to be the dominant polarization pattern' should read 'is expected to be'.
  4. [Abstract and §4.4] The abstract states that the aligned grains are at '<500 au scales', while the quantitative calculation in §4.4 is for a 200 au aperture centered at 600 au from the protostar; please clarify which spatial scales are actually being constrained.
  5. [§4.4, Eq. (5)] The mass derivation uses an opacity quoted at 1 mm (κ = 2.74 cm^2 g^-1) while the observations are at 870 μm; please justify the opacity choice or use the value appropriate to 870 μm.

Circularity Check

1 steps flagged · score 4.0 of 10

Penetration-depth argument is self-contained, but the key thick-wall assumption is imported from an in-prep self-citation by overlapping authors, and the projection caveat is acknowledged but not quantified.

  1. self citation load bearing [Section 4.4, after Eq. (7)]
    "Hull et al. conclude that this scenario of a 'thick' layer of aligned dust grains in BHR 71 is more likely than the scenario where the polarization is produced by an extremely thin layer of grains aligned only by UV/optical photons. However, even given the likelihood of the thick-wall scenario, the numbers we calculate above are still an upper limit to the penetration depth. This is because the 'thick' wall we see will have its thickness increased, at least to a small degree, by the projection of the curved cavity wall onto the plane of the sky."

    The paper's headline inference—that >10 µm grains are present in the Emb 8(N) cavity walls—requires interpreting the observed 200–300 au polarized band as a physically thick layer. The only external justification for preferring the thick-layer interpretation over a thin curved wall projected on the sky is the conclusion of Hull et al. (2019), an in-prep manuscript by overlapping authors (Hull, Le Gouellec, and Girart are all authors of the present work). The calculation in Eqs. (5)–(7) only shows that UV cannot penetrate a layer with the observed line-of-sight column if that layer is physically ~300 au thick; it does not measure the physical thickness along the wall normal.

full rationale

The core derivation is self-contained: polarization fractions and angles are measured directly from ALMA Stokes I/Q/U data, the spectral index is fitted to visibilities, and the penetration-depth argument uses Eqs. (5)–(7) with adopted distance, temperature, and Ossenkopf & Henning (1994) opacities. None of these equations contains the >10 µm conclusion as an input, and no fitted parameter is renamed as a prediction. The grain-growth claim is a conditional inference: if the polarized band is a physically thick (~300 au) wall, then UV/optical photons are extincted within ~1–35 au, so only longer-wavelength photons can align grains there, and RAT theory then requires grains larger than ~10 µm. The weakest link is the geometric assumption, which the authors acknowledge is an upper limit because of projection of the curved cavity wall onto the plane of the sky. That is a robustness caveat, not circularity. The one circularity-relevant feature is that the preference for the thick-wall scenario is imported from Hull et al. (2019), an in-prep paper by overlapping authors, rather than quantified in the present work. This self-citation is load-bearing for the headline claim, but it does not make the derivation equivalent to its inputs: the poloidal-field morphology, depolarization zones, and molecular-line correlations are observational results that stand independently of the grain-size inference. Score 4 reflects one load-bearing self-citation while the central derivation retains independent content.

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

The paper introduces no new entities, forces, or conserved quantities. Its central interpretative claims rest on RAT theory, adopted dust opacities and temperatures, and a distance and inclination prior. The main hand-chosen inputs are the dust temperature (20 to 100 K), the HRO gradient thresholds, and the SMM1-a inclination; the spectral indices are measured fits. The grain-size inference is an abductive argument from penetration depths rather than a fit to the polarization data.

free parameters (4)
  • Dust temperature Td in mass derivation = 20 K (with 100 K used as an alternative)
    Chosen to convert 870 µm flux density to gas mass in Eq. 5; the 20 to 100 K range changes NH2 by roughly an order of magnitude, from 3.4e22 to 2.5e23 cm^-2.
  • Spectral index alpha of inner cores = SMM1-a: 2.39 +/- 0.02; Emb 8(N): 3.04 +/- 0.04; Emb 8: 3.36 +/- 0.01
    Fitted to 3 mm and 870 µm visibilities with UVMULTIFIT (Fig. 13); used to argue that the SMM1-a inner core is optically thick and to exclude self-scattering for Emb 8. This is a measured fit, not a knob introduced to force the central claim.
  • Source inclination of SMM1-a = 50 degrees (from Yildiz et al. 2015, with +/- 30 degrees uncertainty)
    Adopted in Section 4.2 to argue that the radial field pattern in the inner core is a projected poloidal field. The inclination prior affects the poloidal interpretation.
  • Gradient thresholds in HRO analysis = >1/100 (peak minus rms) for CO moment 0; >1/1000 (peak minus rms) for dust continuum
    Chosen by hand in Appendix B to select regions of high gradient; these choices determine which polarization vectors enter the histograms that support the cavity-wall alignment conclusion.
assumptions (6)
  • domain assumption Dust polarization traces the plane-of-sky magnetic field via B-RAT alignment
    Central interpretative assumption of Section 4.2. The authors argue against self-scattering and k-RAT variants in Section 4.1, but the discrimination is not decisive; they note the HRO distribution is broad and no disk is detected.
  • domain assumption RAT theory: photons with wavelength comparable to grain size dominate alignment
    Used in Section 4.4 to convert photon penetration depths into a required grain size greater than 10 µm, based on Lazarian & Hoang (2007).
  • domain assumption Ossenkopf & Henning (1994) opacities and a gas-to-dust ratio of 100 apply to the Serpens cavity walls
    Eqs. 5 to 7 use kappa_1mm = 2.74 cm2/g and standard gas-to-dust ratio; the derived column densities and penetration depths depend directly on these adopted values.
  • domain assumption Distance to Serpens Main is 436 pc
    From Ortiz-Leon et al. (2017); used throughout to convert angular scales to au and to compute masses and linear sizes.
  • domain assumption UV radiation is fully extincted at Av about 1, corresponding to N_H 1e21 to 1e22 cm^-2
    Adopted from Girart et al. (2005) PDR models in Section 4.4 to conclude that UV cannot penetrate the derived cavity-wall column densities.
  • domain assumption CCH and c-C3H2 emission trace UV-irradiated cavity walls
    Used in Section 4.4 to link cavity-wall irradiation to enhanced polarization; the correlation with CCH in Emb 8(N) is shown in Figure 17.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Characterizing magnetic field morphologies in three Serpens protostellar cores with ALMA." pith.science (2026). https://pith.science/paper/MAAHCFBB

@misc{pith2026190900046,
  author       = {Pith},
  title        = {Pith review of: Characterizing magnetic field morphologies in three Serpens protostellar cores with ALMA},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/MAAHCFBB}},
  note         = {Machine review of arXiv:1909.00046}
}
read the original abstract

With the aim of characterizing the dynamical processes involved in the formation of young protostars, we present high angular resolution ALMA dust polarization observations of the Class 0 protostellar cores Serpens SMM1, Emb 8(N), and Emb 8. With spatial resolutions ranging from 150 to 40 au at 870 {\mu}m, we find unexpectedly high values of the polarization fraction along the outflow cavity walls in Serpens Emb8(N). We use 3 mm and 1 mm molecular tracers to investigate outflow and dense gas properties and their correlation with the polarization. These observations allow us to investigate the physical processes involved in the Radiative Alignment Torques (RATs) acting on dust grains along the outflow cavity walls, which experience irradiation from accretion processes and outflow shocks. The inner core of SMM1-a presents a polarization pattern with a poloidal magnetic field at the bases of the two lobes of the bipolar outflow. To the south of SMM1-a we see two polarized filaments, one of which seems to trace the redshifted outflow cavity wall. The other may be an accretion streamer of material infalling onto the central protostar. We propose that the polarized emission we see at millimeter wavelengths along the irradiated cavity walls can be reconciled with the expectations of RAT theory if the aligned grains present at '<' 500 au scales in Class 0 envelopes have grown larger than the 0.1 {\mu}m size of ISM dust grains. Our observations allow us to constrain the star-forming sources magnetic field morphologies within the central cores, along the outflow cavity walls, and in possible accretion streamers.

Figures

Figures reproduced from arXiv: 1909.00046 by the authors.

Figure 1
Figure 1. Magnetic field around Serpens Emb 8(N). Line segments represent the magnetic field orientation, rotated by 90◦ from the dust polarization angle χ (the length of the segments does not represent any quantity). They are plotted where the polarized intensity P > 3σP . The color scale is the total intensity (Stokes I) thermal dust emission, shown from 3σI . The gray contour indicates the 3σI level. Top Left: Dataset A, s… view at source ↗
Figure 2
Figure 2. Moment 0 map of CO (J = 2 → 1) in color scale overlaid with the total intensity contours and magnetic field orientations around Serpens Emb 8(N). The moment 0 map is constructed by integrating emission from –53 to 0 km s−1 (blue) and from 15 to 40 km s−1 (red). The vLSR is ∼ 8.5 km s−1 . The peaks of the red￾and blueshifted moment 0 maps are 2.10 Jy beam−1 km s−1 and 2.52 Jy beam−1 km s−1 , respectively. Same as [P… view at source ↗
Figure 3
Figure 3. shows a significant amount of dust polarization along the outflow cavity walls, whereas the central region is unpolarized, at this resolution, where the Stokes I emis￾sion peaks. The lower resolution map ( [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (18 more)
Figure 4
Figure 4. Figure 4: Moment 0 maps of 13CS (J = 5 → 4), C18O (J = 2 → 1), and DCO+ (J = 3 → 2) around Serpens Emb 8(N). The black contours represent the total intensity (Stokes I) at the following levels: 7, 11, 16, 24, 44, 74, 128, 256 × σI , where σI = 55 µJy beam−1 , from Case-2. The vL…
Figure 5
Figure 5. Figure 5: Magnetic field around Serpens SMM1. Line segments represent the magnetic field orientation, rotated by 90◦ from the dust polarization angle χ (the length of the segments does not represent any quantity). They are plotted where the polarized intensity P > 3σP . The colo…
Figure 6
Figure 6. Figure 6: Moment 0 map of CO (J = 2 → 1) in color scale overlaid with the total intensity contours and magnetic field orientations around Serpens SMM1. Same as [PITH_FULL_IMAGE:figures/full_fig_p009_6.png]
Figure 7
Figure 7. Figure 7: Dust polarization intensity (top) and polarization frac￾tion (bottom) in SMM1a, from Case-1. Same as [PITH_FULL_IMAGE:figures/full_fig_p009_7.png]
Figure 8
Figure 8. Figure 8: Magnetic field around Serpens Emb 8 from Case-1. Line segments represent the magnetic field orientation, rotated by 90◦ from the dust polarization angle χ (the length of the segments does not represent any quantity). They are plotted where the polarized intensity P > 3…
Figure 9
Figure 9. Figure 9: Moment 0 map of CO (J = 2 → 1) in color scale overlaid with the total intensity contours and magnetic field orientations around Serpens Emb 8. Line segments represent the magnetic field orientation, rotated by 90◦ from the dust polarization angle χ (the length of the s…
Figure 10
Figure 10. Figure 10: Dust polarization intensity (top) and polarization fraction (bottom) in Serpens Emb 8 from Dataset A. Same as [PITH_FULL_IMAGE:figures/full_fig_p011_10.png]
Figure 11
Figure 11. Figure 11: Polarization orientations in SMM1-a from Case-3. Same as [PITH_FULL_IMAGE:figures/full_fig_p012_11.png]
Figure 12
Figure 12. Figure 12: Histograms of relative orientation (HRO). Calculated HROs between the inferred magnetic field orientation and the density gradients in the total intensity maps (in grey), or in the blueshifted (in blue) and redshifted (in red) moment 0 maps of the CO (J = 2 → 1) low v…
Figure 13
Figure 13. Figure 13: Flux evolution over frequency from the best-fit vis￾ibility models. The y-axis is the integrated flux in Jy obtained fitting a multiple 2D-Gaussian components to the source visibilities. The x-axis is the frequency in GHz. Two datasets were used here, containing obser…
Figure 14
Figure 14. Figure 14: Brightness temperature map of the inner core of SMM1-a from Case-1. The color scale represents the brightness temperature calculated in the Rayleigh-Jeans approximation, at a wavelength of 870 µm. The brightness temperature peaks at 101 K. The black contours represent…
Figure 15
Figure 15. Figure 15: Magnetic field and outflow around SMM1-a from Case-3. Same as [PITH_FULL_IMAGE:figures/full_fig_p015_15.png]
Figure 16
Figure 16. Figure 16: Distribution of the magnetic field position angles in our three protostars. We selected the position angles in the central ∼ 4 00 zone around each protostar, and where the polarized intensity was above the 3σP level, where σP is the rms noise level of the polarized in…
Figure 17
Figure 17. Figure 17 [PITH_FULL_IMAGE:figures/full_fig_p018_17.png]
Figure 17
Figure 17. Figure 17: Moment 0 map of CCH (N = 3 → 2, J = 7/2 → 5/2, F = 4 → 3) around Serpens Emb 8(N). The black contours represent the total intensity (Stokes I) at the following levels: 11, 16, 24, 44, 74, 128, 256 × the rms level in the Stokes I dust emission map, where σI , where σI …
Figure 18
Figure 18. Figure 18: Schematic view of Serpens SMM1. The color scale is the total intensity (Stokes I) thermal dust emission from Case-1, shown when I > 3σI , from the combination of datasets A, B, and C; see [PITH_FULL_IMAGE:figures/full_fig_p023_18.png]
Figure 19
Figure 19. Figure 19: Gradient maps in Serpens Emb 8(N). The black contours trace the dust continuum from the Case-2 at 11, 16, 24, 44, 74, 128, 256 × σI in the total intensity dust emission map, where σI = 55 µJy beam−1 . Top left: The color scale represents the gradient within the centra…
Figure 20
Figure 20. Figure 20: Gradient maps in Serpens SMM1-a. The black contours trace the dust continuum from the Case-1 at 8, 12, 20, 32, 64, 128, 256 × σI in the total intensity dust emission map, where σI = 0.57 mJy beam−1 . Top left: The color scale represents the gradient derived within the…

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. ALMA observations of Magnetic Fields in the Massive Star-forming Region IRAS 18360-0537

    astro-ph.GA 2026-07 conditional novelty 6.0 of 10

    An ordered hourglass B-field in IRAS 18360-0537 lies perpendicular to the outflow/rotation axis and is reshaped by rotation, outflow cavity walls, and accretion rather than pure magnetic regulation.

Reference graph

Works this paper leans on

130 extracted references · 61 canonical work pages · cited by 1 Pith paper

  1. [1]

    E., Szűcs, L., et al

    Agurto-Gangas, C., Pineda, J. E., Szűcs, L., et al. 2019, A&A, 623, A147

    2019

  2. [2]

    O., Franco, G

    Alves, F. O., Franco, G. A. P., & Girart, J. M. 2008, A&A, 486, L13

    2008

  3. [3]

    O., Girart, J

    Alves, F. O., Girart, J. M., Padovani, M., et al. 2018, A&A, 616, A56

    2018

  4. [4]

    Andersson, B.-G., Lazarian, A., & Vaillancourt, J. E. 2015, ARA&A, 53, 501 André, P., Di Francesco, J., Ward-Thompson, D., et al. 2014, in Protostars and Planets VI, ed. H. Beuther, R. S. Klessen, C. P. Dullemond, & T. Henning, 27 André, P., Ward-Thompson, D., & Barsony, M. 2000, Protostars and Planets IV, 59

    2015

  5. [5]

    G., & Sargent, A

    Arce, H. G., & Sargent, A. I. 2006, ApJ, 646, 1070

    2006

  6. [6]

    G., Shepherd, D., Gueth, F., et al

    Arce, H. G., Shepherd, D., Gueth, F., et al. 2007, in Protostars and Planets V, ed. B. Reipurth, D. Jewitt, & K. Keil, 245 Astropy Collaboration, Price-Whelan, A. M., Sipőcz, B. M., et al. 2018, AJ, 156, 123

    2007

  7. [7]

    M., Padovani, M., et al

    Bacciotti, F., Girart, J. M., Padovani, M., et al. 2018, ApJL, 865, L12

    2018

  8. [8]

    2016, ARA&A, 54, 491

    Bally, J. 2016, ARA&A, 54, 491

    2016

Show all 130 references
  1. [9]

    O., Bruderer, S., van Dishoeck, E

    Benz, A. O., Bruderer, S., van Dishoeck, E. F., et al. 2016, A&A, 590, A105

    2016

  2. [10]

    A., Du, F., Cleeves, L

    Bergin, E. A., Du, F., Cleeves, L. I., et al. 2016, ApJ, 831, 101

    2016

  3. [11]

    J., Chepurnov, A., Lazarian, A., & Kim, J

    Bethell, T. J., Chepurnov, A., Lazarian, A., & Kim, J. 2007, ApJ, 663, 1055

    2007

  4. [12]

    C., Savage, B

    Bohlin, R. C., Savage, B. D., & Drake, J. F. 1978, ApJ, 224, 132

    1978

  5. [13]

    2017, A&A, 604, A52

    Bracco, A., Palmeirim, P., André, P., et al. 2017, A&A, 604, A52

    2017

  6. [14]

    2016, A&A, 588, A129 Chacón-Tanarro, A., Caselli, P., Bizzocchi, L., et al

    Brauer, R., Wolf, S., & Reissl, S. 2016, A&A, 588, A129 Chacón-Tanarro, A., Caselli, P., Bizzocchi, L., et al. 2017, A&A, 606, A142

    2016

  7. [15]

    W., & Tobin, J

    Chiang, H.-F., Looney, L. W., & Tobin, J. J. 2012, ApJ, 756, 168

    2012

  8. [16]

    G., Harris, R

    Cox, E. G., Harris, R. J., Looney, L. W., et al. 2018, ApJ, 855, 92

    2018

  9. [17]

    R., Pilleri, P., et al

    Cuadrado, S., Goicoechea, J. R., Pilleri, P., et al. 2015, A&A, 575, A82

    2015

  10. [18]

    Ray, T. P. 2000, ApJL, 530, L115

    2000

  11. [19]

    Dent, W. R. F., Pinte, C., Cortes, P. C., et al. 2019, MNRAS, 482, L29

    2019

  12. [20]

    2014, A&A, 563, A28

    Bergin, E. 2014, A&A, 563, A28

    2014

  13. [21]

    2010, A&A, 523, A29

    Dionatos, O., Nisini, B., Codella, C., & Giannini, T. 2010, A&A, 523, A29

    2010

  14. [22]

    Dishoeck, E. F. 2015, MNRAS, 451, 3836

    2015

  15. [23]

    L., Peretto, N., & Fuller, G

    Duarte-Cabral, A., Dobbs, C. L., Peretto, N., & Fuller, G. A. 2011, A&A, 528, A50

    2011

  16. [24]

    A., Peretto, N., et al

    Duarte-Cabral, A., Fuller, G. A., Peretto, N., et al. 2010, A&A, 519, A27

    2010

  17. [25]

    M., Allen, L

    Dunham, M. M., Allen, L. E., II, N. J. E., et al. 2015, The Astrophysical Journal Supplement Series, 220, 11

    2015

  18. [26]

    L., Evans, II, N

    Enoch, M. L., Evans, II, N. J., Sargent, A. I., & Glenn, J. 2009, ApJ, 692, 973

    2009

  19. [27]

    L., Corder, S., Duchêne, G., et al

    Enoch, M. L., Corder, S., Duchêne, G., et al. 2011, ApJS, 195, 21

    2011

  20. [28]

    P., Cabrit, S., et al

    Frank, A., Ray, T. P., Cabrit, S., et al. 2014, in Protostars and Planets VI, ed. H. Beuther, R. S. Klessen, C. P. Dullemond, & T. Henning (Tucson, Arizona: University of Arizona Press), 451–474

    2014

  21. [29]

    Frau, P., Galli, D., & Girart, J. M. 2011, A&A, 535, A44

    2011

  22. [30]

    M., et al

    Galametz, M., Maury, A., Girart, J. M., et al. 2018, A&A, 616, A139

    2018

  23. [31]

    Galli, D., & Shu, F. H. 1993, ApJ, 417, 220

    1993

  24. [32]

    M., Rao, R., & Marrone, D

    Girart, J. M., Rao, R., & Marrone, D. P. 2006, Science, 313, 812

    2006

  25. [33]

    M., Viti, S., Estalella, R., & Williams, D

    Girart, J. M., Viti, S., Estalella, R., & Williams, D. A. 2005, A&A, 439, 601

    2005

  26. [34]

    M., Fernández-López, M., Li, Z

    Girart, J. M., Fernández-López, M., Li, Z. Y., et al. 2018, ApJ, 856, L27

    2018

  27. [35]

    R., Cernicharo, J., Karska, A., et al

    Goicoechea, J. R., Cernicharo, J., Karska, A., et al. 2012, A&A, 548, A77

    2012

  28. [36]

    1952, MNRAS, 112, 215

    Gold, T. 1952, MNRAS, 112, 215

    1952

  29. [37]

    2018, A&A, 610, A16 Guzmán, V

    Guillet, V., Fanciullo, L., Verstraete, L., et al. 2018, A&A, 610, A16 Guzmán, V. V., Pety, J., Goicoechea, J. R., et al. 2015, ApJL, 800, L33

    2018

  30. [38]

    J., Cox, E

    Harris, R. J., Cox, E. G., Looney, L. W., et al. 2018, ApJ, 861, 91

    2018

  31. [39]

    Harsono, D., Bjerkeli, P., van der Wiel, M. H. D., et al. 2018, Nature Astronomy, 2, 646

    2018

  32. [40]

    2009, A&A, 506, L29

    Hennebelle, P., & Ciardi, A. 2009, A&A, 506, L29

    2009

  33. [41]

    2016, ApJL, 830, L8

    Hennebelle, P., Commerçon, B., Chabrier, G., & Marchand, P. 2016, ApJL, 830, L8

    2016

  34. [42]

    2018, ApJ, 852, 129

    Hoang, T., Cho, J., & Lazarian, A. 2018, ApJ, 852, 129

    2018

  35. [43]

    2016, ApJ, 831, 159

    Hoang, T., & Lazarian, A. 2016, ApJ, 831, 159

    2016

  36. [44]

    Hoang, T., & Tram, L. N. 2019, arXiv e-prints, arXiv:1902.06438

    2019 arXiv

  37. [45]

    N., Lee, H., & Ahn, S.-H

    Hoang, T., Tram, L. N., Lee, H., & Ahn, S.-H. 2019, Nature Astronomy, 319

    2019

  38. [46]

    2019, ApJ, 871, 100

    Hsieh, T.-H., Hirano, N., Belloche, A., et al. 2019, ApJ, 871, 100

    2019

  39. [47]

    2017, AJ, 153, 173

    Hsieh, T.-H., Lai, S.-P., & Belloche, A. 2017, AJ, 153, 173

    2017

  40. [48]

    M., Cleeves, L

    Huang, J., Andrews, S. M., Cleeves, L. I., et al. 2018, ApJ, 852, 122

    2018

  41. [49]

    Hull, C. L. H., Le Gouellec, V. J. M., Girart, J. M., & Tobin, J. J. 2019, ApJ, in prep

    2019

  42. [50]

    Hull, C. L. H., & Plambeck, R. L. 2015, Journal of Astronomical Instrumentation, 4, 1550005

    2015

  43. [51]

    Hull, C. L. H., & Zhang, Q. 2019, Frontiers in Astronomy and Space Sciences, 6, 3

    2019

  44. [52]

    Hull, C. L. H., Plambeck, R. L., Kwon, W., et al. 2014, ApJS, 213, 13

    2014

  45. [53]

    Hull, C. L. H., Girart, J. M., Kristensen, L. E., et al. 2016, ApJL, 823, L27

    2016

  46. [54]

    Hull, C. L. H., Yang, H., Li, Z.-Y., et al. 2018, ApJ, 860, 82

    2018

  47. [55]

    2016, ApJ, 830, L37

    Imai, M., Sakai, N., Oya, Y., et al. 2016, ApJ, 830, L37

    2016

  48. [56]

    K., Jørgensen, J

    Jacobsen, S. K., Jørgensen, J. K., Di Francesco, J., et al. 2018, arXiv e-prints, arXiv:1809.00390 Jørgensen, J. K., Bourke, T. L., Nguyen Luong, Q., & Takakuwa, S. 2011, A&A, 534, A100 Jørgensen, J. K., Schöier, F. L., & van Dishoeck, E. F. 2004, A&A, 416, 603 Jørgensen, J. K...

    2018 arXiv

  49. [57]

    J., Kristensen, L

    Karska, A., Kaufman, M. J., Kristensen, L. E., et al. 2018, ApJS, 235, 30

    2018

  50. [58]

    H., Qi, C., Gorti, U., et al

    Kastner, J. H., Qi, C., Gorti, U., et al. 2015, ApJ, 806, 75

    2015

  51. [59]

    N., & Tomisaka, K

    Kataoka, A., Machida, M. N., & Tomisaka, K. 2012, ApJ, 761, 40 22 Le Gouellec et al

    2012

  52. [60]

    2017, ApJL, 844, L5

    Kataoka, A., Tsukagoshi, T., Pohl, A., et al. 2017, ApJL, 844, L5

    2017

  53. [61]

    2015, ApJ, 809, 78

    Kataoka, A., Muto, T., Momose, M., et al. 2015, ApJ, 809, 78

    2015

  54. [62]

    2016, ApJL, 831, L12 Kauffmann, J., Bertoldi, F., Bourke, T

    Kataoka, A., Tsukagoshi, T., Momose, M., et al. 2016, ApJL, 831, L12 Kauffmann, J., Bertoldi, F., Bourke, T. L., Evans, II, N. J., & Lee, C. W. 2008, A&A, 487, 993

    2016

  55. [63]

    M., Tang, Y.-W., Ho, P

    Koch, P. M., Tang, Y.-W., Ho, P. T. P., et al. 2018, ApJ, 855, 39 Kölligan, A., & Kuiper, R. 2018, A&A, 620, A182

    2018

  56. [64]

    E., & Dunham, M

    Kristensen, L. E., & Dunham, M. M. 2018, A&A, 618, A158

    2018

  57. [65]

    E., Gusdorf, A., Mottram, J

    Kristensen, L. E., Gusdorf, A., Mottram, J. C., et al. 2017, A&A, 601, L4

    2017

  58. [66]

    E., Klaassen, P

    Kristensen, L. E., Klaassen, P. D., Mottram, J. C., Schmalzl, M., & Hogerheijde, M. R. 2013, A&A, 549, L6

    2013

  59. [67]

    E., van Dishoeck, E

    Kristensen, L. E., van Dishoeck, E. F., van Kempen, T. A., et al. 2010, A&A, 516, A57

    2010

  60. [68]

    E., van Dishoeck, E

    Kristensen, L. E., van Dishoeck, E. F., Bergin, E. A., et al. 2012, A&A, 542, A8

    2012

  61. [69]

    W., Tobin, J

    Kwon, W., Stephens, I. W., Tobin, J. J., et al. 2019, ApJ, 879, 25

    2019

  62. [70]

    2005, in American Institute of Physics Conference

    Lazarian, A. 2005, in American Institute of Physics Conference

    2005

  63. [71]

    Lazarian, A. 2007, J. Quant. Spec. Radiat. Transf., 106, 225

    2007

  64. [72]

    2007, MNRAS, 378, 910

    Lazarian, A., & Hoang, T. 2007, MNRAS, 378, 910

    2007

  65. [73]

    2018, Nature Communications, 9, 4636

    Lee, C.-F., Hwang, H.-C., Ching, T.-C., et al. 2018, Nature Communications, 9, 4636

    2018

  66. [74]

    2016, The Astrophysical Journal, 826, 213

    Lee, C.-F., Hwang, H.-C., & Li, Z.-Y. 2016, The Astrophysical Journal, 826, 213

    2016

  67. [75]

    Lee, J. W. Y., Hull, C. L. H., & Offner, S. S. R. 2017, ApJ, 834, 201

    2017

  68. [76]

    2012, ApJ, 761, 171

    Lee, K., Looney, L., Johnstone, D., & Tobin, J. 2012, ApJ, 761, 171

    2012

  69. [77]

    I., Fernández-López, M., Storm, S., et al

    Lee, K. I., Fernández-López, M., Storm, S., et al. 2014, ApJ, 797, 76

    2014

  70. [78]

    Lee, S., Lee, J.-E., & Bergin, E. A. 2015, The Astrophysical Journal Supplement Series, 217, 30

    2015

  71. [79]

    K., et al

    Li, H.-B., Goodman, A., Sridharan, T. K., et al. 2014, Protostars and Planets VI, 101

    2014

  72. [80]

    2017, A&A, 607, A74

    Liu, Y., Henning, T., Carrasco-González, C., et al. 2017, A&A, 607, A74

    2017

  73. [81]

    N., Matsumoto, T., Hanawa, T., & Tomisaka, K

    Machida, M. N., Matsumoto, T., Hanawa, T., & Tomisaka, K. 2005, MNRAS, 362, 382 —. 2006, ApJ, 645, 1227 Martí-Vidal, I., Vlemmings, W. H. T., Muller, S., & Casey, S. 2014, A&A, 563, A136

    2005

  74. [82]

    C., McPhee, C

    Matthews, B. C., McPhee, C. A., Fissel, L. M., & Curran, R. L. 2009, ApJS, 182, 143

    2009

  75. [83]

    J., Belloche, A., André, P., et al

    Maury, A. J., Belloche, A., André, P., et al. 2014, A&A, 563, L2

    2014

  76. [84]

    J., Girart, J

    Maury, A. J., Girart, J. M., Zhang, Q., et al. 2018, MNRAS, 477, 2760

    2018

  77. [85]

    J., André, P., Testi, L., et al

    Maury, A. J., André, P., Testi, L., et al. 2019, A&A, 621, A76

    2019

  78. [86]

    P., Waters, B., Schiebel, D., Young, W., & Golap, K

    McMullin, J. P., Waters, B., Schiebel, D., Young, W., & Golap, K. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 376, Astronomical Data Analysis Software and Systems XVI, ed. R. A. Shaw, F. Hill, & D. J. Bell, 127

    2007

  79. [87]

    C., Kristensen, L

    Mottram, J. C., Kristensen, L. E., van Dishoeck, E. F., et al. 2014, A&A, 572, A21

    2014

  80. [88]

    C., van Dishoeck, E

    Mottram, J. C., van Dishoeck, E. F., Kristensen, L. E., et al. 2017, A&A, 600, A99

    2017

  81. [89]

    M., Bruderer, S., van Dishoeck, E

    Murillo, N. M., Bruderer, S., van Dishoeck, E. F., et al. 2015, A&A, 579, A114

    2015

  82. [90]

    M., van Dishoeck, E

    Murillo, N. M., van Dishoeck, E. F., van der Wiel, M. H. D., et al. 2018, A&A, 617, A120

    2018

  83. [91]

    2016, ApJ, 824, 132 Öberg, K

    Nagai, H., Nakanishi, K., Paladino, R., et al. 2016, ApJ, 824, 132 Öberg, K. I., van der Marel, N., Kristensen, L. E., & van Dishoeck, E. F. 2011, ApJ, 740, 14 Offner, S. S. R., & Chaban, J. 2017, ApJ, 847, 104 Offner, S. S. R., Dunham, M. M., Lee, K. I., Arce, H. G., &

    2016

  84. [92]

    Fielding, D. B. 2016, ApJL, 827, L11

    2016

  85. [93]

    2014, ApJ, 796, 131

    Ohashi, N., Saigo, K., Aso, Y., et al. 2014, ApJ, 796, 131

    2014

  86. [94]

    2018, ApJ, 864, 81 Ortiz-León, G

    Ohashi, S., Kataoka, A., Nagai, H., et al. 2018, ApJ, 864, 81 Ortiz-León, G. N., Dzib, S. A., Kounkel, M. A., et al. 2017, ApJ, 834, 143

    2018

  87. [95]

    1994, A&A, 291, 943

    Ossenkopf, V., & Henning, T. 1994, A&A, 291, 943

    1994

  88. [96]

    2012, A&A, 538, A2

    Panoglou, D., Cabrit, S., Pineau Des Forêts, G., et al. 2012, A&A, 538, A2

    2012

  89. [97]

    2017, ApJ, 846, 122

    Pattle, K., Ward-Thompson, D., Berry, D., et al. 2017, ApJ, 846, 122

    2017

  90. [98]

    2009, A&A, 502, 833 Pérez, L

    Pelkonen, V.-M., Juvela, M., & Padoan, P. 2009, A&A, 502, 833 Pérez, L. M., Carpenter, J. M., Chandler, C. J., et al. 2012, ApJL, 760, L17 Pérez, L. M., Chandler, C. J., Isella, A., et al. 2015, ApJ, 813, 41 Planck Collaboration, Ade, P. A. R., Aghanim, N., et al. 2016, A&A, 586, A136

    2009

  91. [99]

    E., Ouyed, R., Fendt, C., & Brandenburg, A

    Pudritz, R. E., Ouyed, R., Fendt, C., & Brandenburg, A. 2007, Protostars and Planets V, 277

    2007

  92. [100]

    E., Rogers, C

    Pudritz, R. E., Rogers, C. S., & Ouyed, R. 2006, MNRAS, 365, 1131

    2006

  93. [101]

    P., & Clarke, D

    Ramsey, J. P., & Clarke, D. A. 2019, MNRAS, 484, 2364

    2019

  94. [102]

    M., Lai, S.-P., & Marrone, D

    Rao, R., Girart, J. M., Lai, S.-P., & Marrone, D. P. 2014, ApJL, 780, L6

    2014

  95. [103]

    Reissl, S., Seifried, D., Wolf, S., Banerjee, R., & Klessen, R. S. 2017, A&A, 603, A71

    2017

  96. [104]

    2012, APLpy: Astronomical Plotting Library in Python, Astrophysics Source Code Library, ascl:1208.017 Rodríguez-Kamenetzky, A., Carrasco-González, C., Araudo, A., et al

    Robitaille, T., & Bressert, E. 2012, APLpy: Astronomical Plotting Library in Python, Astrophysics Source Code Library, ascl:1208.017 Rodríguez-Kamenetzky, A., Carrasco-González, C., Araudo, A., et al. 2016, ApJ, 818, 27

    2012

  97. [105]

    I., Stutz, A

    Sadavoy, S. I., Stutz, A. M., Schnee, S., et al. 2016, A&A, 588, A30

    2016

  98. [106]

    2019, ApJ, 872, 196

    Sahu, D., Liu, S.-Y., Su, Y.-N., et al. 2019, ApJ, 872, 196

    2019

  99. [107]

    M., Looney, L

    Segura-Cox, D. M., Looney, L. W., Stephens, I. W., et al. 2015, ApJL, 798, L2

    2015

  100. [108]

    E., & Klessen, R

    Seifried, D., Banerjee, R., Pudritz, R. E., & Klessen, R. S. 2015, MNRAS, 446, 2776

    2015

  101. [109]

    R., Mundy, L

    Spaans, M., Hogerheijde, M. R., Mundy, L. G., & van Dishoeck, E. F. 1995, ApJ, 455, L167 Stäuber, P., Doty, S. D., van Dishoeck, E. F., & Benz, A. O. 2005, A&A, 440, 949 Stäuber, P., Doty, S. D., van Dishoeck, E. F., Jørgensen, J. K., &

    1995

  102. [110]

    Benz, A. O. 2004, A&A, 425, 577

    2004

  103. [111]

    W., Looney, L

    Stephens, I. W., Looney, L. W., Kwon, W., et al. 2013, ApJL, 769, L15

    2013

  104. [112]

    W., Yang, H., Li, Z.-Y., et al

    Stephens, I. W., Yang, H., Li, Z.-Y., et al. 2017, ApJ, 851, 55

    2017

  105. [113]

    N., Tomisaka, K., et al

    Takahashi, S., Machida, M. N., Tomisaka, K., et al. 2019, ApJ, 872, 70

    2019

  106. [114]

    2017, ApJ, 839, 56

    Tazaki, R., Lazarian, A., & Nomura, H. 2017, ApJ, 839, 56

    2017

  107. [115]

    2016, A&A, 588, A53

    Tazzari, M., Testi, L., Ercolano, B., et al. 2016, A&A, 588, A53

    2016

  108. [116]

    2014, Protostars and Planets VI, 339

    Testi, L., Birnstiel, T., Ricci, L., et al. 2014, Protostars and Planets VI, 339

    2014

  109. [117]

    J., Hartmann, L., Looney, L

    Tobin, J. J., Hartmann, L., Looney, L. W., & Chiang, H.-F. 2010, ApJ, 712, 1010

    2010

  110. [118]

    2013, A&A, 558, A64 Tychoniec, Ł., Hull, C

    Trotta, F., Testi, L., Natta, A., Isella, A., & Ricci, L. 2013, A&A, 558, A64 Tychoniec, Ł., Hull, C. L. H., Kristensen, L. E., et al. 2019, Astronomy and Astrophysics, in prep. Tychoniec, Ł., Hull, C. L. H., Tobin, J. J., & van Dishoeck, E. F. 2018, in IAU Symposium, Vol. 332...

    2013

  111. [119]

    Vaillancourt, J. E. 2006, PASP, 118, 1340 Väisälä, M. S., Shang, H., Krasnopolsky, R., et al. 2019, ApJ, 873, 114

    2006

  112. [120]

    2019, arXiv e-prints, arXiv:1907.10945 van Kempen, T

    Valdivia, V., Maury, A., Brauer, R., et al. 2019, arXiv e-prints, arXiv:1907.10945 van Kempen, T. A., Wilner, D., & Gurwell, M. 2009, ApJL, 706, L22

    2019 arXiv

  113. [121]

    D., & Thompson, T

    Velusamy, T., Langer, W. D., & Thompson, T. 2014, ApJ, 783, 6

    2014

  114. [122]

    A., & Jørgensen, J

    Visser, R., Bergin, E. A., & Jørgensen, J. K. 2015, A&A, 577, A102

    2015

  115. [123]

    E., Bruderer, S., et al

    Visser, R., Kristensen, L. E., Bruderer, S., et al. 2012, A&A, 537, A55

    2012

  116. [124]

    J., Nomura, H., et al

    Walsh, C., Millar, T. J., Nomura, H., et al. 2014, A&A, 563, A33

    2014

  117. [125]

    Wong, Y. H. V., Hirashita, H., & Li, Z.-Y. 2016, PASJ, 68, 67

    2016

  118. [126]

    2018, Frontiers in Astronomy and Space Sciences, 5, 39

    Wurster, J., & Li, Z.-Y. 2018, Frontiers in Astronomy and Space Sciences, 5, 39

    2018

  119. [127]

    W., Girart, J

    Yang, H., Li, Z.-Y., Looney, L. W., Girart, J. M., & Stephens, I. W. 2017, MNRAS, 472, 373

    2017

  120. [128]

    W., Kataoka, A., & Looney, L

    Yang, H., Li, Z.-Y., Stephens, I. W., Kataoka, A., & Looney, L. 2019, MNRAS, 483, 2371

    2019

  121. [129]

    M., Takakuwa, S., et al

    Yen, H.-W., Koch, P. M., Takakuwa, S., et al. 2015, ApJ, 799, 193

    2015

  122. [130]

    T., et al

    Yen, H.-W., Zhao, B., Hsieh, I. T., et al. 2019, ApJ, 871, 243 Yıldız, U. A., Kristensen, L. E., van Dishoeck, E. F., et al. 2012, A&A, 542, A86 —. 2015, A&A, 576, A109 High-resolution magnetic fields in Serpens protostars 23 APPENDIX A. SCHEME OF THE SMM1 CORE 18h29m49.6s49.8...

    2019

Pith tools

Reviewed August 14, 2026 · model on record in the stance chip above.