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The nascent wind of AGB star R Doradus: evidence for a recent episode of enhanced mass loss

T0 review · 3 major / 5 minor · reviewed 2026-08-14 · deepseek-v4-flash

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Pith's one-line read SO emission from R Dor shows a clumpy radial outflow and a century-old mass-loss episode

desk verdict A careful ALMA morpho-kinematic study of R Dor's slow wind that identifies plausible radial outflow cores, but the claim of a century-old mass-loss episode is not secure—the SiO map fills the same cavity that SO shows as a depletion. read the letter →

arxiv 1908.03311 v1 pith:J66Y2FGP submitted 2019-08-09 astro-ph.SR astro-ph.GA

P.T. Nhung , D.T. Hoai , P. Tuan-Anh , P. Darriulat , P.N. Diep , N.T. Phuong , T.T. Thai This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords AGBstarscircumstellarenvelopeRDoradusmasslosssulphurmonoxideALMAobservationsmorpho-kinematicsnascentwind
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 analyses ALMA observations of SO line emission from the circumstellar envelope of the nearby oxygen-rich asymptotic-giant-branch star R Dor, probing the region 20 to 100 au from the star where the slow wind is being built. It argues that the wind is not simply a rotating disc: it also contains a radial outflow covering very large solid angles, with clumpy structure taking the form of multiple emission cores. The radial distribution of the emission shows two ring-shaped depletions, the inner one (K1) appearing as a toroidal cavity, which the authors interpret as a quieter phase following an episode of enhanced mass loss about a century ago. If correct, the result means that a single ALMA snapshot can record the recent mass-loss history of an AGB star, and that spherically symmetric smooth-wind models are too simple for R Dor.

What carries the argument

The working object is the ALMA data cube of SO($J_K = 6_5 - 5_4$) emission, a three-dimensional map with two sky axes and one Doppler-velocity axis, at 9 au spatial resolution and 0.29 km s$^{-1}$ velocity resolution. Its main analytical tools are position-velocity (P-V) maps: slices of that cube in the $V_z$ versus position-angle plane, in the $V_z$ versus projected-radius plane, and near the line of sight. The key move is to isolate the radial-outflow candidates in the projected-distance interval 0.6 to 0.8 arcsec, where rotation and expansion effects are balanced enough for outflows to be identifiable, and to define the radial coordinate $\rho = \sqrt{R^2 + V_z^2/V_0^2}$, which measures distance in the cube from an ellipsoid reaching $\pm V_0$ on the velocity axis; the excess of $R f$ near $\rho \sim 0.9$ is the quantitative trace of the proposed mass-loss episode. The K1 cavity is tracked by fitting a torus through the ring of low emission and studying the residual brightness around it, and comparisons with CO, SiO, SO$_2$, and HCN provide cross-checks.

What would settle it

A model of SO line formation in the R Dor envelope that includes optical depth, non-LTE excitation, and the actual uv coverage, and that reproduces the observed data cube without any radial outflow or K1 cavity, would falsify the central claim; so would a purely rotating kinematic model that fits the P-V maps and the ring depletions. A direct observational test is to image the same region in an optically thin tracer (for example C$^{18}$O) at comparable resolution: if no ring cavity at $\sim 0.6$ arcsec and no A/B core pair is seen, the inferred mass-loss episode is an artifact of the SO tracer.

Watch

Extended reading notes

Core claim

The central claim is that the morpho-kinematics of R Dor's nascent wind, as traced by SO($J_K = 6_5 - 5_4$) emission between about 20 and 100 au, combines a previously identified rotating disc with a dominant radial outflow that is strongly inhomogeneous in direction and in radius. Directional inhomogeneity appears as pairs of emission cores (A1/A2 and B1/B2, roughly symmetric about position angle $\sim 140^\circ$, not quite back-to-back) covering large solid angles, and radial inhomogeneity appears as the K1 and K2 ring depletions. The authors read the K1 toroidal cavity as the trace of a quieter mass-loss phase that followed an episode of enhanced mass loss; translating the 0.5 to 1 arcsec scale at roughly 1 arcsec per century gives an episode 'a century or so ago.' They also confirm the inner rotating disc (radius $\sim 25$ au, tangential velocity $\sim 3$ km s$^{-1}$) and show that the outflow symmetry axis ($\sim 140^\circ$) is not aligned with the inner rotation axis ($\sim 20^\circ$), suggesting the outflows and the inner rotation are unrelated. Companion-line comparisons show that CO, SO$_2$, and HCN broadly reproduce the SO pattern, while SiO does not, which the paper takes as evidence that different molecules probe different layers of the envelope.

Load-bearing premise

The load-bearing premise is that the SO line traces the true gas distribution of the wind: that it is effectively optically thin, that the SO/H2 abundance follows a smooth radial profile centered on the star, and that the brightness cavities and cores are real density structures rather than effects of excitation, optical depth, or the interferometer's uv coverage.

Editorial extensions

If this is right

  • If the radial outflow is real, the slow wind of R Dor between 20 and 100 au is governed by expansion rather than rotation, and the outflow geometry implies the wind is far from spherical even before it reaches terminal velocity.
  • A mass-loss episode roughly a century ago would mean that AGB mass loss can vary strongly on human-observable timescales, so single-epoch mass-loss-rate estimates for nearby stars may miss recent history.
  • The non-alignment of the outflow symmetry axis (roughly 140 degrees) with the inner disc axis (roughly 20 degrees) indicates that the mechanism launching the outflow is decoupled from the inner rotating disc.
  • If the outer K2 ring is real, it would suggest a second enhanced episode about another century earlier, extending the mass-loss timeline recorded in the envelope.

Reading between the lines

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

  • An extension the paper does not make: the same ring-cavity technique could be applied to SO or other line data from other AGB stars to date their recent mass-loss episodes, turning single-epoch ALMA observations into a rough mass-loss-history recorder.
  • The SiO discrepancy may hint that SiO emission is dominated by a different, possibly shocked or recently accelerated component, or by absorption; a targeted SiO radiative-transfer study could test whether SiO traces the same outflow or a distinct inner acceleration region.
  • A direct kinematic test of the outflows would be to measure proper motions of the cores across two epochs separated by a few years: at the estimated 6 to 9 km/s outflow speeds and a distance of 59 pc, the expected motion is roughly 0.02 arcsec per year, at the edge of ALMA's astrometric capability.
  • If the radial outflow and cavities are confirmed, one-dimensional spherically symmetric wind models for semi-regular variables would need revision, because the inferred density structure implied by the K1 cavity is strongly non-spherical.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. This paper presents an analysis of ALMA band-6 observations of the SO(J_K=6_5-5_4) line emission toward the oxygen-rich AGB star R Dor, probing projected distances of roughly 20-100 au from the star. The authors characterize the morpho-kinematics of the nascent wind. They confirm the previously reported rotating disc in the inner ~25 au, and report evidence for a radial outflow component between ~30 and 60 au that is inhomogeneous in direction (multiple cores covering large solid angles) and radially (ring-like depletions K1 and K2). The radial structure is interpreted as evidence for an episode of enhanced mass loss about a century ago. The study is based on a single SO line, with comparisons to CO, SiO, SO2, and HCN data from another ALMA project.

Significance. The paper's strength is the high-quality ALMA SO data, with long integration time, and the honest discussion of complexity. The morphological evidence for strong asymmetry and ring-like depletions is well documented in figures and tables. If the interpretation holds, the paper would provide rare morpho-kinematic evidence for episodic, non-spherical mass loss in an AGB star's nascent wind, relevant to wind-driving mechanisms and dust formation. However, the transition from observed brightness maps to a physical episodic mass-loss episode is qualitative and relies on assumptions that are only partially tested. The multi-line comparison is commendable but also reveals a potential internal contradiction that needs to be addressed.

major comments (3)
  1. [Section 4.4, Figure 15] The SiO(8-7) P-V map fills cavity K1, which is a depletion in the SO, CO, SO2, and HCN maps. Since SiO is a refractory species expected to trace the same outflowing gas, its filling of K1 suggests that the K1 minimum is at least partly chemical or excitation in origin, not purely a density cavity. This undermines the Section 4.3 interpretation of K1 as a toroidal cavity associated with a quiet mass-loss period and the inferred recent enhanced mass-loss episode. The authors should address this by modeling or by explicitly explaining how the SiO map can be consistent with a density cavity.
  2. [Sections 3 and 4.3] The identification of K1 and K2 as episodic mass-loss signatures rests on the assumption that SO brightness traces gas density with a smooth abundance profile. No radiative-transfer or excitation modeling is presented, and the ring depletions could arise from variations in SO abundance, temperature, or optical depth. Section 4.4 itself shows that different molecules probe different regions, so the SO-specific depletion pattern cannot be taken at face value. The authors should either perform a simple excitation/abundance test or moderate the episodic claim.
  3. [Section 4.1, Figure 7] The outflows do not extrapolate back to the star, which the authors attribute to combined rotation and expansion. However, the invariance of the core pattern with R, used as evidence for radial expansion, could also be a projection effect of a rotating flow with emissivity inhomogeneities. A quantitative comparison of kinematic models (pure rotation versus rotation plus expansion) is missing, and would be needed to support the radial-outflow claim.
minor comments (5)
  1. [Abstract and Section 1] The distance range '20 to 100 au' should be checked against the actual coverage of the data, which extends to about 1.5 arcsec (~90 au at 59 pc).
  2. [Table 1] The normalized distribution g_n is defined in a way that is not immediately transparent; a short explanation of the normalization would improve readability.
  3. [Figure 7] The extrapolation lines are drawn by hand; an objective linear fit would make the offset claim more robust.
  4. [References] The reference to 'Hoai et al. 2019' as 'submitted to MNRAS' should be updated or clarified, since the present paper relies on it.
  5. [Figure captions, Sections 3 and 4] The sign convention for Doppler velocities (Vz relative to LSR 7.0 km/s) should be stated explicitly in the captions of Figures 4, 6, 11, and 15 for ease of comparison.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the morpho-kinematic analysis is self-contained, and the episodic mass-loss claim is an interpretive reading of the SO data-cube rather than a fitted parameter relabeled as a prediction.

full rationale

The paper's main claims—multiple outflow cores, ring-shaped depletions K1/K2, and a recent enhanced mass-loss episode—are descriptive morpho-kinematic readings of the ALMA SO data-cube, not results forced by construction. The sine-wave asymmetry decomposition attributed to Diep et al. (2016) and Nhung et al. (2018) is a geometric tool stated in the text; its parameters are descriptive fits to the data (A0 = 0.21, theta0 = 17 deg or 58 deg) and are not later relabeled as predictions. The ellipsoidal parameter rho in Section 4.3 is defined with V0 = 4-5 km/s after an enhancement was already identified from the P-V maps, so the resulting excess near rho ~ 0.9 is a consistency display rather than an independent derivation of the episodic claim. Self-citations to Hoai et al. (2019) and the authors' earlier method papers provide background and previously noted depletions, but the present evidence is independently shown in Figures 4, 8, 11 and 12. The SiO filling of cavity K1 (Section 4.4, Fig. 15) is a genuine internal tension for the density-cavity interpretation, and the authors concede that SiO probes significantly different regions (Section 5); however, that is a correctness risk, not circularity, because the episodic claim is neither defined by nor fitted to the SiO data. No circular step meeting the quoted-reduction standard is found.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central claim rests on treating SO brightness as a passive tracer of gas density and on adopting literature values for distance, abundance profile, and terminal velocity. The only hand-chosen numbers are V0 for visualization and an assumed radial velocity for inclination estimates; neither is fitted to make the claim, but both add uncertainty. No new physical entities are postulated.

free parameters (2)
  • V0 = 4 and 5 km/s
    Defines the ellipsoidal radius rho = sqrt(R^2 + Vz^2/V0^2) used to display a radial emission excess; chosen by hand to bracket the terminal speed range, not fitted to the data.
  • assumed common radial velocity of outflow cores = 6 or 9 km/s
    Used in Section 5 to convert Doppler shifts into inclination angles of the outflow plane (about 30 or 20 degrees); not independently measured.
assumptions (5)
  • domain assumption ALMA calibration, continuum subtraction, and imaging are correct.
    The analysis uses archival pipeline-reduced data; the authors verify Gaussian noise but do not independently re-derive the calibration.
  • domain assumption SO(6_5-5_4) line emission is effectively optically thin and brightness traces the column density of SO gas.
    The morpho-kinematic interpretation maps brightness features directly to gas structures; no excitation or radiative transfer model is applied. Load-bearing for the cavity and outflow cores.
  • domain assumption SO abundance relative to H2 follows a smooth Gaussian radial profile centered on the star with HWHM about 80 au.
    Cited from Danilovich et al. 2016; used to justify that variations in SO flux over 20-100 au reflect density and kinematics rather than abundance.
  • domain assumption R Dor is at a distance of 59 pc and the slow wind terminal velocity is about 5-6 km/s.
    Used to convert arcseconds and Doppler velocities to physical scales and to estimate the mass-loss episode timescale; values from Knapp et al. 2003 and Van de Sande et al. 2018.
  • standard math At 59 pc, 1 arcsec corresponds to about 59 au, so a 3 km/s wind crosses 1 arcsec in about a century.
    The timescale estimate for the mass-loss episode is a direct geometric conversion, not a fitted result.

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Cite this review

Pith. "Pith review of The nascent wind of AGB star R Doradus: evidence for a recent episode of enhanced mass loss." pith.science (2026). https://pith.science/paper/J66Y2FGP

@misc{pith2026190803311,
  author       = {Pith},
  title        = {Pith review of: The nascent wind of AGB star R Doradus: evidence for a recent episode of enhanced mass loss},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/J66Y2FGP}},
  note         = {Machine review of arXiv:1908.03311}
}
abstract

We analyse ALMA observations of the SO($J_K=6_5-5_4$) emission of the circumstellar envelope of oxygen-rich AGB star R Dor, probing distances between 20 and 100 au from the star where the nascent wind is building up. We give evidence for the slow wind to host, in addition to a previously observed rotating disc, a radial outflow covering very large solid angles and displaying strong inhomogeneity both in direction and radially: the former takes the form of multiple cores and the latter displays a radial dependence suggesting an episode of enhanced mass loss having occurred a century or so ago.

Figures

Figures reproduced from arXiv: 1908.03311 by the authors.

Figure 1
Figure 1. Distributions of the measured brightness for continuum (left) and SO line (right) emissions. Gaussian fits (red curves) give noise levels (standard deviation) of 0.6 mJy/beam and 1.1 mJy/beam respectively. The continuum distribution is for R < 3 arcsec and the line distribution for |x| < 2 arcsec, |y| < 2 arcsec and |Vz| < 25 km s−1 . intensity map integrated over the −5 to −3 km s−1 inter￾val. The importance of con… view at source ↗
Figure 2
Figure 2. Left: map of continuum emission. A standard deviation of 80 mas (FWHM of 190 mas compared with 150 mas for the beam) is measured in each of x and y. The colour scale is in units of Jy beam−1 . The beam is shown in the lower right corner of the panel. Middle: Doppler velocity spectrum of the line emission over the stellar disc (R < 90 mas) shown as a red circle in the right panel. Right: map of the line intensity int… view at source ↗
Figure 3
Figure 3. Left: Doppler velocity spectrum integrated over 0.2 < R < 1.5 arcsec (black) and its mirror-symmetric with respect to the origin (red). Middle: intensity maps integrated over −25 < Vz < 0 km s−1 (middle left) and 0 < Vz < 25 km s−1 (middle right). The colour scales are in units of Jy beam−1 km s−1 . The beams are shown in the lower left corners of the panels. Right: Dependence on θ of the asymmetry A(x ∗Vz) for the … view at source ↗
Figures from the paper (14 more)
Figure 4
Figure 4. Figure 4: P-V maps of the brightness f (left panel) and of its product Rf by the projected distance R (right panel) in the Vz vs R plane, averaged over position angle ω. age, the more so when extrapolated from shorter distances and also the more so at lower Doppler velocities. T…
Figure 5
Figure 5. Figure 5: Projections of the data-cube on three different planes: as channel maps in y vs x in bins of Vz (left); as P-V maps in Vz vs R in bins of ω (middle); and as P-V maps in Vz vs ω in bins of R (right). Angles are in degrees, distances in arcsec and velocities in km s −1 .…
Figure 6
Figure 6. Figure 6: P-V maps in the Vz vs ω plane for 0.2 < R < 1.2 arcsec (left) and R > 1.2 arcsec (right). The colour scales are in units of Jy beam−1 . fect. One expects a symmetric situation when scanning from west, namely to first meet Vz values centred on ∼+3 km s−1 at x ∼ −0.5 arc…
Figure 7
Figure 7. Figure 7: Left panels: Birth of the southern core of the red-shifted enhancement mapped at three different Doppler velocities (2.03, 2.61 and 3.19 km s−1 , left, centre and right, respectively). The upper, middle and lower rows covers ±0.6 arcsec, ±1 arcsec and ±1.5 arcsec in x …
Figure 8
Figure 8. Figure 8: P-V map in the Vz vs ω plane for projected distances from the star in the interval 0.6 < R < 0.8 arcsec. The colour scale is in units of Jy beam−1 . blue-shifted and red-shifted outflows identified in the pre￾ceding section. In principle, such a cavity could have been …
Figure 9
Figure 9. Figure 9: Projections on different planes of the data-cube environment of the outflows identified in [PITH_FULL_IMAGE:figures/full_fig_p008_9.png]
Figure 10
Figure 10. Figure 10: The data-cube near the line of sight. Upper panels: Vz vs x in steps of y (three leftmost columns) and Vz vs y in steps of x (five rightmost columns). Lower panels: x vs y at selected Doppler velocities near ±0.5, ±1.5, ±2.5 and ±3.5 km s−1 [PITH_FULL_IMAGE:figures/…
Figure 11
Figure 11. Figure 11: Left: Dependence on ω (degree) of Rcent(ω) (arcsec, upper panel) and Vzcent(ω) (km s−1 , lower panel) as estimated from a detailed inspection of the data-cube in the K1 region. Middle: Distribution of fR as a function of R − Rcent(ω) (abscissa) and Vz − Vzcent(ω) (ord…
Figure 12
Figure 12. Figure 12: Left: Dependence on ω of the product Rf for R > 1.2 arcsec. Right: distribution of product Rf as a function of ρ for V0 = 4 (red) and 5 (black) km s−1 . distance from the star over which the abundance of the emit￾ting molecule is significant and the projected distance…
Figure 13
Figure 13. Figure 13: Intensity maps of the red-shifted hemispheres for each of the CO, SiO, SO2 and HCN lines. The colour scales are in units of Jy beam−1 km s−1 [PITH_FULL_IMAGE:figures/full_fig_p011_13.png]
Figure 14
Figure 14. Figure 14: P-V maps in the Vz vs ω plane for projected distances from the star in the interval 0.3 < R < 0.7 arcsec. Lines are identified in the inserts. For the SO line, the interval of R is split in two equal parts. A same triangle embedding the A outflows is shown on each map…
Figure 15
Figure 15. Figure 15: P-V maps of the product of the brightness f by the projected distance R > 0.2 arcsec in the Vz > 0 vs R plane, averaged over position angle ω. Lines are identified in the inserts. A same circle locating cavity K1 is shown on each panel to guide the eye [PITH_FULL_IMA…
Figure 16
Figure 16. Figure 16: Correlation between measured brightness in the interval 0.3 < R < 0.5 arcsec and 0 < Vz < 3 km s−1 (upper rows) or 3 < Vz < 6 km s−1 (lower rows). Lines are identified in the inserts. The scales of abscissa and ordinate are adjusted in each case to cover the whole dis…
Figure 17
Figure 17. Figure 17: Qualitative picture summarizing the results obtained in the present work. Fonfria, J.P., Santander-Garcia, M., Cernicharo, J. et al., 2019, A&A, 622, L14. Heras M. & Hony S., 2005, A&A, 439, 171 Hoai D.T., Nhung P.T., Tuan-Anh P., et al., 2019, submitted to MNRAS Homa…

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Works this paper leans on

26 extracted references · 25 canonical work pages

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    R., Zijlstra A.A., Jones A., & Foster G., 1998, MNRAS, 301, 1073

    Bedding T. R., Zijlstra A.A., Jones A., & Foster G., 1998, MNRAS, 301, 1073

    work page 1998

  3. [3]

    Danilovich T., De Beck E., Black J.H., et al., 2016, A&A 588, A119

    work page 2016

  4. [4]

    & Olofsson H., 2018, A&A, 615, A8

    De Beck E. & Olofsson H., 2018, A&A, 615, A8

    work page 2018

  5. [5]

    Decin L., Richards A.M.S., Danilovich T., et al., 2018, A&A, 615, A28

    work page 2018

  6. [6]

    et al., 2016, MNRAS, 461, 4276

    Diep, P.N., Phuong, N.T., Hoai, D.T. et al., 2016, MNRAS, 461, 4276

    work page 2016

  7. [7]

    Dumm T., & Schild H., 1998, New Astr., 3, 137

    work page 1998

  8. [8]

    et al., 2019, A&A, 622, L14

    Fonfria, J.P., Santander-Garcia, M., Cernicharo, J. et al., 2019, A&A, 622, L14

    work page 2019

Show all 26 references
  1. [9]

    & Hony S., 2005, A&A, 439, 171

    Heras M. & Hony S., 2005, A&A, 439, 171

    2005

  2. [10]

    Hoai D.T., Nhung P.T., Tuan-Anh P., et al., 2019, submitted to MNRAS

    2019

  3. [11]

    Homan W., Danilovich T., Decin L., et al., 2018, A&A, 614, A113

    2018

  4. [12]

    Khouri T., Maercker M., Waters L.B.F.M., et al., 2016, A&A, 591, A70

    2016

  5. [13]

    Knapp G.R., Pourbaix D., Platais, I., and Jorissen, A., 2003, A&A, 403, 993

    2003

  6. [14]

    Lebzelter, T., and Hron, J., 1999, A&A, 351, 533

    1999

  7. [15]

    & Goodson, A., 2000, ApJ, 545, 965

    Matt S., Balick, B., Winglee, R. & Goodson, A., 2000, ApJ, 545, 965

    2000

  8. [16]

    et al., 2018, MNRAS, 480, 3324

    Nhung P.T., Hoai D.T., Tuan-Anh P. et al., 2018, MNRAS, 480, 3324

    2018

  9. [17]

    et al., 2019, A&A, 623A, 1530

    Olofsson, H., Khouri, T., Maercker, M. et al., 2019, A&A, 623A, 1530

    2019

  10. [18]

    Ramstedt, S., & Olofsson H., 2014, A&A 566, A145

    2014

  11. [19]

    et al., 2018, A&A, 616A, 61

    Ramstedt, S., Mohamed, S., Olander, T. et al., 2018, A&A, 616A, 61

    2018

  12. [20]

    et al., 2018, A&A, 618, A164

    S\' a nchez Contreras, C., Alcolea, J., Bujarrabal, V. et al., 2018, A&A, 618, A164

    2018

  13. [21]

    et al., 2015, RAA, 15, 2213

    Tuan Anh, P., Diep, P.N., Hoai, D.T. et al., 2015, RAA, 15, 2213

    2015

  14. [22]

    Tuan-Anh P., Hoai D.T., Nhung P.T., et al., 2019, MNRAS, 487, 622

    2019

  15. [23]

    Van de Sande M., Decin L., Lombaert R., et al., 2018, A&A 609, A63

    2018

  16. [24]

    van Leeuwen F., 2007, A&A, 474, 653

    2007

  17. [25]

    Vlemmings W.H.T., Khouri T., De Beck E., et al., 2018, A&A, 613, L4

    2018

  18. [26]

    & Wyrowski F., 2016, A&A, 590, A127

    Wong K.T., Kaminski T., Menten K.M. & Wyrowski F., 2016, A&A, 590, A127

    2016

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