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This paper presents polarized-light maps of 45 nearby AGB stars and reports 16 resolved dusty envelopes, three of them seen for the first time, all of which depart from spherical symmetry.

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2026-08-04 07:46 UTC pith:PVHX6Y6C

load-bearing objection Useful polarimetric catalogue with three plausible new detections, but the machine-learning 'criteria' are partly circular and the resolution labels rest on an unvalidated PSF proxy. the 4 major comments →

arxiv 2608.02410 v1 pith:PVHX6Y6C submitted 2026-08-03 astro-ph.SR

A catalogue of high angular resolution and contrast polarimetric maps of 45 nearby AGB stars with SPHERE/ZIMPOL

Nekolgne Aymard Badolo , Eric Lagadec , Mamadou N'Diaye , Sie Zacharie Kam , Iain McDonald , Alexis Matter , Jean Koulidiati , Lyu Abe
show 2 more authors
Marcel Carbillet Thierry Fusco
This is my paper
classification astro-ph.SR
keywords AGB starscircumstellar envelopespolarimetric imagingdust shellshigh angular resolutionrandom forestasymptotic giant branchpolarized intensity
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.

Late-stage Sun-like stars shed most of their mass on the asymptotic giant branch, and the dust they form drives that mass loss. This paper assembles the largest homogeneous catalogue to date of 45 nearby AGB stars imaged in scattered, polarized visible light at roughly 20 milliarcsecond resolution, with the aim of finding and characterising their dusty circumstellar envelopes. It reports 16 clearly resolved dust envelopes, including three never before seen (AK Hya, SW Col, W Peg), and shows that every resolved envelope is measurably non-spherical, indicating companion shaping or asymmetric mass ejection. It also trains a random-forest classifier on stellar parameters to predict whether SPHERE/ZIMPOL will resolve a given star's envelope, yielding simple thresholds in luminosity, angular radius, infrared excess, contrast, and axis ratio. If these results hold, they give observers a shortlist of targets and a physical picture in which dust shells around nearby AGB stars are routinely asymmetric.

Core claim

Using Stokes Q and U maps converted to polarized intensity and degree-of-linear-polarization maps, the authors take each star's radial polarized-light profile at a low intensity threshold and compare its width to the point-spread-function width through the ratio η. Stars with η > 1.35 are clearly resolved, 1–1.35 marginally resolved, and η < 1 unresolved: 16, 11, and 18 stars respectively. All 16 clearly resolved envelopes have strictly positive ellipticity, so none is spherical; morphologies include bipolar structures, arcs, clumps, and disk-like elongations. Three resolved objects — AK Hya, SW Col, and W Peg — are reported for the first time in high-resolution polarized visible light. A ra

What carries the argument

The classification machinery is the normalized width ratio η = w*_h / w^PSF_h, computed at a threshold h chosen automatically by maximizing a Dice-coefficient fit of an ellipse to the polarized-intensity image. The ellipse fit supplies the shape descriptors (axis ratio b/a, ellipticity ε) and the contrast Ctr that later enter the predictor. A random forest then ranks variable importance by Gini impurity, and ROC/Youden analysis converts the top variables into interpretable thresholds.

Load-bearing premise

For the 21 stars observed without a dedicated PSF, the classification substitutes the average PSF width of other stars in the same filter; if that proxy is not accurate for a given target, the η ratio will move stars across the 1.35 boundary and bias the labels that train the random forest.

What would settle it

Re-observe the 21 targets lacking a dedicated PSF, each time with a PSF calibrator in the same filter, and recompute η; if any of the three claimed new detections (AK Hya, SW Col, W Peg) drops below η = 1.35, those detections would not survive, and if the resolved/unresolved labels shift, the random-forest thresholds change.

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

If this is right

  • The three newly resolved envelopes make concrete follow-up targets: radial-velocity monitoring and millimetre-wave imaging can test whether the bipolar shapes of AK Hya, SW Col, and W Peg are produced by unseen companions.
  • The catalogue's 45 uniformly reduced polarization maps give a reference sample for comparing dust morphology with gas kinematics and for tracking time variability of clumps and arcs.
  • The derived thresholds give a simple target-selection rule: luminous, dusty, large-angular-radius AGB stars with high envelope contrast are the ones SPHERE will resolve.
  • The universal asymmetry among resolved envelopes means mass-loss models for AGB stars must include non-spherical dust distribution as a standard feature, not an exception.
  • The 16/11/18 resolved/marginal/unresolved breakdown provides a statistical baseline for planning larger surveys of circumstellar dust.

Where Pith is reading between the lines

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

  • Because 21 of the 45 stars lacked a dedicated PSF observation and were classified using an average PSF width, the resolved fraction is sensitive to PSF variability; re-observing those targets with a contemporaneous PSF calibrator would be a direct test of whether the 16 resolved detections and the learned thresholds are stable.
  • The random-forest thresholds are trained on the same small, IR-excess-selected sample they describe, and two of the strongest predictors (contrast and axis ratio) are measured from the same polarization images used to define the labels; the predictive power on a truly independent, unbiased sample is therefore likely lower than the cross-validated accuracy suggests.
  • The data tie visible polarized dust structure to the binary-interaction question: if later companion searches confirm the inferred asymmetries, high-angular-resolution polarimetry could serve as a cheap screening tool for unresolved companions around AGB stars, a testable extension the paper does not itself make.

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

4 major / 5 minor

Summary. The paper presents a catalogue of 45 nearby AGB stars observed in polarized light with SPHERE/ZIMPOL, with uniformly reduced polarized-intensity and degree-of-linear-polarization maps. The authors use an ellipse-fitting procedure and a width-ratio criterion eta = w*_h / w^PSF_h to classify envelopes as clearly resolved, marginally resolved, or unresolved, reporting 16 clearly resolved dusty circumstellar envelopes, including three new ones (AK Hya, SW Col, W Peg). They also compile stellar parameters via SED fitting and train a random forest classifier, combined with ROC-based threshold analysis, to propose criteria for predicting whether SPHERE will resolve an envelope. The reduced maps are publicly released on Zenodo and CDS.

Significance. If the classification is sound, this is the largest homogeneous catalogue of high-angular-resolution polarimetric maps of AGB stars and would provide a valuable observational resource, with three previously unseen resolved dust shells. The public data release and the uniform re-reduction of heterogeneous archival observations are genuine strengths. The random-forest criteria, however, are weakened by two structural problems: circular predictors (Ctr and b/a are derived from the same ellipse-fitting/threshold procedure used to define the labels) and ground-truth labels that depend on an unvalidated average-PSF proxy for 21 of 45 targets. The centre of the paper is therefore not yet on firm footing, although the issues are addressable within the manuscript's scope.

major comments (4)
  1. [Section 3.1, Table 2] For 21/45 targets, including 12 of the 16 'clearly resolved' objects and two of the three new detections (AK Hya and SW Col), w^PSF_h is replaced by the filter-averaged PSF width. Table 2 reports coefficients of variation of 14.9% (N_R), 19.4% (V), and 33.3% (CntHa). A 1-sigma PSF error shifts a star at eta=1.35 to eta~1.15 or eta~1.63, crossing both resolved and unresolved boundaries. The standard deviation is quoted as an uncertainty but is never used to bound the classification. Since these labels also seed the random forest, the central detection count and the predictive criteria rest on an unvalidated assumption. Please provide per-target uncertainties on eta and show that the resolved/unresolved classification is robust to the PSF-proxy choice, or reclassify with conservative intervals.
  2. [Section 4.1, Table 3 vs Appendix A.3 / Table B.1] The ground-truth labels are internally inconsistent. Table 3 lists 18 resolved stars and includes BK Vir and RT Vir; Table A.3 explicitly lists both as 'Unresolved' with 90-100% misclassification rates, while Table B.1 marks Res_stat='yes' for both. Section 4.1 reports 16 clearly resolved, 11 marginally resolved, and 18 unresolved objects. Because these labels define the central detection count and the random-forest training set, this inconsistency must be resolved before the catalogue and the predictive model can be interpreted.
  3. [Section 4.3, Table A.2, Eq. (2)] Two of the main random-forest predictors are circular. Ctr is defined as the optimal height h_hat from Eq. (2), the same quantity used to measure w*_h and assign the resolved/unresolved label; b/a is the axis ratio of the ellipse fitted to the same thresholded region A. The decision rules Ctr>0.04 and b/a<0.97 therefore encode the classification procedure rather than independently predicting it. The claimed cumulative Gini importance (54.81%) for these variables and the 'robust criteria' in the abstract are inflated. Please remove Ctr, b/a, and their derived quantities (epsilon, e) from the feature set, or validate them against labels defined without Eq. (2).
  4. [Section 3.1] The eta=1.35 threshold is set by eye ('the point at which clear morphological features start to become visible') and no uncertainty is attached to it. This is particularly consequential for the new detections AK Hya and SW Col, which lack dedicated PSF observations. The claim of 16 resolved envelopes should be accompanied by a formal treatment of label uncertainty, or by independent confirmation for the new sources.
minor comments (5)
  1. [Abstract / Section 4.1 / Table 3] The abstract says 16 resolved envelopes; Section 4.1 says 16 clearly resolved, 11 marginally resolved, 18 unresolved; Table 3 is titled '18 resolved AGB stars'. Please standardize the counting and explicitly define 'clearly resolved' vs 'resolved' (the random forest groups the two resolved classes into one).
  2. [Section 4.1] The first sentence states that all 45 targets display a clear departure from spherical symmetry, which conflicts with the abstract's wording that the 16 resolved envelopes show this. Clarify that asymmetry is present in many maps, but only 16 are classified as clearly resolved.
  3. [Table 2] I_PRIM has N=1 and Std=0.00; this row is not informative and should be marked as such or removed.
  4. [Eq. (1)] AoLP = 1/2 arctan(U/Q) is undefined when Q=0; please state the convention used (e.g., atan2) and the quadrant handling.
  5. [Section 3.2.11] The phrase 'which had not yet been published at the time of this study' is awkward for a published paper; suggest rewording to 'previously unpublished data'.

Circularity Check

2 steps flagged

The random-forest 'robust criteria' claim is partially circular: Ctr is defined as the same optimal threshold ĥ used to measure the stellar width and assign the resolved label, so the Ctr>0.04 rule restates the classification input; the 16-envelope detection catalogue itself is not circular.

specific steps
  1. self definitional [Section 3.1 (Eq. 2, ĥ and η definition) and Section 4.3 (Ctr definition), Table A.2]
    "With ĥ, we keep the associated ellipse parameters a and b for the remainder of the paper for a given star. ... The ratio η is then calculated as the fraction w ⋆ h /w PSF h , where w ⋆ h and w PSF h are the widths computed for the star and the PSF. ... In this work, Ctr is directly taken as the optimal height ĥ, determined from the radial profile of the polarized intensity map (PIL)."

    Ctr is not an independent physical contrast: it is set equal to ĥ, the threshold that defines the detected pixel set A (Eq. 2) and at which the stellar width w*_h entering η = w*_h / w_PSF_h is measured. The resolved/unresolved label is assigned from η, so the decision rule Ctr>0.04 in Table A.2 is a function of the same segmentation that produces the label. Predicting 'resolved' from Ctr is therefore partly restating the label's own construction.

  2. fitted input called prediction [Section 4.3 (axis-ratio paragraph), Table A.2; Section 3.1 ellipse-fitting procedure]
    "Finally, the axis ratio b/a provides insight into the morphology of the circumstellar envelope. In this case, the decision rule indicates a higher probability of resolution for values below the threshold (b/a<0.97). We emphasize that this threshold should be regarded as an empirical criterion derived from our classification procedure rather than as a strict physical boundary."

    b/a is the semi-minor/semi-major ratio of the ellipse fitted to the same set A defined at the optimal threshold ĥ (Eqs. 2–5), the same fitted region from which w*_h is measured for η and hence for the resolved label. Using b/a<0.97 as a 'criterion to anticipate' resolution thus re-imports the morphology of the very region used to label the star. The paper's own caveat—'derived from our classification procedure'—concedes that this threshold is in-sample rather than an independent prediction.

full rationale

The central catalogue claim—16 resolved dusty envelopes, including three new ones—rests on the measured width ratio η = w*_h / w_PSF_h applied to the polarized intensity maps; that is an observational data product, not a circular reduction to the inputs. The mean-PSF substitution for 21 stars without a dedicated PSF is a serious data-quality and validation weakness (the PSF width dispersion, CV 10–33%, can shift η across the 1.35 threshold), but it is not itself a circularity: it is an assumption about the reference PSF, not a re-use of the target quantity. Likewise, the internal inconsistency between Table 3 (BK Vir and RT Vir listed as resolved) and Table A.3 (same stars classified unresolved) is a reproducibility/labeling problem, not a definitional equivalence. However, the secondary claim of 'robust criteria to anticipate SPHERE's ability to resolve dust envelopes' is partially circular. The random forest and the ROC thresholds are trained on labels that were produced by thresholding and ellipse fitting, and two of the most discriminating variables, Ctr and b/a, are defined by that same thresholding and ellipse fit. In particular, Ctr ≡ ĥ and η is measured at ĥ, so the rule Ctr > 0.04 is, by construction, a statement about the same segmentation that defined the label. The paper itself flags the b/a threshold as 'an empirical criterion derived from our classification procedure.' Thus the detection catalogue has independent content, but the machine-learning 'prediction' criteria are partly a restatement of the classification procedure, warranting a score of 6 rather than 0–2.

Axiom & Free-Parameter Ledger

8 free parameters · 4 axioms · 0 invented entities

The paper introduces no new physical entities. The main ledger items are fitting thresholds: the hand-set η cutoff and the ROC/Youden thresholds in Table A.2, all determined on the same 45-star sample. Two thresholds (Ctr, b/a) are circular because the features are derived from the same maps that define the label. The PSF-proxy assumption is a load-bearing approximation for the classification.

free parameters (8)
  • η resolution threshold = 1.35
    Hand-selected in Section 3.1 as the point where 'clear morphological features start to become visible in the images'.
  • Luminosity threshold = 4681 L☉
    ROC/Youden optimal threshold fitted on the full 45-star sample (Table A.2), not out-of-sample.
  • Extinction threshold = 0.02 mag
    ROC/Youden threshold fitted on the full sample (Table A.2).
  • IR excess threshold = 1.42
    ROC/Youden threshold fitted on the full sample (Table A.2).
  • LIR/L⋆ threshold = 0.007
    ROC/Youden threshold fitted on the full sample (Table A.2).
  • Contrast threshold (Ctr) = 0.04
    Ctr is defined as the optimal height ĥ from the polarization map (Section 3.1) and is circular with the resolved label; the threshold is fitted on the same sample (Table A.2).
  • Stellar radius threshold = 9 mas
    ROC/Youden threshold fitted on the full sample (Table A.2).
  • Axis ratio threshold (b/a) = 0.97
    b/a is derived from the ellipse fitted to the same polarization map that defines resolved status; threshold fitted on the full sample (Table A.2).
axioms (4)
  • domain assumption The PSF width of a target without a dedicated PSF can be replaced by the average PSF width of other stars in the same filter.
    Invoked in Section 3.1 for 21 of 45 stars; if violated, the η ratio and resolved/unresolved labels are biased.
  • ad hoc to paper A width ratio η > 1.35 indicates a genuinely resolved envelope, η between 1 and 1.35 marginally resolved, η < 1 unresolved.
    The 1.35 cutoff is chosen by inspection of when 'clear morphological features start to become visible' (Section 3.1), with no statistical justification.
  • domain assumption Polarized intensity traces scattered light from dust, with negligible contribution from the central star.
    Standard polarimetric technique assumption; stated in Section 1.
  • domain assumption PySSED SED fitting with BT-Settl atmosphere models gives reliable stellar parameters (L, Teff, R⋆, Av).
    Relied on in Section 2.1 and Appendix A.1 to produce the feature values used in the classifier.

pith-pipeline@v1.3.0-daily-deepseek · 3854 in / 6489 out tokens · 135615 ms · 2026-08-04T07:46:02.704208+00:00 · methodology

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read the original abstract

We present the largest catalogue of asymptotic giant branch (AGB) stars, 45 targets in total, observed in polarized light at high angular resolution (~ 20 milliarcsec). The main goal of the study is to detect and characterize dust shells in the close environment of nearby AGB stars. This work also aims to systematically classify the AGB star circumstellar morphologies obtained with the SPHERE instrument installed at the Very Large Telescope (VLT), thanks to its Zurich Imaging Polarimeter (ZIMPOL). We extracted and analyzed polarized intensity maps for 45 AGB stars, constructed from polarimetric observation data obtained with the SPHERE/ZIMPOL instrument. An ellipse fitting method was applied to characterize the circumstellar envelopes. Stellar parameters (luminosity, effective temperature, surface gravity, extinction, metallicity) were compiled and recalculated when necessary from spectral energy distribution (SED) fitting using the Python SED fitting tool (PySSED) software. These data were then used to train a random forest machine learning model to determine the most discriminating variables for a resolved envelope around a given star. We constructed polarization maps for all stars in the sample, revealing a wide diversity of circumstellar morphologies. We detected 16 dusty circumstellar envelopes, including three never observed before. They display a wide range of morphologies, all of them showing a clear departure from spherical symmetry, indicating interaction with a companion or asymmetric mass ejections. The random forest model identified optimal thresholds for several physical parameters, thus providing robust criteria to anticipate SPHERE's ability to resolve dust envelopes around AGB stars. These results facilitate the selection of targets for future observations and contribute to a better understanding of the evolution mechanisms of circumstellar envelopes.

Figures

Figures reproduced from arXiv: 2608.02410 by Alexis Matter, Eric Lagadec, Iain McDonald, Jean Koulidiati, Lyu Abe, Mamadou N'Diaye, Marcel Carbillet, Nekolgne Aymard Badolo, Sie Zacharie Kam, Thierry Fusco.

Figure 1
Figure 1. Figure 1: Distribution of the PSF width wh measured in polarized intensity for each SPHERE/ZIMPOL filter. The boxplots show the median (horizontal red line), the interquartile range (boxes), and the overall spread of the measurements, while the notches indicate the confidence interval on the median and the symbols mark the mean values. This figure illustrates the intrinsic vari￾ability of the PSF width as a function… view at source ↗
Figure 2
Figure 2. Figure 2: Linear polarization degree maps of the 16 clearly resolved objects in our sample. White contours, customized for each star, [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Bi-dimensional projection of the PCA of the full sample [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Variables most discriminative between the full sample and the selected subsample, identified via the KS test in the 2D PCA [PITH_FULL_IMAGE:figures/full_fig_p011_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Histogram of ellipticities ε of the 16 clearly resolved cir￾cumstellar envelopes, calculated for each star from the filter with the largest apparent diameter. The dotted red line indicates the median of the distribution. The ellipticity values reflect the level of elongation or flattening of the observed envelopes. cation scheme also forms the basis for the random forest analysis presented in the following… view at source ↗

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Reference graph

Works this paper leans on

197 extracted references · 44 canonical work pages · 1 internal anchor

  1. [1]

    Evolutionary Changes in the Optical Spectrum of the Peculiar Supergiant IRC+10420. Astron. Rep. , year = 2002, month = feb, volume =. doi:10.1134/1.1451927 , adsurl =

    work page doi:10.1134/1.1451927 2002

  2. [2]

    , keywords =

    The peculiar circumstellar envelope around IRC+10420. , keywords =

  3. [3]

    , keywords =

    The Morphology of IRC+10420's Circumstellar Ejecta. , keywords =. doi:10.1088/0004-6256/140/2/339 , archivePrefix =. 1006.0501 , primaryClass =

    Pith/arXiv arXiv

  4. [4]

    Mechanisms, models and measurements

    Mass loss of stars on the asymptotic giant branch. Mechanisms, models and measurements. , keywords =. doi:10.1007/s00159-017-0106-5 , adsurl =

    doi:10.1007/s00159-017-0106-5

  5. [5]

    SPHERE/ZIMPOL high resolution polarimetric imager. I. System overview, PSF parameters, coronagraphy, and polarimetry. , keywords =. doi:10.1051/0004-6361/201833620 , archivePrefix =. 1808.05008 , primaryClass =

    Pith/arXiv arXiv

  6. [6]

    , keywords =

    Fundamental Parameters, Integrated Red Giant Branch Mass Loss, and Dust Production in the Galactic Globular Cluster 47 Tucanae. , keywords =. doi:10.1088/0067-0049/193/2/23 , archivePrefix =. 1101.1095 , primaryClass =

    Pith/arXiv arXiv

  7. [7]

    , keywords =

    Fundamental parameters and infrared excesses of Tycho-Gaia stars. , keywords =. doi:10.1093/mnras/stx1433 , archivePrefix =. 1706.02208 , primaryClass =

    Pith/arXiv arXiv

  8. [9]

    , keywords =

    Mass loss rates of a sample of irregular and semiregular M-type AGB-variables. , keywords =. doi:10.1051/0004-6361:20020841 , archivePrefix =. astro-ph/0206172 , primaryClass =

    Pith/arXiv arXiv

  9. [10]

    Binarity from proper motion anomaly

    Stellar and substellar companions of nearby stars from Gaia DR2. Binarity from proper motion anomaly. , keywords =. doi:10.1051/0004-6361/201834371 , archivePrefix =. 1811.08902 , primaryClass =

    Pith/arXiv arXiv

  10. [11]

    Technetium and the third dredge up in AGB stars. I. Field stars. , keywords =. doi:10.1051/0004-6361:20031458 , archivePrefix =. astro-ph/0310018 , primaryClass =

    Pith/arXiv arXiv

  11. [12]

    , keywords =

    Oxygen-rich AGB stars with optically thin dust envelopes. , keywords =. doi:10.1051/0004-6361:20042296 , adsurl =

    work page doi:10.1051/0004-6361:20042296

  12. [13]

    Science , keywords =

    (Sub)stellar companions shape the winds of evolved stars. Science , keywords =. doi:10.1126/science.abb1229 , archivePrefix =. 2009.11694 , primaryClass =

    Pith/arXiv arXiv 2009

  13. [14]

    RADMC-3D: A multi-purpose radiative transfer tool

  14. [15]

    , keywords =

    The HIP 79977 debris disk in polarized light. , keywords =. doi:10.1051/0004-6361/201730846 , archivePrefix =. 1709.00417 , primaryClass =

    Pith/arXiv arXiv

  15. [16]

    Limb polarization of Uranus and Neptune. I. Imaging polarimetry and comparison with analytic models. , keywords =. doi:10.1051/0004-6361:20053273 , adsurl =

    doi:10.1051/0004-6361:20053273

  16. [17]

    Polarimetric imaging mode of VLT/SPHERE/IRDIS. I. Description, data reduction, and observing strategy. , keywords =. doi:10.1051/0004-6361/201834989 , archivePrefix =. 1909.13107 , primaryClass =

    Pith/arXiv arXiv 1909

  17. [18]

    Binary planetary nebulae nuclei towards the Galactic bulge. II. A penchant for bipolarity and low-ionisation structures. , keywords =. doi:10.1051/0004-6361/200912176 , archivePrefix =. 0907.2463 , primaryClass =

    Pith/arXiv arXiv

  18. [19]

    The Evolution of Planetary Nebulae. I. Structures, Ionizations, and Morphological Sequences. , keywords =. doi:10.1086/114504 , adsurl =

    doi:10.1086/114504

  19. [20]

    , keywords =

    Mass, linear momentum and kinetic energy of bipolar flows in protoplanetary nebulae. , keywords =. doi:10.1051/0004-6361:20011090 , adsurl =

    doi:10.1051/0004-6361:20011090

  20. [21]

    , keywords =

    Why Magnetic Fields Cannot Be the Main Agent Shaping Planetary Nebulae. , keywords =. doi:10.1086/498829 , archivePrefix =. astro-ph/0501647 , primaryClass =

    Pith/arXiv arXiv

  21. [22]

    , keywords =

    Low-mass binary-induced outflows from asymptotic giant branch stars. , keywords =. doi:10.1111/j.1365-2966.2006.10625.x , archivePrefix =. astro-ph/0604445 , primaryClass =

    arXiv 2006

  22. [23]

    , keywords =

    SPHERE: the exoplanet imager for the Very Large Telescope. , keywords =. doi:10.1051/0004-6361/201935251 , archivePrefix =. 1902.04080 , primaryClass =

    Pith/arXiv arXiv 1902

  23. [24]

    Photoprocessing of the ice and return to the ISM

    Chemical modelling of dust-gas chemistry within AGB outflows - III. Photoprocessing of the ice and return to the ISM. , keywords =. doi:10.1093/mnras/staa3689 , archivePrefix =. 2011.11563 , primaryClass =

    Pith/arXiv arXiv 2011

  24. [25]

    , keywords =

    Circumstellar envelopes of semi-regular long-period variables: mass-loss rate estimates and general model fitting of the molecular gas. , keywords =. doi:10.1051/0004-6361/201936087 , archivePrefix =. 1907.09175 , primaryClass =

    Pith/arXiv arXiv 1907

  25. [26]

    , keywords =

    Distance estimates for AGB stars from parallax measurements. , keywords =. doi:10.1051/0004-6361/202243670 , archivePrefix =. 2209.03906 , primaryClass =

    Pith/arXiv arXiv

  26. [27]

    , keywords =

    Large dust grains in the wind of VY Canis Majoris. , keywords =. doi:10.1051/0004-6361/201527563 , archivePrefix =. 1511.07624 , primaryClass =

    Pith/arXiv arXiv

  27. [28]

    SF2A-2017 , year = 2017, editor =

    The SPHERE Data Center: a reference for high contrast imaging processing. SF2A-2017 , year = 2017, editor =. doi:10.48550/arXiv.1712.06948 , archivePrefix =. 1712.06948 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1712.06948 2017

  28. [29]

    , keywords =

    Astrometric and photometric accuracies in high contrast imaging: The SPHERE speckle calibration tool (SpeCal). , keywords =. doi:10.1051/0004-6361/201832973 , archivePrefix =. 1805.04854 , primaryClass =

    Pith/arXiv arXiv

  29. [30]

    , keywords =

    Shocks and Photoionization of the Inner 650 au Jet of the Interacting Binary Star R Aquarii from Multiwavelength Hubble Space Telescope Observations. , keywords =. doi:10.3847/1538-4357/acc068 , archivePrefix =. 2303.00734 , primaryClass =

    Pith/arXiv arXiv

  30. [31]

    , keywords =

    The spectroscopic orbit and the geometry of R Aquarii. , keywords =. doi:10.1051/0004-6361:200810052 , archivePrefix =. 0804.4139 , primaryClass =

    Pith/arXiv arXiv

  31. [32]

    , keywords =

    CO envelope of the symbiotic star R Aquarii seen by ALMA. , keywords =. doi:10.1051/0004-6361/201833394 , archivePrefix =. 1806.04979 , primaryClass =

    Pith/arXiv arXiv

  32. [33]

    , keywords =

    First Images of R Aquarii and Its Asymmetric H _ 2 O Shell. , keywords =. doi:10.1086/529573 , archivePrefix =. 0801.3488 , primaryClass =

    Pith/arXiv arXiv

  33. [34]

    Direct imaging of the gravitational effects of the secondary on the stellar wind

    High-resolution observations of the symbiotic system R Aqr. Direct imaging of the gravitational effects of the secondary on the stellar wind. , keywords =. doi:10.1051/0004-6361/201833633 , archivePrefix =. 1807.07272 , primaryClass =

    Pith/arXiv arXiv

  34. [35]

    NASA Conference Publication , year = 1982, editor =

    Observations and analysis of the R Aquarii jet. NASA Conference Publication , year = 1982, editor =

    1982

  35. [36]

    , keywords =

    The bipolar jet of the symbiotic star R Aquarii: A study of its morphology using the high-resolution HST WFC3/UVIS camera. , keywords =. doi:10.1051/0004-6361/201731749 , archivePrefix =. 1802.00503 , primaryClass =

    Pith/arXiv arXiv

  36. [37]

    , keywords =

    The Infrared Spectral Classification of Oxygen-rich Dust Shells. , keywords =. doi:10.1086/313156 , adsurl =

    work page doi:10.1086/313156

  37. [38]

    , keywords =

    Silicate Emission at 10 Microns in Variables on the Asymptotic Giant Branch. , keywords =. doi:10.1086/176262 , adsurl =

    work page doi:10.1086/176262

  38. [39]

    ALMA observations of CS, SiS, SiO and HCN

    Molecular line study of the S-type AGB star W Aquilae. ALMA observations of CS, SiS, SiO and HCN. , keywords =. doi:10.1051/0004-6361/201832724 , archivePrefix =. 1806.01622 , primaryClass =

    Pith/arXiv arXiv

  39. [40]

    , keywords =

    Ultraviolet emission from main-sequence companions of AGB stars. , keywords =. doi:10.1093/mnras/stw1547 , archivePrefix =. 1606.09086 , primaryClass =

    Pith/arXiv arXiv

  40. [41]

    , keywords =

    Meandering periods and asymmetries in light curves of Miras: Observational evidence for low mass-loss rates. , keywords =. doi:10.1051/0004-6361/202245593 , archivePrefix =. 2302.02206 , primaryClass =

    Pith/arXiv arXiv

  41. [42]

    , title =

    Cadmus, Robert R. , title =. , abstract =. 2024 , month =. doi:10.3847/1538-3881/ad303a , url =

    work page doi:10.3847/1538-3881/ad303a 2024

  42. [43]

    , volume =

    Ortiz, R and Guerrero, M A , title =. , volume =. 2023 , month =. doi:10.1093/mnras/stad984 , url =

    work page doi:10.1093/mnras/stad984 2023

  43. [44]

    , keywords =

    Locating dust and molecules in the inner circumstellar environment of R Sculptoris with MATISSE. , keywords =. doi:10.1051/0004-6361/202141609 , archivePrefix =. 2208.10845 , primaryClass =

    Pith/arXiv arXiv

  44. [45]

    , keywords =

    Spatially resolving the atmosphere of the non-Mira-type AGB star SW Vir in near-infrared molecular and atomic lines with VLTI/AMBER. , keywords =. doi:10.1051/0004-6361/201834171 , archivePrefix =. 1811.05989 , primaryClass =

    Pith/arXiv arXiv

  45. [46]

    , keywords =

    Systematic Effects in the Visual Estimation of the Brightness of Red Variable Stars. , keywords =

  46. [47]

    , abstract =

    Palen, Stacy , title =. , abstract =. 2001 , month =. doi:10.1086/318874 , url =

    work page doi:10.1086/318874 2001

  47. [48]

    , keywords =

    Full polarization study of SiO masers at 86 GHz. , keywords =. doi:10.1051/0004-6361:20054255 , archivePrefix =. astro-ph/0601098 , primaryClass =

    Pith/arXiv arXiv

  48. [49]

    and Yang, Haneul and Yoon, Suk-Jin , title =

    Kim, Dong-Jin and Cho, Se-Hyung and Yun, Youngjoo and Kyung Choi, Yoon and Yoon, Dong-Hwan and Kim, Jaeheon and Dodson, Richard and Rioja, María J. and Yang, Haneul and Yoon, Suk-Jin , title =. Letters , abstract =. 2018 , month =. doi:10.3847/2041-8213/aae58b , url =

    work page doi:10.3847/2041-8213/aae58b 2018

  49. [50]

    Water vapour masers in long-period variable stars. II. The semi-regular variables R Crt and RT Vir. , keywords =. doi:10.1051/0004-6361/202039157 , archivePrefix =. 2011.00294 , primaryClass =

    Pith/arXiv arXiv 2011

  50. [51]

    , keywords =

    Six years of short-spaced monitoring of the v=1 and v=2, J=1-0 ^ 28 SiO maser emission in evolved stars. , keywords =. doi:10.1051/aas:1999112 , adsurl =

    work page doi:10.1051/aas:1999112

  51. [52]

    Eleven years of short spaced monitoring

    ^ 28 SiO v = 1 and v = 2, J = 1-0 maser variability in evolved stars. Eleven years of short spaced monitoring. , keywords =. doi:10.1051/0004-6361:20040309 , adsurl =

    doi:10.1051/0004-6361:20040309

  52. [53]

    VLT/NACO spectro-imaging from 1.04 to 4.05 m and VLTI interferometry

    An edge-on translucent dust disk around the nearest AGB star, L _ 2 Puppis. VLT/NACO spectro-imaging from 1.04 to 4.05 m and VLTI interferometry. , keywords =. doi:10.1051/0004-6361/201323273 , archivePrefix =. 1404.3189 , primaryClass =

    Pith/arXiv arXiv

  53. [54]

    , keywords =

    Dissecting the AGB star L _ 2 Puppis: a torus in the making. , keywords =. doi:10.1051/0004-6361/201322828 , archivePrefix =. 1503.05031 , primaryClass =

    Pith/arXiv arXiv

  54. [55]

    SPHERE/ZIMPOL polarimetric imaging at visible wavelengths

    The dust disk and companion of the nearby AGB star L _ 2 Puppis. SPHERE/ZIMPOL polarimetric imaging at visible wavelengths. , keywords =. doi:10.1051/0004-6361/201526194 , archivePrefix =. 1511.04448 , primaryClass =

    Pith/arXiv arXiv

  55. [56]

    , volume =

    Van de Sande, M and Walsh, C and Danilovich, T and De Ceuster, F and Ceulemans, T , title =. , volume =. 2024 , month =. doi:10.1093/mnras/stae1553 , url =

    work page doi:10.1093/mnras/stae1553 2024

  56. [57]

    Supplement Series , abstract =

    Yoon, Dong-Hwan and Cho, Se-Hyung and Kim, Jaeheon and Yun, Young joo and Park, Yong-Sun , title =. Supplement Series , abstract =. 2014 , month =. doi:10.1088/0067-0049/211/1/15 , url =

    work page doi:10.1088/0067-0049/211/1/15 2014

  57. [58]

    10.1051/aas:1999501

    Oxygen-rich semiregular and irregular variables* - A catalogue of circumstellar CO observations , DOI= "10.1051/aas:1999501", url= "https://doi.org/10.1051/aas:1999501", journal =

    work page doi:10.1051/aas:1999501

  58. [59]

    , keywords =

    VLBI Observations of SiO Masers around AH Scorpii. , keywords =. doi:10.1086/588186 , archivePrefix =. 0803.1690 , primaryClass =

    Pith/arXiv arXiv

  59. [60]

    A&A , volume=

    The supergiant OH stars S Per and AH SCO-Conditions for OH emission in circumstellar envelopes , author=. A&A , volume=

  60. [61]

    , author=

    Veiling and the presence of circumstellar gas and dust in some infrared stars. , author=. Astrophysical Journal, Vol. 188, p. 75-85 , volume=

  61. [62]

    Modelling VLTI/GRAVITY and MATISSE observations of AH Sco, KW Sgr, V602 Car, CK Car, and V460 Car

    The effect of winds on atmospheric layers of red supergiants II. Modelling VLTI/GRAVITY and MATISSE observations of AH Sco, KW Sgr, V602 Car, CK Car, and V460 Car. , keywords =. doi:10.1051/0004-6361/202348047 , archivePrefix =. 2312.12521 , primaryClass =

    Pith/arXiv arXiv

  62. [63]

    The behaviour of SiO bands in AGB stars

    SiO rotation-vibration bands in cool giants II. The behaviour of SiO bands in AGB stars. , keywords =

  63. [64]

    , keywords =

    ATOMIUM: Molecular inventory of 17 oxygen-rich evolved stars observed with ALMA. , keywords =. doi:10.1051/0004-6361/202347632 , archivePrefix =. 2312.03467 , primaryClass =

    Pith/arXiv arXiv

  64. [65]

    The VLT/SPHERE view of the ATOMIUM cool evolved star sample. I. Overview: Sample characterization through polarization analysis. , keywords =. doi:10.1051/0004-6361/202245398 , archivePrefix =. 2301.02081 , primaryClass =

    Pith/arXiv arXiv

  65. [66]

    10.1051/0004-6361/201220920

    The atmospheric structure and fundamental parameters of the red supergiants AH Scorpii, UY Scuti, and KW Sagittarii , DOI= "10.1051/0004-6361/201220920", url= "https://doi.org/10.1051/0004-6361/201220920", journal =

    doi:10.1051/0004-6361/201220920

  66. [67]

    , keywords =

    Crossing the Yellow Void: Spatially Resolved Spectroscopy of the Post-Red Supergiant IRC +10420 and Its Circumstellar Ejecta. , keywords =. doi:10.1086/341380 , archivePrefix =. astro-ph/0205247 , primaryClass =

    Pith/arXiv arXiv

  67. [68]

    and Groenewegen, M

    Oudmaijer, René D. and Groenewegen, M. A. T. and Matthews, H. E. and Blommaert, J. A. D. L. and Sahu, K. C. , title =. , volume =. 1996 , month =. doi:10.1093/mnras/280.4.1062 , url =

    work page doi:10.1093/mnras/280.4.1062 1996

  68. [69]

    and Jones, Terry J

    Shenoy, Dinesh and Humphreys, Roberta M. and Jones, Terry J. and Marengo, Massimo and Gehrz, Robert D. and Helton, L. Andrew and Hoffmann, William F. and Skemer, Andrew J. and Hinz, Philip M. , title =. , abstract =. 2016 , month =. doi:10.3847/0004-6256/151/3/51 , url =

    work page doi:10.3847/0004-6256/151/3/51 2016

  69. [70]

    , keywords =

    SiO emission from a huge, detached shell in IRC +10420. , keywords =. doi:10.1051/0004-6361:20010211 , adsurl =

    work page doi:10.1051/0004-6361:20010211

  70. [71]

    , abstract =

    Dinh-V-Trung and Wong, Ka tat and Lim, Jeremy , title =. , abstract =. 2017 , month =. doi:10.3847/1538-4357/aa932b , url =

    work page doi:10.3847/1538-4357/aa932b 2017

  71. [72]

    Klochkova, V. G. and Chentsov, E. L. and Miroshnichenko, A. S. and Panchuk, V. E. and Yushkin, M. V. , title =. , volume =. 2016 , month =. doi:10.1093/mnras/stw902 , url =

    work page doi:10.1093/mnras/stw902 2016

  72. [75]

    10.1051/0004-6361:20031110

    Mass-loss from dusty, low outflow-velocity AGB stars* - I. Wind structure and mass-loss rates , DOI= "10.1051/0004-6361:20031110", url= "https://doi.org/10.1051/0004-6361:20031110", journal =

    doi:10.1051/0004-6361:20031110

  73. [76]

    , keywords =

    What Are the R Coronae Borealis Stars?. , keywords =. doi:10.48550/arXiv.1206.3448 , archivePrefix =. 1206.3448 , primaryClass =

    Pith/arXiv arXiv doi:10.48550/arxiv.1206.3448

  74. [77]

    10.1051/0004-6361/201731549

    Unidentified emission features in the R Coronae Borealis star V854 Centauri , DOI= "10.1051/0004-6361/201731549", url= "https://doi.org/10.1051/0004-6361/201731549", journal =

    work page doi:10.1051/0004-6361/201731549

  75. [78]

    10.1051/0004-6361/201424173

    The RCB star V854 Centauri is surrounded by a hot dusty shell ⋆⋆⋆ , DOI= "10.1051/0004-6361/201424173", url= "https://doi.org/10.1051/0004-6361/201424173", journal =

    work page doi:10.1051/0004-6361/201424173

  76. [79]

    , keywords =

    High-resolution spectroscopy of V854 Cen in decline - absorption and emission lines of C _ 2 molecules. , keywords =. doi:10.1046/j.1365-8711.2000.03397.x , archivePrefix =. astro-ph/0002237 , primaryClass =

    arXiv 2000

  77. [80]

    , keywords =

    The evolution of the Mira variable R Hydrae. , keywords =. doi:10.1046/j.1365-8711.2002.05467.x , archivePrefix =. astro-ph/0203328 , primaryClass =

    arXiv 2002

  78. [81]

    The CDS reference database for astronomical objects

    The SIMBAD astronomical database. The CDS reference database for astronomical objects. , keywords =. doi:10.1051/aas:2000332 , archivePrefix =. astro-ph/0002110 , primaryClass =

    Pith/arXiv arXiv

  79. [82]

    , volume=

    New diameter measurements of 10 Mira Variables: implications for effective temperatures, atmospheric structure and pulsation modes , author=. , volume=. 1995 , publisher=

    1995

  80. [83]

    , keywords =

    Detection of a Far-Infrared Bow Shock Nebula around R Hya: The First MIRIAD Results. , keywords =. doi:10.1086/507627 , archivePrefix =. astro-ph/0607303 , primaryClass =

    Pith/arXiv arXiv

Showing first 80 references.