Planet-forming disks and their environment across regions and time from the full NIR census

Andrew Winter; Antonio Garufi; Carlo Felice Manara; Carsten Dominik; Christian Ginski; Jane Huang; Miguel Vioque; Myriam Benisty

REVIEW 4 major objections 5 minor 5 cited by

This census of 268 near-infrared disk images argues that ambient infalling material—not only young planets—produces many of the spirals and shadows seen in planet-forming disks, and that disk brightness jumps sharply between 2 and 5 Myr.

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

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

T0 review · deepseek-v4-flash

2026-08-02 19:33 UTC pith:AFVQU72C

load-bearing objection A valuable, carefully assembled census that should be the reference for NIR disk demographics—but the abstract's claim that environment 'proves' the infall-spiral connection outruns what the body actually establishes. the 4 major comments →

arxiv 2603.01703 v1 pith:AFVQU72C submitted 2026-03-02 astro-ph.SR astro-ph.EP

Planet-forming disks and their environment across regions and time from the full NIR census

Antonio Garufi , Christian Ginski , Myriam Benisty , Miguel Vioque , Andrew Winter , Jane Huang , Carlo Felice Manara , Carsten Dominik This is my paper

classification astro-ph.SR astro-ph.EP

keywords protoplanetary disksnear-infrared polarimetrydisk substructurespiral armslate infallstellar accretiondisk evolutioncircumstellar environment

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.

The paper assembles the largest near-infrared high-contrast census of planet-forming disks to date, 268 sources, and uses it to argue that the surrounding environment is a first-order driver of disk evolution. It finds that disks brighten abruptly between 2 and 5 Myr, that the earliest cavities in single-star disks appear only after 2–3 Myr, and that disks older than 8 Myr are always bright. Its central proposal is that late infall of ambient material, not just embedded planets, produces many of the spiral arms and shadows seen in these disks. The claim matters because it would reframe how spiral structures are interpreted in planet searches and how disk lifetimes are tied to environment.

Core claim

By homogenizing stellar ages, masses, accretion rates, variability, and infrared excesses across a 268-source sample, the paper shows that disks in coeval regions differ systematically: Lupus disks are bright, Chamaeleon disks faint, and Taurus and Corona Australis disks are frequently embedded in ambient emission. The time sequence shows a sharp rise in disk brightness between 2 and 5 Myr, with no near-infrared cavities around single stars younger than about 2.5–3 Myr. The strongest specific result is statistical: among disks with detected ambient material, about half show spiral arms and half show shadows, while none show rings. The paper therefore proposes that late infall from the inters

What carries the argument

The key object is the census itself: a uniformly processed sample of 268 near-infrared scattered-light images with re-derived stellar parameters. The mechanistic load is carried by the classification of ambient material (streamers, envelope leftovers, binary-interaction structures) as a tracer of late infall. Because this infalling gas arrives with a different angular momentum direction, it can warp the inner disk and excite spiral density waves in the outer surface seen in scattered light, while a ring-like structure would require a more symmetric perturbation.

Load-bearing premise

The ages of the stars come from pre-main-sequence evolutionary tracks, which carry factor-of-two-to-three systematic uncertainties for young stars, and every time-dependent claim in the paper rests on this age scale.

What would settle it

A sample of disks with ages measured directly from cluster membership or lithium depletion (instead of isochrones) that showed no sharp brightness jump between 2 and 5 Myr, or a single disk with clear rings embedded in strong infalling ambient material, would contradict the paper's central claims.

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

If this is right

If infall-driven spirals are common, then many spiral patterns in near-infrared images are weak evidence for embedded planets; planet-search programs should treat disks with ambient material as contaminated.
The 2–5 Myr brightness jump implies that disk evolution has a sharp transition at roughly 3 Myr, when inner dust clearing begins in single stars.
Long-lived disks (>8 Myr) are always bright and usually cavity-bearing, supporting the idea that only disks with a strong pressure bump survive.
The region-to-region differences among coeval disks mean that local environment, not age alone, sets the typical disk morphology.
The association of ambient material with higher accretion rates ties episodic accretion to the disk's external environment.

Where Pith is reading between the lines

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

A deeper survey reaching fainter low-mass old disks (e.g., with future 30-m telescopes) could test whether the 'old disks are always bright' statement is an upper-envelope selection effect rather than a physical law.
If infall drives warps, then the fraction of disks with shadows in a region should correlate with the local interstellar gas density; this is testable region by region with current cloud surveys.
The claim that rings never appear in disks with ambient material may be a timescale effect: rings take longer to emerge, and infall either prevents their formation or destroys them, a distinction that ALMA midplane observations could decide.
Spin-orbit misalignment statistics from future astrometric surveys could independently confirm that late infall, rather than companions, is the dominant warp mechanism.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

A valuable, carefully assembled census that should be the reference for NIR disk demographics—but the abstract's claim that environment 'proves' the infall-spiral connection outruns what the body actually establishes.

read the letter

You should know two things about this one. First, the census itself is a real contribution: 268 sources, 51 new SPHERE images, homogenized stellar and disk properties, and an honest completeness analysis (Table 2) that most papers in this field skip. The descriptive findings—region-dependent disk brightness, the abrupt 2–5 Myr brightening, the absence of NIR cavities around young single stars, and the ambient-↔spiral/shadow association with zero rings among ambient sources—are new and will be widely cited. The per-object flags for parallax, extinction, and inclination show careful bookkeeping, and the authors deserve credit for dropping flagged sources from the time plots rather than pretending the data are clean.

The soft spots are real but localized. The age axis rests on isochrone binning with known factor-of-2–3 systematics, and the flagged sources cluster exactly where the 'old disks are always bright' claim lives. That doesn't kill the demographics, but it means the time-dependent statements carry more uncertainty than the figures suggest.

The bigger issue is the central causal claim. The paper shows that ambient material and spirals/shadows co-occur, and that ring disks rarely show ambient signal. But as the paper itself notes (Sect. 4.3), ambient material is preferentially detected around bright, high-NIR-excess disks, and substructures are also detected far more often in bright disks (>90% vs <20%). The stress-test note is correct: without controlling for brightness/selection, the zero-ring result could partly reflect that ring disks are fainter and their ambient material is simply not detected. The body concedes this is 'suggestive rather than conclusive'—yet the abstract upgrades it to 'proves.' That internal mismatch is the weakest link, and it should be fixed before this becomes the field's reference result.

There is no circularity problem here in the fitting sense; this is a census, and the statistics are direct measurements. The self-citations are methodological lineage from prior published work, which is fine. The visual classification is acknowledged as subjective, and the fractions lack error bars or blind-validation, but those are addressable in revision.

Who is this for? Anyone working on disk evolution, scattered-light imaging, or the environmental dependence of planet formation. It deserves a serious referee and careful revision, not a desk reject. My recommendation: engage with it, but push the authors to quantify the selection effects, add mock/detection-sensitivity tests for the ambient-spiral association, and align the abstract with the body's own caution.

Referee Report

4 major / 5 minor

Summary. This manuscript presents a census of 268 young stars with near-IR high-contrast imaging, adding 51 unpublished SPHERE datasets. The authors consistently derive stellar masses, ages, accretion rates, IR excesses, and mm-based dust-mass proxies; they flag sources with poor parallaxes, high extinction, and high disk inclination; and they classify disk detections, disk brightness via alpha_pol, substructures (cavity, rings, spirals), shadows, and ambient material. The main claims are: disk NIR brightness rises abruptly between ~2 and 5 Myr; NIR cavities around single stars appear only after 2–3 Myr; old disks are always bright; ambient material is present in ~20% of sources and decreases with age; and half of disks with ambient material show spirals and shadows while none show rings. The authors propose that late infall from the ISM generally induces the spirals and warps responsible for shadows, and that this infall also boosts stellar variability and accretion.

Significance. If the results hold, this becomes the reference NIR disk census and shifts the interpretation of NIR spirals/shadows from primarily planet-induced to partly environment-induced. The manuscript's strengths are real: a transparent 268-source compilation, 51 new SPHERE images, explicit quality flags for parallax/extinction/inclination, an honest completeness analysis (Table 2), consistent derivation of stellar and disk properties, and open publication of the per-object table. The statistics are direct measurements and no quantity is fitted to a target claim, so circularity is not the concern. The main risks are age-systematics and a brightness/selection confound in the infall–morphology association; both are addressable within this manuscript's scope.

major comments (4)

[§2.2/2.4, Fig. 4b] All time-dependent claims (brightness rise 2–5 Myr, cavity onset at 2.5–3 Myr, declining ambient fraction, “old disks are always bright”) are binned by isochrone ages. The paper acknowledges the difficulty and flags high-extinction/poor-parallax/inclined sources, but flagged sources cluster in the oldest quartile of the young regions, and the age scale depends on the choice among five track sets. A factor-of-2–3 age error would smear or shift the 2–5 Myr transition, while the absence of old faint/low-mass disks is partly an R<13 selection effect. Please provide a robustness test: recompute Fig. 4(b) and the age-bin statistics for each track set separately and with/without flagged sources; ideally anchor the young/mature/old boundaries to region membership as a cross-check.
[§3.3.3 and §3.4, Fig. 6] The core infall–spiral association is not controlled for disk brightness. The same paper states that substructures are found in >90% of bright disks but <20% of faint disks, and ambient sources preferentially occupy the high-NIR-excess, enshrouded quadrant (two-thirds of the 52 ambient sources). Since alpha_pol and NIR excess govern both the detectability of spirals and the detectability of faint ambient scattered light, the reported correlation may be a selection effect. Ring hosts have lower NIR excess and variability than spiral hosts, so the zero-ring count among ambient disks may partly reflect non-detection of ambient material around ring disks. Please stratify the ambient–morphology comparison by alpha_pol and NIR-excess bins, or match non-ambient control disks, and report exact counts with binomial confidence intervals for the 52%/48%/0% fractions.
[§3.4] The “ambient material” category includes 25 sources classified as binary interaction, and stellar systems show a higher ambient fraction (Fig. 3). Stellar companions can independently create spirals, warps, shadows, and variability (e.g., GG Tau, HD100453). Therefore the statistical association between ambient signal and spirals is not uniquely attributable to late infall. Please separate the binary-interaction class from the streamer/environment class in the correlation analysis, or control for multiplicity; at minimum, report how many of the spiral+ambient disks are binary systems.
[§4.3, Table 3] The cross-region test connecting ISM surface density to ambient fraction is acknowledged as “suggestive rather than conclusive,” but as written it is not a test: aggregate Sigma_gas is averaged over YSO sub-regions, Taurus has no quoted uncertainty, and n=7 regions. The same table shows Corona Australis with high ambient fraction but not the highest Sigma_gas, and Ophiuchus has only a slightly higher ambient fraction than Lupus despite a much higher Sigma_gas. This is acceptable as motivation, but it should not be presented as supporting evidence for infall; either provide per-source local density estimates or explicitly mark the comparison as an untested hypothesis.

minor comments (5)

[Abstract and §4] Minor language issues: “why are young disks faint” should be “why young disks are faint”; “two-third” should be “two-thirds”; the opening of §4 has “the our considerations” — remove “the”.
[Fig. 4 and Appendix A tables] The units of disk brightness are inconsistent: Fig. 4 uses percent contrast, while Tables A.1–A.5 quote alpha_pol in 10^-3. Please define the conversion once and use a single convention throughout.
[Table 2] The column header f_obs/II(R<13) is dense and ambiguous. Clarify in the caption whether the denominator is all Class II sources or only those with R<13, and label columns more explicitly.
[§3.4] The ambient categories (envelope, binary interaction, environment) are said to be non-exclusive, but the text reports 8, 25, and 44 sources. State how many unique sources have each flag and how the 52 total is obtained after overlap.
[Appendix A] PDS 144 N is shown in Fig. A.1 but excluded from the sample, and the text also uses “PDS 144 A” and “PDS 144 S.” Please make the naming and inclusion decision consistent in the table and gallery.

Circularity Check

0 steps flagged

No significant circularity: census statistics are direct measurements; no fitted parameter is repackaged as a prediction.

full rationale

This paper is an observational census, not a derivation with fitted parameters that are then used to predict the same data. The central claims—disk brightness trends, substructure fractions, ambient-material incidence, and correlations with variability/accretion—are direct counts, medians, and classifications from the 268-source image sample. No equation in the paper defines a quantity in terms of the very quantity it is used to explain; for example, the brightness measure α_pol is a defined observable, and the paper explicitly notes where its construction affects interpretations (Sect. 3.2.2: 'any flux detected at large radii, by construction of α_pol, significantly contributes to the disk brightness'), rather than treating that as an independent prediction. The infall–spiral proposal (Sect. 4.3) is presented as an interpretation of a statistical association, not as a result forced by fitting a parameter to that association. Self-citations (Garufi et al. 2017 for α_pol, Garufi et al. 2018 for the age method, Garufi et al. 2022a for the SED quadrant scheme) are methodological lineage or prior independent data applied to a larger sample; they are not used in place of evidence for the paper's new claims. The paper also acknowledges and attempts to address known selection effects, such as the faintness of old low-mass stars and the brightness dependence of substructure detectability, rather than hiding them. Thus no step in the claimed chain reduces to its own inputs by construction.

Axiom & Free-Parameter Ledger

4 free parameters · 5 axioms · 0 invented entities

The census introduces no new physical entities and fits no free parameters to a target result. The ledger is dominated by selection and interpretation choices: hand-set age boundaries, an R<13 observability cutoff, sample exclusions, and standard domain assumptions (isochrone ages, α_pol as brightness proxy, visual labels, cavity/infall interpretations). These are all conventional in the field, but they are the load-bearing premises of the time-trend and environment claims and are untested within this paper.

free parameters (4)

Age boundaries (young ≤3 Myr, mature 3–8 Myr, old >8 Myr) = 3 Myr, 8 Myr
Chosen by hand from literature disk-fraction thresholds (Richert et al. 2018, Sect. 2.4); every time-trend claim (brightness jump, cavity timing, ambient decay, old-disk brightness) depends on these cutoffs.
Observability threshold R<13 (G_RP) = R ≈ 13 mag
Adopted technical limit for current AO instruments (Sect. 2.3, footnote 6); drives the completeness table and removes old low-mass stars, directly shaping the 'old disks are always bright' claim.
Sample exclusions (embedded Class I, edge-on disks, no IR excess to 20 µm) = 10 Class I, ~2 edge-on, no-excess sources excluded
Hand-made sample boundaries in Sect. 2.1; they exclude exactly the sources whose NIR appearance differs most from the rest, so the 'full census' is a census of AO-accessible, moderately inclined Class II-like disks.
Millimeter flux → dust mass conversion = ≈100 mJy at 150 pc ≃ 10 M⊕
Used only for the top x-axis of Fig. 4(d) 'under standard assumptions'; the 'very massive disks that are faint' (self-shadowed) reading depends on this conversion, though no headline claim uses it.

axioms (5)

domain assumption Pre-main-sequence isochrones (Siess 2000; Bressan 2012; Baraffe 2015; Choi 2016; Feiden 2016) give unbiased stellar ages for 1–20 Myr stars once extinction/inclination are flagged
Sect. 2.2: the median-of-tracks age is treated as ground truth for all age trends (Fig. 4b); the paper flags difficult cases but does not quantify residual age systematics.
domain assumption Polarized near-IR scattered light (α_pol) is a fair proxy for outer-disk illumination and brightness
Sect. 3.1.2, following Garufi et al. 2017; all brightness comparisons (region, age, mass) rest on this equivalence, including the claim that Lupus disks are 5x brighter than Chamaeleon disks.
domain assumption Visual classification of disks (detection, cavity/ring/spiral/shadow) and of ambient material is uniform and reliable across SPHERE, GPI, NaCo, HiCiao, and HST images
Sect. 3.1.2 admits 'some minor level of subjectivity' in the detection scrutiny; the headline correlations (ambient↔spiral, zero rings with ambient) rest entirely on these labels, with no inter-observer or blind-check described.
domain assumption NIR cavities in scattered light trace dust-depleted inner regions whose opening requires a pressure bump (planet or companion)
Sect. 4.1: the 'cavity formation at 2–3 Myr sets disk longevity' narrative presupposes this interpretation; the paper explicitly states it does not aspire to explain the origin of cavities.
domain assumption Ambient light in the NIR traces late infall from the ISM rather than outflow cavities, envelope remnants, or chance projection
Sect. 4.3: ambient is sub-classified (envelope/binary/environment), but the physical infall claim leans on the region-level ISM-density comparison in Table 3, which the authors call 'suggestive rather than conclusive'.

pith-pipeline@v1.3.0-alltime-deepseek · 45351 in / 16418 out tokens · 161619 ms · 2026-08-02T19:33:00.495757+00:00 · methodology

0 comments

read the original abstract

The evolution of planet-forming disks and the processes of planet formation influence each other, and both of them are possibly impacted by the local environment. Extensive high-resolution imagery of disks across space and time is the best tool for determining their evolution. We compiled a comprehensive list of disk-bearing young stars with near-IR high-contrast images available. The sample sums up to 268 sources, including 51 targets with no prior publications, which makes this study the largest of its kind and the most extensive release of IR disk images to date. Our census reveals very diverse disk and ambient morphologies. Disks in Lupus are bright, in Chamaeleon are faint, in Corona Australis and Taurus are frequently surrounded by ambient emission. Disks experience an abrupt increase in IR brightness between 2 Myr and 5 Myr. The earliest IR disk cavities around single stars arise after 2-3 Myr explaining why are young disks faint in the near-IR, and determining which disks can live longer. Well-known, high-longevity disks (>8 Myr) are always bright. Ambient material is detected in more than 20% of young sources but the fraction drops with time. We find a clear correspondence for the presence of ambient material with the stellar variability, near-IR excess, and mass accretion rate as well as, in turn, with spirals and shadows in disks. Half of the disks with ambient material show spirals while none of them show rings. We therefore propose that the spirals and the disk warps responsible for shadows are generally induced by late infall from the medium, and that this also affects the stellar accretion. The emerging picture proves the fundamental role of the environment for the disk evolution and planet formation.

Figures

Figures reproduced from arXiv: 2603.01703 by Andrew Winter, Antonio Garufi, Carlo Felice Manara, Carsten Dominik, Christian Ginski, Jane Huang, Miguel Vioque, Myriam Benisty.

**Figure 1.** Figure 1: Stellar mass vs age diagram for the entire sample (left) and for the individual star-forming regions (right). The dashed line indicates the zero-age main sequence. In the main diagram, the diamonds indicate the median value of the regions color-coded as in the small panels while the median error bars at the three age stages (see [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗

**Figure 2.** Figure 2: Stellar and disk properties of the sample. Left: median fraction of systems, NIR and FIR excess (fraction of stellar flux), mass accretion rate (log(M⊙ yr−1 )), stellar variability (mag), and integrated millimeter flux at a same distance (mJy) for the sub-samples of [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗

**Figure 3.** Figure 3: Image properties of the sample. Fraction of non-detections, median disk brightness (in units of 10−4 ), fraction of disks with substructures and with shadows within images with a disk detected, and fraction of images with ambient emission for the sub-sample of [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗

**Figure 4.** Figure 4: Census of disk brightness. (a): trend with FIR excess for the seven most represented regions. The dashed line is the fit to all points except Orion, which is outlying due to the larger distance. (b): trend with age for all unflagged, nearby sources. The median value of all regions (including Orion) is shown with colored diamonds as in (a). The dashed line is the median in different age beams. (c): trend wi… view at source ↗

**Figure 5.** Figure 5: Census of disk sub-structures. The analysis of Sect. 3.3 is visually summarized. The stellar mass vs age diagrams for sources with disk cavity, rings, and spirals are shown to the right (see [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗

**Figure 6.** Figure 6: Census of ambient material. The analysis of Sect. 3.4 is visually summarized. The stellar variability vs NIR excess diagram is shown to the left. Faint, ambient structures visible from the images are indicated by arrows. The outermost image regions of DG Tau is in total intensity, and it illustrates the possible origin of the streamer reported by Garufi et al. (2022b). Underlined names indicate images with… view at source ↗

**Figure 7.** Figure 7: Spatial distribution of sample in the Sco-Cen association. Sources in Upper and Lower Centaurus (as well as the outlying HD169142 and HD152404) are in the top map while sources in Upper Scorpius are in the bottom map. No source in Ophiuchus or Lupus is shown here (see [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗

**Figure 8.** Figure 8: Same as [PITH_FULL_IMAGE:figures/full_fig_p013_8.png] view at source ↗

**Figure 9.** Figure 9: Same as [PITH_FULL_IMAGE:figures/full_fig_p014_9.png] view at source ↗

**Figure 10.** Figure 10: Visual synopsis of the census. sion toward lower-mass stars, smaller planet-forming disks, and further star-forming regions. Acknowledgements. The research activities described in this paper were carried out with contribution of the Next Generation EU funds within the National Recovery and Resilience Plan (PNRR), Mission 4 - Education and Research, Component 2 - From Research to Business (M4C2), Investm… view at source ↗

discussion (0)

Forward citations

Cited by 5 Pith papers

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

Interpreting the scattering surface in protoplanetary disks
astro-ph.EP 2026-06 unverdicted novelty 6.0

Semi-analytical model links observed scattering-surface height to small-dust mass, yielding global mass fractions of order 10^{-3} consistent with modest grain growth in ten protoplanetary disks.
Interpreting the scattering surface in protoplanetary disks
astro-ph.EP 2026-06 conditional novelty 6.0

Scattered-light ring heights trace the tau~1 surface and, combined with CO temperature maps, yield small-dust mass fractions near 10^-3 in ten protoplanetary disks.
Scattered light signatures of flyby-induced warps in protoplanetary discs
astro-ph.EP 2026-05 unverdicted novelty 5.0

Flyby-induced warps create broad, time-varying shadows in scattered light that persist for most of a low-viscosity disc lifetime and could be used to constrain disc viscosity.
Scattered light signatures of flyby-induced warps in protoplanetary discs
astro-ph.EP 2026-05 unverdicted novelty 5.0

Flyby-induced warps create observable oscillating shadows in scattered light for low-viscosity discs lasting most of their ~10^6 year lifetime, enabling surveys to probe viscosity.
Analysis of the young disk around WRAY 15-1880: does it contain a primitive planetary system?
astro-ph.SR 2026-06 unverdicted novelty 4.0

A candidate 0.3-7.6 MJup companion is reported in the gap of the ~2.8 Myr pre-transitional disk around WRAY 15-1880, with an ALMA blob interpreted as a vortex at the m=1 Lindblad resonance.

Reference graph

Works this paper leans on

4 extracted references · 1 linked inside Pith · cited by 3 Pith papers

[1]

L., Jensen, E

Akeson, R. L., Jensen, E. L. N., Carpenter, J., et al. 2019, ApJ, 872, 158 Akiyama, E., V orobyov, E. I., Liu, H. B., et al. 2019, AJ, 157, 165 Alcalá, J. M., Manara, C. F., Natta, A., et al. 2017, A&A, 600, A20 André, P., Belloche, A., Motte, F., & Peretto, N. 2007, A&A, 472, 519 André, P., Men’shchikov, A., Bontemps, S., et al. 2010, A&A, 518, L102 Andr...

Pith/arXiv arXiv 2019
[134]

This case is very similar to that of Sz 72 where a deviation from centro-symmetric scattering induced by a very inclined disk is possible

The disk is only marginally detected around the coro- nagraph. This case is very similar to that of Sz 72 where a deviation from centro-symmetric scattering induced by a very inclined disk is possible. Appendix A.2: Y oung intermediate-mass stars Nine stars were observed in the program 0111.C-0369 (PI: Vioque). Two of them (HD158643 – or 51 Oph – and HD50...

2022
[415]

The image shows a very inclined disk

This is a showcase of SPHERE detections. The image shows a very inclined disk. Here, the disk upper rim seems to almost occult the star (since the disk is almost seen edge-on), and the disk back side is almost as bright as the front side. Interestingly, the northern part of the image reveals an asymmetric arm that is intuitively interpreted as a verticall...

2013
[2022]

DoAr 28 was observed with HiCiao by Rich et al

revealing a very inclined disk that looks very similar in the SPHERE image. DoAr 28 was observed with HiCiao by Rich et al. (2015) who reported polarized emission from an inclined disk and from some asymmetric features. The SPHERE image reveals the same inclined disk but shows no obvious evidence of extended emission exterior to it. The SPHERE image of J1...

2015

[1] [1]

L., Jensen, E

Akeson, R. L., Jensen, E. L. N., Carpenter, J., et al. 2019, ApJ, 872, 158 Akiyama, E., V orobyov, E. I., Liu, H. B., et al. 2019, AJ, 157, 165 Alcalá, J. M., Manara, C. F., Natta, A., et al. 2017, A&A, 600, A20 André, P., Belloche, A., Motte, F., & Peretto, N. 2007, A&A, 472, 519 André, P., Men’shchikov, A., Bontemps, S., et al. 2010, A&A, 518, L102 Andr...

Pith/arXiv arXiv 2019

[2] [134]

This case is very similar to that of Sz 72 where a deviation from centro-symmetric scattering induced by a very inclined disk is possible

The disk is only marginally detected around the coro- nagraph. This case is very similar to that of Sz 72 where a deviation from centro-symmetric scattering induced by a very inclined disk is possible. Appendix A.2: Y oung intermediate-mass stars Nine stars were observed in the program 0111.C-0369 (PI: Vioque). Two of them (HD158643 – or 51 Oph – and HD50...

2022

[3] [415]

The image shows a very inclined disk

This is a showcase of SPHERE detections. The image shows a very inclined disk. Here, the disk upper rim seems to almost occult the star (since the disk is almost seen edge-on), and the disk back side is almost as bright as the front side. Interestingly, the northern part of the image reveals an asymmetric arm that is intuitively interpreted as a verticall...

2013

[4] [2022]

DoAr 28 was observed with HiCiao by Rich et al

revealing a very inclined disk that looks very similar in the SPHERE image. DoAr 28 was observed with HiCiao by Rich et al. (2015) who reported polarized emission from an inclined disk and from some asymmetric features. The SPHERE image reveals the same inclined disk but shows no obvious evidence of extended emission exterior to it. The SPHERE image of J1...

2015