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arxiv: 2606.19455 · v1 · pith:IGVP7BIVnew · submitted 2026-06-17 · 🌌 astro-ph.SR

X-Shooter survey of disk accretion in Upper Scorpius II. A lack of correlation between accretion rates and disk properties

A. Empey , C.F. Manara , R. Garcia Lopez , A. Natta , R. Claes , F. Zagaria , J.M. Alcal\'a , R. Anania
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G. Beccari J. Carpenter S. Facchini D. Fedele G. Lodato K. Mauco A. Miotello B. Nisini I. Pascucci L. Piscarreta G. Rosotti A. Scholz L. Testi M. Vioque
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Pith reviewed 2026-06-26 19:06 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords protoplanetary disksaccretion ratesUpper ScorpiusX-ShooterALMA continuumdisk evolutionstellar massstar formation
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The pith

Accretion rates in Upper Scorpius show only weak correlation with stellar mass and none with disk dust mass or radius.

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

The paper measures accretion luminosity for 127 disk-bearing stars in Upper Scorpius from X-Shooter spectra, deriving values or upper limits via excess UV emission after subtracting photospheric and chromospheric contributions. It reports only a weak link between mass accretion rate and stellar mass, with no correlation to disk dust mass or gas radius from ALMA data. Roughly half the sample yields upper limits set by signal quality or chromospheric floors. The scatter around these relations exceeds that in younger regions such as Lupus and Chamaeleon I. The pattern indicates that inner-disk accretion has decoupled from outer-disk structure by the association's age.

Core claim

Measurements of accretion luminosity in Upper Scorpius stars with disks reveal only a weak dependence on stellar mass and no dependence on disk dust mass or gas radius. The dispersion around these relations exceeds that seen in younger star-forming regions, and upper limits on accretion for half the sample support the view that inner-disk accretion has become decoupled from outer-disk properties by this age. Sub-group membership and the presence of binaries or transition disks do not explain the observed scatter.

What carries the argument

FRAPPE method to derive accretion luminosity from UV continuum excess relative to photospheric and chromospheric emission, applied self-consistently with spectral type, extinction, and luminosity, together with a procedure for setting upper limits when the excess falls below the chromospheric floor.

If this is right

  • Evolutionary models must accommodate the loss of accretion-disk correlations and increased dispersion by the age of Upper Scorpius.
  • Inner and outer disk regions operate independently at this stage of evolution.
  • The dispersion is intrinsic and not produced by sub-group membership, binaries, or transition disks.
  • Accretion properties vary more widely than disk structural parameters at this age.

Where Pith is reading between the lines

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

  • Planet-formation models may need to treat gas accretion in the inner disk as independent of outer-disk dust mass after a few million years.
  • Surveys of other associations at similar ages could test whether decoupling of inner and outer disks is a general evolutionary feature.
  • The larger dispersion could revise estimates of how long individual disks sustain accretion before dispersal.

Load-bearing premise

The upper limits on accretion luminosity for half the sample are unbiased and the FRAPPE separation of accretion excess from chromospheric activity holds across the full range of spectral types and extinctions present.

What would settle it

A re-analysis of the sample with deeper spectra that converts a substantial fraction of the upper limits into detections and recovers a statistically significant correlation between accretion rate and disk dust mass would falsify the reported lack of correlation.

Figures

Figures reproduced from arXiv: 2606.19455 by A. Empey, A. Miotello, A. Natta, A. Scholz, B. Nisini, C.F. Manara, D. Fedele, F. Zagaria, G. Beccari, G. Lodato, G. Rosotti, I. Pascucci, J. Carpenter, J.M. Alcal\'a, K. Mauco, L. Piscarreta, L. Testi, M. Vioque, R. Anania, R. Claes, R. Garcia Lopez, S. Facchini.

Figure 1
Figure 1. Figure 1: HR diagram for the sample of disc-bearing stars in Upper [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Lacc/L⋆ as a function of Teff. The dashed grey line rep￾resents the limit of chromospheric emission derived by Manara et al. (2013b). The measured accretion luminosities for any ob￾jects having a ratio equal to or below this line may be contami￾nated by emission from their chromosphere. They are indicated with hollow markers. Upper limits as described in Sect. 3.2 are marked with downward facing arrows. je… view at source ↗
Figure 3
Figure 3. Figure 3: Top panel: Accretion luminosity (Lacc) plotted as a func￾tion of stellar luminosity (L⋆). Magenta solid points are defi￾nite accretors, those with downward pointing arrows have upper limit measurements based on their continuum excess. Hollow magenta points represent those targets whose values of Lacc/L⋆ ratio, are below that of the chromospheric limit (see [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Top panel: Mass accretion rate (M˙ acc) plotted as a func￾tion of stellar mass (M⋆). Symbols and power-law fit as in [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 7
Figure 7. Figure 7: M˙ acc plotted against Mdisc for the most abundant USco subgroups in our sample detected with Gaia (Ratzenböck et al. 2023b). 112 objects in our sample were reported to be associated with 8 subgroup in the region. The sample sizes in each vary from 1 object to 45, here we highlight the objects associated with the δ Sco group (orange points, 45 objects). In grey are the rest of the objects in our sample. Th… view at source ↗
Figure 8
Figure 8. Figure 8: M˙ acc plotted against Mdisc with binary targets highlighted. Cyan diamonds represent known binaries present in the sample. Here we also highlight potential binary systems in the sample identified by Barenfeld et al. (2019), Xie et al. in prep. The grey error bar represents the typical uncertainty on the values of M˙ acc. 5.3. Effect of binarity and disc structures Previous studies have shown that differen… view at source ↗
Figure 9
Figure 9. Figure 9: M˙ acc plotted against Mdisc with transition and structured discs highlighted with lime squares and pink crosses to iden￾tify transition discs and structured discs (evidence of disc sub￾structures), respectively (see Carpenter et al. 2025; Pinilla et al. 2025). The grey error bar represents the typical uncertainty on the values of M˙ acc. of the less massive discs. The values of M˙ acc are once again very … view at source ↗
Figure 11
Figure 11. Figure 11: M˙ acc plotted against Mdisc for this sample alongside val￾ues for the younger star forming regions: ρ Ophiuchus (L1688), Chamaeleon (Cham) I & II, Lupus, and Taurus. Data was col￾lected from Manara et al. (2023). The dashed grey line repre￾sents a disc lifetime (τacc = Mdisc/M˙ acc) of 1 Myr to guide the eye. The grey error bar represents the typical uncertainty on the values of M˙ acc. sured from the ot… view at source ↗
Figure 12
Figure 12. Figure 12: M˙ acc plotted against Mdisc for the Lupus, Chamaeleon I and Upper Scorpius star forming regions. Values for Lupus and Chamaeleon I are those reported in Manara et al. (2023) while the Upper Scorpius sample is the one presented in this paper. In all plots the relations are fit with the linmix python package (Kelly 2007). The fit parameters for each region are shown in the textboxes of each subplot. The da… view at source ↗
read the original abstract

The evolution of protoplanetary discs is intertwined with the process of planet formation, growth and migration. Studies of nearby star forming regions of different ages and properties provide the necessary information needed to understand the processes dictating their evolution. This paper presents the results of a spectroscopic study of the stellar and accretion properties of a large sample of 127 stars with protoplanetary discs in the Upper Scorpius region with disc dust masses inferred from ALMA continuum measurements. The accretion luminosity is derived from the excess UV continuum emission with respect to the photospheric and chromospheric one self-consistently with the stellar spectral types, extinction and luminosity, using FRAPPE. We apply a new method to evaluate upper limits to the accretion luminosity. In ~50% of cases we evaluate upper limits on the accretion luminosity, either because the S/N of the data is insufficient or because the measured value of the accretion luminosity is below the estimate of the emission due to chromospheric activity. The results show that the mass accretion rate has a weak correlation with the stellar mass, while no correlation is observed with disc properties such as dust mass or gas disc radius. The dispersion is larger than what is found in younger star forming regions such as Lupus and Cham. I, and suggests a fading of the correlations with age. We find no evidence that membership to Upper Scorpius sub-groups, nor the properties of known binary or transition discs can explain the origin of this dispersion. The lack of correlation and large dispersion of accretion rates challenge the current expectations of evolutionary models. The observed properties point to a decoupling of the inner and outer disc by the age of Upper Scorpius and a fading of the relations observed in younger star forming regions.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 0 minor

Summary. This paper reports results from an X-Shooter survey of 127 disk-bearing stars in Upper Scorpius with ALMA-derived disk properties. Accretion luminosities (or upper limits) are derived self-consistently via FRAPPE, including a new method for upper limits applied to ~50% of the sample where measured L_acc falls below the chromospheric floor or S/N is insufficient. The central claims are a weak Ṁ_acc–M_* correlation, no correlation with M_dust or R_gas, larger dispersion than in Lupus or Chamaeleon I, and no explanatory power from sub-group membership, binaries, or transition disks, implying inner–outer disk decoupling and fading of relations by the age of Upper Sco.

Significance. If the upper limits prove robust, the result would be significant for disk-evolution studies: a large, homogeneous sample with ancillary ALMA data shows the disappearance of correlations seen at younger ages, directly challenging model expectations of persistent Ṁ_acc–disk links. The new upper-limit method and direct inter-region comparison are strengths that could be cited if validated.

major comments (1)
  1. [Abstract] Abstract and methods (FRAPPE upper-limit procedure): The no-correlation and increased-dispersion claims are load-bearing on the ~50% upper limits being free of systematic bias. The text states that upper limits are evaluated when L_acc is below the chromospheric estimate or S/N is low, but provides no quantitative validation, error budget, or tests of the FRAPPE separation across the sample’s spectral-type and extinction range; this directly affects whether the reported dispersion is physical or methodological.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thorough review and valuable feedback on our manuscript. We address the major comment regarding the validation of the FRAPPE upper-limit procedure below.

read point-by-point responses

  1. Referee: [Abstract] Abstract and methods (FRAPPE upper-limit procedure): The no-correlation and increased-dispersion claims are load-bearing on the ~50% upper limits being free of systematic bias. The text states that upper limits are evaluated when L_acc is below the chromospheric estimate or S/N is low, but provides no quantitative validation, error budget, or tests of the FRAPPE separation across the sample’s spectral-type and extinction range; this directly affects whether the reported dispersion is physical or methodological.

    Authors: We acknowledge that the current manuscript lacks a detailed quantitative validation, error budget, and tests of the FRAPPE method across the spectral type and extinction range of the sample. This is a valid point, as such information would strengthen the robustness of our conclusions on the dispersion and lack of correlations. In the revised version, we will add an appendix or subsection in the methods describing quantitative tests (e.g., recovery tests on simulated spectra and comparisons with literature values for similar objects), an error budget for the upper limits, and verification that the method performs consistently across the parameter space. We believe this will confirm that the increased dispersion is physical rather than methodological. revision: yes

Circularity Check

0 steps flagged

No significant circularity: purely observational data analysis

full rationale

The paper reports direct measurements of accretion luminosities (and upper limits) via the FRAPPE method on X-Shooter spectra for 127 Upper Sco stars, combined with ALMA-derived disk dust masses and radii. Correlations (or lack thereof) with stellar mass, M_dust, and R_gas are computed from these independent observables. No equations derive a 'prediction' that reduces by construction to fitted parameters or self-cited ansatzes; the dispersion and decoupling claims follow from the data distribution itself. FRAPPE and the new upper-limit method are external tools applied to the sample, not self-referential definitions. Self-citations (e.g., to prior X-Shooter surveys) are not load-bearing for the central negative result. This matches the default expectation for an observational survey.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Observational survey paper; no free parameters, mathematical axioms, or invented entities are introduced. The central claim rests on the accuracy of the FRAPPE accretion measurement pipeline and the assumption that upper limits are statistically representative.

pith-pipeline@v0.9.1-grok · 5960 in / 1284 out tokens · 20791 ms · 2026-06-26T19:06:33.335055+00:00 · methodology

discussion (0)

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Reference graph

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