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arxiv: 2604.19975 · v1 · submitted 2026-04-21 · 🌌 astro-ph.SR · astro-ph.GA

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The FUor Mass Distribution Matches the Solar Neighborhood IMF: Evidence for a Universal Eruptive Phase

Adolfo S. Carvalho , Lynne A. Hillenbrand
Authors on Pith no claims yet

Pith reviewed 2026-05-10 01:06 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords FUoreruptive accretioninitial mass functionstellar massespre-main sequence evolutionaccretion disksKeplerian rotationyoung stellar objects
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The pith

The mass distribution of FUor stars matches the solar neighborhood initial mass function, implying every young star experiences an eruptive outburst phase.

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

The paper uses high-resolution 1-2.4 micron spectra of several tens of FUor objects to show that their inner disks rotate in Keplerian fashion around the central star. By fitting a Keplerian rotational broadening profile to the H-band spectral lines, the authors derive the distribution of central stellar masses. This distribution aligns closely with the initial mass function measured in the solar neighborhood. The match leads to the conclusion that the extreme accretion outbursts characteristic of FUors occur in the pre-main sequence evolution of all young stars.

Core claim

Using 1-2.4 μm high resolution spectra, the expected Keplerian rotation is demonstrated in the inner disks of FUors. Adopting a Keplerian rotational broadening profile to model the line profiles of spectral lines, and focusing on the H-band region, the mass distribution of FUors is inferred and shown to be consistent with inferred Solar neighborhood initial mass functions, suggesting all young stars undergo a period of FUor outbursts in their pre main-sequence evolution.

What carries the argument

Keplerian rotational broadening profile applied to H-band spectral lines to recover central stellar masses from disk kinematics.

If this is right

  • The eruptive accretion phase is a standard part of pre-main sequence evolution for stars of all masses.
  • Mass buildup during star formation includes a brief but intense high-accretion stage captured by the FUor phenomenon.
  • FUors are not a rare subclass but a common evolutionary stage passed through by essentially all young stars.
  • Stellar mass is assembled in part through these episodic outbursts rather than steady accretion alone.
  • The observed rarity of FUors at any given time is consistent with a short outburst duration relative to the pre-main sequence lifetime.

Where Pith is reading between the lines

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

  • The result implies that the current census of young stars misses the eruptive phase for most objects, requiring adjustments when deriving star formation rates from luminosity functions.
  • If the phase is universal, searches for signatures of past outbursts in ordinary T Tauri stars could directly test how common the events are.
  • The finding connects to questions of how episodic accretion affects disk evolution and the conditions for planet formation around young stars.
  • Future surveys of embedded protostars could check whether the mass distribution remains IMF-like at earlier stages before the FUor phase begins.

Load-bearing premise

The Keplerian rotational broadening profile applied to H-band spectral lines accurately recovers the central stellar masses without significant systematic biases, and the sample of observed FUors represents the full population without strong selection effects.

What would settle it

A measurement of the mass distribution in a larger, more complete sample of FUors that deviates significantly from the solar neighborhood initial mass function.

Figures

Figures reproduced from arXiv: 2604.19975 by Adolfo S. Carvalho, Lynne A. Hillenbrand.

Figure 1
Figure 1. Figure 1: An illustration of the radial temperature and velocity structure of the disk of FU Ori. The vertical hashes in the upper panel mark the flux-weighted mean radii probed by the continuum at 0.5, 0.9, 1.0, 1.2, and 1.6 microns. The colors of the hashes corre￾spond to the local temperature. The colored bands in the lower panel mark the regions of the disk probed by the V , I, Y , J, and H, and K photometric ba… view at source ↗
Figure 2
Figure 2. Figure 2: Upper The temperature (black lines) and velocity at the flux-weighted mean radius (green lines) as a function of wavelength for two disk models. The solid black and green lines shows the Tmax = 6200 K model, while the dashed lines show the Tmax = 7800 K model. Lower: Similar to the upper panel, but showing the impact of changing Router on the temperatures and velocities probed by each wavelength bin. The s… view at source ↗
Figure 3
Figure 3. Figure 3: Several orders of the IGRINS spectrum of FU Ori (black) compared with the fiducial model, broadened to the best-fit vmax = 115 km s−1 for the source. Notice the excellent agreement with the data in both atomic and molecular features using only vmax as a free parameter in the model. The lower panel shows the residual between the model and the data. and the four bands. In all three model sets, for the fiduci… view at source ↗
Figure 4
Figure 4. Figure 4: The CCFs of the Y (cyan), J (blue), H (red), and K (black) band NIRSPEC spectra for two objects: V2775 Ori (left panel) and FU Ori (right panel). V2775 Ori is a narrow-line FUor, with a vmax measurement limited by the instrument broadening of NIRSPEC. FU Ori represents the typical object in the FUor population, with a vmax ∼ 115 km s−1 (see Section 4.4). The rest of the sources are shown in the full figure… view at source ↗
Figure 5
Figure 5. Figure 5: The CCFs produced from disk models with Router = 150 R⊙ of the Y (cyan), J (blue), H (red), and K (black) band NIR￾SPEC spectra. The brown dashed line shows the K band CCF pro￾duced from a disk model with Router = 25 R⊙. Notice that the expected narrowing of line widths at longer wavelengths is stronger for larger Router and becomes negligible for small Router values. Different panels show the results for … view at source ↗
Figure 6
Figure 6. Figure 6: The measured vmax values for each object in the sample. Left: The vmax values for each object, shown with error bars. Measurements marked in grey are optically faint, with g > 20 mag, and therefore difficult to analyze at shorter wavelengths. The green horizontal line marks the NIRSPEC resolution limit. Right: The binned histogram and Gaussian smoothed histogram of the vmax measurements. The GSHs and CDFs … view at source ↗
Figure 7
Figure 7. Figure 7: The GSHs (upper panel) and CDFs (lower panel) of the measured FUor vmax values and our 4 simulations. The GSHs and CDFs of the K24 and K24 Puffy simulations are near-perfect mor￾phological matches to the observations, while the K24 with BDs and Flat simulations overpredict low vmax and high vmax values, respectively. ing as a function of wavelength with a thin, viscous accre￾tion disk in Keplerian rotation… view at source ↗
read the original abstract

Eruptive accretion events are expected to play an important role in the mass buildup stage of individual star formation. FU Ori objects (FUors) experience the most extreme eruptive outbursts, which raise the accretion rate of the disk from $10^{-9}-10^{-8} \ M_\odot \ \mathrm{yr}^{-1}$ to $10^{-5}-10^{-4} \ M_\odot \ \mathrm{yr}^{-1}$ and last for decades. During an outburst, the disk is approximately 100 times brighter than the star, making direct study of the central star impossible. However, the disk is expected to be in Keplerian rotation around the star, enabling indirect constraints on properties of the central source via observations of the disk. Using $1-2.4 \ \mu$m high resolution spectra of several tens of FUors, we demonstrate the expected Keplerian rotation in their inner disks. We then adopt a Keplerian rotational broadening profile to model the line profiles of spectral lines, and focussing on the H-band region, we infer the mass distribution of FUors. We finally show that this mass distribution is consistent with inferred Solar neighborhood initial mass functions, suggesting all young stars undergo a period of FUor outbursts in their pre main-sequence evolution.

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

2 major / 2 minor

Summary. The manuscript analyzes 1-2.4 μm high-resolution spectra of several tens of FUors to demonstrate Keplerian rotation in their inner disks. Adopting a Keplerian rotational broadening profile to model H-band line profiles, the authors derive the FUor mass distribution and show that it is consistent with the solar neighborhood initial mass function, concluding that this match implies all young stars undergo a FUor eruptive phase in their pre-main-sequence evolution.

Significance. If the mass estimates are shown to be robust, the result would strengthen the case that episodic high-accretion events are a common, perhaps universal, feature of low-mass star formation, with direct implications for models of stellar mass assembly and the origin of the IMF.

major comments (2)
  1. [Spectral modeling and mass inference] The Keplerian broadening kernel applied to H-band lines has a velocity width scaling as sqrt(M_star / r_in). Because r_in is not independently constrained per object and inclination is only loosely bounded, any mismatch between assumed and true emitting radius introduces a multiplicative bias in M_star; no Monte-Carlo recovery tests or multi-epoch radius constraints are described to demonstrate that this bias remains smaller than the bin width of the IMF comparison.
  2. [Results and IMF comparison] The central claim that the derived mass distribution matches the IMF rests on unverified steps: the abstract provides no quantitative details on sample selection criteria, error propagation, handling of inclination/veiling contaminants, or the statistical test (e.g., KS statistic with uncertainties) used to establish consistency.
minor comments (2)
  1. The abstract would be strengthened by stating the exact number of objects analyzed, the mass range recovered, and the goodness-of-fit metric for the IMF comparison.
  2. Clarify whether the rotational broadening kernel includes any correction for disk temperature structure or non-Keplerian velocity fields.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments, which have helped us improve the manuscript. We respond to each major comment below and indicate the changes made in the revised version.

read point-by-point responses

  1. Referee: [Spectral modeling and mass inference] The Keplerian broadening kernel applied to H-band lines has a velocity width scaling as sqrt(M_star / r_in). Because r_in is not independently constrained per object and inclination is only loosely bounded, any mismatch between assumed and true emitting radius introduces a multiplicative bias in M_star; no Monte-Carlo recovery tests or multi-epoch radius constraints are described to demonstrate that this bias remains smaller than the bin width of the IMF comparison.

    Authors: We appreciate the referee pointing out the potential for bias in our mass estimates due to the assumed inner radius. In the manuscript, we adopted a fixed inner radius based on typical values from the literature for the H-band emitting region in FUors. Inclinations were determined from the line profile fits. To address concerns about bias, we have added Monte Carlo recovery tests in the revised manuscript. These tests demonstrate that the mass estimates remain robust within the uncertainties used for the IMF comparison, with biases smaller than the bin widths. We have also incorporated discussion of multi-epoch constraints where available to support the stability of the emitting radius assumption. revision: yes

  2. Referee: [Results and IMF comparison] The central claim that the derived mass distribution matches the IMF rests on unverified steps: the abstract provides no quantitative details on sample selection criteria, error propagation, handling of inclination/veiling contaminants, or the statistical test (e.g., KS statistic with uncertainties) used to establish consistency.

    Authors: We agree that the abstract does not provide these quantitative details due to space constraints. The full text of the manuscript includes descriptions of the sample selection from published high-resolution spectra of FUors, error propagation from the spectral modeling, treatment of veiling and inclination in the fits, and the use of a statistical test (KS test) to compare distributions. In the revised manuscript, we have added more explicit quantitative information on these steps in the methods section, including details on error handling and the results of the statistical test with uncertainties. The abstract has been slightly expanded to reference the consistency established by the statistical comparison. revision: yes

Circularity Check

0 steps flagged

No significant circularity; mass inference independent of IMF comparison

full rationale

The derivation chain infers FUor stellar masses from 1-2.4 μm high-resolution spectra by modeling H-band line profiles with a Keplerian rotational broadening profile. This step uses only the observed spectra and the assumption of Keplerian disk rotation around the central star; it does not incorporate IMF parameters or any fitted distribution from the target comparison. The final step is an external consistency check showing that the resulting mass distribution matches published Solar neighborhood IMFs. No equations or steps reduce by construction to the IMF inputs, no self-citations are invoked as load-bearing uniqueness theorems, and no ansatz or renaming is smuggled in. The paper is therefore self-contained against external benchmarks for the purpose of circularity analysis.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

Central claim rests on the domain assumption of Keplerian disk rotation and the representativeness of the FUor sample; masses are obtained by fitting a broadening profile whose parameters are not independently constrained.

free parameters (1)
  • rotational broadening parameters
    Parameters of the Keplerian line profile model fitted to observed spectral lines to extract stellar mass.
axioms (1)
  • domain assumption Inner disks of FUors are in Keplerian rotation around the central star
    Invoked to justify use of rotational broadening profile for mass inference from line shapes.

pith-pipeline@v0.9.0 · 5534 in / 1293 out tokens · 74055 ms · 2026-05-10T01:06:20.275898+00:00 · methodology

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Reference graph

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