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arxiv: 2605.02032 · v1 · submitted 2026-05-03 · 🌌 astro-ph.SR

Recognition: 3 theorem links

Probing the kinematics of FU Orionis objects through high-resolution near-infrared spectroscopy

Ellen Lee, Michael Connelley

Authors on Pith no claims yet

Pith reviewed 2026-05-08 19:24 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords FU Orionis objectsKeplerian line profilesnear-infrared spectroscopyaccretion disk kinematicsCO molecular linesstellar outburstsline profile modeling
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The pith

High-resolution near-infrared spectra reveal double-peaked Keplerian profiles in five FU Orionis objects.

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

FU Orionis objects are young stars thought to accrete material through a steady-state Keplerian disk, which should produce characteristic double-peaked line profiles in their spectra. These profiles are not commonly observed in near-infrared data, prompting questions about the disk structure or additional effects. This study applies a modeling technique to high-resolution spectra of 15 such objects, successfully identifying double-peaked profiles consistent with Keplerian rotation in five cases. The line profiles match between J and K bands for the subsample observed in both, while M-band CO lines appear distinct, pointing to separate physical origins. The findings suggest that blending and absorption from winds or infall often mask the expected signatures.

Core claim

By convolving model cool atmosphere spectra with linear combinations of Gaussians and fitting to iSHELL high-resolution spectra, five of the fifteen targets are shown to have double-peaked line profiles in K-band that can be fitted by a Keplerian line profile. Line profiles in J-band for eight targets correlate with those in K-band, though the linewidth does not show a clear decrease with increasing wavelength. The CO lines observed in M-band are morphologically different from K-band lines, indicating they originate from a different region or mechanism. Double-peaked profiles prove difficult to detect due to blending with molecular features and possible absorption from disk winds or infaling

What carries the argument

Convolution of cool atmosphere model spectra with a linear combination of Gaussians to model and extract the kinematic line profiles from the observed spectra.

Where Pith is reading between the lines

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

  • Time-series application of the same modeling could test whether the detected velocity fields change as the outbursts evolve.
  • The technique may separate disk kinematics from wind contributions in other classes of accreting young stars.
  • Comparison with resolved millimeter maps of the same objects could confirm whether the NIR lines trace the same radial zones.

Load-bearing premise

Deviations from double-peaked Keplerian profiles are primarily due to blending with molecular features, disk winds, or infalling material, and the Gaussian convolution accurately represents the underlying kinematics without other major unmodeled effects.

What would settle it

Obtaining spectra at higher resolution or in additional bands for the same targets that cannot be reproduced by any Keplerian disk model would challenge the claimed kinematics.

Figures

Figures reproduced from arXiv: 2605.02032 by Ellen Lee, Michael Connelley.

Figure 1
Figure 1. Figure 1: Regions of atomic absorption in the K-band spectrum of FU Ori compared to CX Tau, a typical Class II star (iSHELL data for CX Tau are from Flores et al. (2022)). These metal lines are typically useful as they are not impacted by extraneous material outside of the photosphere, unlike CO, but are not clearly identifiable in our FUor spectra. models after they have been weighted by their respective likelihood… view at source ↗
Figure 2
Figure 2. Figure 2: K-band CO lines of FU Ori, V2775 Ori, and a cool atmosphere model spectrum convolved with the instrument profile of iSHELL. The spectrum of FU Ori is multiplied by 1.5 to better view its spectral features. The spectra appear to be similar, but some objects including V2775 Ori show a small amount of 13CO absorption over the model spectra. Prior to fitting each spectrum, we normalize the con￾tinuum by using … view at source ↗
Figure 4
Figure 4. Figure 4: Template spectra with different surface gravities convolved with the best-fit asymmetrical, double-peaked line profile of FU Ori (shown later in view at source ↗
Figure 5
Figure 5. Figure 5: Reduced chi-squared (χ 2 ν) values for each object fitted over a grid of template spectra in K-band, with decreasing χ 2 ν corresponding to brighter colors. The best template spectra are marked with stars. This figure demonstrates that different objects benefit from using different templates. There appears to be some degeneracy between Teff and log g. However, we combine the results of all template spectra… view at source ↗
Figure 6
Figure 6. Figure 6: Posterior distribution for the single Gaussian convolution kernel for FU Ori. This figure was generated using the corner package (Foreman-Mackey 2016). The best-fit line profile is shown in the panel to the right, outlined in green view at source ↗
Figure 7
Figure 7. Figure 7: Sampled posterior distribution for the best-fit double Gaussian convolution kernel for FU Ori. The two gaussian components of the line profile are shown as colored, dotted lines view at source ↗
Figure 8
Figure 8. Figure 8: Sampled posterior distribution for the best-fit triple Gaussian convolution kernel for FU Ori. The three gaussian components of the line profile are shown as colored, dotted lines view at source ↗
Figure 9
Figure 9. Figure 9: Sampled posterior distribution for the best-fit Keplerian convolution kernel for FU Ori view at source ↗
Figure 10
Figure 10. Figure 10: A selected portion of the observed M-band spectra. Colored dashes above the spectra of FU Ori and V1515 Cyg identify different CO lines. Regions of strong telluric contamination are shaded in red. The model spectrum (example shown in gray: Teff = 2800 K, log g = 5.0) are not a good match to the observed data. The profiles of the CO lines appear markedly different from the K-band data. For example, V883 Or… view at source ↗
Figure 11
Figure 11. Figure 11: Line profile fits to the first CO overtone in K-band in order of decreasing linewidth. The line profiles here are described as a linear combination of Gaussians (right column). The observed spectra are shown in gray while the convolved templates are shown as colored lines. The poor fit to PR Ori B is discussed in Sec. 4 view at source ↗
Figure 11
Figure 11. Figure 11: Continued view at source ↗
Figure 12
Figure 12. Figure 12: Same as view at source ↗
Figure 12
Figure 12. Figure 12: Continued view at source ↗
Figure 13
Figure 13. Figure 13: Keplerian line profiles fitted to the objects with double-peaked line profiles. The quality of the fit appears to be similar as for two Gaussians view at source ↗
Figure 14
Figure 14. Figure 14: Same as view at source ↗
Figure 16
Figure 16. Figure 16: K- versus J-band v sin i. The dotted line has a slope of 1. We do not clearly see the wavelength dependence of the linewidth predicted by a basic Keplerian disk model, which predicts that the objects will fall on a line with a slope less than 1. This does not necessarily mean that the accretion disk model is incorrect (see Sec. 5). PR Ori B is excluded from this plot since we could not obtain a good fit t… view at source ↗
Figure 15
Figure 15. Figure 15: Comparison of the J-band (dashed blue) and K-band (pink) line profiles. They appear to be similar to each other save for V733 Cep, which has low SNR data in J-band. 0 10 20 30 40 50 60 70 80 J-band vsini (km/s) 0 10 20 30 40 50 60 70 80 K-b a n d v sini (k m/s) V1515 Cyg V733 Cep V1735 Cyg Parsamian 21 RNO 1b FU Ori V646 Pup V883 Ori view at source ↗
Figure 17
Figure 17. Figure 17: Stacked CO lines in M-band directly fitted with a sum of two Gaussians (dotted lines for the two components and dashed lines for the sum of the two). The lines here appear to be unrelated to what is seen in J- and K-band view at source ↗
Figure 18
Figure 18. Figure 18: Keplerian line profiles with different amounts of turbulent broadening compared to the line profile of RNO 1b. Below a v sin i of 40 km s−1 , it becomes increasingly dif￾ficult to distinguish the two peaks of the Keplerian profile depending on the amount of turbulent broadening. This would not severely degrade our v sin i measure￾ments given that its width is confined to that of the disk model (Carvalho e… view at source ↗
Figure 19
Figure 19. Figure 19: CO lines of RNO 1b (gray) compared to the fitted single-peaked line profile (cyan) and a test model with a stronger blueshifted component of absorption (pink). Al￾though the overall fit of the test model is worse, it is better at reproducing the slightly bowed, triangular shape of the lines (next to the arrows) and steeper slope between each line. 5.2. Comparisons to the expected Keplerian velocity It is … view at source ↗
Figure 20
Figure 20. Figure 20: A comparison of the HWHM measured for symmetrical Keplerian line profiles versus a linear combination of two gaussians for two objects with asymmetrical line profiles. The HWHM measures the rotational velocities fairly consistently despite the asymmetry, contributing approximately 1.5 km s−1 of uncertainty. The line profiles are normalized for visualization (a constant scaling factor does not affect the H… view at source ↗
Figure 22
Figure 22. Figure 22: Distribution of v sin i of the observed FUors (N = 15) compared to Class I (N = 32) and Class II (N = 39) stars measured by Flores et al. (2024). The v sin i for our sample is comparable to those measured for Class I objects. 1. The 15 objects observed at K-band are well￾described by either single- or double-peaked line profiles. The line profiles seem to be stable over baselines of three to four years view at source ↗
Figure 23
Figure 23. Figure 23: Best-fit line profiles for PR Ori B. Our models are a poor fit to the spectra, particularly in K-band where there are narrower CO lines on top of the very highly broadened spectrum. Cutri, R. M., Skrutskie, M. F., van Dyk, S., et al. 2003, VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003), VizieR On-line Data Catalog: II/246. Originally published in: 2003yCat.2246....0C Cutr… view at source ↗
Figure 24
Figure 24. Figure 24: Zoomed in region of the CO bandhead for the models shown in view at source ↗
Figure 24
Figure 24. Figure 24: Continued view at source ↗
read the original abstract

FU Orionis (FUor) objects are thought to be described by a steady-state Keplerian disk. However, the characteristic double-peaked Keplerian line profile is not readily seen in most near-infrared spectra of FUors. In this paper, we measure the near-infrared line profiles of 15 FUors and FUor-like objects by convolving model cool atmosphere spectra with a linear combination of Gaussians. The models are fit to high-resolution spectra obtained with iSHELL on the NASA Infrared Telescope Facility (IRTF). Five of the targets are found to have double-peaked line profiles in K-band, which can also be fitted by a Keplerian line profile. For eight targets that were also observed in J-band, we find that the line profiles are well-correlated to what is observed in K-band, but the linewidth does not clearly appear to decrease with wavelength. We find that a double-peaked line profile can be difficult to see for several reasons, which include blending with extraneous molecular features and potential absorption from a disk wind or infalling material. The CO lines in M-band are morphologically different from their counterparts in K-band, so they are probably of a different origin.

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

3 major / 2 minor

Summary. The paper presents high-resolution near-infrared spectroscopy of 15 FU Orionis and FUor-like objects obtained with iSHELL on the IRTF. Line profiles are extracted by convolving cool-atmosphere model spectra with linear combinations of Gaussians. Five targets exhibit double-peaked K-band profiles that are also fitted by Keplerian models; for the eight targets with J-band data the profiles correlate with K-band but show no clear wavelength-dependent narrowing of linewidth; M-band CO lines are morphologically distinct from K-band counterparts and are attributed to a different origin. The authors discuss blending, disk winds, and infall as reasons why double-peaked Keplerian signatures are often absent.

Significance. If the Gaussian-convolution extraction method is shown to recover true kinematics, the results would supply direct observational support for steady-state Keplerian disks in a subset of FUors and would explain the frequent non-detection of classic double-peaked profiles. The work is grounded in real telescope data and standard model atmospheres, but its impact is limited by the absence of forward-modeling validation and quantitative fit statistics.

major comments (3)
  1. [§3] §3 (line-profile extraction): the convolution of cool-atmosphere templates with an unconstrained linear combination of Gaussians is not validated on synthetic spectra that include a known Keplerian velocity field, inclination, inner/outer radii, and realistic molecular blending. Without such forward-modeling tests it is impossible to determine whether the recovered double-peaked shapes reliably indicate Keplerian rotation or simply absorb non-Keplerian contributions (winds, turbulence, infall) into the Gaussian basis.
  2. [§4.1] §4.1 (K-band results): the statement that five targets yield double-peaked profiles “that can also be fitted by a Keplerian line profile” is presented without reported error bars on the extracted profiles, quantitative goodness-of-fit metrics (χ², residuals), or comparison to alternative kinematic models. This omission makes it difficult to assess the robustness of the Keplerian interpretation.
  3. [§4.2] §4.2 (J- vs. K-band comparison): the reported lack of linewidth decrease between J and K bands is noted but not quantified (e.g., no measured FWHM values or radial-temperature model predictions). This observation appears inconsistent with the radial temperature structure expected for a Keplerian disk, yet no statistical test or alternative kinematic explanation is provided.
minor comments (2)
  1. Figure captions and text should explicitly state the number of Gaussian components used, their allowed width range, and any regularization applied during the fit.
  2. The M-band CO analysis would benefit from a direct overlay or quantitative cross-correlation metric between K- and M-band profiles to support the claim of different origins.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their detailed and constructive review of our manuscript. Their comments highlight important areas for clarification and strengthening, particularly regarding methodological validation and quantitative analysis. We address each major comment below and outline the revisions we will make.

read point-by-point responses

  1. Referee: [§3] §3 (line-profile extraction): the convolution of cool-atmosphere templates with an unconstrained linear combination of Gaussians is not validated on synthetic spectra that include a known Keplerian velocity field, inclination, inner/outer radii, and realistic molecular blending. Without such forward-modeling tests it is impossible to determine whether the recovered double-peaked shapes reliably indicate Keplerian rotation or simply absorb non-Keplerian contributions (winds, turbulence, infall) into the Gaussian basis.

    Authors: We agree that dedicated forward-modeling tests on synthetic spectra with injected Keplerian fields would provide the strongest validation. Our extraction method follows standard practices in high-resolution NIR spectroscopy for recovering line profiles from blended features, allowing the data to determine the shape without presupposing kinematics. The resulting double-peaked profiles in five targets are then compared to Keplerian models. We will add a dedicated paragraph in §3 discussing the method's assumptions, potential absorption of non-Keplerian effects into the Gaussian basis, and the limitations of the approach. If time permits, we will perform limited synthetic tests; otherwise, we will explicitly note the absence of full forward modeling as a caveat. revision: partial

  2. Referee: [§4.1] §4.1 (K-band results): the statement that five targets yield double-peaked profiles “that can also be fitted by a Keplerian line profile” is presented without reported error bars on the extracted profiles, quantitative goodness-of-fit metrics (χ², residuals), or comparison to alternative kinematic models. This omission makes it difficult to assess the robustness of the Keplerian interpretation.

    Authors: We will revise §4.1 to include error bars on all extracted profiles, estimated from the spectral noise and covariance in the Gaussian convolution fit. We will report χ² values, degrees of freedom, and residual statistics for the Keplerian model fits to the five targets. We will also add direct comparisons to alternative models (single Gaussian and simple wind/infall profiles) with their respective χ² values to quantify the improvement provided by the Keplerian interpretation. revision: yes

  3. Referee: [§4.2] §4.2 (J- vs. K-band comparison): the reported lack of linewidth decrease between J and K bands is noted but not quantified (e.g., no measured FWHM values or radial-temperature model predictions). This observation appears inconsistent with the radial temperature structure expected for a Keplerian disk, yet no statistical test or alternative kinematic explanation is provided.

    Authors: We will add measured FWHM values for the J- and K-band profiles of the eight overlapping targets in a new table in §4.2, along with their uncertainties. We will compute expected linewidth trends using a simple radial temperature model for a Keplerian disk (assuming line formation radii based on excitation temperatures). The observed lack of clear narrowing will be discussed in the context of possible line formation at similar radii, blending, or contributions from disk winds. We will include a statistical measure of the J-K correlation and explicitly consider alternative kinematic explanations such as wind-dominated broadening. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational extraction and comparison

full rationale

The paper measures line profiles directly from IRTF/iSHELL spectra by convolving standard cool-atmosphere models with linear combinations of Gaussians, then compares the resulting shapes to Keplerian profiles and notes morphological differences across bands. No derivation step reduces a reported result to its own fitted parameters by construction, no self-citation chain supports a uniqueness claim, and the central findings (double-peaked profiles in five targets, lack of clear wavelength-dependent narrowing) are empirical outcomes from external data rather than tautological re-expressions of the analysis choices. The method is flexible but the paper does not claim the extracted profiles are predictions forced by the fitting procedure itself.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The analysis rests on the assumption that FUors follow steady-state Keplerian disks and that line profiles can be decomposed via convolution with Gaussian velocity distributions; no new entities are introduced.

free parameters (1)
  • Gaussian combination coefficients and widths
    Parameters of the linear combination of Gaussians used to convolve model spectra are adjusted to fit observed line profiles.
axioms (1)
  • domain assumption FU Orionis objects are described by a steady-state Keplerian disk
    Explicitly stated as the baseline expectation whose characteristic double-peaked profile is tested against observations.

pith-pipeline@v0.9.0 · 5507 in / 1421 out tokens · 47480 ms · 2026-05-08T19:24:12.833368+00:00 · methodology

discussion (0)

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Reference graph

Works this paper leans on

85 extracted references · 38 canonical work pages

  1. [1]

    Annual Review of Astronomy and Astrophysics , volume=

    The FU orionis phenomenon , author=. Annual Review of Astronomy and Astrophysics , volume=. 1996 , publisher=

    1996

  2. [2]

    Astrophysical Journal, Part 1 (ISSN 0004-637X), vol

    On the nature of FU Orionis objects , author=. Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 299, Dec. 1, 1985, p. 462-478. Research supported by the Smithsonian Institution. , volume=

    1985

  3. [6]

    Publications of the Astronomical Society of the Pacific , volume=

    iSHELL: a 1--5 micron R= 80,000 Immersion Grating Spectrograph for the NASA Infrared Telescope Facility , author=. Publications of the Astronomical Society of the Pacific , volume=. 2022 , publisher=

    2022

  4. [9]

    VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)

    2003

  5. [11]

    , keywords =

    Molecular Line Emission from Circumstellar Disks. , keywords =. doi:10.1086/172131 , adsurl =

    work page doi:10.1086/172131

  6. [12]

    Publications of the Astronomical Society of the Pacific , volume=

    emcee: the MCMC hammer , author=. Publications of the Astronomical Society of the Pacific , volume=. 2013 , publisher=

    2013

  7. [14]

    VizieR Online Data Catalog: AllWISE Data Release (Cutri+ 2013)

    2013

  8. [15]

    Astronomy & Astrophysics , volume=

    Probing the rotation curve of the outer accretion disk in FU Orionis objects with long-wavelength spectroscopy , author=. Astronomy & Astrophysics , volume=. 2003 , publisher=

    2003

  9. [17]

    Advances in Methods and Practices in Psychological Science , volume=

    A conceptual introduction to Bayesian model averaging , author=. Advances in Methods and Practices in Psychological Science , volume=. 2020 , publisher=

    2020

  10. [19]

    The Astrophysical Journal , volume=

    Measuring the magnetic field of young stars using iSHELL observations: BP Tau and V347 Aur , author=. The Astrophysical Journal , volume=. 2019 , publisher=

    2019

  11. [20]

    Astronomy and Astrophysics , author =

    Photometric and spectroscopic variability of the FUor star V582 Aurigae. , keywords =. doi:10.1051/0004-6361/201321732 , archivePrefix =. 1306.6647 , primaryClass =

    work page doi:10.1051/0004-6361/201321732

  12. [23]

    Clyde, David Draper and EI George, and a rejoinder by the authors , author=

    Bayesian model averaging: a tutorial (with comments by M. Clyde, David Draper and EI George, and a rejoinder by the authors , author=. Statistical science , volume=. 1999 , publisher=

    1999

  13. [24]

    , keywords =

    Near infrared hydrogen lines as diagnostic of accretion and winds in T Tauri stars. , keywords =. doi:10.1051/0004-6361:20000018 , adsurl =

    work page doi:10.1051/0004-6361:20000018

  14. [25]

    Astronomy & Astrophysics , volume=

    Rotational velocities of nearby young stars , author=. Astronomy & Astrophysics , volume=. 2010 , publisher=

    2010

  15. [31]

    Estimating Distance from Parallaxes. IV. Distances to 1.33 Billion Stars in Gaia Data Release 2. , keywords =. doi:10.3847/1538-3881/aacb21 , archivePrefix =. 1804.10121 , primaryClass =

    work page doi:10.3847/1538-3881/aacb21

  16. [34]

    , keywords =

    Ultraviolet Spectroscopy of Pre--Main-Sequence Accretion Disks. , keywords =. doi:10.1086/167860 , adsurl =

    work page doi:10.1086/167860

  17. [37]

    Astronomy & astrophysics , volume=

    The gaia mission , author=. Astronomy & astrophysics , volume=. 2016 , publisher=

    2016

  18. [40]

    and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and

    Virtanen, Pauli and Gommers, Ralf and Oliphant, Travis E. and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and. Nature Methods , year =

  19. [45]

    Structure and Evolution of Close Binary Systems , year = 1976, editor =

    Common Envelope Binaries. Structure and Evolution of Close Binary Systems , year = 1976, editor =

    1976

  20. [47]

    Zenodo , year=

    csalyk/spectools\_ir: First release , author=. Zenodo , year=

  21. [52]

    The Astrophysical Journal , volume=

    Trigonometric parallaxes of high mass star forming regions: the structure and kinematics of the Milky Way , author=. The Astrophysical Journal , volume=. 2014 , publisher=

    2014

  22. [53]

    The Astronomical Journal , volume=

    Evolution of the Fu Orionis Object BBW 76 , author=. The Astronomical Journal , volume=

  23. [54]

    International Astronomical Union Colloquium , volume=

    A Wide Latitiude CO Survey of Molecular Clouds in the Northern Milky Way , author=. International Astronomical Union Colloquium , volume=. 1984 , organization=

    1984

  24. [55]

    The Gould’s Belt Distances Survey (GOBELINS). II. Distances and structure toward the Orion molecular clouds , author=. The Astrophysical Journal , volume=. 2017 , publisher=

    2017

  25. [56]

    Monthly Notices of the Royal Astronomical Society , volume=

    The star formation environment of the FU Ori type star V582 Aur , author=. Monthly Notices of the Royal Astronomical Society , volume=. 2017 , publisher=

    2017

  26. [57]

    The Astronomer's Telegram , keywords =

    The FUor outburst of PR Ori B. The Astronomer's Telegram , keywords =

  27. [58]

    Astrophysical Journal, Part 2-Letters (ISSN 0004-637X), vol

    The inner-disk and stellar properties of the young stellar object WL 16 , author=. Astrophysical Journal, Part 2-Letters (ISSN 0004-637X), vol. 411, no. 1, p. L37-L40. , volume=

  28. [59]

    Astronomy & Astrophysics , volume=

    The disk of FU Orionis viewed with MATISSE/VLTI-First interferometric observations in L and M bands , author=. Astronomy & Astrophysics , volume=. 2022 , publisher=

    2022

  29. [61]

    Using Accretion and Stellar Rotation to Reveal the Star--Disk Connection in T Tauri Stars , author=

    The ODYSSEUS Survey. Using Accretion and Stellar Rotation to Reveal the Star--Disk Connection in T Tauri Stars , author=. The Astrophysical Journal , volume=. 2025 , publisher=

    2025

  30. [62]

    The Astrophysical Journal , volume=

    High-resolution spectroscopy of FU Orionis stars , author=. The Astrophysical Journal , volume=

  31. [63]

    Allard , F., Homeier , D., Freytag , B., Schaffenberger , W., & Rajpurohit , A. S. 2013, Memorie della Societa Astronomica Italiana Supplementi, 24, 128, 10.48550/arXiv.1302.6559

    work page Pith review doi:10.48550/arxiv.1302.6559 2013

  32. [64]

    S., Tokunaga, A

    Carr, J. S., Tokunaga, A. T., Najita, J., Shu, F. H., & Glassgold, A. E. 1993, Astrophysical Journal, Part 2-Letters (ISSN 0004-637X), vol. 411, no. 1, p. L37-L40., 411, L37

    1993

  33. [65]

    , keywords =

    Carvalho , A., Hillenbrand , L., & Seebeck , J. 2023, , 958, 140, 10.3847/1538-4357/acff59

    work page doi:10.3847/1538-4357/acff59 2023

  34. [66]

    , keywords =

    Carvalho , A., Hillenbrand , L., Seebeck , J., & Covey , K. 2024, , 971, 44, 10.3847/1538-4357/ad5286

    work page doi:10.3847/1538-4357/ad5286 2024

  35. [67]

    , keywords =

    Carvalho , A. S., Hillenbrand , L. A., & K \'o sp \'a l , \'A . 2025, , 993, 38, 10.3847/1538-4357/ae0646

    work page doi:10.3847/1538-4357/ae0646 2025

  36. [68]

    A., Casassus, S., Tobin, J., et al

    Cieza , L. A., Casassus , S., Tobin , J., et al. 2016, , 535, 258, 10.1038/nature18612

    work page doi:10.1038/nature18612 2016

  37. [69]

    , author =

    Connelley , M. S., & Reipurth , B. 2018, , 861, 145, 10.3847/1538-4357/aaba7b

    work page doi:10.3847/1538-4357/aaba7b 2018

  38. [70]

    C., Vacca, W

    Cushing , M. C., Vacca , W. D., & Rayner , J. T. 2004, , 116, 362, 10.1086/382907

    work page doi:10.1086/382907 2004

  39. [71]

    M., Skrutskie , M

    Cutri , R. M., Skrutskie , M. F., van Dyk , S., et al. 2003, VizieR Online Data Catalog: 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003) , VizieR On-line Data Catalog: II/246. Originally published in: 2003yCat.2246....0C

    2003

  40. [72]

    M., Wright , E

    Cutri , R. M., Wright , E. L., Conrow , T., et al. 2021, VizieR Online Data Catalog: AllWISE Data Release (Cutri+ 2013) , VizieR On-line Data Catalog: II/328. Originally published in: IPAC/Caltech (2013)

    2021

  41. [73]

    1984, in International Astronomical Union Colloquium, Vol

    Dame, T., & Thaddeus, P. 1984, in International Astronomical Union Colloquium, Vol. 81, Cambridge University Press, 235--238

    1984

  42. [74]

    S., Reipurth, B., & Boogert, A

    Flores, C., Connelley, M. S., Reipurth, B., & Boogert, A. 2019, The Astrophysical Journal, 882, 75

    2019

  43. [75]

    , keywords =

    Flores , C., Connelley , M. S., Reipurth , B., Boogert , A., & Doppmann , G. 2024, , 972, 149, 10.3847/1538-4357/ad58b1

    work page doi:10.3847/1538-4357/ad58b1 2024

  44. [76]

    S., Reipurth, B., & Duchˆ ene, G

    Flores , C., Connelley , M. S., Reipurth , B., & Duch \^e ne , G. 2022, , 925, 21, 10.3847/1538-4357/ac37bd

    work page doi:10.3847/1538-4357/ac37bd 2022

  45. [77]

    2016 , month =

    Foreman-Mackey, D. 2016, The Journal of Open Source Software, 1, 24, 10.21105/joss.00024

    work page doi:10.21105/joss.00024 2016

  46. [78]

    W., Lang, D., & Goodman, J

    Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, Publications of the Astronomical Society of the Pacific, 125, 306

    2013

  47. [79]

    E., Rothman , L

    Gordon , I. E., Rothman , L. S., Hargreaves , R. J., et al. 2026, , 353, 109807, 10.1016/j.jqsrt.2026.109807

    work page doi:10.1016/j.jqsrt.2026.109807 2026

  48. [80]

    P., Aspin , C., & Reipurth , B

    Greene , T. P., Aspin , C., & Reipurth , B. 2008, , 135, 1421, 10.1088/0004-6256/135/4/1421

    work page doi:10.1088/0004-6256/135/4/1421 2008

  49. [81]

    2004, , 609, 906, 10.1086/421317

    Hartmann , L., Hinkle , K., & Calvet , N. 2004, , 609, 906, 10.1086/421317

    work page doi:10.1086/421317 2004

  50. [82]

    1985, Astrophysical Journal, Part 1 (ISSN 0004-637X), vol

    Hartmann, L., & Kenyon, S. 1985, Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 299, Dec. 1, 1985, p. 462-478. Research supported by the Smithsonian Institution., 299, 462

    1985

  51. [83]

    Hartmann, L., & Kenyon, S. J. 1996, Annual Review of Astronomy and Astrophysics, 34, 207

    1996

  52. [84]

    2003, The Astrophysical Journal, 595, 384

    Herbig, G., Petrov, P., & Duemmler, R. 2003, The Astrophysical Journal, 595, 384

    2003

  53. [85]

    Herbig , G. H. 1966, Vistas in Astronomy, 8, 109, 10.1016/0083-6656(66)90025-0

    work page doi:10.1016/0083-6656(66)90025-0 1966

  54. [86]

    , keywords =

    ---. 1977, , 217, 693, 10.1086/155615

    work page doi:10.1086/155615 1977

  55. [87]

    , author =

    Herbig , G. H., Petrov , P. P., & Duemmler , R. 2003, , 595, 384, 10.1086/377194

    work page doi:10.1086/377194 2003

  56. [88]

    , keywords =

    Herczeg , G. J., & Reipurth , B. 2025, , 994, L43, 10.3847/2041-8213/ae1caf

    work page doi:10.3847/2041-8213/ae1caf 2025

  57. [89]

    F., van den Bergh, D., & Wagenmakers, E.-J

    Hinne, M., Gronau, Q. F., van den Bergh, D., & Wagenmakers, E.-J. 2020, Advances in Methods and Practices in Psychological Science, 3, 200

    2020

  58. [90]

    A., Madigan, D., Raftery, A

    Hoeting, J. A., Madigan, D., Raftery, A. E., & Volinsky, C. T. 1999, Statistical science, 14, 382

    1999

  59. [91]

    , keywords =

    Kenyon , S. J., Hartmann , L., & Hewett , R. 1988, , 325, 231, 10.1086/165999

    work page doi:10.1086/165999 1988

  60. [92]

    N., Kolotilov, E

    Kopatskaya, E. N., Kolotilov, E. A., & Arkharov, A. A. 2013, Monthly Notices of the Royal Astronomical Society, 434, 38, 10.1093/mnras/stt963

    work page doi:10.1093/mnras/stt963 2013

  61. [93]

    2017, The Astrophysical Journal, 834, 142

    Kounkel, M., Hartmann, L., Loinard, L., et al. 2017, The Astrophysical Journal, 834, 142

    2017

  62. [94]

    A., Hillenbrand L

    Kuhn , M. A., & Hillenbrand , L. A. 2019, , 883, 117, 10.3847/1538-4357/ab3a3f

    work page doi:10.3847/1538-4357/ab3a3f 2019

  63. [95]

    2017, Monthly Notices of the Royal Astronomical Society, 468, 2325

    Kun, M., Szegedi-Elek, E., & Reipurth, B. 2017, Monthly Notices of the Royal Astronomical Society, 468, 2325

    2017

  64. [96]

    2003, Astronomy & Astrophysics, 408, 1015

    Lodato, G., & Bertin, G. 2003, Astronomy & Astrophysics, 408, 1015

    2003

  65. [97]

    2022, Astronomy & Astrophysics, 663, A86

    Lykou, F., \'A brah \'a m, P., Chen, L., et al. 2022, Astronomy & Astrophysics, 663, A86

    2022

  66. [98]

    2005, , 437, 627, 10.1051/0004-6361:20042556

    Malbet , F., Lachaume , R., Berger , J.-P., et al. 2005, , 437, 627, 10.1051/0004-6361:20042556

    work page doi:10.1051/0004-6361:20042556 2005

  67. [99]

    The VizieR database of astronomical catalogues , publisher =

    Ochsenbein, F. 1996, The VizieR database of astronomical catalogues, CDS, Centre de Données astronomiques de Strasbourg, 10.26093/CDS/VIZIER

    work page doi:10.26093/cds/vizier 1996

  68. [100]

    Astronomy and Astrophysics Supplement Series , author =

    Ochsenbein , F., Bauer , P., & Marcout , J. 2000, , 143, 23, 10.1051/aas:2000169

    work page doi:10.1051/aas:2000169 2000

  69. [101]

    1976, in IAU Symposium, Vol

    Paczynski , B. 1976, in IAU Symposium, Vol. 73, Structure and Evolution of Close Binary Systems, ed. P. Eggleton , S. Mitton , & J. Whelan , 75

    1976

  70. [102]

    , author =

    Park , S., Lee , J.-E., Pyo , T.-S., et al. 2020, , 900, 36, 10.3847/1538-4357/aba532

    work page doi:10.3847/1538-4357/aba532 2020

  71. [103]

    C., Herczeg , G., Lee , J.-E., et al

    Pena , C. C., Herczeg , G., Lee , J.-E., et al. 2024, The Astronomer's Telegram, 16776, 1

    2024

  72. [104]

    , keywords =

    P \'e rez , S., Hales , A., Liu , H. B., et al. 2020, , 889, 59, 10.3847/1538-4357/ab5c1b

    work page doi:10.3847/1538-4357/ab5c1b 2020

  73. [105]

    , keywords =

    Petrov , P. P., & Herbig , G. H. 2008, , 136, 676, 10.1088/0004-6256/136/2/676

    work page doi:10.1088/0004-6256/136/2/676 2008

  74. [106]

    V., Espaillat, C

    Pittman, C. V., Espaillat, C. C., Zhu, Z., et al. 2025, The Astrophysical Journal, 993, 181

    2025

  75. [107]

    2022, Publications of the Astronomical Society of the Pacific, 134, 015002

    Rayner, J., Tokunaga, A., Jaffe, D., et al. 2022, Publications of the Astronomical Society of the Pacific, 134, 015002

    2022

  76. [108]

    J., Menten, K

    Reid, M. J., Menten, K. M., Brunthaler, A., et al. 2014, The Astrophysical Journal, 783, 130

    2014

  77. [109]

    J., Smette, A., & Bouchet, P

    Reipurth, B., Hartmann, L., Kenyon, S. J., Smette, A., & Bouchet, P. 2002, The Astronomical Journal, 124, 2194

    2002

  78. [110]

    H., Bally , J., et al

    Reipurth , B., Herbig , G. H., Bally , J., et al. 2018, , 156, 25, 10.3847/1538-3881/aac020

    work page doi:10.3847/1538-3881/aac020 2018

  79. [111]

    2022, Zenodo

    Salyk, C. 2022, Zenodo

    2022

  80. [112]

    , keywords =

    Szab \'o , Z. M., K \'o sp \'a l , \'A ., \'A brah \'a m , P., et al. 2021, , 917, 80, 10.3847/1538-4357/ac04b3

    work page doi:10.3847/1538-4357/ac04b3 2021

Showing first 80 references.