pith. machine review for the scientific record. sign in

arxiv: 2605.03883 · v1 · submitted 2026-05-05 · 🌌 astro-ph.GA

Recognition: unknown

The Keplerian disk, envelope, and streamers surrounding an early O-type protostar in the Sagittarius C cloud of the Central Molecular Zone

Jixiang Weng , Xing Lu , Yu Cheng , Hongping Deng , Xiaofeng Mai , Suinan Zhang , Cara Battersby , Adam Ginsburg
show 17 more authors
Elisabeth A.C. Mills Yichen Zhang Tie Liu Thushara Pillai Xindi Tang Fernando Olguin Hauyu Baobab Liu Qizhou Zhang Shanghuo Li Guang-Xing Li Patricio Sanhueza Yunfan Jiao Qilao Gu Kai Smith Yankun Zhang Tianning Lyu Zhiqiang Shen
Authors on Pith no claims yet

Pith reviewed 2026-05-07 15:06 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Keplerian diskmassive protostaraccretionCentral Molecular ZoneSagittarius CCH3OCHOALMAstar formation
0
0 comments X

The pith

A dynamical model of ALMA data shows a 40 solar mass protostar in Sagittarius C accreting through a 1300 au Keplerian disk and free-falling envelope.

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

Observations of a high-mass protostar in the Sagittarius C cloud of the Central Molecular Zone use ALMA to map molecular emission and reveal surrounding disk and envelope structures. A dynamical model with an inner Keplerian disk and outer free-fall envelope is fitted to the three-dimensional position-position-velocity data from stacked CH3OCHO lines, yielding a central mass of about 40 solar masses. The fit also gives a centrifugal radius of 1300 astronomical units and an envelope-to-disk accretion rate of roughly 7 times 10 to the minus 3 solar masses per year. Spiral features in the disk are interpreted as free-falling streamers that channel additional material inward. These results indicate that disk-mediated accretion operates for early O-type stars even in the extreme conditions of the Galactic Center region.

Core claim

ALMA Band 6 observations at 300 au resolution of an early O-type protostar in Sgr C identify a Keplerian disk, free-falling envelope, and spiral streamers traced by complex organic molecules. Fitting a dynamical model of an inner Keplerian disk plus outer free-fall envelope to the stacked CH3OCHO position-position-velocity data constrains the central protostellar mass to approximately 40+2-3 solar masses, with a centrifugal radius of about 1300 au. The envelope accretion rate onto the disk is estimated at 7 times 10 to the minus 3 solar masses per year from the infall velocity, radius, and mass. The spiral-like structures are described as free-falling streamers. These findings demonstrate a

What carries the argument

Dynamical model consisting of an inner Keplerian disk and outer free-fall envelope, fitted directly to three-dimensional position-position-velocity data of stacked CH3OCHO lines to extract mass and radius parameters.

If this is right

  • The central protostar grows at an accretion rate of approximately 7 times 10 to the minus 3 solar masses per year.
  • The disk reaches a centrifugal radius of 1300 astronomical units before material joins the star.
  • Spiral structures within the disk act as free-falling streamers that deliver extra mass.
  • Disk-mediated accretion enables mass buildup for early O-type stars in the dense Central Molecular Zone.
  • The combination of disk and envelope explains how massive protostars accumulate material despite surrounding turbulence.

Where Pith is reading between the lines

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

  • Disks and streamers may allow massive stars to reach high masses before radiation pressure becomes dominant.
  • Similar kinematic signatures could appear in other dense star-forming regions if observed at comparable resolution.
  • The derived accretion rate implies that episodic bursts or continued infall could push the final stellar mass even higher.
  • This accretion geometry offers a template for testing angular momentum transport in extreme gravitational environments.

Load-bearing premise

The stacked CH3OCHO emission traces a single Keplerian disk plus free-fall envelope without significant contamination from other velocity components or optical depth effects.

What would settle it

Higher-resolution observations that map the velocity field across the disk and show systematic deviations from the model's predicted Keplerian rotation curve or multiple distinct kinematic components inconsistent with a single disk-plus-envelope structure.

Figures

Figures reproduced from arXiv: 2605.03883 by Adam Ginsburg, Cara Battersby, Elisabeth A.C. Mills, Fernando Olguin, Guang-Xing Li, Hauyu Baobab Liu, Hongping Deng, Jixiang Weng, Kai Smith, Patricio Sanhueza, Qilao Gu, Qizhou Zhang, Shanghuo Li, Suinan Zhang, Thushara Pillai, Tianning Lyu, Tie Liu, Xiaofeng Mai, Xindi Tang, Xing Lu, Yankun Zhang, Yichen Zhang, Yu Cheng, Yunfan Jiao, Zhiqiang Shen.

Figure 1
Figure 1. Figure 1: Left: ALMA 1.3 mm continuum intensity map of the Sgr C disk. The black contours indicate intensity levels at [5, 10, 20, 30, 50, and 100]×σ, where the RMS noise σ is 18 µJy beam−1 . The dashed ellipse denotes the region over which the spectra in view at source ↗
Figure 2
Figure 2. Figure 2: Spectral line identification results extracted from the four spectral windows averaged over the inner disk region denoted by the dashed ellipse in view at source ↗
Figure 3
Figure 3. Figure 3: Left: Spatial distribution of the CH3OH rotational temperature within the Sgr C disk. The black contours indicate 1.3 mm continuum emission levels identical to view at source ↗
Figure 4
Figure 4. Figure 4: Normalized intensity maps of the two NMF components, derived from the analysis of 40 molecular lines. The black contours represent the 1.3 mm dust continuum emission as described in view at source ↗
Figure 5
Figure 5. Figure 5: Left: Channel map (color scale) of the stacked CH3OCHO. The LSR velocity in unit of km s−1 of each channel is labeled in each panel. The black contours show the normalized intensities from the best-fit model, with levels at [0.1, 0.3, 0.5, 0.7, 0.9]. The red cross marks the position of the high-mass protostar. Right: Residual map showing the difference between the normalized observed data and the model (Ob… view at source ↗
Figure 6
Figure 6. Figure 6: Intensity maps of stacked CH3OCHO emission overlaid with model trajectories of infalling and rotating particles. The white contours denote the continuum emission as described in view at source ↗
Figure 7
Figure 7. Figure 7: Integrated intensity maps of the 40 molecular lines view at source ↗
Figure 8
Figure 8. Figure 8: NMF contribution of of the molecular lines in the Sgr C disk. an intermediate state between Keplerian rotation (α = 0.5) and rotation with conserved specific angular momentum (α = 1.0) view at source ↗
Figure 9
Figure 9. Figure 9: Corner map of the emcee fitting. 2000 1000 0 1000 2000 Offset (au) 60.0 57.5 55.0 52.5 50.0 47.5 45.0 42.5 V elocity (k m s 1 ) ODR ( = 0.49 ± 0.04), Ms = 42.95 M Theoretical ( = 0.5) Theoretical ( = 1.0) vsys: -51.27 km/s xoff: -110.2 au 2000 1000 0 1000 2000 Offset (au) 60.0 57.5 55.0 52.5 50.0 47.5 45.0 42.5 V elocity (k m s 1 ) ODR ( = 0.81 ± 0.06), Ms = 40.73 M Theoretical ( = 0.5) Theoretical ( = 1.0… view at source ↗
Figure 10
Figure 10. Figure 10: Position-velocity diagram of the stacked CH3OCHO emission extracted along the visually determined major axis (42◦ north-to-west) of the Sgr C disk. The data are fitted using Orthogonal Distance Regression at two different signal-to-noise ratio thresholds. Left: The 16σ threshold isolates the inner high-velocity emission (< 1300 au), yielding a power-law index of α = 0.49 ± 0.04. right: The 9σ threshold in… view at source ↗
read the original abstract

Disk-mediated accretion is central to theories of massive star formation, setting the initial conditions for their evolution. Yet observations of Keplerian disks around early O-type protostars remain scarce, as they are often blended into complex surrounding structures. We report ALMA Band 6 observations (300 au resolution) of an accretion disk surrounding a high-mass protostar in the Sagittarius C (Sgr C) cloud in the Central Molecular Zone (CMZ) around the Galactic Center. We identify spectral lines and analyze the spatial distribution of the emission of the complex organic molecules. We use a dynamical model with an inner Keplerian disk and an outer free-fall envelope to fit the three-dimensional position-position-velocity data of the stacked CH$_3$OCHO molecular lines and constrain the mass of the central protostar to be $\sim40^{+2}_{-3} M_{\odot}$. The fitting results additionally show that the disk has a centrifugal radius at about 1300 au. Considering the infall velocity, radius, and mass of the envelope, we estimate the accretion rate from the envelope onto the disk to be $\sim7\times 10^{-3}\ M_{\odot}\,\mathrm{yr^{-1}}$. We also identify spiral-like structures in the disk that can be described by free-falling streamers. Our results highlight the critical role of accretion disks and streamers in the mass accumulation of early O-type stars in the CMZ.

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 / 2 minor

Summary. The paper reports ALMA Band 6 observations (300 au resolution) of an early O-type protostar in the Sagittarius C cloud of the CMZ. It identifies complex organic molecule emission, fits a dynamical model consisting of an inner Keplerian disk and outer free-fall envelope to the stacked CH3OCHO 3D position-position-velocity data, and derives a central protostellar mass of ~40^{+2}_{-3} M_⊙, a centrifugal radius of ~1300 au, an envelope accretion rate of ~7×10^{-3} M_⊙ yr^{-1}, and spiral-like free-falling streamers.

Significance. If the kinematic model fit is robust, the result supplies one of the few direct mass and radius constraints on a Keplerian disk around an early O-type protostar in the extreme CMZ environment, supporting disk-mediated accretion scenarios for massive star formation. The 3D PPV fitting approach and identification of streamers are strengths that allow falsifiable tests against alternative velocity fields.

major comments (1)
  1. [Dynamical modeling and data fitting] The central mass (~40 M_⊙) and centrifugal radius (~1300 au) rest on the assumption that the stacked CH3OCHO PPV cube traces a single, uncontaminated Keplerian+free-fall velocity field. The manuscript provides no residual maps after model subtraction, per-transition optical-depth estimates, or side-by-side PV diagrams for individual lines to demonstrate that blended components or optical-depth gradients (plausible in the CMZ) do not bias the fit (abstract and dynamical modeling description).
minor comments (2)
  1. [Abstract] The abstract quotes asymmetric uncertainties on the mass but does not state the fitting statistic (e.g., χ², posterior width) or whether the errors include systematic contributions from the stacking procedure.
  2. [Results and discussion] Notation for the centrifugal radius and accretion-rate estimates should explicitly reference the equations or fitting parameters used to derive them from the envelope infall velocity and radius.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We are grateful to the referee for their thorough review and for recognizing the potential significance of our results on the Keplerian disk around an early O-type protostar in the CMZ. We address the major comment on the dynamical modeling below and will incorporate the suggested improvements in the revised manuscript.

read point-by-point responses

  1. Referee: The central mass (~40 M_⊙) and centrifugal radius (~1300 au) rest on the assumption that the stacked CH3OCHO PPV cube traces a single, uncontaminated Keplerian+free-fall velocity field. The manuscript provides no residual maps after model subtraction, per-transition optical-depth estimates, or side-by-side PV diagrams for individual lines to demonstrate that blended components or optical-depth gradients (plausible in the CMZ) do not bias the fit (abstract and dynamical modeling description).

    Authors: We thank the referee for highlighting the need for additional validation of our stacked CH3OCHO 3D PPV fit. The stacking was performed to achieve sufficient signal-to-noise for reliable kinematic modeling, as the individual transitions are relatively weak. We agree that residual maps, optical depth checks, and individual line PV diagrams would help confirm that the fit is not biased by blending or optical depth effects in the dense CMZ environment. In the revised manuscript, we will add: (1) residual maps showing the difference between the observed and modeled PPV cubes, (2) estimates of the optical depths for the CH3OCHO lines included in the stack using the observed brightness temperatures and assuming LTE conditions, and (3) major-axis PV diagrams for the two strongest individual transitions used in the stack, compared directly to the stacked data and model. These additions will allow readers to assess the robustness of the derived protostellar mass of ~40 M_⊙ and centrifugal radius of ~1300 au. We believe this will fully address the concern. revision: yes

Circularity Check

0 steps flagged

No significant circularity: mass and radius derived from direct model fit to independent PPV observations.

full rationale

The paper's core derivation fits a standard two-component dynamical model (inner Keplerian disk + outer free-fall envelope) directly to the stacked CH3OCHO position-position-velocity cube extracted from ALMA observations. The resulting central mass (~40 M⊙) and centrifugal radius (~1300 au) are outputs of this fit to external data, with no reduction to self-defined quantities, renamed fits, or load-bearing self-citations. The derivation chain remains self-contained against the observed line velocities and does not invoke prior author work to force the result.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central mass and centrifugal radius are obtained by fitting a two-component dynamical model whose validity rests on the assumption that CH3OCHO traces Keplerian rotation plus free-fall infall.

free parameters (2)
  • central protostar mass
    Fitted parameter in the dynamical model to match observed velocity field; reported as 40+2-3 M⊙.
  • centrifugal radius
    Derived from the same model fit; reported as ~1300 au.
axioms (1)
  • domain assumption CH3OCHO emission traces the three-dimensional velocity field of a Keplerian disk plus free-fall envelope
    Invoked to justify the dynamical model used for fitting the stacked line data.

pith-pipeline@v0.9.0 · 5664 in / 1407 out tokens · 60792 ms · 2026-05-07T15:06:32.206273+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

110 extracted references · 105 canonical work pages

  1. [1]

    M., Ren, Z.-Y., et al

    New maser species tracing spiral-arm accretion flows in a high-mass young stellar object. Nature Astronomy , year = 2020, month = jan, volume =. doi:10.1038/s41550-020-1144-x , adsurl =

    work page doi:10.1038/s41550-020-1144-x 2020

  2. [2]

    Star Formation from Low to High Mass: A Comparative View

    Star Formation from Low to High Mass: A Comparative View. , keywords =. doi:10.1146/annurev-astro-013125-122023 , archivePrefix =. 2501.16866 , primaryClass =

    work page doi:10.1146/annurev-astro-013125-122023

  3. [3]

    Radiation Hydrodynamics of Self-gravitating Protoplanetary Disks. I. Direct Formation of Gas Giants via Disk Fragmentation , author=. The Astrophysical Journal , volume=. 2025 , publisher=

    2025

  4. [4]

    Digging into the Interior of Hot Cores with ALMA (DIHCA). VII. Disk candidates around high-mass stars and evidence of anisotropic infall. arXiv e-prints , keywords =. doi:10.48550/arXiv.2601.15371 , archivePrefix =. 2601.15371 , primaryClass =

    work page doi:10.48550/arxiv.2601.15371

  5. [5]

    2018, ARA&A, 56, 41, doi: 10.1146/annurev-astro-091916-055235

    High-Mass Star and Massive Cluster Formation in the Milky Way. , keywords =. doi:10.1146/annurev-astro-091916-055235 , archivePrefix =. 1706.00118 , primaryClass =

    work page doi:10.1146/annurev-astro-091916-055235

  6. [6]

    F., & Ostriker, E

    Theory of Star Formation. , keywords =. doi:10.1146/annurev.astro.45.051806.110602 , archivePrefix =. 0707.3514 , primaryClass =

    work page doi:10.1146/annurev.astro.45.051806.110602

  7. [7]

    , keywords =

    Cocoons around early-type stars. , keywords =

  8. [8]

    , keywords =

    Conditions for the Formation of Massive Stars. , keywords =. doi:10.1086/165503 , adsurl =

    work page doi:10.1086/165503

  9. [9]

    Science , keywords =

    The Formation of Massive Star Systems by Accretion. Science , keywords =. doi:10.1126/science.1165857 , archivePrefix =. 0901.3157 , primaryClass =

    work page doi:10.1126/science.1165857

  10. [10]

    A., Heckman, T

    Star formation through gravitational collapse and competitive accretion. , keywords =. doi:10.1111/j.1365-2966.2006.10495.x , archivePrefix =. astro-ph/0604615 , primaryClass =

    work page doi:10.1111/j.1365-2966.2006.10495.x 2006

  11. [11]

    , keywords =

    The Formation of Massive Stars: Accretion, Disks, and the Development of Hypercompact H II Regions. , keywords =. doi:10.1086/520320 , archivePrefix =. astro-ph/0603856 , primaryClass =

    work page doi:10.1086/520320

  12. [12]

    T., & de Wit, W

    Accretion disks in luminous young stellar objects. , keywords =. doi:10.1007/s00159-015-0089-z , archivePrefix =. 1509.08335 , primaryClass =

    work page doi:10.1007/s00159-015-0089-z

  13. [13]

    arXiv e-prints , keywords =

    Disks around O-type young stellar objects. arXiv e-prints , keywords =. doi:10.48550/arXiv.2005.06912 , archivePrefix =. 2005.06912 , primaryClass =

    work page doi:10.48550/arxiv.2005.06912 2005

  14. [14]

    , keywords =

    The ALMA view of W33A: a spiral filament feeding the candidate disc in MM1-Main. , keywords =. doi:10.1093/mnrasl/slx010 , archivePrefix =. 1701.06958 , primaryClass =

    work page doi:10.1093/mnrasl/slx010

  15. [15]

    , keywords =

    An Asymmetric Keplerian Disk Surrounding the O-type Protostar IRAS 16547-4247. , keywords =. doi:10.3847/1538-4357/aafedf , archivePrefix =. 1901.04896 , primaryClass =

    work page doi:10.3847/1538-4357/aafedf 1901

  16. [16]

    ALMA observations of G023.01-00.41

    Discovery of a sub-Keplerian disk with jet around a 20 M _ young star. ALMA observations of G023.01-00.41. , keywords =. doi:10.1051/0004-6361/201833411 , archivePrefix =. 1805.09842 , primaryClass =

    work page doi:10.1051/0004-6361/201833411

  17. [17]

    , keywords =

    Chasing discs around O-type (proto)stars: Evidence from ALMA observations. , keywords =. doi:10.1051/0004-6361/201630184 , adsurl =

    work page doi:10.1051/0004-6361/201630184

  18. [18]

    arXiv , author =:1805.05364 , journal =

    Multidirectional Mass Accretion and Collimated Outflows on Scales of 100-2000 au in Early Stages of High-mass Protostars. , keywords =. doi:10.3847/1538-4357/abc88e , archivePrefix =. 1805.05364 , primaryClass =

    work page doi:10.3847/1538-4357/abc88e 2000

  19. [19]

    , keywords =

    A Keplerian-like Disk around the Forming O-type Star AFGL 4176. , keywords =. doi:10.1088/2041-8205/813/1/L19 , archivePrefix =. 1509.08469 , primaryClass =

    work page doi:10.1088/2041-8205/813/1/l19 2041

  20. [20]

    , keywords =

    G11.92-0.61 MM1: a Keplerian disc around a massive young proto-O star. , keywords =. doi:10.1093/mnras/stw1912 , archivePrefix =. 1608.05561 , primaryClass =

    work page doi:10.1093/mnras/stw1912

  21. [21]

    , keywords =

    Dissecting a hot molecular core: the case of G31.41+0.31. , keywords =. doi:10.1051/0004-6361/201117206 , archivePrefix =. 1107.2849 , primaryClass =

    work page doi:10.1051/0004-6361/201117206

  22. [22]

    Hot ammonia around young O-type stars. I. JVLA imaging of NH _ 3 (6, 6) to (14, 14) in NGC 7538 IRS1. , keywords =. doi:10.1051/0004-6361/201424832 , archivePrefix =. 1410.5448 , primaryClass =

    work page doi:10.1051/0004-6361/201424832

  23. [23]

    , keywords =

    Imaging the disk around IRAS 20126+4104 at subarcsecond resolution. , keywords =. doi:10.1051/0004-6361/201323065 , adsurl =

    work page doi:10.1051/0004-6361/201323065

  24. [24]

    , keywords =

    Dissecting the disk and the jet of a massive (proto)star: An ALMA view of IRAS 20126+4104. , keywords =. doi:10.1051/0004-6361/202452686 , archivePrefix =. 2412.06589 , primaryClass =

    work page doi:10.1051/0004-6361/202452686

  25. [25]

    , keywords =

    G11.92-0.61 MM 1: A Fragmented Keplerian Disk Surrounding a Proto-O Star. , keywords =. doi:10.3847/2041-8213/aaeffc , archivePrefix =. 1811.05267 , primaryClass =

    work page doi:10.3847/2041-8213/aaeffc 2041

  26. [26]

    , keywords =

    CO bandhead emission of massive young stellar objects: determining disc properties. , keywords =. doi:10.1093/mnras/sts537 , archivePrefix =. 1212.0554 , primaryClass =

    work page doi:10.1093/mnras/sts537

  27. [27]

    , keywords =

    The Molecular Accretion Flow in G10.6-0.4. , keywords =. doi:10.1086/432254 , archivePrefix =. astro-ph/0506057 , primaryClass =

    work page doi:10.1086/432254

  28. [28]

    The case of G10.6-0.4

    Interpreting observations of edge-on gravitationally unstable accretion flows. The case of G10.6-0.4. , keywords =. doi:10.1051/0004-6361/201629582 , archivePrefix =. 1609.07296 , primaryClass =

    work page doi:10.1051/0004-6361/201629582

  29. [29]

    Science Advances , keywords =

    Massive extended streamers feed high-mass young stars. Science Advances , keywords =. doi:10.1126/sciadv.adw4512 , archivePrefix =. 2508.15889 , primaryClass =

    work page doi:10.1126/sciadv.adw4512

  30. [30]

    Goldsmith and Neal J

    Xiaofeng Mai and Tie Liu and Xunchuan Liu and Bo Zhang and Paul F. Goldsmith and Neal J. Evans and Qizhou Zhang and Kee-Tae Kim and Dongting Yang and Mika Juvela and Fengwei Xu and Wenyu Jiao and Hongli Liu and Patricio Sanhueza and Guido Garay and Xi Chen and Shengli Qin and Jakobus M. Vorster and Anandmayee Tej and Zhiyuan Ren and Sami Dib and Shanghuo ...

    work page doi:10.1126/sciadv.ady6953 2025

  31. [31]

    arXiv , author =:1911.09692 , journal =

    Spiral arms and instability within the AFGL 4176 mm1 disc. , keywords =. doi:10.1051/0004-6361/201937154 , archivePrefix =. 1911.09692 , primaryClass =

    work page doi:10.1051/0004-6361/201937154 1911

  32. [32]

    3D CMZ. II. Hierarchical Structure Analysis of the Central Molecular Zone. , keywords =. doi:10.3847/1538-4357/adb844 , archivePrefix =. 2410.17332 , primaryClass =

    work page doi:10.3847/1538-4357/adb844

  33. [33]

    arXiv , author =:2201.10438 , journal =

    The sharp ALMA view of infall and outflow in the massive protocluster G31.41+0.31. , keywords =. doi:10.1051/0004-6361/202142703 , archivePrefix =. 2201.10438 , primaryClass =

    work page doi:10.1051/0004-6361/202142703

  34. [34]

    1996, ARA&A, 34, 645, doi: 10.1146/annurev.astro.34.1.645 NANOGrav Collaboration, Arzoumanian, Z., Brazier, A., et al

    The Galactic Center Environment. , year = 1996, month = jan, volume =. doi:10.1146/annurev.astro.34.1.645 , adsurl =

    work page doi:10.1146/annurev.astro.34.1.645 1996

  35. [35]

    D., Barnes, A

    Star Formation in the Central Molecular Zone of the Milky Way. Protostars and Planets VII , year = 2023, editor =. doi:10.48550/arXiv.2203.11223 , archivePrefix =. 2203.11223 , primaryClass =

    work page doi:10.48550/arxiv.2203.11223 2023

  36. [36]

    The Galactic Center Molecular Cloud Survey. I. A steep linewidth-size relation and suppression of star formation. , keywords =. doi:10.1051/0004-6361/201628088 , archivePrefix =. 1610.03499 , primaryClass =

    work page doi:10.1051/0004-6361/201628088

  37. [37]

    , keywords =

    Star formation rates and efficiencies in the Galactic Centre. , keywords =. doi:10.1093/mnras/stx941 , archivePrefix =. 1704.03572 , primaryClass =

    work page doi:10.1093/mnras/stx941

  38. [38]

    , keywords =

    What controls star formation in the central 500 pc of the Galaxy?. , keywords =. doi:10.1093/mnras/stu494 , archivePrefix =. 1303.6286 , primaryClass =

    work page doi:10.1093/mnras/stu494

  39. [39]

    2024, ApJ, 962, 39, doi: 10.3847/1538-4357/ad1395

    Magnetic Fields in the Central Molecular Zone Influenced by Feedback and Weakly Correlated with Star Formation. , keywords =. doi:10.3847/1538-4357/ad1395 , archivePrefix =. 2312.01776 , primaryClass =

    work page doi:10.3847/1538-4357/ad1395

  40. [40]

    2019, ApJ, 872, 171, doi: 10.3847/1538-4357/ab017d

    Star Formation Rates of Massive Molecular Clouds in the Central Molecular Zone. , keywords =. doi:10.3847/1538-4357/ab017d , archivePrefix =. 1901.07779 , primaryClass =

    work page doi:10.3847/1538-4357/ab017d 1901

  41. [41]

    , keywords =

    A Census of Early-phase High-mass Star Formation in the Central Molecular Zone. , keywords =. doi:10.3847/1538-4365/ab4258 , archivePrefix =. 1909.02338 , primaryClass =

    work page doi:10.3847/1538-4365/ab4258 1909

  42. [42]

    , keywords =

    The Cologne Database for Molecular Spectroscopy, CDMS. , keywords =. doi:10.1051/0004-6361:20010367 , adsurl =

    work page doi:10.1051/0004-6361:20010367

  43. [43]

    A geometric distance measurement to the Galactic center black hole with 0.3% uncertainty

    A geometric distance measurement to the Galactic center black hole with 0.3\. , keywords =. doi:10.1051/0004-6361/201935656 , archivePrefix =. 1904.05721 , primaryClass =

    work page doi:10.1051/0004-6361/201935656 1904

  44. [44]

    , keywords =

    Subclustering and Star Formation Efficiency in Three Protoclusters in the Central Molecular Zone. , keywords =. doi:10.3847/2041-8213/adb30b , archivePrefix =. 2503.00878 , primaryClass =

    work page doi:10.3847/2041-8213/adb30b 2041

  45. [45]

    , keywords =

    Spectuner: A Framework for Automated Line Identification of Interstellar Molecules. , keywords =. doi:10.3847/1538-4365/adaeba , archivePrefix =. 2408.06004 , primaryClass =

    work page doi:10.3847/1538-4365/adaeba

  46. [46]

    , year = 1981, month = jan, volume =

    On the emission lines from rotating gaseous disks. , year = 1981, month = jan, volume =

    1981

  47. [47]

    , keywords =

    Dust opacities for protostellar cores. , keywords =

  48. [48]

    , keywords =

    Molecular Depletion and Thermal Balance in Dark Cloud Cores. , keywords =. doi:10.1086/322255 , adsurl =

    work page doi:10.1086/322255

  49. [49]

    F., & Langer, W

    Population Diagram Analysis of Molecular Line Emission. , keywords =. doi:10.1086/307195 , adsurl =

    work page doi:10.1086/307195

  50. [50]

    , keywords =

    Disentangling Multiple Emitting Components in Molecular Observations with Nonnegative Matrix Factorization. , keywords =. doi:10.3847/1538-4357/ad1681 , archivePrefix =. 2312.12646 , primaryClass =

    work page doi:10.3847/1538-4357/ad1681

  51. [51]

    E., J rgensen , J

    Testing grain-surface chemistry in massive hot-core regions. , keywords =. doi:10.1051/0004-6361:20065963 , archivePrefix =. astro-ph/0702066 , primaryClass =

    work page doi:10.1051/0004-6361:20065963

  52. [52]

    1964, ApJ, 139, 1217, doi: 10.1086/147861

    On the gravitational stability of a disk of stars. , year = 1964, month = may, volume =. doi:10.1086/147861 , adsurl =

    work page doi:10.1086/147861 1964

  53. [53]

    , keywords =

    Disk and Envelope Streamers of the GGD 27-MM1 Massive Protostar. , keywords =. doi:10.3847/1538-4357/ace786 , archivePrefix =. 2307.06178 , primaryClass =

    work page doi:10.3847/1538-4357/ace786

  54. [54]

    , keywords =

    The First Bird s-eye View of a Gravitationally Unstable Accretion Disk in High-mass Star Formation. , keywords =. doi:10.3847/2041-8213/ab212f , archivePrefix =. 1905.12983 , primaryClass =

    work page doi:10.3847/2041-8213/ab212f 2041

  55. [55]

    , keywords =

    Gas infall via accretion disk feeding Cepheus A HW2. , keywords =. doi:10.1051/0004-6361/202450330 , archivePrefix =. 2502.15070 , primaryClass =

    work page doi:10.1051/0004-6361/202450330

  56. [56]

    , keywords =

    The Difference in Abundance between N-bearing and O-bearing Species in High-mass Star-forming Regions. , keywords =. doi:10.3847/1538-4365/aac8db , archivePrefix =. 1712.06799 , primaryClass =

    work page doi:10.3847/1538-4365/aac8db

  57. [57]

    , keywords =

    Components of star formation in NGC 253: Non-negative matrix factorization analysis with the ALCHEMI integrated intensity images. , keywords =. doi:10.1093/pasj/psae095 , archivePrefix =. 2411.03867 , primaryClass =

    work page doi:10.1093/pasj/psae095

  58. [58]

    doi:10.1093/mnras/stac219 , eprint =

    ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - VIII. A search for hot cores by using C _ 2 H _ 5 CN, CH _ 3 OCHO, and CH _ 3 OH lines. , keywords =. doi:10.1093/mnras/stac219 , archivePrefix =. 2201.10044 , primaryClass =

    work page doi:10.1093/mnras/stac219

  59. [59]

    The LMT 2 millimeter receiver system (B4R). II. Science demonstration observations toward Orion-KL/OMC-1. , keywords =. doi:10.1093/pasj/psaf105 , archivePrefix =. 2511.21845 , primaryClass =

    work page doi:10.1093/pasj/psaf105

  60. [60]

    , keywords =

    Thermal Feedback in the High-mass Star- and Cluster-forming Region W51. , keywords =. doi:10.3847/1538-4357/aa6bfa , archivePrefix =. 1704.01434 , primaryClass =

    work page doi:10.3847/1538-4357/aa6bfa

  61. [61]

    , keywords =

    Chemical Differentiation around Five Massive Protostars Revealed by ALMA: Carbon-chain Species and Oxygen/Nitrogen-bearing Complex Organic Molecules. , keywords =. doi:10.3847/1538-4365/acd110 , archivePrefix =. 2304.13873 , primaryClass =

    work page doi:10.3847/1538-4365/acd110

  62. [62]

    , keywords =

    Disk Structure around the Class I Protostar L1489 IRS Revealed by ALMA: A Warped-disk System. , keywords =. doi:10.3847/1538-4357/ab8065 , archivePrefix =. 2003.07067 , primaryClass =

    work page doi:10.3847/1538-4357/ab8065 2003

  63. [63]

    , keywords =

    A Keplerian Disk around Orion SrCI, a 15 M _ YSO. , keywords =. doi:10.3847/1538-4357/aac205 , archivePrefix =. 1804.10622 , primaryClass =

    work page doi:10.3847/1538-4357/aac205

  64. [64]

    and Bate, Matthew R

    A triple-star system with a misaligned and warped circumstellar disk shaped by disk tearing. Science , keywords =. doi:10.1126/science.aba4633 , archivePrefix =. 2004.01204 , primaryClass =

    work page doi:10.1126/science.aba4633 2004

  65. [65]

    , keywords =

    Protoplanetary Disks in the Orion Nebula Cluster: Gas-disk Morphologies and Kinematics as Seen with ALMA. , keywords =. doi:10.3847/1538-4357/ab86b7 , archivePrefix =. 2003.12580 , primaryClass =

    work page doi:10.3847/1538-4357/ab86b7 2003

  66. [66]

    , keywords =

    Disks and Outflows in the Intermediate-mass Star-forming Region NGC 2071 IR. , keywords =. doi:10.3847/1538-4357/ac7464 , archivePrefix =. 2205.15108 , primaryClass =

    work page doi:10.3847/1538-4357/ac7464 2071

  67. [67]

    An infall model for the T Tauri phenomenon

    An infall model for the T Tauri phenomenon. , keywords =. doi:10.1086/154840 , adsurl =

    work page doi:10.1086/154840

  68. [68]

    , keywords =

    Substructures in the Keplerian disc around the O-type (proto-)star G17.64+0.16. , keywords =. doi:10.1051/0004-6361/201935633 , archivePrefix =. 1906.06548 , primaryClass =

    work page doi:10.1051/0004-6361/201935633 1906

  69. [69]

    The physical and chemical structure of Sagittarius B2. IV. Converging filaments in the high-mass cluster forming region Sgr B2(N). , keywords =. doi:10.1051/0004-6361/201935200 , archivePrefix =. 1906.10979 , primaryClass =

    work page doi:10.1051/0004-6361/201935200 1906

  70. [70]

    Nature Astronomy , keywords =

    A massive Keplerian protostellar disk with flyby-induced spirals in the Central Molecular Zone. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01681-4 , archivePrefix =. 2206.00202 , primaryClass =

    work page doi:10.1038/s41550-022-01681-4

  71. [71]

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

    emcee: The MCMC Hammer. , keywords =. doi:10.1086/670067 , archivePrefix =. 1202.3665 , primaryClass =

    work page doi:10.1086/670067

  72. [72]

    Nature Physics , keywords =

    Disk-mediated accretion burst in a high-mass young stellar object. Nature Physics , keywords =. doi:10.1038/nphys3942 , archivePrefix =. 1704.02628 , primaryClass =

    work page doi:10.1038/nphys3942

  73. [73]

    , keywords =

    Three-dimensional Simulation of Massive Star Formation in the Disk Accretion Scenario. , keywords =. doi:10.1088/0004-637X/732/1/20 , archivePrefix =. 1102.4090 , primaryClass =

    work page doi:10.1088/0004-637x/732/1/20

  74. [74]

    Search for high-mass protostars with ALMA revealed up to kilo-parsec scales (SPARKS). II. Complex organic molecules and heavy water in shocks around a young high-mass protostar. , keywords =. doi:10.1051/0004-6361/201935226 , adsurl =

    work page doi:10.1051/0004-6361/201935226

  75. [75]

    Nature Astronomy , keywords =

    A Keplerian disk with a four-arm spiral birthing an episodically accreting high-mass protostar. Nature Astronomy , keywords =. doi:10.1038/s41550-023-01899-w , archivePrefix =. 2304.14740 , primaryClass =

    work page doi:10.1038/s41550-023-01899-w

  76. [76]

    Massive Star Formation

    Massive Star Formation. Protostars and Planets VI , year = 2014, editor =. doi:10.2458/azu_uapress_9780816531240-ch007 , archivePrefix =. 1402.0919 , primaryClass =

    work page doi:10.2458/azu_uapress_9780816531240-ch007 2014

  77. [77]

    , keywords =

    Digging into the Interior of Hot Cores with ALMA: Spiral Accretion into the High-mass Protostellar Core G336.01-0.82. , keywords =. doi:10.3847/2041-8213/ad1100 , archivePrefix =. 2311.18006 , primaryClass =

    work page doi:10.3847/2041-8213/ad1100 2041

  78. [78]

    Nature Astronomy , keywords =

    A protostellar system fed by a streamer of 10,500 au length. Nature Astronomy , keywords =. doi:10.1038/s41550-020-1150-z , archivePrefix =. 2007.13430 , primaryClass =

    work page doi:10.1038/s41550-020-1150-z 2007

  79. [79]

    C., Rossi, E

    Analytic solutions to the accretion of a rotating finite cloud towards a central object - I. Newtonian approach. , keywords =. doi:10.1111/j.1365-2966.2008.14210.x , archivePrefix =. 0803.1020 , primaryClass =

    work page doi:10.1111/j.1365-2966.2008.14210.x 2008

  80. [80]

    , keywords =

    Tails of Gravity: Persistence of Star Formation in the Central Molecular Zone. , keywords =. doi:10.3847/1538-4357/ae29e6 , archivePrefix =. 2511.20300 , primaryClass =

    work page doi:10.3847/1538-4357/ae29e6

Showing first 80 references.