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Dust Seeding Molecules in a Massive Protostar -- Detection of TiO in Orion Source I

T0 review · 3 major / 5 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read First detection of TiO in a star-forming region positions titanium monoxide as a tracer of refractory dust destruction at the base of a massive protostar's outflow.

desk verdict Genuine first detection of TiO in a star-forming region; the LTE abundance ratio is the soft underbelly, but the detection itself stands. read the letter →

arxiv 2608.01505 v1 pith:VU7MFZO7 submitted 2026-08-02 astro-ph.GA astro-ph.SR

Ziwei E. Zhang , Nami Sakai , Marcelino Agundez , Linda Podio , Claudio Codella , Tomoya Hirota , Adam Ginsburg , Brett McGuire
show 11 more authors
Nadia M. Murillo Yuki Okoda Yoko Oya Giovanni Sabatini Aki Takigawa Kei E. I. Tanaka Yichen Zhang Qiuyi Luo Yu Cheng Izaskun Jimenez-Serra Shogo Tachibana
This is my paper · ORCID
classification astro-ph.GAastro-ph.SR
keywords astrochemistryTiOrefractorymoleculesdustseedingmassiveprotostarsOrionSourceIALMAprotostellaroutflow
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper reports the first detection of TiO in a star-forming region, based on ALMA observations of Orion Source I, a massive protostar about 415 pc away. Six TiO rotational transitions are identified; the three unblended ones show compact emission within roughly 50–100 au, double-peaked line profiles, and a velocity gradient consistent with a rotating outflow launched at the disk center. Under LTE and optically thin assumptions, the TiO column density is derived as $(3.0 \pm 0.4)\times10^{15}$ cm$^{-2}$, giving a TiO/SiO ratio of $(12.8 \pm 1.7)\times10^{-3}$, higher than the Ti/Si ratio in CI chondrites. The paper also presents a tentative AlOH detection with a more extended, disk-surface distribution. The result matters because TiO is a key dust-seeding molecule: its presence near the protostar indicates where refractory dust is vaporized and where minerals like perovskite may re-condense, linking protostellar chemistry to the earliest Solar System solids.

What carries the argument

The central carrier is the rotational spectrum of TiO, observed in six transitions (three unblended: $J=11\!-\!10$ at 348 GHz, $J=21\!-\!20$ at 664 GHz, and $J=27\!-\!26$ at 853 GHz) with ALMA beams of $0.09''$ to $0.38''$. The identification is carried by joint spectral, spatial, and kinematic constraints: each line must appear at the expected rest frequency, originate from the same compact region, show a consistent velocity gradient, and match the morphology of chemically related AlO. Position–velocity diagrams fitted with a Keplerian rotation model place the emission at the base of a rotating outflow and give a central mass near $10\ M_\odot$. The LTE excitation analysis of the two least

What would settle it

Observe the three blended TiO transitions (355, 485, and 646 GHz) at higher spectral resolution and signal-to-noise and check whether their red-shifted components recover the same double-peaked Keplerian pattern as the 348, 664, and 853 GHz lines; simultaneously measure SiO at the same angular resolution as TiO. If the blended features break up into unrelated lines, or the re-measured TiO/SiO ratio drops below the CI-chondrite ratio, the identification or the inferred dust-to-gas conversion is refuted.

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Extended reading notes

Core claim

The paper establishes the first detection of TiO in a star-forming region and, with it, a direct measurement of refractory titanium chemistry at the base of a massive protostellar outflow. Six TiO rotational transitions are identified in ALMA Bands 7–10; the three unblended lines show compact, double-peaked emission and position–velocity structure consistent with a rotating outflow within about 50–100 au of the central object, closely matching the spatial and kinematic signature of AlO. An LTE excitation analysis of the two least blended transitions yields a rotation temperature of $(484.3 \pm 73.0)$ K and a column density of $(3.0 \pm 0.4)\times10^{15}$ cm$^{-2}$. Combined with the previous

Load-bearing premise

The central claim would collapse if the six candidate TiO features, most of them blended, are not real TiO emission, or if the hot, irradiated gas at the outflow base is far from LTE and optically thin so that the derived column density is not trustworthy.

Editorial extensions

If this is right

  • TiO is present and concentrated at the outflow base of Orion Source I, making it a probe of the hottest inner gas where refractory dust is destroyed.
  • The TiO/SiO ratio in Source I exceeds the CI-chondrite Ti/Si ratio, indicating that Ti- and Si-rich dust is efficiently converted to gas near the protostar.
  • TiO kinematics trace the same rotating outflow as Si$^{18}$O and AlO, reinforcing the picture that refractory molecules mark the outflow-launching region rather than the disk.
  • The tentative AlOH detection suggests that AlO + H$_2$/H$_2$O chemistry operates on the disk surface, with AlOH tracing cooler, more extended gas than AlO or TiO.
  • These detections provide observational constraints for condensation and sublimation models of refractory minerals such as corundum and perovskite in protostellar environments, linking them to CAI-like material formation.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If TiO is confirmed in other protostars, it could serve as a generic sublimation-front tracer: one testable prediction is that TiO emission should be sharply bounded at the dust-destruction radius and reappear only where gas is heated above roughly 1400–1500 K.
  • The CI-chondrite comparison rests on a SiO column density measured with a much larger beam; measuring SiO at the same angular resolution as TiO could either strengthen or weaken the claimed efficient dust-to-gas conversion.
  • Higher-resolution observations of the three blended TiO transitions could distinguish real TiO from contaminating species, providing a clean test of whether the multi-line identification holds.
  • A multi-line search for AlOH would test whether its extended, disk-surface distribution is genuine chemistry or a blending artifact, and could discriminate between the proposed AlO + H$_2$ and AlO + H$_2$O formation routes.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 5 minor

Summary. The paper reports the first detection of the refractory molecule TiO in a star-forming region, toward the massive protostar Orion Source I, using archival and new ALMA data in Bands 7–10. Six TiO rotational transitions are identified, of which three (348, 664, and 853 GHz) are described as unblended; the emission is spatially compact (within roughly 50–100 au) and shows PV structure consistent with the base of a rotating outflow, similar to previously detected AlO. Under LTE and optically thin assumptions, a rotation temperature of 484.3 ± 73.0 K and a TiO column density of (3.0 ± 0.4) × 10^15 cm^-2 are derived from two (or, per a later sentence, three) of these transitions. Using a literature SiO column density from a 61-arcsec beam, the authors obtain X_TiO/SiO ≈ (12.8 ± 1.7) × 10^-3, which they note is an upper limit, and compare this with CI-chondrite Ti/Si. A single AlOH line is also tentatively detected and appears more extended than TiO/AlO.

Significance. If the identification holds, this is a valuable and genuinely new result: TiO is a key dust-seeding molecule in AGB star chemistry, and its detection at the outflow-launching region of a massive protostar would extend dust-nucleation studies into star-forming environments. The paper's main strengths are the three unblended transitions spanning a wide frequency range (348–854 GHz), the high signal-to-noise spatially resolved images, and the internal consistency of the spectra, PV diagrams, and morphology with the known source structure. These make a chance spectral coincidence unlikely for the detection itself. The tentative AlOH detection, while single-line, is clearly labeled as tentative and is a reasonable starting point for future work. The quantitative conclusions on the TiO/SiO ratio and dust-to-gas conversion are more fragile, however, because they rely on a two-line LTE excitation analysis and on an SiO column density measured in a much larger beam. With appropriate revision of those quantitative claims, the paper would be an important addition to the refractory astrochemistry of protostars.

major comments (3)
  1. [Section 3.3] The LTE excitation analysis is load-bearing for the column density and abundance claims, but the description is internally inconsistent. The text says the column density is derived from 'the two least blended transitions at 348 and 664 GHz,' while Table 1 and Figure 1 list the 853 GHz line as unblended and the final paragraph of Section 3.3 refers to 'only three transitions are applied.' Please state exactly which transitions are used. If only two lines are used, the rotation temperature and column density are determined with zero degrees of freedom, and there is no way to validate the LTE assumption; if three lines are used, show the rotation diagram and residuals. In either case, the quoted 1-sigma uncertainty of 0.4 × 10^15 cm^-2 reflects only the statistical fit and cannot capture systematic errors from non-LTE excitation, which the text itself concedes is likely at the outflow base.
  2. [Section 3.3 and Abstract] The abundance ratio X_TiO/SiO = (12.8 ± 1.7) × 10^-3 uses N(SiO) = 2.35 × 10^17 cm^-2 from Ziurys & Friberg (1987), a 61-arcsec single-dish measurement, while N(TiO) is measured within a ~100 au region of the ALMA data. The paper notes that this makes the ratio an upper limit, but the abstract and the 'higher than CI chondrites' phrasing present the ratio as a direct comparison. Since the local SiO column density in the compact outflow base could be substantially larger than the 61-arcsec beam average, the CI-chondrite comparison and the 'efficient dust-to-gas conversion' conclusion are not yet supported at the stated precision. Please reframe the abstract and Section 3.3 to present the ratio strictly as a beam-mismatched upper limit, or add a same-resolution SiO measurement from the same ALMA data, which appears feasible in these datasets.
  3. [Section 3.1 and Appendix B] The paper claims 'six rotational transitions are identified,' but three of them are blended with other species (KCl, iCOMs, SiS, SO2) and the appendix discussion is qualitative: the blended transitions are identified primarily by eye in PV diagrams and by expected velocity offsets. Since the detection claim itself does not require all six lines—the three unblended transitions at 348, 664, and 853 GHz already provide strong support—I suggest either downweighting the language about six identifications or providing quantitative fits/deblending for the blended transitions. As written, the 'six transitions' statement overstates the evidence and invites the criticism that the identification is partly based on contaminated features.
minor comments (5)
  1. [Section 3.3 and Figure 3] The rotation temperature is quoted as 484.3 ± 73.0 K in the text, but Figure 3's caption says 483.3 K. Please harmonize.
  2. [Section 3.2] There are typos in the text: 'tentatlively,' 'adn,' 'emisison,' and 'AlOH is could be extended than TiO.' Please proofread.
  3. [Table 1] The 323313.48 and 474687.81 MHz TiO transitions are listed with no intensity or detection status. Please explicitly mark them as 'not detected' (or 'not observed') rather than leaving dots, to avoid ambiguity.
  4. [References] The reference 'Hirota, T., et al. in prep.' is not fully citable. If it is needed for the Band 10 data reduction, provide a more specific citation or describe the data in the text.
  5. [Abstract] The notation 'X_TiO/SiO ∼ 12.8 ± 1.7 ×10^-3' should be parenthesized as (12.8 ± 1.7) × 10^-3, and the abstract should explicitly state that this is an upper limit given the beam mismatch noted in Section 3.3.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the TiO detection and LTE column density rest on measured intensities and independent literature references.

full rationale

The derivation chain is straightforward: observation -> line identification -> LTE excitation analysis -> abundance ratio. Line identification uses four independent criteria (rest frequency, compact region, velocity gradient, chemical consistency), none of which defines TiO in terms of the claimed detection. The three unblended lines (348, 664, 853 GHz) are detected at high S/N, and the blended lines are presented as supporting rather than load-bearing. The LTE column density is a fit to the two cleanest line intensities, not a prediction of those intensities from an assumed abundance, so no fitted quantity is renamed as a prediction. The X_TiO/SiO ratio is obtained by combining the measured TiO column density with an independent SiO column density from Ziurys & Friberg (1987), and the paper explicitly calls the result an upper limit, so the comparison is not forced. Citations to previous source characterizations (Hirota et al. 2017; Tachibana et al. 2019; Oya et al. 2022) provide empirical context; although several authors overlap, the cited results are observational, not a uniqueness argument or ansatz. The AlO consistency check is an internal cross-check, not an input-output tautology. Overall, no equation reduces to its own input; at most there is a minor non-load-bearing self-citation.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

No new physical entities are introduced. The free parameters are the rotation temperature, the rotation model radii and mass, and the adopted SiO column density. The main assumptions are LTE and optically thin emission, the comparison SiO column density, CDMS molecular data, and the identification criteria for blended lines.

free parameters (4)
  • Rotation temperature T_rot = 484.3 +/- 73.0 K
    Fitted from the two least blended TiO transitions (348 and 664 GHz) under LTE, and used to convert line intensities into a TiO column density. The fit is made to the same data that the column density is derived from.
  • Keplerian model parameters for TiO = outer radius ~50 au, inner radius ~25 au, central mass ~10 solar masses
    Rotation model parameters chosen to fit the PV diagrams of the TiO emission, used to argue that TiO traces the outflow base.
  • Keplerian model parameters for AlOH = outer radius ~65 au, inner radius ~50 au, central mass ~10 solar masses
    Rotation model parameters fit to the tentative AlOH PV diagram.
  • SiO column density for abundance ratio = 2.35 x 10^17 cm^-2
    Adopted from the Ziurys and Friberg 1987 observation with a 61 arcsec beam; this value directly sets the X_TiO/SiO ratio, and the mismatch in beam size makes the ratio an upper limit.
assumptions (5)
  • domain assumption The detected lines are optically thin and LTE holds for TiO excitation in the outflow base.
    Section 3.3: the column density is derived assuming LTE and optically thin emission, and the text concedes the outflow base may drive the gas out of LTE.
  • domain assumption The SiO column density from a 61 arcsecond beam (Ziurys and Friberg 1987) can be meaningfully compared with the compact TiO emission.
    Section 3.3: the X_TiO/SiO ratio uses a single literature SiO column density, acknowledged to be an upper limit because the central SiO abundance could be higher and other Si species exist.
  • standard math Molecular line data from CDMS are correct for TiO and AlOH transitions.
    Table 1 uses CDMS catalog line frequencies, Einstein A values, and upper state energies.
  • domain assumption The spatial and kinematic consistency of the blended transitions with AlO and the rotation model confirms their identification as TiO.
    Section 3 detection criteria include cross-checks against chemically related species and kinematics, which is sensible but increases the risk of confirmation bias in line identification.
  • domain assumption Orion Source I distance is 415 pc for converting angular offsets to au.
    Section 3 uses 100 au = 0.24 arcsec at 415 pc, citing Menten et al. 2007 and Kounkel et al. 2018.

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Cite this review

Pith. "Pith review of Dust Seeding Molecules in a Massive Protostar -- Detection of TiO in Orion Source I." pith.science (2026). https://pith.science/paper/VU7MFZO7

@misc{pith2026260801505,
  author       = {Pith},
  title        = {Pith review of: Dust Seeding Molecules in a Massive Protostar -- Detection of TiO in Orion Source I},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/VU7MFZO7}},
  note         = {Machine review of arXiv:2608.01505}
}
abstract

We report the first detection of TiO in star-forming regions based on Atacama Large Millimeter/submillimeter Array observations of Orion Source I, a well-characterized massive protostar. Multiple rotational transitions are identified, with emission spatially resolved within $\sim 50$ au, showing a compact distribution with a velocity structure consistent with the base of a rotating outflow. The spatial and velocity distributions of TiO are consistent with those of AlO, with both species being key dust seeding refractory molecules. \textbf{The column density of TiO is derived to be $(3.0 \pm 0.4)\times10^{15}\ {\rm cm^{-2}}$, corresponding to $X_{\rm TiO/SiO} \sim 12.8 \pm 1.7 \times10^{-3}$, higher than CI chondrites and indicative of efficient dust-to-gas conversion near the protostar.} We also identify a tentative detection of AlOH, which exhibits a more extended distribution along the disk surface, possibly indicating different conditions from those traced by TiO and AlO. The detection of TiO, a key dust seeding species, offers important constraints on refractory chemistry and the formation environments of primitive minerals, linking astrochemical processes in protostellar systems to the earliest stages of Solar System material formation.

Figures

Figures reproduced from arXiv: 2608.01505 by the authors.

Figure 1
Figure 1. Left: Mean spectra of detected TiO transitions within 100 au from the continuum center. These mean spectra include both velocity peaks seen in the PV diagrams. The Gaussian fits of the two velocity components and the overall profile are indicated with the dashed and solid lines, respectively. The peak velocity offsets (Vpeak) are marked with light green dash-dot lines. Vpeak is the velocity of the measured symmetric… view at source ↗
Figure 2
Figure 2. Tentatively detected AlOH J=21-20 transition (fine structure) at 660 GHz. The spectrum is fitted with the same procedure as TiO (see [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Relative TiO line intensities as a function of fre￾quency from LTE calculations at 483.3 K (Section 3.3). The intensities are normalized to the TiO 853 GHz transition. The transitions presented in this work are marked in red. The Ω = 3 transitions, although blended, have intensities ∼ 20% − 50% of that of the 853 GHz transition under LTE conditions. while the Ω = 3 transitions have calculated intensity of ∼ 20%−50% … view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: presents the 1 GHz-wide spectra of the detected TiO and tentatively detected AlOH lines. These transitions are among the most prominent features in the spectra, with intensities comparable to those of commonly detected species such as H2O, SiO, and SO2. The broader lin…
Figure 5
Figure 5. Figure 5: PV diagrams and spectra for the three blended TiO transitions. The red contours are plotted at intervals of 4σ , starting from 4σ. The mean spectra are extracted from a circular area within 100 au from the continuum center. At 415 pc, 100 au = 0. ′′24. The effective em…

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Reference graph

Works this paper leans on

49 extracted references · 30 canonical work pages

  1. [1]

    Explosive Outflows Powered by the Decay of Non-Hierarchical Multiple Systems of Massive Stars: Orion BN/KL

    Explosive Outflows Powered by the Decay of Non-hierarchical Multiple Systems of Massive Stars: Orion BN/KL. , keywords =. doi:10.1088/0004-637X/727/2/113 , archivePrefix =. 1011.5512 , primaryClass =

    work page Pith review arXiv

  2. [2]

    , year = 2008, month = jun, volume =

    Primordial compositions of refractory inclusions. , year = 2008, month = jun, volume =. doi:10.1016/j.gca.2008.04.002 , adsurl =

    work page doi:10.1016/j.gca.2008.04.002 2008

  3. [3]

    Chemical equilibrium in AGB atmospheres: Successes, failures, and prospects for small molecules, clusters, and condensates

    Chemical equilibrium in AGB atmospheres: successes, failures, and prospects for small molecules, clusters, and condensates. , keywords =. doi:10.1051/0004-6361/202037496 , archivePrefix =. 2004.00519 , primaryClass =

    work page Pith review arXiv 2004

  4. [4]

    , keywords =

    Solar System Abundances and Condensation Temperatures of the Elements. , keywords =. doi:10.1086/375492 , adsurl =

    doi:10.1086/375492

  5. [5]

    Maser emission from SiO isotopologues traces the innermost 100 AU around Radio Source I in Orion BN/KL

    Maser Emission from SiO Isotopologues Traces the Innermost 100 AU Around Radio Source I in Orion Becklin-Neugebauer/Kleinmann-Low. , keywords =. doi:10.1088/0004-637X/698/2/1165 , archivePrefix =. 0904.1373 , primaryClass =

    work page Pith review arXiv

  6. [6]

    Salt, Hot Water, and Silicon Compounds Tracing Massive Twin Disks

    Salt, Hot Water, and Silicon Compounds Tracing Massive Twin Disks. , keywords =. doi:10.3847/2041-8213/abadfc , archivePrefix =. 2007.02962 , primaryClass =

    work page Pith review arXiv

  7. [7]

    Extremely high excitation SiO lines in disk-outflow system in Orion Source I

    Extremely High Excitation SiO Lines in Disk-outflow Systems in Orion Source I. , keywords =. doi:10.3847/1538-4357/aafb6b , archivePrefix =. 1901.07208 , primaryClass =

    work page Pith review arXiv 1901

  8. [8]

    Rotational spectra of vibrationally excited AlO and TiO in oxygen rich stars

    Rotational Spectra of Vibrationally Excited AlO and TiO in Oxygen-rich Stars. , keywords =. doi:10.3847/1538-4357/abc079 , archivePrefix =. 2010.06485 , primaryClass =

    work page Pith review arXiv 2010

Show all 49 references
  1. [9]

    , keywords =

    On the Nature of Orion Source I. , keywords =. doi:10.3847/1538-4357/aaa24b , adsurl =

    doi

  2. [10]

    arXiv e-prints , keywords =

    Condensation of Rocky Material in Astrophysical Environments. arXiv e-prints , keywords =. doi:10.48550/arXiv.2306.15043 , archivePrefix =. 2306.15043 , primaryClass =

    doi arXiv

  3. [11]

    , keywords =

    Accretion and Outflow in Orion-KL Source I. , keywords =. doi:10.3847/1538-4357/ad7026 , archivePrefix =. 2408.05114 , primaryClass =

    arXiv

  4. [12]

    Science , keywords =

    The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk. Science , keywords =. doi:10.1126/science.1226919 , adsurl =

    doi

  5. [13]

    Faraday Discussions , year = 1998, month = jan, volume =

    Inorganic dust formation in astrophysical environments. Faraday Discussions , year = 1998, month = jan, volume =. doi:10.1039/a709290c , adsurl =

    1998 doi

  6. [14]

    , keywords =

    High-angular-resolution ALMA imaging of the inhomogeneous dynamical atmosphere of the asymptotic giant branch star W Hya: SiO, H _ 2 O, SO _ 2 , SO, HCN, AlO, AlOH, TiO, TiO _ 2 , and OH lines. , keywords =. doi:10.1051/0004-6361/202554900 , archivePrefix =. 2512.03156 , prima...

  7. [15]

    , keywords =

    Pure rotational spectra of TiO and TiO _ 2 in VY Canis Majoris. , keywords =. doi:10.1051/0004-6361/201220290 , archivePrefix =. 1301.4344 , primaryClass =

    arXiv

  8. [16]

    Indications for the presence of gas-phase (Al _ 2 O _ 3 ) _ n clusters

    Study of the aluminium content in AGB winds using ALMA. Indications for the presence of gas-phase (Al _ 2 O _ 3 ) _ n clusters. , keywords =. doi:10.1051/0004-6361/201730782 , archivePrefix =. 1704.05237 , primaryClass =

    arXiv

  9. [17]

    Science Advances , keywords =

    Dust formation and wind acceleration around the aluminum oxide-rich AGB star W Hydrae. Science Advances , keywords =. doi:10.1126/sciadv.aao2149 , adsurl =

    doi

  10. [18]

    , keywords =

    Millimeter Detection of AlO (X ^ 2 ^ + ): Metal Oxide Chemistry in the Envelope of VY Canis Majoris. , keywords =. doi:10.1088/0004-637X/694/1/L59 , adsurl =

    doi

  11. [19]

    , keywords =

    VLBA imaging of the 3 mm SiO maser emission in the disk-wind from the massive protostellar system Orion Source I. , keywords =. doi:10.1051/0004-6361/201731548 , archivePrefix =. 1707.07455 , primaryClass =

    arXiv

  12. [20]

    Cosmic Masers - from OH to H0 , year = 2012, editor =

    325 GHz Water Masers in Orion Source I. Cosmic Masers - from OH to H0 , year = 2012, editor =. doi:10.1017/S1743921312006916 , adsurl =

    2012 doi

  13. [21]

    , keywords =

    The First Detection of the 232 GHz Vibrationally Excited H _ 2 O Maser in Orion KL with ALMA. , keywords =. doi:10.1088/2041-8205/757/1/L1 , archivePrefix =. 1208.4489 , primaryClass =

    arXiv

  14. [22]

    The APOGEE-2 Survey of the Orion Star-forming Complex. II. Six-dimensional Structure. , keywords =. doi:10.3847/1538-3881/aad1f1 , archivePrefix =. 1805.04649 , primaryClass =

    arXiv

  15. [23]

    , keywords =

    The distance to the Orion Nebula. , keywords =. doi:10.1051/0004-6361:20078247 , archivePrefix =. 0709.0485 , primaryClass =

    arXiv

  16. [24]

    , keywords =

    Salt-bearing Disk Candidates around High-mass Young Stellar Objects. , keywords =. doi:10.3847/1538-4357/ac9f4a , archivePrefix =. 2211.02502 , primaryClass =

    arXiv

  17. [25]

    , keywords =

    Orion SrcI s Disk Is Salty. , keywords =. doi:10.3847/1538-4357/aafb71 , archivePrefix =. 1901.04489 , primaryClass =

    1901 arXiv

  18. [26]

    , keywords =

    ALMA Observations of Orion Source I at 350 and 660 GHz. , keywords =. doi:10.3847/1538-4357/833/2/219 , archivePrefix =. 1608.00996 , primaryClass =

    arXiv

  19. [27]

    , keywords =

    A Protoplanet Candidate in the PDS 66 Disk Indicated by Silicon Sulfide Isotopologues. , keywords =. doi:10.3847/2041-8213/ae45a3 , archivePrefix =. 2602.12522 , primaryClass =

  20. [28]

    , keywords =

    SO and SiS Emission Tracing an Embedded Planet and Compact ^ 12 CO and ^ 13 CO Counterparts in the HD 169142 Disk. , keywords =. doi:10.3847/2041-8213/acdfd0 , archivePrefix =. 2306.13710 , primaryClass =

    arXiv

  21. [29]

    pvextractor: Position-Velocity Diagram Extractor

  22. [30]

    doi:10.5281/zenodo.2573901 , version =

    radio-astro-tools/spectral-cube: v0.4.4. doi:10.5281/zenodo.2573901 , version =

    doi

  23. [31]

    arXiv , Author =:1307.6212 , Journal =

    doi:10.1051/0004-6361/201322068 , Eid =. arXiv , Author =:1307.6212 , Journal =

    arXiv

  24. [32]

    , keywords =

    The Astropy Project: Building an Open-science Project and Status of the v2.0 Core Package. , keywords =. doi:10.3847/1538-3881/aabc4f , archivePrefix =. 1801.02634 , primaryClass =

    arXiv

  25. [33]

    , keywords =

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    arXiv

  26. [34]

    doi:10.5281/zenodo.4905459 , url =

    Angus Comrie and Kuo-Song Wang and Shou-Chieh Hsu and Anthony Moraghan and Pamela Harris and Qi Pang and Adrianna Pińska and Cheng-Chin Chiang and Tien-Hao Chang and Yu-Hsuan Hwang and Hengtai Jan and Ming-Yi Lin and Rob Simmonds , title =. doi:10.5281/zenodo.4905459 , url =

    doi

  27. [35]

    , keywords =

    ALMA Band 8 Continuum Emission from Orion Source I. , keywords =. doi:10.3847/1538-4357/833/2/238 , archivePrefix =. 1611.00855 , primaryClass =

    arXiv

  28. [36]

    STATCONT: Statistical continuum level determination method for line-rich sources

  29. [37]

    , keywords =

    CASA, the Common Astronomy Software Applications for Radio Astronomy. , keywords =. doi:10.1088/1538-3873/ac9642 , archivePrefix =. 2210.02276 , primaryClass =

    arXiv

  30. [38]

    , keywords =

    The chemical make-up of the Sun: A 2020 vision. , keywords =. doi:10.1051/0004-6361/202140445 , archivePrefix =. 2105.01661 , primaryClass =

    2020 arXiv

  31. [39]

    , keywords =

    Observations of SiO toward OMC-1: A New Outflow Source 1.5 South of Orion-KL?. , keywords =. doi:10.1086/184849 , adsurl =

    doi

  32. [40]

    , keywords =

    ALMA Imaging of Millimeter/Submillimeter Continuum Emission in Orion KL. , keywords =. doi:10.1088/0004-637X/801/2/82 , archivePrefix =. 1502.00458 , primaryClass =

    arXiv

  33. [41]

    , keywords =

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

    doi

  34. [42]

    Astrophysical Masers: Unlocking the Mysteries of the Universe , year = 2018, editor =

    ALMA observations of submillimeter H _ 2 O and SiO lines in Orion Source I. Astrophysical Masers: Unlocking the Mysteries of the Universe , year = 2018, editor =. doi:10.1017/S1743921317010225 , archivePrefix =. 1711.08952 , primaryClass =

    2018 arXiv

  35. [43]

    Bottom-up dust nucleation theory in oxygen-rich evolved stars. I. Aluminium oxide clusters. , keywords =. doi:10.1051/0004-6361/202141976 , archivePrefix =. 2110.11139 , primaryClass =

    arXiv

  36. [44]

    ACS Earth and Space Chemistry , year = 2021, month = dec, volume =

    Kinetic Study of the Reactions of AlO with H2O and H2; Precursors to Stellar Dust Formation. ACS Earth and Space Chemistry , year = 2021, month = dec, volume =. doi:10.1021/acsearthspacechem.1c00225 , adsurl =

    2021 doi

  37. [45]

    Nature Astronomy , keywords =

    Disk-driven rotating bipolar outflow in Orion Source I. Nature Astronomy , keywords =. doi:10.1038/s41550-017-0146 , archivePrefix =. 1712.04606 , primaryClass =

    arXiv

  38. [46]

    , keywords =

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

    arXiv

  39. [47]

    , keywords =

    FERIA: Flat Envelope Model with Rotation and Infall under Angular Momentum Conservation. , keywords =. doi:10.1088/1538-3873/ac8839 , archivePrefix =. 2208.04581 , primaryClass =

    arXiv

  40. [48]

    , keywords =

    Spatial Distribution of AlO in a High-mass Protostar Candidate Orion Source I. , keywords =. doi:10.3847/2041-8213/ab1653 , adsurl =

    doi

  41. [49]

    Journal of Molecular Spectroscopy , keywords =

    The Cologne Database for Molecular Spectroscopy, CDMS, in the Virtual Atomic and Molecular Data Centre, VAMDC. Journal of Molecular Spectroscopy , keywords =. doi:10.1016/j.jms.2016.03.005 , archivePrefix =. 1603.03264 , primaryClass =

    2016 arXiv

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.