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Considerations on the Origin of IRAS 19312+1950 Based on Long-Term Maser Observations

T0 review · 2 major / 5 minor · reviewed 2026-08-10 · deepseek-v4-flash

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Pith's one-line read After two decades of maser monitoring, IRAS 19312+1950 remains an unclassified object whose H2O masers make it a candidate Water Fountain star.

desk verdict Careful, honest maser monitoring of a genuinely puzzling object with a reusable 20-year dataset; the maser-to-CO association claim is nearly tautological and should be flagged as an unverified hypothesis. read the letter →

arxiv 2501.13769 v1 pith:OGARMI7M submitted 2025-01-23 astro-ph.GA

Huan-Xue Feng , Jun-ichi Nakashima , D. Engels , S. Etoka , Jaeheon Kim , Yong Zhang , Jia-Yong Xie , Jian-Jie Qiu This is my paper · ORCID
classification astro-ph.GA
keywords IRAS19312+1950SiOmaserH2OOHwaterfountainstarpost-AGBrednovaremnantvariability
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 follows one peculiar infrared source, IRAS 19312+1950 (I19312), whose SiO, H2O, and OH masers have been known for two decades but whose identity has never settled. The authors report roughly two years of new single-dish monitoring of all three maser species and compare it with every earlier spectrum, trying to decide whether I19312 is an evolved star on the way to the post-AGB phase, a young stellar object, a red nova remnant, or something in between. Their conclusion is explicitly open: the origin and evolutionary stage remain unclear. What is established is that the H2O maser emission extends beyond the velocity range of the OH masers, the operational signature of a Water Fountain star, a rare object whose H2O masers trace fast jets while OH masers still trace the older slow wind. The reason to care is that if I19312 really is a Water Fountain, its very large molecular gas mass, carbon-rich chemistry, and 20-year persistence of SiO masers make it an anomalous member of a class that is itself a brief, poorly sampled phase of stellar death.

What carries the argument

The load-bearing structure is the two-component kinematic model of I19312's CO envelope, built from earlier BIMA mapping and a Shape model: a narrow, slowly moving bipolar flow and a broad, roughly spherical expanding inner component. The authors plot the averaged OH, H2O, and SiO maser spectra against the modelled velocity ranges of these two components, and because the maser velocities reach beyond the narrow component, they infer that all three maser species most likely reside in the broad component. The second piece of machinery is the monitoring time series itself, which catches correlated variability, most notably the near-simultaneous brightening of the H2O blueshifted peak and the SiO 42.821 GHz line around May 2018, a relationship invisible in single-epoch observations.

What would settle it

Map the absolute positions of the H2O, SiO, and OH maser spots with very-long-baseline interferometry and compare them with the modelled broad and narrow CO components; if the masers do not lie within the broad component, or if the H2O spots trace a collimated jet, the velocity-overlap argument for the water-fountain interpretation is refuted. Continued monitoring that still detects the SiO 42.821 GHz line after another decade would similarly contradict the expectation that SiO masers fade as an object enters the post-AGB phase.

Watch

Extended reading notes

Core claim

The paper's central claim is negative in form: after combining fresh 2018-2020 monitoring with all archival maser spectra, I19312 cannot be unambiguously assigned to any known class. The new data show OH maser features varying irregularly by up to a factor of about two, a H2O double-peaked profile whose dominant side switched from blueshifted ($22$--$28$ km s$^{-1}$) to redshifted ($38$--$42$ km s$^{-1}$) around January 2019 with brightness changes of more than a factor of 30, and SiO $v=1,2$, $J=1$--$0$ masers persisting near $50$--$55$ km s$^{-1}$ with the $v=2$ line stronger than the $v=1$ line. Because the H2O velocity range lies partly outside the OH range, the paper identifies I19312 as a candidate Water Fountain star, yet it immediately flags inconsistencies: the molecular gas mass of $225$--$478$ solar masses and the chemical abundance pattern fit neither a typical evolved star nor a young stellar object, and the red nova remnant alternative remains speculative.

Load-bearing premise

The load-bearing assumption is that the OH, H2O, and SiO masers genuinely sit inside the broad kinematic component of the CO envelope, a link inferred solely from velocity overlap because the absolute positions of the maser emission regions have never been measured.

Editorial extensions

If this is right

  • If I19312 is a Water Fountain star, it becomes one of a handful of objects observed in the brief phase when H2O masers trace collimated outflows while OH masers still trace the remnant AGB wind.
  • The derived luminosity of about $21500$ solar luminosities and the parallax distance of about $3.8$ kpc imply an intermediate-mass progenitor above roughly $2$ solar masses if the object is an evolved star.
  • The 20-year persistence of SiO masers with the $v=2$, $J=1$--$0$ line stronger than $v=1$ sets a constraint that any successful model, whether evolved star or red nova remnant, must reproduce.
  • The H2O maser switch from blueshifted to redshifted dominance between 2018 and 2020 shows that the maser excitation responds to changes in mass loss on month timescales, providing a new benchmark for envelope models.

Reading between the lines

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

  • A testable extension the paper leaves implicit: if the May 2018 brightening of the H2O blueshifted feature and the SiO 42.821 GHz line shared a single trigger, a delayed response should eventually appear in the OH masers, which form farther out in the envelope, and could be sought in the 2018 NRT data and future monitoring.
  • If future absolute-position measurements place the masers in the narrow bipolar flow instead of the broad component, the paper's kinematic association would fail, yet the water-fountain interpretation would actually be strengthened, because water-fountain H2O masers are expected to trace the jets.
  • The paper's own comparison suggests, though it does not assert, that I19312 may be an interaction product---a merger or a wind-wind collision---rather than a single star in a standard evolutionary sequence; searching for a central binary or an archival outburst light echo would test that possibility.
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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

2 major / 5 minor

Summary. The paper reports long-term single-dish monitoring of SiO, H2O, and OH maser emission toward IRAS 19312+1950 (I19312) using the NRT and KVN telescopes, combined with a compilation of historical maser observations spanning about 20 years. The authors compare the maser properties with those of evolved stars, young stellar objects, water fountains, red nova remnants, and several peculiar objects, and they update the source luminosity from a new infrared SED. They conclude that the origin and evolutionary stage of I19312 remain unclear, while suggesting that the object is a candidate water fountain (WF) star because the H2O maser velocities extend beyond the OH maser velocity range, and that the masers are likely associated with the broad kinematic component of the CO envelope.

Significance. The observational work is careful and well documented: telescope parameters, calibration procedures, rms noise levels, and signal-to-noise ratios are reported, and detections below 5 sigma are explicitly flagged in the tables. The compilation of more than two decades of maser spectra is a useful legacy dataset for a poorly understood object. If the water-fountain candidacy holds, I19312 would be a rare post-AGB-type object, although the paper's cautious bottom line that the origin remains unclear is appropriate. The main value is the new monitoring data and the comparative discussion, rather than a decisive classification.

major comments (2)
  1. [Section 3.4, Figure 16, and Summary point 4] The claim that the OH, H2O, and SiO masers are likely associated with the broad CO component is supported only by velocity overlap. The broad component spans approximately 0-70 km/s in the CO model shown in Figure 16, which covers essentially the full velocity ranges of the masers (OH about 10-46 km/s, H2O about 22-42 km/s, SiO about 50-55 km/s). The overlap criterion therefore has almost no discriminating power. Because the authors explicitly state that absolute maser positions have not been determined, the 'complex geometry' interpretation in Section 4 and Summary point 4 should be presented as an unverified working hypothesis, or the paper should state clearly that the current data cannot distinguish association with the broad component from association with the narrow bipolar outflow or a distinct region.
  2. [Section 4.3.2 and Summary point 2] The water-fountain candidacy rests on the statement that H2O maser emission is detected outside the OH maser velocity range. From Tables 3 and 5, the H2O maser spans about 22-42 km/s while the OH 1612 MHz maser spans about 10-40 km/s, so the extension is only about 2 km/s at the red edge. This is far smaller than the high-velocity jet signatures of established water fountains discussed in the text. The only higher-velocity H2O feature, near 78 km/s on 2019-03-03, is a 3.2 sigma tentative detection and is not included in the analysis. Please either quantify how this marginal velocity extension satisfies the WF search criteria of Fan et al. (2024) or soften the WF-candidate claim accordingly.
minor comments (5)
  1. [Throughout] There are numerous typographical errors that should be corrected, including 'T erm' in the title, 'Wavelenght' in Table 9, 'specifitc' in Section 4.3, 'spieces' in Section 4.3.4, and 'Osb.date' in several figure labels.
  2. [Figure 3 caption] The caption for Figure 3 identifies the displayed line as OH 1665 MHz, while the figure header and the main text refer to the 1667 MHz line; the caption and the plotted transition should be aligned.
  3. [Section 2] The KVN calibration procedure is described in detail, but the absolute flux calibration uncertainty for the KVN measurements is not explicitly stated; please add the estimated uncertainty as is done for the NRT data.
  4. [Appendix A] The SED integration used to derive the luminosity includes optical and near-infrared photometry; please state explicitly whether any extinction correction was applied, since this can affect the derived luminosity.
  5. [Section 4.2] The statement that SiO masers have been detected from 'a total of eight YSOs' cites Cho et al. (2016); because this number may have changed, the sentence should be updated with a more recent census or a qualifying phrase.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the maser monitoring, SED luminosity, and class comparisons are independent; the CO-based broad-component association is a weak but non-circular inference.

full rationale

The paper's new results are measured maser line parameters, integrated fluxes, an SED luminosity, and qualitative comparisons of maser velocity ranges with historical data and with a CO kinematic model. None of these is obtained by defining an input in terms of an output. The luminosity (about 21500 Lsun) is a trapezoidal integral of archived photometry multiplied by the VLBI parallax distance (Imai et al. 2011); the distance and photometry are external to the paper's conclusion. The closest step to a circular construction is the statement that 'from a velocity perspective, it can be inferred that the OH, H2O, and SiO masers are likely associated with the broad component' (Section 3.4). This is not circular: the narrow and broad CO components come from independent CO interferometry and Shape modeling (Nakashima & Deguchi 2005; Qiu et al. 2023), not from the maser velocities, and the authors explicitly acknowledge that absolute maser positions are undetermined. The inference may be weakly constrained because the broad component covers a wide velocity range, but this is a limitation of evidence, not a reduction of the claim to its inputs. Self-citations supply prior observational data and modeling used as context rather than as a self-referential proof; the conclusion that the origin and evolutionary stage 'remain unclear' is non-committal and does not depend on a circular chain. No fitted parameter is relabeled as a prediction, and no uniqueness theorem from the authors' prior work is invoked to force an alternative. I therefore find no significant circularity.

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

The central claim (origin unclear, water fountain candidate) rests on externally measured distance, systemic velocity, and a kinematic CO model from prior literature, some by the same group. These are not fitted in this paper, and no new entities or free parameters are introduced.

assumptions (4)
  • domain assumption Distance to I19312 is 3.8 (-0.58/+0.83) kpc from VLBI annual parallax of the H2O maser (Imai et al. 2011).
    Used to convert SED flux to luminosity and to argue against a low-mass YSO. If the distance is wrong, the luminosity and mass estimates shift accordingly.
  • domain assumption Systemic velocity of about 35 km/s for the broad CO component (Nakashima & Deguchi 2005).
    All maser velocity offsets are referenced to this value, and much of the discussion about blueshifted and redshifted emission depends on it.
  • domain assumption The molecular envelope has narrow and broad kinematic components, as modeled by Qiu et al. (2023).
    The paper assigns all three maser species to the broad component based on velocity overlap, an assumption it explicitly acknowledges is not positionally verified.
  • domain assumption Type I and Type II OH maser classification and radiative pumping assumptions from the literature (e.g., Habing 1996, Lewis 2000).
    Used to argue that the dominance of the 1612 MHz satellite line points to an evolved star. The paper itself notes the pumping mechanism is not fully understood.

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Cite this review

Pith. "Pith review of Considerations on the Origin of IRAS 19312+1950 Based on Long-Term Maser Observations." pith.science (2026). https://pith.science/paper/OGARMI7M

@misc{pith2026250113769,
  author       = {Pith},
  title        = {Pith review of: Considerations on the Origin of IRAS 19312+1950 Based on Long-Term Maser Observations},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/OGARMI7M}},
  note         = {Machine review of arXiv:2501.13769}
}
abstract

IRAS source 19312+1950 (hereafter I19312) is an infrared point source with maser emissions of SiO, H$_2$O, and OH molecules. Although initial observations suggested that I19312 might be an evolved star, its characteristics are not fully consistent with this classification. This study aims to further investigate the nature of I19312 by conducting long-term monitoring of its maser emissions and comparing the results with other known astrophysical objects. We conducted long-term monitoring of SiO, H$_2$O, and OH maser emissions using single-dish radio telescopes. The results were then compared with historical maser data and the characteristics of similar objects to infer the possible origin of I19312. The SiO maser emissions from I19312 were detected over a wide velocity range and exhibited significant time variability. The OH maser lines suggest characteristics of an evolved star, while the H$_2$O maser lines indicate molecular outflows. These features suggest that I19312 could be a candidate for a Water Fountain (WF) star, though there are inconsistencies, such as the large molecular gas mass, that challenge this hypothesis. The possibility of I19312 being a Red Nova Remnant (RNR) is also considered, but this remains speculative due to the lack of direct evidence. The evolutionary stage of I19312 remains unclear, but it shares multiple characteristics with both evolved stars with peculiar properties and RNRs. Further long-term monitoring and high-resolution interferometric observations are required to better constrain the nature of this object.

Figures

Figures reproduced from arXiv: 2501.13769 by the authors.

Figure 1
Figure 1. Spectra of the OH 1612 MHz maser line of I19312 in Stokes I (blue line) from February 2, 2018 to September 30, 2018. The red broken line is the average of the spectra for all observation dates. The numbers in parentheses are the total number of days counted from January 3, 2018, the start date of the present monitoring observation. The green dotted vertical line represents the systemic velocity (∼ 35 km s−1 ) of the… view at source ↗
Figure 2
Figure 2. Spectra of the OH 1665 MHz maser line of I19312 in Stokes I from February 2, 2018, to September 30, 2018. The notations are the same as in [PITH_FULL_IMAGE:figures/full_fig_p019_2.png] view at source ↗
Figure 3
Figure 3. Spectra of the OH 1665 MHz maser line of I19312 in Stokes I from February 2, 2018 to September 30, 2018. Notations are the same as in [PITH_FULL_IMAGE:figures/full_fig_p020_3.png] view at source ↗
Figures from the paper (13 more)
Figure 4
Figure 4. Figure 4: Upper panel: velocity ranges of previously detected OH maser lines. The colors of the horizontal lines correspond to the legend in the lower panel. The dashed parts of the horizontal lines represent the visually corrected velocity range (see main text). Bottom panel: c…
Figure 5
Figure 5. Figure 5: Time evolution of the OH 1612 MHz maser spectra of I19312 over the last 20 years. Arecibo and MERLIN data are taken from Nakashima et al. (2011), and Effelsberg data are taken from Yung et al. (2014). The date of observation (YYMMDD) is given for each spectral line. Th…
Figure 6
Figure 6. Figure 6: Time evolution of the OH 1665 MHz maser spectra of I19312 over the last 20 years. Arecibo data are taken from Nakashima et al. (2011), and Effelsberg data are taken from Yung et al. (2014). The date of observation (YYMMDD) is given for each spectral line. The green dot…
Figure 7
Figure 7. Figure 7: Time evolution of the OH 1667 MHz maser spectra of I19312 over the last 20 years. Arecibo data are taken from Nakashima et al. (2011), and Effelsberg data are taken from Yung et al. (2014). The date of observation (YYMMDD) is given for each spectral line. The green dot…
Figure 8
Figure 8. Figure 8: Spectra of the H2O 22.235 GHz line of I19312 from 2018 January to 2020 May. Notations are the same as in [PITH_FULL_IMAGE:figures/full_fig_p025_8.png]
Figure 10
Figure 10. Figure 10: Spectra of the SiO 42.821 GHz and SiO 43.122 GHz maser lines of I19312 from 2018 January to 2020 May. Notations are the same as in [PITH_FULL_IMAGE:figures/full_fig_p028_10.png]
Figure 11
Figure 11. Figure 11: Selected spectra of the SiO 86.243 GHz line of I19312 from 2018 January to 2020 May. The red arrows represent emission peaks that were considered likely to be detected. Other notations are the same as in [PITH_FULL_IMAGE:figures/full_fig_p029_11.png]
Figure 12
Figure 12. Figure 12: Time evolution of the SiO 42.821 GHz maser spectra of I19312 over the last 20 years. The data were collected from the literature (see text). Nobeyama, VLBA and KVN data were taken from Nakashima & Deguchi (2000); Deguchi et al. (2004); Nakashima & Deguchi (2007); Naka…
Figure 13
Figure 13. Figure 13: Time evolution of the SiO 43.122 GHz maser spectra of I19312 over the last 20 years. Nobeyama, VLBA and KVN data were taken from Nakashima & Deguchi (2000); Deguchi et al. (2004); Nakashima & Deguchi (2007); Nakashima et al. (2011); Kim et al. (2016). The data of obse…
Figure 14
Figure 14. Figure 14: Time evolution of the SiO 86.243 GHz maser spectra of I19312 over the last 20 years. Nobeyama and IRAM data were taken from Nakashima & Deguchi (2000); Deguchi et al. (2004); Qiu et al. (2023). The data of observation (YYMMDD) is given for each spectral line. The conv…
Figure 15
Figure 15. Figure 15: Comparison of the averaged OH 1612 MHz, H2O 22.235 GHz, SiO 43.122 GHz and SiO 42.821 GHz maser spectra. The CO J = 1 − 0 spectrum obtained with BIMA (Nakashima & Deguchi 2005) is superimposed for comparison. The intensity of the maser lines is given in Jy units (see …
Figure 16
Figure 16. Figure 16: Left panel: Model geometry of the Shape model from four different angles (Qiu et al. 2023). The model was built based on the distribution of CO gas. The Free-Form view means the observer’s view with a position angle of −37◦ , where up is north and left is east. The mo…
Figure 17
Figure 17. Figure 17: Spectral energy distribution of IRAS 19312+1950 in the optical and infrared wavelengths based on the latest data set. See Appendix A for details [PITH_FULL_IMAGE:figures/full_fig_p033_17.png]

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Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Unveiling the enigma of the Nakashima-Deguchi object (IRAS 19312+1950): a candidate Orion KL analog

    astro-ph.GA 2026-07 conditional novelty 6.5 of 10

    Multi-telescope continuum and line data show NDO (IRAS 19312+1950) hosts cold dense gas with deuterated species and a bipolar outflow, making it a candidate Orion KL analog at ~3.8 kpc.

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Works this paper leans on

74 extracted references · 37 canonical work pages · cited by 1 Pith paper

  1. [1]

    2001, , 373, 932, 10.1051/0004-6361:20010535

    Alcolea , J., Bujarrabal , V., S \'a nchez Contreras , C., Neri , R., & Zweigle , J. 2001, , 373, 932, 10.1051/0004-6361:20010535

    doi:10.1051/0004-6361:20010535 2001

  2. [2]

    2022, , 163, 85, 10.3847/1538-3881/ac3fb6

    Amada , K., Imai , H., Hamae , Y., et al. 2022, , 163, 85, 10.3847/1538-3881/ac3fb6

    work page doi:10.3847/1538-3881/ac3fb6 2022

  3. [3]

    1996, , 310, 259

    Barnbaum , C., Omont , A., & Morris , M. 1996, , 310, 259

    work page 1996

  4. [4]

    Barvainis , R., & Clemens , D. P. 1984, , 89, 1833, 10.1086/113695

    work page doi:10.1086/113695 1984

  5. [5]

    F., Johnston , K

    Bowers , P. F., Johnston , K. J., & Spencer , J. H. 1983, , 274, 733, 10.1086/161485

    work page doi:10.1086/161485 1983

  6. [6]

    2007, in IAU Symposium, Vol

    Bujarrabal , V., Alcolea , J., Colomer , F., et al. 2007, in IAU Symposium, Vol. 242, Astrophysical Masers and their Environments, ed. J. M. Chapman & W. A. Baan , 271--278, 10.1017/S1743921307013129

    work page doi:10.1017/s1743921307013129 2007

  7. [7]

    2002, , 389, 271, 10.1051/0004-6361:20020455

    Bujarrabal , V., Alcolea , J., S \'a nchez Contreras , C., & Sahai , R. 2002, , 389, 271, 10.1051/0004-6361:20020455

    doi:10.1051/0004-6361:20020455 2002

  8. [8]

    2015, Journal of Korean Astronomical Society, 48, 267, 10.5303/JKAS.2015.48.5.267

    Cho , S.-H., Kim , J., & Yun , Y. 2015, Journal of Korean Astronomical Society, 48, 267, 10.5303/JKAS.2015.48.5.267

    work page doi:10.5303/jkas.2015.48.5.267 2015

Show all 74 references
  1. [9]

    2016, , 826, 157, 10.3847/0004-637X/826/2/157

    Cho , S.-H., Yun , Y., Kim , J., et al. 2016, , 826, 157, 10.3847/0004-637X/826/2/157

    2016 doi

  2. [10]

    J., Bond , H

    Claussen , M. J., Bond , H. E., Starrfield , S., & Healy , K. 2007, in Astronomical Society of the Pacific Conference Series, Vol. 363, The Nature of V838 Mon and its Light Echo, ed. R. L. M. Corradi & U. Munari , 87

    2007

  3. [11]

    A., Boogert , A

    Cordiner , M. A., Boogert , A. C. A., Charnley , S. B., et al. 2016, , 828, 51, 10.3847/0004-637X/828/1/51

    2016 doi

  4. [12]

    M., Chapman , J

    Deacon , R. M., Chapman , J. M., & Green , A. J. 2004, , 155, 595, 10.1086/425329

    2004 doi

  5. [13]

    1999, , 51, 355, 10.1093/pasj/51.3.355

    Deguchi , S., Fujii , T., Izumiura , H., et al. 1999, , 51, 355, 10.1093/pasj/51.3.355

    1999 doi

  6. [14]

    2011, , 63, 309, 10.1093/pasj/63.1.309

    Deguchi , S., Koike , K., Kuno , N., et al. 2011, , 63, 309, 10.1093/pasj/63.1.309

    2011 doi

  7. [15]

    2005, , 57, L25, 10.1093/pasj/57.5.L25

    Deguchi , S., Matsunaga , N., & Fukushi , H. 2005, , 57, L25, 10.1093/pasj/57.5.L25

    2005 doi

  8. [16]

    2004, , 56, 1083, 10.1093/pasj/56.6.1083

    Deguchi , S., Nakashima , J.-I., & Takano , S. 2004, , 56, 1083, 10.1093/pasj/56.6.1083

    2004 doi

  9. [17]

    Dickinson , D. F. 1987, , 313, 408, 10.1086/164978

    1987 doi

  10. [18]

    2013, Advances in Astronomy and Space Physics, 3, 75

    Drozd , K., Swierczynski , E., Ragan , E., & Buil , C. 2013, Advances in Astronomy and Space Physics, 3, 75

    2013

  11. [19]

    2024, , 270, 13, 10.3847/1538-4365/ad0458

    Fan , H., Nakashima , J.-i., Engels , D., et al. 2024, , 270, 13, 10.3847/1538-4365/ad0458

    2024 doi

  12. [20]

    Fok , T. K. T., Nakashima , J.-i., Yung , B. H. K., Hsia , C.-H., & Deguchi , S. 2012, , 760, 65, 10.1088/0004-637X/760/1/65

    2012 doi

  13. [21]

    D., Wittkowski , M., Scholz , M., et al

    Gray , M. D., Wittkowski , M., Scholz , M., et al. 2009, , 394, 51, 10.1111/j.1365-2966.2008.14237.x

    2009

  14. [22]

    Habing , H. J. 1996, , 7, 97, 10.1007/PL00013287

    1996 doi

  15. [23]

    A., Burdon , A., et al

    Hafner , A., Green , J. A., Burdon , A., et al. 2024, , 41, e009, 10.1017/pasa.2024.3

    2024 doi

  16. [24]

    2013, , 125, 539, 10.1086/671125

    Han , S.-T., Lee , J.-W., Kang , J., et al. 2013, , 125, 539, 10.1086/671125

    2013 doi

  17. [25]

    1994, in American Astronomical Society Meeting Abstracts, Vol

    Hartigan , P., Edwards , S., & Ghandour , L. 1994, in American Astronomical Society Meeting Abstracts, Vol. 185, American Astronomical Society Meeting Abstracts, 48.15

    1994

  18. [26]

    Haschick , A. D., ed. 1986, Masers, molecules and mass outflows in star forming regions. Proceedings of a meeting held by the Haystack Observatory, Westford, Mass., USA, 15 - 16 May 1985

    1986

  19. [27]

    He , J. H. 2005, , 10, 283, 10.1016/j.newast.2004.11.001

    2005 doi

  20. [28]

    J., Miyazaki , A., & Deguchi , S

    Imai , H., Nakashima , J.-i., Diamond , P. J., Miyazaki , A., & Deguchi , S. 2005, , 622, L125, 10.1086/429820

    2005 doi

  21. [29]

    2011, , 63, 81, 10.1093/pasj/63.1.81

    Imai , H., Tafoya , D., Honma , M., Hirota , T., & Miyaji , T. 2011, , 63, 81, 10.1093/pasj/63.1.81

    2011 doi

  22. [30]

    2023, , 75, 1183, 10.1093/pasj/psad064

    Imai , H., Hamae , Y., Amada , K., et al. 2023, , 75, 1183, 10.1093/pasj/psad064

    2023 doi

  23. [31]

    R., Snyder , L

    Jewell , P. R., Snyder , L. E., Walmsley , C. M., Wilson , T. L., & Gensheimer , P. D. 1991, , 242, 211

    1991

  24. [32]

    2024, arXiv e-prints, arXiv:2401.03919, 10.48550/arXiv.2401.03919

    Kaminski , T. 2024, arXiv e-prints, arXiv:2401.03919, 10.48550/arXiv.2401.03919

    2024 doi arXiv

  25. [33]

    M., Tylenda , R., et al

    Kami \'n ski , T., Menten , K. M., Tylenda , R., et al. 2015, , 520, 322, 10.1038/nature14257

    2015 doi

  26. [34]

    2017, , 607, A78, 10.1051/0004-6361/201731287

    ---. 2017, , 607, A78, 10.1051/0004-6361/201731287

    2017 doi

  27. [35]

    2020, , 644, A59, 10.1051/0004-6361/202038648

    ---. 2020, , 644, A59, 10.1051/0004-6361/202038648

    2020 doi

  28. [36]

    2018, , 617, A129, 10.1051/0004-6361/201833165

    Kami \'n ski , T., Steffen , W., Tylenda , R., et al. 2018, , 617, A129, 10.1051/0004-6361/201833165

    2018 doi

  29. [37]

    2021, , 655, A32, 10.1051/0004-6361/202141526

    Kami \'n ski , T., Tylenda , R., Kiljan , A., et al. 2021, , 655, A32, 10.1051/0004-6361/202141526

    2021 doi

  30. [38]

    R., Djupvik , A

    Kami \'n ski , T., Schmidt , M. R., Djupvik , A. A., et al. 2024, , 682, A133, 10.1051/0004-6361/202347770

    2024 doi

  31. [39]

    H., Bujarrabal , V., et al

    Kim , J., Cho , S. H., Bujarrabal , V., et al. 2019, , 488, 1427, 10.1093/mnras/stz1830

    2019 doi

  32. [40]

    2016, Journal of Korean Astronomical Society, 49, 261, 10.5303/JKAS.2016.49.6.261

    Kim , J., Cho , S.-H., & Yoon , D.-H. 2016, Journal of Korean Astronomical Society, 49, 261, 10.5303/JKAS.2016.49.6.261

    2016 doi

  33. [41]

    Lewis , B. M. 1989, , 338, 234, 10.1086/167194

    1989 doi

  34. [42]

    2000, , 533, 959, 10.1086/308696

    ---. 2000, , 533, 959, 10.1086/308696

    2000 doi

  35. [43]

    2003, in Astrophysics and Space Science Library, Vol

    Messineo , M., Habing , H., Sjouwerman , L., Omont , A., & Menten , K. 2003, in Astrophysics and Space Science Library, Vol. 283, Mass-Losing Pulsating Stars and their Circumstellar Matter, ed. Y. Nakada , M. Honma , & M. Seki , 363--366, 10.1007/978-94-010-0139-7_83

    2003 doi

  36. [44]

    Millar , T. J. 2020, Chinese Journal of Chemical Physics, 33, 668, 10.1063/1674-0068/cjcp2008145

    2020 doi

  37. [45]

    Morris , M., & Bowers , P. F. 1980, , 85, 724, 10.1086/112732

    1980 doi

  38. [46]

    F., & Turner , B

    Morris , M., Bowers , P. F., & Turner , B. E. 1982, , 259, 625, 10.1086/160198

    1982 doi

  39. [47]

    2007, , 470, 957, 10.1051/0004-6361:20066574

    Murakawa , K., Nakashima , J., Ohnaka , K., & Deguchi , S. 2007, , 470, 957, 10.1051/0004-6361:20066574

    2007 doi

  40. [48]

    2000, , 52, L43, 10.1093/pasj/52.5.L43

    Nakashima , J.-i., & Deguchi , S. 2000, , 52, L43, 10.1093/pasj/52.5.L43

    2000 doi

  41. [49]

    2005, , 633, 282, 10.1086/444609

    ---. 2005, , 633, 282, 10.1086/444609

    2005 doi

  42. [50]

    2007, , 669, 446, 10.1086/520825

    ---. 2007, , 669, 446, 10.1086/520825

    2007 doi

  43. [51]

    Nakashima , J.-i., Deguchi , S., Imai , H., Kemball , A., & Lewis , B. M. 2011, , 728, 76, 10.1088/0004-637X/728/2/76

    2011 doi

  44. [52]

    2004, , 56, 193, 10.1093/pasj/56.1.193

    Nakashima , J.-I., Deguchi , S., & Kuno , N. 2004, , 56, 193, 10.1093/pasj/56.1.193

    2004 doi

  45. [53]

    A., Sobolev , A

    Nakashima , J.-i., Ladeyschikov , D. A., Sobolev , A. M., et al. 2016, , 825, 16, 10.3847/0004-637X/825/1/16

    2016 doi

  46. [54]

    M., Salii , S

    Nakashima , J.-i., Sobolev , A. M., Salii , S. V., et al. 2015, , 67, 95, 10.1093/pasj/psv064

    2015 doi

  47. [55]

    Olofsson , H., Vlemmings , W. H. T., Bergman , P., et al. 2017, , 603, L2, 10.1051/0004-6361/201731170

    2017 doi

  48. [56]

    2019, , 623, A153, 10.1051/0004-6361/201834897

    Olofsson , H., Khouri , T., Maercker , M., et al. 2019, , 623, A153, 10.1051/0004-6361/201834897

    2019 doi

  49. [57]

    Palla , F., & Stahler , S. W. 1999, , 525, 772, 10.1086/307928

    1999 doi

  50. [58]

    2023, , 669, A121, 10.1051/0004-6361/202244559

    Qiu , J.-J., Zhang , Y., Nakashima , J.-i., et al. 2023, , 669, A121, 10.1051/0004-6361/202244559

    2023 doi

  51. [59]

    2000, , 357, 651

    S \'a nchez Contreras , C., Bujarrabal , V., Neri , R., & Alcolea , J. 2000, , 357, 651

    2000

  52. [60]

    2008, , 60, 1077, 10.1093/pasj/60.5.1077

    Shintani , M., Imai , H., Ando , K., et al. 2008, , 60, 1077, 10.1093/pasj/60.5.1077

    2008 doi

  53. [61]

    I., Pashchenko , M

    Slysh , V. I., Pashchenko , M. I., Rudnitski i , G. M., Vitrishchak , V. M., & Colom , P. 2010, Astronomy Reports, 54, 599, 10.1134/S1063772910070048

    2010 doi

  54. [62]

    E., & Buhl , D

    Snyder , L. E., & Buhl , D. 1975, , 197, 329, 10.1086/153517

    1975 doi

  55. [63]

    B., Bond , H

    Sparks , W. B., Bond , H. E., Cracraft , M., et al. 2008, , 135, 605, 10.1088/0004-6256/135/2/605

    2008 doi

  56. [64]

    te Lintel Hekkert , P. T. L., Chapman , J. M., & Zijlstra , A. A. 1992, , 390, L23, 10.1086/186363

    1992 doi

  57. [65]

    K., Kami \'n ski , T., & Schmidt , M

    Tylenda , R., G \'o rny , S. K., Kami \'n ski , T., & Schmidt , M. 2015, , 578, A75, 10.1051/0004-6361/201425592

    2015 doi

  58. [66]

    2016, , 592, A134, 10.1051/0004-6361/201527700

    Tylenda , R., & Kami \'n ski , T. 2016, , 592, A134, 10.1051/0004-6361/201527700

    2016 doi

  59. [67]

    2006, , 451, 223, 10.1051/0004-6361:20054201

    Tylenda , R., & Soker , N. 2006, , 451, 223, 10.1051/0004-6361:20054201

    2006 doi

  60. [68]

    2011, , 528, A114, 10.1051/0004-6361/201016221

    Tylenda , R., Hajduk , M., Kami \'n ski , T., et al. 2011, , 528, A114, 10.1051/0004-6361/201016221

    2011 doi

  61. [69]

    2013, , 555, A16, 10.1051/0004-6361/201321647

    Tylenda , R., Kami \'n ski , T., Udalski , A., et al. 2013, , 555, A16, 10.1051/0004-6361/201321647

    2013 doi

  62. [70]

    Verheyen , L., Messineo , M., & Menten , K. M. 2012, , 541, A36, 10.1051/0004-6361/201118265

    2012 doi

  63. [71]

    A., Indebetouw , R., Bjorkman , J

    Whitney , B. A., Indebetouw , R., Bjorkman , J. E., & Wood , K. 2004, , 617, 1177, 10.1086/425608

    2004 doi

  64. [72]

    Yung , B. H. K., Nakashima , J.-i., & Henkel , C. 2014, , 794, 81, 10.1088/0004-637X/794/1/81

    2014 doi

  65. [73]

    Yung , B. H. K., Nakashima , J.-i., Imai , H., et al. 2013, , 769, 20, 10.1088/0004-637X/769/1/20

    2013 doi

  66. [74]

    A., Menten , K., Reid , M., & Beuther , H

    Zapata , L. A., Menten , K., Reid , M., & Beuther , H. 2009, , 691, 332, 10.1088/0004-637X/691/1/332

    2009 doi

Pith tools

Reviewed August 10, 2026 · model on record in the stance chip above.