Pith. sign in

REVIEW 6 minor 249 references

The Nakashima-Deguchi object sits in a cold, massive molecular cloud with deuterated gas and a bipolar outflow, and the authors propose it is an Orion KL analog ten times farther away.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · grok-4.5

2026-07-14 10:37 UTC pith:JRNZUMVA

load-bearing objection Solid multi-facility campaign that finally puts deuterated molecules and a bipolar high-velocity outflow on the map for NDO; the star-forming-environment case is robust, the Orion KL analogy is a fair postulate, and the mass number is the softest piece.

arxiv 2607.10587 v1 pith:JRNZUMVA submitted 2026-07-12 astro-ph.GA

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

Y. Gong , K. M. Menten , T. Kami\'nski , F. Schuller , F. Navarete , A. Belloche , P. Schilke , F. Wyrowski This is my paper
classification astro-ph.GA
keywords IRAS 19312+1950Nakashima-Deguchi objectSiO maserdeuterated moleculesmolecular outflowhigh-mass star formationOrion KL analogsubmillimeter continuum
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

For two decades the Nakashima-Deguchi object (IRAS 19312+1950) has looked half like a dust-enshrouded evolved star and half like a young massive star-forming region. New single-dish and interferometric continuum and line maps show that the surrounding material is cold (about 25 K), massive (roughly 220 solar masses), chemically rich, and heavily deuterated—properties that are routine in star-forming clouds but essentially never seen in the winds of evolved stars. The dust is resolved into several cores, the brightest of which hosts the famous SiO maser; the high-velocity gas forms a wide-angle bipolar outflow rather than a spherical shell. Taken together, these facts lead the authors to argue that the complex is interstellar and star-forming, and to propose that the object is a more distant twin of the famous Orion KL region.

Core claim

The material immediately around the Nakashima-Deguchi object is a cold, massive, deuterium-rich molecular cloud whose chemistry, mass, and outflow morphology match a high-mass star-forming environment far better than a pure circumstellar envelope of an evolved star; the authors therefore identify the object as a candidate Orion KL analog roughly ten times more distant.

What carries the argument

First detection of the deuterated species DCO+, DCN, DNC and HDCO, combined with SED-derived gas mass (~220 M⊙) and SMA imaging of a compact bipolar outflow, which together force the surrounding gas to be classified as cold interstellar material rather than stellar ejecta.

Load-bearing premise

The total gas mass and column density rest on the assumption that the dust follows the standard interstellar opacity law; if the grains instead have the composition of an evolved-star wind, the mass could be substantially lower.

What would settle it

High-resolution imaging that places the SiO maser, the continuum peak and the outflow driving source on scales of a few hundred au and shows either a clear disk-wind geometry like Source I or a pure AGB-like expansion would decide between the Orion-KL-analog and evolved-star scenarios.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

0 major / 6 minor

Summary. This paper presents a multi-telescope (IRAM 30 m, APEX, SMA) continuum and molecular-line study of the Nakashima-Deguchi object (IRAS 19312+1950). SED fitting of single-dish continuum yields Td = 25 ± 2 K, NH2 = (4.4 ± 0.6) × 10^22 cm^-2, β = 1.7 ± 0.2 and a total gas mass of 220 ± 21 M⊙; SMA continuum resolves at least four cores, with MM1 (associated with the SiO maser) as the dominant mass reservoir. Single-dish spectra detect 59 lines from 12 species, including the first detections of DCO+, DCN, DNC and HDCO; SMA spectra detect 75 lines toward MM1 with diverse ~0.1 pc morphologies. High-velocity CO is shown to be a compact, wide-angle bipolar outflow rather than spherical. From the deuterated inventory, CH3OH morphology, large mass and outflow geometry the authors conclude that the surrounding material is more naturally interstellar/star-forming than a pure CSE, and postulate that NDO is an Orion KL analog ~10 times farther away.

Significance. NDO has remained ambiguous for two decades between evolved-star and star-forming interpretations. The first secure detections of multiple deuterated species (D/H fractions 0.5–7.5 %), the SMA-resolved CH3OH and shock-tracer morphologies, and the high-resolution demonstration that the high-velocity CO is bipolar rather than spherical constitute a substantial observational advance. These data make a pure CSE origin for the bulk of the molecular material difficult to sustain and place the Orion KL analogy on a firmer empirical footing, while correctly framing it as a postulate. The work is of clear interest to the star-formation and late-stage stellar-evolution communities.

minor comments (6)
  1. Abstract, final sentence: the phrasing “The presence of deuterated species, and the overall large mass of the complex, the surrounding material…” is grammatically incomplete; insert “Based on” or restructure for clarity.
  2. Sect. 3.1.1 / Fig. 2: the exclusion of the 65/70 µm points is justified, but a short quantitative remark on how a two-temperature model would change Td and mass would strengthen the SED discussion.
  3. Sect. 4.2 / Table 3: the adopted 12C/13C = 53 (Galactic gradient) is reasonable, yet the text already notes that 12C/13C = 27 would raise D/H by ~2. A brief explicit statement that even the lower ratio still yields D/H ≫ cosmic would make the robustness clearer.
  4. Sect. 3.3 / Fig. 9: the position angle of the high-velocity bipolar outflow is not quoted numerically; adding it would facilitate comparison with the H2O-maser and NIR axes.
  5. Table A.11 and related text: for single-line species the fixed Trot (10 K single-dish, 40 K SMA) is conventional, but a one-sentence sensitivity test (e.g., ±5 K) would quantify the uncertainty on those column densities.
  6. A few typographical issues remain (e.g., “ystemic” in Fig. B.8 caption; inconsistent spacing around ± symbols). A careful proof-read is recommended.

Circularity Check

0 steps flagged

Observational paper with no circular derivation; deuterium detections and morphology are independent of the SED mass assumption.

full rationale

This is a multi-telescope observational study of continuum and molecular lines toward NDO. Column densities and abundances are obtained from measured integrated intensities via the standard LTE rotation-diagram formula (Eq. 5) under stated assumptions (source size 24 arcsec from Gaussian fits, fixed T_rot for single-line species). The SED mass (220 M☉) uses the conventional ISM opacity law, which the authors themselves flag as model-dependent, but that quantity is not required for the central claim: the first detections of DCO+, DCN, DNC and HDCO with D/H fractions 0.5–7.5 % (Table 3) cannot arise in stellar ejecta, and the SMA maps show CH3OH and a wide-angle bipolar high-velocity CO outflow inconsistent with a pure spherical CSE. The Orion KL analogy is explicitly labeled a postulate after the data are reduced. Self-citations of earlier NDO papers supply background context only and do not force any new result. No fitted parameter is renamed a prediction, no uniqueness theorem is imported, and no ansatz is smuggled via citation. Score 1 reflects only the minor, non-load-bearing self-citation of prior NDO work.

Axiom & Free-Parameter Ledger

5 free parameters · 4 axioms · 0 invented entities

Standard observational astronomy assumptions (LTE rotation diagrams, beam dilution, gas-to-dust ratio, ISM dust opacity) plus one adopted distance. No new physical entities are invented; the Orion KL analogy is a classification hypothesis. Free parameters are the usual SED and excitation fits.

free parameters (5)
  • dust temperature T_d = 25±2 K
    Fitted from multi-wavelength SED (Sect. 3.1.1); value 25±2 K used for all mass and column-density conversions.
  • dust emissivity index β = 1.7±0.2
    Fitted simultaneously with T_d and N_H2 in the modified-blackbody SED; adopted 1.7±0.2 for mass scaling and SMA flux extrapolation.
  • source size θ_s for beam dilution = 24 arcsec
    Fixed at 24″ from continuum Gaussian fits for all single-dish column-density calculations.
  • rotational temperatures for single-line species = 10 K / 40 K
    Fixed at 10 K (single-dish) or 40 K (SMA) when only one transition is available (Table A.11).
  • 12C/13C isotope ratio for deuterium fractions = 53
    Adopted from Galactic gradient (Yan et al. 2023) as 53 at the Galactocentric distance of NDO; directly scales D/H values.
axioms (4)
  • domain assumption Gas-to-dust mass ratio r_GDR = 100 and Ossenkopf & Henning (1994) κ_230 = 0.9 cm² g⁻¹ for ISM dust
    Used in Eqs. (2)–(4) to convert continuum flux to N_H2 and mass; authors note evolved-star dust could differ but adopt ISM law because of deuterated molecules.
  • domain assumption LTE and optically thin (or corrected) emission for rotation diagrams
    Standard formula (Eq. 5) applied to derive T_rot and N_tot for all species (Sect. 4.1).
  • domain assumption Parallax distance 3.80 kpc (Imai et al. 2011)
    Adopted throughout for linear scales and masses; all physical quantities scale with d or d².
  • domain assumption Deuterium is destroyed in stellar interiors and therefore cannot be present in pure circumstellar ejecta
    Used in Sect. 4.2–4.3 to argue that detected deuterated molecules require cold interstellar material.

pith-pipeline@v1.1.0-grok45 · 50225 in / 2839 out tokens · 30276 ms · 2026-07-14T10:37:20.699676+00:00 · methodology

0 comments
read the original abstract

The Nakashima-Deguchi object (NDO; aka IRAS 19312+1950) has been recognized as an enigmatic object, exhibiting characteristics of both an evolved star and a star-forming region. However, the actual nature of this object remains a topic of ongoing debate. We conducted observations of this object in (sub)millimeter continuum and molecular line emission using the IRAM-30m and APEX telescopes as well as the SMA. Based on SED fitting of single-dish continuum observations, we determined that the cloud hosting NDO has a dust temperature of $25\pm2$ K, a source-averaged (24$^{\prime\prime}$) H$_2$ column density of $(4.4\pm 0.6) \times 10^{22}$ cm$^{-2}$, a dust emissivity index of $1.7\pm0.2$, and a total gas mass of $220\pm21 M_{\odot}$. SMA continuum observations resolve the cloud into at least four dust continuum cores. The centrally peaked core MM1, associated with an SiO maser, is the primary mass reservoir. Single-dish spectroscopic observations of NDO led to the detection of 59 spectral lines attributed to 12 species and their isotopologues. This includes the first detection of deuterated molecules, DCO$^{+}$, DCN, DNC, and HDCO, indicating substantial deuterium abundance. SMA spectroscopic observations detected 75 spectral lines toward MM1, assigned to 12 species and their isotopologues. These lines exhibit diverse morphologies on a scale of $\sim$0.1 pc, likely due to outflow feedback. The observed high-velocity outflow is inconsistent with a spherical morphology and rather resembles a wide-angle bipolar outflow. The presence of deuterated species, and the overall large mass of the complex, the surrounding material of NDO appears more naturally associated with a star-forming environment than with a purely evolved-star scenario. Our investigations led us to postulate that this enigmatic object may represent an Orion KL analog about ten times farther away.

Figures

Figures reproduced from arXiv: 2607.10587 by A. Belloche, F. Navarete, F. Schuller, F. Wyrowski, K. M. Menten, P. Schilke, T. Kami\'nski, Y. Gong.

Figure 1
Figure 1. Figure 1: shows the continuum emission of NDO at 1.2 mm and 870 µm. Both distributions reveal that this source is rel￾atively isolated. Gaussian fitting was performed to determine the source sizes and flux densities, and the results are sum￾marized in [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: SED of NDO fitted with a single modified blackbody model shown by the dashed line. The fitted values are indicated in the upper-left corner of this panel, while the two data points at λ <80 µm are excluded from the fitting. 3.1.2. SMA results Figure 3a presents the SMA view of the 1.27 mm contin￾uum emission of NDO. The high-angular-resolution observa￾tions have resolved the isolated structure in [PITH_FU… view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the 236.351 GHz (i.e., 1.27 mm) dust continuum maps of NDO from the SMA-only (left panel) and from the SMA data combined with the IRAM 30m single-dish (SD) data, hereafter SMA+SD (right panel). In both panels, the contours start from 2 mJy beam−1 and increase by 2 mJy beam−1 . The position of the SiO maser (αJ2000, δJ2000)=(19h33m24.s245, 19◦56′55.′′689), taken from Nakashima et al. (2011), i… view at source ↗
Figure 4
Figure 4. Figure 4: Raster maps of HCO+ (3–2), H2CO (30,3-20,2), SO (23– 12), and CH3OH (30-20 A + ) integrated over 33–40 km s−1 . The black dots represent the footprints of the grid. The distribution of each transition is fitted with a two-dimensional Gaussian model which is indicated by the red ellipse in each panel. The beam size is shown in the lower-right corner of each panel. The (0, 0) offset corresponds to (αJ2000=19… view at source ↗
Figure 5
Figure 5. Figure 5: SMA view of detected molecular lines within the frequency range of 190–280 GHz toward MM1. The atmospheric trans￾mission with a precipitable water vapor of 2 mm is shown in orange. Zoom-in plots are provided in Fig. C.1. 4. Discussion 4.1. Molecular column densities and fractional abundances We utilized the rotation-diagram method to estimate the ro￾tational temperatures and column densities of the detecte… view at source ↗
Figure 6
Figure 6. Figure 6: Distribution of the 36 selected molecular transitions observed by the SMA. The maps were integrated from 30 km s−1 to 45 km s−1 . The dust continuum peaks are indicated by the plus symbols, while the SiO maser position is indicated by the circle. The beam size is shown in the lower-left corner of each panel. The fractional abundances of most molecules agree with those in IRAS 16293−2422 and Orion KL within… view at source ↗
Figure 7
Figure 7. Figure 7: UKIRT 2.12 µm image overlaid with the SMA DCN (3– 2) intensity contours integrated over 30 km s−1 to 45 km s−1 . The contours are −3σ, 3σ, 5σ, and 7σ (1σ=0.3 Jy beam−1 km s−1 ). The dust continuum peak is indicated by the plus symbol, while the SiO maser position is indicated by the circle. The beam size is shown in the lower-left corner of each panel. 4.2. Isotope ratios Isotope ratios serve as important … view at source ↗
Figure 8
Figure 8. Figure 8: APEX view of the outflow associated with NDO. Top: Observed CO (2–1), (3–2), and (4–3) spectra extracted at the position corresponding to the beam centered near the crosses shown in the bottom panels. Bottom: CO outflow maps. The blueshifted emission integrated from −40 to 0 km s−1 is shown in blue contours. For CO (2–1), the contours start at 1 K km s−1 , and increase by 1 K km s−1 . For CO (3–2), the con… view at source ↗
Figure 9
Figure 9. Figure 9: Overview of the outflow associated with NDO. Left: UKIRT continuum-subtracted 2.12 µm H2 v= 1−0 S(1) image overlaid with the extremely redshifted and blueshifted CO (2–1) lobes. The redshifted lobe, shown in the red contours, is the CO (2–1) intensity map integrated from 60 to 100 km s−1 , while the blueshifted lobe, shown in the blue contours, is the CO (2–1) intensity map integrated from −40 to 0 km s−1 … view at source ↗
Figure 10
Figure 10. Figure 10: Position-velocity diagrams of the SMA+APEX CO (2–1) emission along the cuts indicated by the two orange arrows in the left panel of [PITH_FULL_IMAGE:figures/full_fig_p013_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Comparison of molecular abundances of NDO with those in IRAS 16293−2422 and Orion KL (e.g., Blake et al. 1987, 1994; van Dishoeck et al. 1995; Caux et al. 2011; Tercero et al. 2011). The red and blue points indicate the abundances of NDO measured on 0.4 pc and 0.06 pc scales, respectively. Abundances of the same molecule measured on different scales are connected with black dotted lines. The pink-shaded r… view at source ↗

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

249 extracted references · 84 canonical work pages · 37 internal anchors

  1. [1]

    , keywords =

    The Bubbling Galactic Disk. , keywords =. doi:10.1086/507015 , adsurl =

    doi:10.1086/507015

  2. [2]

    , keywords =

    Stellar Yields from Metal-rich Asymptotic Giant Branch Models. , keywords =. doi:10.3847/0004-637X/825/1/26 , archivePrefix =. 1604.02178 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/0004-637x/825/1/26

  3. [3]

    The near-infrared reflected spectrum of source I in Orion-KL

    The near-infrared reflected spectrum of source I in Orion-KL. , keywords =. doi:10.1051/0004-6361/201014497 , archivePrefix =. 1006.0241 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201014497

  4. [4]

    , keywords =

    The galactic gas-to-dust ratio from observations of eighty-one globular clusters. , keywords =

  5. [5]

    A survey of interstellar H I from Lalpha absorption measurements. II. , keywords =. doi:10.1086/156357 , adsurl =

    doi:10.1086/156357

  6. [6]

    The Bubbling Galactic Disk. II. The Inner 20. , keywords =. doi:10.1086/521646 , adsurl =

    doi:10.1086/521646

  7. [7]

    Astronomical Data Analysis Software and Systems XVI , year = 2007, editor =

    CASA Architecture and Applications. Astronomical Data Analysis Software and Systems XVI , year = 2007, editor =

    2007

  8. [8]

    , keywords =

    Global collapse of molecular clouds as a formation mechanism for the most massive stars. , keywords =. doi:10.1051/0004-6361/201321318 , archivePrefix =. 1307.2590 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201321318

  9. [9]

    ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- XV. Steady Accretion from Global Collapse to Core Feeding in Massive Hub-filament System SDC335

    ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions - XV. Steady accretion from global collapse to core feeding in massive hub-filament system SDC335. , keywords =. doi:10.1093/mnras/stad012 , archivePrefix =. 2301.01895 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad012

  10. [10]

    , keywords =

    One Percent Determination of the Primordial Deuterium Abundance. , keywords =. doi:10.3847/1538-4357/aaab53 , archivePrefix =. 1710.11129 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-4357/aaab53

  11. [11]

    Reviews of Modern Physics , keywords =

    Big bang nucleosynthesis: Present status. Reviews of Modern Physics , keywords =. doi:10.1103/RevModPhys.88.015004 , archivePrefix =. 1505.01076 , primaryClass =

    Pith/arXiv arXiv doi:10.1103/revmodphys.88.015004

  12. [12]

    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 ...

    doi:10.1126/sciadv.ady6953 2025

  13. [13]

    SiO maser astrometry of the red transient V838 Monocerotis

    SiO maser astrometry of the red transient V838 Monocerotis. , keywords =. doi:10.1051/0004-6361/202037712 , archivePrefix =. 2004.01488 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/202037712 2004

  14. [14]

    On massive dust clumps in the envelope of the red supergiant VY Canis Majoris

    Massive dust clumps in the envelope of the red supergiant VY Canis Majoris. , keywords =. doi:10.1051/0004-6361/201935408 , archivePrefix =. 1903.09558 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201935408 1903

  15. [15]

    First VLBI Imaging of SiO $v=0$, $J=1 \rightarrow 0$ Masers in VY Canis Majoris

    First VLBI imaging of SiO v = 0, J = 1 0 masers in VY Canis Majoris. , keywords =. doi:10.1093/pasj/psaf013 , archivePrefix =. 2503.05250 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/pasj/psaf013

  16. [16]

    VLBA imaging of the 3mm SiO maser emission in the disk-wind from the massive protostellar system Orion Source I

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201731548

  17. [17]

    Imaging the Ionized Disk of the High-Mass Protostar Orion-I

    Imaging the Ionized Disk of the High-Mass Protostar Orion I. , keywords =. doi:10.1086/518929 , archivePrefix =. 0704.2309 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1086/518929

  18. [18]

    A Feature Movie of SiO Emission 20-100 AU from the Massive Young Stellar Object Orion Source I

    A Feature Movie of SiO Emission 20-100 AU from the Massive Young Stellar Object Orion Source I. , keywords =. doi:10.1088/0004-637X/708/1/80 , archivePrefix =. 0911.2473 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/708/1/80

  19. [19]

    870 um observations of evolved stars with LABOCA

    870 m observations of evolved stars with LABOCA. , keywords =. doi:10.1051/0004-6361/200913147 , archivePrefix =. 1001.2098 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/200913147 2098

  20. [20]

    Journal of Astronomical Instrumentation , keywords =

    SWARM: A 32 GHz Correlator and VLBI Beamformer for the Submillimeter Array. Journal of Astronomical Instrumentation , keywords =. doi:10.1142/S2251171716410063 , archivePrefix =. 1611.02596 , primaryClass =

    Pith/arXiv arXiv doi:10.1142/s2251171716410063

  21. [21]

    Maser Investigation toward Off-Plane Stars (MIOPS): detection of SiO masers in the Galactic thick disk and halo

    Maser Investigation toward Off-Plane Stars (MIOPS): detection of SiO masers in the Galactic thick disk and halo. arXiv e-prints , keywords =. doi:10.48550/arXiv.2310.13489 , archivePrefix =. 2310.13489 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2310.13489

  22. [22]

    , keywords =

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

    doi:10.1086/307195

  23. [23]

    , year = 2009, month = sep, volume =

    Complex Organic Interstellar Molecules. , year = 2009, month = sep, volume =. doi:10.1146/annurev-astro-082708-101654 , adsurl =

    doi:10.1146/annurev-astro-082708-101654 2009

  24. [24]

    , year = 1974, month = jun, volume =

    Aperture Synthesis with a Non-Regular Distribution of Interferometer Baselines. , year = 1974, month = jun, volume =

    1974

  25. [25]

    , keywords =

    Ammonia from cold high-mass clumps discovered in the inner Galactic disk by the ATLASGAL survey. , keywords =. doi:10.1051/0004-6361/201118107 , archivePrefix =. 1208.4848 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201118107

  26. [26]

    The HI/OH/Recombination line survey of the inner Milky Way (THOR): data release 2 and HI overview

    The HI/OH/Recombination line survey of the inner Milky Way (THOR): data release 2 and H I overview. , keywords =. doi:10.1051/0004-6361/201937095 , archivePrefix =. 1912.08223 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201937095 1912

  27. [27]

    , keywords =

    The Submillimeter Array. , keywords =. doi:10.1086/423245 , archivePrefix =. astro-ph/0406352 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/423245

  28. [28]

    , keywords =

    Weeds: a CLASS extension for the analysis of millimeter and sub-millimeter spectral surveys. , keywords =. doi:10.1051/0004-6361/201015487 , archivePrefix =. 1012.1747 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201015487

  29. [29]

    The Cologne Database for Molecular Spectroscopy, CDMS, in the Virtual Atomic and Molecular Data Centre, VAMDC

    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 =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1016/j.jms.2016.03.005 2016

  30. [30]

    Handbook of Isotopes in the Cosmos

  31. [31]

    , keywords =

    Submillimeter, millimeter and microwave spectral line catalog. , keywords =. doi:10.1016/S0022-4073(98)00091-0 , adsurl =

    doi:10.1016/s0022-4073(98)00091-0

  32. [32]

    , keywords =

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

    Pith/arXiv arXiv doi:10.1086/670067

  33. [33]

    Communications in Applied Mathematics and Computational Science , keywords =

    Ensemble samplers with affine invariance. Communications in Applied Mathematics and Computational Science , keywords =. doi:10.2140/camcos.2010.5.65 , adsurl =

    doi:10.2140/camcos.2010.5.65 2010

  34. [34]

    Hunter, J. D. , Title =. Computing in Science & Engineering , Volume =

  35. [35]

    Jones, Eric and Oliphant, Travis and Peterson, Pearu and others , biburl =

  36. [36]

    , archivePrefix = "arXiv", eprint =

    Astropy: A community Python package for astronomy. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201322068 , adsurl =

    doi:10.1051/0004-6361/201322068

  37. [37]

    SF2A-2015: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics , year = 2015, month = dec, pages =

    CASSIS: a tool to visualize and analyse instrumental and synthetic spectra. SF2A-2015: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics , year = 2015, month = dec, pages =

    2015

  38. [38]

    Computing in Science Engineering , title=

    S. Computing in Science Engineering , title=. 2011 , volume=. doi:10.1109/MCSE.2011.37 , ISSN=

    doi:10.1109/mcse.2011.37 2011

  39. [39]

    APLpy: Astronomical Plotting Library in Python. 2012

    2012

  40. [40]

    corner.py: Scatterplot matrices in Python , Journal =

    Daniel Foreman-Mackey , Doi =. corner.py: Scatterplot matrices in Python , Journal =

  41. [41]

    , archivePrefix = "arXiv", eprint =

    Molecular Rings Around Interstellar Bubbles and the Thickness of Star-Forming Clouds. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/709/2/791 , adsurl =

    doi:10.1088/0004-637x/709/2/791

  42. [42]

    GLIMPSE. I. An SIRTF Legacy Project to Map the Inner Galaxy. , eprint =. doi:10.1086/376696 , adsurl =

    doi:10.1086/376696

  43. [43]

    , archivePrefix = "arXiv", eprint =

    The environment of the infrared dust bubble N65: a multiwavelength study. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/200913617 , adsurl =

    work page doi:10.1051/0004-6361/200913617

  44. [44]

    The nature of the bubbles observed by Spitzer and what ATLASGAL tells us about the surrounding neutral material

    A gallery of bubbles. The nature of the bubbles observed by Spitzer and what ATLASGAL tells us about the surrounding neutral material. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201014422 , adsurl =

    doi:10.1051/0004-6361/201014422

  45. [45]

    , archivePrefix = "arXiv", eprint =

    Infrared Dust Bubbles: Probing the Detailed Structure and Young Massive Stellar Populations of Galactic H II Regions. , archivePrefix = "arXiv", eprint =. doi:10.1086/588005 , adsurl =

    doi:10.1086/588005

  46. [46]

    First results for N49 from the Herschel infrared survey of the Galactic plane

    Star formation triggered by H II regions in our Galaxy. First results for N49 from the Herschel infrared survey of the Galactic plane. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361/201014587 , adsurl =

    doi:10.1051/0004-6361/201014587

  47. [47]

    , archivePrefix = "arXiv", eprint =

    A Catalog of Extended Green Objects in the GLIMPSE Survey: A New Sample of Massive Young Stellar Object Outflow Candidates. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-6256/136/6/2391 , adsurl =

    doi:10.1088/0004-6256/136/6/2391

  48. [48]

    High-resolution radio continuum and methanol maser survey

    Studies of ultracompact HII regions - II. High-resolution radio continuum and methanol maser survey. , keywords =. doi:10.1046/j.1365-8711.1998.02014.x , adsurl =

    doi:10.1046/j.1365-8711.1998.02014.x 1998

  49. [49]

    , eprint =

    Photoionizing feedback in star cluster formation. , eprint =. doi:10.1111/j.1365-2966.2005.08806.x , adsurl =

    doi:10.1111/j.1365-2966.2005.08806.x 2005

  50. [50]

    , archivePrefix = "arXiv", eprint =

    Resolution of the Distance Ambiguity for Galactic H II Regions. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/690/1/706 , adsurl =

    doi:10.1088/0004-637x/690/1/706

  51. [51]

    , keywords =

    Sequential formation of subgroups in OB associations. , keywords =. doi:10.1086/155302 , adsurl =

    doi:10.1086/155302

  52. [52]

    Triggered massive-star formation on the borders of Galactic H II regions. I. A search for ``collect and collapse'' candidates. , eprint =. doi:10.1051/0004-6361:20041946 , adsurl =

    doi:10.1051/0004-6361:20041946

  53. [53]

    , keywords =

    MIPSGAL: A Survey of the Inner Galactic Plane at 24 and 70 m. , keywords =. doi:10.1086/596581 , adsurl =

    doi:10.1086/596581

  54. [54]

    , archivePrefix = "arXiv", eprint =

    The Bolocam Galactic Plane Survey: Survey Description and Data Reduction. , archivePrefix = "arXiv", eprint =. doi:10.1088/0067-0049/192/1/4 , adsurl =

    doi:10.1088/0067-0049/192/1/4

  55. [55]

    , eprint =

    The VLA Galactic Plane Survey. , eprint =. doi:10.1086/505940 , adsurl =

    doi:10.1086/505940

  56. [56]

    , keywords =

    MAGPIS: A Multi-Array Galactic Plane Imaging Survey. , keywords =. doi:10.1086/503253 , adsurl =

    doi:10.1086/503253

  57. [57]

    , keywords =

    The NRAO VLA Sky Survey. , keywords =. doi:10.1086/300337 , adsurl =

    doi:10.1086/300337

  58. [58]

    , keywords =

    The Preferential Formation of High-Mass Stars in Shocked Interstellar Gas Layers. , keywords =

  59. [59]

    , archivePrefix = "arXiv", eprint =

    Clustered and Triggered Star Formation in W5: Observations with Spitzer. , archivePrefix = "arXiv", eprint =. doi:10.1086/592322 , adsurl =

    work page doi:10.1086/592322

  60. [60]

    , archivePrefix = "arXiv", eprint =

    Toward Understanding Massive Star Formation. , archivePrefix = "arXiv", eprint =. doi:10.1146/annurev.astro.44.051905.092549 , adsurl =

    Pith/arXiv arXiv doi:10.1146/annurev.astro.44.051905.092549

  61. [61]

    Origins , year = 1998, series =

    Observations and Theory of Dynamical Triggers for Star Formation. Origins , year = 1998, series =. arXiv:astro-ph/9712352 , editor =

    Pith/arXiv arXiv 1998

  62. [64]

    IEEE Transactions on Terahertz Science and Technology , eprint =

    Development of Superconducting Spectroscopic Array Receiver: A Multibeam 2SB SIS Receiver for Millimeter-Wave Radio Astronomy. IEEE Transactions on Terahertz Science and Technology , eprint =. doi:10.1111/j.1365-2966.2006.11368.x , adsurl =

    doi:10.1111/j.1365-2966.2006.11368.x 2006

  63. [65]

    , year = 2011, month = oct, volume = 35, pages =

    A Research on the Gravity Deformation of Delingha 13.7m Telescope. , year = 2011, month = oct, volume = 35, pages =. doi:10.1016/j.chinastron.2011.10.011 , adsurl =

    work page doi:10.1016/j.chinastron.2011.10.011 2011

  64. [66]

    Triggered massive-star formation on the borders of Galactic H II regions. IV. Star formation at the periphery of Sh2-212. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361:20079233 , adsurl =

    doi:10.1051/0004-6361:20079233

  65. [67]

    Triggered massive-star formation on the borders of Galactic H II regions. II. Evidence for the collect and collapse process around RCW 79. , eprint =. doi:10.1051/0004-6361:20053952 , adsurl =

    doi:10.1051/0004-6361:20053952

  66. [68]

    Triggered massive-star formation on the borders of Galactic H II regions. III. Star formation at the periphery of Sh2-219. , eprint =. doi:10.1051/0004-6361:20054641 , adsurl =

    doi:10.1051/0004-6361:20054641

  67. [69]

    , archivePrefix = "arXiv", eprint =

    Triggered star formation on the borders of the Galactic H ii region RCW 120. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361:20077474 , adsurl =

    doi:10.1051/0004-6361:20077474

  68. [70]

    , keywords =

    A 13CO Survey of Molecular Clouds in Gemini and Auriga. , keywords =. doi:10.1086/313119 , adsurl =

    doi:10.1086/313119

  69. [71]

    , keywords =

    A new look at the dark cloud L1251: Sensitive observations of the molecular emission. , keywords =. doi:10.1086/174813 , adsurl =

    work page doi:10.1086/174813

  70. [72]

    Tools of Radio Astronomy, by Thomas L

    Tools of Radio Astronomy. Tools of Radio Astronomy, by Thomas L. Wilson; Kristen Rohlfs and Susanne H. doi:10.1007/978-3-540-85122-6 , adsurl =

    doi:10.1007/978-3-540-85122-6

  71. [73]

    astro-ph.GA

    Triggered Star Formation. EAS Publications Series , year = 2011, series =. doi:10.1051/eas/1151004 , adsurl =. arXiv:1101.3112 , primaryClass = "astro-ph.GA", editor =

    doi:10.1051/eas/1151004 2011

  72. [74]

    The Physics and Chemistry of the Interstellar Medium, by A

    The Physics and Chemistry of the Interstellar Medium. The Physics and Chemistry of the Interstellar Medium, by A. G. G. M. Tielens, pp. . ISBN 0521826349. Cambridge, UK: Cambridge University Press, 2005. , year = 2005, month = sep, adsurl =

    2005

  73. [75]

    The Green Bank Telescope H II Region Discovery Survey. III. Kinematic Distances. , archivePrefix = "arXiv", eprint =. doi:10.1088/0004-637X/754/1/62 , adsurl =

    doi:10.1088/0004-637x/754/1/62

  74. [76]

    , keywords =

    Pressure-confined clumps in magnetized molecular clouds. , keywords =. doi:10.1086/171638 , adsurl =

    doi:10.1086/171638

  75. [77]

    , keywords =

    Dust opacities for protostellar cores. , keywords =

  76. [78]

    The Green Bank Telescope H II Region Discovery Survey. II. The Source Catalog. , archivePrefix = "arXiv", eprint =. doi:10.1088/0067-0049/194/2/32 , adsurl =

    doi:10.1088/0067-0049/194/2/32

  77. [79]

    , archivePrefix = "arXiv", eprint =

    Triggered star formation on the borders of the Galactic Hii region RCW 82. , archivePrefix = "arXiv", eprint =. doi:10.1051/0004-6361:200811050 , adsurl =

    work page doi:10.1051/0004-6361:200811050

  78. [80]

    The Bolocam Galactic Plane Survey. II. Catalog of the Image Data. , archivePrefix = "arXiv", eprint =. doi:10.1088/0067-0049/188/1/123 , adsurl =

    doi:10.1088/0067-0049/188/1/123

  79. [81]

    , keywords =

    A Spatially Complete \^ 13CO J = 1-0 Survey of the Orion A Cloud. , keywords =. doi:10.1086/300392 , adsurl =

    work page doi:10.1086/300392

  80. [82]

    , keywords =

    The structure and dynamics of NGC 1333 from \^ 13\^ CO and C\^ 18\^ O observations. , keywords =

Showing first 80 references.