Yusuke Aso (KASI) Time-dependent Monte Carlo continuum radiative transfer A. Bensberg® and S. Wolf変光現象は円盤内のダストの温度を変化させる。ダストの非平衡加熱冷却をモンテカルロ輻射輸送で扱う方法がない。→POLARISを拡張する。光度を吸収し、比熱で加熱が決まる。温度Tでエンタルピーを失う時間tc。時間ステップが<<t であれば吸収と放射のバランスで次のエンタルピーが決まる。ステップ毎に温度と散乱はstationary POLARIS。しかし、ステップ毎に画像を作るために光子を読み書きはしない。 c/Δtまでの光線の総輝度を輻射輸送方程式をRunge-Kutta-Fehlbergで解いて保存し、検出器までの残り道程はτで減らすだけで画像にする。前の温度の結果が届くものは今の温度で解いたものに足される。ステップ幅Δtとステップ当りの光子数Nphの影響を調べる。 Nph=103, 105sまでtcを過ぎると放射がないことになる。高温だと冷えやすい。 Δt=2s τが薄いと吸収イベントが見逃されるか、1回で大量にエネルギーが吸収される。冪乗円盤でstationaryと比較。Δt=8s, Nph=105。
τ=0.01で5000sで平衡に達するところ最初の10000sだけ光度を4倍。 １ステップで平衡温度に達し、不連続な高温部が見える。散乱、再放射の光度曲線。傾いていると観測者に向いた散乱が多い。 near/far sideからの時間差でバースト時間が膨らむ。再放射のピークは傾きに依らない。この論文の方法は数時間から数週間のバーストに最適。
Jenny K. Calahan © ¹ ✉, Edwin A. Bergin ® ¹, Arthur D. Bosman ¹, Evan A. Rich ¹, Sean M. Andrews², Jennifer B. Bergner Ø³, L. Ilsedore Cleeves 4 , Viviana V. Guzmán 5,6, Jane Huang 1, John D. Ilee ® 7, Charles J. Law 2, Romane Le Gal 8.9.10 , Karin I. Öberg Ø², Richard Teague ¹¹, Catherine Walsh Ø², David J. Wilner O² & Ke Zhang 12 D円盤には>1 mmのペブルとガップルする<10 μmのダスト。ペブルの組成が惑星コアの組成。惑星の大気になる赤道面のガスは厚いダストと低温で観測できない。 © CH 3 CN, HC 3 Nは前生命分子。 ° CH 3 CNはJ毎のK laddarで温度が分かり25-50 K。低温での有機分子生成のためにダスト表面反応が取り入れられるも光蒸発率が足りない。 →C/O比が上がり（観測も支持）、UVが入って（小さいダストとガスが減れば可能）光化学平衡という新しい化学を提案。その結果できるC₂H, CH₃CNは惑星大気形成段階を見せる。 Molecules with ALMA at Planet-forming Scales (MAPS)が支持。 1-2 MyrのIM LupにCH 3 CN, HC 3 N無し。 1-2 MyrのAS 209はCH 3 CN, HC 3 Nはz/r>0.1から。 >6 MyrのものはCH₃CNが赤道面（K ladder温度とモデルから）。低温高密度でCH 3 CN存在量を計算すると、g/d比と初期ガスC存在量に敏感。 exp tail円盤で密度温度を与えて、小さいダスト（1 μm）と大きいダスト（1 mm）でHD163296とTW HyaのCH 3 CN, HCN, HC 3 Nを再現。小さいダストを減らして、Cも増やす（ベストは小さいダストを10倍減らしてC/O=1-2）。化学進化を1 Myr走らせて平衡にして、UV光化学平衡へ。ガス化学はUMIST, Rate12。円盤では太陽系より高いC/O比が観測されており、そこから系外ガス惑星のC/O>1を説明できる。 1 Myrまでは宇宙線とX線が赤道面の化学を決め、その後は考えられていたよりUVが決める。 UVが入って来るとイオンも増えて、磁気回転不安定領域も増えて、進化した円盤の質量降着に繋がるかも。磁気回転不安定領域の違いThe JCMT BISTRO-2 Survey: Magnetic Fields of the Massive DR21 Filament V Tao-Chung Ching 1,2,93 © , Keping Qiu 2,5,6 © , Zhiyuan Ren 2 © , Shih-Ping Lai 7:8 © , David Ben低密度では磁場はフィラメントに並行、高密度では垂直うフDR21,長さ4 pc,重さ15000 Msun, đ≒1.4 kpc, 24個の大質量コア,収縮流,大σ~3 mJy/beam, I/δl>3, p/δβ$3, δρ<4%, θ=14",老ヴメントは90°回転送浅いα=0.3。構造関数解析角分散関数：角度の違いΔΦ vs  2点距離λ大スケール成分と乱流成分の比がわかる。 1 − 〈cos [ΔΦ(l)]〉 ~ − b 〈Br〉 × [1 − e−l²/2(δ²+2w²)」+ ∑ a'ji²¹，j=1まで(8² + 2W²)△′速度分散はH¹³CO+ 1-0 Ncell = √2π δ³ δB Δ':雲の厚さ, W:ビーム, δ:相関長, a:非乱流の係数, Δ'と<B>比は縮退する。 λ = 7.6 × 10−²¹[N(H₂)/cm−²][B/μG]− mass-to-fluxԷԷλフィラメントではλ>2で重力優勢。薄い部分ではλ~1→重力だけでは集まらない。一方で、強い磁場に沿って質量が集まりフィラメントを形成。サブフィラメントを通って重力優勢へ。右上がりだとするとフィラメントに整列する磁場からコア周りの複雑な磁場への遷移。
M. Agúndez¹©, C. Cabezas¹©, N. Marcelino²,³©, R. Fuentetaja¹©, B. Tercero²,³©, P. de Vicente³, and J. Cernicharo¹© The previous detection of two species related to the nonpolar molecule cyanogen (NCCN), its protonated form (NCCNH*) and one metastable isomer (CNCN), in cold dense clouds supported the hypothesis that dicyanopolyynes are abundant in space. Here we report the first identification in space of NC 4 NH + . This cation is the protonated form of NC 4 N, which is the second member of the series of dicyanopolyynes after NCCN. The detection was based on the observation of six harmonically related lines within the Yebes 40m line survey of TMC-1 QUIJOTE. The six lines can be fitted to a rotational constant B = 1293.90840 ± 0.00060 MHz and a centrifugal distortion constant D = 28.59 ± 1.21 Hz. We confidently assign this series of lines to NC 4 NH + based on high-level ab initio calculations, which supports the previous identification of HC 3 NH + from the observation of a series of lines with a rotational constant 2 MHz lower than that derived here. The column density of NC 4 NH + in TMC-1 is (1.1 ± ) × 10 10 cm −2 , which implies that NC 4 NH* is eight times less abundant than NCCNH*. The species CNCN, previously reported toward L483 and tentatively in TMC-1, is confirmed in this latter source. We estimate that NCCN and NC 4 N are present in TMC-1 with abundances a few times to one order of magnitude lower than HC 3 N and HC 5 N, respectively. This means that dicyanopolyynes NC−(CC),−CN are present at a lower level than the corresponding monocyanopolyynes HCC−(CC),,−CN. The reactions of the radicals CN and C 3 N with HNC arise as the most likely formation pathways to NCCN and NC 4 N in cold dense clouds.ジシアノポリンが多い。新たな例。Yebes 40m, TMC-1キホーテサーベイ。 NCCCCNH+はNCCNH+より8倍少ない。NCCNとNCCCCNは桁で少ない。ジシアノポリンはモノシアノポリンより少ないことを示唆。
Sota Arakawa¹,²© and Eiichiro Kokubo²© The Sun is thought to have been formed within a star cluster. The coexistence of 26 Al-rich and 26 Al-poor calcium–aluminum-rich inclusions indicates that a direct injection of 26 Al-rich materials from a nearby core-collapse supernova would be expected to occur in the first 10 5 years of the existence of the Solar System. Therefore, at least one core-collapse supernova ought to occur within the duration of star formation in the Sun’s birth cluster. Here, we revisit the number of stars in the Sun’s birth cluster from the point of view of the probability of experiencing at least one core-collapse supernova within the finite duration of star formation within the birth cluster. We find that the number of stars in the birth cluster may be significantly greater than that previously considered, depending on the duration of star formation. 26Alリッチな物質は10^5年内の核収縮超新星爆発から。太陽がいる星団の星を数えて超新星爆発の経験確率を求める。考えられていたよりも多い。 RYAN D. BOYDEN¹ AND JOSH EISNER¹ The stellar cluster environment is expected to play a central role in the evolution of circumstellar disks. We use thermochemical modeling to constrain the dust and gas masses, disk sizes, UV and X-ray radiation fields, viewing geometries, and central stellar masses of 20 Class II disks in the Orion Nebula Cluster (ONC). We fit a large grid of disk models to 350 GHz continuum, CO J = 3 − 2, and HCO+ J = 4 − 3 ALMA observations of each target, and we introduce a procedure for modeling interferometric observations of gas disks detected in absorption against a bright molecular cloud background.  We find that the ONC disks are massive and compact, with typical radii < 100 AU, gas masses ≥ 10− 3 M ⊙ , and gas-to-dust ratios ≥ 100. The ISM-like gas-to-dust ratios derived from our modeling suggest that compact, externally-irradiated disks in the ONC are less prone to gas-phase CO depletion than the massive and extended gas disks that are commonly found in nearby low- mass star-forming regions.  The presence of massive gas disks indicates that external photoevaporation may have only recently begun operating in the ONC, though it remains unclear whether other cluster members are older and more evaporated than the ones in our sample.  Finally, we compare our dynamically-derived stellar masses with the stellar masses predicted from evolutionary models and find excellent agreement.  Our study has significantly increased the number of dynamical mass measurements in the mass range ≤ 0.5 M Ω , demonstrating that the ONC is an ideal region for obtaining large samples of dynamical mass measurements towards low-mass M-dwarfs.オリオン星雲クラスターのClass II円盤の種々の量を求める。ALMA, CO 3-2, HCO+ 4-3。 r<100 au, Mgas>10^–3 Msun, g/d>100。ガスCOがdepleteしていない。外からの光蒸発は最近始まった。力学的に求められた質量と進化モデルは一致。
The Star Formation History of the Milky Way’s Nuclear Star Cluster
Zhuo Chen 1 ©, Tuan Do 1 ©, Andrea M. Ghez 1 ©, Matthew W. Hosek, Jr. 1 ,4 ©, Anja Feldmeier-Krause 2 ©, Devin S. Chu 1 ©, Rory O. Bentley 1 ©, Jessica R. Lu 3 ©, and Mark R. Morris 1 © We report the first star formation history study of the Milky Ways nuclear star cluster (NSC), which includes observational constraints from a large sample of stellar metallicity measurements. These metallicity measurements were obtained from recent surveys from Gemini and the Very Large Telescope of 770 late-type stars within the central 1.5 pc. These metallicity measurements, along with photometry and spectroscopically derived temperatures, are forward modeled with a Bayesian inference approach. Including metallicity measurements improves the overall fit quality, as the low-temperature red giants that were previously difficult to constrain are now accounted for, and the best fit favors a two-component model. The dominant component contains 93% ± 3% of the mass, is metal-rich ([M/H] ～ 0.45), and has an age of 5 ±³ Gyr, which is ～3 Gyr younger than earlier studies with fixed (solar) metallicity; this younger age challenges coevolutionary models in which the NSC and supermassive black holes formed simultaneously at early times. The minor population component has low metallicity ([M/H] ～ − 1.1) and contains 〜7% of the stellar mass. The age of the minor component is uncertain (0.1–5 Gyr old). Using the estimated parameters, we infer the following NSC stellar remnant population (with ～18% uncertainty): 1.5 × 10³ neutron stars, 2.5 × 10° stellar-mass black holes (BHs), and 2.2 × 10° BH–BH binaries. These predictions result in 2–4 times fewer neutron stars compared to earlier predictions that assume solar metallicity, introducing a possible new path to understand the so-called "missing-pulsar problem". Finally, we present updated predictions for the BH–BH merger rates (0.01–3 Gpc-³yr-¹). Gemini, VLT, 770後期星,銀河系中心1.5 pc以内,金属量測定。金属量測定によって、今までできなかった低温赤色巨星のモデルフィットが可能に。質量で93％が金属リッチで5 Gyr。この若い年齢は銀河系核星団と中心のブラックホールの共進化に疑問を呈する。missing-pulsar問題の解決の糸口。
Making the Solar System
John Chambers © We model the early stages of planet formation in the solar system, including continual planetesimal formation, and planetesimal and pebble accretion onto planetary embryos in an evolving disk driven by a disk wind. The aim is to constrain aspects of planet formation that have large uncertainties by matching key characteristics of the solar system. The model produces a good fit to these characteristics for a narrow range of parameter space. Planetary growth beyond the ice line is dominated by pebble accretion. Planetesimal accretion is more important inside the ice line. Pebble accretion inside the ice line is slowed by higher temperatures, partial removal of inflowing pebbles by planetesimal formation and pebble accretion further out in the disk, and increased radial velocities due to gas advection. The terrestrial planets are prevented from accreting much water ice because embryos beyond the ice line reach the pebble-isolation mass before the ice line enters the terrestrial-planet region. When only pebble accretion is considered, embryos typically remain near their initial mass or grow to the pebble-isolation mass. Adding planetesimal accretion allows Mars-sized objects to form inside the ice line, and allows giant-planet cores to form over a wider region beyond the ice line. In the region occupied by Mercury, pebble Stokes numbers are small. This delays the formation of embryos and stunts their growth, so that only low-mass planets can form here.太陽系の初期惑星形成。円盤風に駆動される微惑星形成と微惑星ペブル降着。惑星形成に関わる量を精密に制限。氷線の外ではペブル降着、中では微惑星降着。中側のペブル降着は、高温と微惑星形成によって抑制される。氷線が地球型惑星領域に入る前にペブル孤立質量に達するために地球型惑星は水の氷を集められない。微惑星形成を考えることで氷線以内の火星サイズ惑星や広い領域での巨大惑星コアができる。
Length-scales and dynamics of Carina's Western wall
Turlough P. Downes ®,¹* Patrick Hartigan 2 and Andrea Isella 2 We present a variety of analyses of the turbulent dynamics of the boundary of a photodissociation region (PDR) in the Carina Nebula using high resolution ALMA observations. Using principal component analysis, we suggest that the turbulence in this molecular cloud is driven at large scales. Analysis of the centroid velocity structure functions indicate that the turbulence is dominated by shocks rather than local (in k-space) transport of energy. We further find that length-scales in the range 0.02– 0.03 pc are important in the dynamics of this cloud and this finding is supported by analysis of the dominant emission structure length-scale. These length-scales are well resolved by the observational data and we conclude that the apparent importance of this range of scales is physical in origin. Given that it is also well within the range strongly influenced by ambipolar diffusion, we conclude that it is not primarily a product of turbulence alone, but is more likely to be a result of the interplay between gravity and turbulence. Finally, through comparison of these results with previous observations of H 2 emission from the Western Wall, we demonstrate that observations of a PDR can be used to probe the internal structure of the undisturbed portion of a molecular cloud.カリーナ星雲のPDRの境界での乱流をALMAで解析。PCAはラージスケールが乱流を駆動することを示す。重心速度構造関数は乱流が衝撃波に支配されていると示す。支配構造長解析は0.02-0.03 pcが重要と示す。ambipolar diffusionの範囲でもあるので、乱流と重力が影響。 Discovery of a New Molecular Bubble–Outflow Structure in the Taurus B18 Cloud Yan Duan¹-²©, Di L i¹-³-4©, Paul F. Goldsmith 5©, Laurent Paganı 6©, Tao-Chung Ching¹-7©, Shu Liu¹ ©, Jinjin Xie 8 ©, and Chen Wang 1 O Star formation can produce bubbles and outflows, as a result of stellar feedback. Outflows and bubbles inject momentum and energy into the surrounding interstellar medium, and so are related to the overall energy balance of the molecular cloud. Molecular bubbles can be resolved by higher-resolution radio telescopes to quantify the effect of star formation on molecular clouds. We report here the identification of a new molecular bubble with an outflow, and a Herbig–Haro object, HH 319, located at the bubble center. Multiwavelength data have been utilized to study its spatial structure, energy injection, and dynamical timescale. This bubble has a kinetic energy of 5.8 × 10 43 erg within the smallest radius of a bubble in Taurus, 0.077 pc. The bubble formed ～70,000 yr ago. According to the proper-motion velocities of protostars from Gaia EDR3, the T Tauri binary stars (FY Tau and FZ Tau) at the southwest edge of the bubble may have produced the outflow–bubble structure. This is an unusual new structure found in low- and intermediate-mass star formation regions. Only a bubble in Orion A, driven by V380 Ori, has a similar structure. The bubble–outflow structure provides additional observational evidence for the theory of stellar wind from T Tauri stars. It enhances our understanding of how stellar feedback acts on molecular clouds.星からのフィードバックでバブルとアウトフロー。HH319の新しいバブル。 5.8e48 erg, 0.077 pc, 70,000年前に形成。FY Tau, FZ Tauが作ったか。バブル観測はT Tauriの星風理論を検証したり、分子雲へのフィードバックを理解したりできる。
Riccardo Franceschi 1 , Tilman Birnstiel 2, 3 , Thomas Henning 1 , Anirudh Sharma 2 Context. Observations of protoplanetary disks provide information on planet formation and the reasons for the diversity of planetary systems. The key to understanding planet formation is the study of dust evolution from small grains to pebbles. Smaller grains (~ 1 μm) are well-coupled to the gas dynamics, and their distribution is significantly extended above the disk midplane. Larger grains settle much faster and are efficiently formed only in the midplane. By combining near-infrared polarized light and millimeter observations, it is possible to constrain the spatial distribution of both the small and large grains. Aims. We aim to construct detailed models of the size distribution and vertical/radial structure of the dust particles in protoplanetary disks based on observational data. In particular, we are interested in recovering the dust distribution in the IM Lup protoplanetary disk. Methods. We create a physical model for the dust distribution of protoplanetary disks. We then simulate the radiative transfer of the millimeter continuum and the near-infrared polarized radiation. Using a Markov chain Monte Carlo method, we compare the derived images to the observations available for the IM Lup disk to constrain the best physical model for IM Lup and to recover the vertical grain size distribution. Results. The millimeter and near-infrared emission tightly constrain the dust mass and grain size distribution of our model. We find size segregation in the dust distribution, with millimeter-sized grains in the disk midplane. These grains are efficiently formed in the disk, possibly by sedimentation-driven coagulation, in accord with the short settling timescales predicted by our model. This also suggests a high dust-to-gas ratio at smaller radii in the midplane, possibly triggering streaming instabilities and planetesimal formation in the inner disk. We obtain a turbulent α parameter of 3 × 10 − 3 .惑星系の多様性。赤外偏光とミリ波でIM Lup円盤の大小のダストの空間分布。輻射輸送、MCMCで物理量決定。ミリメートル粒子は赤道面にあり、sedimentation-driven凝縮を示唆。内側の赤道面ではg/dが高い可能性も示唆し、ストリーミング不安定で惑星形成を誘発。 Michael M. Forbes O, 1, * Alyssa Goodman O, 1 Catherine Zucker O, 2, ↑ John C. Forbes O, 3 Ralf Konietzka O, 1, 4 Cameren Swiggum O,5 João Alves O,5 John Bally O,6 Juan D. Soler O,7 Josefa E. Großschedl O,5 S HMUEL B IALY O ,8 M ICHAEL Y. G RUDIC O ,9 ,1 R EIMAR L EIKE O ,10 ,4 AND T ORSTEN E NSSLIN O 10 ,4 Barnard’s Loop is a famous arc of Hα emission located in the Orion star-forming region.  Here, we provide evidence of a possible formation mechanism for Barnard’s Loop and compare our results with recent work suggesting a major feedback event occurred in the region around 6 Myr ago.  We present a 3D model of the large-scale Orion region, indicating coherent, radial, 3D expansion of the OBP-Near/Briceño-1 (OBP-B1) cluster in the middle of a large dust cavity. The large-scale gas in the region also appears to be expanding from a central point, originally proposed to be Orion X. OBP-B1 appears to serve as another possible center, and we evaluate whether Orion X or OBP-B1 is more likely to be the cause of the expansion. We find that neither cluster served as the single expansion center, but rather a combination of feedback from both likely propelled the expansion.  Recent 3D dust maps are used to characterize the 3D topology of the entire region, which shows Barnard’s Loop’s correspondence with a large dust cavity around the OPB-B1 cluster. The molecular clouds Orion A, Orion B, and Orion λ reside on the shell of this cavity. Simple estimates of gravitational effects from both stars and gas indicate that the expansion of this asymmetric cavity likely induced anisotropy in the kinematics of OBP-B1.  We conclude that feedback from OBP-B1 has affected the structure of the Orion A, Orion B, and Orion λ molecular clouds and may have played a major role in the formation of Barnard’s Loop.オリオン星形成領域のバーナードループの形成メカニズムとフィードバックイベントとの比較。ダスト空洞の中でOBP-B1クラスターが膨張するという３次元モデル。OBP-B1とOrion Xが共同で膨張を推進。バーナードループはOBP-B1の周りのダスト空洞に対応。分子雲A, B, λはこの空洞のシェルで、空洞の非対称性がOBP-B1の非等方力学を引き起こしている。OBP-B1のフィードバックが分子雲たちの構造に影響し、バーナードループの形成に寄与している。
Yuya Fukuhara ©,¹,* Satoshi Okuzumi ©,¹ and Tomohiro Ono¹,² Turbulence in protoplanetary disks plays an important role in dust evolution and planetes- imal formation. The vertical shear instability (VSI) is one of the candidate hydrodynamic mechanisms that can generate turbulence in the outer disk regions. The VSI requires rapid gas cooling in addition to vertical shear. A linear stability analysis suggests that the VSI may not operate around the midplane where gas cooling is inefficient. In this study, we investigate the nonlinear outcome of the VSI in disks with a linearly VSI-stable midplane region. We perform two-dimensional global hydrodynamical simulations of an axisymmetric disk with vertically varying cooling times. The vertical cooling time pro- file determines the thicknesses of the linearly VSI-stable midplane layer and unstable layers above and below the midplane. We find that the thickness of the midplane stable layer determines the vertical structure of VSI-driven turbulence in the nonlinear sat- urated state. We identify two types of final saturated state: (i) T states, characterized by vertical turbulent motion penetrating into the VSI-stable midplane layer, and (ii) pT states, characterized by turbulent motion confined in the unstable layers. The pT states are realized when the midplane VSI-stable layer is thicker than two gas scale heights. We also find that the VSI-driven turbulence is largely suppressed at all heights when the VSI-unstable region lying above and below the midplane is thinner than two gas scale heights. We present empirical formulas that predict the strength of VSI-driven turbulence as a function of the thicknesses of the unstable and stable layers. These formulas will be useful for studying how VSI-driven turbulence and dust grains controlling the disk cooling efficiency evolve simultaneously.垂直シア不安定は外円盤の乱流を作れる。ガス冷却が非効率な赤道面では起きない。冷却時間が安定な領域の幅を決める。２タイプの非線形サチュレーション。T状態：不安定が赤道面まで貫く。pT状態：乱流が不安定な領域を制限する。安定不安定の境が２スケールハイト以上と以下で状況が変わる。安定領域の幅の関数として乱流の強さを予想。
Distance determination of molecular clouds in
the first quadrant of the Galactic plane using

Shinji Fujita ©, 1,2,* Atsushi M. Ito, 3 Yusuke Miyamoto ©, 4,5 Yasutomo Kawanishi ©, 6 Kazufumi Torii, 5 Yoshito Shimajiri ©, 7 Atsushi Nishimura ©,8 Kazuki Tokuda ©,9 Toshikazu Ohnishi ©,2 Hiroyuki Kaneko ©,5,10 Tsuyoshi Inoue,11 Shunya Takekawa ©,12 Mikito Kohno ©, 13, 14 Shota Ueda, 2 Shimpei Nishimoto, 2 Ryuki Yoneda, 2 Kaoru Nishikawa,¹ 4 and Daisuke Yoshida¹ 4 Machine learning has been successfully applied in various field but whether it is a viable tool for determining the distance to molecular clouds in the Galaxy is an open question. In the Galaxy, the kinematic distance is commonly employed to represent the distance to a molecular cloud. However, for the inner Galaxy, two different solutions, i.e., the “Near” solution and the “Far” solution, can be derived simultaneously. We attempt to construct a two-class (“Near” or “Far”) inference model using a convolutional neural network (CNN), which is a form of deep learning that can capture spatial features generally. In this study, we use the CO dataset in the first quadrant of the Galactic plane obtained with the Nobeyama 45 m radio telescope ( / = 62 − 10 ﾟ, | b | < 1 ﾟ). In the model, we apply the three- dimensional distribution (position-position-velocity) of the ¹²CO (J = 1–0) emissions as the main input. To train the model, a dataset with “Near” or “Far” annotation was created from the HII region catalog of the infrared astronomy satellite WISE. Consequently, we construct a CNN model with a 76% accuracy rate on the training dataset. Using the proposed model, we determine the distance to the molecular clouds identified by the CLUMPFIND algorithm. We found that the mass of molecular clouds with a distance of <8.15kpc identified in the 12CO data follows a power-law distribution with an index of approximately −2.3 in the mass range M > 10³ Mい. In addition, the detailed molecular gas distribution of the Galaxy, as seen from the Galactic North pole, was determined.銀河系内の分子雲の距離の近距離解と遠距離解を深層学習で解く野辺山4  5 m, CO 2-1銀河面第一限のPPV分布を入力し、WISEのHII領域カタログから近距離と遠距離を教える。CLUMPFINDで見つけた分子雲に適用。 Clustered Formation of Massive Stars within an Ionized Rotating Disk Roberto Galván-Madrid 1 ©, Qizhou Zhang 2 ©, Andrés Izquierdo 3,4 ©, Charles J. Law 2 ©, Thomas Peters 5 , Eric Keto 2 , Hauyu Baobab Liu 6,7 ©, Paul T. P. Ho 7,8 ©, Adam Ginsburg ®, and Carlos Carrasco-González 1 © We present Atacama Large Millimeter/submillimeter Array observations with a 800 au resolution and radiative- transfer modeling of the inner part ( r ≈ 6000 au) of the ionized accretion flow around a compact star cluster in formation at the center of the luminous ultracompact H II region G10.6-0.4. We modeled the flow with an ionized Keplerian disk with and without radial motions in its outer part, or with an external Ulrich envelope. The Markov Chain Monte Carlo fits to the data give total stellar masses M x from 120 to 200 M ⊙ , with much smaller ionized-gas  masses  Mjon-gas = 0.2–0.25 M 。 The  stellar  mass  is  distributed  within  the  gravitational  radius Rç ≈ 1000 to 1500 au, where the ionized gas is bound. The viewing inclination angle from the face-on orientation is i = 49°–56°. Radial motions at radii r > R e converge to v r 0 ≈ 8.7 km s−¹, or about the speed of sound of ionized gas, indicating that this gas is marginally unbound at most. From additional constraints on the ionizing-photon rate and far-IR luminosity of the region, we conclude that the stellar cluster consists of a few massive stars with M star = 32–60 M ω , or one star in this range of masses accompanied by a population of lower- mass stars. Any active accretion of ionized gas onto the massive (proto)stars is residual. The inferred cluster density is very large, comparable to that reported at similar scales in the Galactic center. Stellar interactions are likely to occur within the next million years. UCHII G10.6-0.4の中心で形成中の星団周囲のイオン降着流のr<6000 auの輻射輸送モデル。ケプラー円盤の外に動径方向の運動の有る無し。星の質量は120-200 Msun。イオンの質量は0.2-0.25 Msun。傾き角49-56度。星とイオンが束縛されている外のVrは音速の8.7 km/sに収束。星団はいくつかの大質量星か小質量星の集団を伴う一つの大質量星を含む。星団の密度は銀河中心のそのスケールの密度と同じくらい大きく、100万年以内に星の相互作用が起こる。