kaz29Вестник Казахстанско-Британского технического университетаHerald of the Kazakh-British Technical University1998-66882959-8109Казахстанско-Британский Технический Университет10.55452/1998-6688-2026-23-1-334-345kaz29-2527Research ArticleФИЗИЧЕСКИЕ НАУКИPHYSICAL SCIENCESАНАЛИЗ МОЛЕКУЛЯРНЫХ ЛИНИЙ В ОБЛАСТИ G23.21−0.38 ПО ДАННЫМ ALMA: СВИДЕТЕЛЬСТВА ВРАЩЕНИЯ И ГРАДИЕНТОВ ВОЗБУЖДЕНИЯKINEMATICS AND STRUCTURE OF THE MASSIVE STAR-FORMING REGION G350.29+0.12https://orcid.org/0009-0002-0532-9641АбдирахманA.AbdirakhmanA.

магистрант

г. Алматы

Master’s student

Almaty

armiyaqyzyaidana@gmail.comhttps://orcid.org/0000-0002-5604-3742ОмарA.OmarA.

PhD

г. Алматы

PhD

Almaty

omaruzhan@gmail.comhttps://orcid.org/0009-0006-5496-4501ИслямЖ.IslyamZh.

магистрант

г. Алматы

Master’s student

Almaty

islyamovzhomart@gmail.comhttps://orcid.org/0000-0002-4596-1855АлимгазиноваН.AlimgazinovaN.

к.ф.-м.н.

г. Алматы

Cand. Phys.-Math Sc.

Almaty

Nazgul.Alimgazinova@kaznu.kzhttps://orcid.org/0000-0001-5049-9338ДемессиноваA. A.DemessinovaA.

PhD

г. Алматы

PhD

Almaty

aizat.dem@gmail.comhttps://orcid.org/0000-0002-0045-5457НодяровA.NodyarovA.

PhD

г. Алматы

PhD

Almaty

nodyarov.atilkhan@gmail.comhttps://orcid.org/0009-0003-8572-1850ТуяқбаеваD.TuiakbaevaD.

магистрант

г. Кокшетау

Master’s student

Kokshetau

duria1510@outlook.comhttps://orcid.org/0000-0002-0322-1509MанапбаеваA.ManapbayevaA.

PhD

г. Алматы

PhD

Almaty

manapbayeva.arailym@gmail.comhttps://orcid.org/0000-0003-4136-3935АдилжанK.AdilzhanK.

докторант

г. Алматы

PhD student

Almaty

kami_adilzhan@mail.ruhttps://orcid.org/0000-0001-9557-8590ШаймолдинН.ShaimoldinN.

докторан

г. Урумчи

PhD student

Urumqi

nurzhan@xao.ac.cnКазахский национальный университет им. аль-ФарабиКазахстанAl-Farabi Kazakh National UniversityKazakhstanКазахский национальный университет им. аль-Фараби; Институт экспериментальной и теоретической физики Казахский национальный университет им. аль-ФарабиКазахстанAl-Farabi Kazakh National University; Institute of Experimental and Theoretical Physics, Al-Farabi Kazakh National UniversityKazakhstanУниверситет имени Ш. УалихановаКазахстанSh. Ualikhanov Kokshetau UniversityKazakhstanИнститут экспериментальной и теоретической физики, Казахский национальный университет им. аль-Фараби; Казахский национальный женский педагогический университетКазахстанInstitute of Experimental and Theoretical Physics, Al-Farabi Kazakh National University; Kazakh National Women’s Teacher Training UniversityKazakhstanАстрономическая обсерватория Синьцзянского отделения Китайской академии наукКитайXinjiang Astronomical Observatory, Chinese Academy of SciencesChina202629032026231334345Copyright © Абдирахман A., Омар A., Ислям Ж., Алимгазинова Н., Демессинова A.A., Нодяров A., Туяқбаева D., Mанапбаева A., Адилжан K., Шаймолдин Н., 20262026Абдирахман A., Омар A., Ислям Ж., Алимгазинова Н., Демессинова A.A., Нодяров A., Туяқбаева D., Mанапбаева A., Адилжан K., Шаймолдин Н.Abdirakhman A., Omar A., Islyam Z., Alimgazinova N., Demessinova A., Nodyarov A., Tuiakbaeva D., Manapbayeva A., Adilzhan K., Shaimoldin N.Данная работа распространяется под лицензией Creative Commons Attribution 4.0.This work is licensed under a Creative Commons Attribution 4.0 License.https://vestnik.kbtu.edu.kz/jour/article/view/2527

Мы представляем наблюдения континуума на длине волны 1.3 мм с высоким угловым разрешением, а также молекулярных линий в области массивного звездообразования G350.29+0.12, выполненные с использованием вращательных переходов CH₃CN и CH₃¹³CN. Континуумное излучение разрешает два основных ядра: яркое компактное северное ядро G350.29+0.12 A и более слабое южное ядро G350.29+0.12 B. Ядро A демонстрирует шесть компактных субструктур, вложенных в более протяженное излучение. Обнаружены множественные K-компоненты переходов CH₃CN J = 14→13 и CH₃¹³CN J = 14→13, при этом излучение преимущественно исходит из ядра A. Карты момента 0 для CH₃CN показывают, что интегральные интенсивности достигают максимума в положении основного континуумного источника, указывая на то, что молекулярное излучение трассирует теплый и плотный газ. Карты момента 1 выявляют выраженный градиент скорости порядка ∼2 км/с через ядро A, ориентированный с северо-запада на юговосток, тогда как карты момента 2 демонстрируют зависящие от K-компоненты вариации дисперсии скоростей. Диаграммы положение–скорость дополнительно указывают на организованные вращательные движения, проявляющиеся в виде компактной скоростной структуры с центральным максимумом и систематическими градиентами. Анализ вращательной температуры дает T₍rot₎ = 360.6 ± 34.8 K для CH₃CN, что указывает на наиболее горячий и плотный газ, и T₍rot₎ = 138 ± 45 K для CH₃¹³CN, что согласуется с более холодным и протяженным веществом. В совокупности эти результаты демонстрируют, что G350.29+0.12 A является вращающимся горячим молекулярным ядром, находящимся на стадии активного массивного звездообразования.

We present high–angular resolution 1.3 mm continuum and molecular line observations toward the highmass star-forming region G350.29+0.12, using CH₃CN and CH₃¹³CN rotational transitions. The continuum emission resolves two main cores: a bright, compact northern core G350.29+0.12 A and a weaker southern core G350.29+0.12 B. Core A exhibits six compact substructures embedded within more extended emission. M K-components of the CH3CN J = 14→13 and CH3 13CN J = 14→13 transitions are detected, with the emission arising primarily from core A. The CH3CN moment 0 maps show that the integrated intensities peak at the main continuum position, indicating that the molecular emission traces warm and dense gas. The moment 1 maps reveal a pronounced velocity gradient of ∼2 km s-1 across core A, oriented from northwest to southeast, while the moment 2 maps show K-dependent variations in velocity dispersion. Position–velocity diagrams further indicate organized rotational motions, exhibiting a compact velocity structure with a central peak and systematic gradients. Rotational temperature analysis yields = 360.6 ± 34.8 K for CH3CN, tracing the hottest and densest gas and Trot = 138 ± 45 K for CH3 13CN, consistent with cooler and more extended material. Together, these results demonstrate that G350.29+0.12 A is a rotating hot molecular core undergoing active high-mass star formation.

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The authors declare that there are no conflicts of interest present.