The formaldehyde H₂CO(1₁₀–1₁₁) absorption line and H110α radio recombination line have been observed toward the Aquila Molecular Cloud using the Nanshan 25 m telescope operated by the Xinjiang Astronomical Observatory CAS. These first observations of the H₂CO (1₁₀–1₁₁) absorption line determine the extent of the molecular regions that are affected by the ongoing star formation in the Aquila molecular complex and show some of the dynamic properties. The distribution of the excitation temperature T _ex for H₂CO identifies the two known star formation regions W40 and Serpens South as well as a smaller new region Serpens 3. The intensity and velocity distributions of H₂CO and ¹³CO(1−0) do not agree well with each other, which confirms that the H₂CO absorption structure is mostly determined by the excitation of the molecules resulting from the star formation rather than by the availability of molecular material as represented by the distribution. Some velocity-coherent linear ¹³CO(1−0) structures have been identified in velocity channel maps of H₂CO and it is found that the three star formation regions lie on the intersect points of filaments. The H110α emission is found only at the location of the W40 H ii region and spectral profile indicates a redshifted spherical outflow structure in the outskirts of the H ii region. Sensitive mapping of H₂CO absorption of the Aquila Complex has correctly identified the locations of star formation activity in complex molecular clouds and the spectral profiles reveal the dominant velocity components and may identify the presence of outflows.

We study the G013.313+0.193 (G013.313) region, a complex environment characterised by molecular cloud interactions indicative of cloud-cloud collision (CCC). Observations of the NH₃ (1,1) and (2,2) inversion transitions were obtained using the Nanshan 26 m radio telescope, while HCO⁺ (J = 1–0), ¹²CO, ¹³CO, and C¹⁸O (J = 1–0) transitions from the 14 m Purple Mountain Observatory Delingha (PMODLH) 14 m telescope. Archival data are also included. We identified key observational signatures of CCC, including complementary spatial distributions, U-shaped structures, bridge features, and V-shaped velocity distributions. The position–velocity (P–V) diagrams reveal clear indications of gas interaction between two velocity components, suggesting an ongoing collision at an estimated angle of ∼ 45° to the line of sight. The estimated collision timescale is 0.35–1.03 Myr, aligned with the inferred ages of young stellar objects (YSOs) in the region, supporting the hypothesis of collision-induced star formation. Hub-filament systems (HFSs) are identified in the compressed gas region, where filaments converge towards a dense hub, suggesting the CCC as a potential driver of HFS and massive star formation. The high column density (∼2 × 10²³ cm⁻²) suggests favourable conditions for the formation of massive stars. Although alternative kinematic drivers such as longitudinal collapse and shear motion are considered, CCC remains the most plausible explanation for the observed features. Our findings contribute to our understanding of the mechanisms of cloud dynamics and massive star formation in turbulent molecular environments.

We present high-angular resolution observations, conducted with the Atacama Large Millimeter/Submillimeter Array (ALMA) in Band 6, of high-excitation molecular lines of ${\mathrm{CH}}_3\mathrm{CN}$, CH₃OH, and the H29$\alpha$ radio recombination line, towards the G333.6-0.2 ultracompact (UC) H ii region. Our observations reveal three hot molecular cores: A, B, and C, where emission is detected in ten components of the $J=14\to 13$ rotational ladder of ${\mathrm{CH}}_3\mathrm{CN}$ and in the CH₃OH $J=5_{1,4}\to 4_{1,3}$ transition. Rotational diagram analysis of ${\mathrm{CH}}_3\mathrm{CN}$ reveals excitation temperatures ranging from 380 to 430 K. First-order moment maps of ${\mathrm{CH}}_3\mathrm{CN}$ and CH₃OH reveal distinct velocity gradients in all cores, suggesting rotating structures, with core A also showing evidence of expansion motions. The H29$\alpha$ recombination line shows a linewidth of $30.2\pm 0.12$ km s⁻¹, dominated by dynamical and thermal broadening, indicative of large-scale motions in ionized gas. Analysis of the ionized gas properties yields an electron density of $(4.8\pm 0.4)\times {10}^5$ cm⁻³, an emission measure of $(1.23\pm 0.06)\times {10}^9$ pc cm⁻⁶, and a Lyman continuum photon flux consistent with an O5–O6 V (Zero-Age Main Sequence; ZAMS) star. Our results suggest that G333.6-0.2 is in an intermediate evolutionary stage between hypercompact (HC) and ultracompact (UC) H ii regions, hosting active high-mass star formation with rotating hot cores and ionized gas dynamics.

Over the past decade, the most important observations of the interstellar medium have been made in the infrared and radio regions of electromagnetic radiation. Of particular interest were GLIMPSE (Galactic Legacy Infrared Midplane Survey Extraordinaire), MIPSGAL and WISE (Wide-field Infrared Survey Explorer) surveys of several areas of star formation. Distinctive features of the infrared view of the Galactic disk at wavelengths from 3.4 μm to 22 μm include regions of ionized hydrogen HII, infrared bubbles, young stellar objects, massive star formation, infrared dark clouds, diffuse dust, include hydrocarbons and radiation from millions of stars. Based on current literature, infrared signatures in hot regions around young massive stars have been identified as dust bubbles, so in this paper, the regions around bubble N10, one of the northern infrared bubbles included in Churchwell's catalog, were investigated. Using archival data from the WISE and 2MASS catalogs, we searched for candidates for young stellar objects around the N10 dust bubble and found 117 emission objects. Koenig et al. (2014) plotted diagrams of their color indices and energy distribution in the spectrum for each studied object under different classification conditions. According to the results of studies around the infrared dust bubble N10, objects at an early stage of evolution were discovered: 13 objects are young class I stars and 13 objects are young class II stars, 3 objects are classified as transitional disks. За последнее десятилетие важнейшие наблюдения межзвездной среды выполнены в инфракрасном и радиодиапазонах электромагнитного излучения. Особый интерес представляли обзоры GLIMPSE (экстраординарный инфракрасный обзор срединной плоскости галактики), MIPSGAL и WISE (Wide-field Infrared Survey Explorer) нескольких областей звездообразования. Отличительные особенности инфракрасного изображения галактического диска на длинах волн от 3,4 мкм до 22 мкм включают области ионизированного водорода HII, инфракрасные пузыри, молодые звездные объекты, массивное звездообразование, инфракрасные темные облака, диффузную пыль, включают углеводороды и излучение миллионов звезды. Основываясь на современной литературе, инфракрасные сигнатуры в горячих областях вокруг молодых массивных звезд были идентифицированы как пылевые пузыри, поэтому в этой статье были исследованы области вокруг пузыря N10, одного из северных инфракрасных пузырей, включенных в каталог Черчвелла. Используя архивные данные из каталогов WISE и 2MASS, мы провели поиск кандидатов в молодые звездные объекты вокруг пылевого пузыря N10 и нашли 117 эмиссионных объектов. Кениг и др. (2014) построили графики их показателей цвета и распределения энергии в спектре для каждого исследуемого объекта при разных условиях классификации. По результатам исследований вокруг инфракрасного пылевого пузыря N10 были обнаружены объекты, находящиеся на ранней стадии эволюции: 13 объектов — молодые звезды I класса и 13 объектов — молодые звезды II класса, 3 объекта относятся к категории переходных дисков. Соңғы онжылдық ішінде жұлдызаралық ортадағы ең маңызды бақылаулар электромагниттік сәулеленудің инфрақызыл және радио аймақтарында жасалды. Жұлдыздардың түзілуінің бірнеше бағыттары бойынша GLIMPSE (Galactic Legacy Infrared Midplane Survey Extraordinaire), MIPSGAL және WISE (Wide-field Infrared Survey Explorer) барлаулары ерекше қызығушылық тудырды. 3,4 мкм-ден 22 мкм-ге дейінгі толқын ұзындығындағы Галактикалық дискінің инфрақызыл көрінісінің ерекше белгілеріне иондалған сутегі аймақтары HII, инфрақызыл көпіршіктер, жас жұлдыздар объектілері, жұлдыздардың жаппай түзілуі, инфрақызыл қара бұлттар, диффуздық шаң, көмірсутектер мен миллиондаған жұлдыздардың сәулеленуін жатқызуға болады. Заманауи әдебиеттерге талдау жасау арқылы жас массивті жұлдыздардың айналасындағы қыздырылған аймақтардағы инфрақызыл белгілер шаң көпіршіктер екені анықталды, сол себепті бұл жұмыста Churchwell каталогына енгізілген солтүстік инфрақызыл көпіршіктердің бірі – N10...

The geography of Kazakhstan is characterized by a diverse landscape and a small population. Therefore, certain automobile roads pass through unpopulated mountain regions, where physical road diagnostics are rare or almost absent, while landscape factors continue to affect the road. However, modern geo-information approaches and remote sensing could effectively provide the road diagnostics necessary to make timely control decisions regarding a road’s design, construction, and maintenance. To justify this assumption, we researched the deformation of a mountain road near Almaty city. Open access satellite images of and meteorological archival data for the region were processed. The resulting data were compared to validate the road’s deformation triggers. Extreme weather conditions’ impacts could be identified via road destruction (nearly 40 m longitudinal cracks, 15 m short transversal cracks, and two crack networks along a 50 m road section). The remotely sensed parameters (vertical displacement velocity, slope exposure, dissections, topographic wetness index, aspect, solar radiation, SAVI, and snow melting) show the complexity of triggers of extensive road deformations. The article focuses only on open access data from remote sensing images and meteorological archives. All the resulting data are available and open for all interested parties to use.