A5075158362- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Spectroscopy and Laser Applications
- Atmospheric Ozone and Climate
- Astronomy and Astrophysical Research
- Molecular Spectroscopy and Structure
- Atomic and Subatomic Physics Research
- Astronomical Observations and Instrumentation
- Cold Atom Physics and Bose-Einstein Condensates
- Advanced Chemical Physics Studies
- Quantum, superfluid, helium dynamics
- Astro and Planetary Science
- Advanced Chemical Sensor Technologies
- Phase Equilibria and Thermodynamics
- Ionosphere and magnetosphere dynamics
- Advanced Thermodynamic Systems and Engines
- Solid State Laser Technologies
- Astrophysical Phenomena and Observations
- Luminescence Properties of Advanced Materials
- Laser Design and Applications
- Galaxies: Formation, Evolution, Phenomena
- Atmospheric chemistry and aerosols
- Criminal Law and Evidence
- Plasma Diagnostics and Applications
- Chemical Reactions and Isotopes
Xinjiang Astronomical Observatory
2012-2025
Chinese Academy of Sciences
2012-2025
University of Chinese Academy of Sciences
2018-2025
Qingdao University
2006
Abstract We conducted an ammonia survey targeting 217 sources from the BGPS v1.0 using Nanshan 26 m radio telescope, focusing on $\rm NH_3$(1,1) and (2,2) lines, selecting based criteria that their 1.1 mm fluxes are greater than 5 Jy they observable with telescope at Xinjiang Astronomical Observatory. successfully detected 188 (86.6%) of our sources. These span a galactic longitude range 1.2○ to 192.6○ reside in local, Perseus, Saggitarius-Carina, Scutum-Centaurus Norma spiral arms between...
We studied the hub filament system G323.46-0.08 based on archival molecular line data from SEDIGISM 13CO survey and infrared GLIMPSE, MIPS, Hi-GAL surveys. consists of three filaments, F-north, F-west, F-south, that converge toward central high_mass clump AGAL 323.459-0.079. F-west Part 1 F-south show clear large-scale velocity gradients 0.28 0.44 km s-1 pc-1, respectively. They seem to be channeling materials into The minimum accretion rate was estimated 1216 M Myr-1. A characteristic...
Single-pointing observations of NH$_3$ (1,1) and (2,2) were conducted towards 672 Planck Early Release Cold Cores (ECCs) using the Nanshan 26-m radio telescope. Out these sources, a detection rate 37% (249 cores) was achieved, with NH$_3$(1,1) hyperfine structure detected in 187 NH$_3$(2,2) emission lines 76 cores. The NH3 is positively correlated continuum fluxes at frequency 857 GHz. Among observed cores, ~22% have associated stellar IR objects within beam size (~2$\arcmin$). This suggests...
The feedback effect of massive stars can either accelerate or inhibit star formation activity within molecular clouds. Studying the morphology clouds near W5 offers an excellent opportunity to examine this effect. We conducted a comprehensive survey complex using Purple Mountain Observatory 13.7 m millimeter telescope. This includes 12 CO, 13 and C 18 O ( J = 1 − 0), with sky coverage 6.6 deg 2 (136.0° < l 138.75°, 0° b 2.4°). Furthermore, we performed simultaneous observations NH 3 (1,1)...
Abstract We investigate the evolutionary dynamics with archival continuum and line data of 27 giant molecular clouds (GMCs) in Milky Way, focusing on their influence star formation. Examining dense gas mass fraction (DGMF) among GMCs, we categorize them into low-DGMF (DGMF < 20%), medium-DGMF (20% DGMF 60%), high-DGMF (60% DGMF) groups. The analysis uncovers systematic trends free-fall time, virial parameter, surface density, formation rate (SFR), SFR per unit area (Σ ), efficiency for as...
The bubble G15.684-0.29 has a radius of 15.7 pc. Its large size indicates that it may have enough time to trigger star formation. We identify 39 dense cold clumps around the from Hi-GAL survey. All them satisfy criteria for forming massive stars, and most lie in shell. 19 molecular 12CO(3–2) survey, all which are gravitationally bound. found 9 Class I YSOs, 28 II 12 transition disks (TDs) bubble. For those young stellar objects (YSOs) located within boundary, 6 7 YSOs shell, 15 22 inside...
In LTE, the two inner satellite lines (ISLs) and outer (OSLs) of NH$_{3}$ (1,1) transition are each predicted to have equal intensities. However, hyperfine intensity anomalies (HIAs) observed be omnipresent in star formation regions, which is still not fully understood. addressing this issue, we find that computation method HIA by ratio peak intensities may defects, especially when being used process spectra with low velocity dispersions. Therefore define integrated HIAs ISLs (HIA$_{\rm...
Young protoclusters (embedded stellar clusters) are responsible for the vast majority of star formation currently occurring in Galaxy. Recent observations suggest a scenario which filamentary structures interstellar medium represent first step towards precluster clumps and eventually formation. Whether filaments continuously fuel process when cluster accretes material is still an open question. In this paper, we present case study famous 'integral shaped filament' (ISF) Orion A molecular...
Single-pointing observations of NH 3 (1,1) and (2,2) were conducted toward 672 Planck Early Cold Cores (ECCs) using the Nanshan 26-m radio telescope. Out these sources, a detection rate 37% (249 cores) was achieved, with hyperfine structure detected in 187 cores emission lines 76 them. The is positively correlated continuum fluxes at frequency 857 GHz. Among observed cores, ~22% have associated stellar infrared objects within beam size (~2′). This suggests that most our sample may be...
W49A is a prominent giant molecular cloud (GMC) that exhibits strong star formation activities, yet its structural and kinematic properties remain uncertain. Our study aims to investigate the large-scale structure kinematics of W49A, elucidate role filaments hub-filament systems (HFSs) in activity. We utilized continuum data from Herschel James Clerk Maxwell Telescope (JCMT) as well lines 12CO (3-2), 13CO C18O (3-2) identify HFS structures within W49A. Further analysis focused on physical...
Aims. W49A is a prominent giant molecular cloud (GMC) that exhibits strong star formation activities, yet its structural and kinematic properties remain uncertain. Our study aims to investigate the large-scale structure kinematics of W49A, elucidate role filaments hub-filament systems (HFSs) in activity. Methods. We utilized continuum data from Herschel James Clerk Maxwell Telescope (JCMT) as well lines 12 CO (3–2), 13 C 18 O (3–2) identify HFSs within W49A. Further analysis focused on...
Abstract The excitation temperature T ex for molecular emission and absorption lines is an essential parameter interpreting the environment. This can be obtained by observing multiple transitions or hyperfine structures of a single transition, but it remains unknown transition without structure lines. Earlier H 2 CO experiments adopted constant value , which not correct regions with active star formation ii regions. For CO, two equations unknowns may used to determine optical depth τ if...
Abstract The observations of the Aquila Rift cloud complex at 23.708 and 115.271 GHz made using Nanshan 26 m radio telescope 13.7 millimeter-wavelength are presented. We find that CO(1 − 0) gas distribution is similar to NH 3 in complex. In some diffusion regions characterized by CO, we identified several dense clumps based on detected ammonia molecular emission. Through comparison spectral line parameters for , 13 C 18 O, our study reveals center velocities O lines comparable positively...
Identifying infall motions is crucial for our understanding of accretion processes in regions star formation. The NH 3 (1,1) hyperfine intensity anomaly (HIA) has been proposed to be a readily usable tracer such star-forming harboring young stellar objects at very early evolutionary stages. In this paper, we seek study the HIA toward 15 candidate order assess its reliability as an tracer. Using deep observations (1, 1) transition with Effelsberg 100 m telescope, identified HIAs all targets....
Identifying infall motions is crucial for our understanding of accretion processes in regions star formation. The NH3 (1,1) hyperfine intensity anomaly (HIA) has been proposed to be a readily usable tracer such star-forming harboring young stellar objects at very early evolutionary stages. In this paper, we seek study the HIA toward fifteen candidate assess its reliability as an tracer. By using deep observations transition with Effelsberg 100 m telescope, HIAs have identified all targets....
The W3/4 Giant Molecular Cloud (GMC) was an ideal target to study the impact of H ii regions onto surrounding molecular gas and star formation. We utilized PMO CO (1--0) data from Milky Way Imaging Scroll Painting (MWISP) survey analyze cloud structure feedback effect W4 region. Our observations showed that cold gas, traced by CO, mainly resided in W3 GMC, with C18O concentrated dense regions, while around dispersed. 13CO position-position-velocity (PPV) distributions revealed a "C" shaped...
By using a pump-probe technique, the nascent rotational and vibrational state distributions of CsH are obtained in Cs(62D,72D) plus H2 reaction. The molecules found to populate lowest two (ν'' = 0 1) levels ground electronic state. comparing spectral intensities action spectra with those pertinent Cs atomic fluorescence excitation spectra, relative reactivity is an order 62D3/2 > 62D5/2 72D3/2 72D5/2. temperatures be slightly below cell temperature. fractions (⟨fV⟩, ⟨fR⟩, ⟨fT⟩) average...
We studied the cloud-cloud collision candidate G323.18+0.15 based on signatures of induced filaments, clumps, and star formation. used archival molecular spectrum line data from SEDIGISM $^{13}$CO($J$\,=\,2--1) survey, Mopra southern Galactic plane CO infrared to radio GLIMPSE, MIPS, Hi-GAL, SGPS surveys. Our new result shows that complex is 3.55kpc away us consists three cloud components, G323.18a, G323.18b, G323.18c. G323.18b a perfect U-shape structure, which can be fully complemented by...
Abstract Infrared bubbles provide a unique opportunity to study the interactions between massive stars and surrounding material. We conduct multi-wavelength on environment star formation around an infrared bubble N 13. Three dust clumps two molecular are identified 13, which all distributed layer. Young stellar objects (YSOs) carefully searched using colors YSO candidates of WISE Gaia DR2, three Class I/II YSOs found in In addition, four O-type 13 probably exciting stars. The dynamical...
We studied the hub filament system G323.46-0.08 based on archival molecular line data from SEDIGISM 13CO survey and infrared GLIMPSE, MIPS, Hi-GAL surveys. consists of three filaments, F-north, F-west, F-south, that converge toward central high_mass clump AGAL 323.459-0.079. F-west Part 1 F-south show clear large-scale velocity gradients 0.28 0.44 km s-1 pc-1, respectively. They seem to be channeling materials into The minimum accretion rate was estimated 1216 M Myr-1. A characteristic...