J/A+A/706/A242 13CO clump catalog from FUGIN in the Milky Way (Zheng+, 2026)
Catalog of 13CO clumps from FUGIN in the Milky Way at l = 10 deg - 50 deg.
Zheng S., Pan X., Urquhart J.S., Luo X., Huang Y., Jiang Z., Chen Z.,
Zeng S., Zeng X., Zhang J.
<Astron. Astrophys. 706, A242 (2026)>
=2026A&A...706A.242Z 2026A&A...706A.242Z (SIMBAD/NED BibCode)
ADC_Keywords: Surveys ; Galactic plane ; Molecular clouds ; Radio lines ;
Carbon monoxide
Keywords: molecular data - techniques: image processing - ISM: molecules
Abstract:
Since stars and star clusters emerge from the gravitational collapse
of clumps and cores, studying molecular clumps is fundamental to
understanding the processes of star formation. The FOREST Unbiased
Galactic Plane Imaging (FUGIN) survey offers insights into the
distribution of clumps and physical properties across different
environments, aiding in studies of environmental effects, such as the
location within the galaxy on star formation.
This study aims to produce a catalog of clumps from the FUGIN survey
to understand the complete mechanism of high-mass star formation in
giant molecular clouds (GMCs). We use the catalog to analyze the
physical properties of clumps in high-mass star-forming regions,
enhancing our understanding of how different environments impact the
star-formation process.
Our process for the detection and verification of 13CO clumps in the
FUGIN survey comprised two steps. First, the source extraction code
FacetClumps was used to detect as many molecular clump candidates as
possible from the FUGIN 13CO data. Second, a trained and validated
semi-supervised deep learning model, SS-3D-Clump, was applied to
verify these candidates, providing confidence levels for the clumps
and filtering out false candidates to enhance the accuracy of the
detection results.
The resulting catalog containing 23150 clumps extracted from the
13CO (J=1-0) data covers the first quadrant (10≤l≤50°,
|b|≤1°). By matching with CHIMPS and inheriting the distances of
the matched CHIMPS clumps, we found that the sizes of the FUGIN clumps
range from 0.1 to 3pc, demonstrating that the dense structures belong
to the clump scale. The catalog achieves an 80% completeness level
above 466K.km/s.
The proposed two-step approach effectively integrates clump detection
algorithms with semi-supervised deep learning, achieving an accuracy
comparable to manual verification and thereby improving the extraction
of clumps from large-scale survey data. The resulting clump catalog
enables the analysis of the physical properties of clumps in high-mass
star-forming regions, contributing to a better understanding of
environmental influences on clump formation and the star formation
process.
Description:
Since stars and star clusters emerge from the gravitational collapse
of clumps and cores, studying molecular clumps is fundamental to
understanding star formation. The FUGIN (FOREST Unbiased Galactic
Plane Imaging) survey provides a comprehensive view of molecular gas
in the Galactic plane. This work presents a catalog of molecular
clumps identified in the FUGIN 13CO (J=1-0) data. Clump detection is
performed using the FacetClumps algorithm, followed by verification
with a semi-supervised deep learning model (SS-3D-Clump). The
resulting catalog contains 23150 clumps in the first Galactic quadrant
(10°≤l≤ 50°, |b|≤1°). By matching with the CHIMPS
survey and adopting distance estimates, the physical sizes of the
clumps range from 0.1 to 3pc. The catalog reaches 80% completeness
above 466K.km/s.
The file table1.dat contains the catalog of 13CO molecular clumps
detected in the FUGIN survey, for a total of 23150 sources.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 87 23150 Catalog of FUGIN 13CO clumps
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 26 A26 --- ID Clump identifier
28- 33 F6.3 deg GLON Galactic longitude of centroid
35- 40 F6.3 deg GLAT Galactic latitude of centroid
42- 47 F6.2 km/s Vel Velocity centroid
49- 52 F4.1 arcsec sGLON RMS size along Galactic longitude
54- 57 F4.1 arcsec sGLAT RMS size along Galactic latitude
59- 62 F4.2 km/s DeltaV RMS velocity dispersion
64- 66 I3 deg theta Position angle of the clump
68- 71 F4.1 K Tpeak Peak brightness temperature
73- 77 F5.1 1000K.km/s W Integrated intensity
79- 82 F4.1 --- SNR Peak signal-to-noise ratio
84- 87 F4.2 --- alpha Confidence from SS-3D-Clump
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Acknowledgements:
Xiaoyu Luo, vastlxy(at)163.com
Yao Huang, huangyao(at)ctgu.edu.cn
(End) Patricia Vannier [CDS] 17-Dec-2025