J/A+A/663/A56 SEDIGISM: Molecular Cloud morphology I. (Neralwar+, 2022)
The SEDIGISM survey: Molecular cloud morphology.
I. Classification and star formation.
Neralwar K.R., Colombo D., Duarte-Cabral A., Urquhart J.S., Mattern M.,
Wyrowski F., Menten K.M., Barnes P., Sanchez-Monge A., Beuther H.,
Rigby A.J., Mazumdar P., Eden D., Csengeri T., Dobbs C.L., Veena V.S.,
Neupane S., Henning T., Schuller F., Leurini S., Wienen M., Yang A.Y.,
Ragan S.E., Medina S., Nguyen-Luong Q.
<Astron. Astrophys. 663, A56 (2022)>
=2022A&A...663A..56N 2022A&A...663A..56N (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Molecular clouds
Keywords: ISM: clouds - local interstellar matter - ISM: bubbles -
stars: formation - submillimeter: ISM
Abstract:
We present one of the very first extensive classifications of a large
sample of molecular clouds based on their morphology. This is achieved
using a recently published catalogue of 10663 clouds obtained from the
first data release of the Structure, Excitation and Dynamics of the
Inner Galactic InterStellar Medium (SEDIGISM) survey. The clouds are
classified into four different morphologies by visual inspection and
using an automated algorithm - J plots. The visual inspection also
serves as a test for the J plots algorithm, as this is the first time
it has been used on molecular gas. Generally, it has been found that
the structure of molecular clouds is highly filamentary and our
observations indeed verify that most of our molecular clouds are
elongated structures. Based on our visual classification of the 10663
SEDIGISM clouds, 15% are ring-like, 57% are elongated, 15% are
concentrated and 10% are clumpy clouds. The remaining clouds do not
belong to any of these morphology classes and are termed unclassified.
We compare the SEDIGISM molecular clouds with structures identified
through other surveys, i.e. the elongated structures from APEX
Telescope Large Area Survey of the Galaxy (ATLASGAL) and the bubbles
from Milky Way Project (MWP). We find that many of the ATLASGAL and
MWP structures are velocity coherent. ATLASGAL elongated structures
overlap with ∼21% of the SEDIGISM elongated structures (elongated and
clumpy clouds) and MWP bubbles overlap with ∼ 25% of the SEDIGISM
ring-like clouds. We also analyse the star-formation associated with
different cloud morphologies using two different techniques. The first
technique examines star formation efficiency (SFE) and the dense gas
fraction (DGF), based on SEDIGISM clouds and ATLASGAL clumps data. The
second technique uses the high-mass star formation (HMSF) threshold
for molecular clouds. The results indicate that clouds with ring-like
and clumpy morphologies show a higher degree of star formation.
Description:
We provide the morphologies for the 10663 molecular clouds that were
identified by Duarte-Cabral et al. 2021 from the SEDIGISM survey. The
original catalogue of the molecular clouds is available at the
SEDIGISM database. tableA1.dat provides the cloud morphologies
identified using the J plots algorithm and by visual (by-eye)
analysis. It also provides the identifiers for clouds in the science,
VC and MR samples. The tableA2.dat, tableA3.dat and tableA4.dat list
the ATLASGAL filaments, ATLASGAL elongated structures and the MWP
bubbles that overlap with our molecular clouds respectively.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 116 10663 Morphologies of the clouds from the SEDIGISM
cloud catalogue
tablea2.dat 21 1657 ATLASGAL filaments overlapping with the
SEDIGISM clouds
tablea3.dat 21 3661 ATLASGAL elongated structures overlapping with
the SEDIGISM clouds
tablea4.dat 23 4977 MWP bubbles overlapping with the SEDIGISM clouds
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See also:
J/A+A/591/A5 : ATLASGAL dense filamentary structures (Li+, 2016)
J/MNRAS/488/1141 : Milky Way Project DR2 bubbles + bow shocks
(Jayasinghe+, 2019)
https://sedigism.mpifr-bonn.mpg.de/cgi-bin-seg/SEDIGISM_DATABASE.cgi :
SEDIGISM cloud catalogue
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- CloudID [1/10663] Unique cloud ID number described
by DC21 (1)
7- 23 A17 --- Name Cloud name, SDG followed by Galactic
coordinates as described by DC21 (1)
25- 42 F18.15 --- J1 [-0.44/0.89] J moment of the cloud
corresponding to principal inertial axis
I1
44- 64 E21.15 --- J2 [-0.88/0.34] J moment of the cloud
corresponding to principal inertial axis
I2
66- 73 A8 --- JStructure Structure of the cloud determined by
J plot analysis
75- 90 A16 --- Subclass Original sub-class of cloud estimated
using by-eye analysis (App: ks test)
92-103 A12 --- Structure Structure of cloud determined using
by-eye analysis
105 I1 --- science [0/1] tag identifying if the cloud belongs
to science sample (described in DC20)
(yes = 1, no = 0)
107 I1 --- VCSamp [0/1] tag identifying if the cloud belongs
to visually classified (VC) sample
(yes = 1, no = 0)
109 I1 --- MR [0/1] tag identifying if the cloud belongs
to morphologically reliable (MR) sample
(yes = 1, no = 0)
111 I1 --- NAG-El Number of AG-El overlapping with the cloud
113 I1 --- NAG-Fil Number of AG-Fil overlapping with the cloud
115-116 I2 --- NMWP Number of MWP bubbles overlapping with the
cloud
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Note (1): DC21 : Duarte-cabral et al. 2021MNRAS.500.3027D 2021MNRAS.500.3027D; see they Table A1.
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Byte-by-byte Description of file: tablea[23].dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- CloudID [16/10657] ID number of SEDIGISM cloud
7- 21 A15 --- ATLASGAL Name of the ATLASGAL structure overlapping
with the SEDIGISM cloud (2)
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Note (2): Refer column 'ATLASGAL' in list.dat in Li et al.,
2016, Cat. J/A+A/359/A5).
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Byte-by-byte Description of file: tablea4.dat
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Bytes Format Units Label Explanations
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1- 5 I5 --- CloudID [6/10657] ID number of SEDIGISM cloud
7- 23 A17 --- MWP Name of the MWP bubble overlapping with the
SEDIGISM cloud (3)
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Note (3): Refer column 'MWP' in table3.dat in Jayasingheet al., 2019,
Cat. J/MNRAS/488/1141.
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Acknowledgements:
Kartik Rajan Neralwar, kneralwar(at)mpifr-bonn.mpg.de
(End) Patricia Vannier [CDS] 14-Mar-2022