J/MNRAS/511/3618 ATOMS ALMA 3 mm VII SiO clumps with ACA (Liu+, 2022)
ATOMS ALMA three-millimeter observations of massive star-forming regions - VII.
A catalogue of SiO clumps from ACA observations.
Liu R., Liu T., Chen G., Liu H.-L., Wang K., Li J.-Z., Lee C.W., Liu X.,
Juvela M., Garay G., Dewangan L., Soam A., Bronfman L., He J.,
Eswaraiah C., Zhang S.-J., Zhang Y., Xu F.-W., Toth L.V., Shen Z.-Q.,
Li S., Wu Y.-F., Qin S.-L., Ren Z., Zhang G., Tej A., Goldsmith P.F.,
Baug T., Luo Q., Zhou J., Zhang C.
<Mon. Not. R. Astron. Soc. 511, 3618-3635 (2022)>
=2022MNRAS.511.3618L 2022MNRAS.511.3618L (SIMBAD/NED BibCode)
ADC_Keywords: Milky Way ; Molecular clouds ; H II regions ; Radio lines ;
Star Forming Region ; Interstellar medium ; Molecular data ;
Radio sources ; Millimetric/submm sources ; Positional data ;
Photometry ; Spectroscopy ; Space velocities ; Velocity dispersion
Keywords: ISM: clouds - ISM: jets and outflows -
ISM: molecules; stars: formation - stars: massive - radio lines: ISM
Abstract:
To understand the nature of SiO emission, we conducted ACA
observations of the SiO (2-1) lines toward 146 massive star-forming
regions, as part of the ALMA Three-millimeter Observations of Massive
Star-forming regions (ATOMS) survey. We detected SiO emission in 128
(87.7 per cent) sources and identified 171 SiO clumps, 105 of which
are spatially separated from 3 mm continuum emission. A large amount
of the SiO line profiles (60 per cent) are non-Gaussian. The velocity
dispersion of the SiO lines ranges from 0.3 to 5.43 km/s. In 63
sources the SiO clumps are associated with H II regions characterized
by H40α emission. We find that 68 per cent (116) of the SiO
clumps are associated with strong outflows. The median velocity
dispersion of the SiO line for outflow sources and non-outflow sources
is 1.91 km/s and 0.99 km/s, respectively. These results indicate that
outflow activities could be connected to strongly shocked gas. The
velocity dispersion and [SiO]/[H13CO+] intensity ratio do not show
any correlation with the dust temperature and particle number density
of clumps. We find a positive correlation between the SiO line
luminosity and the bolometric luminosity, implying stronger shock
activities are associated with more luminous protoclusters. The SiO
clumps in associations with H II regions were found to show a steeper
feature in LSiO / Lbol. The SiO line luminosity and the fraction
of shocked gas have no apparent evidence of correlation with the
evolutionary stages traced by luminosity to mass ratio (Lbol / M).
Description:
The ALMA Three-millimeter Observations of Massive Star-forming regions
(ATOMS) survey employed the Band 3 and covered eight spectral windows
(two wide spectral windows in upper side band and six spectral windows
in lower side band) toward 146 massive star-forming sources (Liu et
al. 2020MNRAS.496.2790L 2020MNRAS.496.2790L, Cat. J/MNRAS/496/2790). The survey provides
us larger samples and high resolution to systemically study various
molecular gas involved in star formation. In this paper, we
statistically analyse SiO emission of 146 sources using the Atacama
Compact 7 m Array observations (ACA) to better understand shocked gas
under different conditions and in different evolutionary trends. We
establish a catalogue of the SiO clumps for future studies. We present
the level of shock activities and estimate the fraction of the shocked
gas in the clumps, (i.e see section Introduction).
As section 2 Observations explained,the present study is based on the
ATOMS survey data (Project ID: 2019.1.00685.S; PI: Tie Liu). The
survey has collected both 12m-array and ACA data. We focus the latter
in this work with an aim at compiling a complete catalogue of SiO
emission clumps owing to the benefit from the large field of view of
the ACA observations. The Atacama Compact 7 m Array (ACA) observations
were conducted from 2019 September to mid-November. The SiO J = 2-1,
HCO+ J = 1-0, H13CO+ J = 1-0 lines are included in SPWs 1∼6 at the
lower side band with the spectral resolutions of 0.21, 0.11, and 0.21
km/s, respectively (Liu et al. 2020MNRAS.496.2790L 2020MNRAS.496.2790L, Cat.
J/MNRAS/496/2790; 2020MNRAS.496.2821L 2020MNRAS.496.2821L, Cat. J/MNRAS/496/2821 and
2021MNRAS.505.2801L 2021MNRAS.505.2801L, Cat. J/MNRAS/505/2801). The H40α and CS J = 2-1
lines are included in SPWs 7 at the upper side band with the spectral
resolutions of 1.49 km/s. The ACA data were calibrated and imaged by
casa software.
We produced moment 0, 1 and 2 intensity maps of SiO emissions and also
for other presented lines to identify SiO clumps and emissions. The
derived parameters as line intensity/luminosity, radius, velocity and
dispersion are explicited in the section 3 Results and presented for
171 clumps in the table1.dat and table2.dat. Next, focusing on line
wings and outflows of SiO, HCO+, and CS emissions, we associated line
wings and outflows with the help of spectra shown in Appendix. The
derived data as intensity ratio, number density and line associations
are presented in the tablea3.dat.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 130 153 SiO (2-1) line parameters and clump properties
in the region with clear detections
tablea2.dat 97 18 SiO (2-1) line parameters and clump properties
in the region without clear detections
tablea3.dat 66 171 SiO (2-1) line parameters and clump properties
associated to H40α, HCO+, CS and outflow
emissions
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See also:
J/MNRAS/496/2790 : ATOMS I Description and a first look at G9.62+0.19
(Liu+, 2020)
J/MNRAS/496/2821 : ATOMS II Compact objects in ACA observations (Liu+, 2020)
J/MNRAS/505/2801 : ATOMS Paper III, massive star-forming regions (Liu+, 2021)
J/MNRAS/510/4998 : ATOMS IV Gas clumps properties and SFRs (Zhang+, 2022)
J/A+A/586/A149 : SiO in ATLASGAL-selected massive clumps (Csengeri+, 2016)
J/A+A/570/A1 : Cygnus-X CO and SiO outflows datacubes (Duarte-Cabral+,2014)
J/A+A/570/A49 : APEX spectra of massive YSOs (Leurini+, 2014)
J/ApJ/756/60 : A 3mm line survey in 37 IR dark clouds (Sanhueza+, 2012)
J/A+A/557/A94 : SiO and HCO+ massive molecular outflows
(Sanchez-Monge+, 2013)
J/A+A/476/1243 : Millimeter continuum mapping of Cygnus X (Motte+, 2007)
J/A+A/563/A97 : IRAM 30m reduced spectra of 59 sources (Gerner+, 2014)
J/A+A/481/345 : SED evolution in massive young stellar objects
(Molinari+, 2008)
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- IRAS IRAS source clump identifier
(IRAS HHMMm±DDMM) with CN for clump
number (IRAS)
16- 17 I2 h RAh Right ascension (J2000)
19- 20 I2 min RAm Right ascension (J2000)
22- 26 F5.2 s RAs Right ascension (J2000)
28 A1 --- DE- Declination sign (J2000)
29- 30 I2 deg DEd Declination (J2000)
32- 33 I2 arcmin DEm Declination (J2000)
35- 39 F5.2 arcsec DEs Declination (J2000)
41- 44 F4.2 pc Rad The linear radius of SiO clump (Ra)
46- 50 F5.3 pc e_Rad ? Mean error of radius (errorR_a)
52 A1 --- n_IRAS SiO clump is unresolved by CASA (Note)
54- 60 F7.3 Jy.km/s Fint The integrated intensity of SiO clump
(intFvdv)
62- 67 F6.2 Jy.km/s e_Fint Mean error of Fint (errorFvdv)
69- 75 F7.2 km/s v The velocity of SiO clump (v)
77- 81 F5.2 km/s e_v Mean error of the velocity (errorv)
83- 87 F5.2 km/s sigmaMin The velocity dispersion min of SiO clump
(Dmin)
89- 93 F5.2 km/s sigmaMax The velocity dispersion max of SiO clump
(Dmax)
95- 98 F4.2 km/s sigmaMean The velocity dispersion mean of SiO clump
(Dmean)
100- 103 F4.2 km/s sigmaMed The velocity dispersion median of SiO
clump (Dmedian)
105- 110 F6.2 km/s sigmaStd The velocity dispersion standard deviation
of SiO clump (Dstd)
112- 118 F7.3 Lsun logLSiO Logarithm of the luminosity of the SiO
clump as computed in the equation 1 of the
section 3.3 SiO clumps properties (logLSiO)
120- 124 F5.3 Lsun e_logLSiO Mean error of the logLSiO (errorlogLSiO)
126- 130 F5.3 Jy/beam rms The rms level σ for each source
(σ)
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Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- IRAS IRAS source clump identifier
(IRAS HHMMm±DDMM) with CN for clump
number (IRAS)
13- 14 I2 h RAh Right ascension (J2000)
16- 17 I2 min RAm Right ascension (J2000)
19- 23 F5.2 s RAs Right ascension (J2000)
25 A1 --- DE- Declination sign (J2000)
26- 27 I2 deg DEd Declination (J2000)
29- 30 I2 arcmin DEm Declination (J2000)
32- 35 F4.1 arcsec DEs Declination (J2000)
37- 40 F4.2 pc Rad The linear radius of SiO clump (Ra)
42- 46 F5.3 pc e_Rad ? Mean error of radius (errorR_a)
48 A1 --- n_IRAS SiO clump is unresolved by CASA (Note)
50- 54 F5.2 Jy.km/s Fint The integrated intensity of SiO clump
(intFvdv)
56- 59 F4.2 Jy.km/s e_Fint Mean error of Fint (errorFvdv)
61- 65 F5.1 km/s v The velocity of SiO clump (v)
67- 69 F3.1 km/s e_v Mean error of the velocity (errorv)
71- 74 F4.2 km/s sigma The velocity dispersion mean of SiO clump
(σv)
76- 78 F3.1 km/s e_sigma Mean error of the sigma (errorσv)
80- 85 F6.2 Lsun logLSiO Logarithm of the luminosity of the SiO clump
as computed in the equation 1 of the section
3.3 SiO clumps properties (logLSiO)
87- 91 F5.3 Lsun e_logLSiO Mean error of the logLSiO (errorlogLSiO)
93- 97 F5.3 Jy/beam rms The rms level σ for each source
(σ)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 14 A14 --- IRAS IRAS source clump identifier
(IRAS HHMMm±DDMM) with CN for
clump number (IRAS)
16- 21 F6.2 Lsun/Msun Lbol/Mclump The total SED bolometric luminosity
to clump mass ratio from Liu et al.
(2020MNRAS.496.2790L 2020MNRAS.496.2790L,
Cat. J/MNRAS/496/2790) (Lbol/M)
23- 26 F4.2 [cm-3] logn The logarithm of n particle number
density can be derived as the
equation 2 of the section 4.1 The
line broadening of SiO emission
(logn)
28- 32 F5.2 --- [SiO]/[H13CO+] ? The integrated intensity ratio of
SiO emission and H13CO+
emission ([SiO]/[H13CO+])
34- 39 F6.3 --- e_[SiO]/[H13CO+] ? Mean error on [SiO]/[H13CO+],
source without this error has
absorption features in their
spectra
41- 44 F4.2 pc Dd The separated linear distance
between the central position of SiO
clumps and the peak position of the
3 mm continuum emission (D_d)
46- 48 A3 --- FlagH40a [yes no] Flag indicates that the
SiO clump is associated with
H40α emission, 86 yes
and 85 no (H40α)
50- 52 A3 --- FlagWingSiO [yes no] Flag indicates that the
SiO clump shows line wing emission,
103 yes and 68 no (WingSiO)
54- 56 A3 --- FlagWingHCO+ [yes no] Flag indicates that the
HCO+ shows line wing emission,
62 yes and 109 no (WingHCO+)
58- 60 A3 --- FlagWingCS [yes no] Flag indicates that the CS
shows line wing emission, 88 yes
and 83 no (WingCS)
62- 64 A3 --- Outflow [yes no] Flag indicates that the
SiO clump is with outflow, 116 yes
and 55 no (outflow)
66 A1 --- Type [A B C D] Type for SiO clump
associations to H40α and/or
3 mm continuum emission (type) (1)
--------------------------------------------------------------------------------
Note (1): Type for SiO clump associations are as follows:
A = The SiO clumps associated with both H40α emission and 3 mm
continuum emission, 27 sources in our sample
B = The SiO clumps separated from both H40α emission and 3 mm
continuum emission, 59 sources in our sample
C = The SiO clumps associated with 3mm continuum emission
undetected H40α emission, 39 sources in our sample
D = The SiO clumps partly separated from 3mm continuum emission
undetected H40α emission, 46 sources in our sample
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History:
From electronic version of the journal
References:
Liu et al., Paper I 2020MNRAS.496.2790L 2020MNRAS.496.2790L, Cat. J/MNRAS/496/2790
Liu et al., Paper II 2020MNRAS.496.2821L 2020MNRAS.496.2821L, Cat. J/MNRAS/496/2821
Liu et al., Paper III 2021MNRAS.505.2801L 2021MNRAS.505.2801L, Cat. J/MNRAS/505/2801
Zhang et al., Paper IV 2022MNRAS.510.4998Z 2022MNRAS.510.4998Z, Cat. J/MNRAS/510/4998
Liu et al., Paper V 2022MNRAS.510.5009L 2022MNRAS.510.5009L
Zhou et al., Paper VI 2021MNRAS.508.4639Z 2021MNRAS.508.4639Z
Qing et al., Paper VIII 2022MNRAS.511.3463Q 2022MNRAS.511.3463Q
Liu et al., Paper IX 2022MNRAS.511.4480L 2022MNRAS.511.4480L
Peng et al., Paper X 2022MNRAS.512.4419P 2022MNRAS.512.4419P
Zhou et al., Paper XI 2022MNRAS.514.6038Z 2022MNRAS.514.6038Z
Saha et al., Paper XII 2022MNRAS.516.1983S 2022MNRAS.516.1983S
Zhang et al., Paper XIII 2023MNRAS.520..322Z 2023MNRAS.520..322Z
Zhang et al., Paper XIV 2023MNRAS.520.3245Z 2023MNRAS.520.3245Z
Xu et al., Paper XV 2023MNRAS.520.3259X 2023MNRAS.520.3259X
Zhang et al., Paper XVI 2024MNRAS.533.4234Z 2024MNRAS.533.4234Z
Das et al., Paper XVII 2024MNRAS.534.3832D 2024MNRAS.534.3832D
Zhang et al., Paper XVIII 2024MNRAS.535.1364Z 2024MNRAS.535.1364Z
Liu et al. Paper XIX 2025MNRAS.536.1894L 2025MNRAS.536.1894L
(End) Luc Trabelsi [CDS] 24-Jan-2025