J/MNRAS/496/2821 ATOMS II Compact objects in ACA observations (Liu+, 2020)
ATOMS: ALMA three-millimeter observations of massive star-forming regions - II.
Compact objects in ACA observations and star formation scaling relations.
Liu T., Evans N.J., Kim K.-T., Goldsmith P.F., Liu S.-Y., Zhang Q.,
Tatematsu K., Wang K., Juvela M., Bronfman L., Cunningham M.R., Garay G.,
Hirota T., Lee J.-E., Kang S.-J., Li D., Li P.-S., Mardones D., Qin S.-L.,
Ristorcelli I., Tej A., Toth L.V., Wu J.-W., Wu Y.-F., Yi H.-W., Yun H.-S.,
Liu H.-L., Peng Y.-P., Li J., Li S.H., Lee C.W., Shen Z.-Q., Baug T.,
Wang J.-Z., Zhang Y., Issac N., Zhu F.-Y., Luo Q.-Y., Liu X.-C., Xu F.-W.,
Wang Y., Zhang C., Ren Z., Zhang C.
<Mon. Not. R. Astron. Soc., 496, 2821-2835 (2020)>
=2020MNRAS.496.2821L 2020MNRAS.496.2821L (SIMBAD/NED BibCode)
ADC_Keywords: Star Forming Region ; Interstellar medium ; Molecular clouds ;
Milky Way ; Radio sources
Keywords: stars: formation - ISM: clouds - ISM: molecules -
galaxies: star formation
Abstract:
We report studies of the relationships between the total bolometric
luminosity (Lbol or LTIR) and the molecular line luminosities of
J=1-0 transitions of H13CN, H13CO+, HCN, and HCO+ with data
obtained from ACA observations in the 'ATOMS' survey of 146 active
Galactic star-forming regions. The correlations between Lbol and
molecular line luminosities L'mol of the four transitions all
appear to be approximately linear. Line emission of isotopologues
shows as large scatters in Lbol-L'_ mol_ relations as their main
line emission. The log(Lbol/L'mol) for different molecular line
tracers have similar distributions. The Lbol-to-L'_ mol_ ratios do
not change with galactocentric distances (RGC) and clump masses
(Mclump). The molecular line luminosity ratios (HCN-to-HCO+,
H13CN-to-H13CO+, HCN-to-H13CN, and HCO+-to-H13CO+) all
appear constant against Lbol, dust temperature (Td), Mclump, and
RGC. Our studies suggest that both the main lines and isotopologue
lines are good tracers of the total masses of dense gas in Galactic
molecular clumps. The large optical depths of main lines do not affect
the interpretation of the slopes in star formation relations. We find
that the mean star formation efficiency (SFE) of massive Galactic
clumps in the 'ATOMS' survey is reasonably consistent with other
measures of the SFE for dense gas, even those using very different
tracers or examining very different spatial scales.
Description:
The ALMA observations of the 'ATOMS' survey have been summarized in
Liu et al. (2020MNRAS.496.2790, Cat. J/MNRAS/496/2790). We here
briefly introduce the observations with the ACA. Observations with the
ACA were conducted from late September to mid November in 2019 with
band 3 (Project ID: 2019.1.00685.S; PI: Tie Liu). The IRAS names,
phase centers, systemic velocities, distances, and galactocentric
distances of the targeted sources are listed in Table A1. The typical
ACA observing time per source is ∼8min. The angular resolution and
maximum recovered angular scale (MRS) in ACA observations are
∼13.1-13.8arcsec and ∼53.8-76.2arcsec, respectively. The ACA
observations are sensitive to angular scales smaller than ∼60arcsec
but the MRS is larger than the angular sizes of most clumps in the
sample (Faundez et al. 2004A&A...426...97F 2004A&A...426...97F, Cat. J/A+A/426/97). The
J=1-0 transitions of HCN, HCO+, H13CN, and H13CO+ are included
in four spectral windows in the lower side-band. The spectral
resolution for HCN J=1-0 and HCO+ J=1-0 is 61.035kHz (or ∼0.2km/s),
while the spectral resolution for H13CN J=1-0 and H13CO+ J=1-0
is 0.122MHz (or ∼0.4km/s). The continuum visibility data are
constructed using the line-free spectral channels. All images are
primary beam corrected. The achieved sensitivity of the ACA
observations is around 50-90mJy/beam per 0.122MHz channel for lines.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 91 173 Compact objects identified in 3mm continuum
emission
tablea2.dat 71 189 Compact objects identified in H13CO+ J=1-0
tablea3.dat 58 184 Compact objects identified in H13CN J=1-0
tablea4.dat 71 182 Compact objects identified in HCO+ J=1-0
tablea5.dat 58 189 Compact objects identified in HCN J=1-0
tablea6.dat 63 119 Parameters of 119 sources
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See also:
J/A+AS/115/81 : A CS(2-1) survey of UC HII regions (Bronfman+, 1996)
J/A+A/426/97 : SIMBA survey. 1.2-mm/IRAS sources (Faundez+, 2004)
J/MNRAS/473/1059 : Complete sample of Galactic clump properties
(Urquhart+, 2018)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 11 A11 --- Name Source name (IHHMMs+DDMM)
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- 42 F6.1 km/s VLSR Systemic velocity from Bronfman et al.
(1996A&AS..115...81B 1996A&AS..115...81B, Cat. J/A+AS/115/81)
44- 48 F5.2 kpc Dist Distance (1)
50- 54 F5.2 kpc RGC Galactocentric distance (1)
56 I1 --- ID [1/3] Internal identifier of the compact
object
58- 63 F6.2 arcsec OffsetRA Offset in right ascension
65- 70 F6.2 arcsec OffsetDE Offset in declination
72- 75 F4.2 --- rasp Aspect ratio (G1)
77- 80 F4.2 pc Reff Effective radius (G2)
82- 85 F4.2 Jy/beam Speak Peak integrated intensity
87- 91 F5.2 Jy Stotal Total integrated intensity
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Note (1): The distances are from Urquhart et al. (2018MNRAS.473.1059U 2018MNRAS.473.1059U,
Cat. J/MNRAS/473/1059) and Faundez et al. (2004A&A...426...97F 2004A&A...426...97F,
Cat. J/A+A/426/97)
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Byte-by-byte Description of file: tablea[24].dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name (IHHMMs+DDMM)
13 I1 --- ID [1/5] Internal identifier of the
compact object
15- 20 F6.2 arcsec OffsetRA Offset in right ascension
22- 27 F6.2 arcsec OffsetDE Offset in declination
29- 33 F5.2 --- rasp ? Aspect ratio (G1)
35- 38 F4.2 pc Reff ? Effective radius (G2)
40- 43 F4.2 pc dpeak Offset from brightest continuum
emission peak
45- 50 F6.2 Jy/beam.km/s Speak Peak integrated intensity
52- 58 F7.2 Jy.km/s Stotal Total integrated intensity
60- 66 F7.2 km/s Vcmp Source-averaged velocity
68- 71 F4.2 km/s sigma Velocity dispersion
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Byte-by-byte Description of file: tablea[35].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name (IHHMMs+DDMM)
13 I1 --- ID [1/6] Internal identifier of the
compact object
15- 20 F6.2 arcsec OffsetRA Offset in right ascension
22- 27 F6.2 arcsec OffsetDE Offset in declination
29- 33 F5.2 --- rasp ? Aspect ratio (G1)
35- 38 F4.2 pc Reff ? Effective radius (G2)
40- 43 F4.2 pc dpeak Offset from brightest continuum
emission peak
45- 50 F6.2 Jy/beam.km/s Speak Peak integrated intensity
52- 58 F7.2 Jy.km/s Stotal Total integrated intensity
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea6.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Name Source name (IHHMMs+DDMM)
13- 16 F4.2 pc Reff Effective radius (1)
18- 19 I2 K Tdust Dust temperature (1)
21- 24 F4.2 [Lsun] logLbol Logarithm of the dust temperature (1)
26- 29 F4.2 [Msun] logMclump Logarithm of the clump's mass (1)
31- 35 F5.2 [K.km/s.pc2] logLH13CO+ Logarithm of the H13CO+
luminosity
37- 41 F5.2 [K.km/s.pc2] logLH13CN Logarithm of the H13CN luminosity
43- 47 F5.2 [K.km/s.pc2] logLHCO+ Logarithm of the HCO+ luminosity
49- 53 F5.2 [K.km/s.pc2] logLHCN Logarithm of the HCN luminosity
55- 58 F4.2 [Msun] logM13vir Logarithm of the virial mass derived
from H13CO+ line emission
60- 63 F4.2 [Msun] logM12vir Logarithm of the virial mass derived
from HCO+ line emission
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Note (1): Reff, Td, Lbol, and Mclump are compiled by Liu et al.
(2020MNRAS.496.2790L 2020MNRAS.496.2790L, Cat. J/MNRAS/496/2790), which are adopted from
Urquhart et al. (2018MNRAS.473.1059U 2018MNRAS.473.1059U, Cat. J/MNRAS/473/1059) and
Faundez et al. (2004A&A...426...97F 2004A&A...426...97F, Cat. J/A+A/426/97)
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Global notes:
Note (G1): The aspect ratio value is defined as the ratio between de-convolved
FWHM major dimension (a) and minor dimension (b)
Note (G2): The effective radius is defined as Reff=sqrt(ab)
--------------------------------------------------------------------------------
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 III 2021MNRAS.505.2801L 2021MNRAS.505.2801L
Zhang et al., Paper IV 2022MNRAS.510.4998Z 2022MNRAS.510.4998Z
Liu et al., Paper V 2022MNRAS.510.5009L 2022MNRAS.510.5009L
Zhou et al., Paper VI 2021MNRAS.508.4639Z 2021MNRAS.508.4639Z
Liu et al., Paper VII 2022MNRAS.511.3618L 2022MNRAS.511.3618L
Qin 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
(End) Ana Fiallos [CDS] 03-Jul-2023