J/ApJS/235/3 Massive outflows associated with ATLASGAL clumps (Yang+, 2018)
Massive outflows associated with ATLASGAL clumps.
Yang A.Y., Thompson M.A., Urquhart J.S., Tian W.W.
<Astrophys. J. Suppl. Ser., 235, 3 (2018)>
=2018ApJS..235....3Y 2018ApJS..235....3Y
ADC_Keywords: Interstellar medium; Millimetric/submm sources; Carbon monoxide
Keywords: ISM: jets and outflows ; ISM: molecules ; stars: early-type ;
stars: formation ; stars: massive ; submillimeter: ISM
Abstract:
We have undertaken the largest survey for outflows within the Galactic
plane using simultaneously observed 13CO and C18O data. Out of a
total of 919 ATLASGAL clumps, 328 have data suitable to identify
outflows, and 228 (69%±3%) show high-velocity outflows. The clumps
with detected outflows show significantly higher clump masses
(Mclump), bolometric luminosities (Lbol), luminosity-to-mass
ratios (Lbol/Mclump), and peak H2 column densities (NH2)
compared to those without outflows. Outflow activity has been detected
within the youngest quiescent clump (i.e., 70µm weak) in this
sample, and we find that the outflow detection rate increases with
Mclump, Lbol, Lbol/Mclump, and NH2, approaching 90% in some
cases (UC HII regions = 93%±3%; masers = 86%±4%; HC HII regions
= 100%). This high detection rate suggests that outflows are ubiquitous
phenomena of massive star formation (MSF). The mean outflow mass
entrainment rate implies a mean accretion rate of ∼10-4M☉/yr,
in full agreement with the accretion rate predicted by theoretical
models of MSF. Outflow properties are tightly correlated with
Mclump, Lbol, and Lbol/Mclump and show the strongest relation
with the bolometric clump luminosity. This suggests that outflows
might be driven by the most massive and luminous source within the
clump. The correlations are similar for both low-mass and high-mass
outflows over 7 orders of magnitude, indicating that they may share a
similar outflow mechanism. Outflow energy is comparable to the
turbulent energy within the clump; however, we find no evidence that
outflows increase the level of clump turbulence as the clumps evolve.
This implies that the origin of turbulence within clumps is fixed
before the onset of star formation.
Description:
The 13CO/C18O (J=3->2) Heterodyne Inner Milky Way Plane Survey
(CHIMPS) covers a region of 28°≲l≲46° and |b|≤0.5° in
the inner Galactic plane (Rigby+ 2016MNRAS.456.2885R 2016MNRAS.456.2885R) and has been
carried out using the James Clerk Maxwell Telescope (JCMT). The
observations have an angular resolution of 15" and velocity resolution
of 0.5km/s. This sensitivity corresponds to column densities of
NH2∼3x1020 and NH2∼4x1021cm-2 for 13CO and C18O,
respectively.
The APEX Telescope Large Area Survey of the Galaxy (ATLASGAL) is an
unbiased 870um submillimeter (submm) survey that covers the inner
Galactic plane (|l|≤60 with |b|≤1.5°). ATLASGAL has a resolution
of 19". A comprehensive database of ∼10163 massive star formation
(MSF) clumps has been compiled (ATLASGAL compact source catalog (CSC);
Contreras+ 2013, J/A+A/549/A45 ; Urquhart+ 2014, J/A+A/568/A41 and
2018, J/MNRAS/473/1059) that allows us to undertake a blind search for
CO outflow activity toward star-forming clumps.
See section 2 for further details on the final sample of 328 clumps
from CHIMPS and ATLASGAL.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 57 328 Clump properties of all 328 ATLASGAL clumps
to search for outflows;
updated version by the author
table3.dat 72 228 The 13CO outflow calculations of all blue and
red wings
table4.dat 85 153 The 13CO outflow properties of all blue and
red lobes
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See also:
J/ApJ/428/693 : Rosette Nebula and Maddalena Cloud structures (Williams+ 1994)
J/A+A/417/615 : Maser and outflows in UC HII region (Codella+, 2004)
J/A+A/426/503 : High velocity molecular outflows (Update) (Wu+ 2004)
J/AJ/131/2525 : MAGPIS 20cm survey (Helfand+, 2006)
J/A+A/453/1003 : SCUBA ultracompact HII regions (Thompson+, 2006)
J/A+A/472/187 : 12CO outflows towards submm cores in Perseus (Hatchell+, 2007)
J/ApJS/184/1 : Molecular clouds in the LMC by NANTEN. II. (Kawamura+, 2009)
J/ApJ/723/1019 : Galactic SFR and gas surface densities (Heiderman+, 2010)
J/MNRAS/418/1689 : Red MSX water maser and ammonia emissions (Urquhart+, 2011)
J/A+A/549/A45 : ATLASGAL Compact Source Catalog: 330<l<21 (Contreras+, 2013)
J/A+A/557/A94 : SiO and HCO+ massive molecular outflows (Sanchez-Monge+, 2013)
J/MNRAS/435/400 : ATLASGAL compact HII regions (Urquhart+, 2013)
J/MNRAS/444/566 : Methanol maser associated outflows (de Villiers+, 2014)
J/A+A/568/A41 : ATLASGAL Compact Source Catalog: 280<l<60 (Urquhart+, 2014)
J/A+A/570/A65 : ATLASGAL massive clumps CO depletion (Giannetti+, 2014)
J/MNRAS/443/1555 : ATLASGAL massive star forming clumps (Urquhart+, 2014)
J/MNRAS/453/645 : Massive molecular outflows distance-limited sample
(Maud+, 2015)
J/MNRAS/446/3461 : 6.7-GHz methanol masers-dust associations (Urquhart+, 2015)
J/AJ/152/92 : Ammonia & CO outflow around methanol masers (Li+, 2016)
J/A+A/599/A139 : ATLASGAL massive clumps dust characterization (Koenig+, 2017)
J/MNRAS/473/1059 : Complete sample of Galactic clumps (Urquhart+, 2018)
J/A+A/611/A6 : ATLASGAL massive clumps H2CO data (Tang+, 2018)
http://doi.org/10.11570/16.0001 : CHIMPS landing page
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- AGAL ATLASGAL identifier (GLLL.lll+BB.bbb) (G1)
17- 22 F6.3 deg GLON [27.7/46.2] Galactic longitude
24- 29 F6.3 deg GLAT [-0.5/0.5] Galactic latitude
31- 36 F6.2 Jy Fint [0.9/320] Integrated flux density at 870 microns
38- 41 F4.1 kpc Dist [0.3/13.1]? Heliocentric distance
43- 48 F6.3 [cm-2] logNH2 [21.7/24]? Log peak H2 column density (1)
50- 52 F3.1 [Lsun] logLb [0.5/7]? Log bolometric luminosity (1)
54- 57 F4.1 [Msun] logMc [-0.3/5]? Log clump mass (1)
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Note (1): These physical values are from Urquhart+ (2018, J/MNRAS/473/1059).
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 16 A16 --- AGAL ATLASGAL identifier (G1)
18- 22 F5.1 km/s 13COVel [6.3/116.2] Observed peak 13CO velocity
24- 27 F4.1 K 13COTmb [2/30.6] Antenna temperature of 13CO (1)
29- 33 F5.1 km/s 18COVel [6.8/116] Observed peak C18O velocity
35- 38 F4.1 K 18COTmb [0.9/14.4] Antenna temperature of C18O (1)
40- 44 F5.1 km/s loDelVb [-2.2/113.4]? Lower velocity range of 13CO
blue wing
46- 50 F5.1 km/s upDelVb [-0.2/116]? Upper velocity range of 13CO
blue wing
52- 56 F5.1 km/s loDelVr [9.8/118]? Lower velocity range of 13CO
red wing
58- 62 F5.1 km/s upDelVr [10.8/118.4]? Upper velocity range of 13CO
red wing
64- 67 F4.1 km/s Vmaxb [1.2/17]? Maximum projected velocity for blue (2)
69- 72 F4.1 km/s Vmaxr [0.3/17.6]? Maximum projected velocity for red (2)
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Note (1): The antenna temperatures are corrected for main-beam
efficiency (0.72).
Note (2): Shifted relative to the peak C18O velocity.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- AGAL ATLASGAL identifier (G1)
17- 19 F3.1 pc lb [0.1/2.8] Blue lobe length
21- 23 F3.1 pc lr [0.2/3] Red lobe length
25- 30 F6.1 Msun Mb [0.5/1145.1] Blue lobe mass
32- 36 F5.1 Msun Mr [0.9/950.3] Red lobe mass
38- 43 F6.1 Msun Mout [1.4/2065.3] Total Blue+Red lobe mass
45- 50 F6.1 10Msun.km/s p [0.6/2964.6] Momentum
52- 58 F7.3 10+39J E [0.02/786.4] Energy
60- 63 F4.1 10+4yr td [2.5/89] Dynamic time
65- 70 F6.2 10-4Msun/yr dM/dt [0.08/172.3] Mass entrainment rate
72- 77 F6.2 10-3Msun.km/s/yr FCO [0.04/225.2] CO mechanical force
79- 85 F7.3 Lsun LCO [0.01/502.8] CO mechanical luminosity
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Global note:
Note (G1): ATLASGAL compact source catalog (CSC) identifier
from Urquhart+ 2014, J/A+A/568/A41 ; in Simbad.
History:
* From electronic version of the journal
* One misprint corrected in Table 3:
G031.596+00.33 is in fact G031.596-00.336
* 3 objects added by the author in Table 2:
G030.691+00.227, G030.008-00.272, and G045.466+00.04
Acknowledgements:
Aiyuan Yang [Max Planck Institute for Radio Astronomy; mpifr-bonn.mpg.de]
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-Aug-2018