J/ApJ/960/48 ALMA-IM. IX. SiO outflows in massive protoclusters (Towner+, 2024)
ALMA-IMF.
IX. Catalog and physical properties of 315 SiO outflow candidates in
15 massive protoclusters.
Towner A.P.M., Ginsburg A., Dell'Ova P., Gusdorf A., Bontemps S.,
Csengeri T., Galvan-Madrid R., Louvet F.K., Motte F., Sanhueza P.,
Stutz A.M., Bally J., Baug T., Chen H.-R.V., Cunningham N.,
Fernandez-Lopez M., Liu H.-L., Lu X., Nony T., Valeille-Manet M., Wu B.,
Alvarez-Gutierrez R.H., Bonfand M., Di Francesco J., Nguyen-Luong Q.,
Olguin F., Whitworth A.P.
<Astrophys. J., 960, 48 (2024)>
=2024ApJ...960...48T 2024ApJ...960...48T
ADC_Keywords: Interstellar medium; Molecular data; YSOs; Radio lines;
Interferometry
Keywords: Young stellar objects ; Star forming regions ; Protostars ;
Massive stars ; Stellar jets ; Stellar winds ; Catalogs ;
Interstellar molecules ; Radio interferometry ; Astrochemistry ;
Molecular gas ; Protoclusters
Abstract:
We present a catalog of 315 protostellar outflow candidates detected
in SiO J=5-4 in the ALMA-IMF Large Program, observed with ∼2000au
spatial resolution, 0.339km/s velocity resolution, and 2-12mJy/beam
(0.18-0.8K) sensitivity. We find median outflow masses, momenta, and
kinetic energies of ∼0.3M☉, 4M☉km/s, and 1045erg,
respectively. Median outflow lifetimes are 6000 yr, yielding median
mass, momentum, and energy rates of dM/dt=10-4.4M☉/yr,
dP/dt=10-3.2M☉km.s-1.yr-1, and dE/dt=1L☉. We analyze
these outflow properties in the aggregate in each field. We find
correlations between field-aggregated SiO outflow properties and total
mass in cores (∼3σ-5σ), and no correlations above 3σ
with clump mass, clump luminosity, or clump luminosity-to-mass ratio.
We perform a linear regression analysis and find that the correlation
between field-aggregated outflow mass and total clump mass-which has
been previously described in the literature-may actually be mediated
by the relationship between outflow mass and total mass in cores. We
also find that the most massive SiO outflow in each field is typically
responsible for only 15%-30% of the total outflow mass (60% upper
limit). Our data agree well with the established mechanical
force-bolometric luminosity relationship in the literature, and our
data extend this relationship up to L≥106L☉ and
dP/dt≥1M☉km/s/yr. Our lack of correlation with clump L/M is
inconsistent with models of protocluster formation in which all
protostars start forming at the same time.
Description:
The SiO J=5-4 data presented herein were taken as part of the ALMA-IMF
(Motte+ 2022A&A...662A...8M 2022A&A...662A...8M) Large Program (2017.1.01355.L,
PIs: Motte, Ginsburg, Louvet, Sanhueza), with the exception of the SiO
observations for W43-MM1, which were taken as part of the pilot
program 2013.1.01365.S (Nony+ 2020, J/A+A/636/A38). The ALMA-IMF Large
Program targets were observed in Band 6 (∼216-234GHz, ∼1.3mm) and
Band 3 (∼91-106GHz, ∼3mm), with matching linear spatial resolution
(≲2000au) for all fields and in both bands.
In this work, we examine only the data taken with the 12m array. These
line cubes can be found at https://www.almaimf.com/data.html
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 74 15 ALMA-IMF SiO line cube properties
table3.dat 122 354 Catalog of SiO outflow candidates
tablec1.dat 543 315 Derived properties of individual outflow candidates
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See also:
J/A+A/321/293 : SiO production in interstellar shocks (Schilke+ 1997)
J/A+A/476/1243 : Millimeter continuum mapping of Cygnus X (Motte+, 2007)
J/A+A/557/A94 : SiO & HCO+ massive molecular outflows (Sanchez-Monge+, 2013)
J/MNRAS/444/566 : Methanol maser associated outflows (de Villiers+, 2014)
J/A+A/570/A1 : Cygnus-X CO & SiO outflows datacubes (Duarte-Cabral+, 2014)
J/A+A/570/A49 : APEX spectra of massive YSOs (Leurini+, 2014)
J/MNRAS/453/645 : Massive mol. outflows distance-limited sample (Maud+, 2015)
J/A+A/586/A149 : SiO in ATLASGAL-selected massive clumps (Csengeri+, 2016)
J/A+A/591/A149 : Hi-GAL. inner Milky Way: +68≥l≥70 (Molinari+, 2016)
J/ApJ/867/167 : High-mass outflows from the COHRS CO(3-2) survey (Li+, 2018)
J/ApJS/251/20 : ALMA survey of Orion PGCCs (ALMASOP). II. (Dutta+, 2020)
J/A+A/636/A38 : W43-MM1 ALMA 12CO(2-1) datacube (Nony+, 2020)
J/A+A/662/A9 : Dense molecular cloud regions ALMA images (Ginsburg+, 2022)
J/MNRAS/511/3618 : ATOMS ALMA 3 mm VII SiO clumps with ACA (Liu+, 2022)
J/A+A/674/A75 : W43-MM1 and W43-MM2+MM3 ALMA datacubes (Nony+, 2023)
http://www.almaimf.com/data.html : ALMA IMF homepage
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Field Field identifier
10- 11 I2 h RAh [15/19] Hour of right ascension (ICRS) (1)
13- 14 I2 min RAm Minute of right ascension (ICRS)
16- 20 F5.2 s RAs Second of right ascension (ICRS)
22 A1 --- DE- Sign of declination (ICRS) (1)
23- 24 I2 deg DEd Degree of declination (ICRS) (1)
26- 27 I2 arcmin DEm Arcminute of declination (ICRS)
29- 32 F4.1 arcsec DEs Arcsecond of declination (ICRS)
34- 42 A9 arcsec Beam Synthesized beam size
44- 46 I3 deg PA [-85/88] Synthesized beam position angle
48- 51 F4.2 arcsec Pixel [0.08/0.2] Pixel size
53- 56 F4.2 K SigMed [0.18/0.9] Median σ for each cube
in K (2)
58- 62 F5.2 mJy/beam SigMedb [2.4/15.6] Median σ for each cube
in mJy/beam (2)
64- 68 F5.2 mJy/beam b_SigMedb [2.2/14.3] Minimum σ (2)
70- 74 F5.2 mJy/beam B_SigMedb [2.58/16.9] Maximum σ (2)
--------------------------------------------------------------------------------
Note (1): The ICRS coordinates of the reference position (center) of each
mosaic, taken from the SiO line cube image headers.
Note (2): Median σ for each cube, in both kelvin and mJy/beam. In all
cases, σ=1.4826*MAD, where MAD is the median absolute deviation
from the median. σ is measured for every channel in the image
cube within an emission-free region near the center of the field. The
emission-free region is the same for all channels in a given field.
The median, minimum, and maximum σ reported in these columns are
calculated across all channels in the cube.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Field Field or Clump
10- 11 I2 --- ID [1/47] Outflow ID (Unique for Field)
13- 14 I2 h RAh [15/19] Hour of Right Ascension (ICRS) (1)
16- 17 I2 min RAm Minute of Right Ascension (ICRS) (1)
19- 24 F6.3 s RAs Second of Right Ascension (ICRS) (1)
26- 26 A1 --- DE- [±] Sign of the Declination (ICRS)(1)
27- 28 I2 deg DEd [1/54] Degree of Declination (ICRS) (1)
30- 31 I2 arcmin DEm Arcminute of Declination (ICRS) (1)
33- 37 F5.2 arcsec DEs Arcsecond of Declination (ICRS) (1)
39- 46 A8 --- Color Lobe Color (2)
48- 54 F7.2 km.s-1 Vmin [-156/128] Velocity range, minimum (3)
56- 61 F6.2 km.s-1 Vmax [-71/194] Velocity range, maximum (3)
63- 68 F6.2 km.s-1 Vpeak [-87.1/151] Velocity peak aperture-integrated
spectrum (4)
70- 76 F7.1 mJy Fpeak [6.6/13430] Peak aperture-integrated flux density
78- 81 F4.1 mJy e_Fpeak [0.6/30] Uncertainty in Fpeak
83- 89 F7.3 Jy Ftot [0.059/570] Total aperture- and
velocity-integrated flux density
91- 96 F6.3 Jy e_Ftot [0.006/30] Lower uncertainty in Ftot
98-103 F6.3 Jy E_Ftot [0.006/40] Upper uncertainty in Ftot
105-122 A18 --- Class Classification (5)
--------------------------------------------------------------------------------
Note (1): The ICRS coordinates of the center of the bounding box for
each polygonal region. Uncertainties on each position are ±1 pixel,
where pixel sizes are listed in Table 2.
Note (2): Bipolar outflow candidates (classified as "red+blue") have
their properties listed on two consecutive rows instead of a single
row; the first line is always the blue lobe and the second line is
always the red lobe. Red and blue lobes in a bipolar candidate have
the same overall classification, i.e. both "likely," "possible," or
"complex or cluster."
Note (3): Velocity range is identified from aperture-integrated
intensities and position-velocity diagrams and shown in the
upper-right panels of Figures 1 and 2. In most cases, the velocity
range -5km/s<VLSR,candidate<+5km/s is excluded. In some rare cases,
we exclude more or less of the velocity range around VLSR,candidate,
based on line shape in the integrated spectrum.
Note (4): The velocity at which the aperture-integrated spectrum peaks,
within the velocity range listed in the preceding column. In other
words, this is the peak within an outflow candidate excluding the
ambient emission.
Note (5): Classifications as follows:
likely = candidates are those we consider significantly
likely to be protostellar outflows, based on their brightness,
morphology, aperture-integrated spectrum, and structure in the
PV diagram. Most of the candidates which have bright continuum
sources in or near the polygonal aperture fall into this
category;
possible = candidates are those we consider likely or
probable outflow candidates, but either their brightness,
morphology, spectral structure, or PV structure is not quite
definitive enough to place them in the "likely" class;
complex or cluster = candidates are those which clearly exhibit
high-velocity emission but either a) do not display the typical
morphology of a protostellar outflow or b) appear to be blended
emission from multiple outflows and individual driving sources
cannot be identified.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablec1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- Field Field or Clump
10- 11 I2 --- ID [1/47] Outflow ID (Unique for Field)
13- 30 A18 --- Class Classification (1)
32- 49 F18.1 cm-2 Ncolblue ? Median column density, blue lobe
51- 67 F17.1 cm-2 e_Ncolblue ? Uncertainty in Ncolblue, in
scaled MAD
69- 86 F18.1 cm-2 Ncolred ? Median column density, red lobe
88- 105 F18.1 cm-2 e_Ncolred ? Uncertainty in Ncolred, in
scaled MAD
107- 113 F7.4 Msun Mblue [0.003/10]? Mass, blue lobe
115- 120 F6.4 Msun e_Mblue [0.0006/0.6]? Lower Uncertainty in
Mblue
122- 127 F6.4 Msun E_Mblue [0.0007/0.2]? Upper Uncertainty in
Mblue
129- 135 F7.4 Msun Mred [0.003/14.1]? Mass, red lobe
137- 142 F6.4 Msun e_Mred [0.0003/0.4]? Lower Uncertainty in Mred
144- 149 F6.4 Msun E_Mred [0.0003/0.4]? Upper Uncertainty in Mred
151- 157 F7.4 Msun Mtot [0.005/14.1] Mass, total
159- 164 F6.4 Msun e_Mtot [0.0006/0.6] Lower Uncertainty in Mtot
166- 171 F6.4 Msun E_Mtot [0.0006/0.4] Upper Uncertainty in Mtot
173- 179 F7.3 km.Msun/s Pblue [0.019/402]? Momentum, blue lobe
181- 186 F6.3 km.Msun/s e_Pblue [0.003/13]? Lower Uncertainty in Pblue
188- 192 F5.3 km.Msun/s E_Pblue [0.004/6]? Upper Uncertainty in Pblue
194- 200 F7.3 km.Msun/s Pred [0.03/538]? Momentum, red lobe
202- 206 F5.3 km.Msun/s e_Pred [0.003/9]? Lower Uncertainty in Pred
208- 213 F6.3 km.Msun/s E_Pred [0.003/13]? Upper Uncertainty in Pred
215- 221 F7.3 km.Msun/s Ptot [0.03/538] Momentum, total
223- 228 F6.3 km.Msun/s e_Ptot [0.004/13] Lower Uncertainty in Ptot
230- 235 F6.3 km.Msun/s E_Ptot [0.004/13] Upper Uncertainty in Ptot
237- 244 E8.3 10-7J Eblue [/2.4e+47]? Kinetic energy, ergs, blue
lobe
246- 253 E8.3 10-7J e_Eblue ? Lower Uncertainty in Eblue
255- 261 E7.3 10-7J E_Eblue ? Upper Uncertainty in Eblue
263- 270 E8.3 10-7J Ered [/3.5e+47]? Kinetic energy, ergs, red
lobe
272- 278 E7.3 10-7J e_Ered ? Lower Uncertainty in Ered
280- 286 E7.3 10-7J E_Ered ? Upper Uncertainty in Ered
288- 295 E8.3 10-7J Etot [/3.5e+47] Kinetic energy, ergs, total
297- 304 E8.3 10-7J e_Etot Lower Uncertainty in Etot
306- 312 E7.3 10-7J E_Etot Upper Uncertainty in Etot
314- 320 F7.1 yr tdyn [510/70000]? Outflow dynamical time (2)
322- 328 F7.1 yr e_tdyn [80/10000]? Uncertainty in tdyn (2)
330- 336 E7.3 Msun.yr-1 Mdotblue [3.4e-07/0.006]? Mass flow rate, blue
lobe
338- 344 E7.3 Msun.yr-1 e_Mdotblue [7e-08/0.001]? Lower Uncertainty in
Mdotblue
346- 351 E6.3 Msun.yr-1 E_Mdotblue [8e-08/0.001]? Upper Uncertainty in
Mdotblue
353- 359 E7.3 Msun.yr-1 Mdotred [6e-07/0.004]? Mass flow rate, red
lobe
361- 366 E6.3 Msun.yr-1 e_Mdotred [1e-07/0.0005]? Lower Uncertainty in
Mdotred
368- 373 E6.3 Msun.yr-1 E_Mdotred [1e-07/0.0005]? Upper Uncertainty in
Mdotred
375- 381 E7.3 Msun.yr-1 Mdottot [1e-06/0.006]? Mass flow rate, total
383- 389 E7.3 Msun.yr-1 e_Mdottot [2e-07/0.001]? Lower Uncertainty in
Mdottot
391- 396 E6.3 Msun.yr-1 E_Mdottot [2e-07/0.001]? Upper Uncertainty in
Mdottot
398- 404 E7.3 km.Msun/s/yr Pdotblue [1.9e-06/0.22]? Momentum supply rate,
blue lobe
406- 411 E6.3 km.Msun/s/yr e_Pdotblue [4e-07/0.04]? Lower Uncertainty in
Pdotblue
413- 418 E6.3 km.Msun/s/yr E_Pdotblue [4e-07/0.04]? Upper Uncertainty in
Pdotblue
420- 426 E7.3 km.Msun/s/yr Pdotred [6e-06/0.17]? Momentum supply rate,
red lobe
428- 434 E7.3 km.Msun/s/yr e_Pdotred [1e-06/0.03]? Lower Uncertainty in
Pdotred
436- 441 E6.3 km.Msun/s/yr E_Pdotred [1e-06/0.03]? Upper Uncertainty in
Pdotred
443- 449 E7.3 km.Msun/s/yr Pdottot [6e-06/0.22]? Momentum supply rate,
total
451- 456 E6.3 km.Msun/s/yr e_Pdottot [1e-06/0.04]? Lower Uncertainty in
Pdottot
458- 463 E6.3 km.Msun/s/yr E_Pdottot [1e-06/0.04]? Upper Uncertainty in
Pdottot
465- 472 F8.3 Lsun Edotblue [0.001/1100]? Outflow power, blue lobe
474- 481 F8.4 Lsun e_Edotblue [0.0002/200]? Lower Uncertainty in
Edotblue
483- 490 F8.4 Lsun E_Edotblue [0.0002/200]? Upper Uncertainty in
Edotblue
492- 499 F8.4 Lsun Edotred [0.003/900]? Outflow power, red lobe
501- 507 F7.4 Lsun e_Edotred [0.0007/90]? Lower Uncertainty in
Edotred
509- 515 F7.4 Lsun E_Edotred [0.0007/90]? Upper Uncertainty in
Edotred
517- 525 F9.4 Lsun Edottot [0.003/1100]? Outflow power, total
527- 534 F8.4 Lsun e_Edottot [0.0007/200]? Lower Uncertainty in
Edottot
536- 543 F8.4 Lsun E_Edottot [0.0007/200]? Upper Uncertainty in
Edottot
--------------------------------------------------------------------------------
Note (1): Classifications as follows:
likely = candidates are those we consider significantly
likely to be protostellar outflows, based on their brightness,
morphology, aperture-integrated spectrum, and structure in the
PV diagram. Most of the candidates which have bright continuum
sources in or near the polygonal aperture fall into this
category;
possible = candidates are those we consider likely or
probable outflow candidates, but either their brightness,
morphology, spectral structure, or PV structure is not quite
definitive enough to place them in the "likely" class;
complex or cluster = candidates are those which clearly exhibit
high-velocity emission but either a) do not display the typical
morphology of a protostellar outflow or b) appear to be blended
emission from multiple outflows and individual driving sources
cannot be identified.
Note (2): Dynamical times are not reported for the complex or cluster class
nor where the outflow axis is unresolved on its longest axis.
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History:
From electronic version of the journal
References:
Motte et al. Paper I. 2022A&A...662A...8M 2022A&A...662A...8M
Ginsburg et al. Paper II. 2022A&A...662A...9G 2022A&A...662A...9G Cat. J/A+A/662/9
Pouteau et al. Paper III. 2022A&A...664A..26P 2022A&A...664A..26P Cat. J/A+A/664/A26
Brouillet et al. Paper IV. 2022A&A...665A.140B 2022A&A...665A.140B
Nony et al. Paper V. 2023A&A...674A..75N 2023A&A...674A..75N Cat. J/A+A/674/A75
Pouteau et al. Paper VI. 2023A&A...674A..76P 2023A&A...674A..76P
Cunningham et al. Paper VII. 2023A&A...678A.194C 2023A&A...678A.194C
Diaz-Gonzalez et al. Paper VIII. 2023ApJS..269...55D 2023ApJS..269...55D Cat. J/ApJS/269/55
Towner et al. Paper IX. 2024ApJ...960...48T 2024ApJ...960...48T This catalog
Armante et al. Paper X. 2024A&A...686A.122A 2024A&A...686A.122A
Bonfand et al. Paper XI. 2024A&A...687A.163B 2024A&A...687A.163B Cat. J/A+A/687/163
Dell'Ova et al. Paper XII. 2024A&A...687A.217D 2024A&A...687A.217D Cat. J/A+A/687/217
Alvarez-Gutierrez et al. Paper XIII. 2024A&A...689A..74A 2024A&A...689A..74A
Galvan-Madrid et al. Paper XIV. 2024ApJS..274...15G 2024ApJS..274...15G
Louvet et al. Paper XV. 2024A&A...690A..33L 2024A&A...690A..33L Cat. J/A+A/690/33
Motte et al. Paper XVI. 2025A&A...694A..24M 2025A&A...694A..24M Cat. J/A+A/694/24
Valeille-Manet et al. Paper XVII. 2025A&A...696A..11V 2025A&A...696A..11V Cat. J/A+A/696/11
Sandoval-Garrido et al. Paper XVIII. 2025A&A...696A.202S 2025A&A...696A.202S
Koley et al. Paper XIX. 2025A&A...702A.133K 2025A&A...702A.133K
Yoo et al. Paper XX. 2025ApJ...994..233Y 2025ApJ...994..233Y
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 06-Mar-2026