J/ApJS/235/15 CO obs. toward Gem OB1 molecular cloud complex. II. (Li+, 2018)
Molecular gas toward the Gemini OB1 molecular cloud complex.
II. CO outflow candidates with possible WISE associations.
Li Y., Li F.-C., Xu Y., Wang C., Du X.-Y., Yang W., Yang J.
<Astrophys. J. Suppl. Ser., 235, 15-15 (2018)>
=2018ApJS..235...15L 2018ApJS..235...15L (SIMBAD/NED BibCode)
ADC_Keywords: Molecular clouds; Interstellar medium; Carbon monoxide;
Galactic plane
Keywords: ISM: jets and outflows; ISM: Molecules; stars: formation
Abstract:
We present a large-scale survey of CO outflows in the Gem OB1
molecular cloud complex and its surroundings, using the Purple
Mountain Observatory Delingha 13.7m telescope. A total of 198 outflow
candidates were identified over a large area (∼58.5deg2), of which
193 are newly detected. Approximately 68% (134/198) are associated
with the Gem OB1 molecular cloud complex, including clouds GGMC 1,
GGMC 2, BFS 52, GGMC 3, and GGMC 4. Other regions studied are: the
Local arm (Local Lynds, West Front), Swallow, Horn, and Remote cloud.
Outflow candidates in GGMC 1, BFS 52, and Swallow are mainly located
at ring-like or filamentary structures. To avoid excessive uncertainty
in distant regions (≳3.8kpc), we only estimated the physical
parameters for clouds in the Gem OB1 molecular cloud complex and in
the Local arm. In those clouds, the total kinetic energy and the
energy injection rate of the identified outflow candidates are ≲1%
and ≲3% of the turbulent energy and the turbulent dissipation rate of
each cloud, indicating that the identified outflow candidates cannot
provide enough energy to balance turbulence of their host cloud at the
scale of the entire cloud (several to dozens of parsecs). The
gravitational binding energy of each cloud is ≳135 times the total
kinetic energy of the identified outflow candidates within the
corresponding cloud, indicating that the identified outflow candidates
cannot cause major disruptions to the integrity of their host cloud at
the scale of the entire cloud.
Description:
The observations of 12CO(1-0) (115.271GHz) and 13CO(1-0)
(110.201GHz) were used to search for outflows in GOS (the Gem OB1
molecular cloud complex and its surroundings). These data are a part
of the Milky Way Imaging Scroll Painting Project (MWISP), which is a
survey of the northern Galactic plane within -10.25°≤l≤250.25°
and -5.25°≤b≤5.25°, as well as other regions of interest.
The 12CO and 13CO molecular lines were observed simultaneously
between 2012 September and 2013 May using the Purple Mountain
Observatory Delingha (PMODLH) 13.7m telescope with its nine-beam
superconducting array receiver (SSAR).
The pointing accuracy was better than 4" during the observations. The
receiver provides a total bandwidth of 1GHz over 16384 channels for
both the upper and lower sidebands, corresponding to velocity
resolutions of about 0.16km/s for 12CO and 0.17km/s for 13CO,
respectively.
GOS can be decomposed to 10 sub-regions (all of which are molecular
clouds; see details in Paper I; Wang+ 2017ApJS..230....5W 2017ApJS..230....5W). These
sub-regions are listed in Table 1, which summarizes the distances and
main component velocity ranges (13CO).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 30 10 Distances and velocity ranges (13CO) of the
10 sub-regions
table12.dat 63 198 Outflow sample statistics
table13.dat 76 199 Physical properties of the outflow samples
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See also:
VII/20 : Catalogue of HII Regions (Sharpless 1959)
VII/50 : CO Radial Velocities Toward Galactic H II Regions (Blitz+ 1982)
VIII/39 : Composite CO Survey of the Milky Way (Dame+ 1987)
J/A+A/426/503 : Cat. of high velocity molecular outflows (Update) (Wu+ 2004)
J/A+A/472/187 : 12CO outflows towards submm cores in Perseus (Hatchell+, 2007)
J/ApJ/688/1142 : Star formation in W5: Spitzer observations (Koenig+, 2008)
J/ApJS/181/321 : Properties of Spitzer c2d dark clouds (Evans+, 2009)
J/ApJS/186/259 : Taurus Spitzer survey: new candidate members (Rebull+, 2010)
J/MNRAS/418/2121 : CO 3-2 observations of outflows in W5 (Ginsburg+, 2011)
J/MNRAS/432/3445 : YSOs on HII complex Sh2-252 (Jose+, 2013)
J/A+A/556/A65 : LDN 1570 BV(RI)c polarisation & photometry (Eswaraiah+, 2013)
J/ApJ/774/22 : CO observations of YSOs in NGC 1333 (Plunkett+, 2013)
J/A+A/569/A11 : G35.20-0.74N cont. and line data cubes (Sanchez-Monge+, 2014)
J/ApJS/219/20 : Outflows and bubbles in Taurus (Li+, 2015)
J/A+A/594/A28 : Planck Catalog of Galactic cold clumps (PGCC) (Planck+, 2016)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Reg Sub-region identifier
13- 15 F3.1 kpc Dist Distance
16 A1 --- u_Dist [?] ?=the distances are undetermined (1)
18- 19 I2 km/s Vel1 [-5/16] 13CO lower velocity range
21- 22 I2 km/s Vel2 [7/28] 13CO upper velocity range
24- 30 A7 --- Ref Reference(s) (2)
--------------------------------------------------------------------------------
Note (1): We adopted the recommended distances in
Paper I (Wang+ 2017ApJS..230....5W 2017ApJS..230....5W).
Note (2): References as follows:
1 = Carpenter et al. (1995ApJ...450..201C 1995ApJ...450..201C)
2 = Reid et al. (2009ApJ...693..397R 2009ApJ...693..397R)
3 = Niinuma et al. (2011PASJ...63....9N 2011PASJ...63....9N)
4 = Rygl et al. (2010A&A...511A...2R 2010A&A...511A...2R)
5 = Bok & McCarthy (1974AJ.....79...42B 1974AJ.....79...42B)
6 = Eswaraiah et al. (2013, J/A+A/556/A65)
7 = Planck Collaboration et al. (2015, J/A+A/594/A28)
8 = Paper I (Wang+ 2017ApJS..230....5W 2017ApJS..230....5W)
9 = Moffat et al. (1979A&AS...38..197M 1979A&AS...38..197M).
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Byte-by-byte Description of file: table12.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Reg Sub-region identifier as in Table 1
13- 17 A5 --- ID Identifier
19- 25 F7.3 deg GLON [187/195.1] Galactic longitude
27- 32 F6.3 deg GLAT [-3.4/1.8] Galactic latitude
34- 37 F4.1 km/s bLWVel1 [-7/21.3]? Blue line wing velocity lower range
39- 42 F4.1 km/s bLWVel2 [-3.5/23.1]? Blue line wing velocity upper range
44- 47 F4.1 km/s rLWVel1 [1.5/27.5]? Red line wing velocity lower range
49- 52 F4.1 km/s rLWVel2 [3/30]? Red line wing velocity upper range
54- 56 A3 --- Qb-Qr Blue-Red quality level flag (A=most reliable) (1)
58- 59 A2 --- WISE? WISE detection?
61 A1 --- New? New detection?
63 A1 --- r_New? Reference if not new (2)
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Note (1): Because the outflow candidates with score D were removed
from the final sample (see Appendix A.6), we did not include them in
this table. Code as follows:
A = high-velocity outflows and the most reliable outflow candidates
B = reliable
C = the characteristics of the outflows are not obvious, but we cannot rule
out the possibility of outflow activity in those candidates
Note (2): Reference as follows:
a = Wu et al. (2004, J/A+A/426/503) and references therein.
b = Bally & Lada (1983ApJ...265..824B 1983ApJ...265..824B).
c = Snell et al. (1988ApJ...325..853S 1988ApJ...325..853S).
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Byte-by-byte Description of file: table13.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 --- Reg Sub-region identifier as in Table 1
13- 17 A5 --- ID Identifier
19- 22 A4 --- Lobe Lobe: "Red" or "Blue"
24- 30 F7.3 deg GLON [187/194.7] Galactic longitude
32- 37 F6.3 deg GLAT [-3.4/1.8] Galactic latitude
39- 41 F3.1 km/s DelV [1/7.1] Lobe velocity, <Δνlobe>
43- 46 F4.2 pc llobe [0.28/5.7] Length, llobe
48- 52 F5.2 Msun Mlobe [0.02/11.4] Mass
54- 58 F5.2 Msun.km/s Plobe [0.05/53.2] Momentum, Plobe
60- 65 F6.2 10+36J Elobe [0.06/365] Kinetic energy
67- 70 F4.1 10+5yr tlobe [0.4/22.3] Dynamical timescale
72- 76 F5.1 10+23W Llobe [0.1/358] Luminosity, Llobe
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History:
From electronic version of the journal
References:
Wang et al. Paper I. 2017ApJS..230....5W 2017ApJS..230....5W
Wang et al. Paper III. 2019ApJS..243...25W 2019ApJS..243...25W
(End) Emmanuelle Perret [CDS] 06-Oct-2023