J/MNRAS/441/256 RCW 106 Giant Molecular Cloud NH3 emission (Lowe+, 2014)
Molecular line mapping of the giant molecular cloud associated with RCW 106.
IV. Ammonia towards dust emission.
Lowe V., Cunningham M.R., Urquhart J.S., Marshall J.P., Horiuchi S., Lo N.,
Walsh A.J., Jordan C.H., Jones P.A., Hill T.
<Mon. Not. R. Astron. Soc., 441, 256-273 (2014)>
=2014MNRAS.441..256L 2014MNRAS.441..256L
ADC_Keywords: H II regions ; Molecular clouds ; Radio sources
Keywords: stars: formation - ISM: clouds - ISM: molecules - ISM: structure -
radio lines: ISM
Abstract:
Here we report observations of the two lowest inversion transitions of
ammonia (NH3) with the 70-m Tidbinbilla radio telescope. The aim of
the observations is to determine the kinetic temperatures in the dense
clumps of the G333 giant molecular cloud associated with RCW 106 and
to examine the effect that accurate measures of temperature have on
the calculation of derived quantities such as mass. This project is
part of a larger investigation to understand the time-scales and
evolutionary sequence associated with high-mass star formation,
particularly its earliest stages. Assuming that the initial chemical
composition of a giant molecular cloud is uniform, any abundance
variations within will be due to evolutionary state. We have
identified 63 clumps using SEST Imaging Bolometer Array 1.2-mm dust
continuum maps and have calculated gas temperatures for most (78 per
cent) of these dense clumps. After using Spitzer Galactic Legacy
Infrared Mid-Plane Survey Extraordinaire 8.0µm emission to separate
the sample into infrared (IR)-bright and IR-faint clumps, we use
statistical tests to examine whether our classification shows
different populations in terms of mass and temperature.
Description:
We have utilized the 1.2-mm dust continuum emission from the SIMBA
instrument on the Swedish-ESO Telescope (SEST)
as a tracer for dense molecular material.
Observations using the 70-m Tidbinbilla radio telescope were conducted
in good weather conditions on 2011 July 11 and 12.
The G333 GMC was observed by Herschel with the Photoconductor Array
Camera and Spectrometer (PACS) and the Spectral and Photometric
Imaging Receiver (SPIRE) instruments in parallel mode at 70, 160, 250,
350 and 500um as part of the Open Time Key Programme `Hi-Gal' (PI: S.
Molinari; Molinari et al. 2010PASP..122..314M 2010PASP..122..314M).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 101 63 The parameters of the 63 SIMBA 1.2-mm dust
clumps identified with CLUMPFIND
table3.dat 97 51 Summary of physical parameters calculated
following Section 3.2 (NH3(1,1) non-detections
with a TA*<0.1K have been excluded)
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See also:
II/293 : GLIMPSE Source Catalog (I + II + 3D) (IPAC 2008)
VIII/96 : 6-GHz methanol multibeam maser catalog (Caswell+ 2010-12)
J/MNRAS/359/1498 : Class I and class II methanol masers (Ellingsen+, 2005)
J/other/PASA/26.454 : Precise positions of methanol masers (Caswell, 2009)
J/MNRAS/416/1764 : H2O Southern Galactic Plane Survey (HOPS) (Walsh+, 2011)
J/MNRAS/367/1609 : RCW 106 Giant Molecular Cloud 13CO mapping (Bains+, 2006)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- ID1 [1/63] Sequential number
4- 17 A14 --- Clump Clump name (GLLL.lll+B.bbb)
19- 20 I2 h RAh Clump centroid right ascension (J2000)
22- 23 I2 min RAm Clump centroid right ascension (J2000)
25- 28 F4.1 s RAs Clump centroid right ascension (J2000)
30 A1 --- DE- Clump centroid declination sign (J2000)
31- 32 I2 deg DEd Clump centroid declination (J2000)
34- 35 I2 arcmin DEm Clump centroid declination (J2000)
37- 38 I2 arcsec DEs Clump centroid declination (J2000)
40- 43 F4.1 Jy Peak SIMBA 1.2mm peak flux (in Jy/beam)
45- 48 F4.2 pc Rad Clump radius
50- 54 F5.1 Jy Int SIMBA 1.2mm total integrated flux
56- 71 A16 --- Assoc Nearby (<30") IR and maser associations (1)
72- 89 A18 --- RMStype Type of RMS object if RMS object in Assoc (2)
91- 99 A9 --- IRtype Infrared type (IR-bright or IR-faint) (3)
101 A1 --- Reg Region (A B C) where the clump has been
allocated to (see Section 4.3 for more details)
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Note (1): nearby (<30") IR and maser associations for each clump, with the
number denoting the quantity:
n = denotes Spitzer 3.6um emission (Benjamin et al. 2003PASP..115..953B 2003PASP..115..953B,
Cat. II/293; Churchwell et al., 2009PASP..121..213C 2009PASP..121..213C; Spitzer Science
Center 2009)
s = denotes Spitzer 4.5um emission (Benjamin et al. 2003PASP..115..953B 2003PASP..115..953B,
Cat. II/293; Churchwell et al., 2009PASP..121..213C 2009PASP..121..213C; Spitzer Science
Center 2009)
p = denotes Spitzer 8.0um emission (Benjamin et al. 2003PASP..115..953B 2003PASP..115..953B,
Cat. II/293; Churchwell et al., 2009PASP..121..213C 2009PASP..121..213C; Spitzer Science
Center 2009)
h = denotes the presence of a Herschel 160um source
o = denotes an OH maser
M1 = denotes a 44.07GHz Class I CH3OH maser
M2 = denotes a 95.1GHz Class I methanol maser
m1 = denotes a 6.7GHz Class II CH3OH maser
m2 = denotes a 12.2GHz Class II CH3OH maser
w = denotes a H2O maser
References:
* water 22GHz H2O maser = Braz & Scalise, 1982A&A...107..272B 1982A&A...107..272B; Breen et al.,
2007MNRAS.377..491B 2007MNRAS.377..491B, 2010MNRAS.406.1487B 2010MNRAS.406.1487B; Walsh et al.,2011MNRAS.416.1764W 2011MNRAS.416.1764W,
Cat. J/MNRAS/416/1764
* Class I 44.01GHz maser = Slysh et al., 1994MNRAS.268..464S 1994MNRAS.268..464S; Voronkov et al.,
2014MNRAS.439.2584V 2014MNRAS.439.2584V, Cat. J/MNRAS/439/2584
* Class I 95.1GHz maser = Ellingsen, 2005MNRAS.359.1498E 2005MNRAS.359.1498E, J/MNRAS/359/1498)
* Class II 6.7GHz methanol (CH3OH) maser = Caswell 1996MNRAS.279...79C 1996MNRAS.279...79C,
1997MNRAS.289..203C 1997MNRAS.289..203C, 2009PASA...26..454C 2009PASA...26..454C, Cat. J/other/PASA/26.454;
Caswell et al., 2011MNRAS.417.1964C 2011MNRAS.417.1964C, Cat. VIII/96; Ellingsen et al.,
1996MNRAS.280..378E 1996MNRAS.280..378E
* Class II 12.2GHz methanol (CH3OH) maser = Breen et al. 2012MNRAS.421.1703B 2012MNRAS.421.1703B
* Class II hydroxyl OH maser 1665, 1667 and 1720MHz = Caswell, Haynes & Goss,
1980AuJPh..33..139B 1980AuJPh..33..139B; Caswell, Vaile & Forster, 1995MNRAS.277..210C 1995MNRAS.277..210C;
Caswell, 1998MNRAS.297..215C 1998MNRAS.297..215C and 6.035GHz; Caswell, 1997MNRAS.289..203C 1997MNRAS.289..203C)
Note (2): If a Red MSX Source (RMS) object was within 30" of the SIMBA
dust peak. Types are "Diffuse HII region", "HII region", "YSO", or
combinations of these.
Note (3): identifies whether the clump has been classified,
via Spitzer 8.0um GLIMPSE emission, as IR-bright or IR-faint.
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID3 [1/63] Sequential number
4- 17 A14 --- Clump Clump name (GDDD.ddd+B.bbb)
19 A1 --- l_Trot Limit flag on Trot
20- 23 F4.1 K Trot [9/36]?=- Rotation temperature
25 A1 --- l_Tkin Limit flag on Tkin
26- 29 F4.1 K Tkin [9/64]?=- Kinematic temperature
31 A1 --- l_logN Limit flag on logN
32- 35 F4.1 [cm-2] logN [14/17]?=- NH3 column density
37 A1 --- l_logn Limit flag on logn
38- 41 F4.2 [cm-3] logn [3.6/6.2]?=- H2 volume density
43 A1 --- l_TA*1 Limit flag on TA*1
44- 46 F3.1 K TA*1 [0.2/2.5] NH3(1,1) antenna temperature scale
48- 53 F6.2 km/s V1 ?=- NH3(1,1) LSR velocity
55- 58 F4.2 km/s DV1 ?=- NH3(1,1) FWHM
60- 63 F4.2 --- tau1 ?=- Optical depth of NH3 transition,
τ(m,1,1)
65- 67 F3.1 K TA*2 [0.1/1.8]?=- NH3(2,2) antenna temperature
69- 74 F6.2 km/s V2 ?=- NH3(2,2) LSR velocity
76- 79 F4.2 km/s DV2 ?=- NH3(2,2) FWHM
81- 84 F4.2 [Msun] logMCl [2.4/4.2]?=- Clump mass
86- 89 F4.2 [Msun] logMVir [2.0/3.7]?=- Virial mass
91- 97 A7 --- Spect Spectral features (4)
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Note (4): Spectral features are:
H = NH3(1,1) hyperfine structure
A = absorption feature for NH3(1,1)
B = blended spectra for NH3(1,1)
g = Gaussian was fit to the NH3(2,2)
hg = NH3(2,2) hyperfine structure could be seen but since the
signal-to-noise ratio was below 3σ, a Gaussian was used to
model the fit
g* = a NH3(2,2) characteristic not included in any of the other cases
(see Section 3.2 for further details)
a = absorption feature for NH3(2,2)
b = blended spectra for NH3(2,2)
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History:
From electronic version of the journal
References:
Bains et al., Paper I 2006MNRAS.367.1609B 2006MNRAS.367.1609B, Cat. J/MNRAS/367/1609
Wong et al., Paper II 2008MNRAS.386.1069W 2008MNRAS.386.1069W
Lo et al., Paper III 2009MNRAS.395.1021L 2009MNRAS.395.1021L
(End) Patricia Vannier [CDS] 31-Jan-2015