J/A+A/622/A135 Mid-J CO emission of Top100 clumps (Navarete+, 2019)
ATLASGAL-selected high-mass clumps in the inner Galaxy.
VII. Characterisation of mid-J CO emission.
Navarete F., Leurini S., Giannetti A., Wyrowski F., Urquhart J.S.,
Koenig C., Csengeri T., Guesten R., Damineli A., Menten K.M.
<Astron. Astrophys. 622, A135 (2019)>
=2019A&A...622A.135N 2019A&A...622A.135N (SIMBAD/NED BibCode)
ADC_Keywords: Interstellar medium ; Molecular clouds ; Radial velocities ;
Line Profiles
Keywords: astrochemistry - stars: formation - stars: protostars -
ISM: molecules - ISM: kinematics and dynamics - line: profiles
Abstract:
High-mass stars are formed within massive molecular clumps, where a
large number of stars form close together. The evolution of the clumps
with different masses and luminosities is mainly regulated by their
high-mass stellar content and the formation of such objects is still
not well understood.
In this work, we characterise the mid-J CO emission in a statistical
sample of 99 clumps (TOP100) selected from the ATLASGAL survey that
are representative of the Galactic proto-cluster population.
High-spatial resolution APEX-CHAMP+ maps of the CO (6-5) and CO (7-6)
transitions were obtained and combined with additional single-pointing
APEX-FLASH+ spectra of the CO (4-3) line. The data were convolved to a
common angular resolution of 13.4". We analysed the line profiles by
fitting the spectra with up to three Gaussian components, classified
as narrow or broad, and computed CO line luminosities for each
transition. Additionally, we defined a distance-limited sample of 72
sources within 5kpc to check the robustness of our analysis against
beam dilution effects. We have studied the correlations of the line
luminosities and profiles for the three CO transitions with the clump
properties and investigate if and how they change as a function of the
evolution.
All sources were detected above 3-σ in all three CO transitions
and most of the sources exhibit broad CO emission likely associated
with molecular outflows. We find that the extension of the mid-J CO
emission is correlated with the size of the dust emission traced by
the Herschel-PACS 70um maps. The CO line luminosity (LCO) is
correlated with the luminosity and mass of the clumps. However, it
does not correlate with the luminosity-to-mass ratio.
The dependency of the CO luminosity with the properties of the clumps
is steeper for higher-J transitions. Our data seem to exclude that
this trend is biased by self-absorption features in the CO emission,
but rather suggest that different J transitions arise from different
regions of the inner envelope. Moreover, high-mass clumps show similar
trends in CO luminosity as lower mass clumps, but are systematically
offset towards larger values, suggesting that higher column density
and (or) temperature (of unresolved) CO emitters are found inside
high-mass clumps.
Description:
The tabular data contain the entries of the full Tables A.1-A.7 from
Appendix A.
tablea1.dat presents the properties of the observed clumps.
tablea2.dat, tablea3.dat and tablea4.dat present the Gaussian
components of each source for the CO(4-3), CO(6-5) and CO(7-6)
transitions, respectively.
The extension of the CO(6-5) emission is listed in tablea5.dat.
tablea6.dat displays the integrated properties of the CO lines studied
in this work.
Finally, the excitation temperature derived from the CO(6-5) spectra
is presented in tablea7.dat.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 112 99 Properties of the TOP100 sources
tablea2.dat 87 66 Gaussian decomposition of the CO(4-3) profiles
tablea3.dat 87 91 Gaussian decomposition of the CO(6-5) profiles
tablea4.dat 87 95 Gaussian decomposition of the CO(7-6) profiles
tablea5.dat 78 99 Extension of the CO(6-5) and the Herschel-PACS
70 micron emission towards the TOP100 clumps
tablea6.dat 123 99 Integrated properties of the CO emission
profiles convolved to 13.4"
tablea7.dat 51 99 Excitation temperature of the TOP100 clumps
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See also:
J/A+A/570/A65 : ATLASGAL massive clumps CO depletion (Giannetti+, 2014)
J/A+A/586/A149 : SiO in ATLASGAL-selected massive clumps (Csengeri+, 2016)
J/A+A/599/A139 : ATLASGAL massive clumps dust characterization (Koenig+, 2017)
J/A+A/602/A37 : Millimeter RRL in ATLASGAL-selected massive clumps (Kim+ 2017)
J/A+A/603/A33 : Temperature evolution in massive clumps (Giannetti+, 2017)
J/A+A/611/A6 : ATLASGAL massive clumps H2CO data (Tang+, 2018)
Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID [1/99] ID of the TOP100 clump
4- 21 A18 --- CSC CSC Name (AGALLLL.lll+BB.bbb)
23- 24 I2 h RAh Right ascension (J2000)
26- 27 I2 min RAm Right ascension (J2000)
29- 33 F5.2 s RAs Right ascension (J2000)
35 A1 --- DE- Declination sign (J2000)
36- 37 I2 deg DEd Declination (J2000)
39- 40 I2 arcmin DEm Declination (J2000)
42- 45 F4.1 arcsec DEs Declination (J2000)
47- 51 F5.1 arcsec OffX Offset in the RA axis between the CSC position
and the centre of the CHAMP+ map
53- 57 F5.1 arcsec OfFY Offset in the Dec axis between the CSC
position and the centre of the CHAMP+ map
59- 74 A16 --- GCSC GCSC Name (GLLL.llll+BB.bbbb)
76- 80 F5.1 arcsec OfFXg Offset in the RA axis between the GCSC
position and the centre of the CHAMP+ map
82- 86 F5.1 arcsec OfFYg Offset in the Dec axis between the GCSC
position and the centre of the CHAMP+ map
88- 93 F6.1 km/s Vlsr Radial velocity of the clump
95- 98 F4.1 kpc Dist Distance of the clump
100-103 F4.2 [Lsun] logL Bolometric luminosity of the clump
(in logarithm of solar luminosities)
105-108 F4.2 [Msun] logM Mass of the clump
(in logarithm of solar masses)
110-112 A3 --- Class Classification of the clump (1)
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Note (1): Classification of the clump as follows:
70w = 70-micron weak
IRw = infrared weak
IRb = infrared bright
HII = HII region
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Byte-by-byte Description of file: tablea[234].dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID [1/99] ID of the TOP100 clump
4- 21 A18 --- CSC CSC Name (AGALLLL.lll+BB.bbb)
23- 24 A2 --- C1 Classification of the Gaussian component No. 1
26- 31 F6.1 km/s Vpeak1 Peak velocity of the component No. 1
33- 37 F5.1 km/s FWHM1 Full-width at half maximum of component No. 1
39- 43 F5.1 K Tpeak1 Peak temperature of the component No. 1
45- 46 A2 --- C2 Classification of the Gaussian component No. 2
48- 53 F6.1 km/s Vpeak2 ?=- Peak velocity of the component No. 2
55- 59 F5.1 km/s FWHM2 ?=- Full-width at half maximum of
component No. 2
61- 65 F5.1 K Tpeak2 ?=- Peak temperature of the component No. 2
67- 68 A2 --- C3 Classification of the Gaussian component No. 3
70- 75 F6.1 km/s Vpeak3 ?=- Peak velocity of the component No. 2
77- 81 F5.1 km/s FWHM3 ?=- Full-width at half maximum of
component No. 2
83- 87 F5.1 K Tpeak3 ?=- Peak temperature of the component No. 3
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Byte-by-byte Description of file: tablea5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID [1/99] ID of the TOP100 clump
4- 21 A18 --- CSC CSC Name (AGALLLL.lll+BB.bbb)
23- 27 F5.1 arcsec COmax ?=- Maximum elongation of the CO emission
29- 33 F5.1 arcsec COmin ?=- Minimum elongation of the CO emission
35- 39 F5.1 arcsec COavg ?=- Mean elongation of the CO emission
41- 45 F5.3 pc COlin ?=- Linear mean elongation of the CO emission
47- 51 F5.3 pc e_COlin ?=- Error on the linear mean elongation of
the CO emission
53- 56 F4.1 arcsec 70max ?=- Maximum elongation of the FIR emission
58- 61 F4.1 arcsec 70min ?=- Minimum elongation of the FIR emission
63- 66 F4.1 arcsec 70avg ?=- Mean elongation of the FIR emission
68- 72 F5.3 pc 70lin ?=- Linear mean elongation of the FIR emission
74- 78 F5.3 pc e_70lin ?=- Error on the linear mean elongation of
the FIR emission
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Byte-by-byte Description of file: tablea6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID [1/99] ID of the TOP100 clump
4- 21 A18 --- CSC CSC Name (AGALLLL.lll+BB.bbb)
23- 26 F4.2 K rms43 rms of the CO(4-3) profiles
28- 30 I3 km/s FWZP43 full width at zero power of the line
32- 38 F7.2 K.km/s Sint43 integrated intensity of the line
40- 46 F7.2 K.km/s/pc2 LCO43 line luminosity of the CO emission
48- 53 F6.2 K.km/s/pc2 e_LCO43 uncertainty on the line luminosity
55 A1 --- f43 [*] an asterisk mark indicates if the
line is contaminated by a
self-absorption feature
57- 60 F4.2 K rms65 rms of the CO(6-5) profiles
62- 64 I3 km/s FWZP65 full width at zero power of the line
66- 72 F7.2 K.km/s Sint65 integrated intensity of the line
74- 80 F7.2 K.km/s/pc2 LCO65 line luminosity of the CO emission
82- 87 F6.2 K.km/s/pc2 e_LCO65 uncertainty on the line luminosity
89 A1 --- f65 [*] an asterisk mark indicates if the
line is contaminated by a
self-absorption feature
91- 94 F4.2 K rms76 rms of the CO(6-5) profiles
96- 98 I3 km/s FWZP76 full width at zero power of the line
100-106 F7.2 K.km/s Sint76 integrated intensity of the line
108-114 F7.2 K.km/s/pc2 LCO76 line luminosity of the CO emission
116-121 F6.2 K.km/s/pc2 e_LCO76 uncertainty on the line luminosity
123 A1 --- f76 [*] an asterisk mark indicates if the
line is contaminated by a
self-absorption feature
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- ID [1/99] ID of the TOP100 clump
4- 21 A18 --- CSC CSC Name (AGALLLL.lll+BB.bbb)
23- 27 F5.1 K Tex Excitation temperature derived from the peak
intensity of the CO(6-5) line
29- 31 F3.1 K e_Tex Uncertainty of the excitation temperature
33- 37 F5.1 K GTex Excitation temperature derived from the peak
intensity of the Gaussian fit of the CO(6-5) line
39- 43 F5.1 K E_GTex Upper uncertainty of the GTex value
45- 49 F5.1 K e_GTex Lower uncertainty of the GTex value
51 A1 --- f_Tex [*] Note on Tex (2)
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Note (2): an asterisk mark indicates the cases where the excitation temperature
was obtained from the equation listed in tablea7.dat and in Sect. 4.4:
log(Tex)=(0.75±0.10)+(0.21±0.02)log(Lbol).
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Acknowledgements:
Felipe Navarete, navarete(at)gmail.com
Max-Planck Institute for Radio Astronomy
References:
Giannetti et al., Paper I 2014A&A...570A..65G 2014A&A...570A..65G, Cat. J/A+A/570/A65
Csengeri et al., Paper II 2016A&A...586A.149C 2016A&A...586A.149C, Cat. J/A+A/586/A149
Konig et al., Paper III 2017A&A...599A.139K 2017A&A...599A.139K, Cat. J/A+A/599/A139
Kim et al., Paper IV 2017A&A...602A..37K 2017A&A...602A..37K, Cat. J/A+A/602/A37
Giannetti et al., Paper V 2017A&A...603A..33G 2017A&A...603A..33G, Cat. J/A+A/603/A33
Tang et al., Paper VI 2018A&A...611A...6T 2018A&A...611A...6T, Cat. J/A+A/611/A6
(End) Felipe Navarete [Max-Planck Inst], Patricia Vannier [CDS] 06-Jan-2019