ELSEVIER Chinese Astronomy and Astrophysics 38 (2014) 265–293

CHINESEASTRONOMYAND ASTROPHYSICS

12CO J=2-1 and J=3-2 Line Observations ofMolecular Clouds toward the Directions of 59

EGOs in the Northern Sky† �

LI Zhi-guang1,2,3� HE Jin-hua1,2

1Yunnan Astronomical Observatory, Chinese Academy of Sciences, Kunming 6500112Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of

Sciences, Kunming 6500113University of Chinese Academy of Sciences, Beijing 100049

Abstract In order to investigate the differences between the molecular cloudswhich are associated with the massive star forming regions and those which arenot, we have performed the single-dish simultaneous observations of 12CO J=2-1and J=3-2 lines toward a sample of 59 Spitzer Extended Green Objects (EGOs)as the massive star forming regions in the northern sky. Combining our resultswith the data of the 12CO J=1-0 observations toward the same sample EGOs inthe literature, we have made the statistical comparisons on the intensities andlinewidths of multiple 12CO lines between the molecular clouds associated withEGOs (EGO molecular clouds, in brief) and other non-EGO molecular clouds.On this basis, we have discussed the effects of the gas temperature, density, andvelocity field distributions on the statistical characteristics of the two kinds ofmolecular clouds. It is found that both the EGO molecular clouds and non-EGO molecular clouds have similar mass ranges, hence we conclude that forthe formation of massive stars, the key-important factor is probably not thetotal mass of a giant molecular cloud (GMC), but the volume filling factor of themolecular clumps in the GMC (or the compression extent of the molecular gasin the cloud).

Key words: stars: formation—ISM: clouds—ISM: spectral lines and bands—ISM: molecules —submillimeter: ISM

† Supported by National Natural Science Foundation (11173056)Received 2013–04–02; revised version 2013–04–29

� A translation of Acta Astron. Sin. Vol. 55, No. 1, pp. 40–65, 2014� lzhg04wj@ynao.ac.cn

0275-1062/01/$-see front matter c© 2014 Elsevier Science B. V. All rights reserved.PII:

0275-1062/14/$-see front matter © 2014 Elsevier B.V. All rights reserved.doi:10.1016/j.chinastron.2014.07.005

266 Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293

1. INTRODUCTION

The study of large-mass star formation is a very active research field at present. By meansof stellar wind, jet, HII region collision, and supernova explosion, the massive stars releasea large amount of heavy elements and ultraviolet radiation to the cosmic space, which affectthe formation processes of other stars and planets, and further the chemical and physicalproperties, as well as the morphologic structure of the whole galaxy via the interactions withthe parent molecular cloud.

However, the human knowledge on the large-mass star formation is much less than thatof small-mass star formation. In which the main reason is the difficulty of observation. Thelarge-mass star forming regions are generally very distant, and most of them are situatedon the Galactic plane, hence heavy extinction exists at the optical waveband, in addition tothe short evolutionary timescale of large-mass stars, the number of forming large-mass starswhich can be observed and studied is very small.

According to the review made by Zinnecker et al.[1], now in observation the processof large-mass star formation is roughly divided into four stages: (1) IR dark cloud; (2) hotmolecular core; (3) hypercompact and ultracompact HII regions; and (4) compact and clas-sical HII regions. Similarly in theory the process of large-mass star formation can also bedivided into four stages: (1) the formation of cool and dense molecular cloud core or fila-mentary structure; (2) the gravitational collapse of molecular cloud core; (3) the accretionof mass; and (4) the disruption of parent molecular cloud. But these theoretically dividedevolutionary stages can hardly correspond one by one strictly to the stages divided in ob-servation. These are only the rough divisions of the process of large-mass star formation,in fact, about the formation of large-mass stars there are still many problems remained tosolve, for example, the formation of a large-mass star is caused by whether the accretionof a single star or the merge of small molecular clouds? how about the cloud structure inthe young massive star formation region? what are the conditions for the formation of alarge-mass star? what is the relation between the mass of the finally formed star and theproperty of its parent molecular cloud? and so on.

From the Galactic infrared survey observation of the Spitzer infrared space telescope,Cyganowski et al.[2] found a group (about 300) of new objects—Extended Green Objects (EGOs).By the statistical study on the correlations of the EGOs with the infrared dark clouds andtype-II methanol masers, as well as their positions on the infrared color-color diagram, theyverified the reasonableness that the EGOs may be the candidates of large-mass star forma-tion regions. This increases about one fold of observational sample for the exploration oflarge-mass star formation, and provides us with new opportunities to study the process oflarge-mass star formation by observations.

Recently, people have made a series of succeeding multi-wavelength observations on thisgroup of EGOs, including the millimeter wave single-point spectral observations of H13CO+

J=1-0, 12CO J=1-0, 13CO J=1-0, and C18O J=1-0 lines, that were made by Chen et al.[3]

toward a group of EGOs in the northern sky with the 13.7m millimeter radio telescope ofPurple Mountain Observatory at Delingha. They obtained the conclusion that the infallmotion of matter exists in these EGOs. Dr. Cyganowski, the discoverer of EGOs, madehimself the millimeter wave single-dish spectral observations and the interferometric imagingobservations on some selected EGOs[4−5] in detail, and made comparison with the result of

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methanol maser observations, he confirmed that the phenomena of jets really exist in theseobjects, and discussed the mechanism for the coexistence of different kinds of methanolmasers in the EGOs. He et al.[6] made the single-dish spectral observations at the molecularlines H13CO+ J=3-2, SiO J=6-5 and the SO, CH3OH lines to trace the dense gas of a groupof EGOs in the northern sky, and made a joint statistical analysis in combination with theobserved data of the CO isotopic lines 12CO J=1-0, 13CO J=1-0, and C18O J=1-0, theyrevealed that most EGO molecular clouds are associated with dense gas, many EGOs exhibitjets and shocks, and that the different EGO molecular clouds exhibit universal similaritiesin density and temperature structures.

In this work, using the KOSMA 3m sub-millimeter wave telescope we make the spec-tral observations at the rotational transition lines 12CO J=2-1 and J=3-2 on a group ofEGOs in the northern sky, and in combination with the data observed previously at the12CO J=1-0 line with the Delingha 13.7m telescope[3], we statistically analyze the differ-ences between the molecular clouds associated with EGOs (EGO molecular clouds) and theother molecular clouds without large-mass star formation in the same directions (non-EGOmolecular clouds), and hereby to reveal the environmental characteristics of the molecularclouds associated with large-mass star formation regions.

2. OBSERVATION AND DATA PROCESSING

On 5th-13th Nov. 2009, with the German 3m diameter KOSMA sub-millimeter wave tele-scope on the Gornergrat mountain in the Swiss Alps before its moving to Yangbajing inTibet, we made the single-point spectral observations at the 12CO J=2-1 (230.538GHz) andJ=3-2 (345.796GHz) molecular lines toward 59 EGOs in the northern sky. The positions ofthese objects were taken from Reference [2]. The KOSMA’s double-sideband receiver wasused to observe simultaneously the two spectral lines, this would help to reduce the fluxcalibration error between the two spectral lines. The acousto-optic spectrometers (AOSs) ofhigh resolution (HRS) and of low resolution (LRS), and a digital Fourier transform spec-trometer (DFT) were simultaneously used to analyze the spectral signal of the 12CO J=2-1line, and an AOS of variable resolution (VRS) was used to analyze the spectral signal of the12CO J=3-2 line. In this work, we adopted mainly the data of LRS (1.419GHz bandwidthfor 1048 channels) and VRS (0.695GHz bandwidth for 2048 channels). Because of the oc-casional failure of the LRS, for the G35.20-0.74, G39.39-0.14, G44.01-0.03, G57.61+0.02,and G59.79+0.63 five objects, we adopted the 12CO J=2-1 line data recorded by the DFT(1 GHz bandwidth for 16 384 channels). At the 12CO J=2-1 line, the KOSMA’s main-beamwidth was 130′′, the main-beam efficiency was 0.68; at the 12CO J=3-2 line, they were 82′′

and 0.70, respectively. During the observations, the mode of position switching was adoptedto reduce the effect of atmospheric noise. Since all the directions of our observations are veryclose to the Galactic plane, for most observations the reference position (off) of the positionswitching had been checked, the position without significant CO radiation or with only apiece of narrow spectral feature was adopted as the off-position. Only in a few observations,their off-positions had not been checked, the influences of the possible 12CO emission atthe off-position on the observed spectra are unknown, this may cause some effects on thespectra of a small part of molecular clouds.

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In order to make comparisons of multiple transitions, we adopted also the 12CO J=1-0spectral data observed by Chen et al.[3] toward the same directions of these objects. Theymade the observations on 12th-17th Feb. 2009 with the Delingha 13.7m millimeter wavetelescope, the corresponding main-beam width was 62.4′′, and the main-beam efficiency was0.61. Since that Chen et al.[3] published only the parameters of the spectral lines corre-sponding to the EGO velocities in these observations, however we are also interested inthe remained 12CO J=1-0 spectral data of non-EGO molecular clouds, which are not corre-sponding to EGO velocities, hence we have downloaded this group of data from the databaseof the Delingha 13.7m telescope, and reprocessed them. These observations adopted alsothe position switching mode, the reference positions were about 10’ apart from the Galacticplane, without the contamination of the 12CO line emission[3].

All the spectral data processing was performed by using the GILDAS/CLASS software.The obtained KOSMA spectral data generally have a relatively flat baseline, hence only alow-order polynomial fitting was used to remove the spectral baseline. The 12CO J=1-0spectral data of the Delingha 13.7m telescope generally have a undulant baseline, hence thesine function fitting was used for the baseline subtraction. But for such sinusoidal baselines,the effect of baseline subtraction is not very ideal, hence for the 12CO J=1-0 data, thespectral profiles are not so reliable as those we observed at the 12CO J=2-1 and J=3-2 lines.

In order to obtain the parameters of all the molecular clouds with different radialvelocities along the directions of these EGOs, it was assumed that for the every EGO, theprofiles of the 12CO J=2-1 and J=3-2 lines are Gaussian. This assumption is consistentwith the observed results of other molecular clouds in the literature[7−8]. But it is wellknown that in the celestial areas close to the Galactic plane, the overlap of 12CO lines isquite serious, this brings a difficulty to the discrimination between the cloud components ofdifferent radial velocities. In order to overcome this difficulty to a certain extent, we havemade a detailed comparison on the spectral profiles of the three transitions, and hereby tojudge the line center positions and linewidths of a part of overlapped spectral componentsaccording to the differences in the spectral profiles of different transitions. Since the criticaldensity and excitation temperature are relatively high for the transitions from a largerupper-level quantum number, hence, the higher transitions generally exhibit a less overlapof spectral lines. After such a comparison and adjustment, the obtained cloud velocitiesfrom the spectra of the three 12CO transitions are basically coincident. In this way, thebroad line wings of some broad spectra or some small narrow features superposed on ratherbroad spectral profiles may be fitted as isolated Gaussian components, and mistaken asindependent molecular clouds. Because of the complexity caused by the overlap of spectrallines, some times we could not help fixing some parameters of the spectral line (for examplethe line-center velocity, linewidth, etc.) in order to fit satisfactorily the partially overlappedspectral profiles. These cloud components with significantly overlapped spectra may benot a physically independent molecular cloud, but an assembly of a few molecular cloudswith rather similar velocities. This point should be properly taken into consideration in thesucceeding data analysis. At the same time, according to the extent of spectral overlap,the data of different clouds were treated separately. For example, according to some givencriterions, the seriously overlapped spectra are excluded from the linewidth analysis, etc.

For some spectra which are affected by the 12CO line emission at their off-positions,we performed as well the Gaussian profile fitting, but their parameters were not used in

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the following statistical analysis. For the spectra which are affected by the 12CO line emis-sion at their off-positions so seriously that an obvious negative baseline appears, they werecompletely omitted.

3. OBSERVED RESULTS

By the Gaussian profile fitting mentioned above, in the directions of 59 EGOs we havedetected 354 different molecular cloud components, the fitting parameters of the 12CO J=1-0, J=2-1, and J=3-2 three lines of the every radial velocity component in each EGO directionare listed in Table 1. In this table, the first column (source) is the observing direction (i.e.,the name of the corresponding EGO, the asterisk possibly appeared behind it indicates thatthis velocity component is associated with the EGO which is considered as a large-mass starformation region), the later 18 columns are divided into 3 groups, which indicate respectivelythe main-beam line peak temperature (TMB), spectral line area (

∫TMBdV ), radial velocity

(VLSR), linewidth (full width at half maximum, FWHM), baseline noise (RMS), and thedescription about the 12CO line pollution at the off-position (Note) for each of the threespectral lines. The brackets behind each datum gives the 1σ fitting error. If the error isdisplayed as “(*)”, it means no error information because that a fixed value is adopted in theGaussian fitting. For some molecular clouds, if the emission line corresponding to a certaintransition was failed to be detected or lacking in observed data, it is denoted by “–”.

In the following we will make a statistical analysis on the linewidths and intensities ofthe three 12CO lines of these molecular cloud components, respectively. At first, accordingto the EGO radial velocities observed by Chen et al.[3] and He et al.[6], we make comparisonswith the radial velocities obtained from Gaussian fittings to distinguish the EGO molecularclouds that are associated with EGOs in visual velocities from those non-EGO molecularclouds that are not associated with EGOs in the same directions, namely with no large-massstar formation, it is expected that by the statistical analysis, we can find out the trend ofthe variations of the 12CO line emission with the mass and size of a molecular cloud, as wellas the statistical differences between the EGO molecular clouds associated with large-massstar formation regions (EGOs) and the non-EGO molecular clouds with no evidence of starformation.

3.1 Correlation of 12CO LinewidthsAt first, in Fig.1 we have compared directly the widths (FWHMs) of the 12CO J=1-0 andJ=3-2 lines with the width of the 12CO J=2-1 line for the EGO molecular clouds associatedwith large-mass star formation regions (two upper panels) and the non-EGO clouds (twolower panels), respectively. In this figure, the molecular clouds, whose 12CO spectrumhas been obviously affected by the 12CO line pollution at the off-position, or whose 12COspectrum is seriously overlapped with the neighboring spectral lines, have been excluded.

Although at first glance Fig.1 gives us the impression that the widths of the three linesare close to each other (the deviations from the dotted lines of Fig.1 are not very large), butafter a careful investigation we can find the following trends: (1) the EGO molecular cloudsand non-EGO clouds have about the same linewidth range (FWHM ≈ 3∼9 km·s−1), only asmall number of non-EGO molecular clouds have rather narrow spectra (FWHM<3 km·s−1).(2) For most molecular clouds (including the EGO and non-EGO clouds), the linewidth is

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gradually reduced according to the sequence from 12CO J=1-0 to 12CO J=2-1 to 12COJ=3-2. (3) For the non-EGO molecular clouds, as the 12CO linewidth increases, the 12COJ=2-1 line becomes narrower than the other two transitions (namely, in the lower panels,the distributions of data are steeper than the dotted lines). In addition, around FWHM ≈6 km·s−1 there exists a demarcation point, for the non-EGO clouds of FWHM ≤ 6 km·s−1,the 12CO J=1-0 and J=2-1 linewidths are close to each other, but the 12CO J=3-2 linewidthtends to be narrow; for the non-EGO clouds of FWHM ≥ 6 km·s−1, the 12CO J=1-0 lineis slightly broader than the J=2-1 line, and the widths of the 12CO J=3-2 and J=2-1 linesare close to each. However, in the upper two linewidth correlation diagrams for the EGOmolecular clouds, this trend disappears. (4) In the correlation diagrams of 12CO J=2-1and J=3-2 linewidths, the dispersion of data points increases with the linewidth (this isconsistent with the variation of the dispersion of data points in the linewidth correlationdiagrams among the three isotopic lines of CO J=1-0 as revealed by He et al.[6]), but thistrend has not appeared in the correlation diagrams of 12CO J=1-0 and J=2-1 linewidths.

Fig. 1 The comparisons of 12CO J=1-0 and J=3-2 linewidths with that of the 12CO J=2-1 line for the

EGO and non-EGO molecular clouds. The upper two panels indicate the EGO clouds that are associated

with the massive star forming regions, while the lower two panels indicate the non-EGO clouds. The

dashed lines mark the positions where the two compared linewidths are equal.

In order to show more distinctly the difference between the EGO and non-EGO cloudsin the linewidth correlation diagrams of 12CO lines, we have plotted the correlation diagrambetween the 12CO J=1-0/J=2-1 and 12CO J=3-2/J=2-1 linewidth ratios into the logarithmicdiagram of Fig.2. In the left panel, the distribution of linewidth ratios of the EGO molecularclouds exhibits no any significant trend, while in the right panel, the 12CO J=1-0/J=2-1and 12CO J=3-2/J=2-1 linewidth ratios of the non-EGO molecular clouds show obviously a

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positive correlation. This trend is exactly the another exhibition of the systematic deviationof the linewidth correlation of the non-EGO clouds from a positively proportional relationas seen in Fig.1. This trend may be resulted by the fact that the 12CO J=1-0 and J=3-2linewidths vary consistently, but they vary inconsistently with the 12CO J=2-1 linewidth.

Fig. 2 The correlation between the 12CO J=1-0/J=2-1 and 12CO J=3-2/J=2-1 linewidth ratios for the

EGO and non-EGO molecular clouds

Fig. 3 The correlations of the 12CO J=1-0/J=2-1 and 12CO J=3-2/J=2-1 linewidth ratios with the dense

gas tracer (the spectral area ratio between the H13CO+ J=3-2 and 12CO J=2-1 lines). The nominal flux

calibration uncertainty of 20% has been included in the error bars of the spectral area ratios

From Fig.1 and Fig.2 we can find that according to whether they are associated withthe massive star forming regions (EGOs), the molecular clouds can be classified into twogroups with different statistical properties of CO linewidths. Based on the results observedby He et al.[6], an important restrictive characteristic of EGOs is the existence of the hotand dense gas cores traced by the H13CO+ J=3-2 line. Hence we can further ask: in theEGO molecular clouds associated with these hot dense gas cores, is there any relationshipbetween the CO linewidth ratio which reflects the density and velocity field distributionsin the molecular cloud and the mass ratio of the hot and dense gas in the whole molecularcloud? In order to answer this question, we extract the spectral area of the H13CO+ J=3-2line from the result observed by He et al.[6], and by using its ratio with respect to the spectral

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area of the CO J=2-1 line that we observed, to measure the proportions occupied by the hotdense gas in these EGO molecular clouds. Hence, we plot the relationships of the above-mentioned 12CO J=1-0/J=2-1 and 12CO J=3-2/J=2-1 linewidth ratios with the dense gastracer (the spectral area ratio between the H13CO+ J=3-2 and 12CO J=2-1 lines) as shownin Fig.3. From the left panel of this figure, we can find a weak trend that the stronger thedense gas emission in the EGO clouds, the broader the 12CO J=1-0 line as compared withthe 12CO J=2-1 line. However, in the right panel it seems that the distribution of EGOmolecular clouds has no evident trend.

3.2 Correlation of 12CO Line AreasDescribed the statistical properties of the 12CO linewidths of the EGO clouds and non-EGO clouds, we turn to investigate the statistical properties of their 12CO line intensities.Similarly, we compare directly the 12CO J=1-0 and J=3-2 line areas of the two kinds ofmolecular clouds with their 12CO J=2-1 line areas as shown in Fig.4. From this figure wecan find that the spectral line areas of the EGO clouds are greater than those of most non-EGO clouds. The 12CO line intensities of both kinds of molecular clouds vary in a ratherlarge range: the differences of the 12CO line intensities of the EGO molecular clouds exceedone order of magnitude, and those of the non-EGO clouds exceed two orders of magnitude.

Fig. 4 The comparisons of 12CO J=1-0 and J=3-2 line areas with the J=2-1 line area for the EGO and

non-EGO molecular clouds. The nominal flux calibration uncertainty of 20% has been included in the

error bars of the 12CO J=1-0/J=2-1 ratios, but not in the error bars of the 12CO J=3-2/J=2-1 ratios,

because the later two lines were observed simultaneously by the same telescope. The dashed lines mark the

positions where the two compared spectral areas are equal.

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From the two upper panels in this figure we can find that the three 12CO line intensitiesof the EGO clouds exhibit such a trend: the 12CO J=1-0 line is strongest, the 12CO J=2-1 and J=3-2 line areas are smaller, but close to each other. The calculated mean 12COJ=1-0/J=2-1 line area ratio of the EGO molecular clouds is 2.09±0.15, and the mean 12COJ=3-2/J=2-1 line area ratio is 0.87±0.06. Besides, from the upper left panel we can find thatwith the increase of the J=2-1 line intensity, the J=1-0 line intensity is gradually weakenedwith respect to the J=2-1 line (i.e., gradually approaching to the dashed line of the figure).

From the two lower panels we can find that the three 12CO line intensities of the non-EGO clouds exhibit slightly different trends: the 12CO J=1-0 line is strongest, the J=2-1 linenext, and the J=3-2 line weakest. The calculated mean 12CO J=1-0/J=2-1 line area ratioof the non-EGO molecular clouds is 2.06±0.09, and the mean 12CO J=3-2/J=2-1 line arearatio is 0.74±0.04. Besides, from the lower right panel we can find that with the increase ofthe J=2-1 line intensity, the J=3-2 line intensity is gradually intensified with respect to theJ=2-1 line (i.e., gradually approaching to the dashed line of the figure).

We have tried to compare the EGO and non-EGO clouds by their respective 12CO J=1-0/J=2-1 and J=3-2/J=2-1 line area ratios, as shown in Fig.5. In the correlation diagrams ofthe two kinds of molecular clouds, we cannot find any statistically meaningful trends, mostclouds are concentrated around the mean intensity ratios mentioned above.

Fig. 5 The correlation between the 12CO J=1-0/J=2-1 and J=3-2/J=2-1 line area ratios for the EGO and

non-EGO molecular clouds. The nominal flux calibration uncertainty of 20% has been included in the

error bars of the 12CO J=1-0/J=2-1 ratios, but not in the error bars of the 12CO J=3-2/J=2-1 ratios,

because the later two lines were observed simultaneously by the same telescope.

We have compared also the 12CO J=1-0/J=2-1 and J=3-2/J=2-1 line area ratios ofthe EGO molecular clouds with the dense gas tracer (the area ratio between the H13CO+

J=3-2 and 12CO J=2-1 lines), as shown in Fig.6. From the left panel we can find that asthe emission of hot dense gas intensifies, the 12CO J=1-0 line emission has a weak trend tointensify with respect to the J=2-1 line. In the right panel, the data are rather scattered, nosignificant trend can be found from the distribution of the data. However, the range of the12CO J=1-0/J=2-1 line area ratios in the left panel is quite consistent with the range of the12CO J=1-0/J=2-1 linewidth ratios of Fig.3, hence we guess that the increase of the 12COJ=1-0/J=2-1 line area ratio with the increasing emission of hot dense gas may be caused

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only by the similar variational trend of the 12CO J=1-0/J=2-1 linewidth ratio in Fig.3.

Fig. 6 The correlation of the 12CO J=1-0/J=2-1 and J=3-2/J=2-1 line area ratios with the dense gas

tracer (the spectral area ratio between the H13CO+ J=3-2 and 12CO J=2-1 lines) for the EGO clouds.

The nominal flux calibration uncertainty of 20% has been included in the error bars of the 12CO

J=1-0/J=2-1 ratios and dense gas tracers, but not in the error bars of the 12CO J=3-2/J=2-1 ratios,

because the later two lines were observed simultaneously by the same telescope.

3.3 Correlation between the 12CO Line Peak Temperature and the LinewidthThe 12CO linewidths tell us the information about the virial mass of a molecular cloud, andthe 12CO line intensities and intensity ratios tell us the information about the intensities andspatial distributions of the density, temperature, and velocity fields in the molecular cloud.In order to investigate the variations of the physical properties of the molecular clouds withthe masses of these clouds, in this section we will analyze the correlations of the intensitiesand intensity ratios of the three 12CO lines with their linewidths.

Fig.7 gives the correlations between the main-beam peak temperatures (TMB) and thewidths (FWHM) of the 12CO J=1-0, J=2-1 and J=3-2 lines for both the EGO and non-EGOmolecular clouds. From the three upper panels of this figure, we can find that although thedistribution of data is rather scattered, the three CO lines of the EGO clouds exhibit plausi-bly a weak trend of the broader linewidth corresponding to a higher line peak temperature.But this trend is insignificant for the non-EGO clouds as shown by the three lower panels. Tocompare the upper and lower panels on by one, we can find again that in general, the EGOmolecular clouds have stronger CO line emissions than the non-EGO clouds. In the threelower panels we have noticed that for a few non-EGO clouds with especially strong CO lines,they have lg(TMB(J = 1− 0)) ≥ 0.8K, lg(TMB(J = 2− 1)) ≥ 0.8K, lg(TMB(J = 3− 2)) ≥0.6K, and lg(FWHM) ≥ 0.7 km · s−1. The observed properties of this small number ofnon-EGO clouds are very close to that of the EGO clouds associated with massive starforming regions, hence they may be the molecular clouds preparing to form massive stars.

The correlations of the main-beam peak temperature ratios of 12CO J=1-0/J=2-1 andJ=3-2/J=2-1 with the linewidth for the EGO and non-EGO molecular clouds are shownin Fig.8. Obviously, the CO line intensities of the two groups of sample clouds have nosignificant correlations with the linewidth.

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Fig. 7 The correlations between the main-beam peak temperatures and linewidths of 12CO J=1-0, J=2-1,

and J=3-2 lines for both the EGO and non-EGO molecular clouds

Fig. 8 The correlations between the peak main-beam temperature ratios (12CO J=1-0/J=2-1 and

J=3-2/J=2-1) and the J=2-1 linewidth for both the EGO and non-EGO molecular clouds. The nominal

flux calibration uncertainty of 20% has been included in the error bars of the 12CO J=1-0/J=2-1 ratios,

but not in the error bars of the 12CO J=3-2/J=2-1 ratios, because the later two lines were observed

simultaneously by the same telescope.

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4. DISCUSSIONS

4.1 Comparison of Observed Characteristics of the EGO and non-EGO Molec-ular CloudsThis paper aims to discuss the differences between the EGO and non-EGO molecular clouds,here we at first make a summary on the similarities and differences in the observed charac-teristics of the EGO and non-EGO molecular clouds mentioned above.4.1.1 Similarities

For both the EGO and non-EGO molecular clouds, all the three 12CO lines exhibitsignificantly the correlation between the linewidth and the line area. Their linewidths areall distributed in nearly the same range (FWHM ≈ 3 ∼ 9 km · s−1), only the linewidths of afew non-EGO clouds are distributed in the narrower range FWHM ≈ 2 ∼ 3 km ·s−1. TheirCO line intensities are all vary in a rather broad range of 1∼2 orders of magnitude. Andtheir peak intensity ratios between two different 12CO lines are all not correlated with the12CO linewidth.4.1.2 Differences

(1) The difference of the variational trend of linewidth: for the EGO clouds, thelinewidths of the three 12CO lines are almost proportional to each other, the J=2-1 andJ=3-2 linewidths are very close to each other, and slightly narrower than that of the J=1-0line; for the non-EGO clouds, the linewidth correlation deviates systematically the pro-portional relation, namely, as the linewidth increases, the J=1-0 line becomes narrower incomparison with the other two lines. Besides, for the non-EGO clouds, when the linewidthis less than ∼ 6 km · s−1, the J=1-0 and J=2-1 linewidths are equivalent to each other,and the J=3-2 line is narrower than the J=2-1 line; when the linewidth is greater than∼ 6 km · s−1, the J=1-0 line becomes broader in comparison with the J=2-1 line, and theJ=3-2 line becomes as broad as the J=2-1 line.

(2) The difference of line intensity: the 12CO line integrated intensities of the EGOmolecular clouds are generally stronger than those of the non-EGO clouds.

(3) The difference of line intensity ratio: for the EGO molecular clouds, the 12CO J=2-1and J=3-2 line integrated intensities are very close to each other, almost the one half of theJ=1-0 line integrated intensity; for the non-EGO clouds, the integrated intensities of thethree 12CO lines are decreased according the sequence from J=1-0 to J=2-1 then J=3-2, theJ=2-1 line integrated intensity is also the one half of the J=1-0 line integrated intensity, butthe J=3-2 line integrated intensity is about the 74% of the J=2-1 line.

(4) The difference of the variational trend of line intensity: for the EGO molecularclouds, the integrated intensities of the 12CO J=3-2 and J=2-1 lines are proportional toeach other, but compared with the J=2-1 line, the integrated intensity of the J=1-0 linehas a trend to become slightly weaker as the line intensity increases (for the EGO cloudswith weak 12CO lines, the J=1-0 line is stronger than the J=2-1 line, only in several EGOclouds with strongest 12CO lines, the J=1-0 line is weakened to be as strong as the J=2-1line); for the non-EGO molecular clouds, the integrated intensities of the 12CO J=3-2 andJ=2-1 lines are basically proportional to each other, but compared with the J=2-1 line, theintegrated intensity of the J=3-2 line has a trend to become slightly stronger as the lineintensity increases (for the non-EGO clouds with weak 12CO lines, the J=3-2 line is weakerthan the J=2-1 line, only in several non-EGO clouds with strongest 12CO lines the J=3-2

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line is intensified to be as strong as the J=2-1 line).(5) The difference of the correlation of line peak intensity versus linewidth: for the EGO

clouds, the 12CO line peak intensity has a weak trend to increase with the linewidth, however,for the non-EGO clouds, the 12CO line peak intensity and linewidth are not correlated.

4.2 Physical Images Adopted for the Molecular CloudsIn order to understand these observed results, we have to analyze at first what factors deter-mine the 12CO linewidths and intensities of the molecular clouds that we observed. The im-portant physical parameters may include the diameter and distance of the cloud (concernedwith the beam filling factor), the gas temperature, density and velocity field distributions,the filling factor of the projected area of molecular clumps on the celestial sphere, the columndensity of 12CO molecular gas (concerned with the optical thickness), and the excitationstate of the rotational energy levels of the 12CO molecule.

First of all, we estimate the main-beam filling factors of the observed molecular clouds.The 12CO linewidths of all these clouds are about in the range of FWHM≈ 3 ∼ 9 km ·s−1. According to the relation between the 3-dimensional velocity dispersion of macroscopicturbulence-dominated molecular gas and the scale: L(pc) = σ(km · s−1)2[7−8], and therelation between the linewidth (FWHM) observed along the line-of-sight direction and the 3-dimensional velocity dispersion of gaseous matter: FWHM= ((8 ln 2)/3)1/2σ, this linewidthrange corresponds to the cloud’s geometrical diameters in the range of 5∼44pc, only thesizes of a few non-EGO clouds are less than this range (but still greater than 2.2 pc). Withthe Galactic kinematic distance model proposed by Reid et al.[9], we have calculated theremote distance and near distance for all the sample clouds. According to the empiricalrelation between the cloud’s virial mass and the 12CO linewidth given by Solomon et al.[8],the broader the 12CO linewidth, the greater the cloud’s virial mass. As the 12CO linewidthsof most clouds in our sample are distributed in the 3 ∼ 9 km ·s−1 range, hence we artificiallyassume that the molecular clouds with the 12CO linewidths less than 5 km·s−1 are small-massclouds. These small clouds may be situated in the near kinematic distances, otherwise theywill not be observed by us with a rather small telescope. For all the large-mass clouds withthe 12CO linewidths greater than 5 km·s−1, we conservatively adopt the remote kinematicdistances. From the calculated distances and diameters of the molecular clouds, we canobtain the beam filling factors of these clouds. The calculated result indicates that besidesthe 24 sample clouds whose beam filling factor is less than 0.9, the beam filling factorsof other 330 molecular clouds are all close to 1 (>0.9). Hence, the beam filling factors ofthese molecular clouds will have a rather small effect on the observed 12CO line intensities.Similarly, the cloud distance is also not the key factor to determine the statistical propertyof the observed 12CO line intensities.

Molecular clouds are caused by the gravitational collapse of interstellar gas, so we canqualitatively predict that the gas density in a molecular cloud increases toward the cloudcenter. But the magnitude of density gradient will differ with the particular cloud, so it isa variable in the explanation of the 12CO line observations. The temperature of gas in amolecular cloud is mainly determined by the thermal equilibrium of gas, generally in the10∼20K range, it is also treated as a variable parameter in this work. The gradient oftemperature distribution in a molecular cloud may depend on the existence of the radiationheating of forming stars in the interior, so it is also a variable parameter. Qualitatively, the

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gas temperature in the center of the molecular cloud (namely the cloud core) with large-massstar formation will be higher than that in the starless cloud core.

About the clumps in the molecular cloud, we adopt the fog grain model of molecularclouds proposed by Solomon et al.[8]. The observed 12CO line from the interstellar cloudgenerally has an optically-thick Gaussian profile, its linewidth represents mainly the velocitydispersion of the motions of the small clumps (i.e., the so-called fog grains in this model)in this cloud, and the line intensity represents the magnitude of gas temperature in theclumps as well as the magnitude of filling factor of the projected area of the clumps onthe celestial sphere along the line-of-sight direction. This observed velocity dispersion canroughly reflect the virial mass of the whole molecular cloud. According to the relationbetween the 3-dimensional velocity dispersion and the mass: M (M�) = 2000σ (km · s−1)4,from the above-mentioned 12CO linewidth range we can estimate that the virial masses ofthese molecular clouds are about in the range of 5 × 104 ∼ 4 × 106 M�, only the virialmasses of a small number of non-EGO clouds are less than this range (but still greater than104 M�). Although the real molecular clouds may not situate in the ideal virial equilibriumstate, but the analysis of observed data made by Solomon et al. in 1987 indicates that thevirial mass determined from the 12CO linewidth is actually correlated very well with the12CO line luminosity, and further the total mass of the cloud. Hence, the virial mass isreally a very good indicator of mass of a molecular cloud. Therefore, the above-mentionedsimilar ranges of the 12CO linewidths of the EGO and non-EGO molecular clouds implythat the ranges of the masses and sizes of the two kinds of molecular clouds are basicallysimilar, they are totally the giant molecular clouds(GMCs).

This molecular cloud model brings about another parameter which may affect the ob-served 12CO line intensity: the area filling factor of the clumps in the molecular cloud. Sincethe rotational energy levels of 12CO molecules are very easy to be excited by collisions, andthe abundance of 12CO molecules is very high, we can predict that the 12CO line emis-sion in each small molecular clump has already been optically thick. Thus the parameterthat influences on our observed 12CO line intensities is mainly the above-mentioned areafilling factor of molecular clumps, rather than the difference of optical thickness betweentwo different 12CO transitions. The clumping in a molecular cloud is closely related withthe random turbulent velocity field within the cloud, which can be roughly described by the4-dimensional volume filling factor of gas clumps in the X-Y-Z-V 4-dimensional parametricspace constituted by the 3-dimensional position space and one-dimensional velocity space.For the convenience of discussion, we assume that all the clumps in the cloud have similarvelocity dispersions, thus the magnitude of this 4-dimensional clump filling factor will bereversely proportional to the velocity dispersion of the whole cloud, namely the bigger the ve-locity space of this 4-dimensional parametric space, the smaller the clump filling factor. Forthe molecular clouds with similar velocity dispersions, the magnitude of the 4-dimensionalclump filling factor depends on mainly the volume filling factor in the 3-dimensional positionspace. Hence, at an arbitrarily given radial velocity, the area filling factor of the molecularclumps along the line-of-sight direction projected on the celestial sphere is determined by theconjunction of the 3-dimensional volume filling factor of the molecular clumps, the velocitydispersion, and the longitudinal size of the molecular cloud. In this work we take the areafilling factor of the molecular clumps as a variable parameter

Generally, under the typical cloud temperature (10K) and density (> 103 cm−3), the

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lower rotational energy levels of the 12CO molecules observed by this work are well ther-malized, so we will adopt the postulate of local thermal equilibrium (LTE) to deal with theexcitations of rotational energy levels of 12CO molecules, namely all the excitation temper-atures of the three 12CO transitions are equal to the gas temperature. But because thatunder the typical 10K temperature, the critical density (the density that the collision exci-tation rate is sufficient to match the spontaneous radiation rate) for the excitations of the12CO J=1-0, J=2-1, and J=3-2 lines is 2.57×103 cm−3, 7.43×103 cm−3, and 1.93×104 cm−3,respectively, the increasing critical density makes the radiation regions of the transitions ofhigher rotational quantum numbers concentrate in the region of higher gas density. Ac-cording to the assumption that the gas density in a molecular cloud increases toward thecloud center, the transitions of higher rotational quantum numbers mainly come from theregion close to the cloud core. If in the molecular cloud exist simultaneously the densitygradient and temperature gradient, then this difference will cause the intensity differencesof the three 12CO thermal lines.

4.3 Explanation on the Observed Characteristics of the EGO and Non-EGOMolecular CloudsBased on these physical images, we infer that the EGO and non-EGO molecular cloudsshould have the following structural differences in order to explain naturally what we haveobserved: EGO molecular clouds are the molecular clouds in which there are massive starsforming, non-EGO molecular clouds are the cool molecular clouds with no star formation;in both the EGO and non-EGO molecular clouds the gas density increases toward the cloudcenter (or the center of each cloud in a complex of GMCs); the radiation regions of thethree observed 12CO rotational lines are mainly distributed in the large-radius outer regionof the molecular cloud, where the gas temperature is determined by the balance between theheating of interstellar radiation and the cooling of molecular rotational line emission, hencethere exists a general trend that the gas temperature decreases towards the cloud center;but in the EGO molecular clouds, because of the radiation heating of newly born stars, intheir high-density regions the decrease of gas temperature is more gentle than that in thenon-EGO clouds.

These structural differences of molecular clouds can naturally explain a part of theobserved characteristics mentioned above:

(1) Because of the heating of internal stellar radiation, the temperature of the innermost12CO J=3-2 line emission region is raised, and the gas temperatures in the 12CO J=2-1 andJ=3-2 line emission regions of the EGO molecular cloud may be close to each other, sothey have similar integrated intensities, while the J=1-0 line emission comes mainly fromthe gas of higher temperature and lower density near the outer periphery of the cloud, soits intensity is stronger than the other two lines. Similarly, since the J=1-0 line traces thelarge-sized structures in the molecular cloud, in which the turbulent velocity dispersion isgreater, so it is broader than the other two lines.

(2) In the non-EGO molecular clouds, the three 12CO lines come from the regions ofdifferent densities and temperatures, the gas temperatures of their radiation regions arereduced successively in the sequence from 12CO J=1-0 to J=2-1 then J=3-2, thus, theobserved result that in the non-EGO molecular clouds, the observed intensities of the three12CO lines are reduced in the same sequence is naturally explained.

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Besides, the EGO and non-EGO molecular clouds exhibit also many other differenceswhich can not be explained by the above images, they probably imply some more differencesin physical properties. For example:

(1) For the non-EGO molecular clouds, the correlations of the three 12CO linewidthsdeviate apparently from a proportional relation, but they do not for the EGO molecularclouds (see Fig.1). When the 12CO linewidth increases (i.e., when the virial mass increases),the J=2-1 linewidth tends to be narrower than J=1-0 line, which implies that the non-EGOmolecular cloud with a greater virial mass may have a denser cloud core, and therefore theJ=2-1 line is more likely to be the contribution of the small-sized dense core (and hencewith a smaller velocity dispersion). When the 12CO linewidth increases (i.e., when thevirial mass increases), the J=2-1 linewidth tends also to be narrower than J=3-2 line, whichimplies that in the non-EGO molecular clouds with a greater virial mass may more likelyexist some unknown velocity dispersions (for example, the turbulence or the infall motion ofmatter caused by the gravitational collapse), which make the originally narrow J=3-2 linethat comes from a small-sized region become as broad as the J=2-1 line. The reason thatthis trend does not exist in the EGO molecular clouds may be the rather small number ofour sample EGO clouds.

(2) The 12CO line areas of the EGO and non-EGO molecular clouds vary in a ratherlarge range (spanning 1∼2 orders of magnitude). As mentioned above, the telescope’s beamfilling factor corresponding to the geometric diameter of the molecular cloud, as well as thedistance of the molecular cloud, are not the key factors to determine the observed 12CO lineintensities, the main reasons to cause the variety of the observed 12CO line intensities arethe differences of the gas temperatures in the different molecular clouds, and the differencesof the area filling factors of their interior clumps along the radial velocity direction projectedon the celestial sphere.

The following two facts make us assure that the radiation heating of young stellarobjects and the intenseness of the heating effect will not be the main reasons to cause thedifferences of the observed 12CO line intensities: (1) in the non-EGO clouds, there are nostars forming; (2) if the radiation heating of young stellar objects was the main reason tocause the difference of gas temperature in the outer 12CO radiation regions (and thereforethe difference of the 12CO line intensity), then we will find that in both the EGO and non-EGO molecular clouds the line intensity ratios of 12CO J=1-0/J=2-1 and J=3-2/J=2-1 arereversely correlated. But this has not appeared in our correlation diagrams (see Fig.5).

If we assume again that in the different molecular clouds the interstellar radiationenvironments are similar, then the 12CO radiation regions of the different molecular cloudsshould have similar gas temperatures (namely, the similar LTE excitation temperatures of12CO), and the remained area filling factor of the clumps in the interior of a molecularcloud will be the key factor to determine the observed 12CO line intensities. However, as wementioned above, only in the EGO molecular clouds there exists a weak correlation betweenthe 12CO linewidth (tracing the cloud’s geometric diameter) and the line peak temperature,and there is no correlation in the non-EGO clouds (see Fig.7). This indicates that thedifferences of the clump area filling factors of these molecular clouds are not caused by thedifferences of their longitudinal sizes. On the other hand, if the velocity dispersion of amolecular cloud has an important influence on the 12CO line intensity, then we will findthat the broader the 12CO linewidth (namely, the smaller the clump filling factor in the

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X-Y-Z-V 4-dimensional space), the weaker the inverse correlation of the 12CO linewidthand peak temperature, this is opposite to the weak positive correlation shown in Fig.7 forthe EGO clouds, and this is also inconsistent with the non correlation for the non-EGOclouds. Hence the differences of the 12CO linewidths among the molecular clouds will notbe the main reason to cause the broad range of our observed 12CO line intensities. Then,only the variation of the 3-dimensional volume filling factor with the different molecularcloud may be the factor affecting significantly the 12CO line intensities. And it is verypossible that this variation of clump volume filling factor is closely related to the process ofgravitational collapse triggered by the factors such as the Galactic spiral shock, the shearingeffect of differential Galactic rotation, the compression of stellar wind shocks, the collisionof molecular clouds, etc. And the process of cloud collapse is further related closely with theformation and evolution of a molecular cloud, as well as the star formation in which (see thesimulative study made by Dobbs et al.[10] and the analysis made by Elmergreen et al.[11]).

(3) The 12CO line intensities of the EGO molecular clouds are generally greater thanthose of the non-EGO clouds (see Fig.4), it implies that the area filling factor of the smallclumps in an EGO molecular cloud with star formation may be some what greater thanthat of a non-EGO cloud with no star formation. As analyzed above, the EGO and non-EGO molecular clouds have similar mass and size ranges, the differences in their clump areafilling factors will not be caused by the differences of the longitudinal sizes of these molecularclouds along the line-of-sight direction, nor the different velocity dispersions of the two kindsof molecular clouds, but the systematic difference of the 3-dimensional volume filling factorbetween the interior clumps of the two kinds of molecular clouds, namely the distributionof interior clumps in an EGO cloud is denser than that in a non-EGO molecular cloud.

(4) In the EGO molecular clouds, as the 12CO line intensity increases, compared withthe J=2-1 line, the 12CO J=1-0 line integrated intensity tends to be slightly weakened (seethe upper left panel of Fig.4), according to the above discussion, it implies that probably inthe EGO molecular clouds with greater clump area filling factors, the effect of gas heating(the stellar radiation or gravitational collapse may cause the J=2-1 line intensify relative tothe J=1-0 line) is more prominent. This explanation can be described in detail as follows:in the EGO molecular clouds with a weaker 12CO emission (and therefore a smaller clumparea filling factor), such kind of heating effect is relatively weak, the gas temperature in thesmall-radius 12CO J=2-1 radiation region is obviously lower than that in the large-radius12CO J=1-0 radiation region, making the observed J=2-1 line weaker than the J=1-0 line; inthe EGO molecular clouds with a stronger 12CO emission (and therefore a larger clump areafilling factor), the heating effect is more significant, and the gas temperature in the small-radius 12CO J=1-0 radiation region is raised to be equivalent to that in the large-radius12CO J=1-0 radiation region, making the observed J=2-1 line as strong as the J=1-0 line.It is very possible that under the influence of this heating effect, the gas temperatures in boththe J=2-1 and J=3-2 line emission regions increase synchronously, so that the intensities ofthese two lines are basically proportional to each other as shown by the upper right panelin Fig.4.

(5) In the non-EGO molecular clouds, as the 12CO line intensity increases, the inte-grated intensity of the 12CO J=3-2 line tends to be slightly intensified relative to the J=2-1line (see the lower right panel of Fig.4), this implies that in these non-EGO molecular clouds,may exist some gas heating (for example, the heating caused by gravitational collapse) which

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becomes increasingly significant as the clump area filling factor increases. This explanationcan be further described as follows: in the non-EGO molecular clouds with a weaker 12COemission (and therefore a smaller clump area filling factor), such kind of heating effect maybe relatively weak, because of the screen effect on the interstellar radiation, and the gastemperature in the small-radius 12CO J=3-2 radiation region is obviously lower than thatin the large-radius 12CO J=2-1 radiation region, making the observed J=3-2 line weakerthan the J=2-1 line; in the non-EGO molecular clouds with a stronger 12CO emission (andtherefore a larger clump area filling factor), such kind of heating effect may become moresignificant, the gas temperature in the small-radius 12CO J=3-2 radiation region is raised tobe equivalent to that of the large-radius 12CO J=2-1 radiation region, making the observedJ=3-2 line as strong as the J=2-1 line. But the effect of gas heating may have a very smallinfluence on the 12CO J=1-0 and J=2-1 line emission regions near the outer periphery of anon-EGO molecular cloud, hence as shown in the lower left panel of Fig.4, the intensities ofthese two lines are basically proportionate.

In the correlation diagrams of the linewidths of the three 12CO lines in the EGO andnon-EGO molecular clouds, we can find a weak trend that the data dispersion increaseswith the linewidth (Fig.1), this is basically consistent with what shown by He et al.[6] inthe correlation diagrams of the linewidths of the 12CO J=1-0, 13CO J=1-0, and C18O J=1-0 lines in the EGO molecular clouds. To a certain extent, our result has supported theirconclusion that in the turbulent velocity field of a molecular cloud, the randomness increaseswith the cloud size.

4.4 New Images of the EGO and Non-EGO Molecular Clouds and Their Impli-cations to Massive Star FormationFrom the above discussion, for all these molecular clouds including EGO clouds and non-EGO clouds, we can obtain the following images: the EGO and non-EGO molecular cloudsare GMCs whose virial mass is greater than 104 M�, they have not only the common char-acteristics that the gas density increases toward the cloud center, and that the linewidthsof the 12CO rotational transitions of low quantum numbers are mainly dominated by themacroscopic turbulent velocity, but also the common trend that the gas temperature reducestoward the cloud center. But the temperatures in the central dense cores of the EGO molec-ular clouds with massive star formation will be a little higher, it makes the gas temperaturesin the emission regions of the 12CO J=2-1 and J=3-2 lines approximate to each other. Whilein the non-EGO clouds with no star formation the trend that the gas temperature decreasestoward the cloud center is more evident, making the gas temperature in the emission regionof the 12CO J=3-2 line become lower than that of the J=2-1 line emission region. The EGOmolecular clouds have a larger clump volume filling factor than the non-EGO clouds, and thedifferences of the clump volume filling factor between the different EGO molecular cloudsand between the different non-EGO molecular clouds are very large, making it become thedominant factor to affect our observed 12CO line intensities.

Besides, according to the correlations of data we infer: for a non-EGO molecular cloud,the greater the virial mass, the greater the interior density gradient; in the non-EGO molec-ular cloud, the 12CO J=3-2 line emission region may have some extra unknown velocitydispersions (for example, the turbulence caused by gravitational collapse or the infall mo-tion of matter), and the greater the virial mass, the stronger the extra velocity dispersion; in

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addition to the gas heating of stellar radiation in the EGO molecular clouds, the EGO andnon-EGO molecular clouds may have some extra mechanisms of gas heating (for example,the gas heating caused by the gravitational collapse), and such kind of extra gas heatingtends to intensify with the increasing clump volume filling factor.

From the data analysis made here we can obtain further the following conclusions: the12CO rotational transition lines of low quantum numbers so far observed by the ground-based single-dish millimeter wave telescopes generally come from the GMCs with a virialmass greater than 104 M�, as regards whether there are massive stars forming in theseGMCs, it has no direct relation with the magnitude of virial mass of the GMC, but it isrelated with the extent of gas compression in the GMC (namely, the magnitude of the clumpvolume filling factor of the molecular cloud). The massive star formation generally happensin the GMCs in which the molecular clumps are sufficient compressed so that to result in arather large clump volume filling factor.

4. SUMMARY AND PROSPECT

We have made the single-point spectral observations at the 12CO J=2-1 and J=3-2 lines to-ward 59 EGOs as the massive star formation regions in the northern sky, and in combinationwith the 12CO J=1-0 data obtained previously along the same directions of these EGOs inthe literature, we have compared and analyzed the correlation between the line intensitiesand the linewidths of the molecular clouds associated with the EGOs in the velocity space,and the correlation between those of the non-EGO molecular clouds which are not associ-ated with the EGOs. From this analysis, we have obtained the similarities and a series ofdifferences in the density and temperature structures between the EGO molecular cloudsand the non-EGO clouds. On this basis, we suggest that the appearance of massive starformation in a GMC has no direct relation with the mass of the GMC, it appears mainlyin the GMCs with larger clump volume filling factors (therefore, the molecular gas in whichhas been sufficiently compressed). In the GMC which has not been sufficiently compressedby interstellar shocks, and keeps constantly a dispersed state, the massive star formationwill not be triggered.

In this work, the data of CO line observations to be used are very limited, in the future,by analyzing a bigger observation sample and by using the data of mapping observations,many conclusions and inferences about the molecular clouds made by this work will befurther verified. We plan also to make detailed numerical simulations on the spectral-line radiative transfer in molecular clouds, in order to explain these observed phenomenamore self-consistently, and to investigate the effects of different physical parameters on theobserved phenomena.

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Table 1 The line parameters of all CO molecular clouds observed toward the directions of 59 EGOs

CO J=1-0 CO J=2-1 CO J=3-2

Source TMB

∫TMBdV V LSR FWHM RMS Note TMB

∫TMBdV V LSR FWHM RMS Note TMB

∫TMBdV V LSR FWHM RMS Note

(K) (K·km·s−1) (km·s−1) (km·s−1) (K) (K) (K·km·s−1) (km·s−1) (km·s−1) (K) (K) (K·km·s−1) (km·s−1) (km·s−1) (K)G10.29-0.13 3.35(0.28) 27.59(0.75) -11.66(0.10) 7.73(0.27) 0.26 1.83(0.06) 11.95(1.10) -13.02(0.27) 6.15(0.59) 0.17 0.55(0.20) 5.28(1.36) -10.16(1.31) 9.01(2.51) 0.39G10.29-0.13* 14.45(0.45) 117.06(0.95) 12.26(0.37) 7.61(0.37) 0.26 9.90(0.38) 82.28(1.45) 10.87(0.07) 7.81(0.15) 0.17 3.86(0.31) 34.72(1.72) 10.77(*) 8.44(0.47) 0.39G10.29-0.13 4.38(0.45) 32.51(0.95) 20.79(0.37) 6.98(0.37) 0.26 3.44(0.38) 23.19(1.31) 18.79(*) 6.34(*) 0.17 1.41(0.31) 12.19(1.41) 18.10(*) 8.14(0.00) 0.39G10.29-0.13 3.33(0.45) 25.56(0.95) 27.46(0.37) 7.20(0.37) 0.26 1.90(0.38) 9.62(0.81) 25.39(0.36) 4.75(*) 0.17 0.80(0.31) 1.95(0.68) 24.43(*) 2.30(0.84) 0.39G10.29-0.13 3.52(0.45) 27.24(0.95) 37.97(0.37) 7.28(*) 0.26 1.62(0.14) 13.37(1.75) 36.77(*) 7.77(1.05) 0.17 0.80(0.22) 4.89(1.48) 37.08(0.96) 5.76(0.00) 0.39G10.29-0.13 4.19(0.45) 30.39(0.95) 45.79(0.37) 6.81(0.37) 0.26 2.70(0.14) 19.21(1.19) 44.78(0.25) 6.68(*) 0.17 1.05(0.22) 8.01(2.12) 44.48(0.75) 7.18(2.41) 0.39G10.29-0.13 1.65(0.29) 8.76(0.70) 56.27(0.20) 4.99(0.43) 0.26 — — — — 0.17 — — — — 0.39G10.29-0.13 2.97(0.29) 28.47(0.95) 67.10(0.13) 9.01(0.41) 0.26 1.50(0.17) 13.17(1.46) 65.95(0.40) 8.27(1.17) 0.17 — — — — 0.39G10.29-0.13 0.71(0.13) 3.88(0.59) 97.50(0.38) 5.10(0.92) 0.26 — — — — 0.17 — — — — 0.39G10.29-0.13 1.68(0.26) 13.33(0.74) 154.37(0.20) 7.46(0.51) 0.26 0.88(0.07) 6.01(1.08) 153.66(0.59) 6.42(1.11) 0.17 — — — — 0.39G10.34-0.14 4.03(0.35) 37.83(0.63) -12.38(0.07) 8.81(0.18) 0.23 2.15(0.09) 17.11(1.41) -14.20(0.31) 7.49(0.63) 0.16 — — — — 1.62G10.34-0.14* 15.37(0.48) 126.31(1.08) 11.55(0.37) 7.72(0.37) 0.23 11.67(0.41) 99.12(1.83) 10.54(0.07) 7.98(0.16) 0.16 12.32(1.92) 118.43( 5.17) 11.36(0.25) 9.03(0.00) 1.62G10.34-0.14 4.90(0.48) 76.05(1.08) 24.58(0.37) 14.57(0.37) 0.23 2.51(0.41) 25.01(1.51) 22.54(0.46) 9.36(*) 0.16 — — — — 1.62G10.34-0.14 3.04(0.48) 15.42(1.08) 38.48(0.37) 4.76(0.37) 0.23 1.72(0.22) 9.16(2.19) 35.92(0.39) 5.02(0.88) 0.16 — — — — 1.62G10.34-0.14 5.16(0.48) 61.45(1.08) 47.20(0.37) 11.20(0.37) 0.23 4.97(0.22) 53.41(2.53) 44.55(0.23) 10.09(0.49) 0.16 5.40(0.87) 69.05(6.55) 45.06(0.56) 12.00(1.31) 1.62G10.34-0.14 3.06(0.24) 24.43(0.61) 67.46(0.09) 7.49(0.24) 0.23 1.69(0.15) 12.81(1.41) 66.89(0.39) 7.12(0.83) 0.16 — — — — 1.62G10.34-0.14 2.21(0.17) 10.67(0.44) 98.28(0.09) 4.53(0.21) 0.23 — — — — 0.16 — — — — 1.62G10.34-0.14 1.73(0.18) 12.59(0.54) 154.75(0.14) 6.84(0.33) 0.23 1.53(0.15) 9.29(1.22) 154.69(0.39) 5.69(0.74) 0.16 — — — — 1.62G11.11-0.11 1.01(0.18) 7.47(1.22) 11.81(0.53) 6.95(1.50) 0.20 0.74(0.11) 4.03(0.77) 10.18(0.53) 5.09(0.94) 0.21 — — — — 0.51G11.11-0.11 1.04(0.18) 3.68(1.00) 18.04(0.33) 3.32(0.85) 0.20 2.19(0.19) 12.81(0.89) 17.84(0.19) 5.50(0.42) 0.21 1.09(0.38) 7.95(1.43) 17.35(0.66) 6.86(1.13) 0.51G11.11-0.11* 6.55(0.33) 55.90(0.97) 30.38(0.07) 8.01(0.14) 0.20 1.69(0.19) 14.28(1.18) 28.62(0.27) 7.92(0.79) 0.21 1.17(0.21) 4.21(1.06) 30.65(0.42) 3.37(0.93) 0.51G11.11-0.11 1.41(0.33) 7.76(0.98) 40.49(0.21) 5.18(*) 0.20 1.15(0.19) 4.28(0.76) 37.67(0.26) 3.49(0.59) 0.21 1.00(0.48) 5.68(2.03) 38.34(0.86) 5.32(3.08) 0.51G11.11-0.11 2.88(0.33) 33.21(1.78) 48.30(0.26) 10.83(0.65) 0.20 2.11(0.19) 15.53(0.91) 46.58(0.20) 6.92(0.43) 0.21 0.96(0.47) 9.53(1.49) 50.19(0.92) 9.36(*) 0.51G11.11-0.11 0.84(0.15) 7.16(0.94) 76.33(0.55) 7.99(1.05) 0.20 — — — — 0.21 — — — — 0.51G11.11-0.11 1.98(0.20) 12.30(0.89) 90.97(0.20) 5.83(0.49) 0.20 — — — — 0.21 — — — — 0.51G11.11-0.11 1.42(0.20) 4.23(0.69) 97.63(0.22) 2.81(0.56) 0.20 — — — — 0.21 — — — — 0.51G11.11-0.11 1.24(0.15) 6.58(0.77) 123.08(0.29) 5.00(0.65) 0.20 — — — — 0.21 — — — — 0.51G11.11-0.11 1.48(0.18) 7.33(0.77) 151.47(0.24) 4.67(0.59) 0.20 — — — — 0.21 — — — — 0.51G11.92-0.61 1.41(0.20) 22.48(0.79) 8.94(0.26) 14.94(0.64) 0.20 — — — — 0.18 — — — — 0.49G11.92-0.61* 5.45(0.37) 64.91(0.61) 32.95(0.08) 11.20(0.26) 0.20 3.55(0.46) 36.67(1.35) 33.42(*) 9.70(0.37) 0.18 2.77(0.53) 18.06(1.97) 33.23(0.26) 6.14(0.92) 0.49G11.92-0.61 5.37(0.37) 51.28(0.16) 39.45(0.08) 8.98(0.20) 0.20 5.96(0.46) 32.84(0.99) 39.83(0.05) 5.18(0.14) 0.18 9.21(0.53) 36.00(1.56) 40.13(0.06) 3.67(0.17) 0.49G12.02-0.21* 6.33(0.21) 41.79(0.82) -3.10(0.06) 6.20(0.15) 0.29 2.34(0.12) 18.57(1.67) -3.65(0.33) 7.46(0.71) 0.14 2.22(0.64) 39.86(3.45) -2.00(0.76) 16.87(1.49) 0.71G12.02-0.21 2.88(0.21) 17.92(0.89) 5.23(0.22) 5.84(*) 0.29 1.57(0.12) 8.10(2.85) 4.78(0.62) 4.85(1.54) 0.14 — — — — 0.71G12.02-0.21 1.75(0.21) 10.04(2.48) 10.58(*) 5.38(0.81) 0.29 1.74(0.12) 8.57(2.15) 10.59(0.65) 4.62(0.84) 0.14 f — — — — 0.71G12.02-0.21 1.84(0.21) 22.55(2.21) 19.78(0.43) 11.48(1.32) 0.29 — — — — 0.14 — — — — 0.71G12.02-0.21 1.02(0.22) 6.88(2.59) 29.17(*) 6.34(2.51) 0.29 — — — — 0.14 — — — — 0.71G12.02-0.21 2.34(0.22) 4.69(0.87) 32.85(0.08) 1.88(0.23) 0.29 — — — — 0.14 — — — — 0.71G12.02-0.21 5.13(0.22) 43.98(2.07) 39.00(0.11) 8.05(0.45) 0.29 3.18(0.14) 15.29(1.50) 36.92(0.18) 4.52(0.33) 0.14 f 2.63(0.39) 10.92(1.81) 37.26(0.31) 3.91(0.72) 0.71G12.02-0.21 2.54(0.22) 17.24(1.76) 48.79(0.23) 6.39(0.60) 0.29 1.42(0.14) 13.85(1.85) 45.50(0.62) 9.15(1.27) 0.14 1.09(0.39) 8.68(4.25) 47.30(1.59) 7.50(3.84) 0.71G12.02-0.21 0.30(0.22) 2.63(1.00) 55.54(1.51) 8.12(*) 0.29 — — — — 0.14 1.01(0.39) 8.88(3.98) 57.16(1.85) 8.26(3.82) 0.71G12.02-0.21 2.67(0.25) 12.01(0.53) 118.81(0.10) 4.22(0.20) 0.29 1.57(0.10) 7.87(1.01) 117.19(0.30) 4.71(0.64) 0.14 — — — — 0.71

Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293 285

Table

1C

onti

nued

CO

J=

1-0

CO

J=

2-1

CO

J=

3-2

Sourc

eT

MB

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

G12.2

0-0

.03

2.3

8(0

.25)

32.5

7(3

.12)

8.1

4(0

.55)

12.8

8(1

.25)

0.1

71.9

5(0

.38)

16.3

6(3

.11)

5.5

9(0

.70)

7.8

7(1

.72)

0.4

1—

——

—0.8

3G

12.2

0-0

.03

2.3

3(0

.25)

11.4

2(2

.39)

15.3

0(0

.12)

4.6

2(0

.48)

0.1

74.0

3(0

.38)

15.1

5(2

.46)

12.8

3(0

.22)

3.5

4(0

.43)

0.4

1f

——

——

0.8

3G

12.2

0-0

.03

4.1

7(0

.25)

35.1

7(1

.05)

23.6

1(0

.09)

7.9

3(0

.27)

0.1

76.0

7(0

.65)

22.8

6(1

.27)

22.7

7(0

.10)

3.5

4(0

.17)

0.4

1f

——

——

0.8

3G

12.2

0-0

.03

3.9

4(0

.25)

18.2

3(0

.55)

33.0

3(0

.05)

4.3

5(0

.17)

0.1

72.8

3(0

.19)

5.4

3(0

.84)

33.4

0(0

.15)

1.8

0(0

.24)

0.4

1f

——

——

0.8

3G

12.2

0-0

.03*

8.2

6(0

.20)

64.2

7(0

.10)

49.7

2(*

)7.3

1(0

.05)

0.1

712.4

5(0

.42)

84.4

8(1

.65)

48.4

3(0

.06)

6.3

8(0

.13)

0.4

13.4

3(0

.69)

26.7

1(2

.62)

49.3

5(0

.35)

7.3

1(0

.84)

0.8

3G

12.2

0-0

.03

0.9

0(0

.20)

8.1

3(0

.48)

67.6

2(0

.27)

8.4

9(0

.64)

0.1

71.6

2(0

.42)

9.4

9(1

.54)

66.4

7(0

.49)

5.4

9(1

.01)

0.4

1—

——

—0.8

3G

12.2

0-0

.03

2.6

2(0

.12)

14.4

7(0

.38)

96.8

3(0

.07)

5.1

8(0

.16)

0.1

72.7

3(0

.24)

14.5

2(1

.52)

95.5

0(0

.26)

5.0

0(0

.53)

0.4

1—

——

—0.8

3G

12.2

0-0

.03

0.6

5(0

.12)

8.9

7(1

.32)

113.6

3(0

.89)

13.0

3(1

.72)

0.1

7—

——

—0.4

1—

——

—0.8

3G

12.2

0-0

.03

0.8

0(0

.12)

3.1

7(0

.90)

119.2

5(0

.19)

3.7

0(0

.66)

0.1

7—

——

—0.4

1—

——

—0.8

3G

12.4

2+

0.5

01.5

6(0

.27)

18.9

2(0

.81)

6.3

3(0

.24)

11.3

7(0

.58)

0.1

7—

——

—0.5

9—

——

—0.9

0G

12.4

2+

0.5

0*

10.2

4(0

.27)

59.7

8(2

.04)

18.1

6(0

.03)

5.4

8(0

.10)

0.1

719.1

5(1

.14)

131.6

2(2

.19)

17.4

8(0

.05)

6.4

6(0

.12)

0.5

97.6

9(0

.99)

44.2

9(3

.02)

17.6

6(0

.18)

5.4

1(0

.45)

0.9

0G

12.4

2+

0.5

01.6

0(0

.27)

9.0

9(0

.66)

30.8

4(0

.16)

5.3

4(0

.53)

0.1

72.1

4(0

.45)

10.4

8(1

.92)

30.3

1(0

.42)

4.6

1(0

.97)

0.5

9—

——

—0.9

0G

12.6

8-0

.18

3.6

8(0

.11)

35.7

2(2

.17)

8.8

3(0

.26)

9.1

2(0

.44)

0.1

72.5

7(0

.07)

18.9

9(0

.96)

7.3

5(0

.18)

6.9

5(0

.35)

0.1

41.6

3(0

.38)

16.3

8(2

.25)

8.1

0(0

.60)

9.4

6(1

.79)

0.5

6G

12.6

8-0

.18

1.4

0(0

.11)

8.8

4(1

.60)

14.8

4(0

.38)

5.9

2(*

)0.1

71.4

4(0

.07)

6.4

2(0

.91)

13.9

3(0

.21)

4.1

8(0

.45)

0.1

4—

——

—0.5

6G

12.6

8-0

.18

2.4

6(0

.11)

12.7

9(0

.96)

21.0

4(0

.13)

4.8

9(0

.38)

0.1

71.2

6(0

.07)

6.1

1(0

.47)

22.0

6(0

.17)

4.5

6(0

.39)

0.1

4—

——

—0.5

6G

12.6

8-0

.18

1.6

6(0

.11)

5.2

3(0

.54)

25.3

2(0

.14)

2.9

6(*

)0.1

7—

——

—0.1

4—

——

—0.5

6G

12.6

8-0

.18

15.2

7(0

.37)

98.4

5(0

.94)

35.0

3(0

.37)

6.0

6(0

.37)

0.1

712.2

7(0

.27)

72.0

2(1

.45)

33.2

3(0

.90)

5.5

1(0

.81)

0.1

411.4

3(0

.60)

65.6

4(1

.57)

33.9

0(0

.06)

5.4

0(0

.16)

0.5

6G

12.6

8-0

.18

2.5

4(0

.37)

21.6

1(0

.94)

41.0

2(0

.37)

8.0

0(*

)0.1

71.8

9(0

.27)

12.5

9(1

.45)

39.8

3(0

.90)

6.2

5(0

.81)

0.1

41.7

9(0

.60)

7.4

5(1

.09)

41.5

4(*

)3.9

2(*

)0.5

6G

12.6

8-0

.18

6.8

4(0

.37)

50.4

4(0

.94)

48.9

6(0

.37)

6.9

3(0

.37)

0.1

74.2

4(0

.27)

21.0

9(1

.45)

47.1

3(0

.90)

4.6

7(0

.81)

0.1

43.2

1(0

.60)

24.1

0(1

.46)

48.5

9(*

)7.0

5(*

)0.5

6G

12.6

8-0

.18*

7.2

1(0

.37)

50.8

5(0

.94)

57.4

7(0

.37)

6.6

3(0

.37)

0.1

73.5

7(0

.27)

33.2

1(1

.45)

55.8

4(0

.90)

8.7

4(0

.81)

0.1

44.3

1(0

.60)

24.3

2(1

.53)

57.

38(0

.16)

5.3

0(0

.39)

0.5

6G

12.6

8-0

.18

2.8

3(0

.37)

13.3

2(0

.94)

73.6

1(0

.37)

4.4

3(0

.37)

0.1

71.7

9(0

.27)

10.9

1(1

.45)

72.6

8(0

.90)

5.7

1(0

.81)

0.1

4—

——

—0.5

6G

12.9

1-0

.03

2.9

3(0

.46)

32.0

5(0

.69)

11.1

5(0

.37)

10.2

8(0

.37)

0.1

71.4

0(0

.23)

15.9

2(0

.57)

10.0

3(*

)10.7

0(*

)0.1

41.3

9(0

.72)

17.6

1(2

.68)

10.9

0(*

)11.9

1(1

.73)

0.6

3G

12.9

1-0

.03

3.7

5(0

.46)

36.0

5(0

.69)

23.0

6(0

.37)

9.0

3(0

.37)

0.1

71.9

5(0

.23)

13.8

2(0

.63)

21.8

3(0

.14)

6.6

5(0

.30)

0.1

41.3

5(0

.72)

9.3

7(2

.54)

21.8

0(*

)6.5

3(1

.50)

0.6

3G

12.9

1-0

.03

6.0

0(0

.46)

58.1

4(0

.69)

35.9

7(0

.37)

9.1

0(0

.37)

0.1

73.7

5(0

.23)

36.4

5(0

.77)

33.9

8(0

.08)

9.1

4(0

.21)

0.1

42.1

1(0

.72)

23.3

8(2

.91)

33.3

4(*

)10.3

9(1

.68)

0.6

3G

12.9

1-0

.03

6.6

9(0

.46)

53.3

8(0

.69)

48.2

0(0

.37)

7.4

9(0

.37)

0.1

72.7

5(0

.23)

21.5

1(1

.15)

47.3

8(0

.16)

7.3

4(0

.39)

0.1

41.1

6(0

.72)

11.7

0(2

.11)

47.9

7(*

)9.4

5(*

)0.6

3G

12.9

1-0

.03*

6.7

9(0

.46)

49.9

6(0

.69)

57.1

3(0

.37)

6.9

1(0

.37)

0.1

73.7

0(0

.23)

23.5

5(1

.00)

55.6

6(0

.11)

5.9

7(0

.21)

0.1

43.0

5(0

.72)

26.5

3(1

.86)

55.

96(*

)8.1

7(*

)0.6

3G

12.9

1-0

.03

0.7

9(0

.11)

2.3

3(0

.32)

127.9

8(0

.20)

2.7

9(0

.41)

0.1

70.8

1(0

.11)

4.4

7(0

.45)

126.9

3(0

.26)

5.1

7(0

.56)

0.1

4—

——

—0.6

3G

12.9

1-0

.26

3.9

0(0

.28)

42.5

8(0

.54)

12.2

6(0

.06)

10.2

5(0

.16)

0.1

71.6

6(0

.13)

15.2

8(0

.63)

10.6

1(0

.18)

8.6

4(0

.37)

0.1

51.1

4(0

.30)

7.1

3(1

.37)

9.7

9(0

.56)

5.8

8(1

.30)

0.5

1G

12.9

1-0

.26

3.5

8(0

.51)

16.6

4(0

.52)

23.9

6(0

.06)

4.3

7(0

.15)

0.1

72.1

0(0

.19)

10.9

7(1

.15)

22.7

0(0

.90)

4.9

0(0

.81)

0.1

51.6

1(0

.35)

10.7

0(3

.32)

24.6

2(0

.75)

6.2

4(2

.19)

0.5

1G

12.9

1-0

.26

12.9

4(0

.51)

105.8

9(1

.21)

33.6

0(0

.04)

7.6

8(0

.10)

0.1

77.0

5(0

.19)

46.2

0(1

.15)

31.9

9(0

.90)

6.1

5(0

.81)

0.1

55.2

9(0

.35)

32.1

3(4

.34)

32.0

3(0

.22)

5.7

1(0

.72)

0.5

1G

12.9

1-0

.26*

6.8

3(0

.51)

32.2

7(0

.79)

39.5

9(0

.05)

4.4

4(*

)0.1

73.8

3(0

.19)

23.0

0(1

.15)

38.6

0(0

.90)

5.6

3(0

.81)

0.1

52.1

8(0

.35)

9.9

8(2

.94)

38.9

2(0

.40)

4.3

0(0

.90)

0.5

1G

12.9

1-0

.26

7.0

9(0

.51)

44.6

9(0

.49)

45.3

2(0

.06)

5.9

2(*

)0.1

73.1

5(0

.19)

25.0

1(1

.15)

46.3

5(0

.90)

7.4

7(0

.81)

0.1

52.5

0(0

.35)

37.8

1(8

.40)

45.1

8(*

)14.2

1(2

.76)

0.5

1G

12.9

1-0

.26

7.0

8(0

.51)

72.4

7(0

.57)

53.1

6(0

.06)

9.6

2(*

)0.1

73.0

9(0

.19)

30.5

2(1

.15)

54.3

9(0

.90)

9.2

9(0

.81)

0.1

50.9

5(0

.35)

10.0

8(4

.59)

54.0

8(*

)9.9

6(1

.21)

0.5

1G

12.9

1-0

.26

2.5

3(0

.18)

9.5

5(0

.34)

74.9

1(0

.06)

3.5

5(0

.17)

0.1

70.7

5(0

.06)

3.2

2(0

.43)

73.3

2(0

.26)

4.0

3(0

.61)

0.1

5—

——

—0.5

1G

12.9

1-0

.26

0.4

9(0

.18)

2.2

9(0

.27)

86.3

1(0

.36)

4.3

7(*

)0.1

70.6

3(0

.06)

2.0

0(0

.35)

85.6

7(0

.28)

2.9

8(0

.55)

0.1

5—

——

—0.5

1G

14.3

3-0

.64

9.4

4(0

.43)

59.4

8(0

.66)

18.9

7(0

.04)

5.9

2(*

)0.1

73.5

9(0

.21)

20.3

4(1

.90)

17.2

0(0

.18)

5.3

2(0

.45)

0.1

93.3

8(0

.46)

16.8

3(4

.02)

17.5

0(0

.44)

4.6

7(0

.85)

0.5

2G

14.3

3-0

.64*

9.4

5(0

.43)

59.5

6(0

.64)

24.4

1(0

.05)

5.9

2(*

)0.1

76.3

4(0

.21)

36.1

0(1

.45)

22.2

7(0

.11)

5.3

5(*

)0.1

95.1

9(0

.46)

27.8

2(4

.20)

22.8

0(0

.31)

5.0

4(0

.73)

0.5

2G

14.3

3-0

.64

3.6

0(0

.43)

37.9

3(0

.87)

35.5

8(0

.10)

9.8

9(0

.28)

0.1

72.1

4(0

.21)

22.4

9(1

.02)

34.7

2(0

.21)

9.8

7(0

.52)

0.1

9—

——

—0.5

2G

14.3

3-0

.64

0.9

9(0

.43)

10.7

1(0

.74)

52.9

4(0

.34)

10.1

7(0

.79)

0.1

70.8

1(0

.21)

3.4

6(0

.49)

52.1

8(0

.37)

4.0

1(*

)0.1

9—

——

—0.5

2G

14.6

3-0

.58*

16.7

8(0

.35)

112.1

5(0

.84)

18.8

3(0

.37)

6.2

8(0

.37)

0.2

09.7

1(0

.21)

59.1

4(1

.10)

17.6

3(0

.90)

5.7

2(0

.81)

0.1

89.6

9(0

.58)

56.6

1(1

.90)

18.1

7(0

.08)

5.4

9(0

.22)

0.5

7G

14.6

3-0

.58

3.3

4(0

.35)

15.5

8(0

.84)

26.1

7(0

.37)

4.3

8(0

.37)

0.2

02.2

9(0

.21)

13.9

2(1

.10)

25.2

7(0

.90)

5.7

1(0

.81)

0.1

81.3

5(0

.58)

10.5

3(1

.72)

26.6

1(0

.94)

7.3

5(*

)0.5

7

286 Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293

Table

1C

onti

nued

CO

J=

1-0

CO

J=

2-1

CO

J=

3-2

Sourc

eT

MB

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

G14.6

3-0

.58

3.5

6(0

.35)

26.8

0(0

.84)

31.9

8(0

.37)

7.0

7(0

.37)

0.2

01.4

3(0

.21)

12.2

0(1

.10)

30.0

8(*

)7.9

9(*

)0.1

8—

——

—0.5

7G

14.6

3-0

.58

5.3

6(0

.35)

12.8

5(0

.84)

37.8

4(0

.37)

2.2

5(0

.37)

0.2

01.2

9(0

.21)

4.1

8(1

.10)

37.4

3(*

)3.0

5(*

)0.1

8—

——

—0.5

7G

14.6

3-0

.58

1.9

6(0

.35)

23.1

1(0

.84)

42.8

6(0

.37)

11.1

1(0

.37)

0.2

01.3

8(0

.21)

12.1

6(1

.10)

43.0

3(0

.90)

8.2

7(0

.81)

0.1

8—

——

—0.5

7G

14.6

3-0

.58

1.3

8(0

.25)

8.8

7(0

.44)

59.3

3(0

.21)

6.0

2(*

)0.2

00.8

7(0

.09)

2.2

8(0

.37)

59.6

8(0

.22)

2.4

6(0

.35)

0.1

8—

——

—0.5

7G

16.5

8-0

.08

0.8

8(0

.06)

3.4

0(0

.26)

-9.8

1(0

.14)

3.6

2(0

.29)

0.2

00.4

8(0

.06)

2.1

6(0

.31)

-10.3

0(0

.31)

4.2

3(0

.58)

0.1

20.9

9(0

.08)

2.2

2(0

.95)

-10.1

4(0

.42)

2.1

1(1

.39)

0.4

7G

16.5

8-0

.08

1.0

3(0

.07)

2.8

5(*

)18.5

2(0

.10)

2.6

0(0

.20)

0.2

0—

——

—0.1

2—

——

—0.4

7G

16.5

8-0

.08

2.0

0(0

.60)

10.6

9(0

.61)

27.1

9(0

.37)

5.0

2(*

)0.2

0—

——

—0.1

2—

——

—0.4

7G

16.5

8-0

.08*

2.4

2(0

.60)

22.1

8(0

.61)

39.8

1(*

)8.6

1(*

)0.2

00.9

9(0

.25)

5.1

6(1

.01)

41.4

1(0

.48)

4.9

1(0

.84)

0.1

2f

1.8

7(0

.26)

5.0

8(1

.16)

39.2

2(0

.23)

2.5

6(0

.73)

0.4

7G

16.5

8-0

.08

5.0

0(0

.60)

13.3

4(0

.61)

51.0

3(0

.37)

2.5

1(0

.37)

0.2

02.2

7(0

.25)

7.7

9(0

.47)

49.9

2(0

.07)

3.2

3(0

.24)

0.1

2f

1.4

6(0

.44)

8.4

9(2

.26)

50.5

5(0

.45)

5.4

7(2

.15)

0.4

7G

16.5

8-0

.08

7.6

7(0

.60)

46.0

9(0

.61)

58.8

8(0

.37)

5.6

4(0

.37)

0.2

05.9

2(0

.25)

28.7

9(0

.36)

58.4

2(0

.03)

4.5

7(0

.06)

0.1

24.1

3(0

.44)

16.4

6(1

.22)

58.7

7(0

.13)

3.7

4(0

.35)

0.4

7G

16.5

8-0

.08

1.0

6(0

.13)

7.5

0(0

.37)

70.4

4(0

.16)

6.6

2(0

.38)

0.2

00.5

2(0

.25)

4.9

6(0

.50)

69.8

1(0

.47)

9.0

0(0

.94)

0.1

2—

——

—0.4

7G

16.5

8-0

.08

3.6

2(0

.13)

15.0

3(0

.27)

103.2

4(0

.04)

3.9

0(0

.08)

0.2

02.5

3(0

.12)

10.7

0(0

.30)

102.0

7(0

.06)

3.9

8(0

.11)

0.1

21.4

3(0

.18)

5.7

7(0

.99)

102

.19(0

.33)

3.7

9(0

.74)

0.4

7G

16.5

9-0

.05

1.5

2(0

.17)

5.6

5(0

.42)

-9.5

9(0

.14)

3.4

9(0

.27)

0.2

0—

——

—0.2

0—

——

—0.4

8G

16.5

9-0

.05

3.4

0(0

.29)

10.5

2(0

.37)

19.3

4(0

.37)

2.9

1(0

.37)

0.2

0—

——

—0.2

0—

——

—0.4

8G

16.5

9-0

.05

2.2

3(0

.29)

6.8

9(0

.37)

23.2

2(0

.37)

2.9

1(0

.37)

0.2

0—

——

—0.2

0—

——

—0.4

8G

16.5

9-0

.05

2.0

2(0

.29)

13.8

2(0

.37)

28.3

0(0

.37)

6.4

3(0

.37)

0.2

0—

——

—0.2

0—

——

—0.4

8G

16.5

9-0

.05

1.6

6(0

.29)

10.8

6(0

.37)

34.6

9(0

.37)

6.1

6(0

.37)

0.2

0—

——

—0.2

0—

——

—0.4

8G

16.5

9-0

.05

4.2

1(0

.29)

42.6

2(0

.37)

42.5

9(0

.37)

9.5

1(0

.37)

0.2

00.8

8(0

.41)

7.4

9(0

.73)

44.1

2(*

)8.0

2(*

)0.2

0f

——

——

0.4

8G

16.5

9-0

.05

3.8

5(0

.62)

14.9

7(0

.99)

51.1

6(0

.07)

3.6

5(0

.35)

0.2

00.8

9(0

.41)

4.4

3(0

.56)

48.8

0(*

)4.6

8(*

)0.2

0f

——

——

0.4

8G

16.5

9-0

.05*

13.9

4(0

.62)

78.5

8(0

.64)

59.0

4(0

.02)

5.2

9(0

.05)

0.2

07.4

2(0

.41)

38.8

2(0

.65)

57.9

9(0

.04)

4.9

1(0

.09)

0.2

06.6

0(0

.50)

31.7

8(1

.26)

58.3

7(0

.09)

4.5

2(0

.21)

0.4

8G

16.5

9-0

.05

4.1

6(0

.17)

13.9

6(0

.42)

103.2

2(0

.05)

3.1

5(0

.11)

0.2

01.2

1(0

.10)

4.3

8(0

.57)

101.5

4(0

.22)

3.4

1(0

.48)

0.2

0—

——

—0.4

8G

16.6

1-0

.24

——

——

—2.1

6(0

.26)

17.5

2(0

.65)

28.3

1(0

.14)

7.6

3(0

.28)

0.1

7f

1.9

4(0

.40)

12.2

4(1

.71)

29.2

6(0

.42)

5.9

2(0

.99)

0.5

8G

16.6

1-0

.24*

——

——

—3.9

7(0

.18)

28.1

5(0

.63)

44.3

5(0

.07)

6.6

7(0

.15)

0.1

7f

3.6

2(0

.40)

23.6

4(1

.66)

44.2

1(0

.22)

6.1

3(0

.47)

0.5

8G

16.6

1-0

.24

——

——

—3.7

5(0

.18)

17.4

5(0

.52)

55.4

0(0

.06)

4.3

7(0

.14)

0.1

72.8

5(0

.40)

8.5

6(1

.10)

55.4

3(0

.18)

2.8

2(0

.39)

0.5

8G

16.6

1-0

.24

——

——

—1.0

7(0

.12)

4.4

0(0

.49)

72.4

0(0

.21)

3.8

5(0

.47)

0.1

7—

——

—0.5

8G

17.9

6+

0.0

8*

9.0

4(0

.31)

50.4

9(0

.49)

22.6

0(0

.02)

5.2

5(0

.06)

0.2

04.9

5(0

.17)

24.3

7(0

.28)

22.0

4(0

.02)

4.6

3(0

.06)

0.0

95.4

9(0

.45)

23.8

6(0

.98)

22.

08(0

.08)

4.0

8(0

.20)

0.4

1G

17.9

6+

0.0

81.6

4(0

.31)

10.3

1(0

.44)

32.4

4(0

.21)

5.9

2(*

)0.2

00.5

6(0

.17)

5.0

1(0

.38)

32.4

4(*

)8.3

5(*

)0.0

9—

——

—0.4

1G

17.9

6+

0.0

83.0

8(0

.31)

24.2

4(0

.49)

40.4

5(0

.12)

7.4

0(*

)0.2

00.6

9(0

.17)

5.7

8(0

.39)

39.7

8(0

.26)

7.8

6(0

.49)

0.0

9—

——

—0.4

1G

17.9

6+

0.0

81.5

5(0

.31)

8.5

7(0

.38)

50.3

5(0

.18)

5.1

8(*

)0.2

00.3

6(0

.17)

1.2

7(0

.19)

50.5

8(0

.34)

3.3

4(*

)0.0

9—

——

—0.4

1G

17.9

6+

0.0

82.0

8(0

.31)

11.4

7(0

.37)

58.6

8(0

.11)

5.1

8(*

)0.2

00.7

2(0

.17)

3.5

4(0

.26)

57.4

3(0

.17)

4.5

9(0

.33)

0.0

9—

——

—0.4

1G

17.9

6+

0.0

81.9

6(0

.13)

7.0

5(0

.34)

112.8

6(0

.08)

3.3

9(0

.19)

0.2

00.6

1(0

.05)

2.5

1(0

.24)

111.9

6(0

.18)

3.8

3(0

.41)

0.0

91.1

1(0

.01)

1.5

2(0

.57)

112.9

7(0

.25)

1.2

9(0

.88)

0.4

1G

17.9

6+

0.0

82.2

0(0

.13)

11.8

1(0

.41)

128.6

1(0

.09)

5.0

4(0

.19)

0.2

01.1

1(0

.05)

6.2

9(0

.29)

127.4

5(0

.12)

5.3

1(0

.27)

0.0

91.0

1(0

.13)

2.3

4(0

.67)

127.

25(0

.37)

2.1

8(0

.63)

0.4

1G

18.6

7+

0.0

30.9

8(0

.15)

3.5

0(0

.81)

17.2

8(0

.27)

3.3

4(0

.94)

0.1

6—

——

—0.0

9—

——

—0.6

2G

18.6

7+

0.0

31.7

1(0

.15)

6.2

7(2

.49)

21.9

6(0

.19)

3.4

6(0

.89)

0.1

61.4

4(0

.23)

7.8

1(0

.35)

21.1

3(0

.10)

5.1

0(0

.27)

0.0

92.5

7(0

.35)

2.4

2(0

.85)

21.3

2(0

.09)

0.8

8(1

3.0

6)

0.6

2G

18.6

7+

0.0

33.8

5(0

.15)

24.1

2(2

.16)

26.5

7(0

.24)

5.8

8(0

.45)

0.1

61.4

8(0

.23)

8.2

5(0

.37)

26.9

8(0

.05)

5.2

3(0

.23)

0.0

91.3

5(0

.35)

8.3

9(1

.73)

27.0

7(0.5

9)

5.8

5(1

.53)

0.6

2G

18.6

7+

0.0

32.0

4(0

.15)

12.2

7(0

.44)

36.3

9(0

.09)

5.6

4(0

.26)

0.1

60.7

9(0

.23)

7.8

9(0

.33)

36.8

1(0

.27)

9.3

6(*

)0.0

9—

——

—0.6

2G

18.6

7+

0.0

31.8

4(0

.38)

7.1

6(0

.35)

43.6

2(0

.09)

3.6

5(0

.18)

0.1

6—

——

—0.0

9—

——

—0.6

2G

18.6

7+

0.0

38.1

5(0

.38)

44.9

3(0

.61)

49.9

0(0

.03)

5.1

7(0

.08)

0.1

63.7

3(0

.23)

25.8

7(0

.47)

50.0

1(0

.05)

6.5

2(0

.13)

0.0

93.0

5(0

.23)

12.4

1(1

.30)

49.6

6(0

.21)

3.8

3(0

.42)

0.6

2G

18.6

7+

0.0

33.5

8(0

.38)

30.4

5(0

.64)

59.0

5(0

.07)

7.9

8(0

.21)

0.1

61.2

6(0

.23)

11.7

7(0

.50)

60.1

6(*

)8.7

9(0

.37)

0.0

91.0

6(0

.29)

11.8

0(3

.42)

60.3

3(1

.30)

10.4

2(3

.88)

0.6

2G

18.6

7+

0.0

31.3

1(0

.26)

11.4

4(0

.69)

69.4

6(0

.19)

8.1

8(0

.60)

0.1

6—

——

—0.0

9—

——

—0.6

2G

18.6

7+

0.0

3*

7.6

7(0

.26)

54.8

5(0

.56)

79.6

3(0

.03)

6.7

2(0

.08)

0.1

64.0

6(0

.21)

25.8

2(0

.33)

78.7

8(0

.04)

5.9

8(0

.08)

0.0

93.4

5(0

.40)

23.9

1(1

.84)

78.

89(0

.24)

6.5

0(0

.63)

0.6

2

Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293 287

Table

1C

onti

nued

CO

J=

1-0

CO

J=

2-1

CO

J=

3-2

Sourc

eT

MB

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

G18.6

7+

0.0

30.8

7(0

.08)

5.6

8(0

.53)

92.9

6(0

.24)

6.1

2(0

.70)

0.1

6—

——

—0.0

9—

——

—0.6

2G

18.6

7+

0.0

30.5

2(0

.08)

1.3

5(0

.37)

98.0

2(0

.23)

2.4

4(0

.55)

0.1

60.3

0(0

.04)

1.2

0(0

.27)

96.0

1(0

.41)

3.7

2(0

.89)

0.0

9—

——

—0.6

2G

18.6

7+

0.0

31.6

8(0

.08)

7.3

0(0

.33)

103.8

1(0

.09)

4.0

8(0

.23)

0.1

60.8

7(0

.04)

4.2

1(0

.40)

102.3

8(0

.19)

4.5

7(0

.44)

0.0

9—

——

—0.6

2G

18.6

7+

0.0

31.0

2(0

.08)

4.0

7(0

.31)

110.2

1(0

.14)

3.7

6(0

.35)

0.1

60.3

9(0

.04)

2.3

0(0

.43)

109.4

5(0

.43)

5.6

0(1

.17)

0.0

9—

——

—0.6

2G

18.6

7+

0.0

32.2

5(0

.13)

11.5

4(0

.44)

123.1

3(0

.08)

4.8

3(0

.21)

0.1

60.8

8(0

.07)

6.7

6(0

.47)

121.7

1(0

.22)

7.2

1(0

.56)

0.0

9—

——

—0.6

2G

18.6

7+

0.0

32.5

2(0

.13)

12.5

9(0

.45)

129.6

7(0

.07)

4.7

0(0

.20)

0.1

60.7

5(0

.07)

3.1

8(0

.36)

128.8

8(0

.19)

3.9

9(0

.36)

0.0

9—

——

—0.6

2G

19.0

1-0

.03

2.5

8(0

.60)

30.2

9(1

.01)

23.2

9(0

.37)

11.0

4(0

.37)

0.1

60.8

4(0

.30)

11.1

1(0

.78)

22.8

1(0

.43)

12.4

6(0

.83)

0.1

3—

——

—0.7

3G

19.0

1-0

.03

3.3

3(0

.60)

28.3

5(1

.01)

35.9

1(0

.37)

7.9

9(0

.37)

0.1

61.8

1(0

.30)

11.7

5(0

.87)

34.7

6(*

)6.1

0(0

.41)

0.1

32.3

4(0

.64)

11.3

9(1

.93)

35.4

3(0

.38)

4.5

8(0

.95)

0.7

3G

19.0

1-0

.03

12.0

0(0

.60)

99.3

8(1

.01)

46.2

7(0

.37)

7.7

8(0

.37)

0.1

66.9

2(0

.30)

54.2

0(0

.64)

44.8

0(0

.04)

7.3

6(0

.10)

0.1

37.5

5(0

.64)

46.8

9(2

.11)

45.

15(0

.13)

5.8

4(0

.30)

0.7

3G

19.0

1-0

.03

3.0

8(0

.60)

10.5

3(1

.01)

53.1

4(0

.37)

3.2

1(0

.37)

0.1

61.8

0(0

.30)

8.9

9(0

.40)

52.8

1(*

)4.6

8(*

)0.1

3—

——

—0.7

3G

19.0

1-0

.03*

10.8

7(0

.60)

104.9

8(1

.01)

60.2

9(0

.37)

9.0

7(0

.37)

0.1

65.3

4(0

.30)

37.1

3(0

.06)

59.6

5(0

.04)

6.5

2(0

.08)

0.1

34.9

8(0

.64)

29.3

9(2

.21)

60.0

4(0

.21)

5.5

4(0

.55)

0.7

3G

19.0

1-0

.03

1.9

9(0

.17)

17.4

4(1

.07)

112.2

4(0

.22)

8.2

6(0

.58)

0.1

61.4

6(0

.14)

10.7

2(0

.48)

111.7

1(0

.15)

6.9

2(0

.33)

0.1

3—

——

—0.7

3G

19.0

1-0

.03

1.7

0(0

.17)

16.0

7(0

.99)

123.7

4(0

.29)

8.8

6(0

.59)

0.1

60.7

4(0

.14)

5.4

3(0

.46)

123.1

3(0

.29)

6.8

9(0

.59)

0.1

3—

——

—0.7

3G

34.2

6+

0.1

52.5

5(0

.26)

10.3

9(0

.25)

12.3

0(0

.05)

3.8

3(0

.10)

0.1

6—

——

—0.1

2—

——

—0.3

8G

34.2

6+

0.1

52.1

8(0

.11)

5.0

3(0

.24)

27.2

0(0

.05)

2.1

6(0

.12)

0.1

60.8

3(0

.06)

1.7

4(0

.29)

26.2

4(0

.17)

1.9

7(0

.35)

0.1

2—

——

—0.3

8G

34.2

6+

0.1

51.5

1(0

.11)

5.4

5(0

.31)

31.5

3(0

.09)

3.4

0(0

.27)

0.1

60.9

7(0

.06)

3.5

8(0

.41)

31.1

9(0

.18)

3.4

8(0

.49)

0.1

2—

——

—0.3

8G

34.2

6+

0.1

50.7

4(0

.50)

4.3

1(0

.43)

39.8

5(0

.25)

5.5

0(0

.66)

0.1

6—

——

—0.1

2—

——

—0.3

8G

34.2

6+

0.1

53.2

9(0

.50)

22.2

3(0

.82)

48.6

3(0

.09)

6.3

4(0

.25)

0.1

61.3

7(0

.22)

7.8

0(0

.54)

47.0

9(0

.16)

5.3

5(0

.47)

0.1

20.6

6(0

.41)

6.0

5(1

.30)

48.6

6(0.9

8)

8.6

1(*

)0.3

8G

34.2

6+

0.1

5*

8.7

1(0

.50)

42.1

6(0

.89)

55.2

9(0

.02)

4.5

5(0

.09)

0.1

64.9

5(0

.22)

23.3

1(0

.51)

54.7

1(0

.04)

4.4

3(0

.11)

0.1

28.2

2(0

.41)

34.9

2(1

.20)

55.

32(0

.06)

3.9

9(0

.14)

0.3

8G

34.2

6+

0.1

56.6

8(0

.50)

49.3

8(0

.60)

63.9

2(0

.03)

6.9

4(0

.12)

0.1

65.0

8(0

.22)

30.6

1(0

.55)

63.0

9(0

.04)

5.6

7(0

.11)

0.1

24.5

4(0

.41)

23.3

4(1

.13)

63.0

9(0

.11)

4.8

3(0

.30)

0.3

8G

34.2

6+

0.1

50.8

9(0

.50)

4.9

2(0

.35)

72.5

3(0

.28)

5.1

7(*

)0.1

60.5

5(0

.22)

3.6

2(0

.47)

71.9

3(*

)6.2

2(*

)0.1

2—

——

—0.3

8G

34.2

6+

0.1

51.9

3(0

.18)

15.6

4(0

.54)

78.7

2(0

.10)

7.6

2(0

.34)

0.1

61.1

7(0

.22)

7.7

3(0

.42)

78.7

0(0

.22)

6.2

2(*

)0.1

2—

——

—0.3

8G

34.2

6+

0.1

52.4

2(0

.18)

36.1

5(0

.57)

96.8

3(0

.11)

14.0

2(0

.24)

0.1

61.3

4(0

.07)

16.8

0(0

.74)

97.9

8(0

.26)

11.7

6(0

.54)

0.1

2—

——

—0.3

8G

34.2

6+

0.1

52.9

9(0

.18)

3.9

7(0

.18)

102.3

4(0

.02)

1.2

5(0

.06)

0.1

61.2

6(0

.07)

2.1

0(0

.33)

101.2

8(0

.10)

1.5

6(0

.21)

0.1

2—

——

—0.3

8G

34.2

8+

0.1

80.4

8(0

.18)

3.5

5(0

.29)

-24.8

7(0

.31)

6.9

4(0

.49)

0.1

60.4

8(0

.07)

3.3

6(0

.47)

-24.8

9(0

.45)

6.6

2(1

.00)

0.1

3—

——

—0.3

5G

34.2

8+

0.1

82.4

1(0

.22)

11.1

9(0

.23)

12.0

2(0

.05)

4.3

7(0

.10)

0.1

6—

——

—0.1

3—

——

—0.3

5G

34.2

8+

0.1

81.6

4(0

.22)

5.7

1(0

.59)

27.5

4(0

.17)

3.2

6(0

.29)

0.1

60.6

0(0

.03)

2.7

3(2

.66)

27.7

3(1

.94)

4.2

8(2

.72)

0.1

3—

——

—0.3

5G

34.2

8+

0.1

81.3

2(0

.22)

5.1

8(0

.66)

31.8

3(0

.20)

3.6

9(0

.52)

0.1

60.6

7(0

.03)

2.1

7(2

.64)

31.0

7(1

.01)

3.0

6(1

.63)

0.1

3—

——

—0.3

5G

34.2

8+

0.1

83.5

9(0

.39)

25.2

3(0

.70)

49.9

0(0

.07)

6.6

0(0

.23)

0.1

61.6

4(0

.14)

5.3

0(0

.48)

48.2

6(0

.10)

3.0

4(0

.27)

0.1

31.1

3(0

.22)

1.9

4(0

.51)

48.5

3(0.2

1)

1.6

1(0

.35)

0.3

5G

34.2

8+

0.1

8*

4.6

3(0

.39)

29.1

5(0

.69)

55.8

7(*

)5.9

2(*

)0.1

62.3

0(0

.14)

15.9

6(1

.27)

55.4

7(0

.18)

6.5

3(0

.49)

0.1

33.9

5(0

.22)

20.9

7(1

.15)

55.4

0(0

.12)

4.9

9(0

.32)

0.3

5G

34.2

8+

0.1

86.4

1(0

.39)

39.5

3(0

.40)

63.2

2(0

.03)

5.8

0(0

.08)

0.1

63.0

9(0

.14)

18.0

7(1

.10)

62.4

8(0

.13)

5.4

9(0

.27)

0.1

32.6

6(0

.22)

13.7

2(1

.14)

62.4

9(0

.18)

4.8

4(0

.47)

0.3

5G

34.2

8+

0.1

82.2

1(0

.18)

14.3

7(0

.43)

78.8

4(0

.07)

6.1

0(0

.22)

0.1

61.2

5(0

.14)

10.7

1(0

.69)

77.0

6(0

.21)

8.0

6(0

.69)

0.1

30.6

9(0

.26)

5.3

9(0

.91)

76.8

7(*

)7.3

5(*

)0.3

5G

34.2

8+

0.1

81.3

6(0

.18)

6.1

5(0

.47)

85.3

8(0

.11)

4.2

4(0

.26)

0.1

60.6

2(0

.14)

1.9

6(0

.36)

85.8

6(0

.25)

2.9

8(0

.48)

0.1

3—

——

—0.3

5G

34.2

8+

0.1

82.5

5(0

.18)

27.0

8(0

.60)

95.2

6(0

.08)

9.9

8(0

.28)

0.1

61.0

6(0

.04)

8.1

6(0

.69)

95.3

8(0

.29)

7.2

3(0

.68)

0.1

30.7

5(0

.27)

6.7

5(1

.23)

96.0

1(0.7

2)

8.4

2(1

.98)

0.3

5G

34.2

8+

0.1

82.2

8(0

.18)

4.2

2(0

.25)

102.3

8(0

.03)

1.7

4(0

.10)

0.1

60.9

9(0

.04)

2.6

2(0

.61)

101.4

7(0

.17)

2.4

8(0

.50)

0.1

3—

——

—0.3

5G

34.2

8+

0.1

80.6

9(0

.18)

2.8

9(0

.26)

106.6

1(*

)3.9

5(0

.43)

0.1

60.6

5(0

.04)

1.8

3(0

.40)

105.1

6(0

.27)

2.6

5(0

.57)

0.1

3—

——

—0.3

5G

34.3

9+

0.2

23.6

5(0

.33)

15.6

4(0

.40)

12.7

7(0

.05)

4.0

3(0

.12)

0.1

6—

——

—0.0

91.2

7(*

)1.1

9(0

.39)

11.6

5(0

.18)

0.8

8(1

1.4

1)

0.3

2G

34.3

9+

0.2

23.0

8(0

.40)

12.9

7(0

.40)

29.2

6(0

.06)

3.9

6(0

.14)

0.1

61.2

3(0

.07)

4.9

9(0

.40)

27.9

3(0

.15)

3.8

3(0

.32)

0.0

90.7

5(0

.04)

2.1

6(0

.57)

27.8

9(0.3

8)

2.7

1(0

.77)

0.3

2G

34.3

9+

0.2

20.9

2(0

.11)

3.8

8(0

.46)

41.8

6(0

.20)

3.9

7(0

.65)

0.1

6—

——

—0.0

9—

——

—0.3

2G

34.3

9+

0.2

23.3

5(0

.25)

24.7

6(1

.93)

51.7

0(0

.26)

6.9

4(0

.45)

0.1

61.6

9(0

.21)

5.8

8(0

.52)

53.0

7(0

.11)

3.2

7(0

.21)

0.0

92.9

4(0

.40)

10.0

9(1

.00)

54.3

8(*

)3.2

3(0

.32)

0.3

2G

34.3

9+

0.2

23.9

0(0

.25)

10.6

1(1

.22)

55.0

8(0

.05)

2.5

5(0

.14)

0.1

6—

——

—0.0

9—

——

—0.3

2

288 Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293

Table

1C

onti

nued

CO

J=

1-0

CO

J=

2-1

CO

J=

3-2

Sourc

eT

MB

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

G34.3

9+

0.2

2*

4.6

0(0

.25)

36.5

5(0

.72)

59.9

6(0

.15)

7.4

6(*

)0.1

63.4

5(0

.21)

28.5

6(1

.04)

60.2

8(0

.10)

7.7

8(0

.30)

0.0

93.5

8(0

.40)

26.8

0(0

.92)

59.7

4(0.2

2)

7.0

4(*

)0.3

2G

34.3

9+

0.2

22.9

7(0

.25)

19.0

2(0

.99)

67.6

5(0

.07)

6.0

1(0

.34)

0.1

61.6

4(0

.21)

10.0

0(0

.95)

67.5

1(*

)5.7

2(0

.41)

0.0

91.0

7(0

.40)

7.1

6(0

.88)

67.0

4(0

.55)

6.2

6(*

)0.3

2G

34.3

9+

0.2

23.0

0(0

.25)

24.9

4(0

.58)

79.0

0(0

.09)

7.8

2(0

.20)

0.1

61.2

7(0

.21)

9.0

2(0

.54)

78.2

8(0

.19)

6.6

7(0

.44)

0.0

90.8

0(0

.24)

6.2

4(0

.77)

77.9

8(0.3

9)

7.3

5(*

)0.3

2G

34.3

9+

0.2

22.2

8(0

.13)

15.1

0(3

.00)

89.2

3(0

.31)

6.2

1(0

.57)

0.1

61.2

2(0

.07)

7.7

0(1

.30)

88.8

4(0

.37)

5.9

2(0

.82)

0.0

90.5

7(0

.24)

2.5

6(0

.73)

89.0

9(0.0

1)

4.2

1(1

.23)

0.3

2G

34.3

9+

0.2

22.7

7(0

.13)

29.2

5(3

.53)

97.1

7(0

.43)

9.9

1(1

.18)

0.1

61.3

4(0

.07)

10.5

8(1

.76)

97.3

9(0

.35)

7.3

9(1

.32)

0.0

90.7

3(0

.24)

5.2

0(0

.79)

97.8

3(0

.70)

6.6

8(*

)0.3

2G

34.3

9+

0.2

24.0

4(0

.13)

11.3

1(0

.70)

105.4

1(0

.04)

2.6

3(0

.12)

0.1

61.7

6(0

.07)

6.2

8(0

.88)

104.0

8(0

.13)

3.3

4(0

.30)

0.0

91.4

4(0

.24)

4.1

8(0

.58)

104.

30(0

.19)

2.7

3(0

.40)

0.3

2G

34.4

1+

0.2

43.7

6(0

.34)

15.6

8(0

.32)

12.7

6(0

.04)

3.9

2(0

.09)

0.1

6—

——

—0.0

9—

——

—0.3

4G

34.4

1+

0.2

43.0

0(0

.34)

9.3

5(0

.28)

28.7

0(0

.04)

2.9

2(0

.11)

0.1

61.0

5(0

.11)

4.4

3(0

.36)

28.0

3(0

.16)

3.9

5(0

.36)

0.0

9—

——

—0.3

4G

34.4

1+

0.2

4*

3.8

8(0

.38)

25.0

7(0

.53)

53.4

0(0

.37)

6.0

7(0

.37)

0.1

61.5

7(0

.14)

6.9

6(0

.31)

53.1

4(0

.12)

4.1

5(*

)0.0

92.1

0(0

.23)

9.8

2(1

.07)

54.3

6(0

.25)

4.4

0(0

.55)

0.3

4G

34.4

1+

0.2

43.9

8(0

.38)

23.3

7(0

.53)

60.2

0(0

.37)

5.5

1(0

.37)

0.1

63.7

1(0

.14)

14.7

9(1

.18)

58.9

9(0

.06)

3.7

5(0

.16)

0.0

94.0

2(0

.23)

10.9

5(1

.10)

58.9

0(0

.09)

2.5

6(0

.26)

0.3

4G

34.4

1+

0.2

42.8

1(0

.38)

18.3

7(0

.53)

67.9

3(0

.37)

6.1

4(0

.37)

0.1

62.1

1(0

.14)

20.6

1(1

.43)

65.3

8(0

.29)

9.1

6(0

.61)

0.0

91.3

6(0

.23)

13.5

9(1

.12)

63.5

0(*

)9.3

6(*

)0.3

4G

34.4

1+

0.2

42.5

0(0

.38)

16.6

1(0

.53)

79.4

1(0

.37)

6.2

3(0

.37)

0.1

61.3

2(0

.05)

7.6

9(0

.47)

78.0

7(0

.16)

5.4

7(0

.35)

0.0

90.6

6(0

.21)

3.8

9(0

.88)

79.0

2(0.6

3)

5.5

8(1

.25)

0.3

4G

34.4

1+

0.2

43.8

9(0

.16)

36.9

6(1

.23)

90.3

4(0

.13)

8.9

3(0

.33)

0.1

61.0

8(0

.05)

9.5

7(0

.64)

89.2

0(0

.26)

8.2

9(0

.63)

0.0

90.6

2(0

.21)

3.1

2(0

.86)

89.0

9(0.8

0)

4.7

3(1

.56)

0.3

4G

34.4

1+

0.2

42.3

7(0

.16)

13.2

8(1

.33)

98.6

2(0

.13)

5.2

7(0

.45)

0.1

60.6

7(0

.05)

2.5

4(0

.53)

97.8

0(0

.30)

3.5

9(0

.67)

0.0

9—

——

—0.3

4G

34.4

1+

0.2

44.2

4(0

.16)

16.8

5(0

.54)

104.6

9(0

.05)

3.7

3(0

.12)

0.1

61.8

6(0

.05)

7.9

5(0

.45)

103.1

5(0

.11)

4.0

1(0

.24)

0.0

91.0

8(0

.21)

3.9

8(0

.67)

103.

89(0

.30)

3.4

5(0

.57)

0.3

4G

35.0

3+

0.3

55.1

5(0

.30)

23.6

6(0

.39)

13.7

1(0

.03)

4.3

2(0

.09)

0.1

6—

——

—0.1

4—

——

—0.3

4G

35.0

3+

0.3

55.6

5(0

.50)

23.1

6(0

.41)

43.6

1(0

.04)

3.8

5(0

.07)

0.1

62.9

4(0

.37)

17.1

4(0

.69)

43.0

6(0

.11)

5.4

7(0

.24)

0.1

41.7

1(0

.42)

8.5

0(1

.07)

43.9

4(0

.27)

4.6

6(0

.70)

0.3

4G

35.0

3+

0.3

5*

11.1

5(0

.50)

91.4

0(1

.45)

51.9

9(0

.04)

7.7

0(0

.10)

0.1

69.0

1(0

.37)

52.3

1(0

.80)

51.0

1(0

.03)

5.4

5(0

.09)

0.1

46.9

2(0

.42)

38.2

9(1

.47)

51.6

2(0

.08)

5.2

0(0

.21)

0.3

4G

35.0

3+

0.3

54.2

3(0

.50)

7.2

4(0

.30)

53.7

3(0

.03)

1.6

1(0

.05)

0.1

6—

——

—0.1

4—

——

—0.3

4G

35.0

3+

0.3

53.0

3(0

.50)

26.4

4(1

.53)

56.5

5(*

)8.1

9(*

)0.1

61.6

6(0

.37)

9.9

4(0

.53)

56.8

9(*

)5.6

1(*

)0.1

41.2

8(0

.42)

8.5

2(1

.08)

57.6

2(0

.45)

6.2

6(*

)0.3

4G

35.0

3+

0.3

52.1

1(0

.15)

14.1

1(0

.63)

73.9

5(0

.11)

6.2

7(0

.40)

0.1

61.0

5(0

.07)

6.8

0(1

.04)

72.8

6(0

.42)

6.0

8(0

.87)

0.1

4—

——

—0.3

4G

35.0

3+

0.3

52.1

7(0

.15)

5.8

7(0

.53)

79.9

5(0

.07)

2.5

4(0

.20)

0.1

61.4

0(0

.07)

6.3

7(1

.01)

78.8

1(0

.24)

4.2

8(0

.53)

0.1

4—

——

—0.3

4G

35.0

3+

0.3

51.3

6(0

.15)

10.0

1(0

.98)

86.5

6(0

.22)

6.9

0(0

.80)

0.1

60.6

0(0

.07)

3.3

3(0

.76)

87.0

5(0

.49)

5.1

9(1

.26)

0.1

4—

——

—0.3

4G

35.0

3+

0.3

51.8

6(0

.15)

10.3

4(0

.75)

94.4

3(0

.17)

5.2

2(0

.36)

0.1

60.3

5(0

.07)

1.1

5(0

.66)

92.3

2(0

.65)

3.0

8(1

.56)

0.1

4—

——

—0.3

4G

35.0

3+

0.3

52.6

0(0

.15)

9.7

1(0

.33)

102.9

7(0

.06)

3.5

1(0

.13)

0.1

61.7

0(0

.10)

5.8

0(0

.37)

102.2

2(0

.10)

3.2

1(0

.21)

0.1

40.8

8(0

.28)

4.3

8(0

.71)

103.2

4(0

.44)

4.7

0(*

)0.3

4G

35.0

4-0

.47

4.8

6(0

.40)

16.8

9(0

.22)

14.0

9(0

.02)

3.2

7(0

.05)

0.1

6—

——

—0.1

31.6

0(0

.11)

1.5

0(0

.38)

15.4

0(0

.07)

0.8

8(2

.44)

0.3

3G

35.0

4-0

.47

0.6

1(0

.40)

2.7

8(0

.54)

29.4

1(0

.37)

4.2

7(0

.37)

0.1

6—

——

—0.1

3—

——

—0.3

3G

35.0

4-0

.47

1.5

7(0

.40)

2.5

9(0

.54)

36.6

3(0

.37)

1.5

5(0

.37)

0.1

6—

——

—0.1

3—

——

—0.3

3G

35.0

4-0

.47

7.8

7(0

.40)

52.6

8(0

.54)

44.2

7(0

.37)

6.2

9(0

.37)

0.1

64.1

1(0

.09)

21.9

5(1

.18)

42.9

3(0

.12)

5.0

2(0

.21)

0.1

32.4

4(0

.34)

10.0

8(1

.78)

43.7

3(0

.28)

3.8

8(0

.59)

0.3

3G

35.0

4-0

.47*

6.9

7(0

.40)

41.5

4(0

.54)

51.0

8(0

.37)

5.6

0(0

.37)

0.1

64.5

8(0

.09)

32.1

4(1

.25)

49.9

8(0

.12)

6.5

9(0

.25)

0.1

34.0

7(0

.34)

28.0

3(1

.91)

50.

05(0

.23)

6.4

7(0

.48)

0.3

3G

35.0

4-0

.47

1.0

7(0

.40)

2.3

7(0

.54)

61.8

1(0

.37)

2.0

7(0

.37)

0.1

61.0

1(0

.06)

2.3

3(0

.52)

61.6

2(0

.20)

2.1

7(0

.45)

0.1

31.0

2(0

.08)

1.9

2(0

.45)

62.0

7(0

.22)

1.7

7(0

.40)

0.3

3G

35.0

4-0

.47

0.5

2(0

.12)

3.1

9(0

.36)

83.0

9(0

.31)

5.7

6(0

.74)

0.1

60.3

8(0

.11)

1.3

5(0

.47)

80.0

6(0

.60)

3.3

3(1

.20)

0.1

3—

——

—0.3

3G

35.0

4-0

.47

6.3

7(0

.12)

26.4

8(0

.29)

90.3

8(0

.02)

3.9

0(0

.04)

0.1

63.5

6(0

.11)

18.4

8(0

.58)

89.5

6(0

.07)

4.8

8(0

.17)

0.1

32.6

3(0

.23)

10.6

1(0

.75)

90.4

8(0

.13)

3.7

9(0

.35)

0.3

3G

35.1

3-0

.74

2.9

6(0

.20)

11.7

1(0

.27)

13.5

1(0

.04)

3.7

2(0

.10)

0.1

6—

——

—0.3

8—

——

—0.6

0G

35.1

3-0

.74*

23.7

8(1

.08)

172.6

1(0

.36)

33.8

3(*

)6.8

2(0

.02)

0.1

619.7

6(0

.70)

157.9

3(1

.53)

33.3

0(0

.04)

7.5

1(0

.07)

0.3

813.8

6(1

.18)

104.3

7(1

.90)

34.1

6(0

.07)

7.0

7(0

.15)

0.6

0G

35.1

3-0

.74

4.0

3(1

.08)

24.4

8(0

.51)

47.2

3(0

.06)

5.7

1(0

.13)

0.1

61.9

0(0

.70)

8.0

3(1

.11)

46.2

7(0

.26)

3.9

7(0

.60)

0.3

81.3

0(0

.32)

6.1

4(1

.69)

46.7

9(0.5

6)

4.4

4(1

.64)

0.6

0G

35.1

3-0

.74

3.6

5(1

.08)

18.0

0(0

.48)

53.8

4(0

.06)

4.6

3(0

.13)

0.1

61.5

6(0

.70)

4.0

6(0

.93)

53.1

1(0

.28)

2.4

4(0

.53)

0.3

8—

——

—0.6

0G

35.1

5+

0.8

00.6

2(0

.11)

3.4

4(0

.55)

51.1

5(0

.67)

5.1

8(*

)0.1

60.4

7(0

.04)

1.3

3(0

.22)

50.3

2(0

.25)

2.6

5(0

.42)

0.1

2—

——

—0.3

4G

35.1

5+

0.8

00.9

9(0

.11)

3.9

0(0

.51)

56.1

8(0

.32)

3.7

0(*

)0.1

60.4

7(0

.04)

1.4

8(0

.26)

55.4

5(0

.23)

2.9

4(0

.58)

0.1

2—

——

—0.3

4G

35.1

5+

0.8

0*

9.3

5(0

.38)

38.2

3(0

.55)

74.2

7(0

.03)

3.8

4(0

.07)

0.1

64.4

4(0

.17)

19.3

6(0

.29)

73.2

9(0

.03)

4.0

9(0

.07)

0.1

23.5

3(0

.22)

16.0

1(0

.82)

73.

67(0

.10)

4.2

6(0

.26)

0.3

4G

35.2

0-0

.74

3.3

4(0

.43)

13.2

8(0

.24)

14.0

5(0

.03)

3.7

4(0

.08)

0.1

6—

——

—0.8

8—

——

—0.5

8

Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293 289

Table

1C

onti

nued

CO

J=

1-0

CO

J=

2-1

CO

J=

3-2

Sourc

eT

MB

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

G35.2

0-0

.74*

9.7

0(0

.24)

50.0

1(1

.40)

30.7

0(0

.04)

4.8

4(0

.08)

0.1

67.2

1(0

.84)

46.2

1(1

.71)

30.8

0(0

.18)

6.0

2(*

)0.8

83.4

5(0

.46)

34.3

4(5

.41)

31.0

3(0.8

0)

9.3

6(*

)0.5

8G

35.2

0-0

.74

10.6

5(0

.24)

68.4

6(1

.39)

35.9

2(0

.05)

6.0

4(0

.09)

0.1

66.0

8(0

.84)

38.9

1(1

.71)

37.2

9(0

.22)

6.0

2(*

)0.8

84.1

5(0

.46)

35.4

0(5

.34)

37.0

2(0.5

3)

8.0

2(*

)0.5

8G

35.2

0-0

.74

1.1

5(0

.24)

3.2

0(0

.29)

47.7

1(0

.08)

2.6

2(0

.20)

0.1

6—

——

—0.8

8—

——

—0.5

8G

35.2

0-0

.74

1.0

8(0

.24)

2.4

9(0

.20)

54.4

7(0

.05)

2.1

5(0

.16)

0.1

6—

——

—0.8

8—

——

—0.5

8G

35.6

8-0

.18

3.3

3(0

.54)

18.5

3(0

.44)

13.6

6(0

.05)

5.2

3(0

.18)

0.1

6—

——

—0.1

6—

——

—0.3

8G

35.6

8-0

.18*

9.1

4(0

.54)

45.8

9(0

.39)

28.4

3(0

.02)

4.7

1(0

.05)

0.1

64.7

7(0

.24)

20.1

9(0

.58)

27.2

6(0

.05)

3.9

7(0

.13)

0.1

63.2

0(0

.32)

10.6

5(0

.90)

28.

47(0

.11)

3.1

3(0

.37)

0.3

8G

35.6

8-0

.18

4.5

8(0

.29)

21.6

5(0

.35)

51.5

1(0

.06)

4.4

4(*

)0.1

61.6

4(0

.08)

9.4

5(1

.10)

50.6

8(0

.26)

5.4

2(0

.72)

0.1

60.8

9(0

.20)

3.6

6(1

.44)

50.5

6(0

.77)

3.8

8(1

.95)

0.3

8G

35.6

8-0

.18

3.2

7(0

.29)

12.8

8(0

.37)

56.1

9(0

.10)

3.7

0(*

)0.1

62.4

6(0

.08)

8.7

5(0

.72)

55.5

7(0

.15)

3.3

4(*

)0.1

61.4

0(0

.20)

4.8

2(3

.53)

55.5

6(0

.47)

3.2

5(1

.29)

0.3

8G

35.6

8-0

.18

4.4

8(0

.29)

21.1

9(0

.46)

60.2

8(0

.08)

4.4

4(*

)0.1

62.0

5(0

.08)

8.7

5(0

.87)

59.9

1(0

.19)

4.0

1(*

)0.1

61.2

8(0

.20)

8.5

0(3

.58)

59.5

6(1

.23)

6.2

5(2

.36)

0.3

8G

35.6

8-0

.18

2.3

9(0

.29)

17.0

2(0

.70)

66.7

2(0

.09)

6.6

8(0

.33)

0.1

60.7

4(0

.08)

5.6

7(1

.24)

65.3

5(0

.76)

7.2

0(1

.54)

0.1

6—

——

—0.3

8G

35.6

8-0

.18

1.0

1(0

.29)

7.9

9(0

.30)

80.0

0(0

.29)

7.4

0(*

)0.1

6—

——

—0.1

6—

——

—0.3

8G

35.7

9-0

.17

——

——

—4.3

7(0

.12)

15.2

6(0

.50)

27.4

0(0

.05)

3.2

8(0

.11)

0.1

64.1

9(0

.14)

13.5

9(0

.77)

28.2

1(0

.09)

3.0

5(0

.20)

0.3

8G

35.7

9-0

.17

——

——

—0.8

0(0

.02)

1.9

8(0

.40)

44.1

6(0

.24)

2.3

3(0

.46)

0.1

61.3

8(0

.31)

3.0

2(0

.60)

44.7

4(0

.23)

2.0

6(0

.41)

0.3

8G

35.7

9-0

.17

——

——

—1.7

2(0

.09)

6.4

0(0

.56)

50.2

6(0

.14)

3.4

9(0

.32)

0.1

6—

——

—0.3

8G

35.7

9-0

.17*

——

——

—2.6

5(0

.09)

21.6

4(0

.79)

59.5

9(0

.14)

7.6

8(0

.30)

0.1

61.0

7(0

.34)

11.5

0(1

.58)

61.3

9(0

.61)

10.1

3(1

.91)

0.3

8G

35.7

9-0

.17

——

——

—0.5

5(0

.07)

1.8

6(0

.49)

71.3

5(0

.43)

3.2

0(0

.93)

0.1

6—

——

—0.3

8G

35.7

9-0

.17

——

——

—1.1

0(0

.07)

4.8

6(0

.53)

79.5

4(0

.23)

4.1

6(0

.44)

0.1

6—

——

—0.3

8G

35.7

9-0

.17

——

——

—0.2

8(0

.07)

1.3

5(0

.53)

87.4

1(0

.97)

4.5

6(1

.48)

0.1

6—

——

—0.3

8G

35.7

9-0

.17

——

——

—0.6

6(0

.07)

1.3

4(0

.35)

96.3

2(0

.26)

1.9

1(0

.45)

0.1

6—

——

—0.3

8G

35.8

3-0

.20

2.5

0(0

.24)

9.6

3(0

.63)

12.7

9(0

.10)

3.6

1(0

.33)

0.1

6—

——

—0.2

5—

——

—0.3

0G

35.8

3-0

.20*

9.0

1(0

.57)

49.7

9(0

.72)

28.4

6(0

.04)

5.1

9(0

.10)

0.1

64.9

4(0

.35)

20.8

0(0

.85)

27.6

9(0

.08)

3.9

5(0

.18)

0.2

53.3

6(0

.28)

14.9

4(0

.75)

28.

40(0

.10)

4.1

8(0

.25)

0.3

0G

35.8

3-0

.20

4.4

3(0

.30)

16.6

8(0

.44)

44.7

9(0

.37)

3.5

4(0

.37)

0.1

61.7

5(0

.20)

7.4

0(1

.10)

44.2

3(0

.27)

3.9

8(0

.77)

0.2

51.4

6(0

.16)

4.0

7(0

.56)

44.5

6(0.1

9)

2.6

2(0

.39)

0.3

0G

35.8

3-0

.20

2.8

7(0

.30)

14.4

1(0

.44)

51.5

9(0

.37)

4.7

2(0

.37)

0.1

61.6

0(0

.20)

9.2

7(0

.93)

51.8

6(0

.54)

5.4

3(*

)0.2

50.8

5(0

.20)

5.5

3(0

.28)

53.9

3(0

.88)

6.1

2(0

.88)

0.3

0G

35.8

3-0

.20

2.3

8(0

.30)

3.7

9(0

.44)

54.5

1(0

.37)

1.4

9(*

)0.1

6—

——

—0.2

5—

——

—0.3

0G

35.8

3-0

.20

4.6

2(0

.30)

26.1

5(0

.44)

58.7

6(0

.37)

5.3

2(0

.37)

0.1

62.6

1(0

.20)

14.8

7(1

.32)

58.8

3(0

.23)

5.3

5(0

.51)

0.2

51.1

1(0

.20)

5.5

8(0

.28)

59.6

8(0

.88)

4.7

1(0

.88)

0.3

0G

35.8

3-0

.20

2.4

8(0

.30)

17.7

0(0

.44)

63.0

4(0

.37)

6.7

2(*

)0.1

6—

——

—0.2

5—

——

—0.3

0G

35.8

3-0

.20

0.8

7(0

.14)

4.1

2(0

.75)

80.2

6(0

.57)

4.4

3(*

)0.1

6—

——

—0.2

5—

——

—0.3

0G

35.8

3-0

.20

1.5

5(0

.14)

7.0

1(0

.97)

85.1

0(0

.28)

4.2

4(0

.62)

0.1

61.1

6(0

.10)

3.5

9(0

.67)

83.8

7(0

.29)

2.9

0(0

.54)

0.2

5—

——

—0.3

0G

36.0

1-0

.20

2.5

6(0

.08)

8.7

3(0

.28)

12.7

2(0

.05)

3.2

0(0

.12)

0.1

6—

——

—0.2

2—

——

—0.4

0G

36.0

1-0

.20

2.4

9(0

.20)

3.8

8(0

.20)

29.3

0(0

.03)

1.4

6(0

.10)

0.1

6—

——

—0.2

2—

——

—0.4

0G

36.0

1-0

.20

2.2

7(0

.20)

16.9

8(0

.42)

37.7

0(0

.08)

7.0

1(0

.22)

0.1

6—

——

—0.2

2—

——

—0.4

0G

36.0

1-0

.20

3.7

2(0

.18)

37.6

8(0

.69)

57.5

7(0

.08)

9.5

2(0

.17)

0.1

61.0

8(0

.10)

7.0

6(1

.23)

55.6

2(0

.61)

6.1

3(1

.00)

0.2

2—

——

—0.4

0G

36.0

1-0

.20

1.8

1(0

.18)

17.2

2(0

.89)

65.1

5(*

)8.9

4(0

.07)

0.1

60.6

9(0

.10)

3.4

8(0

.89)

62.0

7(1

.01)

4.7

3(*

)0.2

2—

——

—0.4

0G

36.0

1-0

.20

0.4

0(0

.18)

2.0

2(0

.38)

78.9

5(0

.30)

4.7

2(*

)0.1

6—

——

—0.2

2—

——

—0.4

0G

36.0

1-0

.20*

4.5

2(0

.18)

13.6

8(0

.30)

87.1

3(0

.02)

2.8

4(0

.06)

0.1

61.8

0(0

.15)

6.2

9(0

.63)

86.1

2(0

.16)

3.2

9(0

.34)

0.2

21.1

9(0

.23)

4.0

6(0

.89)

87.5

7(*

)3.2

2(0

.76)

0.4

0G

39.1

0+

0.4

90.8

6(0

.12)

2.8

1(0

.55)

-22.6

1(0

.24)

3.0

8(0

.61)

0.2

6—

——

—0.1

6—

——

—0.2

1G

39.1

0+

0.4

90.8

3(0

.12)

5.7

5(0

.73)

-15.9

1(0

.36)

6.4

8(1

.08)

0.2

6—

——

—0.1

6—

——

—0.2

1G

39.1

0+

0.4

92.1

8(0

.26)

17.3

5(0

.80)

14.9

1(0

.16)

7.4

7(0

.40)

0.2

60.7

8(0

.15)

5.5

6(0

.70)

13.3

7(0

.41)

6.6

6(0

.96)

0.1

6—

——

—0.2

1G

39.1

0+

0.4

9*

4.3

0(0

.26)

16.2

6(0

.83)

21.9

5(0

.06)

3.5

5(0

.16)

0.2

61.7

6(0

.15)

6.8

9(0

.65)

21.1

1(0

.15)

3.6

7(0

.30)

0.1

61.0

4(0

.26)

3.9

8(0

.47)

20.5

3(0

.21)

3.6

0(0

.46)

0.2

1G

39.1

0+

0.4

94.0

4(0

.26)

28.5

7(1

.16)

29.1

8(0

.09)

6.6

4(0

.34)

0.2

62.6

3(0

.15)

15.6

9(0

.90)

27.7

6(0

.13)

5.5

9(0

.36)

0.1

61.4

0(0

.26)

10.9

8(0

.57)

27.4

1(*

)7.3

5(*

)0.2

1G

39.1

0+

0.4

91.9

1(0

.26)

7.6

9(1

.11)

35.9

5(0

.18)

3.7

8(0

.43)

0.2

60.8

3(0

.15)

4.4

7(0

.94)

34.7

6(*

)5.0

6(1

.03)

0.1

6—

——

—0.2

1

290 Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293

Table

1C

onti

nued

CO

J=

1-0

CO

J=

2-1

CO

J=

3-2

Sourc

eT

MB

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

G39.1

0+

0.4

91.4

5(0

.26)

11.4

5(0

.98)

42.6

5(0

.26)

7.4

4(0

.77)

0.2

60.6

2(0

.15)

3.4

8(0

.70)

42.8

4(0

.43)

5.2

5(1

.27)

0.1

6—

——

—0.2

1G

39.3

9-0

.14

0.9

5(0

.27)

3.3

8(0

.22)

11.5

0(0

.15)

3.3

4(*

)0.1

4—

——

—0.5

6—

——

—0.4

4G

39.3

9-0

.14

2.8

2(0

.27)

10.1

9(0

.31)

16.5

2(0

.05)

3.4

0(0

.13)

0.1

41.9

1(0

.32)

4.7

5(0

.69)

16.3

4(0

.17)

2.3

4(0

.46)

0.5

61.3

1(0

.25)

9.3

9(1

.42)

16.2

5(0.4

9)

6.7

2(1

.22)

0.4

4G

39.3

9-0

.14

3.0

7(0

.27)

12.3

1(0

.29)

30.4

4(0

.04)

3.7

7(0

.11)

0.1

41.4

9(0

.20)

6.0

6(0

.70)

30.1

4(0

.22)

3.8

2(0

.46)

0.5

61.3

4(0

.06)

2.6

7(0

.71)

29.3

1(0.2

6)

1.8

7(0

.55)

0.4

4G

39.3

9-0

.14

3.6

2(0

.20)

11.9

2(0

.23)

42.4

4(0

.03)

3.0

9(0

.07)

0.1

41.9

3(0

.30)

5.7

6(0

.62)

42.4

4(0

.15)

2.8

0(0

.33)

0.5

60.9

8(0

.35)

7.0

4(0

.37)

42.3

7(0.8

8)

6.7

6(0

.88)

0.4

4G

39.3

9-0

.14*

6.3

2(0

.18)

37.0

0(0

.42)

66.0

6(0

.02)

5.5

0(0

.07)

0.1

42.7

7(0

.26)

12.7

9(1

.01)

65.8

5(0

.14)

4.3

4(0

.36)

0.5

64.1

9(0

.36)

22.4

6(1

.32)

65.

08(0

.13)

5.0

4(0

.39)

0.4

4G

39.3

9-0

.14

1.7

6(0

.18)

19.2

1(0

.56)

78.0

4(0

.13)

10.2

4(0

.40)

0.1

40.9

7(0

.26)

12.2

7(1

.41)

78.6

2(0

.58)

11.8

1(1

.65)

0.5

6—

——

—0.4

4G

39.3

9-0

.14

1.1

1(0

.18)

5.6

3(0

.37)

89.0

0(0

.13)

4.7

6(0

.32)

0.1

4—

——

—0.5

6—

——

—0.4

4G

39.3

9-0

.14

3.7

9(0

.18)

41.3

4(0

.60)

55.2

1(0

.06)

10.2

4(*

)0.1

41.9

3(0

.26)

18.4

3(1

.19)

54.6

5(0

.26)

8.9

5(0

.67)

0.5

62.0

0(0

.36)

16.5

3(1

.84)

52.7

4(0.3

7)

7.7

6(1

.17)

0.4

4G

40.2

8-0

.22

1.4

2(0

.15)

9.2

8(0

.36)

30.5

0(0

.11)

6.1

3(0

.29)

0.1

40.4

6(0

.06)

2.1

2(0

.29)

28.6

9(0

.30)

4.3

5(0

.54)

0.1

0—

——

—0.3

6G

40.2

8-0

.22

1.1

2(0

.16)

11.3

5(0

.53)

41.3

8(0

.20)

9.5

5(0

.57)

0.1

40.5

9(0

.15)

4.8

7(0

.41)

41.7

2(0

.05)

7.7

2(0

.64)

0.1

0—

——

—0.3

6G

40.2

8-0

.22

4.1

6(0

.30)

46.4

1(0

.91)

58.9

8(0

.09)

10.4

8(0

.22)

0.1

41.4

1(0

.15)

10.6

0(0

.96)

55.7

7(0

.22)

7.0

5(0

.43)

0.1

01.1

9(0

.30)

4.9

0(1

.65)

55.7

8(0

.58)

3.8

7(1

.29)

0.3

6G

40.2

8-0

.22

2.2

5(0

.30)

8.5

9(0

.63)

65.3

5(0

.06)

3.5

9(0

.14)

0.1

41.3

0(0

.15)

10.2

3(1

.09)

61.7

0(0

.19)

7.4

0(0

.60)

0.1

00.9

9(0

.30)

5.8

0(1

.71)

61.8

1(0.8

5)

5.4

7(1

.76)

0.3

6G

40.2

8-0

.22*

7.0

0(0

.30)

49.5

0(1

.36)

72.5

3(0

.07)

6.6

5(*

)0.1

43.9

3(0

.15)

23.3

3(0

.50)

71.4

1(0

.05)

5.5

8(0

.12)

0.1

03.7

9(0

.30)

22.5

3(1

.16)

71.2

1(0.1

4)

5.5

9(0

.34)

0.3

6G

40.2

8-0

.22

3.8

6(0

.30)

29.9

6(1

.68)

78.3

5(0

.15)

7.2

9(0

.33)

0.1

40.9

7(0

.15)

6.5

7(0

.37)

78.5

4(*

)6.3

6(*

)0.1

01.0

5(0

.30)

5.0

4(1

.10)

77.8

7(*

)4.5

0(0

.99)

0.3

6G

40.2

8-0

.22

1.0

4(0

.30)

10.5

8(0

.56)

86.6

6(0

.03)

9.6

0(*

)0.1

4—

——

—0.1

0—

——

—0.3

6G

40.2

8-0

.27

1.0

2(0

.21)

11.5

2(1

.01)

43.2

6(0

.34)

10.6

6(1

.42)

0.2

40.3

6(0

.07)

1.4

5(0

.30)

41.8

9(0

.43)

3.8

4(0

.82)

0.1

1—

——

—0.3

7G

40.2

8-0

.27

4.4

1(0

.21)

41.3

2(0

.99)

60.3

1(0

.09)

8.8

0(0

.27)

0.2

41.4

7(0

.08)

18.8

9(0

.51)

61.5

0(0

.90)

12.0

5(0

.81)

0.1

11.1

4(0

.29)

10.8

3(1

.37)

60.

67(0

.55)

8.9

7(1

.33)

0.3

7G

40.2

8-0

.27

2.2

9(0

.21)

10.9

4(*

)66.3

3(0

.16)

4.4

9(0

.27)

0.2

4—

——

—0.1

1—

——

—0.3

7G

40.2

8-0

.27*

6.6

1(0

.21)

27.8

4(0

.80)

71.9

7(0

.04)

3.9

6(0

.13)

0.2

44.1

8(0

.08)

17.2

5(0

.51)

70.2

3(0

.90)

3.8

8(0

.81)

0.1

13.8

6(0

.29)

14.9

5(0

.94)

70.

03(0

.10)

3.6

4(0

.24)

0.3

7G

40.2

8-0

.27

2.7

9(0

.21)

13.1

7(0

.43)

77.7

0(0

.11)

4.4

4(*

)0.2

40.9

8(0

.08)

4.4

9(0

.51)

76.2

5(0

.90)

4.3

1(0

.81)

0.1

1—

——

—0.3

7G

40.6

0-0

.72

1.3

8(0

.18)

4.1

7(0

.22)

36.4

8(0

.06)

2.8

5(0

.24)

0.0

80.9

3(0

.07)

2.2

1(0

.26)

34.8

9(0

.12)

2.2

2(0

.31)

0.1

0—

——

—0.4

3G

40.6

0-0

.72

2.6

8(0

.18)

17.1

2(0

.26)

55.8

3(0

.04)

6.0

1(0

.11)

0.0

81.0

5(0

.09)

5.9

4(0

.34)

54.3

8(0

.15)

5.3

3(0

.30)

0.1

0—

——

—0.4

3G

40.6

0-0

.72*

6.0

3(0

.18)

30.1

5(0

.36)

65.9

1(0

.02)

4.7

0(0

.05)

0.0

82.5

0(0

.09)

14.1

6(0

.33)

65.4

1(0

.06)

5.3

3(0

.11)

0.1

01.9

6(0

.20)

6.3

2(0

.87)

64.9

7(0

.20)

3.0

2(0

.49)

0.4

3G

40.6

0-0

.72

1.6

4(0

.18)

3.2

6(0

.15)

77.2

6(0

.04)

1.8

7(0

.09)

0.0

80.7

2(0

.09)

3.5

0(0

.34)

76.3

6(0

.22)

4.5

9(0

.53)

0.1

0—

——

—0.4

3G

43.0

4-0

.45

3.4

5(0

.22)

7.2

1(0

.28)

10.3

5(0

.04)

1.9

6(0

.10)

0.2

41.4

1(0

.08)

2.6

2(0

.15)

9.7

7(0

.05)

1.7

5(0

.10)

0.0

81.1

1(0

.01)

1.7

7(0

.55)

10.2

7(0

.24)

1.5

0(0

.56)

0.4

1G

43.0

4-0

.45

0.5

2(0

.17)

3.2

7(0

.65)

32.0

8(0

.66)

5.9

5(1

.08)

0.2

4—

——

—0.0

8—

——

—0.4

1G

43.0

4-0

.45

1.3

2(0

.17)

5.1

8(0

.80)

36.5

6(*

)3.6

9(*

)0.2

40.3

3(0

.06)

1.6

9(0

.39)

33.8

0(0

.53)

4.8

4(1

.18)

0.0

8—

——

—0.4

1G

43.0

4-0

.45

2.6

5(0

.17)

12.5

6(0

.93)

40.6

6(0

.02)

4.4

4(0

.33)

0.2

41.1

6(0

.06)

4.4

6(0

.37)

39.4

9(0

.13)

3.6

2(0

.27)

0.0

8—

——

—0.4

1G

43.0

4-0

.45

1.1

3(0

.17)

7.1

1(0

.57)

46.1

3(0

.34)

5.9

1(*

)0.2

40.4

7(0

.06)

2.5

1(0

.26)

44.1

2(*

)5.0

2(*

)0.0

8—

——

—0.4

1G

43.0

4-0

.45*

9.3

8(0

.42)

49.1

5(0

.74)

57.4

7(0

.03)

4.9

2(0

.09)

0.2

42.0

1(0

.08)

8.0

4(0

.46)

56.1

5(0

.09)

3.7

6(0

.19)

0.0

82.9

6(0

.21)

9.5

7(1

.03)

56.4

1(0

.14)

3.0

3(0

.33)

0.4

1G

43.0

4-0

.45

2.0

2(0

.42)

7.1

9(0

.49)

62.3

7(0

.16)

3.3

4(*

)0.2

41.4

9(0

.08)

5.0

3(0

.44)

60.3

6(0

.11)

3.1

7(0

.24)

0.0

80.6

9(0

.21)

3.4

5(0

.98)

60.3

4(0

.78)

4.6

8(*

)0.4

1G

43.0

4-0

.45

1.8

0(0

.42)

10.2

4(0

.41)

67.8

1(0

.18)

5.3

5(*

)0.2

40.5

2(0

.08)

3.7

0(0

.30)

65.5

1(*

)6.6

8(*

)0.0

8—

——

—0.4

1G

44.0

1-0

.03

1.1

4(0

.24)

11.1

4(0

.51)

18.1

5(0

.20)

9.1

5(0

.50)

0.2

40.9

9(0

.12)

3.0

0(0

.57)

20.0

2(0

.25)

2.8

3(0

.65)

0.4

1—

——

—0.3

8G

44.0

1-0

.03

1.6

1(0

.28)

19.2

7(0

.49)

46.0

4(0

.17)

11.2

6(0

.14)

0.2

41.0

3(0

.15)

6.7

4(0

.78)

45.2

9(0

.34)

6.1

6(0

.79)

0.4

10.9

5(0

.16)

4.1

7(0

.84)

43.9

5(0

.42)

4.1

4(0

.94)

0.3

8G

44.0

1-0

.03

3.2

3(0

.28)

20.7

3(0

.68)

58.1

3(0

.09)

6.0

3(0

.22)

0.2

41.8

8(0

.44)

10.3

2(1

.36)

59.3

4(0

.34)

5.1

6(0

.78)

0.4

11.4

0(0

.34)

11.2

3(4

.75)

58.9

0(1

.38)

7.5

4(3

.14)

0.3

8G

44.0

1-0

.03*

8.8

7(0

.28)

43.8

9(0

.59)

64.7

8(0

.03)

4.6

5(0

.06)

0.2

45.1

7(0

.44)

22.3

6(1

.24)

65.8

1(0

.11)

4.0

6(0

.22)

0.4

14.5

0(0

.34)

20.9

0(4

.20)

64.

61(0

.22)

4.3

7(0

.38)

0.3

8G

45.4

7+

0.0

51.4

2(0

.18)

6.5

1(0

.53)

8.4

7(0

.17)

4.3

0(0

.39)

0.3

01.2

2(0

.12)

6.7

9(0

.63)

8.1

4(0

.25)

5.2

5(0

.45)

0.2

4—

——

—0.8

6G

45.4

7+

0.0

51.1

9(0

.12)

4.3

3(0

.50)

25.8

6(0

.19)

3.4

2(0

.50)

0.3

0—

——

—0.2

4—

——

—0.8

6G

45.4

7+

0.0

51.3

6(0

.26)

18.7

7(0

.79)

48.9

0(0

.37)

12.9

3(0

.37)

0.3

00.4

4(0

.24)

2.9

6(1

.95)

52.0

5(*

)6.3

1(*

)0.2

41.7

3(0

.68)

15.7

4(3

.42)

48.9

4(1

.31)

8.5

4(*

)0.8

6G

45.4

7+

0.0

511.0

5(0

.26)

71.6

9(0

.79)

57.3

6(0

.37)

6.0

9(0

.37)

0.3

07.2

9(0

.24)

56.9

8(2

.71)

57.3

6(0

.09)

7.3

4(0

.31)

0.2

47.8

9(0

.68)

51.7

0(5

.45)

57.

21(0

.21)

6.1

5(0

.72)

0.8

6

Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293 291

Table

1C

onti

nued

CO

J=

1-0

CO

J=

2-1

CO

J=

3-2

Sourc

eT

MB

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

TM

B

∫T

MB

dV

VLSR

FW

HM

RM

SN

ote

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

(K)

(K·k

m·s−

1)

(km·s−

1)

(km·s−

1)

(K)

G45.4

7+

0.0

5*

6.2

1(0

.26)

53.3

2(0

.79)

62.9

0(0

.37)

8.0

7(0

.37)

0.3

02.6

2(0

.24)

17.5

8(1

.58)

63.0

9(*

)6.3

1(*

)0.2

43.2

2(0

.68)

23.2

7(4

.62)

62.9

0(*

)6.7

9(0

.98)

0.8

6G

45.4

7+

0.1

30.7

3(0

.19)

7.0

0(0

.51)

10.0

3(0

.31)

8.9

5(0

.81)

0.3

0—

——

—0.1

6—

——

—0.6

5G

45.4

7+

0.1

31.5

9(0

.26)

6.5

4(0

.41)

26.0

2(0

.10)

3.8

6(0

.38)

0.3

0—

——

—0.1

6—

——

—0.6

5G

45.4

7+

0.1

35.4

8(0

.74)

23.4

1(0

.90)

55.5

0(0

.04)

4.0

1(0

.09)

0.3

03.6

1(0

.28)

24.2

7(3

.79)

55.9

6(0

.13)

6.3

1(*

)0.1

67.5

3(0

.71)

42.6

1(1

1.8

9)

56.8

6(0.6

4)

5.3

2(0

.79)

0.6

5G

45.4

7+

0.1

3*

12.0

1(0

.74)

99.0

0(1

.06)

61.6

5(0

.04)

7.7

4(0

.10)

0.3

05.8

0(0

.28)

52.5

8(3

.95)

60.2

5(0

.29)

8.5

2(0

.36)

0.1

66.6

7(0

.71)

38.3

2(1

1.8

9)

61.9

7(0

.73)

5.3

9(1

.00)

0.6

5G

45.5

0+

0.1

20.8

3(0

.16)

8.0

3(0

.70)

9.0

3(0

.39)

9.1

3(0

.94)

0.2

40.4

8(0

.11)

3.1

9(0

.47)

7.1

5(0

.50)

6.2

6(0

.87)

0.1

4—

——

—0.6

2G

45.5

0+

0.1

21.3

4(0

.15)

3.7

5(0

.38)

25.7

1(0

.13)

2.6

3(0

.32)

0.2

4—

——

—0.1

4—

——

—0.6

2G

45.5

0+

0.1

2*

8.9

6(0

.39)

95.1

5(0

.71)

59.3

9(0

.04)

9.9

7(0

.09)

0.2

45.5

6(0

.35)

59.3

2(0

.61)

58.7

9(0

.05)

10.0

2(0

.10)

0.1

45.9

9(0

.51)

54.0

4(1

.90)

58.5

7(0

.15)

8.4

8(0

.33)

0.6

2G

45.8

0-0

.36

——

——

—0.6

4(0

.09)

5.6

2(2

.00)

45.1

1(1

.51)

8.2

9(2

.33)

0.1

7—

——

—0.9

6G

45.8

0-0

.36

——

——

—0.7

9(0

.09)

4.3

9(2

.40)

51.9

2(0

.67)

5.2

2(1

.45)

0.1

7—

——

—0.9

6G

45.8

0-0

.36*

——

——

—1.5

0(0

.09)

17.0

7(1

.25)

61.0

1(0

.40)

10.6

5(0

.77)

0.1

72.4

5(0

.77)

35.8

8(4

.25)

62.2

7(0

.81)

13.7

7(2

.00)

0.9

6G

48.6

6-0

.30

1.4

5(0

.07)

4.6

1(0

.20)

6.0

4(0

.06)

2.9

9(0

.15)

0.2

4—

——

—0.2

1—

——

—0.6

6G

48.6

6-0

.30*

6.3

0(0

.28)

24.5

3(0

.27)

33.5

9(0

.37)

3.6

6(0

.37)

0.2

42.5

5(0

.18)

13.4

8(1

.05)

33.0

9(0

.15)

4.9

6(0

.43)

0.2

12.6

9(0

.23)

12.0

7(1

.57)

33.

27(0

.27)

4.2

2(0

.65)

0.6

6G

48.6

6-0

.30

1.9

6(0

.28)

5.8

1(0

.27)

39.3

8(0

.37)

2.7

9(0

.37)

0.2

4—

——

—0.2

1—

——

—0.6

6G

48.6

6-0

.30

0.9

4(0

.28)

3.7

3(0

.27)

51.1

7(0

.37)

3.7

2(0

.37)

0.2

4—

——

—0.2

1—

——

—0.6

6G

48.6

6-0

.30

2.3

6(0

.28)

16.7

4(0

.27)

58.4

6(0

.37)

6.6

7(0

.37)

0.2

4—

——

—0.2

1—

——

—0.6

6G

49.4

2+

0.3

3*

7.0

7(0

.23)

30.8

8(0

.28)

-21.0

8(0

.02)

4.1

1(0

.04)

0.1

53.1

9(0

.10)

13.9

8(0

.23)

-21.3

3(0

.03)

4.1

1(0

.07)

0.0

82.7

5(0

.22)

11.3

0(0

.40)

-21.1

6(0

.07)

3.8

6(0

.16)

0.1

6G

49.4

2+

0.3

30.7

8(0

.08)

3.2

4(0

.61)

-0.2

1(0

.18)

3.8

8(0

.52)

0.1

5—

——

—0.0

8—

——

—0.1

6G

49.4

2+

0.3

30.8

3(0

.08)

1.2

0(0

.23)

7.5

4(0

.09)

1.3

5(0

.23)

0.1

5—

——

—0.0

8—

——

—0.1

6G

49.4

2+

0.3

33.5

9(0

.16)

21.8

6(0

.33)

63.1

7(0

.04)

5.7

3(0

.10)

0.1

51.8

4(0

.07)

13.8

2(0

.29)

61.9

7(0

.07)

7.0

5(0

.15)

0.0

80.8

6(0

.10)

4.7

2(0

.47)

61.9

9(0

.24)

5.1

6(0

.65)

0.1

6G

49.9

1+

0.3

7—

——

——

1.4

6(0

.11)

7.9

6(0

.33)

-1.8

8(0

.10)

5.1

4(0

.23)

0.1

10.8

3(0

.13)

3.4

6(0

.56)

-0.6

2(0

.33)

3.8

9(0

.77)

0.2

4G

49.9

1+

0.3

7*

——

——

—2.9

0(0

.11)

14.7

9(0

.32)

7.5

3(0

.05)

4.7

9(0

.11)

0.1

12.3

3(0

.13)

9.6

4(0

.54)

8.0

0(0

.11)

3.8

8(0

.25)

0.2

4G

49.9

1+

0.3

7—

——

——

0.3

5(0

.11)

1.6

9(0

.25)

17.6

4(*

)4.5

2(*

)0.1

1—

——

—0.2

4G

49.9

1+

0.3

7—

——

——

0.2

7(0

.07)

1.5

4(0

.27)

34.8

5(0

.61)

5.3

5(*

)0.1

1—

——

—0.2

4G

49.9

1+

0.3

7—

——

——

0.4

9(0

.07)

1.3

8(0

.23)

47.3

0(0

.22)

2.6

6(0

.45)

0.1

1—

——

—0.2

4G

49.9

1+

0.3

7—

——

——

0.4

8(0

.07)

1.1

2(0

.22)

59.2

1(0

.21)

2.1

9(0

.47)

0.1

1—

——

—0.2

4G

50.3

6-0

.42

——

——

—1.2

8(0

.13)

4.1

5(0

.51)

13.3

1(0

.19)

3.0

3(0

.35)

0.2

1—

——

—0.5

0G

50.3

6-0

.42*

——

——

—2.6

2(0

.15)

11.6

1(0

.67)

37.1

3(0

.11)

4.1

7(0

.27)

0.2

11.2

9(0

.34)

4.5

0(1

.07)

39.2

3(0

.42)

3.2

7(0

.78)

0.5

0G

50.3

6-0

.42

——

——

—1.6

9(0

.15)

14.5

3(0

.87)

61.8

8(0

.24)

8.0

8(0

.51)

0.2

10.8

6(0

.31)

9.6

6(1

.84)

64.4

7(1

.16)

10.4

9(1

.72)

0.5

0G

53.9

2-0

.07

5.0

0(0

.33)

15.6

4(0

.16)

23.7

4(0

.02)

2.9

4(0

.03)

0.1

12.5

6(0

.17)

9.3

4(0

.45)

22.7

0(0

.08)

3.4

3(0

.16)

0.1

71.5

7(0

.08)

3.6

9(0

.68)

23.7

6(0.2

1)

2.2

1(0

.45)

0.4

2G

53.9

2-0

.07*

1.7

8(0

.16)

12.1

8(0

.14)

43.4

1(0

.37)

6.4

1(0

.37)

0.1

11.7

8(0

.23)

10.3

8(0

.65)

42.0

4(0

.16)

5.4

7(0

.41)

0.1

71.5

5(0

.41)

13.9

5(1

.47)

44.

05(0

.42)

8.4

3(1

.17)

0.4

2G

53.9

2-0

.07

1.3

2(0

.16)

5.1

2(0

.14)

59.4

8(0

.37)

3.6

3(0

.37)

0.1

1—

——

—0.1

7—

——

—0.4

2G

54.1

1-0

.04

2.4

7(0

.26)

4.5

5(0

.16)

23.4

3(0

.03)

1.7

3(0

.07)

0.1

10.9

6(0

.04)

2.1

0(0

.36)

22.0

1(0

.18)

2.0

5(0

.36)

0.1

8—

——

—0.3

9G

54.1

1-0

.04

0.7

4(0

.39)

3.1

7(0

.59)

31.9

5(0

.37)

4.0

3(0

.37)

0.1

10.7

6(0

.17)

3.3

7(0

.61)

31.1

2(*

)4.1

4(0

.70)

0.1

80.3

4(0

.45)

1.9

4(0

.89)

31.7

6(*

)5.

43(*

)0.3

9G

54.1

1-0

.04

13.3

7(0

.39)

81.2

4(0

.59)

39.8

5(0

.37)

5.7

1(0

.37)

0.1

111.0

3(0

.17)

76.2

0(0

.75)

38.8

7(0

.03)

6.4

9(0

.07)

0.1

89.4

0(0

.45)

58.9

6(1

.10)

40.0

1(0

.05)

5.8

9(0

.13)

0.3

9G

54.1

1-0

.04

2.1

0(0

.39)

14.6

6(0

.59)

48.7

3(0

.37)

6.5

5(0

.37)

0.1

10.6

8(0

.17)

4.2

7(0

.62)

49.1

3(0

.44)

5.9

2(0

.73)

0.1

8—

——

—0.3

9G

54.1

1-0

.04

0.3

4(0

.39)

3.1

5(0

.59)

59.0

3(0

.37)

8.7

4(0

.37)

0.1

1—

——

—0.1

8—

——

—0.3

9G

54.1

1-0

.08

1.1

4(0

.10)

2.8

5(0

.17)

-30.0

8(0

.07)

2.3

4(0

.16)

0.1

10.7

8(0

.07)

1.9

4(0

.35)

-31.4

0(0

.22)

2.3

4(0

.42)

0.1

7—

——

—0.4

0G

54.1

1-0

.08

2.8

4(0

.25)

5.2

8(0

.15)

23.0

8(0

.03)

1.7

5(0

.06)

0.1

11.1

4(0

.16)

4.0

3(0

.51)

21.9

4(0

.17)

3.3

3(0

.55)

0.1

7—

——

—0.4

0G

54.1

1-0

.08

2.9

3(0

.46)

13.4

1(0

.62)

33.2

4(0

.37)

4.3

0(*

)0.1

12.4

8(0

.21)

16.3

3(4

.65)

33.6

2(0

.78)

6.2

0(0

.90)

0.1

71.5

5(0

.40)

6.6

2(0

.84)

34.0

9(*

)4.0

1(*

)0.4

0G

54.1

1-0

.08*

12.6

3(0

.46)

79.8

7(0

.62)

39.9

7(0

.37)

5.9

4(0

.37)

0.1

110.3

8(0

.21)

61.4

2(4

.74)

38.9

4(0

.15)

5.5

6(0

.18)

0.1

79.4

0(0

.40)

52.0

9(1

.08)

39.9

2(0

.05)

5.2

1(0

.13)

0.4

0

292

Li Z

hi-g

uan

g a

nd H

e J

in-h

ua / C

hin

ese A

str

on

om

y a

nd A

str

ophysic

s 3

8 (

2014) 2

65–293

Table 1 Continued

CO J=1-0 CO J=2-1 CO J=3-2

Source TMB

∫TMBdV V LSR FWHM RMS Note TMB

∫TMBdV V LSR FWHM RMS Note TMB

∫TMBdV V LSR FWHM RMS Note

(K) (K·km·s−1) (km·s−1) (km·s−1) (K) (K) (K·km·s−1) (km·s−1) (km·s−1) (K) (K) (K·km·s−1) (km·s−1) (km·s−1) (K)G54.11-0.08 1.57(0.46) 6.76(0.62) 48.41(0.37) 4.04(0.37) 0.11 0.84(0.21) 2.86(0.43) 47.18(0.24) 3.18(0.54) 0.17 — — — — 0.40G54.11-0.08 0.48(0.46) 5.06(0.62) 53.99(0.37) 9.93(0.37) 0.11 — — — — 0.17 — — — — 0.40G54.45+1.01 1.26(0.26) 7.15(0.38) -5.14(0.14) 5.32(0.34) 0.16 — — — — 0.17 — — — — 0.45G54.45+1.01 2.09(0.26) 11.51(0.37) 7.75(0.08) 5.16(0.19) 0.16 1.09(0.06) 3.38(0.40) 7.23(0.17) 2.91(0.34) 0.17 1.33(0.13) 3.38(0.73) 7.90(0.27) 2.38(0.52) 0.45G54.45+1.01 1.92(0.34) 4.10(0.23) 26.57(0.06) 2.01(0.14) 0.16 0.93(0.26) 3.59(0.39) 25.77(*) 3.62(*) 0.17 1.07(0.28) 3.03(0.93) 26.39(0.35) 2.66(1.06) 0.45G54.45+1.01* 10.86(0.34) 70.61(0.40) 34.99(0.02) 6.11(0.04) 0.16 6.31(0.26) 37.07(0.58) 33.48(0.04) 5.51(0.09) 0.17 4.56(0.28) 27.70(1.24) 34.03(0.12) 5.70(0.30) 0.45G56.13+0.22 — — — — — 1.69(0.19) 12.42(0.93) 35.65(0.27) 6.89(0.50) 0.15 — — — — 2.85G56.13+0.22 — — — — — 2.41(0.19) 14.41(0.89) 43.71(0.17) 5.62(0.30) 0.15 6.92(1.57) 39.42(6.61) 44.12(*) 5.35(*) 2.85G57.61+0.02* — — — — — 1.93(0.41) 14.10(1.32) 32.99(0.31) 6.86(0.72) 0.66 1.50(0.21) 10.54(1.22) 34.52(0.36) 6.61(1.03) 0.38G58.09-0.34 — — — — — 1.01(0.06) 3.10(0.20) 10.12(0.09) 2.90(0.20) 0.07 0.76(0.09) 3.65(0.49) 9.25(0.30) 4.49(0.68) 0.19G58.09-0.34 — — — — — 0.57(0.08) 5.13(0.97) 21.68(0.72) 8.49(1.47) 0.07 — — — — 0.19G58.09-0.34 — — — — — 1.84(0.08) 8.42(0.85) 27.78(0.09) 4.30(0.19) 0.07 0.93(0.19) 3.90(0.45) 28.33(0.23) 3.94(0.50) 0.19G58.09-0.34 — — — — — 0.61(0.08) 3.44(0.26) 37.31(0.18) 5.30(0.47) 0.07 — — — — 0.19G58.78+0.64 0.42(0.14) 0.81(0.30) 25.59(0.23) 1.80(0.55) 0.16 0.10(0.27) 0.74(0.60) 26.74(*) 6.68(*) 0.15 — — — — 0.52G58.78+0.64* 2.59(0.14) 30.17(4.77) 31.55(0.71) 10.93(0.91) 0.16 1.77(0.27) 16.36(0.65) 32.09(*) 8.69(*) 0.15 1.37(0.41) 10.81(1.67) 30.84(0.59) 7.41(1.31) 0.52G58.78+0.64 1.90(0.14) 3.37(0.33) 30.95(0.05) 1.67(0.14) 0.16 — — — — 0.15 — — — — 0.52G58.78+0.64 1.06(0.14) 12.30(4.85) 41.29(1.68) 10.88(2.31) 0.16 0.64(0.27) 5.04(0.51) 42.78(*) 7.35(*) 0.15 — — — — 0.52G58.79+0.63 — — — — — 0.40(0.09) 1.86(0.53) 23.93(0.73) 4.36(1.44) 0.12 — — — — 0.56G58.79+0.63 — — — — — 1.58(0.09) 8.85(1.82) 31.38(0.33) 5.27(0.88) 0.12 1.62(0.37) 8.22(1.51) 31.57(0.41) 4.75(1.08) 0.56G58.79+0.63 — — — — — 0.96(0.09) 5.93(1.76) 37.25(0.66) 5.79(1.12) 0.12 — — — — 0.56G58.79+0.63 — — — — — 0.50(0.09) 1.50(0.42) 43.08(0.33) 2.81(0.63) 0.12 — — — — 0.56G59.79+0.63 1.05(0.15) 5.16(0.25) 10.42(0.11) 4.63(0.28) 0.16 — — — — 0.60 — — — — 0.43G59.79+0.63 2.35(0.43) 7.17(0.23) 25.80(0.04) 2.87(0.12) 0.16 1.47(0.40) 2.08(0.41) 21.23(0.14) 1.33(0.22) 0.60 0.65(0.28) 3.45(1.62) 23.47(1.18) 4.99(3.84) 0.43G59.79+0.63* 5.52(0.43) 34.19(0.28) 34.38(0.02) 5.81(0.06) 0.16 3.07(0.40) 15.70(0.82) 30.15(0.13) 4.80(0.21) 0.60 3.05(0.28) 10.78(1.05) 30.68(0.15) 3.32(0.38) 0.43G62.70-0.51 — — — — — 1.16(0.08) 2.96(0.14) 24.63(0.05) 2.40(0.14) 0.06 0.99(0.04) 1.58(0.21) 24.88(0.10) 1.49(0.20) 0.15G62.70-0.51 — — — — — 2.30(0.08) 6.71(0.14) 31.83(0.03) 2.74(0.06) 0.06 2.02(0.04) 4.89(0.26) 32.31(0.06) 2.28(0.14) 0.15

Note:(1) The “*” at the end of a source name indicates the velocity component associated with an EGO. Note that the EGO velocities of 5 sources (G54.11-0.04,G56.13+0.22, G58.09-0.34, G58.79+0.63, and G62.70-0.51) are unknown.(2) The uncertainties of some line parameters are shown as “*” which means that the corresponding line parameters were fixed during the Gaussian profilefitting (no error estimate is available).(3) When the values of some line parameters are shown as “-”, it means that the corresponding velocity component is either not detected (RMS is anumerical value) or not observed (RMS is a “-”) for that CO transition.(4) The letter “f” in the Note column indicates the possible contamination by the off-position emission during the position-switching observation.

Li Zhi-guang and He Jin-hua / Chinese Astronomy and Astrophysics 38 (2014) 265–293 293

References

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2 Cyganowski C. J., Whitney B. A., Holden E., et al. AJ, 2008, 136, 2391

3 Chen X., Shen Z. Q., Li J. J., et al., ApJ, 2010, 710, 150

4 Cyganowski C. J., Brogan C. L,, Hunter T. R., et al., ApJ, 2011, 729, 124

5 Cyganowski C. J., Brogan C. L., Hunter T. R., et al., ApJ, 2012, 760, L20

6 He J. H., Takahashi S., Chen X., ApJS, 2012, 202, 1

7 Larson R. B., MNRAS, 1981, 194, 809

8 Solomon P. M., Rivolo A. R., Barrett J., et al., ApJ, 1987, 319, 730

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