11institutetext:  Xinjiang Astronomical Observatory, Chinese Academy of
Sciences, 830011 Urumqi, P. R. China
e-mail<EMAIL_ADDRESS><EMAIL_ADDRESS><EMAIL_ADDRESS>22institutetext: University of Chinese Academy of Sciences, 100080 Beijing, P.
R. China 33institutetext: Key Laboratory of Radio Astronomy, Chinese Academy
of Sciences, Nanjing, JiangSu 210008, P. R. China 44institutetext: Xinjiang
Key Laboratory of Radio Astrophysics, Urumqi 830011, PR China 55institutetext:
Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
66institutetext: Astronomy Department, King Abdulaziz University, PO Box
80203, 21589 Jeddah, Saudi Arabia 77institutetext: Shanghai Astronomical
Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030,
People’s Republic of China 88institutetext: Energetic Cosmos Laboratory,
Nazarbayev University, Astana 010000, Kazakhstan 99institutetext: Institute of
Experimental and Theoretical Physics, Al-Farabi Kazakh National University,
Almaty 050040, Kazakhstan

# Ammonia Observations of Planck Cold Cores

Dilda Berdikhan 1122 Jarken Esimbek 113344 Christian Henkel 551166 Jianjun
Zhou 113344 Xindi Tang 11223344 Tie Liu 77 Gang Wu 55 Dalei Li 11223344 Yuxin
He 11223344 Toktarkhan Komesh 8899 Kadirya Tursun 113344 Dongdong Zhou 113344
Ernar Imanaly 1122 Qaynar Jandaolet 1122

Single-pointing observations of NH3 (1,1) and (2,2) were conducted towards 672
Planck Early Release Cold Cores (ECCs) using the Nanshan 26-m radio telescope.
Out of these sources, a detection rate of 37% (249 cores) was achieved, with
NH3 (1,1) hyperfine structure detected in 187 and NH3 (2,2) emission lines
detected in 76 cores. The detection rate of NH3 is positively correlated with
the continuum emission fluxes at a frequency of 857 GHz. Among the observed
672 cores, $\sim$22% have associated stellar and IR objects within the beam
size ($\sim$2$\arcmin$). This suggests that most of the cores in our sample
may be starless. The kinetic temperatures of the cores range from 8.9 to 20.7
K, with an average of 12.3 K, indicating a coupling between gas and dust
temperatures. The ammonia column densities range from 3.6 $\times$ 1014 to
6.07 $\times$ $10^{15}$ cm-2, with a median value of 2.04 $\times$ $10^{15}$
cm-2. The fractional abundances of ammonia range from 0.3 to 9.7 $\times$
10-7, with an average of 2.7 $\times$ 10-7, which is one order of magnitude
larger than that of Massive Star-Forming (MSF) regions and Infrared Dark
Clouds (IRDCs). The correlation between thermal and non-thermal velocity
dispersion of the NH3 (1,1) inversion transition indicates the dominance of
supersonic non-thermal motions in the dense gas traced by NH3, and the
relationship between these two parameters in Planck cold cores is weaker, with
lower values observed for both parameters relative to other samples under our
examination. The cumulative distribution shapes of line widths in the Planck
cold cores closely resemble those of the dense cores found in regions of
Cepheus, and Orion L1630 and L1641, with higher values compared to Ophiuchus.
However, the higher line width values in the Planck cold cores, when compared
to these dense cores in Ophiuchus, suggest that they might be in more advanced
and warmer stages of evolution. Additionally, the line width remains
relatively small among the various samples examined. A comparison of NH3 line-
center velocities with those of 13CO and C18O shows small differences (0.13 km
s-1 and 0.12 km s-1 ), suggesting quiescence on small scales.

###### Key Words.:

surveys – radio lines: ISM – ISM: molecules – ISM: kinetics and dynamics –
stars: formation

##  1 Introduction

Molecular cores, representing the earliest stages of potential star formation,
are crucial for our understanding of the initial conditions of this important
process shaping the morphology of galaxies. One approach is to conduct a
statistical study of cold dense clumps from unbiased large surveys in the
Milky Way. The Planck satellite has carried out the first all-sky survey in
the submm-to-mm range, providing a wealth of galactic cold dust cores (Planck
Collaboration et al., 2011a). The first release of the all-sky Cold Clump
Catalogue of Planck Objects (C3PO) was presented by the Planck Collaboration
et al. (2011c). This comprehensive catalog profiles 10,342 distinctive cold
sources that stand out against a warmer background. Within the collection of
C3PO clumps, a subset of 915 Early Cold Cores (ECCs) was identified using
specific criteria, namely a signal-to-noise ratio (S/N) greater than 15 and
color temperatures below 14 K. The S/N is based on one of the four matched
multi-frequency filter (MMF) algorithms (Planck Collaboration et al., 2011b;
Melin et al., 2012)

This particular ECC sample is included as part of the Planck Early Release
Compact Source Catalogue (ERCSC), as presented by the Planck Collaboration et
al. (2011b). The Planck Collaboration et al. (2016) released the Planck
Catalog of Galactic cold clumps (PGCCs) with 13188 sources as the full version
of the ECC catalog. These sources, found in various environments, are useful
for investigating the initial conditions of star formation, including dynamic
processes and the evolution of cores in molecular clouds, making use of their
characteristic low temperatures and low levels of activity (Juvela et al.,
2010, 2012; Liu et al., 2012; Tatematsu et al., 2020; Kim et al., 2020; Fehér
et al., 2022).

Plenty of works have been dedicated to the PGCCs using different molecular
spectral lines. The Purple Mountain Observatory (PMO) 14m telescope was used
to observe 12CO, 13CO, and C18O transitions in multiple regions. Specifically,
674 cores in Planck cold clumps of the ECCs were observed (Wu et al., 2012),
along with 71 cores in Taurus, Perseus, and in the California nebula (Meng et
al., 2013), 51 cores in Orion (Liu et al., 2012), 96 cores in the second
quadrant (Zhang et al., 2016), 65 cores in the first Quadrant, and 31 cores in
the Anti-Center direction region (Zhang et al., 2020). Additionally, the $J$ =
1-0 transitions of HCO+ and HCN (Yuan et al., 2016) as well as C2H $N$ = 1-0
and N2H+ $J$ = 1-0, were observed toward the 621 CO selected cores (Liu et
al., 2019). Two large projects were also conducted to study PGCCs
systematically: the Taeduk Radio Astronomy Observatory (TRAO) mapped the $J$ =
1-0 transitions of 12CO and 13CO, while the James Clerk Maxwell Telescope
(JCMT) surveyed the 850 $\mu$m continuum emission of more than 1000 PGCCs
selected from the TRAO sample in the SCUBA-2 Continuum Observations of Pre-
protostellar Evolution (SCOPE) project (Liu et al., 2018). Further studies of
several molecular species toward subsets of the SCOPE objects were made using
the SMT 10m, KVN 21m, Atacama Large Millimeter/submillimeter Array, SMA, NRO
45m and Effelsberg 100m telescopes (Liu et al., 2016; Tatematsu et al., 2017,
2020; Kim et al., 2020; Fehér et al., 2022). Based on these studies above, it
has been discovered that PGCCs demonstrate a state of quiescence and are often
believed to represent the earliest stage of star formation.

To characterize the physical properties of the interior of these objects in a
large, relatively unbiased sample, observations in dense gas tracers are
crucial. Ammonia (NH3) has been established as a reliable dense gas tracer of
molecular clouds (e.g., Ho & Townes 1983; Walmsley & Ungerechts 1983; Danby et
al. 1988). Specifically, NH3 (1,1) and (2,2), both belonging to the para-
species of ammonia, have been proven to be excellent thermometers at $T_{\rm
kin}$ $<$ 40 K (Walmsley & Ungerechts, 1983). Additionally, the critical
densities of NH3 (1,1) and (2,2) are about $10^{3}$ cm-3 (Evans, 1999;
Shirley, 2015), making them a suitable tracer for dense regions and suffering
from minimal freeze-out (Bergin & Tafalla, 2007). Therefore, we present a
pilot study of NH3 (1,1), and (2,2) towards ECCs in different environments,
complemented by archival CO data, and calculate the characteristics of these
cold cores. Fehér et al. (2022) conducted a study of PGCCs using the
Effelsberg 100m radio antenna to observe the NH3 (1,1) and (2,2) lines as a
supplement to SCOPE targets. The selection of regions for observation was
based on two main criteria. Preference was given to regions covered by
Herschel observations and to regions characterized by high column density
clumps (Liu et al., 2018). In contrast to the SCOPE targets, our sample
consists of the whole ECC sample obtained under good observational conditions.

This paper presents a survey of Planck Early Release Cold Cores (ECCs) using
ammonia lines, conducted with the Nanshan 26-m telescope. In Sect. 2, we
provide a detailed description of the sample and observations. In Sect. 3, we
describe the sample properties, and in Sect. 4 we present the results of our
survey. In Sect. 5, a comprehensive discussion of the data is given. Our main
findings are summarized in Sect. 6.

##  2 Samples, observations and data reduction

###  2.1 The sample

To ensure optimal observational conditions, we carefully chose cold cores from
the 915 Planck Early Release Cold Cores (ECCs) dataset (as previously
mentioned in Sec. 1). Specifically, we focused on ECCs with a declination
above $-$30 degrees (to observe with a sufficiently high elevation for the
Nanshan 26-m telescope). As a result of this selection process, our dataset
comprises a total of 672 sources, achieved after the exclusion of sources
situated within the Galactic center region, where Galactic longitudes fell
within $\left|l\right|$ $\leq$ 5 ∘. These exclusions were made due to the
complex interstellar medium environment and intense stellar activity prevalent
in the central region of the Milky Way (Ao et al., 2013; Ginsburg et al.,
2016; Immer et al., 2016). By removing these sources, we aimed to mitigate the
potential biases introduced by the unique environment of the Galactic center
and obtain a more representative sample of dense cores that better reflect
their characteristics in other regions of the galaxy. Subsequently, our
observations were conducted with NH3 lines using the Nanshan 26-m telescope.
The selected sources are listed in Table 8 of Appendix A and shown in the top
panel of Fig. 1.

Previous investigations have explored extensive sets of individual sources
employing ammonia as a probe to examine the dense cores within molecular
clouds (Jijina et al., 1999; Sridharan et al., 2002; Rosolowsky et al., 2008;
Dunham et al., 2011; Wienen et al., 2012; Svoboda et al., 2016). By conducting
a cross-match analysis with these surveys, we identified 27 our sources that
overlap with the sample that has been previously detected in ammonia surveys.
We also conducted a cross-match analysis with Planck cold cores observed in
ammonia (Fehér et al., 2022): Only six of our sources have been previously
observed in ammonia survey specifically targeting Planck cold cores.

Figure 1: Top panel: The distribution of observed cores in the Galactic plane.
The selected cores with and without detections of NH3 emission lines are
denoted by blue and yellow circles, respectively. The red triangles denote
Planck sources not only being part of our sample but having also been
previously detected in ammonia by Fehér et al. (2022). Lower left: Detection
rate distribution of NH3 emission lines. The grey histogram represents the
whole sample of 672 sources where we searched for NH3 lines. The red histogram
represents the number of sources that we detected in the NH3 (1,1) line and
the blue histogram refers to sources we also detected in the NH3 (2,2) line.
The green triangles denote the detection rate for a given 857 $\mu$m flux
density. lower right: Distribution of distances. Here the grey histogram also
refers to the entire sample, while the red histogram visualizes those sources
detected in NH3 (1,1). The blue histogram refers to sources we also detected
in the NH3 (2,2) line.

###  2.2 NH3 observations

We conducted single-point observations of NH3 (1,1), and (2,2) lines from
March 2017 to August 2018 using the Nanshan 26-m telescope. A 22.0-24.2 GHz
dual polarization channel superheterodyne receiver was employed, with the rest
frequency centered at 23.708 GHz to simultaneously observe NH3 (1,1) (23.694
GHz) and (2,2) (23.723 GHz).

To convert antenna temperatures $T^{\ast}_{A}$ into main beam brightness
temperatures $T_{\rm MB}$, a beam efficiency of $\sim$0.59 was adopted (Wu et
al., 2018), with $T_{\rm MB}$ uncertainty about 14%. The telescope is equipped
with a dual-input Digital Filter Bank (DFB) system with 8192 channels. The
typical system temperature is $\sim$50 K ($T^{\ast}_{A}$ scale) at 23.708564
GHz. The FWHM beam of the telescope is 115$\arcsec$ obtained from point-like
continuum calibrators, and the bandwidth is 64 MHz, resulting in a channel
spacing of 0.098 km s-1. All velocities are with respect to the Local Standard
of Rest (LSR). The total integration time for each on-and off-position was 360
s, with some sources requiring multiple observations to increase the signal-
to-noise ratio (S/N). All observations were obtained under good weather
conditions and above an elevation of $30\degr$, resulting in a typical RMS
noise level of $\sim$20 mK.

###  2.3 CO archival data

In this study we also utilized the $J$=1-0 transitions of 12CO, 13CO, and C18O
from the PMO (Liu et al., 2012; Meng et al., 2013; Zhang et al., 2016, 2018,
2020). The 3$\times$3 beam sideband separation Superconduction Spectroscopic
Array Receiver system was used as the front end (Shan et al., 2012). The Half
Power Beam Width (HPBW) is 52 arcsec in the 115 GHz band, with a mean beam
efficiency of about 50% and the pointing and tracking accuracies are better
than 5$\arcsec$. Fast Fourier Transform Spectrometers (FFTSs) were used with
each FFTS providing 16384 channels and a total bandwidth of 1 GHz. The channel
spacing is $\sim$0.16 km s-1 for 12CO, 13CO and C18O. The On-The-Fly (OTF)
observing mode was applied, with the antenna continuously scanning a region of
22$\arcmin$$\times$22$\arcmin$ centered on each clump, while only the central
14$\arcmin$$\times$ 14$\arcmin$ regions were used due to the noisy edges of
the OTF maps.

After matching the spatial resolution of previous PMO mapping observations
(Liu et al., 2012; Meng et al., 2013; Zhang et al., 2016, 2018, 2020) with
that of the ammonia data (2$\arcmin$), we extracted the spectra of the $J$ = 1
- 0 transitions of 12CO, 13CO, and C18O at the 2$\arcmin$ $\times$ 2$\arcmin$
peak position of each source in our sample to construct a data set. In the PMO
observations, 195 sources match our NH3 detected sub-sample (see Sect. 4.1).

###  2.4 Data reduction

The data reduction was performed using the CLASS package of
GILDAS111http://www.iram.fr/IRAMFR/GILDAS/, and the python plot packages
matplotlib (Hunter, 2007). The NH3 data were spectrally smoothed to better
compare and analyze these together with the CO data, resulting in a velocity
resolution of 0.16 km s-1. A feature was considered a genuine detection when
the signal-to-noise ratio (S/N) was above 3. To convert hyperfine blended line
widths to intrinsic line widths in the NH3 inversion spectrum (e.g., Barranco
& Goodman, 1998), we also fitted the averaged spectra using the GILDAS built-
in “NH3 (1,1)” fitting method which can fit all 18 hyperfine components
simultaneously. From this NH3 (1,1) fit we can obtain integrated intensity,
line center velocity, intrinsic line widths of individual hyperfine structure
(hfs) components, and optical depth (see Table 2) of AppendixA.

Main beam brightness temperatures $T_{\rm MB}$ are obtained from GAUSS fit.
Because the hyperfine satellite lines of the NH3 (2,2) transition are mostly
weak, NH3 (2,2) optical depths are not determined. A single Gaussian profile
was fitted to the main group of NH3 (2,2) hyperfine components. A total of
eight NH3 cores were fitted with two velocity components. The spectral line of
each distinguishable component was fitted with Gaussian and ”NH3(1,1)”
fittings. These components are denoted by the labels ”a” and ”b” appended to
the respective source names, as presented in Table 2. We treated these two
velocity components as separate entities (i.e., plotted them as two distinct
cores). However, most of the cores in our observations required only a single
velocity component fit. Physical parameters of the dense gas such as
rotational temperature ($T_{\rm rot}$), kinetic temperature ($T_{\rm kin}$),
and NH3 column density ($N_{\rm NH_{3}}$) were derived (see Sects. 3.2 and
3.3). Fig. 2 provides examples of reduced and calibrated spectra of NH3 (1,1),
and (2,2) inversion lines. Examples for typical ammonia spectrum in different
S/N ratios are shown in Fig.8 of Appendix B

For the 12CO, 13CO and C18O spectra, peak main-beam brightness temperature,
Local Standard of Rest (LSR) velocities, and line widths have been obtained by
fitting Gaussian profiles (see Table 1 of Appendix C). The excitation
temperature for CO ($T_{\rm ex(CO)}$), 13CO opacity ($\tau_{\rm{}^{13}CO}$),
C18O opacity ($\tau_{\rm C^{18}O}$), 13CO column density ($N_{\rm{}^{13}CO}$),
C18O column density ($N_{\rm C^{18}O}$), and hydrogen column density
($N\rm_{H_{2}}$) were also calculated (see Table 2 of Appendix C).

Figure 2: Example for a typical ammonia spectrum. Shown are NH3 inversion
lines from G092.26+03.8. The solid black line represents the observed NH3
(1,1) spectrum and the solid red line indicates the corresponding NH3 (2,2)
profile.

##  3 Sample properties

###  3.1 Distances

The distances of our sources were obtained from the literature (Wu et al.,
2012; Planck Collaboration et al., 2016). For sources whose distances were
unavailable in the literature, we employed the distance with the highest
probability from the parallax-based distance estimator of the Bar and Spiral
Structure Legacy Survey (Reid et al., 2016). The histogram of the kinematic
distances is presented in the lower right panel of Fig. 1. It can be deduced
from the distance distribution that the NH3(1,1) detection rate is
significantly increased beyond 0.6 kpc, and the NH3(2,2) detection rate does
not exhibit a clear correlation with distance. The distances of all sources
range from 0.11 to 4.09 kpc, with a mean of 0.98 kpc and a median of 0.94 kpc.
56% of the sources have distances within 0.5 and 1.5 kpc.

###  3.2 Kinetic temperature

With the measured data, the rotational temperature ($T_{\rm rot}$), kinetic
temperature ($T_{\rm kin}$), NH3 column density ($N_{\rm NH_{3}}$), thermal
velocity dispersion $\sigma_{\rm Therm}$, non-thermal velocity dispersion
$\sigma_{\rm NT}$, thermal-to-non-thermal pressure ratio $R_{\rm p}$, thermal
sound speed $c_{\rm s}$ and Mach number ($\mathcal{M}$) of cores can be
calculated.

Once the optical depth is determined by the ”NH3(1,1)” fitting as described in
Sect 2.4, we can calculate the excitation temperature of the NH3 (1,1)
inversion transition through the relation (Ho & Townes, 1983),

$\displaystyle T_{\mbox{\tiny ex}}=\frac{T_{\rm MB(1,1)}}{\left(1-\rm
exp(-\tau)\right)}\ \ +2.7\,{\rm K,}$ (1)

where $T_{\rm MB}$ and $\tau$ represent the temperature and the optical depth
of the (1,1) line derived using the GILDAS built-in ‘GAUSS’ and ‘NH3 (1,1)’
fitting methods. A histogram of the optical depths of the (1,1) lines for our
positions with NH3 (1,1) signal-to-noise ratios $>$ 3$\sigma$ is summarized in
Fig. 3b.

Since the relative populations of the K = 1 and 2 ladders of NH3 are not
directly connected radiatively, they are highly sensitive to collisional
processes. This allows us to use them as a thermometer of the gas kinetic
temperature. The method described in Ho & Townes (1983), has been used to
obtain the rotation temperature.

The rotation temperature is given by the expression

$\displaystyle T_{\mbox{\tiny
rot}}=\frac{-41.5}{\ln\left(\frac{-0.282}{\tau}\ln\left(1-\frac{T_{\rm
MB}(2,2)}{T_{\rm MB}(1,1)}\left(1-\rm exp(-\tau)\right)\right)\right)}\ \ {\rm
K,}$ (2)

where $T_{\rm MB}$ (2,2) is the main beam brightness temperatures of the (2,2)
line derived using the GILDAS built-in ‘GAUSS’ fitting method.

We estimated the kinetic temperature $T_{\rm kin}$ using the approximation of
Tafalla et al. (2004) :

$\displaystyle T_{\mbox{\tiny kin}}=\frac{T_{\mbox{\tiny
rot}}(1,2)}{1-\frac{T_{\mbox{\tiny rot}}(1,2)}{41.5}\ln\left(1+1.1\,{\rm
exp}\left(\frac{-16}{T_{\mbox{\tiny rot}}(1,2)}\right)\right)}\ \ {\rm K,}$
(3)

where the energy gap between the (1,1) and (2,2) states is $\Delta E_{\rm
12}$= 41.5 K. This approximation has been derived with Monte Carlo models and
provides an accuracy of 5% in the range between 5 and 20 K. Most of our
sources can be found in this interval.

###  3.3 NH3 column density

Computing the ammonia column density requires the optical depth and line width
of the (1, 1) inversion transition along with the rotational temperature,
which is obtained from Eqs. (2). As the optical depth and the rotational
temperature depend only on line ratios, the resulting column density is a
source-averaged quantity.

Realistically assuming that for our cold sources, the bulk of the ammonia
populations resides in the metastable (J = K), (J,K) = (0,0) to (3,3) levels,
the total NH3 column densities can be calculated from NH3 (1,1) following
(Wienen et al., 2012),

$\displaystyle N_{\rm{NH_{3}}}\approx N(1,1)\Bigg{(}\frac{1}{3}\,{\rm
exp}\left(\frac{23.1}{T_{\mbox{\tiny rot}}(1,2)}\right)+1+\frac{5}{3}\,{\rm
exp}\left(-\frac{41.2}{T_{\mbox{\tiny rot}}(1,2)}\right)$ (4)
$\displaystyle+\frac{14}{3}\,{\rm exp}\left(-\frac{99.4}{T_{\mbox{\tiny
rot}}(1,2)}\right)\Bigg{)}\ \ {\rm cm^{-2}}$

and

$\displaystyle N(1,1)=6.60\times 10^{4}\,\Delta v\,\tau\,\frac{\,T_{\rm
rot}}{\,\nu}\,\ \ {\rm cm^{-2},}$ (5)

where $N$(1,1) is the column density of the NH3 (1,1) transition, the FWHM
line width $\Delta v$ is in km s-1, the line frequency $\nu$ is in GHz, and
the rotational temperature $T_{\rm rot}$ is in Kelvin.

###  3.4 Velocity dispersions, sound speed, and gas pressure ratio

The observed line widths provide a measure of the internal motions within each
Planck source. Here we computed non-thermal velocity dispersion ($\sigma_{\rm
NT}$), thermal velocity dispersion ($\sigma_{\rm TH}$), and sound speed
($c_{\rm s}$) following Levshakov et al. (2014), Tang et al. (2017, 2018a,
2018b, 2021).

$\displaystyle\sigma_{\rm NT}=\sqrt{\sigma_{\rm v}^{2}-\sigma_{\rm TH}^{2}}\ \
\,\rm km\,s^{-1},$ (6)

where $\sigma_{\rm v}$ = $\Delta v(1,1)$/8ln(2), and $\sigma_{\rm TH}$ =
($k_{\rm B}$$T_{\rm kin}$/17$m_{\rm H}$)1/2. $m_{\rm H}$ is the mass of a
single hydrogen atom, and $k_{\rm B}$ is the Boltzmann constant.

The thermal sound speed can be calculated with

$\displaystyle c_{\rm s}=\sqrt{\frac{k_{\rm B}T_{\rm kin}}{\mu m_{\rm H}}}\ \
\,\rm km\,s^{-1}.$ (7)

where $\mu$ = 2.37 is the mean molecular weight for molecular clouds (Dewangan
et al., 2016).

We also calculated the thermal-to-nonthermal pressure ratio ($R_{\rm
P}$=$\sigma_{\rm TH}^{2}$/$\sigma_{\rm NT}^{2}$; Lada et al. 2003) and Mach
number (given as $\mathcal{M}$=$\sigma_{\rm NT}$/$c_{\rm s}$).

The statistical properties of the sample are summarised in Table 1 including
the mean values and the medians of the derived quantities, as well as the
minimal and maximal values. The derived values of $T_{\rm ex}$, $T_{\rm rot}$,
$T_{\rm kin}$, $N_{\rm tot}$, $\sigma_{\rm TH}$, $\sigma_{\rm NT}$, $c_{\rm
s}$, $\mathcal{M}$ and $R_{\rm P}$ for individual Planck sources are listed
separately in Table 2 of Appendix A.

##  4 Results

###  4.1 NH3 detection rates

Out of the 672 Planck Early Release Cold Cores (ECCs) that were surveyed with
the Nanshan 26-m telescope for NH3, 249 sources (37%) were detected with NH3
(1,1) emission lines. Of these, 187 sources reveal NH3 (1,1) hyperfine
structure, while 76 sources (11%) also show NH3 (2,2) emission lines. Observed
parameters and calculated parameters are given in Tables 2-3 of Appendix A.

The highest angular resolution of the Planck survey is 5 arcmin, at a
frequency of 857 GHz. We plotted the distribution of observed sources and the
NH3 lines detected in this work as well as the detection rate of the NH3 (1,1)
line as a function of the 857 GHz aperture flux density S857 of the Planck
Sources in the lower left panel of Fig. 1. We observe that sources with S857
larger than 3 Jy have a 100% detection rate. Furthermore, the detection rate
of the NH3 (1,1) line increases from 0 to 100 percent as the flux density S857
rises from 1.5 to 4.6 Jy. However, it should be noted that while the detection
rates of the NH3 (1,1) line are 100 percent in the last bins, the number of
sources within these bins is limited, with only 8, 6, 4, 3, 2, and 2 sources
in total.

In the lower right panel of Fig. 1, we observed an unexpectedly low detection
rate of ammonia in regions with small kinematic distances. To understand this
phenomenon, we performed a column density analysis of sources situated within
a distance of less than 0.45 kpc. Utilizing hydrogen column density data from
the Planck Collaboration et al. (2011c), we found a difference in column
densities between sources where ammonia was detected and those where it was
not, within this near distance (less than 0.45 kpc). Specifically, sources
with detected ammonia exhibited an average hydrogen column density of 4.32
$\times$ 1021 cm-2, while those without ammonia detection had an average
hydrogen column density of 1.99 $\times$ 1021 cm-2. Moreover, it’s important
to consider that sources in these nearby regions may have relatively extended
spatial distributions. This spatial extension implies that during our
observations of ammonia point sources, we may inadvertently miss the real
peaks of the Planck cold cores.

The top panel of Fig. 1 presents the spatial distribution of the detected
sources, which are mainly located in local star-forming regions such as Taurus
and Orion and the galactic plane. This trend is shared by all of the ECCs and
CO-selected cores in the sample (Wu et al., 2012; Yuan et al., 2016). As
mentioned in Sect.2.1, we cross-matched our sample with sources observed by
Fehér et al. (2022), owing to distinct criteria detailed in Section. 1.
Consequently, there is a disparity in the distribution of sources across the
galaxy between the two samples (see also Sect.2.1).

###  4.2 Properties of the NH3 emitting gas

Figure 3 shows the statistics of observed and physical properties for the NH3
detected sample. The top left panel shows the intrinsic line width of an
individual hfs component, $\Delta V\,(\rm NH_{3}\,(1,1))$, which ranges
approximately from 0.36 to 2.36 km s-1, with an average of 0.89 $\pm$ 0.29 km
s-1, which suggests that the non-thermal turbulence of these sources is
significant (errors correspond to the standard deviations of the mean
throughout this article). The top middle panel of Figure 3 shows the sample
optical depths, which range from 0.1 to 5.3 with an average value of 1.6,
implying that NH3 (1,1) lines in most of the detected PGCC cores are optically
thick (see Table 1).

The top right panel shows the excitation temperature, $T_{\rm ex}$, which
ranges approximately from 2.8 to 5.4 K, with a mean and median of 3.2 and 3.1
K, respectively. The bottom left panel of Figure 3 shows the derived
rotational temperature, which exhibits a range of 8.6 to 17.6 K, with an
average value of 11.4 $\pm$ 2.2 K. The median value of the rotational
temperature is 10.7 K, with a typical value of approximately 10 K. Remarkably,
83% of the sources exhibit values lying between 8 and 14 K. The NH3 kinetic
temperature distribution, illustrated in the bottom middle panel of Fig. 3,
ranges from 8.9 to 20.7 K, with an average of 12.3 $\pm$ 2.9 K and a median
value of 11.4 K. The total NH3 column density ranges from 0.36 to 6.07
$\times$ 1015 cm-2, with an average of 2.04 $\times$ 1015 cm-2. The total
column densities of NH3 are presented as a histogram in the bottom right panel
of Fig. 3, exhibiting a peak around 1015.4 cm-2 in our sample.

The thermal velocity dispersion of NH3 (1,1) lines detected at a $>$3$\sigma$
level shows a range of 0.07 to 0.10 km s-1, with an average of 0.08 $\pm$ 0.01
km s-1 and a median of 0.07 km s-1. The non-thermal velocity dispersion of NH3
(1,1) for cores ranges from 0.30 to 1.09 km s-1, with an average of 0.55 $\pm$
0.18 km s-1 and a median of 0.49 km s-1. The thermal linewidth is
significantly smaller than the non-thermal linewidth, which suggests that non-
thermal motions dominate the dense gas in the PGCCs. The sound speed of the
gas ranges from 0.18 to 0.27 km s-1, with an average of 0.21 $\pm$ 0.02 km s-1
and median of 0.20 km s-1. The thermal to non-thermal pressure ratio in the
gas traced by NH3 (1,1) ranges from 0.01 to 0.06, with an average of 0.02
$\pm$ 0.01, and a median of 0.02. The Mach number ranges from 1.6 to 5.0 with
an average of 2.7 $\pm$ 0.8, and a median of 2.5.

Figure 3: Histograms of physical parameters derived from NH3. (a) Intrinsic
line widths of individual NH3 (1,1) hyperfine structure components with
hyperfine structure and a peak line flux threshold of 3$\sigma$; (b) peak
optical depths of the main group of hf components $\tau_{m}$ (1,1) for those
positions with NH3 (1,1) hyperfine structure and S/N ¿ 3 (these line widths
and peak optical depths are derived from the GILDAS built-in “NH3 (1,1)”
fitting method); (c) excitation temperature $T_{\rm ex}$; (d) rotational
temperature $T_{\rm rot}$; (e) kinetic temperature $T_{\rm kin}$; (f) NH3
column densities. Table 1: NH3 parameters of our sample of PGCC cores

Parameter | Range | Mean | Median
---|---|---|---
$\Delta$$V$(NH3(1,1)) [km s-1] | 0.36–2.36 |  0.89 $\pm$ 0.29 | 0.83
$\tau$ | 0.1–5.3 |  1.6 $\pm$ 1.1 | 1.4
$T_{\rm ex}$ [K] | 2.8–5.4 |  3.2 $\pm$ 0.4 | 3.1
$T_{\rm rot}$ [K] | 8.6–17.6 |  11.4 $\pm$ 2.2 | 10.7
$T_{\rm kin}$ [K] | 8.9–20.7 |  12.3 $\pm$ 2.9 | 11.4
N$\rm{}_{NH_{3}}$ [$10^{15}$ cm-2] | 0.36–6.07 |  2.04 $\pm$ 1.2 | 1.83
$\sigma_{\rm TH}$ [km s-1] | 0.07–0.10 |  0.08 $\pm$ 0.01 | 0.07
$\sigma_{\rm NT}$ [km s-1] | 0.30–1.09 |  0.55 $\pm$ 0.18 | 0.49
$c_{\rm s}$ [ km s-1] | 0.18–0.27 |  0.21 $\pm$ 0.02 | 0.20
$\mathcal{M}$ | 1.6–5.0 |  2.7 $\pm$ 0.8 | 2.5
$R_{\rm P}$ | 0.01–0.06 |  0.02 $\pm$ 0.01 | 0.02
$N\rm_{H_{2}}$(13CO) [$10^{22}$ cm-2] | 0.07–2.88 |  0.74 $\pm$ 0.42 | 0.63
$\chi_{\rm\tiny NH_{3}}$ [$10^{-7}$] | 0.3-9.7 |  2.7 $\pm$ 2.2 | 1.9
$T_{\rm dust}$ [K] | 8.6-13.9 |  11.5 $\pm$ 1.07 | 11.6
222The dust temperature ($T_{\rm dust}$) values presented in this table
correspond to a cross-matching of NH3-detected 249 sources with the dust
temperature data obtained from Planck Collaboration et al. (2016).

###  4.3 Thermal and non-thermal motions

The clumps are supported against their gravity by both thermal and non-thermal
motions (Cho & Lazarian, 2003). The former is a manifestation of the kinetic
temperature within a clump, while the latter originates from star-forming
activities such as infall motions and outflows that can broaden the non-
thermal velocity dispersion. However, the quiescent nature of PGCCs suggests
that these motions are not particularly vigorous. Therefore, turbulent motion
is the primary contributor to the non-thermal motion of these cores. Ammonia
is one of the few dense gas tracers that allows for the simultaneous
computation of line width and kinetic temperature, as well as thermal and non-
thermal line widths. Our data are particularly well-suited for investigating
these two types of motion.

When turbulent energy is converted into heat, a correlation is expected to
exist between the kinetic temperature and linewidth (Guesten et al., 1985;
Molinari et al., 1996; Ao et al., 2013; Ginsburg et al., 2016; Immer et al.,
2016; Tang et al., 2017, 2018a, 2018b, 2021). In this study, we investigate
the existence of a correlation between temperature and turbulence in PGCCs
traced by the dense gas. To achieve this, we utilized the NH3 (1,1) and (2,2)
line ratio derived kinetic temperature and NH3 non-thermal velocity dispersion
($\sigma_{\rm NT}$) as a decent approximation proxy for turbulence. The non-
thermal velocity dispersions versus the kinetic temperature for the sources
are shown in Fig. 4, with the dotted line representing the thermal sound
speed. Our results indicate a weak correlation between non-thermal velocity
dispersion and kinetic temperature, suggesting that turbulent heating may
contribute to gas temperature in these cold cores.

Figure 4: Left: Non-thermal velocity dispersion $\sigma_{\rm NT}$ vs. gas
kinetic temperature derived from NH3 (1,1). The black dotted line at the
bottom represents the thermal sound speed (left).

###  4.4 Associated stellar objects

Table 2: Numbers of associated stellar objects

Types of matched cores |  Matching criteria | Number of associated stellar objects | Number of cores containing stellar objects
---|---|---|---
|  |  with IR objects |  with YSOs |  with YSO candidates |  contain IR objects |  contain YSOs |  contain YSO candidates
672 observed cores |  $\sim$2$\arcmin$ |  131 ($\sim$19%) |  57 ($\sim$8%) |  58 ($\sim$8%) |  112 ($\sim$17%) |  29 ($\sim$4%) |  23 ($\sim$3%)
249 NH3 detected cores |  $\sim$2$\arcmin$ |  66 ($\sim$27%) |  48 ($\sim$19%) |  52 ($\sim$21%) |  53 ($\sim$21%) |  23 ($\sim$9%) |  17 ($\sim$7%)

333Matching criteria refer to associated objects within the $\sim$2$\arcmin$
ammonia beam size.

Table 3: Matching results by types of stellar objects

Types of matched cores |  Matching criteria | Single-source matches | Multi-source matches
---|---|---|---
|  |  IR |  YSO |  YSO candidate |  YSOs & YSO candidate |  IR & YSOs |  IR & YSO candidate |  IR&YSOs&YSO candidate
672 observed cores |  $\sim$2$\arcmin$ |  102 ($\sim$15%) |  18 ($\sim$3%) |  16 ($\sim$2%) |  4 ($\sim$1%) |  7 ($\sim$1%) |  3 ($\sim$1%) |
249 NH3 detected cores |  $\sim$2$\arcmin$ |  45 ($\sim$18%) |  13 ($\sim$5%) |  9 ($\sim$4%) |  5 ($\sim$2%) |  5 ($\sim$2%) |  3 ($\sim$1%) |

444”Single-source matches” are sources that are exclusively associated with
either an IR source or with one specific type of stellar object. ”Multi-source
matches” refer to sources that are associated with multiple types.

The associated objects of the cores are crucial for our understanding of their
environment and evolutionary stages. Therefore, we investigated the objects
associated with the cores, including infrared (IR) objects, young stellar
objects (YSOs), and young stellar object candidates (YSO candidates). We
obtained the stellar objects from the Simbad website. Statistical properties
are given in Tables 2-3. YSOs are distinguished by their manifestation of not
only infrared excess but also additional spectral features, providing evidence
of active star formation processes (Allen et al., 2004; Gutermuth et al.,
2004). Conversely, YSO candidates represent potential YSOs necessitating
further scrutiny and validation.

In our study, we adopted the ammonia beam size ($\sim$2$\arcmin$) as a
matching criterion. Among the 672 cores observed, our analysis revealed the
presence of 131 ($\sim$19%) IR objects, 57 ($\sim$ 8%) YSOs and 58 ($\sim$ 8%)
YSO candidates. The rare association may indicate low star formation activity
(Lada et al., 2009; Lombardi et al., 2010). However, it cannot be entirely
excluded that the associated objects originate from different gas clumps
located along the line-of-sight (Wu et al., 2006). It is important to note
that certain cores in our sample may encompass multiple IR sources, as well as
multiple YSOs or YSO candidates. Notably, the majority of these IR objects
correspond to single-point sources detected by the Infrared Astronomical
Satellite (IRAS). Overall, our findings indicate that 149 ($\sim$22%) cores
have different types of associated objects within a beam size of
$\sim$2$\arcmin$. Additionally, we find that 112 ($\sim$17%) cores contain at
least one IR object, 29 ($\sim$4%) cores have YSOs, and 23 ($\sim$3%) cores
contain YSO candidates. Among these, 102 sources only associate with IR
objects, 18 cores only associate with YSOs and 16 cores only associate with
YSO candidates. 4 cores are associated with both YSOs and YSO candidates, 7
cores with both YSO and IR objects, 3 cores with both IR objects and YSO
candidates.

Considering the 249 cores where NH3 (1,1) emission was detected, we find 66
($\sim$27%) IR objects, 48 ($\sim$19%)YSOs, and 52 ($\sim$21%) YSO candidate
sources associated with these cores using the aforementioned $\sim$2$\arcmin$
criterion. In general, 80 ($\sim$32%) cores have different types of associated
objects. Additionally, we find that 53 ($\sim$21%) cores contain at least one
IR object, 23 ($\sim$9%) cores host YSOs, and 17 ($\sim$7%) cores harbor YSO
candidates. 45 sources only associate with IR objects, 13 cores only associate
with YSOs and 9 cores only associate with YSO candidates. 5 cores are
associated with both YSOs and YSO candidates, 5 cores with both YSOs and IR
objects, and 3 cores with both IR objects and YSO candidates.

Based on preliminary statistical analysis, the proportion of sources with NH3
emission matching IR sources and stellar objects is higher than the overall
proportion of the total sample matching IR sources and YSOs. The ammonia
detection rate of sources matching young stellar objects or their candidates
in the 672 observed cores is 66%, while the ammonia detection rate of sources
matching IR objects is 45%. The ammonia detection rate is higher in sources
with matching stellar objects. Not all sources with matched stellar objects
and IR objects have been detected in NH3 (1,1). There can be several reasons
for this. Firstly, distance plays a significant role. If the YSOs or IR
objects are located at a large distance, the faint emission signal from
ammonia may be too weak to be detected. Secondly, the spatial resolution of
the observing instrument can also be a factor. Other factors include line-of-
sight effects and environmental conditions, where the physical environment
surrounding the YSOs may influence the presence of ammonia molecules. The
inescapable issue at hand is that our matching could potentially be limited to
line-of-sight coincidence, lacking the necessary distance information for
spatial alignment.

###  4.5 NH3 abundances

The column densities of ammonia in our sample range from 0.36 $\sim$ 6.07 ×
1015 cm-2, with a mean value of approximately 2.04 $\times$ 1015 cm-2 and a
median value of about 1.83 × 1015 cm-2 (Table 1). We utilized 13CO to derive
the H2 column densities as described in Appendix C. The H2 column densities
$N\rm_{H_{2}}$(13CO) range from 7.0 $\times$ 1020 to 2.88 $\times$ 1022 cm-2,
with an average of 7.4 $\times$ 1021 cm-2. The column densities of NH3 denoted
as $N_{\rm NH_{3}}$, were compared with the column densities of H2, denoted as
$N_{\rm H_{2}}$, derived from 13CO to determine the fractional abundance of
ammonia in each source. The fractional abundance, $\chi_{\rm NH_{3}}$, is
defined as the ratio of $N_{\rm NH_{3}}$ to $N_{\rm H_{2}}$(13CO). The ammonia
abundances in the sources range from 0.3 to 9.7 $\times$ 10-7, with an average
of 2.7 $\times$ 10-7.

Fig. 5 illustrates the column densities of NH3 and its abundances, $\chi_{\rm
NH_{3}}$, as a function of H2 column density and kinetic temperature $T_{\rm
kin}$. It is observed that the NH3 column densities and fractional abundances
are inversely proportional to the kinetic temperatures. Moreover, there is a
trend of decreasing fractional NH3 abundance, $\chi_{\rm NH_{3}}$, with
increasing $N_{\rm H_{2}}$.

Figure 5:  (a,b) Column densities and fractional abundances $N_{\rm
NH_{3}}$/$N_{\rm H_{2}}$(13CO) versus kinetic temperature $T_{\rm kin}$ and
(c,d) vs. the column density of H2 derived from 13CO ($N_{\rm H_{2}}$(13CO)).

##  5 Discussion

###  5.1 Column densities and abundances

The ammonia column densities in our results are consistent with the findings
of PGCC selected sources from SCUBA-2, whose column densities range from 0.4
to 1.5 $\times$ 1016 cm-2, with a mean value of approximately 1.3 $\times$
1015 cm-2 (Fehér et al., 2022). The ammonia column densities we obtained in
our observations are also consistent with those reported in most star-forming
environments (Dunham et al., 2011; Wienen et al., 2012; Cyganowski et al.,
2013).

The average value of $N\rm_{H_{2}}$(13CO), 7.4 $\times$ 1021 cm-2, is
consistent with the results obtained from the Planck cold cores observed by
PMO (Wu et al., 2012; Meng et al., 2013; Zhang et al., 2016). In the SCOPE-2
follow-up observations, the H2 column densities of 97 Planck cold cores range
from 1022 to 1024 cm-2 (Fehér et al., 2022), which are higher than the column
densities obtained in our work. This may be attributed to the fact that the
SCOPE-2 survey does not include sources with column densities $N_{\rm H_{2}}$
¡ 2 $\times$1021 cm-2 (Eden et al., 2019).

Previous observations of NH3 fractional abundance in high-mass star-forming
clumps suggest a median value of 2.7 $\times$ 10-8 (Urquhart et al., 2015).
Additionally, Dunham et al. (2011), Wienen et al. (2012), and Merello et al.
(2019) obtained average abundance values of 1.2 $\times$ 10-7, 4.6 $\times$
10-8, and 1.5 $\times$ 10-8, respectively, in clumps of the Bolocam Galactic
Plane Survey (BGPS), the APEX Telescope Large Area Survey of the GALaxy
(ATLASGAL), and the Hi-GAL survey. Furthermore, fractional abundances of 4
$\times$ 10-8, 8 $\times$ 10-7 and 1 $\times$ 10-8 were derived for infrared
dark clouds by Pillai et al. (2006), Ragan et al. (2011), and Chira et al.
(2013), respectively. The average NH3 abundance derived from PGCCs in this
study is one order of magnitude greater than that of MSF regions and IRDCs and
exhibits a narrow distribution similar to that of IRDCs. The elevated NH3
fractional abundance in PGCCs relative to other star-forming regions is likely
attributable to the earlier phase of cloud evolution of PGCCs compared to
Massive Star-forming (MSF) regions or even IRDCs. Ammonia is more abundant in
cold, dense cores than most other molecules (Bergin & Langer, 1997). The
average NH3 abundances obtained in our study are consistent with those
predicted for low-mass pre-protostellar cores by chemical models (Bergin &
Langer, 1997).

The NH3 column densities and fractional abundances are inversely proportional
to the kinetic temperatures (see in Fig. 5 a, b), which is consistent with the
findings of previous studies on infrared dark clouds (Chira et al., 2013). The
NH3 column densities in all cores tend to increase with $N_{\rm H_{2}}$, as
shown in Fig. 5 (c), following the general trend that the NH3 emission follows
the dust continuum emission in the cores. This is in agreement with the
results reported by Ragan et al. (2011), who found that IRDCs with no evidence
of embedded star formation activity exhibit a strong correlation between
ammonia and H2 column density. A similar trend is observed in the cold cores
in our observation.

Table 4: Fundamental information on different NH3 samples Sources | Reference | Type |  NH3 source number
---|---|---|---
BGPS | Dunham et al. (2011) | High-mass star-forming clumps, | 456
|  | at various evolutionary stages |
ATLASGAL | Wienen et al. (2012) | High-mass star-forming clumps, | 752
|  | at various evolutionary stages |
UC Hii Cand | Molinari et al. (1996) |  Percursors of ultraconpact Hii regions | 163
High contrast IRDCs | Chira et al. (2013) | Capable of harbouring high-mass star-forming regions | 109
|  | Early evolutionary stages |
High IR extinction clouds | Rygl et al. (2010) | Cold and compact high extinction clouds | 54
EGOs | Cyganowski et al. (2013) | Northern extended green objects (EGOs) | 94
Ophiuchus | Friesen et al. (2009) | Studies of isolated starless clumps | 21
Perseus | Schnee et al. (2009) | Starless cores | 49
Cepheus & Orion L1630 / L1641 | Harju et al. (1993, 1991) | Warm, massive clumps | 51

###  5.2 Comparative analysis of thermal and non-thermal motions

To obtain comprehensive statistics on PGCCs, we conducted a comparative
analysis of the non-thermal velocity dispersions and kinetic temperatures.
Studies encompass a diverse range of samples, including high-mass star-forming
clumps at various evolutionary stages from ATLASGAL and BGPS surveys (Dunham
et al., 2011; Wienen et al., 2012), high contrast Infrared Dark Clouds (IRDCs)
(Chira et al., 2013), as well as starless cores in the Perseus region
(Rosolowsky et al., 2008; Schnee et al., 2009), and dense cores in the
Ophiuchus, Cepheus, and Orion L1630 and L1641 molecular clouds (Harju et al.,
1991, 1993; Friesen et al., 2009). This comprehensive approach allows us to
gain valuable insights into the physical properties of these objects and their
evolutionary characteristics. In Table 4, we have compiled a list containing
the fundamental information of the sources used for comparison in this study.

As seen in Fig. 4, unlike high-mass star-forming clumps and dense cores in
star-forming regions (Dunham et al., 2011; Wienen et al., 2012), the
relationship between non-thermal velocity dispersion and kinetic temperatures
in PGCCs is much weaker, which is similar to or even less than for infrared
dark clouds (Chira et al., 2013). Additionally, the distribution of non-
thermal velocity dispersion and kinetic temperatures of Planck cold cores is
narrower when compared to the observations of the other samples. Spearman’s
rank correlation coefficients ($\rho$) for non-thermal velocity dispersion
versus kinetic temperatures in different samples and the resultant
$\rho$-values are presented in Table 5 of Appendix A. The table presents the
obtained $\rho$-values along with their corresponding P-values. The analysis
of this table reveals varying degrees of correlation between non-thermal
velocity dispersion and kinetic temperature across different samples.
Particularly, a conspicuous positive correlation is discernible in the
ATLASGAL, BGPS, Ophiuchus, Cepheus, and Orion L1630/L1641 samples, underscored
by small P-values. However, in the High-contrast IRDCs, the correlation is
relatively weak, with a Spearman correlation coefficient of 0.07 and a p-value
of 0.45, suggesting a weak and non-significant linear relationship between
these two variables. The Perseus sample also manifests a relatively weak
correlation, featuring a Spearman correlation coefficient of 0.2 and a p-value
of 0.16, implying a modest positive correlation trend that lacks statistical
significance. In contrast, our Planck cold cores sample displays a pronounced
positive correlation between non-thermal velocity dispersion and kinetic
temperature. With a Spearman correlation coefficient of 0.33 and a p-value of
4.00 $\times$ $10^{-3}$.

Furthermore, gas pressure ratios derived from our results closely align with
those obtained by Urquhart et al. (2015), who conducted a study on 66 massive
young stellar objects and compact Hii regions from the RMS survey (Red MSX
Source survey, Lumsden et al., 2013). Urquhart et al. (2015) obtained gas
pressure ratios ($R_{\rm p}$) of 0.01-0.02 for both massive star-forming and
quiescent clumps. In contrast, Lada et al. (2003) reported significantly
higher values of $R_{\rm p}$ = 4-5 for low-mass star-forming cores, such as
Barnard 68, based on C18O and C34S data. Our sample, which includes non-
thermal movements that significantly contribute to the kinetic energy balance,
more closely aligns with samples of massive clumps compared to others.

###  5.3 Correlation between NH3 and other molecular species

Figure 6: Distributions between differences of line-center velocities (a, b)
and line widths (c, d) of 13CO, C18O and NH3. The average sound speed is
indicated as dotted lines in (a, b).

In their survey of 674 Planck cold clumps, Wu et al. (2012) discovered that
the velocities of transitions from CO and its isotopologues were highly
consistent with one another. We plot the absolute value of the difference
between $J$=1-0 transitions of 13CO and C18O and the NH3(1,1) line-center
velocities from Gaussian fits in Fig. 6 (a, b). When multiple 13CO velocities
were detected along the line of sight, we assumed that the velocity component
closest to the NH3 velocity is associated with the core (Kirk et al., 2007).

The minute discrepancy in centroid velocity between NH3 and 13CO ($\sim$0.17
km s-1), and between NH3 and C18O ($\sim$0.18 km s-1), can be compared to the
distinction in line-center velocities of N2H+ and C18O in low-mass, starless,
and protostellar cores Walsh et al. (2004); Kirk et al. (2007). Fig. 6 (a, b)
illustrate that the majority of cores (64% for the difference between 13CO
NH3(1,1) line-center velocities and 70% for the difference between C18O and
NH3(1,1) line-center velocities) exhibit differences smaller than the sound
speed (dotted lines), and the remaining cores have differences that are not
much larger. This phenomenon was investigated in the Perseus molecular cloud
by Kirk et al. (2007), who found that the relative motions of dense N2H+ cores
and their envelopes (measured in C18O) generally exhibit velocity differences
lower than thermal motions in the majority of cases ($\sim$ 90%). This is also
consistent with the findings of Walsh et al. (2004), who measured a core-to-
envelope velocity difference that exceeded the sound speed in only 3% of their
sample. These samples consisted of isolated low-mass cores. Therefore, these
comparisons suggest that the velocity differences between low and high-density
tracers in the Planck cores observed by NH3 are similar to those in low-mass,
starless, or prestellar cores. In the survey of CO-selected cores in Planck
cold clumps, Yuan et al. (2016) found that the central velocity differences of
transitions from 13CO, HCO+ and HCN are strikingly consistent with each other.
The central velocities (obtained by fitting Gaussian profiles) between 13CO
and HCO+ ($V_{{}^{13}\rm CO}$ \- $V_{\rm HCO^{+}}$ ), 13CO and HCN
($V_{{}^{13}\rm CO}$ \- $V_{\rm HCN}$), HCO+ and HCN ($V_{\rm HCO^{+}}$ \-
$V_{\rm HCN}$) in their study have mean values of 0.006, 0.05, and 0.002 km
s-1, respectively. The smaller deviations from Yuan et al. (2016) may indicate
that 13CO, HCO+, and HCN are better coupled with each other. It is important
to note that the channel spacing employed in their study was 0.21 km s-1. In
this work, the mean value of the velocity difference among the central
velocities of 13CO and NH3 is 0.17 km s-1, with channel spacing of 0.16 km
s-1. It is worth noting that the relatively low-velocity resolution might
impact the interpretation of the small velocity differences observed in both
cases, To address this, future observations with higher resolution would be
beneficial for a more accurate comparison. By improving the velocity
resolution, we can measure and compare the central velocity differences
between different molecular lines more accurately, providing deeper insights.
Such observations would help further validate and explain the consistency
among these molecular transitions and enhance our understanding of the
physical processes occurring within Planck cold clumps. Therefore, future
high-resolution observations will be would help to further validate this
matter.

The mean intrinsic line width of the NH3 (1,1) lines obtained from GAUSS fit
is approximately 0.89 km s-1, which is comparable to that of C18O $J$=1-0 (0.8
km s-1) in Wu et al. (2012), C2H $N$= 1-0 (1.0 km s-1) reported in Liu et al.
(2019), and HCN $J$ = 1-0 (1.06 km s-1) in Yuan et al. (2016). The differences
in line widths among different molecular tracers may result from turbulence at
different scales. Fig. 6 (c, d) show the distributions of the differences in
line widths between 13CO and C18O with NH3. The mean widths of NH3 and 13CO
are nearly identical, with an average difference of $\sim$0.14 km s-1. In
contrast to high-mass star-forming clumps, where the average difference
between NH3 and 13CO is 4.3 km s-1 (Wienen et al., 2012), the intrinsic line
widths of NH3, 13CO and C18O are approximately equal in our sample. This
finding is consistent with the notion that these PGCCs are quiescent, as the
majority of them appear to be transitioning from clouds to dense cores (Wu et
al., 2012).

###  5.4 A comparison with different star formation samples

To investigate the physical conditions and assess the potential for star
formation within the cold clumps, we conducted a comparative analysis of
various NH3 molecular line surveys targeting different types of celestial
objects. This analysis involved a comprehensive examination of line widths,
kinetic temperatures, NH3 column densities, as well as column densities of H2,
and fractional abundances. In this particular study, to conduct a more
comprehensive comparative analysis, we have incorporated not only the samples
mentioned in Sec. 4.3, but also included additional statistical samples,
ultra-compact Hii (UC Hii) regions or UC Hii region candidates (Molinari et
al., 1996), High Infrared (IR) extinction clouds (Rygl et al., 2010) and
Extended Green Objects (EGOs) (Cyganowski et al., 2013). The fundamental
information regarding these sources has been presented in Table 4. It is
crucial to emphasize that not all papers provide data for every parameter. In
certain studies, some parameters were not reported. Therefore, in the
comparison involving these parameters, we opted to consider only those papers
that presented available data.

The kinetic temperatures of the cores range from 8.9 to 20.7 K, with an
average of 12.3 $\pm$ 2.9 K and a median value of 11.4 K (as mentioned in
Sect. 4.2), and after cross-matching our NH3 detected 249 sources with PGCCs
from Planck Collaboration et al. (2016), we have observed that the dust
temperature ($T_{\rm dust}$) of these 249 sources falls within the range of
8.6 to 13.9 K, with an average value of 11.5 K. The similarity in temperature
ranges between $T_{\rm kin}$ and $T_{\rm dust}$ indicates an efficient
coupling of gas and dust. The cumulative distribution of the kinetic
temperature of NH3 for different samples is presented in Fig. 7 (a). The
results indicate that the UC Hii candidates exhibit the highest kinetic
temperatures (Molinari et al., 1996), while the Planck cold cores show lower
temperatures compared to other classes of sources. The temperature
distribution of the samples is distinct and follows the expected evolutionary
sequence. Hence, the kinetic temperature can serve as a reliable indicator for
distinguishing between different evolutionary stages.

Fig. 7 (b) depicts the cumulative distribution of NH3 (1,1) line widths. Our
analysis indicates that the line widths of ATLASGAL sources are the largest.
The changes in the ATLASGAL and UC Hii regions flatten off when the line width
exceeds $\sim$2.5 km s-1, and their slopes are nearly identical when the line
width is smaller than 2.5 km s-1. The variation of the cumulative fraction
function of line width for the Planck cold cores is narrower when compared to
other star-forming samples (Dunham et al., 2011; Wienen et al., 2012; Chira et
al., 2013), and exhibits a similar cumulative distribution figure to those
found in the dense cores of regions like Cepheus, and Orion L1630 and L1641,
and Ophiuchus, as reported in Harju et al. (1991, 1993) and Friesen et al.
(2009). However, the average linewidth in the Planck cold cores is slightly
larger than that observed in Ophiuchus (0.62 km s-1). Notably, the higher line
width values observed in the Planck cold cores, in comparison to the dense
cores in Ophiuchus, may imply that they are in more advanced and warmer stages
of evolution. However, it is worth highlighting that the line width remains
relatively small across the various samples under examination. Fig. 7 (c),
(d), and (e) presents the cumulative distribution of column densities for NH3,
H2, and fractional ammonia abundances for various samples. The ammonia column
densities of cold cores are generally higher than those of other samples and
are even comparable to those of ATLASGAL and EGO sources. Conversely, the
cumulative distribution for Planck cold clumps exhibits the smallest H2 column
density range, resulting in high ammonia abundances. Despite the relatively
high NH3 column density observed in Planck cold cores, comprehensive
consideration of its lower temperature, linewidth, and other parameters still
leads to the conclusion that Planck sources are in an early stage of
evolution.

To quantitatively compare the distributions, we conducted two-sample
Kolmogorov-Smirnov (K-S) tests using the scipy.stats.ks_2samp procedure in the
scipy package. This statistical test assesses the dissimilarity between two
samples, with the K-S statistic serving as a measure of this dissimilarity,
ranging from 0 to 1. A K-S statistic of 0 implies that there is no significant
difference, suggesting the two samples may be from the same distribution.
Conversely, a higher K-S statistic suggests a lower likelihood of the samples
originating from the same distribution. Additionally, we computed P-values for
each pair of samples, representing the probability that the samples share the
same distribution. The outcomes of these tests are summarized in Table 4 of
Appendix A. In summary, the K-S test results for all examined parameters,
including kinetic temperature, line width, ammonia column density, hydrogen
molecule column density, and ammonia abundance, consistently yielded P-values
below 0.05. These findings strongly imply substantial disparities between the
Planck cold cores and the comparison samples in the examined parameters, which
may reflect variations in their physical properties or the influence of
distinct environmental conditions. Nevertheless, it is noteworthy that, in the
distributions of kinetic temperature and linewidth, the Perseus, Cepheus, and
Orion L1630/L1641 samples exhibit smaller KS statistic values. Moreover, their
P-values are comparatively larger than those of other samples. In contrast,
there is no pronounced similarity in the distributions of ammonia column
density and hydrogen molecule column density among these samples.
Additionally, in the abundance distribution, Planck displays relatively
smaller KS values and larger P-values when compared to BGPS and ATLASGAL
samples.

Figure 7: Comparisons for the cumulative distribution of the line widths of
NH3 (1,1), kinetic temperatures, column densities, and abundances of different
star formation samples.

##  6 Summary

We used the Nanshan 26-m radio telescope to perform single-pointing
observations of NH3 (1,1) and (2,2) inversion transitions towards 672 Planck
sources. The main results of this study are as follows:

  1. 1.

Among the observed 672 Planck sources, 249 (37%) were detected. Among these
detections, 187 cores exhibit NH3 (1,1) hyperfine structure while 76 (11%)
cores also show corresponding NH3 (2,2) emission lines. The observed sources
are mainly located in local star-forming regions. The detection rate of NH3 is
positively correlated with the continuum emission fluxes of Planck sources at
a frequency of 857 GHz, increasing as the 857 GHz flux density increases.

  2. 2.

Among the observed 672 sources, $\sim$22% have associated stellar and IR
objects within the beam size ($\sim$2$\arcmin$). This may indicate low star
formation activity of the cores in our sample and the ammonia detection rate
is higher in sources with matching stellar objects.

  3. 3.

The correlation between thermal and non-thermal velocity dispersion in NH3
(1,1) indicates the dominance of non-thermal pressure and supersonic non-
thermal motions in the dense gas traced by NH3. In contrast to high-mass star-
forming clumps and dense cores in star-forming regions, the relationship
between non-thermal velocity dispersion and kinetic temperatures in PGCCs is
notably weaker, with lower values observed for both parameters relative to
other samples under our examination.

  4. 4.

The comparison of the line-center velocities of NH3 with those from 13CO and
C18O reveals small discrepancies (0.17$\pm$0.33 km s-1, 0.12$\pm$0.18 km s-1).
The widths of NH3, 13CO, and C18O in our sample were almost undistinguishable.
These are consistent with the idea that these PGCCs are quiescent, as the
majority of them appear to be transitioning from clouds to dense clumps.

  5. 5.

The ammonia column densities range between 0.36 to 6.07 $\times$ 1015 cm-2.
The mean value is approximately 2.04 $\times$ 1015 cm-2, and the fractional
abundances of ammonia range from 0.3 to 9.7 $\times$ 10-7, with an average of
2.7 $\times$ 10-7. Our observed fractional abundances of NH3 are consistently
one order of magnitude larger in PGCCs than in Massive Star-forming (MSF)
regions and Infrared Dark Clouds (IRDCs) This significant difference in NH3
fractional abundance suggests that PGCCs are in an earlier phase of cloud
evolution compared to MSF regions and IRDCs. The elevated NH3 fractional
abundance in PGCCs relative to other star-forming regions is likely
attributable to the earlier phase of cloud evolution of PGCCs compared to
Massive Star-forming (MSF) regions or even IRDCs.

  6. 6.

The kinetic temperatures of the cores range from 8.9 to 20.7 K, with an
average of 12.3 $\pm$ 2.9 K. Similar temperature ranges between $T_{\rm kin}$
and $T_{\rm dust}$ indicate that the gas and dust are well coupled.

  7. 7.

The cumulative distribution shapes of line widths in the Planck cold cores
closely resemble those of the dense cores found in regions Cepheus, and Orion
L1630 and L1641, but with slightly higher values compared to Ophiuchus.
However, the higher line width values in the Planck cold cores, when compared
to these dense cores in Ophiuchus, suggest that they might be in more advanced
and warmer stages of evolution. Nevertheless, it is worth noting that line
width values remain small across the various samples under examination. This
observation highlights the unique characteristics of the Planck cold cores in
the context of their evolutionary stages.

###### Acknowledgements.

This work was mainly funded by the National Key R&D Program of China under
grant No. 2022YFA1603103. It was also partially funded by the Regional
Collaborative Innovation Project of Xinjiang Uyghur Autonomous Region grant
2022E01050, the Tianshan Talent Program of Xinjiang Uygur Autonomous Region
under grant No. 2022TSYCLJ0005, the Natural Science Foundation of Xinjiang
Uygur Autonomous Region under grant No. 2022D01E06, the Chinese Academy of
Sciences (CAS) “Light of West China” Program under grant Nos. xbzg-
zdsys-202212, 2020-XBQNXZ-017, and 2021-XBQNXZ-028, the National Key R&D
Program of China with grant 2023YFA1608002, the National Natural Science
Foundation of China (NSFC) under grants Nos. 12173075, 12373029, and 12103082,
the Xinjiang Key Laboratory of Radio Astrophysics under grant No. 2023D04033,
the Youth Innovation Promotion Association CAS. C.H. has been funded by the
Chinese Academy of Sciences President’s International Fellowship Initiative by
grant No. 2023VMA0031. Moreover, this work is sponsored (in part) by the
Science Committee of the Ministry of Science and Higher Education of the
Republic of Kazakhstan grant No. AP13067768. This work is based on
observations made with the Nanshan 26-m radio telescope, the Nanshan 26-m
Radio Telescope is partly supported by the Operation, Maintenance and
Upgrading Fund for Astronomical Telescopes and Facility Instruments, budgeted
from the Ministry of Finance of China (MOF) and administrated by the Chinese
Academy of Sciences (CAS), and the Urumqi Nanshan Astronomy and Deep Space
Exploration Observation and Research Station of Xinjiang.

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##  Appendix A ECC Clump Catalogue

Table 5: Basic information of the observed sources Num |  Name |  Glon |  Glat |  Dist |  Num |  Name |  Glon |  Glat |  Dist |  Num |  Name |  Glon |  Glat |  Dist
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
|  |  ∘ |  ∘ |  kpc |  |  |  ∘ |  ∘ |  kpc |  |  |  ∘ |  ∘ |  kpc
1 |  G005.03+19.07 |  5.03 |  19.08 |  1.50 |  71 |  G052.99+03.07 |  53.00 |  3.08 |  |  141 |  G098.50-03.24 |  98.50 |  -3.25 |
2 |  G005.29+14.47 |  5.30 |  14.48 |  |  72 |  G054.03-02.38 |  54.03 |  -2.39 |  |  142 |  G098.52+13.88 |  98.53 |  13.88 |  1.22
3 |  G005.29+11.07 |  5.30 |  11.07 |  1.44 |  73 |  G056.84+04.81 |  56.84 |  4.82 |  |  143 |  G098.89+14.01 |  98.90 |  14.02 |  1.17
4 |  G005.31+10.78 |  5.32 |  10.79 |  0.12 |  74 |  G057.08+04.46 |  57.08 |  4.46 |  |  144 |  G098.96+13.68 |  98.96 |  13.69 |  1.17
5 |  G005.69+36.84 |  5.69 |  36.84 |  0.21 |  75 |  G057.10+03.65 |  57.11 |  3.66 |  0.77 |  145 |  G099.11+13.97 |  99.12 |  13.98 |
6 |  G005.80+19.92 |  5.80 |  19.93 |  1.05 |  76 |  G057.17+03.41 |  57.17 |  3.42 |  |  146 |  G099.97+14.76 |  99.98 |  14.77 |
7 |  G006.04+36.74 |  6.04 |  36.75 |  1.19 |  77 |  G057.26+04.01 |  57.26 |  4.01 |  -0.66 |  147 |  G100.32+14.84 |  100.33 |  14.84 |
8 |  G006.08+20.26 |  6.09 |  20.26 |  1.33 |  78 |  G058.02+03.02 |  58.03 |  3.02 |  |  148 |  G100.45+14.95 |  100.46 |  14.96 |
9 |  G006.32+20.44 |  6.33 |  20.44 |  1.38 |  79 |  G058.07+03.20 |  58.07 |  3.21 |  |  149 |  G101.14-15.28 |  101.14 |  -15.29 |
10 |  G006.41+20.56 |  6.42 |  20.56 |  1.42 |  80 |  G058.16+03.50 |  58.16 |  3.51 |  0.67 |  150 |  G101.49+16.80 |  101.49 |  16.80 |
11 |  G006.70+20.66 |  6.70 |  20.66 |  1.17 |  81 |  G058.97-01.66 |  58.97 |  -1.66 |  |  151 |  G101.62-28.84 |  101.62 |  -28.84 |
12 |  G006.94+05.84 |  6.94 |  5.85 |  0.43 |  82 |  G060.75-01.23 |  60.75 |  -1.23 |  0.88 |  152 |  G101.88+15.17 |  101.89 |  15.17 |
13 |  G006.96+00.89 |  6.97 |  0.90 |  |  83 |  G061.76-10.80 |  61.77 |  -10.81 |  |  153 |  G102.17+07.27 |  102.17 |  7.27 |  -0.77
14 |  G006.98+20.72 |  6.99 |  20.72 |  0.95 |  84 |  G065.30-08.44 |  65.30 |  -8.44 |  |  154 |  G102.19+15.24 |  102.19 |  15.25 |
15 |  G007.14+05.94 |  7.14 |  5.94 |  1.36 |  85 |  G065.43-03.15 |  65.43 |  -3.15 |  0.35 |  155 |  G102.34+15.96 |  102.35 |  15.97 |  0.88
16 |  G007.53+21.10 |  7.54 |  21.10 |  0.88 |  86 |  G070.44-01.54 |  70.44 |  -1.55 |  1.25 |  156 |  G102.70+15.19 |  102.70 |  15.19 |  0.17
17 |  G007.80+21.10 |  7.80 |  21.10 |  0.82 |  87 |  G070.72-00.63 |  70.73 |  -0.63 |  1.23 |  157 |  G102.72-25.98 |  102.72 |  -25.99 |
18 |  G008.43+36.35 |  8.44 |  36.35 |  |  88 |  G074.11+00.11 |  74.11 |  0.11 |  2.22 |  158 |  G102.72+15.36 |  102.72 |  15.37 |  0.32
19 |  G008.52+21.84 |  8.53 |  21.84 |  0.94 |  89 |  G084.11+15.50 |  84.11 |  15.50 |  |  159 |  G103.18-17.09 |  103.18 |  -17.09 |  14.52
20 |  G008.67+22.14 |  8.68 |  22.15 |  0.84 |  90 |  G084.79-01.11 |  84.79 |  -1.12 |  2.22 |  160 |  G103.22-15.23 |  103.23 |  -15.23 |
21 |  G009.62+21.28 |  9.62 |  21.28 |  0.12 |  91 |  G089.03-41.28 |  89.03 |  -41.29 |  0.21 |  161 |  G103.49+13.07 |  103.49 |  13.08 |
22 |  G009.79+00.87 |  9.80 |  0.88 |  2.91 |  92 |  G089.29+04.01 |  89.30 |  4.01 |  |  162 |  G103.71+14.88 |  103.71 |  14.88 |
23 |  G011.09+03.43 |  11.10 |  3.43 |  1.12 |  93 |  G089.36-00.67 |  89.36 |  -0.67 |  0.73 |  163 |  G103.77+13.90 |  103.78 |  13.90 |
24 |  G011.40+36.19 |  11.40 |  36.19 |  0.20 |  94 |  G089.62+02.16 |  89.63 |  2.16 |  1.62 |  164 |  G103.90+13.97 |  103.91 |  13.98 |  0.89
25 |  G013.86+04.55 |  13.86 |  4.56 |  |  95 |  G089.64-06.86 |  89.65 |  -6.86 |  0.54 |  165 |  G104.06+12.19 |  104.06 |  12.20 |
26 |  G014.74+04.06 |  14.74 |  4.07 |  |  96 |  G089.75-02.16 |  89.76 |  -2.16 |  0.62 |  166 |  G104.78+11.49 |  104.79 |  11.49 |
27 |  G014.87+19.62 |  14.88 |  19.63 |  |  97 |  G089.64-06.59 |  89.65 |  -6.60 |  0.67 |  167 |  G105.55+10.40 |  105.56 |  10.41 |  0.90
28 |  G015.16+07.23 |  15.16 |  7.24 |  0.29 |  98 |  G089.93-07.03 |  89.93 |  -7.03 |  |  168 |  G106.30+13.57 |  106.30 |  13.57 |
29 |  G016.67-02.76 |  16.68 |  -2.76 |  |  99 |  G089.93-01.94 |  89.93 |  -1.94 |  1.18 |  169 |  G106.89+16.72 |  106.90 |  16.72 |
30 |  G017.22-01.47 |  17.23 |  -1.47 |  3.02 |  100 |  G090.76-04.55 |  90.77 |  -4.56 |  0.48 |  170 |  G107.51-09.36 |  107.51 |  -9.37 |
31 |  G018.39+19.39 |  18.39 |  19.39 |  |  101 |  G091.29-38.15 |  91.30 |  -38.16 |  |  171 |  G107.64-09.29 |  107.64 |  -9.29 |
32 |  G018.61+08.87 |  18.61 |  8.88 |  0.74 |  102 |  G091.73+04.36 |  91.74 |  4.37 |  2.07 |  172 |  G108.10+13.19 |  108.11 |  13.19 |  1.06
33 |  G019.86+20.40 |  19.86 |  20.40 |  |  103 |  G092.02+03.93 |  92.02 |  3.94 |  0.80 |  173 |  G108.23+15.61 |  108.24 |  15.62 |
34 |  G020.52+01.69 |  20.52 |  1.70 |  1.78 |  104 |  G092.26+03.80 |  92.26 |  3.81 |  1.63 |  174 |  G108.85-00.80 |  108.85 |  -0.80 |  0.18
35 |  G021.20+04.96 |  21.20 |  4.97 |  0.28 |  105 |  G092.48-02.64 |  92.48 |  -2.65 |  |  175 |  G110.41+11.52 |  110.41 |  11.53 |  0.90
36 |  G021.26+12.12 |  21.27 |  12.12 |  |  106 |  G092.79+09.14 |  92.79 |  9.14 |  0.31 |  176 |  G110.52+19.17 |  110.52 |  19.17 |  1.47
37 |  G021.66+03.78 |  21.67 |  3.79 |  0.63 |  107 |  G092.83-11.03 |  92.83 |  -11.03 |  0.41 |  177 |  G110.54+11.91 |  110.54 |  11.91 |  0.30
38 |  G023.33+11.81 |  23.33 |  11.82 |  |  108 |  G093.12-10.40 |  93.12 |  -10.41 |  0.24 |  178 |  G110.65+09.65 |  110.65 |  9.65 |  0.30
39 |  G023.37+08.21 |  23.38 |  8.22 |  0.54 |  109 |  G093.16+09.61 |  93.16 |  9.61 |  0.44 |  179 |  G110.76+19.43 |  110.76 |  19.43 |  0.24
40 |  G023.68+07.53 |  23.69 |  7.54 |  0.67 |  110 |  G093.20+09.53 |  93.21 |  9.54 |  1.46 |  180 |  G110.76+20.18 |  110.76 |  20.18 |  0.22
41 |  G025.48+06.18 |  25.49 |  6.19 |  0.23 |  111 |  G093.22-04.59 |  93.23 |  -4.59 |  0.69 |  181 |  G110.96+19.49 |  110.96 |  19.49 |  0.36
42 |  G026.45+08.02 |  26.46 |  8.03 |  -0.82 |  112 |  G093.31-11.68 |  93.32 |  -11.68 |  0.40 |  182 |  G111.04+14.03 |  111.05 |  14.03 |  0.40
43 |  G026.85+06.78 |  26.85 |  6.79 |  0.55 |  113 |  G093.36-12.06 |  93.36 |  -12.06 |  0.14 |  183 |  G111.33+19.94 |  111.34 |  19.95 |
44 |  G026.93-20.68 |  26.94 |  -20.68 |  |  114 |  G093.44-04.66 |  93.45 |  -4.67 |  0.12 |  184 |  G111.42+19.82 |  111.42 |  19.83 |  0.40
45 |  G027.09-20.70 |  27.09 |  -20.70 |  |  115 |  G093.51-04.31 |  93.52 |  -4.31 |  0.12 |  185 |  G111.46+20.18 |  111.47 |  20.18 |  0.63
46 |  G027.66+05.71 |  27.66 |  5.72 |  0.59 |  116 |  G093.62-04.44 |  93.63 |  -4.44 |  0.14 |  186 |  G111.66+20.20 |  111.67 |  20.20 |  1.30
47 |  G027.70-21.02 |  27.71 |  -21.02 |  0.41 |  117 |  G093.66+04.66 |  93.67 |  4.67 |  |  187 |  G111.68+19.74 |  111.69 |  19.75 |  1.40
48 |  G028.45-06.39 |  28.45 |  -6.39 |  0.93 |  118 |  G093.69+09.99 |  93.69 |  9.99 |  0.21 |  188 |  G111.77+13.78 |  111.77 |  13.79 |  0.30
49 |  G028.56-00.24 |  28.56 |  -0.24 |  4.09 |  119 |  G093.75-04.59 |  93.76 |  -4.59 |  0.63 |  189 |  G111.77+20.26 |  111.77 |  20.26 |  1.31
50 |  G028.71+03.88 |  28.72 |  3.88 |  0.55 |  120 |  G093.91+10.02 |  93.91 |  10.03 |  1.40 |  190 |  G111.97+20.52 |  111.97 |  20.52 |
51 |  G028.87+04.23 |  28.87 |  4.24 |  0.52 |  121 |  G093.99-04.91 |  94.00 |  -4.91 |  0.67 |  191 |  G112.03+17.89 |  112.04 |  17.90 |
52 |  G030.43+02.35 |  30.43 |  2.35 |  0.44 |  122 |  G094.08+09.46 |  94.09 |  9.46 |  0.98 |  192 |  G112.25+13.82 |  112.26 |  13.82 |  0.78
53 |  G030.78+05.22 |  30.78 |  5.23 |  0.57 |  123 |  G095.11+06.50 |  95.12 |  6.50 |  1.37 |  193 |  G112.52+08.38 |  112.52 |  8.39 |
54 |  G031.26-05.37 |  31.27 |  -5.38 |  |  124 |  G095.29-09.66 |  95.30 |  -9.67 |  0.39 |  194 |  G112.60+08.53 |  112.61 |  8.54 |  0.27
55 |  G031.44+04.18 |  31.44 |  4.18 |  0.78 |  125 |  G095.51+09.97 |  95.52 |  9.97 |  1.37 |  195 |  G112.63+20.80 |  112.63 |  20.80 |
56 |  G032.38-15.26 |  32.39 |  -15.27 |  |  126 |  G095.75+08.17 |  95.76 |  8.18 |  0.80 |  196 |  G113.42+16.97 |  113.42 |  16.98 |
57 |  G032.93+02.68 |  32.94 |  2.69 |  0.84 |  127 |  G095.97+08.17 |  95.98 |  8.18 |  -0.73 |  197 |  G113.62+15.01 |  113.62 |  15.02 |
58 |  G033.70-00.01 |  33.71 |  -0.02 |  0.70 |  128 |  G096.30+10.01 |  96.31 |  10.01 |  |  198 |  G113.75+14.90 |  113.75 |  14.90 |
59 |  G034.69-06.57 |  34.69 |  -6.58 |  0.67 |  129 |  G096.37+10.29 |  96.37 |  10.29 |  |  199 |  G114.16+14.80 |  114.17 |  14.81 |  0.77
60 |  G035.13+11.37 |  35.13 |  11.38 |  |  130 |  G096.59+10.29 |  96.59 |  10.29 |  1.29 |  200 |  G114.41-13.93 |  114.41 |  -13.94 |
61 |  G037.51+44.57 |  37.52 |  44.57 |  0.20 |  131 |  G096.94+10.25 |  96.94 |  10.26 |  1.26 |  201 |  G114.56+14.72 |  114.57 |  14.73 |  0.79
62 |  G038.36-00.95 |  38.36 |  -0.95 |  1.11 |  132 |  G097.09+10.12 |  97.10 |  10.12 |  1.27 |  202 |  G114.67+14.47 |  114.68 |  14.48 |  0.77
63 |  G043.02+08.36 |  43.02 |  8.37 |  0.30 |  133 |  G097.20+09.87 |  97.21 |  9.88 |  1.22 |  203 |  G115.81-03.54 |  115.82 |  -3.55 |  0.37
64 |  G046.75-07.68 |  46.76 |  -7.69 |  |  134 |  G097.38+09.95 |  97.38 |  9.95 |  1.17 |  204 |  G115.92+09.46 |  115.93 |  9.46 |  1.00
65 |  G047.74-05.56 |  47.75 |  -5.57 |  |  135 |  G097.71+15.32 |  97.71 |  15.33 |  |  205 |  G116.01+09.12 |  116.02 |  9.12 |
66 |  G048.25-05.73 |  48.25 |  -5.74 |  |  136 |  G097.77+08.59 |  97.78 |  8.59 |  1.10 |  206 |  G116.08-02.38 |  116.08 |  -2.39 |  0.39
67 |  G048.40-05.82 |  48.41 |  -5.83 |  |  137 |  G097.80+15.21 |  97.80 |  15.21 |  |  207 |  G116.12+08.98 |  116.13 |  8.99 |
68 |  G048.82-03.82 |  48.82 |  -3.83 |  0.24 |  138 |  G097.84+15.32 |  97.84 |  15.33 |  |  208 |  G116.23+20.36 |  116.24 |  20.36 |
69 |  G049.06-04.18 |  49.06 |  -4.18 |  0.82 |  139 |  G098.06+13.97 |  98.06 |  13.98 |  0.36 |  209 |  G116.25+20.18 |  116.26 |  20.18 |
70 |  G049.76-07.25 |  49.77 |  -7.26 |  1.53 |  140 |  G098.10+15.83 |  98.11 |  15.83 |  |  210 |  G116.30+12.29 |  116.30 |  12.29 |  0.38
Table 6: Continued Num |  Name |  Glon |  Glat |  Dist |  Num |  Name |  Glon |  Glat |  Dist |  Num |  Name |  Glon |  Glat |  Dist
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
|  |  ∘ |  ∘ |  kpc |  |  |  ∘ |  ∘ |  kpc |  |  |  ∘ |  ∘ |  kpc
211 |  G117.11+12.42 |  117.11 |  12.43 |  0.11 |  286 |  G144.44+08.55 |  144.45 |  8.56 |  -0.66 |  361 |  G159.41-34.36 |  159.41 |  -34.36 |  1.20
212 |  G118.08-09.68 |  118.08 |  -9.69 |  |  287 |  G144.49+08.70 |  144.49 |  8.71 |  |  362 |  G159.52+03.26 |  159.52 |  3.27 |  3.50
213 |  G118.14+08.83 |  118.15 |  8.84 |  |  288 |  G144.66+00.16 |  144.67 |  0.17 |  0.85 |  363 |  G159.58-32.84 |  159.59 |  -32.84 |  0.25
214 |  G118.25-52.70 |  118.25 |  -52.71 |  0.26 |  289 |  G144.66+06.11 |  144.67 |  6.11 |  0.53 |  364 |  G159.65-19.68 |  159.65 |  -19.69 |  0.29
215 |  G118.34+08.66 |  118.34 |  8.67 |  |  290 |  G144.84+00.76 |  144.84 |  0.76 |  |  365 |  G159.65+11.39 |  159.65 |  11.40 |  0.17
216 |  G118.36+21.74 |  118.37 |  21.74 |  0.38 |  291 |  G145.08-39.30 |  145.09 |  -39.31 |  0.28 |  366 |  G159.67-05.71 |  159.68 |  -5.72 |  0.14
217 |  G120.16+03.09 |  120.17 |  3.10 |  1.36 |  292 |  G145.48+09.51 |  145.48 |  9.52 |  -0.66 |  367 |  G159.67-34.31 |  159.68 |  -34.32 |  0.43
218 |  G120.67+02.66 |  120.67 |  2.67 |  1.82 |  293 |  G145.81+10.97 |  145.81 |  10.98 |  |  368 |  G159.76-19.62 |  159.76 |  -19.63 |  0.31
219 |  G120.98+02.66 |  120.98 |  2.67 |  0.87 |  294 |  G145.87+17.77 |  145.88 |  17.78 |  0.20 |  369 |  G159.78-24.80 |  159.79 |  -24.81 |
220 |  G121.35+03.39 |  121.35 |  3.40 |  0.72 |  295 |  G146.05+17.81 |  146.05 |  17.82 |  0.20 |  370 |  G159.82-10.48 |  159.83 |  -10.48 |
221 |  G121.50-20.92 |  121.51 |  -20.92 |  |  296 |  G146.11+07.80 |  146.12 |  7.80 |  |  371 |  G160.33+03.24 |  160.33 |  3.25 |
222 |  G121.57+23.39 |  121.57 |  23.40 |  0.38 |  297 |  G146.18+08.80 |  146.18 |  8.80 |  |  372 |  G160.35-06.37 |  160.36 |  -6.37 |
223 |  G121.88-08.76 |  121.88 |  -8.76 |  |  298 |  G146.71+02.05 |  146.71 |  2.05 |  -1.03 |  373 |  G160.51-17.07 |  160.51 |  -17.07 |  0.14
224 |  G121.90-01.54 |  121.90 |  -1.55 |  -1.23 |  299 |  G147.01+03.39 |  147.02 |  3.40 |  0.59 |  374 |  G160.51-16.84 |  160.51 |  -16.84 |  1.12
225 |  G121.92-07.66 |  121.93 |  -7.67 |  |  300 |  G147.76+09.17 |  147.77 |  9.18 |  |  375 |  G160.53-19.72 |  160.53 |  -19.73 |  0.37
226 |  G121.92-01.71 |  121.93 |  -1.72 |  |  301 |  G147.96-08.02 |  147.96 |  -8.03 |  -0.82 |  376 |  G160.53-09.84 |  160.53 |  -9.84 |  0.65
227 |  G121.99+24.23 |  121.99 |  24.24 |  0.38 |  302 |  G148.00+00.09 |  148.01 |  0.09 |  0.77 |  377 |  G160.62-16.70 |  160.62 |  -16.70 |  0.14
228 |  G122.01-07.48 |  122.01 |  -7.48 |  |  303 |  G148.24+00.41 |  148.25 |  0.41 |  |  378 |  G160.64-35.04 |  160.64 |  -35.04 |
229 |  G122.18-10.27 |  122.19 |  -10.28 |  |  304 |  G149.23+03.07 |  149.24 |  3.08 |  0.86 |  379 |  G160.83-09.46 |  160.84 |  -9.46 |  0.14
230 |  G122.62-12.13 |  122.63 |  -12.14 |  |  305 |  G149.41+03.37 |  149.41 |  3.38 |  0.50 |  380 |  G161.08-21.78 |  161.08 |  -21.78 |
231 |  G122.73+09.61 |  122.74 |  9.61 |  0.32 |  306 |  G149.52-01.23 |  149.52 |  -1.23 |  0.89 |  381 |  G161.21-08.72 |  161.21 |  -8.73 |  0.71
232 |  G123.66+24.89 |  123.66 |  24.89 |  0.69 |  307 |  G149.58+03.45 |  149.59 |  3.45 |  0.17 |  382 |  G161.34-09.32 |  161.35 |  -9.33 |  0.25
233 |  G123.74+24.76 |  123.75 |  24.77 |  0.38 |  308 |  G149.65+03.54 |  149.66 |  3.55 |  0.17 |  383 |  G161.43-35.59 |  161.43 |  -35.59 |  1.49
234 |  G125.17+11.64 |  125.18 |  11.64 |  |  309 |  G150.22+03.91 |  150.23 |  3.92 |  0.18 |  384 |  G161.60-08.34 |  161.61 |  -8.35 |  0.59
235 |  G125.66-00.55 |  125.66 |  -0.56 |  |  310 |  G150.35-38.06 |  150.36 |  -38.06 |  0.55 |  385 |  G161.85-08.66 |  161.85 |  -8.67 |  0.47
236 |  G125.70+12.52 |  125.71 |  12.52 |  0.37 |  311 |  G150.44+03.95 |  150.45 |  3.96 |  0.87 |  386 |  G161.85-35.75 |  161.85 |  -35.75 |  1.74
237 |  G125.77+04.12 |  125.77 |  4.13 |  -1.01 |  312 |  G151.08+04.46 |  151.08 |  4.46 |  0.83 |  387 |  G162.24-09.04 |  162.25 |  -9.05 |  0.14
238 |  G126.27+05.11 |  126.28 |  5.12 |  0.48 |  313 |  G151.45+03.95 |  151.46 |  3.96 |  0.80 |  388 |  G162.46-08.70 |  162.47 |  -8.71 |  0.30
239 |  G126.49-01.30 |  126.50 |  -1.31 |  |  314 |  G151.58-38.58 |  151.59 |  -38.59 |  |  389 |  G162.64-31.67 |  162.64 |  -31.67 |
240 |  G126.62+24.54 |  126.63 |  24.54 |  0.13 |  315 |  G153.34-08.00 |  153.35 |  -8.01 |  |  390 |  G162.79+01.34 |  162.80 |  1.34 |  -1.26
241 |  G126.65-71.43 |  126.66 |  -71.44 |  |  316 |  G153.34+11.26 |  153.35 |  11.26 |  0.30 |  391 |  G162.83-18.44 |  162.84 |  -18.45 |  0.14
242 |  G126.73+06.18 |  126.74 |  6.19 |  |  317 |  G153.74+35.91 |  153.74 |  35.92 |  0.35 |  392 |  G162.86-05.24 |  162.86 |  -5.25 |  0.14
243 |  G126.95-01.06 |  126.96 |  -1.06 |  -1.17 |  318 |  G154.07+05.09 |  154.07 |  5.10 |  0.24 |  393 |  G162.90-08.63 |  162.91 |  -8.63 |  0.14
244 |  G127.22-02.25 |  127.22 |  -2.26 |  0.57 |  319 |  G154.07+05.21 |  154.07 |  5.21 |  0.23 |  394 |  G163.21-08.40 |  163.21 |  -8.40 |  0.76
245 |  G127.31-70.09 |  127.32 |  -70.10 |  |  320 |  G154.48-15.17 |  154.49 |  -15.17 |  |  395 |  G163.32-08.42 |  163.32 |  -8.42 |  0.41
246 |  G127.66+13.95 |  127.66 |  13.96 |  |  321 |  G154.55-01.24 |  154.56 |  -1.25 |  |  396 |  G163.67-08.34 |  163.67 |  -8.35 |  0.44
247 |  G127.79+13.68 |  127.79 |  13.69 |  |  322 |  G154.68-15.34 |  154.69 |  -15.35 |  0.39 |  397 |  G163.82-08.32 |  163.83 |  -8.33 |  0.42
248 |  G127.85+14.16 |  127.86 |  14.17 |  0.49 |  323 |  G154.90+04.61 |  154.91 |  4.61 |  0.26 |  398 |  G164.13-08.85 |  164.14 |  -8.86 |  0.42
249 |  G127.88+02.66 |  127.88 |  2.67 |  1.16 |  324 |  G154.95-15.19 |  154.95 |  -15.19 |  0.14 |  399 |  G164.57-24.48 |  164.58 |  -24.48 |  0.14
250 |  G128.21+13.70 |  128.21 |  13.71 |  |  325 |  G155.45-14.59 |  155.46 |  -14.59 |  0.35 |  400 |  G164.75-24.19 |  164.75 |  -24.19 |
251 |  G128.25+20.78 |  128.25 |  20.78 |  0.38 |  326 |  G155.52-08.93 |  155.52 |  -8.93 |  |  401 |  G164.81-05.67 |  164.82 |  -5.68 |  0.14
252 |  G128.89+13.68 |  128.89 |  13.69 |  0.13 |  327 |  G155.67+05.11 |  155.68 |  5.12 |  0.16 |  402 |  G164.92-12.65 |  164.93 |  -12.65 |
253 |  G128.95-00.18 |  128.96 |  -0.19 |  1.43 |  328 |  G156.04+06.03 |  156.05 |  6.04 |  |  403 |  G164.94-08.57 |  164.95 |  -8.57 |  0.42
254 |  G128.95+04.44 |  128.96 |  4.44 |  0.21 |  329 |  G156.20+05.26 |  156.20 |  5.27 |  0.23 |  404 |  G164.94-05.71 |  164.95 |  -5.72 |  0.33
255 |  G129.22+15.17 |  129.22 |  15.17 |  0.21 |  330 |  G156.42+32.53 |  156.42 |  32.53 |  |  405 |  G165.16-07.55 |  165.17 |  -7.56 |  0.26
256 |  G129.90+11.62 |  129.90 |  11.62 |  0.78 |  331 |  G156.53-08.63 |  156.53 |  -8.63 |  0.14 |  406 |  G165.34-07.51 |  165.34 |  -7.52 |  0.38
257 |  G129.94+11.73 |  129.95 |  11.74 |  |  332 |  G156.90-08.49 |  156.91 |  -8.50 |  1.12 |  407 |  G165.69-09.14 |  165.70 |  -9.14 |  0.83
258 |  G129.96+13.78 |  129.97 |  13.79 |  0.31 |  333 |  G156.92-09.72 |  156.93 |  -9.73 |  0.14 |  408 |  G165.91-44.02 |  165.92 |  -44.03 |
259 |  G130.14+11.07 |  130.14 |  11.07 |  |  334 |  G157.10-08.70 |  157.10 |  -8.71 |  1.09 |  409 |  G166.70-15.05 |  166.71 |  -15.06 |  0.14
260 |  G130.14+11.68 |  130.14 |  11.68 |  |  335 |  G157.12-11.56 |  157.13 |  -11.57 |  0.89 |  410 |  G166.99-15.34 |  166.99 |  -15.35 |  0.14
261 |  G130.14+13.78 |  130.14 |  13.79 |  0.45 |  336 |  G157.19-08.81 |  157.19 |  -8.82 |  0.14 |  411 |  G167.23-15.32 |  167.23 |  -15.33 |  0.14
262 |  G130.36+11.26 |  130.36 |  11.26 |  0.60 |  337 |  G157.25-01.00 |  157.26 |  -1.01 |  0.43 |  412 |  G168.00-15.69 |  168.00 |  -15.69 |  1.29
263 |  G130.56+11.51 |  130.56 |  11.51 |  |  338 |  G157.54-04.05 |  157.54 |  -4.05 |  |  413 |  G168.13-16.39 |  168.13 |  -16.39 |  1.10
264 |  G131.35-45.73 |  131.36 |  -45.73 |  0.24 |  339 |  G157.58-08.89 |  157.59 |  -8.89 |  0.14 |  414 |  G168.46-17.93 |  168.46 |  -17.94 |
265 |  G131.72+09.70 |  131.73 |  9.71 |  1.07 |  340 |  G157.60-12.17 |  157.61 |  -12.18 |  1.17 |  415 |  G168.72-15.48 |  168.73 |  -15.48 |  0.99
266 |  G132.03+08.95 |  132.03 |  8.95 |  0.85 |  341 |  G157.91-08.23 |  157.92 |  -8.23 |  0.14 |  416 |  G168.85-15.83 |  168.86 |  -15.83 |  1.18
267 |  G132.07+08.80 |  132.08 |  8.80 |  0.85 |  342 |  G158.20-20.28 |  158.20 |  -20.28 |  0.14 |  417 |  G168.85-14.70 |  168.86 |  -14.71 |  0.14
268 |  G132.07+13.63 |  132.08 |  13.63 |  |  343 |  G158.22-20.14 |  158.23 |  -20.15 |  0.14 |  418 |  G169.14-01.13 |  169.15 |  -1.14 |
269 |  G132.27+13.26 |  132.28 |  13.27 |  |  344 |  G158.24-21.80 |  158.25 |  -21.80 |  0.37 |  419 |  G169.32-16.15 |  169.32 |  -16.16 |  1.03
270 |  G132.29+09.36 |  132.30 |  9.37 |  1.25 |  345 |  G158.37-20.72 |  158.38 |  -20.72 |  0.73 |  420 |  G169.43-16.17 |  169.43 |  -16.18 |  1.08
271 |  G133.28+08.81 |  133.29 |  8.82 |  1.56 |  346 |  G158.40-21.86 |  158.40 |  -21.86 |  0.14 |  421 |  G169.76-16.15 |  169.76 |  -16.16 |  1.07
272 |  G133.48+09.02 |  133.48 |  9.03 |  1.68 |  347 |  G158.77-33.30 |  158.77 |  -33.31 |  0.60 |  422 |  G169.82-19.39 |  169.83 |  -19.39 |  0.14
273 |  G133.72-45.31 |  133.73 |  -45.32 |  |  348 |  G158.86-21.60 |  158.86 |  -21.60 |  0.52 |  423 |  G169.84-07.61 |  169.85 |  -7.61 |  1.18
274 |  G135.08+12.92 |  135.09 |  12.92 |  |  349 |  G158.88-34.18 |  158.88 |  -34.18 |  0.33 |  424 |  G169.98-18.97 |  169.98 |  -18.98 |  1.58
275 |  G135.28+12.90 |  135.29 |  12.90 |  |  350 |  G158.97-33.01 |  158.97 |  -33.02 |  0.32 |  425 |  G169.98-04.27 |  169.98 |  -4.28 |  1.18
276 |  G136.31-01.77 |  136.32 |  -1.77 |  |  351 |  G159.01-08.46 |  159.02 |  -8.46 |  0.73 |  426 |  G170.00-16.14 |  170.00 |  -16.14 |  1.15
277 |  G139.17+15.07 |  139.17 |  15.08 |  |  352 |  G159.03-08.32 |  159.04 |  -8.33 |  0.14 |  427 |  G170.13-16.06 |  170.13 |  -16.06 |  1.39
278 |  G140.49+06.07 |  140.49 |  6.07 |  |  353 |  G159.14-08.76 |  159.15 |  -8.76 |  0.14 |  428 |  G170.26-16.02 |  170.27 |  -16.02 |  1.35
279 |  G140.77+05.00 |  140.78 |  5.00 |  0.58 |  354 |  G159.16-05.58 |  159.17 |  -5.59 |  0.62 |  429 |  G170.57-07.85 |  170.57 |  -7.86 |
280 |  G140.97+05.73 |  140.98 |  5.74 |  1.21 |  355 |  G159.21-20.44 |  159.21 |  -20.44 |  0.21 |  430 |  G170.77-08.51 |  170.77 |  -8.52 |  0.23
281 |  G142.25+05.43 |  142.25 |  5.44 |  0.50 |  356 |  G159.21-20.12 |  159.21 |  -20.13 |  0.71 |  431 |  G170.81-18.34 |  170.82 |  -18.35 |  1.71
282 |  G142.29+07.65 |  142.29 |  7.65 |  |  357 |  G159.23-34.49 |  159.24 |  -34.50 |  1.17 |  432 |  G170.83-15.90 |  170.84 |  -15.91 |  0.23
283 |  G142.49+07.48 |  142.49 |  7.48 |  |  358 |  G159.34+11.20 |  159.35 |  11.21 |  0.17 |  433 |  G170.88-10.92 |  170.88 |  -10.92 |  0.57
284 |  G142.62+07.29 |  142.62 |  7.29 |  |  359 |  G159.34-24.39 |  159.35 |  -24.40 |  0.14 |  434 |  G170.99-15.81 |  170.99 |  -15.81 |  1.41
285 |  G143.85+11.49 |  143.85 |  11.49 |  |  360 |  G159.36+03.77 |  159.37 |  3.77 |  3.31 |  435 |  G171.03+02.66 |  171.04 |  2.67 |
Table 7: Continued Num |  Name |  Glon |  Glat |  Dist |  Num |  Name |  Glon |  Glat |  Dist |  Num |  Name |  Glon |  Glat |  Dist
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
|  |  ∘ |  ∘ |  kpc |  |  |  ∘ |  ∘ |  kpc |  |  |  ∘ |  ∘ |  kpc
436 |  G171.14-17.58 |  171.15 |  -17.58 |  0.79 |  511 |  G177.86+01.04 |  177.87 |  1.04 |  1.71 |  586 |  G206.54-14.45 |  206.54 |  -14.46 |  0.42
437 |  G171.32+04.40 |  171.32 |  4.41 |  |  512 |  G177.89-20.16 |  177.89 |  -20.17 |  0.36 |  587 |  G206.60-14.40 |  206.61 |  -14.40 |  0.62
438 |  G171.34-10.67 |  171.34 |  -10.67 |  0.23 |  513 |  G177.97-09.72 |  177.98 |  -9.73 |  0.60 |  588 |  G206.87-04.36 |  206.87 |  -4.37 |  0.42
439 |  G171.34+02.59 |  171.34 |  2.59 |  1.78 |  514 |  G178.28-00.61 |  178.29 |  -0.62 |  0.94 |  589 |  G207.35-19.82 |  207.36 |  -19.83 |  0.42
440 |  G171.43-17.36 |  171.43 |  -17.37 |  0.23 |  515 |  G178.48-06.76 |  178.48 |  -6.77 |  0.23 |  590 |  G208.56+02.36 |  208.56 |  2.37 |  1.14
441 |  G171.49-14.90 |  171.50 |  -14.90 |  1.47 |  516 |  G178.72-07.01 |  178.73 |  -7.01 |  0.23 |  591 |  G209.20+02.12 |  209.20 |  2.13 |  1.13
442 |  G171.51-10.59 |  171.52 |  -10.60 |  1.35 |  517 |  G178.98-06.74 |  178.99 |  -6.75 |  0.59 |  592 |  G209.28-19.62 |  209.29 |  -19.63 |  1.08
443 |  G171.67-18.05 |  171.67 |  -18.05 |  0.23 |  518 |  G179.14-06.27 |  179.14 |  -6.28 |  0.23 |  593 |  G210.01-20.16 |  210.01 |  -20.17 |  0.42
444 |  G171.73-17.13 |  171.74 |  -17.13 |  0.23 |  519 |  G179.18-19.62 |  179.19 |  -19.63 |  0.31 |  594 |  G210.30-00.03 |  210.30 |  -0.03 |  5.44
445 |  G171.78-15.65 |  171.78 |  -15.66 |  0.23 |  520 |  G179.29+04.20 |  179.30 |  4.20 |  |  595 |  G210.67-36.77 |  210.67 |  -36.77 |  0.14
446 |  G171.78-08.44 |  171.78 |  -8.44 |  0.23 |  521 |  G179.40+04.06 |  179.41 |  4.07 |  0.70 |  596 |  G210.89-36.53 |  210.89 |  -36.54 |  0.14
447 |  G171.80-15.32 |  171.80 |  -15.33 |  1.64 |  522 |  G180.81-19.66 |  180.81 |  -19.67 |  0.35 |  597 |  G211.48-19.27 |  211.49 |  -19.27 |  0.61
448 |  G171.80-09.78 |  171.80 |  -9.78 |  0.23 |  523 |  G180.92+04.53 |  180.92 |  4.54 |  0.96 |  598 |  G211.70-12.17 |  211.71 |  -12.18 |  0.42
449 |  G171.84-05.22 |  171.85 |  -5.23 |  1.55 |  524 |  G181.16+04.33 |  181.16 |  4.33 |  |  599 |  G212.10-19.15 |  212.10 |  -19.16 |  0.65
450 |  G171.91-15.65 |  171.91 |  -15.66 |  0.23 |  525 |  G181.42-03.73 |  181.43 |  -3.73 |  |  600 |  G212.18+05.11 |  212.19 |  5.12 |
451 |  G172.06-15.21 |  172.07 |  -15.21 |  1.65 |  526 |  G181.71+04.16 |  181.71 |  4.16 |  |  601 |  G213.92-13.61 |  213.93 |  -13.61 |  0.42
452 |  G172.13-16.93 |  172.13 |  -16.94 |  1.98 |  527 |  G181.73-19.35 |  181.74 |  -19.35 |  0.25 |  602 |  G213.96-19.64 |  213.97 |  -19.65 |  0.42
453 |  G172.15-16.02 |  172.16 |  -16.02 |  0.23 |  528 |  G181.84+00.31 |  181.85 |  0.32 |  1.76 |  603 |  G214.21-13.40 |  214.21 |  -13.40 |  1.39
454 |  G172.15-09.93 |  172.16 |  -9.93 |  0.23 |  529 |  G181.88+04.49 |  181.89 |  4.50 |  |  604 |  G214.43-19.90 |  214.43 |  -19.91 |  0.46
455 |  G172.30-09.91 |  172.31 |  -9.92 |  0.23 |  530 |  G182.02-00.16 |  182.02 |  -0.17 |  |  605 |  G214.54+00.98 |  214.54 |  0.99 |
456 |  G172.33-18.24 |  172.33 |  -18.25 |  0.23 |  531 |  G182.04+00.41 |  182.04 |  0.41 |  1.76 |  606 |  G214.69-19.94 |  214.69 |  -19.95 |  0.42
457 |  G172.57-18.11 |  172.57 |  -18.11 |  |  532 |  G182.15-17.95 |  182.15 |  -17.95 |  0.23 |  607 |  G215.00-15.13 |  215.00 |  -15.13 |
458 |  G172.83-05.17 |  172.84 |  -5.17 |  0.23 |  533 |  G182.19-17.71 |  182.20 |  -17.72 |  0.23 |  608 |  G215.41-16.39 |  215.42 |  -16.39 |  0.42
459 |  G172.85-14.74 |  172.86 |  -14.75 |  0.23 |  534 |  G182.30-19.19 |  182.31 |  -19.19 |  0.23 |  609 |  G215.70-15.05 |  215.71 |  -15.06 |  0.42
460 |  G172.85+02.27 |  172.86 |  2.28 |  1.71 |  535 |  G182.54-25.34 |  182.55 |  -25.34 |  |  610 |  G215.88-17.58 |  215.88 |  -17.58 |  0.42
461 |  G172.92-16.74 |  172.92 |  -16.74 |  1.43 |  536 |  G185.29-02.27 |  185.30 |  -2.28 |  |  611 |  G215.92-15.32 |  215.93 |  -15.33 |  0.42
462 |  G172.94-05.49 |  172.95 |  -5.49 |  1.75 |  537 |  G185.33-02.12 |  185.34 |  -2.13 |  |  612 |  G216.01-15.94 |  216.01 |  -15.95 |  0.42
463 |  G173.07-17.89 |  173.08 |  -17.90 |  0.23 |  538 |  G185.80-09.12 |  185.80 |  -9.12 |  0.24 |  613 |  G216.18-15.24 |  216.19 |  -15.25 |  0.42
464 |  G173.07-16.52 |  173.08 |  -16.53 |  1.29 |  539 |  G188.04-03.71 |  188.04 |  -3.71 |  |  614 |  G216.32-15.71 |  216.32 |  -15.71 |  0.42
465 |  G173.10+07.23 |  173.10 |  7.24 |  |  540 |  G190.08-13.51 |  190.09 |  -13.52 |  |  615 |  G216.51-13.88 |  216.52 |  -13.88 |  1.12
466 |  G173.12-13.32 |  173.12 |  -13.32 |  1.47 |  541 |  G190.15-14.34 |  190.15 |  -14.34 |  0.22 |  616 |  G216.69-13.88 |  216.69 |  -13.88 |  0.42
467 |  G173.18-09.12 |  173.19 |  -9.12 |  |  542 |  G190.17-13.78 |  190.17 |  -13.79 |  0.27 |  617 |  G216.76+02.12 |  216.76 |  2.13 |  12.90
468 |  G173.32+31.27 |  173.32 |  31.28 |  |  543 |  G190.50-02.29 |  190.50 |  -2.29 |  -1.10 |  618 |  G216.76-16.06 |  216.76 |  -16.06 |  0.42
469 |  G173.36-16.27 |  173.36 |  -16.28 |  1.32 |  544 |  G191.00-04.59 |  191.01 |  -4.59 |  0.51 |  619 |  G217.13-12.54 |  217.13 |  -12.54 |  1.16
470 |  G173.45-13.34 |  173.45 |  -13.34 |  1.52 |  545 |  G191.03-16.74 |  191.03 |  -16.74 |  |  620 |  G217.41-13.93 |  217.42 |  -13.94 |  0.42
471 |  G173.45-05.43 |  173.45 |  -5.44 |  0.23 |  546 |  G191.51-00.76 |  191.51 |  -0.76 |  0.18 |  621 |  G217.46-13.78 |  217.46 |  -13.79 |  0.42
472 |  G173.60-17.89 |  173.61 |  -17.90 |  |  547 |  G191.51-00.77 |  192.51 |  0.24 |  12.45 |  622 |  G217.70-16.12 |  217.71 |  -16.12 |
473 |  G173.69-15.55 |  173.69 |  -15.56 |  0.23 |  548 |  G192.28-11.33 |  192.28 |  -11.34 |  0.42 |  623 |  G217.79-17.36 |  217.79 |  -17.37 |  0.42
474 |  G173.78-05.26 |  173.78 |  -5.27 |  0.32 |  549 |  G192.32-11.87 |  192.33 |  -11.87 |  0.38 |  624 |  G219.06-07.46 |  219.07 |  -7.46 |  0.42
475 |  G173.80-15.88 |  173.80 |  -15.89 |  1.77 |  550 |  G192.54-11.56 |  192.55 |  -11.57 |  0.40 |  625 |  G219.24-10.02 |  219.24 |  -10.03 |  1.29
476 |  G173.89-17.64 |  173.89 |  -17.64 |  1.10 |  551 |  G192.94-03.73 |  192.94 |  -3.73 |  1.00 |  626 |  G219.24-07.95 |  219.24 |  -7.95 |  0.42
477 |  G173.91-16.25 |  173.91 |  -16.26 |  0.23 |  552 |  G194.69-16.84 |  194.70 |  -16.84 |  0.40 |  627 |  G219.26-17.89 |  219.27 |  -17.90 |  0.42
478 |  G173.91+31.16 |  173.91 |  31.17 |  |  553 |  G194.80-03.41 |  194.81 |  -3.42 |  1.56 |  628 |  G219.28-09.27 |  219.29 |  -9.27 |  0.91
479 |  G173.95-13.74 |  173.96 |  -13.75 |  1.74 |  554 |  G194.94-16.74 |  194.94 |  -16.74 |  0.40 |  629 |  G219.30-08.15 |  219.31 |  -8.16 |
480 |  G174.06-15.81 |  174.07 |  -15.81 |  1.97 |  555 |  G195.00-16.95 |  195.01 |  -16.96 |  0.40 |  630 |  G219.33-17.64 |  219.33 |  -17.64 |  0.42
481 |  G174.08-13.24 |  174.09 |  -13.25 |  1.65 |  556 |  G195.09-16.41 |  195.10 |  -16.41 |  0.40 |  631 |  G219.35-09.70 |  219.35 |  -9.71 |  0.91
482 |  G174.22-13.43 |  174.22 |  -13.44 |  1.70 |  557 |  G196.21-15.50 |  196.22 |  -15.50 |  0.40 |  632 |  G219.37-07.68 |  219.37 |  -7.69 |  0.42
483 |  G174.39-13.43 |  174.40 |  -13.44 |  1.84 |  558 |  G196.65+13.99 |  196.66 |  14.00 |  |  633 |  G220.67-01.86 |  220.67 |  -1.87 |  1.22
484 |  G174.44-15.75 |  174.44 |  -15.75 |  1.78 |  559 |  G198.03-15.24 |  198.04 |  -15.25 |  0.14 |  634 |  G220.95-08.32 |  220.96 |  -8.33 |
485 |  G174.50-19.88 |  174.51 |  -19.89 |  0.23 |  560 |  G198.56-09.10 |  198.57 |  -9.10 |  2.03 |  635 |  G220.97-07.74 |  220.98 |  -7.75 |
486 |  G174.57-13.66 |  174.57 |  -13.67 |  0.23 |  561 |  G198.96+01.41 |  198.96 |  1.42 |  |  636 |  G221.06-02.72 |  221.07 |  -2.72 |
487 |  G174.70-15.48 |  174.70 |  -15.48 |  2.06 |  562 |  G199.88+00.93 |  199.89 |  0.93 |  0.97 |  637 |  G221.46-17.89 |  221.46 |  -17.90 |
488 |  G174.81-15.15 |  174.81 |  -15.15 |  2.00 |  563 |  G200.34-10.97 |  200.35 |  -10.98 |  |  638 |  G221.68-17.07 |  221.68 |  -17.07 |  0.42
489 |  G174.81+05.96 |  174.81 |  5.96 |  |  564 |  G201.13+00.31 |  201.14 |  0.32 |  0.79 |  639 |  G222.01-17.13 |  222.01 |  -17.13 |  0.42
490 |  G174.88-17.11 |  174.88 |  -17.11 |  0.23 |  565 |  G201.26+00.46 |  201.27 |  0.47 |  |  640 |  G222.14-16.97 |  222.14 |  -16.98 |
491 |  G174.99-04.83 |  174.99 |  -4.84 |  0.38 |  566 |  G201.44+00.65 |  201.45 |  0.65 |  0.53 |  641 |  G222.23+01.21 |  222.23 |  1.21 |  2.47
492 |  G175.16-16.74 |  175.17 |  -16.74 |  0.23 |  567 |  G201.59+00.55 |  201.60 |  0.56 |  0.68 |  642 |  G222.95-05.45 |  222.96 |  -5.45 |  0.54
493 |  G175.20+01.28 |  175.21 |  1.29 |  4.59 |  568 |  G201.84+02.81 |  201.84 |  2.82 |  0.76 |  643 |  G224.27-00.82 |  224.27 |  -0.82 |  1.42
494 |  G175.31-20.50 |  175.32 |  -20.50 |  |  569 |  G202.21-09.17 |  202.21 |  -9.18 |  0.42 |  644 |  G224.47-00.65 |  224.47 |  -0.65 |  1.52
495 |  G175.34-10.82 |  175.34 |  -10.83 |  0.23 |  570 |  G202.30-08.91 |  202.30 |  -8.91 |  0.41 |  645 |  G226.16-00.41 |  226.16 |  -0.41 |  1.05
496 |  G175.49-16.80 |  175.50 |  -16.80 |  1.96 |  571 |  G202.58-08.70 |  202.59 |  -8.71 |  0.42 |  646 |  G226.29-00.63 |  226.30 |  -0.63 |
497 |  G175.53+01.34 |  175.54 |  1.34 |  |  572 |  G203.00-03.69 |  203.01 |  -3.70 |  0.18 |  647 |  G226.36-00.50 |  226.36 |  -0.50 |  0.77
498 |  G175.58-16.60 |  175.58 |  -16.61 |  0.23 |  573 |  G203.11-08.70 |  203.12 |  -8.71 |  0.42 |  648 |  G226.38+01.30 |  226.38 |  1.31 |  0.88
499 |  G175.97-20.38 |  175.98 |  -20.38 |  |  574 |  G203.20-11.20 |  203.20 |  -11.21 |  0.41 |  649 |  G226.71-07.46 |  226.71 |  -7.46 |  0.56
500 |  G176.17-02.10 |  176.18 |  -2.11 |  1.57 |  575 |  G203.57-30.08 |  203.58 |  -30.09 |  0.19 |  650 |  G226.80-07.04 |  226.80 |  -7.05 |
501 |  G176.35+01.92 |  176.35 |  1.92 |  |  576 |  G203.75-08.49 |  203.75 |  -8.50 |  1.65 |  651 |  G227.30-03.77 |  227.31 |  -3.77 |
502 |  G176.37-02.05 |  176.37 |  -2.05 |  1.57 |  577 |  G204.49-11.33 |  204.50 |  -11.34 |  0.42 |  652 |  G227.70+11.18 |  227.70 |  11.19 |  0.28
503 |  G176.46-21.10 |  176.46 |  -21.10 |  0.23 |  578 |  G204.82-13.88 |  204.83 |  -13.88 |  1.27 |  653 |  G227.76+11.32 |  227.77 |  11.32 |  0.18
504 |  G176.52-09.80 |  176.53 |  -9.80 |  -0.65 |  579 |  G205.29-06.01 |  205.29 |  -6.02 |  0.40 |  654 |  G227.90-03.37 |  227.90 |  -3.38 |  2.00
505 |  G176.94+04.63 |  176.95 |  4.63 |  |  580 |  G205.42-08.15 |  205.42 |  -8.16 |  0.42 |  655 |  G228.51+11.77 |  228.52 |  11.78 |
506 |  G177.09+02.85 |  177.10 |  2.85 |  0.21 |  581 |  G205.57-08.25 |  205.58 |  -8.25 |  0.97 |  656 |  G229.30-08.44 |  229.31 |  -8.44 |
507 |  G177.14-01.21 |  177.14 |  -1.21 |  0.17 |  582 |  G206.05-08.36 |  206.06 |  -8.37 |  0.42 |  657 |  G229.72-06.88 |  229.72 |  -6.88 |  0.15
508 |  G177.60-20.58 |  177.60 |  -20.58 |  0.23 |  583 |  G206.10-15.77 |  206.10 |  -15.77 |  0.33 |  658 |  G230.29+12.44 |  230.30 |  12.44 |
509 |  G177.62-20.36 |  177.63 |  -20.36 |  0.23 |  584 |  G206.21-08.42 |  206.21 |  -8.42 |  0.42 |  659 |  G231.81-02.07 |  231.81 |  -2.07 |  3.53
510 |  G177.67-20.20 |  177.67 |  -20.20 |  0.23 |  585 |  G206.34-08.57 |  206.35 |  -8.57 |  0.42 |  660 |  G232.95+00.91 |  232.95 |  0.91 |
Table 8: Continued Num |  Name |  Glon |  Glat |  Dist |  Num |  Name |  Glon |  Glat |  Dist |  Num |  Name |  Glon |  Glat |  Dist
---|---|---|---|---|---|---|---|---|---|---|---|---|---|---
|  |  ∘ |  ∘ |  kpc |  |  |  ∘ |  ∘ |  kpc |  |  |  ∘ |  ∘ |  kpc
661 |  G236.68-05.21 |  236.69 |  -5.21 |  |  665 |  G238.71-01.47 |  238.71 |  -1.47 |  1.13 |  669 |  G353.54+15.73 |  353.54 |  15.73 |  0.12
662 |  G237.30-04.76 |  237.30 |  -4.76 |  |  666 |  G239.58-04.61 |  239.59 |  -4.61 |  |  670 |  G354.17+15.32 |  354.18 |  15.33 |  0.12
663 |  G238.44-04.16 |  238.45 |  -4.16 |  |  667 |  G240.99-01.21 |  241.00 |  -1.21 |  6.15 |  671 |  G354.19+16.27 |  354.20 |  16.28 |  0.12
664 |  G238.51-03.88 |  238.51 |  -3.88 |  1.00 |  668 |  G353.49+15.57 |  353.50 |  15.58 |  0.12 |  672 |  G354.46+16.15 |  354.46 |  16.16 |  0.12
Table 2: Observed parameters of the NH3 (1,1) and NH3 (2,2 ) emission lines in the NH3 detected sources. Name | $V_{\rm LSR}(1,1)$ | $\Delta v(1,1)$ | $\tau(1,1)$ | $T_{\rm MB}(1,1)$ | $V_{\rm LSR}(2,2)$ | $\Delta v(2,2)$ | $T_{\rm MB}(2,2)$
---|---|---|---|---|---|---|---
|  km s-1 |  km s-1 |  | K |  km s-1 |  km s-1 | K
G005.03+19.07 | 3.88(0.03) | 0.76(0.06) |  | 0.07(0.01) |  |  |
G005.29+11.07 | 4.04(0.03) | 0.83(0.08) | 0.64(0.47) | 0.12(0.01) |  |  |
G005.69+36.84 | 1.76(0.04) | 0.48(0.08) |  | 0.03(0.01) |  |  |
G005.80+19.92 | 2.79(0.04) | 0.65(0.09) |  | 0.27(0.04) |  |  |
G006.04+36.74 | 2.37(0.02) | 0.68(0.04) | 4.16(0.30) | 1.11(0.09) | 2.30(0.03) | 0.32(0.06) | 0.20(0.03)
G006.08+20.26 | 3.96(0.05) | 0.92(0.14) |  | 0.21(0.04) |  |  |
G006.32+20.44 | 4.13(0.01) | 0.69(0.03) | 0.85(0.10) | 0.71(0.04) | 4.21(0.02) | 0.50(0.05) | 0.12(0.01)
G006.41+20.56 | 4.30(0.02) | 0.68(0.05) |  | 0.40(0.04) |  |  |
G006.70+20.66 | 3.55(0.02) | 0.84(0.04) | 0.39(0.15) | 0.37(0.02) | 3.46(0.04) | 0.57(0.12) | 0.06(0.01)
G006.94+05.84 | 9.82(0.02) | 0.76(0.05) | 1.94(0.44) | 0.34(0.03) |  |  |
G006.98+20.72 | 2.95(0.03) | 0.71(0.06) | 1.04(0.56) | 0.13(0.01) | 2.97(0.04) | 0.40(0.07) | 0.06(0.01)
G007.14+05.94 | 10.28(0.03) | 0.92(0.07) | 2.25(0.35) | 0.51(0.05) |  |  |
G007.53+21.10 | 2.91(0.02) | 0.79(0.04) |  | 0.22(0.02) | 2.94(0.05) | 0.75(0.14) | 0.05(0.01)
G007.80+21.10 | 3.55(0.10) | 0.90(0.18) | 1.43(0.69) | 0.08(0.01) | 3.45(0.13) | 1.20(0.27) | 0.03(0.01)
G008.52+21.84 | 3.66(0.03) | 0.60(0.06) | 0.97(0.69) | 0.23(0.03) |  |  |
G008.67+22.14 | 3.39(0.02) | 0.65(0.03) | 3.88(0.18) | 0.61(0.04) | 3.39(0.02) | 0.28(0.07) | 0.10(0.01)
G009.79+00.87 | 28.85(0.05) | 1.83(0.14) | 2.07(0.20) | 0.30(0.04) | 28.79(0.08) | 0.94(0.21) | 0.08(0.02)
G011.09+03.43 | 6.56(0.03) | 0.65(0.05) | 2.81(0.80) | 0.08(0.01) |  |  |
G015.16+07.23 | 2.68(0.04) | 0.86(0.12) |  | 0.08(0.01) |  |  |
G018.61+08.87 | 6.74(0.03) | 0.57(0.07) |  | 0.13(0.02) |  |  |
G020.52+01.69 | 27.12(0.04) | 1.00(0.09) | 1.10(0.54) | 0.19(0.03) |  |  |
G021.20+04.96 | 3.42(0.03) | 0.79(0.06) | 2.52(0.77) | 0.24(0.03) |  |  |
G021.66+03.78 | 6.73(0.03) | 0.89(0.07) | 1.19(0.44) | 0.29(0.03) |  |  |
G023.37+08.21 | 7.81(0.04) | 0.75(0.09) | 3.07(0.94) | 0.21(0.03) |  |  |
G023.68+07.53 | 7.69(0.04) | 0.77(0.10) | 2.82(0.91) | 0.13(0.02) |  |  |
G025.48+06.18 | 7.63(0.02) | 0.67(0.05) | 2.53(0.62) | 0.41(0.04) |  |  |
G026.85+06.78 | 7.05(0.02) | 0.67(0.06) | 1.67(0.54) | 0.28(0.03) |  |  |
G027.66+05.71 | 8.03(0.02) | 0.75(0.05) | 0.10(0.12) | 0.13(0.01) |  |  |
G028.45-06.39 | 11.95(0.03) | 0.81(0.06) | 0.89(0.39) | 0.30(0.03) |  |  |
G028.56-00.24 | 85.18(0.29) | 1.79(0.51) | 0.51(0.16) | 0.39(0.11) | 85.18(0.06) | 1.82(0.14) | 0.15(0.01)
G028.71+03.88 | 7.52(0.03) | 0.94(0.07) | 5.35(0.01) | 0.80(0.09) | 7.47(0.01) | 0.60(0.04) | 0.22(0.01)
G028.87+04.23 | 6.57(0.02) | 0.76(0.04) | 1.93(0.19) | 0.29(0.02) | 6.57(0.12) | 0.65(0.43) | 0.03(0.01)
G030.43+02.35 | 9.03(0.04) | 1.11(0.10) | 1.66(0.45) | 0.27(0.04) |  |  |
G030.78+05.22 | 8.06(0.03) | 1.22(0.06) | 1.56(0.10) | 0.47(0.04) | 7.98(0.03) | 1.13(0.07) | 0.12(0.01)
G031.44+04.18 | 10.93(0.03) | 1.00(0.08) | 0.79(0.38) | 0.28(0.03) |  |  |
G032.93+02.68 | 11.53(0.03) | 0.86(0.08) | 0.49(0.36) | 0.34(0.03) |  |  |
G038.36-00.95 | 16.62(0.03) | 1.29(0.07) | 1.42(0.15) | 0.77(0.07) | 16.66(0.06) | 1.04(0.12) | 0.16(0.03)
G049.76-07.25 | 21.45(0.02) | 0.77(0.06) | 0.42(0.38) | 0.14(0.01) | 30.26(0.05) | 0.42(0.12) | 0.04(0.01)
G057.10+03.65 | 11.59(0.05) | 1.10(0.09) | 1.97(0.50) | 0.19(0.03) |  |  |
G065.43-03.15 | 5.93(0.04) | 1.04(0.11) | 1.37(0.50) | 0.21(0.03) |  |  |
G070.44-01.54 | 10.90(0.03) | 1.71(0.08) | 1.34(0.49) | 0.24(0.02) | 10.81(0.07) | 1.77(0.17) | 0.05(0.01)
G070.72-00.63 | 12.11(0.07) | 1.52(0.19) |  | 0.05(0.01) |  |  |
G074.11+00.11a | -2.23(0.17) | 1.25(0.17) | 0.96(0.37) | 0.20(0.03) |  |  |
G074.11+00.11b | -0.77(0.17) | 1.19(0.17) | 0.86(0.50) | 0.22(0.03) |  |  |
G084.79-01.11 | 0.85(0.04) | 1.57(0.08) | 1.84(0.15) | 0.85(0.09) | 0.91(0.07) | 1.27(0.13) | 0.17(0.04)
G089.36-00.67 | 2.51(0.02) | 1.13(0.06) | 1.12(0.01) | 0.30(0.02) | 2.53(0.06) | 1.01(0.24) | 0.05(0.01)
G089.62+02.16 | -0.40(0.02) | 0.87(0.05) | 3.35(0.16) | 0.46(0.04) | -0.39(0.03) | 0.37(0.06) | 0.08(0.01)
G089.64-06.59 | 12.35(0.04) | 0.88(0.09) |  | 0.06(0.01) |  |  |
G089.75-02.16 | 1.87(0.05) | 1.17(0.11) | 1.55(0.46) | 0.05(0.01) |  |  |
G089.93-01.94 | 1.45(0.04) | 1.12(0.09) | 1.92(0.53) | 0.10(0.01) |  |  |
G091.73+04.36 | -4.55(0.02) | 0.89(0.05) | 1.77(0.13) | 0.40(0.03) | -4.51(0.06) | 0.84(0.13) | 0.04(0.01)
G092.02+03.93 | -1.66(0.03) | 0.87(0.07) | 0.35(0.41) | 0.25(0.03) |  |  |
G092.26+03.80 | -1.87(0.03) | 1.22(0.07) | 2.55(0.09) | 0.55(0.05) | -1.89(0.04) | 1.06(0.10) | 0.10(0.01)
G093.20+09.53 | -1.84(0.12) | 0.51(0.19) | 5.15(0.43) | 0.17(0.03) | -2.01(0.04) | 0.41(0.11) | 0.04(0.01)
G093.22-04.59 | 3.97(0.09) | 0.79(0.17) | 1.83(0.87) | 0.10(0.01) |  |  |
G093.62-04.44 | 3.61(0.03) | 0.88(0.07) | 0.78(0.41) | 0.24(0.03) | 3.68(0.10) | 0.83(0.25) | 0.08(0.03)
G093.91+10.02 | -1.96(0.03) | 0.80(0.06) | 2.88(0.48) | 0.13(0.01) | -2.06(0.07) | 0.58(0.14) | 0.03(0.01)
G093.99-04.91 | 4.79(0.02) | 0.78(0.04) | 2.60(0.35) | 0.16(0.01) | 4.79(0.08) | 0.82(0.18) | 0.03(0.01)
G094.08+09.46 | 0.02(0.02) | 0.84(0.05) | 3.02(0.18) | 0.30(0.03) | -0.09(0.06) | 0.68(0.17) | 0.04(0.01)
G095.51+09.97 | -2.75(0.02) | 0.78(0.06) | 0.58(0.40) | 0.12(0.01) |  |  |
G095.75+08.17 | 0.37(0.02) | 0.76(0.05) | 0.44(0.34) | 0.11(0.01) | 0.18(0.04) | 0.32(0.09) | 0.04(0.01)
G096.59+10.29 | -2.71(0.02) | 0.68(0.06) | 0.47(0.52) | 0.11(0.01) | -3.51(0.04) | 0.29(0.08) | 0.04(0.01)
G096.94+10.25 | -2.65(0.02) | 0.60(0.05) | 1.91(0.63) | 0.24(0.02) |  |  |
G097.09+10.12 | -2.65(0.02) | 0.79(0.05) | 3.78(0.19) | 0.43(0.04) | -2.72(0.05) | 0.51(0.09) | 0.05(0.01)
Table 2: Continued Name | $V_{\rm LSR}(1,1)$ | $\Delta v(1,1)$ | $\tau(1,1)$ | $T_{\rm MB}(1,1)$ | $V_{\rm LSR}(2,2)$ | $\Delta v(2,2)$ | $T_{\rm MB}(2,2)$
---|---|---|---|---|---|---|---
|  km s-1 |  km s-1 |  | K |  km s-1 |  km s-1 | K
G097.20+09.87 | -2.59(0.04) | 1.02(0.08) | 1.92(0.47) | 0.25(0.03) |  |  |
G097.38+09.95 | -2.38(0.03) | 0.75(0.06) | 3.20(0.67) | 0.12(0.01) |  |  |
G098.52+13.88 | -3.21(0.02) | 0.69(0.05) | 0.88(0.50) | 0.13(0.01) |  |  |
G098.89+14.01 | -2.85(0.02) | 0.71(0.04) | 2.37(0.34) | 0.22(0.02) | -2.73(0.04) | 0.28(0.10) | 0.04(0.01)
G098.96+13.68 | -2.91(0.03) | 0.62(0.07) | 1.60(0.85) | 0.05(0.01) |  |  |
G102.34+15.96 | 2.44(0.02) | 0.76(0.04) | 2.98(0.15) | 0.72(0.05) | 2.39(0.05) | 0.66(0.10) | 0.08(0.02)
G102.70+15.19 | 1.81(0.02) | 0.71(0.04) | 2.14(0.39) | 0.18(0.01) |  |  |
G102.72+15.36 | 1.17(0.02) | 0.71(0.05) | 2.99(0.53) | 0.29(0.03) |  |  |
G103.90+13.97 | 2.73(0.02) | 0.76(0.04) | 2.71(0.21) | 0.44(0.03) | 2.71(0.02) | 0.39(0.05) | 0.09(0.01)
G108.10+13.19 | -5.54(0.02) | 0.73(0.05) | 3.07(0.48) | 0.34(0.03) |  |  |
G110.65+09.65 | -4.60(0.02) | 0.92(0.05) | 2.35(0.15) | 0.54(0.04) | -4.54(0.04) | 0.68(0.07) | 0.10(0.02)
G111.66+20.20 | -8.24(0.02) | 0.83(0.04) | 2.16(0.08) | 0.53(0.04) | -8.24(0.02) | 0.61(0.05) | 0.08(0.01)
G111.68+19.74 | -9.06(0.02) | 0.80(0.06) | 1.60(0.44) | 0.08(0.01) |  |  |
G111.77+20.26 | -8.41(0.03) | 0.64(0.06) | 1.78(0.95) | 0.14(0.02) |  |  |
G114.16+14.80 | -4.39(0.02) | 0.63(0.05) | 4.29(0.54) | 0.45(0.04) |  |  |
G114.56+14.72 | -4.58(0.06) | 0.55(0.10) |  | 0.02(0.01) |  |  |
G114.67+14.47 | -4.56(0.02) | 1.11(0.06) | 1.89(0.11) | 0.77(0.06) | -4.47(0.06) | 1.11(0.16) | 0.07(0.01)
G115.81-03.54 | -0.97(0.01) | 0.65(0.03) | 1.67(0.24) | 0.44(0.03) | -1.07(0.07) | 0.59(0.20) | 0.05(0.01)
G116.08-02.38 | -1.13(0.04) | 1.42(0.09) | 0.10(0.10) | 0.07(0.01) |  |  |
G117.11+12.42 | 3.84(0.02) | 0.79(0.05) | 3.17(0.28) | 0.60(0.05) | 3.87(0.05) | 0.33(0.11) | 0.11(0.03)
G120.16+03.09 | -19.83(0.17) | 1.02(0.17) | 0.31(0.53) | 0.18(0.03) |  |  |
G120.67+02.66 | -16.95(0.02) | 0.87(0.05) | 0.88(0.29) | 0.21(0.02) | -17.02(0.04) | 0.59(0.10) | 0.07(0.01)
G120.98+02.66 | -17.30(0.04) | 1.35(0.08) | 1.10(0.27) | 0.12(0.01) |  |  |
G121.35+03.39 | -5.51(0.04) | 0.71(0.11) | 2.32(0.92) | 0.21(0.04) |  |  |
G123.66+24.89 | -3.72(0.10) | 0.55(0.19) |  | 0.01(0.00) |  |  |
G127.85+14.16 | 2.64(0.03) | 0.64(0.07) |  | 0.11(0.02) |  |  |
G127.88+02.66 | -11.70(0.03) | 0.96(0.07) | 1.47(0.45) | 0.10(0.01) |  |  |
G128.89+13.68 | 3.80(0.02) | 0.80(0.05) | 3.03(0.32) | 0.39(0.04) | 3.95(0.10) | 0.77(0.26) | 0.05(0.02)
G128.95-00.18 | -14.83(0.03) | 0.66(0.05) |  | 0.06(0.01) |  |  |
G132.29+09.36 | -12.52(0.04) | 1.32(0.09) | 0.65(0.28) | 0.11(0.01) |  |  |
G133.28+08.81 | -11.09(0.04) | 1.09(0.09) |  | 0.06(0.01) |  |  |
G133.48+09.02a | -16.99(0.11) | 1.58(0.20) | 0.75(0.11) | 0.24(0.03) | -16.56(0.11) | 2.34(0.27) | 0.05(0.01)
G133.48+09.02b | -15.23(0.17) | 1.70(0.30) | 0.70(0.20) | 0.17(0.03) |  |  |
G140.97+05.73 | -11.68(0.06) | 1.05(0.12) |  | 0.06(0.01) |  |  |
G144.66+00.16 | -7.88(0.02) | 0.69(0.05) | 2.51(0.58) | 0.15(0.01) |  |  |
G147.01+03.39 | -4.75(0.02) | 0.76(0.04) | 1.95(0.28) | 0.27(0.02) |  |  |
G149.23+03.07 | 2.98(0.06) | 1.30(0.12) |  | 0.06(0.01) |  |  |
G149.41+03.37 | 3.35(0.04) | 0.95(0.09) | 0.10(0.45) | 0.07(0.01) |  |  |
G149.52-01.23 | -8.06(0.24) | 1.33(0.43) | 0.87(0.56) | 0.07(0.01) |  |  |
G150.22+03.91 | 3.07(0.03) | 0.60(0.06) | 0.79(0.01) | 0.24(0.03) |  |  |
G150.35-38.06 | 4.86(0.02) | 0.72(0.06) | 0.10(0.35) | 0.10(0.01) |  |  |
G150.44+03.95 | 3.31(0.03) | 0.63(0.05) | 4.10(0.70) | 0.36(0.04) |  |  |
G151.08+04.46 | 3.15(0.02) | 0.66(0.04) | 1.45(0.43) | 0.49(0.04) |  |  |
G151.45+03.95 | 1.82(0.04) | 1.20(0.09) | 0.81(0.33) | 0.10(0.01) |  |  |
G154.07+05.09 | 4.43(0.05) | 1.63(0.12) | 0.94(0.33) | 0.06(0.01) |  |  |
G154.07+05.21 | 4.39(0.04) | 0.91(0.12) |  | 0.17(0.03) |  |  |
G154.68-15.34 | 3.18(0.03) | 0.58(0.07) |  | 0.24(0.03) |  |  |
G154.90+04.61a | 2.82(0.13) | 0.84(0.18) | 0.77(0.32) | 0.06(0.01) |  |  |
G154.90+04.61b | 3.69(0.13) | 0.99(0.24) | 0.48(0.75) | 0.08(0.01) |  |  |
G155.45-14.59 | 1.67(0.03) | 0.81(0.09) | 0.10(8.91) | 0.10(0.01) |  |  |
G155.67+05.11 | 4.43(0.04) | 0.90(0.09) |  | 0.17(0.02) |  |  |
G156.20+05.26 | 5.36(0.02) | 0.62(0.05) | 0.10(0.13) | 0.26(0.02) |  |  |
G156.90-08.49 | -7.92(0.04) | 0.63(0.10) |  | 0.05(0.01) |  |  |
G157.10-08.70 | -7.51(0.04) | 0.74(0.09) |  | 0.06(0.01) |  |  |
G157.12-11.56 | -1.68(0.02) | 1.08(0.06) | 0.10(0.23) | 0.14(0.01) |  |  |
G157.25-01.00 | 5.20(0.04) | 0.69(0.10) |  | 0.15(0.03) |  |  |
G157.60-12.17 | -7.73(0.03) | 0.88(0.06) | 1.43(0.43) | 0.23(0.02) |  |  |
G158.20-20.28 | 7.39(0.01) | 0.70(0.03) | 2.13(0.14) | 0.60(0.04) | 7.38(0.03) | 0.46(0.09) | 0.07(0.01)
G158.22-20.14 | 8.12(0.01) | 0.67(0.03) | 1.88(0.11) | 0.83(0.05) | 8.13(0.02) | 0.35(0.05) | 0.10(0.01)
G158.24-21.80 | 3.92(0.02) | 0.77(0.05) |  | 0.23(0.02) |  |  |
G158.37-20.72 | 7.08(0.02) | 0.93(0.05) | 1.61(0.09) | 0.52(0.04) | 6.99(0.04) | 0.40(0.10) | 0.06(0.01)
G158.77-33.30 | -2.64(0.04) | 1.13(0.10) | 0.95(0.44) | 0.08(0.01) |  |  |
G158.86-21.60 | 4.73(0.02) | 0.87(0.04) | 0.64(0.17) | 0.33(0.02) | 4.81(0.05) | 0.50(0.11) | 0.07(0.02)
G159.01-08.46 | -4.72(0.03) | 0.90(0.08) | 1.17(0.41) | 0.12(0.01) |  |  |
G159.21-20.44 | 6.35(0.02) | 1.02(0.05) | 2.13(0.07) | 1.05(0.08) | 6.30(0.02) | 0.82(0.04) | 0.20(0.01)
G159.21-20.12 | 6.44(0.04) | 0.70(0.08) |  | 0.14(0.02) |  |  |
G159.23-34.49 | -5.39(0.03) | 1.05(0.06) | 1.11(0.31) | 0.18(0.02) |  |  |
G159.34+11.20 | 2.30(0.06) | 0.58(0.16) |  | 0.09(0.02) |  |  |
G159.41-34.36 | -5.36(0.03) | 0.86(0.07) | 0.36(0.41) | 0.19(0.02) |  |  |
G159.65-19.68 | 2.14(0.04) | 1.09(0.09) | 1.32(0.49) | 0.06(0.01) |  |  |
G159.65+11.39 | 7.28(0.04) | 0.79(0.09) |  | 0.13(0.02) |  |  |
G159.67-34.31 | -1.58(0.04) | 0.89(0.12) |  | 0.06(0.01) |  |  |
G159.76-19.62 | 7.72(0.06) | 1.45(0.14) |  | 0.06(0.01) |  |  |
G160.51-16.84 | 10.03(0.02) | 0.86(0.04) | 0.92(0.19) | 0.24(0.02) | 10.03(0.05) | 0.51(0.20) | 0.05(0.01)
Table 2: Continued Name | $V_{\rm LSR}(1,1)$ | $\Delta v(1,1)$ | $\tau(1,1)$ | $T_{\rm MB}(1,1)$ | $V_{\rm LSR}(2,2)$ | $\Delta v(2,2)$ | $T_{\rm MB}(2,2)$
---|---|---|---|---|---|---|---
|  km s-1 |  km s-1 |  | K |  km s-1 |  km s-1 | K
G160.53-19.72 | -3.84(0.02) | 0.99(0.05) | 0.58(0.23) | 0.38(0.03) |  |  |
G160.53-09.84 | 3.50(0.02) | 0.87(0.05) |  | 0.11(0.01) |  |  |
G161.21-08.72 | -3.86(0.02) | 0.62(0.05) | 1.68(0.65) | 0.22(0.02) |  |  |
G161.43-35.59 | -5.87(0.05) | 0.87(0.10) |  | 0.12(0.02) |  |  |
G161.60-08.34 | -3.26(0.03) | 0.68(0.08) |  | 0.12(0.02) |  |  |
G161.85-08.66 | -2.50(0.03) | 0.70(0.06) | 2.54(0.71) | 0.22(0.03) |  |  |
G161.85-35.75 | -6.91(0.04) | 0.86(0.13) | 2.00(0.90) | 0.20(0.03) |  |  |
G162.46-08.70 | -1.21(0.02) | 0.86(0.06) | 0.99(0.33) | 0.34(0.03) |  |  |
G163.21-08.40 | -2.40(0.05) | 1.21(0.12) |  | 0.10(0.02) |  |  |
G163.32-08.42 | -2.04(0.03) | 0.87(0.06) | 2.91(0.35) | 0.38(0.04) |  |  |
G163.67-08.34 | -2.04(0.06) | 0.92(0.18) |  | 0.24(0.05) |  |  |
G164.94-08.57 | -0.85(0.02) | 0.88(0.04) | 0.88(0.11) | 0.45(0.03) | -0.88(0.11) | 1.04(0.24) | 0.03(0.01)
G165.16-07.55 | -0.83(0.03) | 0.62(0.07) |  | 0.10(0.01) |  |  |
G165.34-07.51a | -1.71(0.06) | 0.47(0.14) |  | 0.04(0.01) |  |  |
G165.34-07.51b | -0.64(0.11) | 1.22(0.30) |  | 0.04(0.01) |  |  |
G165.69-09.14 | -0.82(0.02) | 0.72(0.04) | 2.16(0.38) | 0.47(0.04) |  |  |
G168.00-15.69 | 7.30(0.04) | 0.55(0.09) |  | 0.12(0.02) |  |  |
G168.13-16.39 | 6.26(0.01) | 0.62(0.03) | 1.53(0.22) | 0.51(0.03) | 6.20(0.04) | 0.34(0.08) | 0.07(0.01)
G168.72-15.48 | 7.15(0.02) | 0.60(0.04) | 2.03(0.44) | 0.54(0.04) |  |  |
G168.85-15.83 | 6.29(0.05) | 1.33(0.11) | 1.35(0.47) | 0.16(0.02) |  |  |
G169.32-16.15a | 5.00(0.04) | 0.73(0.11) |  | 0.21(0.03) |  |  |
G169.32-16.15b | 6.77(0.04) | 0.93(0.11) |  | 0.21(0.03) |  |  |
G169.43-16.17 | 5.43(0.03) | 1.29(0.07) | 0.37(0.24) | 0.31(0.03) |  |  |
G169.76-16.15a | 5.25(0.04) | 0.98(0.12) |  | 0.17(0.03) |  |  |
G169.76-16.15b | 6.65(0.03) | 0.72(0.08) |  | 0.22(0.03) |  |  |
G169.84-07.61 | 6.38(0.03) | 0.67(0.06) |  | 0.10(0.01) |  |  |
G169.98-18.97 | 7.52(0.05) | 0.68(0.11) |  | 0.09(0.02) |  |  |
G169.98-04.27 | 7.66(0.02) | 0.76(0.03) | 1.30(0.00) | 0.34(0.02) | 7.69(0.02) | 0.21(0.06) | 0.08(0.01)
G170.00-16.14 | 6.59(0.01) | 0.60(0.03) | 1.13(0.32) | 0.30(0.02) | 6.64(0.05) | 0.31(0.08) | 0.05(0.01)
G170.13-16.06 | 6.78(0.02) | 0.81(0.05) | 1.19(0.35) | 0.43(0.04) |  |  |
G170.26-16.02 | 6.56(0.02) | 0.74(0.04) | 4.01(0.19) | 0.65(0.05) | 6.59(0.03) | 0.39(0.07) | 0.09(0.01)
G170.81-18.34 | 7.87(0.04) | 0.79(0.09) | 3.04(0.98) | 0.07(0.01) |  |  |
G170.88-10.92 | 5.85(0.02) | 0.61(0.04) | 1.43(0.55) | 0.34(0.03) |  |  |
G170.99-15.81 | 6.26(0.04) | 0.90(0.09) | 0.90(0.31) | 0.22(0.03) |  |  |
G171.14-17.58 | 7.37(0.04) | 0.62(0.07) |  | 0.15(0.03) |  |  |
G171.34+02.59 | -19.58(0.06) | 2.36(0.15) | 0.10(0.66) | 0.10(0.01) |  |  |
G171.49-14.90 | 6.40(0.02) | 0.74(0.04) | 4.35(0.13) | 1.04(0.08) | 6.42(0.02) | 0.35(0.04) | 0.14(0.01)
G171.51-10.59 | 5.96(0.02) | 0.67(0.05) | 3.30(0.74) | 0.31(0.03) |  |  |
G171.80-15.32 | 6.75(0.02) | 0.69(0.03) | 3.30(0.22) | 0.69(0.05) | 6.76(0.03) | 0.34(0.06) | 0.08(0.01)
G171.84-05.22 | 6.96(0.02) | 0.65(0.04) | 2.78(0.40) | 0.62(0.05) |  |  |
G172.06-15.21 | 6.57(0.04) | 0.52(0.10) |  | 0.14(0.03) |  |  |
G172.13-16.93 | 7.00(0.02) | 0.67(0.04) | 1.12(0.40) | 0.35(0.03) |  |  |
G172.85+02.27 | -17.67(0.03) | 1.57(0.07) | 0.90(0.12) | 0.22(0.02) | -17.66(0.05) | 1.34(0.12) | 0.08(0.01)
G172.92-16.74 | 4.71(0.13) | 0.96(0.29) |  | 0.03(0.01) |  |  |
G172.94-05.49 | 6.76(0.03) | 0.47(0.06) |  | 0.23(0.03) |  |  |
G173.12-13.32 | 5.15(0.02) | 0.53(0.05) |  | 0.11(0.01) |  |  |
G173.36-16.27 | 6.28(0.02) | 0.70(0.04) | 2.14(0.22) | 0.47(0.03) | 6.32(0.04) | 0.30(0.07) | 0.06(0.01)
G173.45-13.34 | 5.22(0.04) | 0.36(0.07) | 3.64(0.26) | 0.48(0.04) |  |  |
G173.80-15.88 | 5.81(0.02) | 0.70(0.04) | 2.74(0.03) | 0.90(0.06) | 5.88(0.02) | 0.25(0.07) | 0.11(0.01)
G173.89-17.64 | 5.03(0.04) | 0.63(0.07) |  | 0.14(0.02) |  |  |
G173.95-13.74 | 6.43(0.04) | 0.88(0.11) | 1.17(0.68) | 0.19(0.03) |  |  |
G174.06-15.81 | 6.09(0.02) | 0.75(0.04) | 1.83(0.17) | 0.80(0.05) |  |  |
G174.08-13.24 | 5.15(0.02) | 0.70(0.04) | 3.28(0.15) | 0.90(0.06) | 5.18(0.03) | 0.41(0.09) | 0.10(0.01)
G174.22-13.43 | 5.76(0.02) | 1.05(0.05) | 1.10(0.08) | 0.63(0.05) | 6.01(0.04) | 0.24(0.07) | 0.06(0.01)
G174.39-13.43 | 5.62(0.02) | 0.72(0.05) | 0.58(0.39) | 0.34(0.03) |  |  |
G174.44-15.75 | 6.58(0.04) | 1.03(0.09) |  | 0.17(0.02) |  |  |
G174.70-15.48 | 5.82(0.02) | 0.76(0.04) | 1.51(0.14) | 0.58(0.04) | 5.86(0.05) | 0.56(0.13) | 0.05(0.01)
G174.81-15.15 | 5.72(0.03) | 0.61(0.06) |  | 0.15(0.02) |  |  |
G175.49-16.80 | 5.43(0.01) | 0.66(0.03) | 2.48(0.09) | 0.87(0.05) | 5.41(0.02) | 0.31(0.05) | 0.10(0.01)
G177.14-01.21 | -17.32(0.05) | 1.64(0.13) | 0.52(0.27) | 0.12(0.02) |  |  |
G177.86+01.04 | -18.22(0.15) | 1.47(0.36) |  | 0.03(0.01) |  |  |
G177.89-20.16 | 6.88(0.04) | 0.59(0.10) |  | 0.11(0.02) |  |  |
G177.97-09.72 | 7.11(0.02) | 0.79(0.05) | 4.59(0.21) | 0.81(0.07) | 7.09(0.03) | 0.40(0.08) | 0.14(0.03)
G178.28-00.61 | -1.11(0.05) | 0.84(0.13) | 1.99(0.77) | 0.08(0.01) |  |  |
G178.98-06.74 | 7.61(0.02) | 0.66(0.04) | 3.86(0.26) | 0.44(0.03) |  |  |
G180.81-19.66 | 8.74(0.03) | 0.70(0.09) |  | 0.17(0.02) |  |  |
G180.92+04.53 | 1.52(0.03) | 1.02(0.08) | 1.84(0.40) | 0.35(0.04) |  |  |
G181.73-19.35 | 8.67(0.03) | 0.82(0.09) |  | 0.07(0.01) |  |  |
G181.84+00.31 | 2.95(0.02) | 1.05(0.05) | 1.28(0.19) | 0.27(0.02) |  |  |
G182.04+00.41 | 2.50(0.04) | 1.06(0.08) | 0.98(0.42) | 0.09(0.01) |  |  |
G190.17-13.78 | 1.03(0.04) | 0.86(0.11) |  | 0.12(0.02) |  |  |
G191.51-00.76 | 0.08(0.03) | 0.87(0.07) | 0.25(0.39) | 0.09(0.01) |  |  |
G192.12-10.90 | 9.87(0.02) | 0.67(0.05) | 0.10(0.42) | 0.16(0.01) |  |  |
G192.28-11.33 | 9.96(0.04) | 0.88(0.08) | 0.94(0.55) | 0.09(0.01) |  |  |
G192.32-11.87 | 11.98(0.03) | 0.96(0.06) | 1.47(0.26) | 0.39(0.04) |  |  |
Table 2: Continued Name | $V_{\rm LSR}(1,1)$ | $\Delta v(1,1)$ | $\tau(1,1)$ | $T_{\rm MB}(1,1)$ | $V_{\rm LSR}(2,2)$ | $\Delta v(2,2)$ | $T_{\rm MB}(2,2)$
---|---|---|---|---|---|---|---
|  km s-1 |  km s-1 |  | K |  km s-1 |  km s-1 | K
G192.94-03.73 | 4.00(0.05) | 1.36(0.12) |  | 0.05(0.01) |  |  |
G194.80-03.41 | 12.14(0.04) | 1.24(0.10) | 1.25(0.35) | 0.11(0.01) |  |  |
G198.03-15.24 | -0.13(0.03) | 0.94(0.07) | 0.40(0.43) | 0.07(0.01) |  |  |
G198.56-09.10 | 11.25(0.02) | 0.72(0.05) | 1.39(0.44) | 0.41(0.04) |  |  |
G199.88+00.93 | 5.70(0.03) | 0.98(0.07) | 1.42(0.35) | 0.33(0.04) |  |  |
G201.13+00.31 | 4.75(0.04) | 0.90(0.08) | 1.24(0.60) | 0.15(0.02) |  |  |
G201.44+00.65 | 6.32(0.02) | 0.89(0.05) | 1.35(0.25) | 0.30(0.02) | 6.26(0.05) | 0.41(0.14) | 0.05(0.01)
G201.59+00.55a | 3.94(0.05) | 1.21(0.11) | 0.71(0.15) | 0.31(0.03) | 4.28(0.14) | 1.75(0.25) | 0.04(0.01)
G201.59+00.55b | 5.13(0.05) | 0.77(0.10) | 1.42(0.39) | 0.20(0.03) |  |  |
G202.30-08.91 | 11.83(0.02) | 1.16(0.05) | 0.55(0.10) | 0.24(0.02) | 12.07(0.07) | 0.73(0.14) | 0.03(0.01)
G203.20-11.20 | 10.35(0.02) | 1.09(0.05) | 1.40(0.10) | 0.41(0.03) | 10.61(0.13) | 0.66(0.45) | 0.04(0.01)
G203.75-08.49 | 11.57(0.04) | 0.64(0.09) |  | 0.06(0.01) |  |  |
G204.82-13.88 | 8.06(0.04) | 1.13(0.12) | 0.30(0.42) | 0.17(0.02) |  |  |
G205.57-08.25 | 11.47(0.04) | 0.66(0.09) |  | 0.06(0.01) |  |  |
G206.10-15.77 | 9.09(0.02) | 0.67(0.04) | 2.64(0.20) | 0.64(0.05) | 9.13(0.02) | 0.43(0.05) | 0.11(0.01)
G206.60-14.40 | 3.95(0.05) | 1.44(0.12) | 0.51(0.36) | 0.08(0.01) |  |  |
G208.56+02.36 | 9.20(0.05) | 0.88(0.13) |  | 0.06(0.01) |  |  |
G209.28-19.62a | 7.57(0.16) | 1.71(0.30) | 0.24(0.20) | 0.20(0.03) |  |  |
G209.28-19.62b | 8.92(0.05) | 0.98(0.11) |  | 0.32(0.03) | 8.29(0.10) | 1.34(0.23) | 0.06(0.01)
G211.48-19.27 | 3.79(0.04) | 1.61(0.09) | 0.95(0.14) | 0.34(0.04) | 3.66(0.07) | 0.99(0.17) | 0.06(0.01)
G212.10-19.15 | 4.30(0.02) | 1.04(0.06) | 1.52(0.10) | 0.54(0.04) | 4.24(0.09) | 1.26(0.18) | 0.04(0.01)
G214.21-13.40 | 11.95(0.03) | 0.85(0.08) | 0.10(1.19) | 0.21(0.02) |  |  |
G214.43-19.90 | 2.76(0.03) | 0.97(0.07) | 0.66(0.35) | 0.26(0.03) |  |  |
G216.51-13.88 | 9.86(0.04) | 0.78(0.09) | 2.97(0.92) | 0.15(0.02) |  |  |
G217.13-12.54 | 11.53(0.03) | 0.64(0.05) |  | 0.10(0.01) |  |  |
G219.24-10.02 | 12.28(0.03) | 0.73(0.08) |  | 0.12(0.02) |  |  |
G220.67-01.86 | 12.08(0.03) | 1.11(0.07) | 1.22(0.26) | 0.28(0.03) |  |  |
G222.23+01.21 | 28.44(0.05) | 1.09(0.13) | 1.31(0.60) | 0.06(0.01) |  |  |
G224.27-00.82 | 14.10(0.03) | 1.44(0.07) | 1.61(0.09) | 0.57(0.05) | 14.19(0.05) | 1.32(0.12) | 0.08(0.01)
G224.47-00.65 | 15.57(0.02) | 1.22(0.07) | 0.93(0.11) | 0.44(0.04) | 15.45(0.05) | 0.70(0.12) | 0.07(0.01)
G238.71-01.47 | 19.25(0.06) | 1.65(0.13) | 0.97(0.38) | 0.10(0.01) |  |  |
G353.49+15.57 | 4.13(0.02) | 0.80(0.03) | 1.47(0.08) | 1.04(0.06) | 4.12(0.02) | 0.66(0.05) | 0.20(0.02)