# The Difference in abundances between N-bearing and O-bearing Species in High-Mass Star-Forming Regions

Taiki Suzuki, Masatoshi Ohishi, Masao Saito, Tomoya Hirota, Liton

Majumdar, Valentine Wakelam

► To cite this version:

Taiki Suzuki, Masatoshi Ohishi, Masao Saito, Tomoya Hirota, Liton Majumdar, et al.. The Difference in abundances between N-bearing and O-bearing Species in High-Mass Star-Forming Regions. The Astrophysical Journal, 2018, 237 (1), pp.id. 3. 10.3847/1538-4365/aac8db. hal-01685065

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# The Difference in Abundance between N-bearing and O-bearing Species in High-mass Star-forming Regions

Taiki Suzuki¹,², Masatoshi Ohishi¹,³, Masao Saito¹,³, Tomoya Hirota¹,³, Liton Majumdar⁴, and Valentine Wakelam⁵

¹Department of Astronomy, the Graduate University for Advanced Studies (SOKENDAI), Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan; taiki.suzuki@nao.ac.jp
²Astrobiology Center, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan

³National Astronomical Observatory of Japan, Osawa 2-21-1, Mitaka, Tokyo 181-8588, Japan

⁴Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA; liton.majumdar@jpl.nasa.gov

⁵Laboratoire d'Astrophysique de Bordeaux, Univ. Bordeaux, CNRS, B18N, allée Geoffroy Saint-Hilaire, F-33615 Pessac, France

Received 2017 November 17; revised 2018 May 25; accepted 2018 May 26; published 2018 July 3

## Abstract

The different spatial distributions of N-bearing and O-bearing species, as are well known toward Orion KL, is a longstanding mystery. We conducted a survey observation and chemical modeling study to investigate if the different distributions of O- and N-bearing species are widely recognized in general star-forming regions. First, we report our observational results of complex organic molecules (COMs) with the 45 m radio telescope at the Nobeyama Radio Observatory toward eight star-forming regions. Through our spectral survey ranging from 80 to 108 GHz, we detected CH₃OH, HCOOCH₃, CH₃OCH₃, (CH₃)₂CO, CH₃CHO, CH₃CH₂CN, CH₂CHCN, and NH₂CHO. Their molecular abundances were derived via the rotation diagram and the least squares methods. We found that N-bearing molecules tend to show stronger correlations with other N-bearing molecules rather than O-bearing molecules. While G10.47+0.03 showed high fractional abundances of N-bearing species, those in NGC 6334F were not so rich, being less than 0.01 compared to CH₃OH. Then the molecular abundances toward these sources were evaluated by chemical modeling with the NAUTILUS three-phase gas-grain chemical code. Based on the simulations of time evolution for the abundance of COMs, we suggest that the observed correlations of fractional abundances between COMs can be explained by a combination of different temperature structures inside the hot cores and the different evolutionary phases. Since our modeling could not fully explain the observed excitation temperatures, it is important to investigate the efficiency of grain surface reactions and their activation barriers and the binding energy of COMs to further promote our understanding.

**Key words:** ISM: abundances – ISM: clouds – ISM: molecules – line: identification – methods: numerical – methods: observational

## 1. Introduction

In the interstellar medium (ISM), almost 200 molecules (as listed by CDMS<fnref n="6" />) ranging from simple linear molecules to complex organic molecules (COMs) have been detected, mainly toward dark clouds and low-mass and high-mass star-forming regions. While relatively simple species have been a prime target for previous astronomical studies, the study of the interstellar chemistry of COMs is still limited and has a lot of room for debate.

Among COMs, methanol (CH₃OH), dimethyl ether (CH₃OCH₃), and methyl formate (HCOOCH₃) have been detected toward various sources. Since the first detection by Ball et al. (1970), CH₃OH was detected toward various high-mass and low-mass star-forming regions and circumstellar shells. HCOOCH₃ was first detected by Brown et al. (1975), and then HCOOCH₃ was reported toward several star-forming regions (e.g., Bisschop et al. 2007). Since the first detection by Snyder et al. (1974), CH₃OCH₃ is known as one of the abundant species in hot cores (Ikeda et al. 2001) and hot corinos such as IRAS 16293-2422 (Cazaux et al. 2003; Bottinelli et al. 2004). N-bearing COMs have been less studied compared to these O-bearing species. Well-known N-bearing species are vinyl cyanide (CH₂CHCN) and ethyl cyanide (CH₃CH₂CN), which have been detected toward Sgr B2, Orion KL, and other star-forming regions (e.g., Gardner &

Winnewisser 1975; Johnson et al. 1977). Recently, our group has successfully detected CH₂NH and CH₃NH₂ toward several star-forming regions (Suzuki et al. 2016, M. Ohishi et al. 2017, in preparation).

However, the overall picture of COM evolution along with star formation is still under debate. The correlations of molecular abundances among certain species would be a good clue to connect the evolution of COMs and the physical condition of hot cores. Such molecular correlation has been discussed for Orion KL. Blake et al. (1987) claimed that O- and N-bearing species had different radial velocities. Recent interferometric observations enabled us to see the different spatial distributions of COMs directly (e.g., Friedel & Snyder 2008; Peng et al. 2013), giving us direct evidence that O-bearing species are enhanced in the Orion Compact Ridge and N-bearing species are rich in the Orion Hot Core. Caselli et al. (1993) discussed the origin of chemical differences in the Hot Core and Compact Ridge by chemical modeling studies. They claimed that the different chemistries would be due to the efficiency of thermal evaporation before the warm-up of the cores, assuming that the initial temperature of the Hot Core (40 K) would be hotter than that of the Compact Ridge (20 K). They reported that H₂CO was more efficiently converted to CH₃OH in the Compact Ridge than in the Hot Core, resulting in an increase of not only CH₃OH but also CH₃OCH₃ and HCOOCH₃, through the formation of CH₃OCH₃ and HCOOCH₃ via gas-phase reactions using CH₃OH. Their result also suggests that the difference in molecular abundances is

<footnote n="6">⁶ https://www.astro.uni-koeln.de/cdms/molecules</footnote>
<figure><img src="image_3.png" /><figcaption>**Figure 1.** Observed frequency ranges for our sources are shown in black.</figcaption></figure>

caused by their chemical connections, but strongly enhanced by the source properties.

Since the chemical differences in hot cores would be key to improving our knowledge of the chemical evolution of COMs, it would be quite important to know if such correlations of molecular abundances are ubiquitous phenomena or limited to only special sources. The first survey of O- and N-bearing COMs, CH<sub>2</sub>CHCN, CH<sub>3</sub>CH<sub>2</sub>CN, and CH<sub>3</sub>OCH<sub>3</sub>, was conducted by Fontani et al. (2007), reporting the correlation of not only “CH<sub>2</sub>CHCN and CH<sub>3</sub>CH<sub>2</sub>CN,” but also “CH<sub>2</sub>CHCN and CH<sub>3</sub>OCH<sub>3</sub>” and “CH<sub>3</sub>CH<sub>2</sub>CN and CH<sub>3</sub>OCH<sub>3</sub>.” They reported the correlations of molecular abundances of O- and N-bearing species. Clear evidence of different spatial distributions between O- and N- bearing species was not obtained. In this paper, we will present the results of our single-dish survey observations of COMs toward high-mass star-forming regions, with a larger number of COMs than used by Fontani et al. (2007). Since we could not obtain the spatial distributions of COMs, we use the radial velocities to discuss if molecules coexist. Then we will investigate if the differences in molecular abundances of O- and N-bearing species are widely recognized. Furthermore, we will discuss the connection between molecular correlation and the key physical conditions of sources using our state-of-the-art chemical model. As a result, we will report that not only the connection of chemical reactions but also the degree of absorption onto grains determined by gas temperature may strongly affect the molecular abundances. The observational method will be described in Section 2, and our results will be described in Section 3. We will compare the modeling results and the observed abundances in Section 4. We will summarize our work in Section 5.

## 2. Observations

In this paper, we report the observational results for well-known COMs in hot cores: CH<sub>3</sub>OH, CH<sub>3</sub>OCH<sub>3</sub>, (CH<sub>3</sub>)<sub>2</sub>CO, CH<sub>3</sub>CHO, NH<sub>2</sub>CHO, CH<sub>2</sub>CHCN, and CH<sub>3</sub>CH<sub>2</sub>CN. We conducted survey observations of COMs with the 45 m radio telescope at the Nobeyama Radio Observatory (NRO), National Astronomical Observatory of Japan. Our data were simultaneously obtained with our previous observations aimed at detecting CH<sub>2</sub>NH and CH<sub>3</sub>NH<sub>2</sub> (Suzuki et al. 2016; M. Ohishi et al. 2018, in preparation), from 2013 March to 2014 May. We used the TZ receiver (Nakajima et al. 2013) in the dual polarization mode to obtain spectra between 78.8 and 108.4 GHz. Since the molecular line data in this paper were side products of our previous surveys, our observed frequency ranges did not entirely cover this frequency range and differ from source to source. The observed frequency ranges for each source are shown in black in Figure 1, and the actual values are

summarized in Table 1. We note that the observed frequency ranges are limited for DR21(OH) and G19.61–0.23, where a CH<sub>3</sub>NH<sub>2</sub> survey was not conducted.

The SAM45 spectrometer was used for the back end with a frequency resolution of 122 kHz, corresponding to a velocity resolution of 0.35 km s<sup>-1</sup> at 105 GHz but 0.46 km s<sup>-1</sup> at 79 GHz. The system temperatures ranged from 150 to 300 K. The main beam efficiency (η<sub>mb</sub>) was 0.37 for more than 90 GHz and 0.41 for less than 90 GHz, and the beam size (FWHM) was linearly decreased from 20''/6 at 80'' to 15''/5 at 106 GHz. Observations were performed in the position switching mode. The pointing accuracy was checked by observing nearby SiO masers, and the pointing error was typically 5'', but 10'' under windy conditions.

Our targets were eight hot core sources: G10.47+0.03, G31.41+0.3, Orion KL, NGC 6334F, G34.3+0.2, W51 e1/e2, G19.61–0.23, and DR21 (OH), where we detected CH<sub>2</sub>NH (Suzuki et al. 2016). Suzuki et al. (2016) conducted a survey observation of CH<sub>2</sub>NH toward hot core sources, where CH<sub>3</sub>OH was known to be rich. Since CH<sub>3</sub>OH is known to be formed via hydrogenation processes on grains, CH<sub>3</sub>OH would be a good indicator for other grain surface reactions, which would form various COMs. The most abundant CH<sub>2</sub>NH source in this survey was G10.47+0.03, with its fractional abundance compared to H<sub>2</sub> molecules of 3.1 × 10<sup>-8</sup>. The abundances of CH<sub>2</sub>NH were almost 10 times less than G10.47+0.03 in W51 e1/e2, NGC 6334F, and G19.61–0.23, where CH<sub>2</sub>NH abundances were, respectively, 2.8 × 10<sup>-9</sup>, 2.4 × 10<sup>-9</sup>, and 1.4 × 10<sup>-9</sup>. The different fractional abundances of CH<sub>2</sub>NH indicate that other N-bearing species may be enhanced in these sources, as is known in the Orion KL Hot Core and Compact Ridge. The observed sources and their properties are summarized in Table 2.

## 3. Results

### 3.1. Observed Spectra

In our survey, we detected more than 1000 molecular lines of CH<sub>3</sub>OH, CH<sub>3</sub>OCH<sub>3</sub>, HCOOCH<sub>3</sub>, CH<sub>3</sub>CHO, (CH<sub>3</sub>)<sub>2</sub>CO, NH<sub>2</sub>CHO, CH<sub>2</sub>CHCN, and CH<sub>3</sub>CH<sub>2</sub>CN. The rms noise levels per channel ranged from 5 to ~20 mK, depending on the source and the frequency. This difference is due to the system temperature and the condition of the TZ receiver. The rms noise levels are sometimes different from source to source due to our original purpose of detecting CH<sub>2</sub>NH and CH<sub>3</sub>NH<sub>2</sub> and the strategy to achieve it.

An example of the observed spectra for all sources from 105.6 to 105.9 GHz is shown in Figure 2. Although the observed frequency ranges are different from source to source
<table><caption>**Table 1**
Observed Frequency Range</caption><thead><tr><th>Source</th><th>From (GHz)</th><th>To (GHz)</th></tr></thead><tbody><tr><td rowspan="12">Orion KL</td><td>78.80</td><td>79.80</td></tr><tr><td>80.75</td><td>81.95</td></tr><tr><td>83.70</td><td>85.00</td></tr><tr><td>85.70</td><td>86.20</td></tr><tr><td>86.50</td><td>87.00</td></tr><tr><td>87.50</td><td>88.00</td></tr><tr><td>88.20</td><td>88.70</td></tr><tr><td>88.80</td><td>91.05</td></tr><tr><td>91.45</td><td>91.95</td></tr><tr><td>92.40</td><td>93.45</td></tr><tr><td>93.65</td><td>95.20</td></tr><tr><td>95.75</td><td>97.25</td></tr><tr><td>99.05</td><td>99.85</td></tr><tr><td>100.25</td><td>101.25</td></tr><tr><td>101.75</td><td>102.25</td></tr><tr><td>103.00</td><td>104.00</td></tr><tr><td>105.40</td><td>105.90</td></tr><tr><td>106.85</td><td>107.85</td></tr><tr><td>108.15</td><td>108.65</td></tr><tr><td rowspan="12">NGC 6334F</td><td>78.80</td><td>79.80</td></tr><tr><td>80.50</td><td>81.95</td></tr><tr><td>83.70</td><td>85.00</td></tr><tr><td>85.50</td><td>87.00</td></tr><tr><td>87.50</td><td>88.75</td></tr><tr><td>88.80</td><td>91.05</td></tr><tr><td>91.45</td><td>91.95</td></tr><tr><td>92.40</td><td>93.45</td></tr><tr><td>93.65</td><td>95.20</td></tr><tr><td>95.75</td><td>97.25</td></tr><tr><td>98.25</td><td>98.75</td></tr><tr><td>99.05</td><td>100.20</td></tr><tr><td>100.25</td><td>101.25</td></tr><tr><td>101.75</td><td>102.25</td></tr><tr><td>103.00</td><td>104.00</td></tr><tr><td>105.40</td><td>105.90</td></tr><tr><td>106.85</td><td>107.85</td></tr><tr><td>108.40</td><td>108.65</td></tr><tr><td rowspan="12">G10.47+0.03</td><td>78.80</td><td>79.80</td></tr><tr><td>80.80</td><td>81.70</td></tr><tr><td>83.70</td><td>85.00</td></tr><tr><td>85.70</td><td>86.20</td></tr><tr><td>86.50</td><td>87.00</td></tr><tr><td>87.50</td><td>88.00</td></tr><tr><td>88.80</td><td>89.70</td></tr><tr><td>89.05</td><td>89.30</td></tr><tr><td>89.20</td><td>89.45</td></tr><tr><td>90.05</td><td>91.05</td></tr><tr><td>92.45</td><td>93.45</td></tr><tr><td>94.00</td><td>94.50</td></tr><tr><td>95.75</td><td>97.25</td></tr><tr><td>99.05</td><td>99.85</td></tr><tr><td>100.25</td><td>101.25</td></tr><tr><td>103.00</td><td>104.30</td></tr><tr><td>104.50</td><td>106.80</td></tr><tr><td rowspan="12">G19.61-0.23<br>G31.41+0.3</td><td>103.00</td><td>106.80</td></tr><tr><td>78.80</td><td>79.80</td></tr><tr><td>80.80</td><td>81.70</td></tr><tr><td>83.70</td><td>85.00</td></tr><tr><td>85.70</td><td>86.20</td></tr><tr><td>86.50</td><td>87.00</td></tr><tr><td>87.50</td><td>88.00</td></tr><tr><td>88.80</td><td>89.70</td></tr><tr><td>90.05</td><td>91.05</td></tr><tr><td>92.45</td><td>93.45</td></tr></tbody></table>

<table><caption>**Table 1**
(Continued)</caption><thead><tr><th>Source</th><th>From (GHz)</th><th>To (GHz)</th></tr></thead><tbody><tr><td rowspan="12">G34.3+0.2</td><td>94.00</td><td>94.50</td></tr><tr><td>95.75</td><td>97.25</td></tr><tr><td>99.05</td><td>99.85</td></tr><tr><td>100.25</td><td>101.25</td></tr><tr><td>103.00</td><td>104.30</td></tr><tr><td>104.50</td><td>106.80</td></tr><tr><td>78.80</td><td>79.80</td></tr><tr><td>80.50</td><td>81.00</td></tr><tr><td>81.45</td><td>81.95</td></tr><tr><td>85.50</td><td>86.50</td></tr><tr><td>87.75</td><td>88.75</td></tr><tr><td>89.50</td><td>91.00</td></tr><tr><td>91.45</td><td>91.95</td></tr><tr><td>92.40</td><td>93.40</td></tr><tr><td>93.65</td><td>94.15</td></tr><tr><td>94.20</td><td>95.20</td></tr><tr><td>98.25</td><td>98.75</td></tr><tr><td>99.20</td><td>100.20</td></tr><tr><td>100.40</td><td>101.25</td></tr><tr><td>101.75</td><td>102.25</td></tr><tr><td>103.00</td><td>104.00</td></tr><tr><td>105.40</td><td>105.90</td></tr><tr><td>106.85</td><td>107.85</td></tr><tr><td>108.40</td><td>108.65</td></tr><tr><td rowspan="12">W51 e1/e2</td><td>78.80</td><td>79.80</td></tr><tr><td>80.50</td><td>81.95</td></tr><tr><td>83.70</td><td>85.00</td></tr><tr><td>85.50</td><td>87.00</td></tr><tr><td>87.50</td><td>88.75</td></tr><tr><td>88.80</td><td>91.05</td></tr><tr><td>91.45</td><td>91.95</td></tr><tr><td>92.40</td><td>93.45</td></tr><tr><td>93.65</td><td>95.20</td></tr><tr><td>95.75</td><td>97.25</td></tr><tr><td>98.25</td><td>98.75</td></tr><tr><td>99.05</td><td>100.20</td></tr><tr><td>100.25</td><td>101.25</td></tr><tr><td>101.75</td><td>102.25</td></tr><tr><td>103.00</td><td>104.00</td></tr><tr><td>105.40</td><td>105.90</td></tr><tr><td>106.85</td><td>107.85</td></tr><tr><td>108.40</td><td>108.65</td></tr><tr><td rowspan="12">DR21 (OH)</td><td>103.00</td><td>106.80</td></tr></tbody></table>

(Figure 1), this frequency range enables us to compare the spectra for all observed sources. These species are well known in hot cores, and most of the detections were also supported by many authors through radio observations (see, for example, Ikeda et al. 2001; Zernickel et al. 2012; Widicus Weaver et al. 2017). The detailed line parameters, such as radial velocities and line widths, were obtained by the task “Gaussian fitting” with “NEWSTAR,”<fnref n="7" /> which was developed by NRO. As the results of this procedure, our molecular lines were relatively well fitted unless they are blended with other transitions. These line parameters will be described in a subsequent section for each source. All of the observed lines are summarized in the Appendix.

<footnote n="7">⁷ http://www.nro.nao.ac.jp/~nro45mrt/html/obs/newstar/</footnote>
<table><caption>**Table 2**
List of Observed Sources</caption><thead><tr><th>Source</th><th>α(J2000)<br>h m s</th><th>δ(J2000)<br>°/"</th><th>V<sub>LSR</sub><br>(km s<sup>-1</sup>)</th><th>Distance<br>(kpc)</th><th>χ[CH<sub>2</sub>NH]<br>(×10<sup>-8</sup>)</th><th>Reference</th></tr></thead><tbody><tr><td>Orion KL</td><td>05 35 14.5</td><td>-05 22 30.6</td><td>6</td><td>0.4</td><td>3.3</td><td>1, 2</td></tr><tr><td>NGC 6334F</td><td>17 20 53.4</td><td>-35 47 1.0</td><td>-7</td><td>1.3</td><td>0.24</td><td>1, 3</td></tr><tr><td>G10.47+0.03</td><td>18 08 38.13</td><td>-19 51 49.4</td><td>68</td><td>8.5</td><td>3.1</td><td>1, 3</td></tr><tr><td>G19.61-0.23</td><td>18 27 38.0</td><td>-11 56 42</td><td>41.9</td><td>4.0</td><td>0.14</td><td>1, 4</td></tr><tr><td>G31.41+0.3</td><td>18 47 34.6</td><td>-01 12 43</td><td>97</td><td>7.9</td><td>0.88</td><td>1, 5</td></tr><tr><td>G34.3+0.2</td><td>18 53 18.54</td><td>+01 14 57.0</td><td>58</td><td>1.6</td><td>0.24</td><td>1, 3</td></tr><tr><td>W51 e1/e2</td><td>19 23 43.77</td><td>+14 30 25.9</td><td>57</td><td>5.4</td><td>0.28</td><td>1, 3</td></tr><tr><td>DR21 (OH)</td><td>20 39 01.1</td><td>+42 22 50.2</td><td>-3</td><td>1.5</td><td>0.14</td><td>1, 3</td></tr></tbody></table>

**Note.** The coordinate, radial velocity, and the distance to sources are summarized. The fractional abundance of CH₂NH compared to hydrogen reported in Suzuki et al. (2016) is also shown.

**References.** (1) Ikeda et al. (2001), (2) Menten et al. (2007), (3) Reid et al. (2014), (4) Hofner & Churchwell (1996), (5) Churchwell et al. (1990).

## 3.2. Derivation of Abundance

Here we will describe the methodologies used to derive fractional abundances of COMs. In sources where enough transitions were available, we calculated column densities ($N_{rot}$) of COMs using the rotation diagram method described in Turner (1991), and the following equation was employed:

$$ \log \frac{3kW}{8\pi^3\nu\mu^2Sg_1g_K} = \log \frac{N_{rot}}{Q(T_{rot})} - \frac{E_u}{k} \frac{\log e}{T_{rot}} \quad (1) $$

where W is the integrated intensity, S is the intrinsic line strength, d is the permanent electric dipole moment, $g_1$ and $g_K$ are the nuclear spin degeneracy and the K-level degeneracy, respectively, N is the column density, $Q_{rot}$ is the rotational partition function, $E_u$ is the upper level energy, and $T_{rot}$ is the rotation temperature. The column density is derived from the intercept of a diagram, and its slope will give us the excitation temperature. In this derivation, a source size of 10'' was assumed. As an example, the rotation diagrams of G10.47 +0.03 and NGC 6334F are shown in Figures 3 and 4.

The rotation diagram method assumes that observed transitions are optically thin, but this assumption is not always correct. Also, the source size may have a large uncertainty. A more accurate way to derive abundances is to use the least squares fitting method with the equations of the radiative transfer model described in Suzuki et al. (1992). This method does not require the assumption of an optically thin property of the observed transitions, but assumes a local thermal equilibrium (LTE) condition. As we will show below, the observed transitions are well explained by this method, suggesting this assumption is not so bad. In our calculation, we also assumed the effect of the source size, which leads to the beam dilution. Then, if the column density and excitation temperature are given, the brightness temperature can be calculated with the following formula:

$$ T_B = (J(T_{ex}) - J(T_{bb}))(1 - \exp(-\tau))\eta_{mb}\left(\frac{\Theta_{Source}}{\Theta_{beam}}\right)^2, \quad (2) $$

where

$$ J(T) = \frac{h\nu}{k} \frac{1}{\exp\left(\frac{h\nu}{kT}\right) - 1} \quad (3) $$

$$ \tau = 1.248 \times 10^{-13} \left(\frac{\mu}{D}\right)^2 S \left(\frac{N_{rot}}{\text{cm}^{-2}}\right) \left(\frac{\Delta\nu}{\text{km s}^{-1}}\right)^{-1} \frac{f(T, E_u)}{Q(T_{ex})} \quad (4) $$

$$ f(T, E_u) = \exp\left(\frac{h\nu}{kT} - 1\right) \times \exp(-E_u/kT). \quad (5) $$

Here, $T_{bb}$ is the brightness temperature of the cosmic background radiation (2.7 K), $\eta_{mb}$ is the main beam efficiency, $\Theta_{Source}$ is the source size, and $\Theta_{beam}$ is the beam size.

Thus, if more than three transitions are available, the best-estimated source size, the column density, and the excitation temperatures, which make the $\chi^2$ minimum, can be derived utilizing the Marquard method:

$$ \chi^2(N, T, \Theta) = \sum_i (Ta^*(i) - T_{calc}(N, T, \Theta, i))^2. \quad (6) $$

Here, i represents the number of observed transitions. In this method, $T_{calc}(N, T, \Theta, i)$ is the theoretically predicted brightness temperature of a certain transition number i via Equation (2), under a given column density N, excitation temperature $T_{ex}$, and source size $\Theta$. In Equation (6), squares of subtractions of observed $Ta^*(i)$ values from corresponding predicted $T_{calc}(N, T, \Theta, i)$ values are calculated for all i, and $\chi^2(N, T, \Theta)$ is given as their sum. The initial column density and the excitation temperature are assumed from the rotation diagram method. The initial column density for the Marquard method was given by multiplying the factor $(\frac{10''}{\Theta_{continuum}})^2$ by $N_{rot}$, where $\Theta_{continuum}$ is the size of the continuum emission:

$$ N_{initial} = N_{rot} \times \left( \frac{10''}{\Theta_{continuum}} \right)^2. \quad (7) $$

## 3.3. Observational Results and Obtained Abundances for Each Source

Our results can be found in Tables 3 and 4 for (1) the rotational diagram method assuming a source size of 10'' and (2) using the $\chi^2$ method with a variable source size. Although the value for source size of 10'' is quite uncertain, estimating the fractional abundance assuming a 10'' source size and a H₂ column density from CO would be one good route (Suzuki et al. 2016). The column densities and the excitation temperatures were used as the initial values in the analysis of the least squares method. We note that, if available, the source sizes derived in the least squares method would be better. With
<figure><img src="image_4.png" /></figure>

<figure><img src="image_5.png" /></figure>

<figure><img src="image_6.png" /><figcaption>**Figure 2.** (a) Observed spectra for all sources are compared from 105.6 to 105.9 GHz. Besides CH<sub>2</sub>NH analyzed in Suzuki et al. (2016), CH<sub>3</sub>OCH<sub>3</sub> transitions are detected. (b) Observed spectra for all sources are compared from 84.3 to 84.6 GHz. CH<sub>3</sub>OH, HCOOCH<sub>3</sub>, and NH<sub>2</sub>CHO are detected. This frequency was not observed for G19.61−0.23, G34.3+0.2, and DR21(OH). (c) Observed spectra for all sources are compared from 86.74 to 87 GHz. CH<sub>3</sub>OH, CH<sub>2</sub>CHCN, and CH<sub>3</sub>CH<sub>2</sub>CN are detected. This frequency was not observed for G19.61−0.23, G34.3+0.2, and DR21(OH).</figcaption></figure>

the error propagation from rms noise level for the observed transitions, we calculated the error of column densities at the 1σ level. In addition, we added the additional error of 15% compared to the main value as the calibration error when the transitions were obtained from the different setup. With the least squares method, the source sizes were always smaller than 10". We will refer to this as the compact source case. If the numbers of detected lines were small, we fixed the source size or the excitation temperatures. We summarize these exceptions, line properties for individual sources, and a comparison with previous studies in subsequent sections.

The typical excitation temperature for CH<sub>3</sub>CHO was ~17 K, suggesting that CH<sub>3</sub>CHO would exist in the envelopes. These low excitation temperatures of CH<sub>3</sub>CHO agree with the result from Ikeda et al. (2001). Therefore, we will exclude CH<sub>3</sub>CHO in the subsequent discussion for hot cores. The averages of fractional abundances for the compact source sizes were 9.8 × 10<sup>-7</sup>, 3.6 × 10<sup>-7</sup>, 4.3 × 10<sup>-8</sup>, and 2.2 × 10<sup>-9</sup> for CH<sub>3</sub>OH, HCOOCH<sub>3</sub>, CH<sub>3</sub>OCH<sub>3</sub>, and CH<sub>3</sub>CHO. Their dispersions were 6.3 × 10<sup>-7</sup>, 3.3 × 10<sup>-7</sup>, 2.7 × 10<sup>-8</sup>, and 8.8 × 10<sup>-10</sup>, respectively, which were lower than their average fractional abundances. On the other hand, the averages of fractional abundances for the compact source sizes were 1.1 × 10<sup>-8</sup>, 4.0 × 10<sup>-8</sup>, and 1.6 × 10<sup>-8</sup> for NH<sub>2</sub>CHO, CH<sub>2</sub>CHCN, and CH<sub>3</sub>CH<sub>2</sub>CN. Their dispersions of fractional abundances, 2.1 × 10<sup>-8</sup>, 5.6 × 10<sup>-8</sup>, and 2.5 × 10<sup>-8</sup>, respectively, were larger than their main values of fractional abundances. Hence, N-bearing molecules tend to show a wider range of fractional abundances than O-bearing molecules, suggesting that abundances of N-bearing molecules would be more affected by the physical conditions of the sources.

In Table 5, we summarize the correlation coefficients between the observed abundances of COMs based on Table 4. We added CH<sub>2</sub>NH abundances from Suzuki et al. (2016) in this table. The correlation coefficients of “CH<sub>3</sub>OH and CH<sub>3</sub>OCH<sub>3</sub>,” “NH<sub>2</sub>CHO and CH<sub>3</sub>CH<sub>2</sub>CN,” and “CH<sub>2</sub>CHCN and CH<sub>2</sub>NH” were higher than 0.7, suggesting a strong positive correlation. In addition, observed N-bearing molecules tended to have larger correlation coefficients with other N-bearing molecules, rather than with O-bearing molecules. The correlation coefficients between N-bearing species and O-bearing species were usually less than 0.2 and sometimes even negative, although the correlation coefficient of “CH<sub>3</sub>OH and CH<sub>2</sub>CHCN” has an exceptionally high value of 0.51. (CH<sub>3</sub>)<sub>2</sub>CO was a unique molecule that showed higher correlation coefficients with CH<sub>3</sub>OH, HCOOCH<sub>3</sub>, CH<sub>3</sub>CH<sub>2</sub>N, CH<sub>2</sub>CHCN, and CH<sub>2</sub>NH.

Since our source number is small, it is essential to find the probability that our correlation coefficients are identical to those of the parent population, that is, the general star-forming region. The *t*-test, described in detail in Section 2.2 of Wall (1996), is a powerful tool to evaluate if the derived correlation coefficients represent that of the parent population. We performed the *t*-test to see the significance of these correlation coefficients. With a correlation coefficient, *r*, it is known that a parameter of *t* = $\frac{r\sqrt{n-2}}{\sqrt{1-r^2}}$ obeys a *t* distribution. We summarize this value in Table 6. In the *t*-test, the value of *t* represents the probability that the correlation coefficients of our sample are the same as those of the parent population. This probability also depends on the degree of freedom of the *t* distribution, *n* − 2, with *n* being the number of sources where molecules were detected. In this work, *n* is six for CH<sub>3</sub>OH, NH<sub>2</sub>OH, CH<sub>3</sub>CH<sub>2</sub>CN, and CH<sub>2</sub>NH and seven for the other sources. Then the significance level of the correlation
<figure><img src="image_7.png" /><figcaption>**Figure 3.** Rotation diagrams for G10.47+0.03.</figcaption></figure>
<figure><img src="image_8.png" /><figcaption>Figure 4. Rotation diagrams for NGC 6334F.</figcaption></figure>
<table><caption>**Table 3**
Abundances Assuming 10" Source Size</caption><thead><tr><th>Source</th><th>N[H<sub>2</sub>]<br>(10<sup>23</sup> cm<sup>-2</sup>)</th><th>Species</th><th>N<br>(cm<sup>-2</sup>)</th><th>Tex<br>(K)</th><th>X</th></tr></thead><tbody><tr><td rowspan="10">G10.47+0.03</td><td rowspan="10">1.3</td><td>CH<sub>3</sub>OH</td><td>2.7 ± 0.8 (17)</td><td>185 ± 20</td><td>2.1 ± 0.6 (-6)</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>7.1 ± 2.9 (15)</td><td>60 ± 39</td><td>5.5 ± 2.2 (-8)</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>3.0 ± 0.9 (15)</td><td>119 ± 14</td><td>2.3 ± 0.7 (-8)</td></tr><tr><td>CH<sub>3</sub>CHO</td><td>3.0 ± 1.4 (14)</td><td>10 ± 2</td><td>2.3 ± 1.1 (-9)</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>1.9 ± 29.0 (15)</td><td>119 ± 58</td><td>1.5 ± 22.4 (-8)</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>2.3 ± 0.6 (16)</td><td>398 ± 209</td><td>1.8 ± 0.5 (-7)</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>6.2 ± 1.4 (15)</td><td>382 ± 104</td><td>4.8 ± 1.1 (-8)</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>1.3 ± 0.4 (16)</td><td>[71]</td><td>1.0 ± 0.3 (-7)</td></tr><tr><td>Orion KL</td><td>1.0</td><td>CH<sub>3</sub>OH</td><td>4.1 ± 0.9 (17)</td><td>183 ± 10</td><td>4.1 ± 0.9 (-6)</td></tr><tr><td rowspan="10">NGC 6334F</td><td rowspan="10">2.0</td><td>HCOOCH<sub>3</sub></td><td>3.4 ± 2.5 (16)</td><td>80 ± 43</td><td>3.4 ± 2.5 (-7)</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>1.7 ± 0.4 (16)</td><td>91 ± 7</td><td>1.7 ± 0.4 (-7)</td></tr><tr><td>CH<sub>3</sub>CHO</td><td>1.5 ± 0.3 (14)</td><td>19 ± 4</td><td>1.5 ± 0.3 (-9)</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>3.6 ± 2.6 (14)</td><td>[100]</td><td>3.6 ± 2.6 (-9)</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>9.9 ± 2.7 (15)</td><td>146 ± 28</td><td>9.9 ± 2.7 (-8)</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>1.0 ± 0.2 (15)</td><td>97 ± 7</td><td>1.0 ± 0.2 (-8)</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>1.3 ± 1.0 (16)</td><td>[100]</td><td>1.3 ± 1.0 (-7)</td></tr><tr><td>CH<sub>3</sub>OH</td><td>3.1 ± 1.0 (17)</td><td>201 ± 24</td><td>1.6 ± 0.5 (-6)</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>1.5 ± 0.5 (17)</td><td>313 ± 347</td><td>7.7 ± 2.5 (-7)</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>7.0 ± 2.7 (15)</td><td>140 ± 42</td><td>3.5 ± 1.3 (-8)</td></tr><tr><td>CH<sub>3</sub>CHO</td><td>7.4 ± 2.1 (14)</td><td>28 ± 11</td><td>3.7 ± 1.1 (-9)</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>2.2 ± 0.9 (14)</td><td>50 ± 30</td><td>1.1 ± 0.4 (-9)</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>3.4 ± 1.3 (14)</td><td>83 ± 31</td><td>1.7 ± 0.6 (-9)</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>9.7 ± 4.9 (13)</td><td>[80]</td><td>4.9 ± 2.4 (-10)</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>6.4 ± 4.7 (15)</td><td>[80]</td><td>3.2 ± 2.3 (-8)</td></tr><tr><td rowspan="10">W51 e1/e2</td><td rowspan="10">3.6</td><td>CH<sub>3</sub>OH</td><td>2.3 ± 0.7 (17)</td><td>197 ± 28</td><td>6.3 ± 2.1 (-7)</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>3.5 ± 1.3 (16)</td><td>113 ± 32</td><td>9.8 ± 3.6 (-8)</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>7.0 ± 1.9 (15)</td><td>165 ± 40</td><td>1.9 ± 0.5 (-8)</td></tr><tr><td>CH<sub>3</sub>CHO</td><td>4.5 ± 2.4 (14)</td><td>11 ± 3</td><td>1.3 ± 0.7 (-9)</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>1.6 ± 1.3 (14)</td><td>27 ± 23</td><td>4.5 ± 3.7 (-10)</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>7.5 ± 2.2 (14)</td><td>118 ± 38</td><td>2.1 ± 0.6 (-9)</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>1.2 ± 0.5 (14)</td><td>60 ± 24</td><td>3.3 ± 1.3 (-10)</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>4.3 ± 2.8 (15)</td><td>[60]</td><td>1.2 ± 0.8 (-8)</td></tr><tr><td>CH<sub>3</sub>OH</td><td>1.1 ± 0.4 (17)</td><td>217 ± 37</td><td>6.6 ± 2.2 (-7)</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>1.8 ± 0.9 (15)</td><td>32 ± 15</td><td>1.1 ± 0.6 (-8)</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>3.2 ± 1.0 (15)</td><td>137 ± 25</td><td>2.0 ± 0.6 (-8)</td></tr><tr><td>CH<sub>3</sub>CHO</td><td>4.0 ± 2.9 (14)</td><td>[10]</td><td>2.5 ± 1.8 (-9)</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>3.2 ± 0.9 (14)</td><td>62 ± 15</td><td>2.0 ± 0.6 (-9)</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>2.1 ± 1.0 (14)</td><td>[100]</td><td>1.3 ± 0.7 (-9)</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>1.5 ± 1.0 (15)</td><td>[100]</td><td>9.2 ± 6.0 (-9)</td></tr><tr><td rowspan="10">G31.41+0.3</td><td rowspan="10">1.6</td><td>CH<sub>3</sub>OH</td><td>1.2 ± 0.6 (17)</td><td>196 ± 42</td><td>4.1 ± 1.9 (-7)</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>5.5 ± 1.8 (16)</td><td>350 ± 412</td><td>1.8 ± 0.6 (-7)</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>2.0 ± 0.9 (15)</td><td>133 ± 106</td><td>6.6 ± 2.9 (-9)</td></tr><tr><td>CH<sub>3</sub>CHO</td><td>5.2 ± 2.0 (14)</td><td>[10]</td><td>1.7 ± 0.7 (-9)</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>2.1 ± 0.9 (14)</td><td>[60]</td><td>6.9 ± 3.1 (-10)</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>5.7 ± 1.9 (14)</td><td>167 ± 83</td><td>1.9 ± 0.6 (-9)</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>0.0 ± 0.0 (15)</td><td>25 ± 10</td><td>1.5 ± 1.1 (-10)</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>3.2 ± 2.6 (15)</td><td>[60]</td><td>1.1 ± 0.9 (-8)</td></tr><tr><td>CH<sub>3</sub>OH</td><td>3.5 ± 3.3 (16)</td><td>131 ± 68</td><td>5.2 ± 4.9 (-9)</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>1.9 ± 0.7 (14)</td><td>78 ± 57</td><td>2.9 ± 1.1 (-11)</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>1.4 ± 1.0 (14)</td><td>[60]</td><td>2.1 ± 1.5 (-11)</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>5.3 ± 3.0 (14)</td><td>[60]</td><td>8.0 ± 4.5 (-11)</td></tr><tr><td rowspan="2">DR21(OH)</td><td rowspan="2">2.0</td><td>CH<sub>3</sub>OH</td><td>4.6 ± 1.0 (15)</td><td>[150]</td><td>2.3 ± 0.5 (-8)</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>1.1 ± 0.7 (15)</td><td>[150]</td><td>5.5 ± 3.5 (-9)</td></tr></tbody></table>

Note. a (b) means $a \times 10^b$. A 10" source size was assumed. Hydrogen column densities of these sources were summarized in Ikeda et al. (2001). Reliable data for hydrogen column density under an extended source were not available for G19.61–0.23.

coefficients is more than 95% if *t* is larger than 2.78 for *n* = 6 and 2.57 for *n* = 7.

As a result, we can confirm enough of a significance level only for the correlations with NH<sub>2</sub>CHO and CH<sub>2</sub>CHCN, CH<sub>3</sub>CH<sub>2</sub>CN and CH<sub>2</sub>NH, and (CH<sub>3</sub>)<sub>2</sub>CO and CH<sub>2</sub>NH. While NH<sub>2</sub>CHO and (CH<sub>3</sub>)<sub>2</sub>CO contain O atoms, these species also

showed correlations with other N-bearing species. This result suggests that the correlations among different species are not determined by only the atoms they contain. For the correlation coefficients between other species, the significance level is not enough for most cases with the current source number. An expansion of survey observations would be required to confirm
<table><caption>**Table 4**
Abundances in Compact Source Size</caption><thead><tr><th>Species</th><th>Source</th><th>Θ<br>Initial<br>(s)</th><th>N<br>Initial<br>(cm<sup>-2</sup>)</th><th>Tex<br>Initial<br>(K)</th><th>Θ<br>(s)</th><th>N<br>(cm<sup>-2</sup>)</th><th>Tex<br>(K)</th><th>X</th></tr></thead><tbody><tr><td rowspan="6">CH<sub>3</sub>OH</td><td>G10.47+0.03</td><td>...</td><td>4.3 (18)</td><td>185</td><td>[2.5]</td><td>4.7 ± 1.3 (18)</td><td>135 ± 32</td><td>7.0 ± 2.0 (-7)</td></tr><tr><td>Orion KL</td><td>...</td><td>1.5 (18)</td><td>183</td><td>[5.2]</td><td>2.3 ± 0.5 (18)</td><td>225 ± 23</td><td>1.8 ± 0.4 (-6)</td></tr><tr><td>NGC 6334F</td><td>3.5</td><td>2.5 (18)</td><td>201</td><td>3.8 ± 0.5</td><td>2.6 ± 1.3 (18)</td><td>116 ± 37</td><td>1.8 ± 0.9 (-6)</td></tr><tr><td>W51 e1/e2</td><td>2</td><td>5.7 (18)</td><td>197</td><td>2.5 ± 0.2</td><td>7.1 ± 2.0 (18)</td><td>293 ± 62</td><td>1.3 ± 0.4 (-6)</td></tr><tr><td>G31.41+0.3</td><td>1.7</td><td>3.7 (18)</td><td>217</td><td>1.8 ± 0.1</td><td>3.8 ± 1.1 (18)</td><td>185 ± 51</td><td>1.1 ± 0.3 (-6)</td></tr><tr><td>G34.3+0.2</td><td>2.0</td><td>3.1 (18)</td><td>196</td><td>2.3 ± 0.3</td><td>3.2 ± 0.9 (18)</td><td>98 ± 27</td><td>7.1 ± 2.1 (-7)</td></tr><tr><td rowspan="6">HCOOCH<sub>3</sub></td><td>G19.61-0.23</td><td>...</td><td>...</td><td>...</td><td>[2.5]</td><td>5.6 ± 5.3 (17)</td><td>[131]</td><td>8.3 ± 7.9 (-8)</td></tr><tr><td>G10.47+0.03</td><td>...</td><td>1.8 (17)</td><td>60</td><td>[2.0]</td><td>3.1 ± 2.3 (17)</td><td>83 ± 54</td><td>4.6 ± 3.4 (-8)</td></tr><tr><td>Orion KL</td><td>...</td><td>2.7 (17)</td><td>80</td><td>[3.5]</td><td>1.4 ± 0.4 (17)</td><td>44 ± 3</td><td>1.1 ± 0.3 (-7)</td></tr><tr><td>NGC 6334F</td><td>3.5</td><td>1.3 (18)</td><td>313</td><td>1.9 ± 0.1</td><td>1.3 ± 0.4 (18)</td><td>101 ± 10</td><td>9.3 ± 3.0 (-7)</td></tr><tr><td>W51 e1/e2</td><td>2</td><td>8.8 (17)</td><td>113</td><td>1.5 ± 0.1</td><td>2.5 ± 1.0 (18)</td><td>98 ± 20</td><td>4.7 ± 1.6 (-7)</td></tr><tr><td>G31.41+0.3</td><td>...</td><td>6.1 (16)</td><td>32</td><td>[1.7]</td><td>3.1 ± 3.0 (17)</td><td>82 ± 19</td><td>8.9 ± 8.6 (-8)</td></tr><tr><td rowspan="6">CH<sub>3</sub>OCH<sub>3</sub></td><td>G34.3+0.2</td><td>2.0</td><td>1.4 (18)</td><td>350</td><td>1.3 ± 0.4</td><td>2.4 ± 1.7 (18)</td><td>48 ± 29</td><td>5.3 ± 3.7 (-7)</td></tr><tr><td>G10.47+0.03</td><td>...</td><td>7.6 (16)</td><td>119</td><td>[2.0]</td><td>1.7 ± 0.4 (17)</td><td>89 ± 10</td><td>2.5 ± 0.6 (-8)</td></tr><tr><td>Orion KL</td><td>...</td><td>1.4 (17)</td><td>91</td><td>[3.5]</td><td>6.5 ± 1.9 (16)</td><td>178 ± 24</td><td>5.0 ± 1.5 (-8)</td></tr><tr><td>NGC 6334F</td><td>3.5</td><td>5.7 (16)</td><td>140</td><td>2.1 ± 0.2</td><td>1.2 ± 0.6 (17)</td><td>82 ± 16</td><td>8.6 ± 4.0 (-8)</td></tr><tr><td>W51 e1/e2</td><td>2</td><td>1.8 (17)</td><td>165</td><td>1.4 ± 0.1</td><td>2.9 ± 1.2 (17)</td><td>91 ± 23</td><td>5.4 ± 2.3 (-8)</td></tr><tr><td>G31.41+0.3</td><td>...</td><td>1.1 (17)</td><td>137</td><td>[1.7]</td><td>1.0 ± 0.3 (17)</td><td>85 ± 21</td><td>2.9 ± 0.9 (-8)</td></tr><tr><td rowspan="6">(CH<sub>3</sub>)<sub>2</sub>CO</td><td>G34.3+0.2</td><td>...</td><td>...</td><td>...</td><td>[2.0]</td><td>4.9 ± 2.9 (16)</td><td>[117]</td><td>1.1 ± 0.6 (-8)</td></tr><tr><td>G10.47+0.03</td><td>...</td><td>...</td><td>...</td><td>[2.0]</td><td>3.3 ± 1.1 (17)</td><td>[71]</td><td>4.9 ± 1.6 (-8)</td></tr><tr><td>Orion KL</td><td>...</td><td>...</td><td>...</td><td>[2.8]</td><td>1.7 ± 1.3 (17)</td><td>[100]</td><td>1.3 ± 1.0 (-7)</td></tr><tr><td>NGC 6334F</td><td>...</td><td>...</td><td>...</td><td>[3.5]</td><td>5.2 ± 3.8 (16)</td><td>[80]</td><td>3.7 ± 2.7 (-8)</td></tr><tr><td>W51 e1/e2</td><td>...</td><td>...</td><td>...</td><td>[2.0]</td><td>1.1 ± 0.7 (17)</td><td>[60]</td><td>2.0 ± 1.4 (-8)</td></tr><tr><td>G31.41+0.3</td><td>...</td><td>...</td><td>...</td><td>[1.7]</td><td>2.3 ± 1.0 (16)</td><td>[100]</td><td>6.5 ± 3.0 (-9)</td></tr><tr><td rowspan="6">NH<sub>2</sub>CHO</td><td>G34.3+0.2</td><td>...</td><td>...</td><td>...</td><td>[2.0]</td><td>8.1 ± 6.5 (16)</td><td>[60]</td><td>1.8 ± 1.4 (-8)</td></tr><tr><td>G10.47+0.03</td><td>...</td><td>8.5 (16)</td><td>119</td><td>[1.5]</td><td>1.3 ± 0.6 (17)</td><td>121 ± 69</td><td>1.9 ± 0.8 (-8)</td></tr><tr><td>Orion KL</td><td>...</td><td>...</td><td>...</td><td>[2.8]</td><td>2.9 ± 2.1 (15)</td><td>[100]</td><td>2.3 ± 1.6 (-9)</td></tr><tr><td>NGC 6334F</td><td>...</td><td>...</td><td>...</td><td>[3.5]</td><td>1.8 ± 0.7 (15)</td><td>[50]</td><td>1.3 ± 0.5 (-9)</td></tr><tr><td>W51 e1/e2</td><td>...</td><td>...</td><td>...</td><td>[2.0]</td><td>4.0 ± 3.9 (15)</td><td>[27]</td><td>7.6 ± 7.4 (-10)</td></tr><tr><td>G31.41+0.3</td><td>1.7</td><td>1.1 (16)</td><td>62</td><td>1.8 ± 0.3</td><td>1.0 ± 0.7 (16)</td><td>41 ± 18</td><td>2.9 ± 1.9 (-9)</td></tr><tr><td rowspan="6">CH<sub>3</sub>CH<sub>2</sub>CN</td><td>G34.3+0.2</td><td>...</td><td>...</td><td>...</td><td>[2.0]</td><td>5.2 ± 2.3 (15)</td><td>[60]</td><td>1.2 ± 0.5 (-9)</td></tr><tr><td>G19.61-0.23</td><td>...</td><td>...</td><td>...</td><td>[2.5]</td><td>3.1 ± 1.2 (15)</td><td>[78]</td><td>4.6 ± 1.8 (-10)</td></tr><tr><td>G10.47+0.03</td><td>...</td><td>5.7 (17)</td><td>398</td><td>[2.0]</td><td>1.8 ± 0.6 (17)</td><td>71 ± 3</td><td>2.7 ± 0.8 (-8)</td></tr><tr><td>Orion KL</td><td>...</td><td>1.2 (17)</td><td>146</td><td>[2.8]</td><td>1.7 ± 0.8 (17)</td><td>63 ± 6</td><td>1.3 ± 0.6 (-7)</td></tr><tr><td>NGC 6334F</td><td>...</td><td>2.8 (15)</td><td>83</td><td>[3.5]</td><td>1.8 ± 0.8 (15)</td><td>58 ± 23</td><td>1.3 ± 0.6 (-9)</td></tr><tr><td>W51 e1/e2</td><td>...</td><td>1.9 (16)</td><td>118</td><td>[2.0]</td><td>2.6 ± 2.3 (16)</td><td>106 ± 82</td><td>4.9 ± 4.3 (-9)</td></tr><tr><td rowspan="6">CH<sub>2</sub>CHCN</td><td>G31.41+0.3</td><td>1.1</td><td>1.0 (17)</td><td>118</td><td>1.7 ± 0.6</td><td>3.8 ± 2.5 (17)</td><td>59 ± 44</td><td>1.1 ± 0.7 (-7)</td></tr><tr><td>G34.3+0.2</td><td>2.0</td><td>1.4 (16)</td><td>167</td><td>1.4 ± 0.4</td><td>3.3 ± 2.9 (16)</td><td>49 ± 30</td><td>7.3 ± 6.4 (-9)</td></tr><tr><td>G19.61-0.23</td><td>...</td><td>...</td><td>...</td><td>[2.5]</td><td>2.2 ± 1.6 (15)</td><td>[60]</td><td>3.3 ± 2.4 (-10)</td></tr><tr><td>G10.47+0.03</td><td>...</td><td>2.8 (17)</td><td>382</td><td>[1.5]</td><td>1.4 ± 0.5 (17)</td><td>217 ± 51</td><td>2.1 ± 0.8 (-8)</td></tr><tr><td>Orion KL</td><td>...</td><td>1.3 (16)</td><td>97</td><td>[2.8]</td><td>1.6 ± 0.9 (16)</td><td>122 ± 50</td><td>1.2 ± 0.7 (-8)</td></tr><tr><td>NGC 6334F</td><td>...</td><td>...</td><td>...</td><td>[3.5]</td><td>7.9 ± 4.0 (14)</td><td>[80]</td><td>5.7 ± 2.8 (-10)</td></tr><tr><td rowspan="6"></td><td>G31.41+0.3</td><td>...</td><td>7.1 (15)</td><td>...</td><td>[1.7]</td><td>3.0 ± 1.2 (15)</td><td>[60]</td><td>5.7 ± 2.3 (-10)</td></tr><tr><td>G34.3+0.2</td><td>...</td><td>...</td><td>...</td><td>[2.0]</td><td>7.1 ± 3.6 (15)</td><td>[100]</td><td>2.0 ± 1.0 (-9)</td></tr><tr><td>G19.61-0.23</td><td>...</td><td>...</td><td>...</td><td>[2.5]</td><td>8.5 ± 4.8 (15)</td><td>[60]</td><td>1.3 ± 0.7 (-9)</td></tr></tbody></table>

Note. a (b) means $a \times 10^b$. Fractional abundances were calculated from the H<sub>2</sub> column densities: 6.69 × 10<sup>24</sup> cm<sup>-2</sup> for G10.47+0.03, 1.35 × 10<sup>24</sup> cm<sup>-2</sup> for NGC 6334F, 5.27 × 10<sup>24</sup> cm<sup>-2</sup> for W51 e1/e2, 3.53 × 10<sup>24</sup> cm<sup>-2</sup> for G31.41+0.03 (Hernández-Hernández et al. 2014), 4.50 × 10<sup>24</sup> cm<sup>-2</sup> for G34.3+0.2 (Fontani et al. 2007), and 1.3 × 10<sup>24</sup> cm<sup>-2</sup> (Hirota et al. 2015) for Orion KL.

their correlations. Although we should have more data to confirm the general trend, there are some sources where N-bearing species NH<sub>2</sub>CHO, CH<sub>2</sub>CHCN, CH<sub>3</sub>CH<sub>2</sub>CN, and CH<sub>2</sub>NH are depleted compared to CH<sub>3</sub>OH, a representative O-bearing species. With the fractional abundances under the compact source size, all abundances of the above four N-bearing species compared to CH<sub>3</sub>OH are less than 0.01 for NGC 6334F and W51 e1/e2. Therefore, at least NGC 6334F and W51 e1/e2 are special sources where N-bearing species

are poor compared to O-bearing species. The physical conditions that lead to the different abundances of N-bearing species will be discussed using the chemical abundances of representative sources G10.47+0.03 and NGC 6334F, where N-bearing species are rich and not so rich.

### 3.3.1. G10.47+0.03

For an extended source size, the abundances of O-bearing species CH<sub>3</sub>OCH<sub>3</sub>, CH<sub>3</sub>OH, and CH<sub>3</sub>CHO were consistent
<table><caption>**Table 5**
Calculated Correlation Coefficients</caption><thead><tr><th></th><th>HCOOCH<sub>3</sub></th><th>CH<sub>3</sub>OCH<sub>3</sub></th><th>(CH<sub>3</sub>)<sub>2</sub>CO</th><th>NH<sub>2</sub>CHO</th><th>CH<sub>3</sub>CH<sub>2</sub>CN</th><th>CH<sub>2</sub>CHCN</th><th>CH<sub>2</sub>NH</th></tr></thead><tbody><tr><td>CH<sub>3</sub>OH</td><td>0.31</td><td>0.70</td><td>0.60</td><td>-0.12</td><td>0.51</td><td>-0.05</td><td>0.34</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>...</td><td>0.58</td><td>-0.34</td><td>-0.52</td><td>-0.62</td><td>-0.68</td><td>-0.74</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>...</td><td>...</td><td>0.22</td><td>-0.34</td><td>-0.14</td><td>-0.25</td><td>-0.21</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>...</td><td>...</td><td>...</td><td>0.09</td><td>0.54</td><td>0.55</td><td>0.78</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>...</td><td>...</td><td>...</td><td>...</td><td>0.01</td><td>0.88</td><td>0.66</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>0.26</td><td>0.92</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>0.60</td></tr></tbody></table>

**Note.** Correlation coefficients were calculated with our observed abundances for compact source sizes. The fractional abundances reported in Suzuki et al. (2016) were also added in this discussion.

<table><caption>**Table 6**
Results of *t*-tests</caption><thead><tr><th></th><th>HCOOCH<sub>3</sub></th><th>CH<sub>3</sub>OCH<sub>3</sub></th><th>(CH<sub>3</sub>)<sub>2</sub>CO</th><th>NH<sub>2</sub>CHO</th><th>CH<sub>3</sub>CH<sub>2</sub>CN</th><th>CH<sub>2</sub>CHCN</th><th>CH<sub>2</sub>NH</th></tr></thead><tbody><tr><td>CH<sub>3</sub>OH</td><td>0.65</td><td>1.96</td><td>1.50</td><td>-0.27</td><td>1.33</td><td>-0.10</td><td>0.81</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>...</td><td>1.42</td><td>-0.72</td><td>-1.22</td><td>-1.58</td><td>-1.85</td><td>-2.20</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>...</td><td>...</td><td>0.45</td><td>-0.72</td><td>-0.28</td><td>-0.52</td><td>-0.43</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>...</td><td>...</td><td>...</td><td>0.18</td><td>1.28</td><td>1.32</td><td><strong>2.49</strong></td></tr><tr><td>NH<sub>2</sub>CHO</td><td>...</td><td>...</td><td>...</td><td>...</td><td>0.02</td><td><strong>3.71</strong></td><td>1.96</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>0.54</td><td><strong>5.25</strong></td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td><td>1.50</td></tr></tbody></table>

**Note.** Result of *t*-tests to evaluate the reliability of correlation coefficients. Values with significance level greater than 95% are shown in boldface.

<table><caption>**Table 7**
Binding Energies</caption><thead><tr><th>Species</th><th><i>E</i><sub>D</sub> (K)</th></tr></thead><tbody><tr><td>CH<sub>3</sub>OH</td><td>5534</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>6295</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>3151</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>3500</td></tr><tr><td>CH<sub>2</sub>NH</td><td>5534</td></tr><tr><td>CH<sub>3</sub>NH<sub>2</sub></td><td>6584</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>5484</td></tr><tr><td>CH<sub>3</sub>CH<sub>2</sub>CN</td><td>5540</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>5556</td></tr><tr><td>CH<sub>3</sub>CHO</td><td>2450</td></tr></tbody></table>

**Note.** Binding energies used our chemical reaction model.

with that in Ikeda et al. (2001) within a factor of 3, considering that Ikeda et al. (2001) used a source size of 20". The line widths were typically 9 km s⁻¹ for the observed COMs, except for CH₃OCH₃, whose transitions of EE, EA, AE, and AA states were heavily blended with each other. While the radial velocities of CH₂CHCN and CH₃CH₂CN were 67.7 ± 0.4 and 66.9 ± 0.6 km s⁻¹, CH₃OH and NH₂CHO showed slightly lower average radial velocities of 66.2 ± 0.3 and 66.4 ± 0.3 km s⁻¹. However, although the radial velocity of CH₂CHCN is suggestive of the different peak position, the difference in radial velocity for other species is small compared to the standard deviation of the radial velocities.

In G10.47+0.03, we determined the source sizes of observed species with previous mapping observations (Rolffs et al. 2011). Then the column densities and the excitation temperatures were given by the least squares method. The number of observed transitions were not enough to analyze the abundances of (CH₃)₂CO via LTE analysis. Assuming that the

distribution of (CH₃)₂CO was the same as CH₃CH₂CN, similar to Orion KL (Peng et al. 2013), we employed a source size of 2" for the case of a compact source and an excitation temperature of 71 K. For other species, the source sizes for the case of a compact source were determined by the least squares method. The column densities of HCOOCH₃, CH₂CHCN, and CH₃CH₂CN for the compact source size were consistent with the results by Fontani et al. (2007), where the source size was estimated from the line widths. Rolffs et al. (2011) also reported the abundances of CH₃OH, HCOOCH₃, CH₃OCH₃, (CH₃)₂CO, NH₂CHO, CH₃CH₂CN, and CH₂CHCN with interferometric observations. We note that our column densities of CH₃OCH₃, CH₃CH₂CN, and CH₂CHCN were almost one order of magnitude lower than those reported by Rolffs et al. (2011); they used a smaller source size of 1"5, which corresponds to the densest part of the core. We got more extended source sizes and lower column densities through our least squares method probably because our single-dish observation could not resolve such structure.

### 3.3.2. Orion KL

Our column densities under the extended source size were consistent with Ikeda et al. (2001) for CH₃OH, HCOOCH₃, CH₃CH₂CN, and CH₂CHCN. In addition, the comparable abundance of NH₂CHO was reported by Turner (1991). For the abundances under the compact source size, the column densities of CH₃CH₂CN and CH₂CHCN were consistent with Rizzo et al. (2017) for the Hot Core, but our column densities of (CH₃)₂CO were three times higher than that of Peng et al. (2013). This discrepancy would have come from the assumption of an excitation temperature of 100 K in our survey, due to a lack of observed transitions with a wide range of the energy levels.

As has already been discussed by many authors, the characteristics of molecular lines are clearly different for O-bearing molecules and N-bearing molecules, which originate
in the Compact Ridge and Hot Core, respectively. These different distributions were also indicated from the different radial velocities obtained in our survey. HCOOCH₃, CH₃OCH₃, and CH₃OH had average radial velocities of 7.6 ± 0.3, 7.6 ± 0.6, and 7.7 ± 0.4 km s⁻¹, respectively, while CH₂CHCN and CH₃CH₂CN showed radial velocities of 4.9 ± 0.8 and 4.6 ± 0.9 km s⁻¹.

We calculated the abundances for compact source sizes based on previously reported spatial distributions of the observed species. We used 5′′2 for CH₃OH (Peng et al. 2012), 2′′8 for CH₃CH₂CN and (CH₃)₂CO (Peng et al. 2013) and CH₃OCH₃ (Brouillet et al. 2013), and 3′′5 for HCOOCH₃ (Favre et al. 2011). We employed a source size of 2′′8 for CH₂CHCN considering the distribution of CH₃CH₂CN, assuming that their distributions would be similar to that of (CH₃)₂CO (Peng et al. 2013).

### 3.3.3. NGC 6334F

The previous observations of COMs to compare with our results were limited for NGC 6334F; however, our column densities of CH₃OH and CH₃OCH₃ agreed with Ikeda et al. (2001).

The typical line width was ~4.0 km s⁻¹ in this source. The average radial velocities of O-bearing species CH₃OH, HCOOCH₃, and CH₃OCH₃ were -7.8 ± 0.6, -7.5 ± 0.4, and -7.7 ± 0.8 km s⁻¹, respectively, while that of CH₃CH₂CN is -6.7 ± 0.6 km s⁻¹. Hence, in this source, it is difficult to claim the different radial velocities with their standard deviations, and this result would suggest that COMs exist in the same position.

Due to the lack of available data, the excitation temperatures of (CH₃)₂CO and CH₂CHCN were assumed to be 80 K, referring to that of CH₃CH₂CN. The least squares fitting method was employed to estimate abundances under the compact source sizes of CH₃OH, HCOOCH₃, and CH₃OCH₃. The initial source size was assumed to be 3′′5 from the source size of continuum emission (Hernández-Hernández et al. 2014). For CH₃CH₂CN, CH₂CHCN, (CH₃)₂CO, and NH₂CHO, we fixed the source size to be 3′′5 because the number of emission lines was lacking.

### 3.3.4. W51 e1/e2

While our column densities of CH₃OH, HCOOCH₃, and CH₃OCH₃ agreed with the previous studies (Ikeda et al. 2001; Fuchs et al. 2005), those of CH₃CH₂CN and CH₂CHCN were lower than Ikeda et al. (2001) by a factor of four.

The average radial velocities of CH₂CHCN and CH₃CH₂CN were 58.1 ± 1.1 and 57.8 ± 1.3 km s⁻¹, and their line widths were about 10.0 km s⁻¹. On the other hand, the radial velocities of CH₃OH and HCOOCH₃ were respectively 56.3 ± 0.4 and 56.6 ± 0.9 km s⁻¹, and their typical line widths were 8.0 km s⁻¹. It is known that W51 e1/e2 contains two UCHII regions named e2 and e8 (Zhang et al. 1989). Since the systematic velocities for e2 and e8 are 55 and 59 km s⁻¹, O-bearing and N-bearing molecules would be dominant in e2 and e8, respectively. While the differences in radial velocities of CH₂CHCN, CH₃CH₂CN, CH₃OH, and HCOOCH₃ may be due to their origins from different UCHII regions, the difference is not clear, due to the relatively high standard deviation.

NH₂CHO showed a low excitation temperature of 27 K. However, we note that the observed energy range is too limited for this species to determine an accurate excitation temperature. For HCOOCH₃, we could not obtain a reliable abundance by the usual rotation diagram method, due to large scattering. This would be due to the optical thickness of some transitions. Considering that the strongest HCOOCH₃ line shows Ta* of ~400 mK, we selected only a weak (Ta* < 0.1 K, corresponding to the quarter of 400 mK) line to select potentially optical thin lines in the rotation diagram method. As a result, we obtained its excitation temperature and column density of 113 K and 3.5 × 10¹⁶ cm⁻² assuming a 10'' source size. We used the least squares method using all observed lines, which can calculate the effect of optical thickness, with this excitation temperature and the column density of 1.3 × 10¹⁸ cm⁻², which was obtained by multiplying a factor of (10''/2'')² by the column density obtained in the 10'' source size. We note that there is an uncertainty in using the column density and the excitation temperatures obtained through this method as the initial values for the least squares method due to the effect of optical thickness. Therefore, as the initial values for the least squares method, we changed the excitation temperature from 50 to 150 K and the initial column density from 5 × 10¹⁷ to 5 × 10¹⁷ cm⁻², to obtain the range of these parameters. Finally, we obtained the excitation temperature and column density of 98 ± 20 K and (2.5 ± 1) × 10¹⁸ cm⁻², respectively.

The abundances under compact source size for (CH₃)₂CO were derived by assuming that the source size is the same as the continuum emission size of 2'' (Hernández-Hernández et al. 2014) and assuming the excitation temperature of 60 K, referring to that of CH₂CHCN. The excitation temperatures of CH₂CHCN and NH₂CHO were fixed at 60 K and 27 K, respectively, in deriving the abundances for compact source size due to the limited number of observed transitions and the limited range of observed energy levels.

### 3.3.5. G31.41+0.03

The observed column densities of CH₃OH, HCOOCH₃, CH₃CH₂CN, and CH₂CHCN agreed with Ikeda et al. (2001) and Fontani et al. (2007). Ikeda et al. (2001) reported a higher column density for CH₃OCH₃ by a factor of four compared to our abundance.

The average radial velocities of CH₃OH, CH₂CHCN, CH₃CH₂CN, and NH₂CHO fell into 97.5 ± 0.4 km s⁻¹. It would be difficult to discuss their distributions from these results with our velocity resolution of 0.4 km s⁻¹. While the radial velocity for HCOOCH₃ of 98.5 ± 1.0 km s⁻¹ is relatively high, its standard deviation makes it difficult to distinguish from other species.

The source sizes of CH₃OCH₃ and HCOOCH₃ were determined based on previous mapping observations (Rivilla et al. 2017). The abundance of CH₃CH₂CN was not determined from the rotation diagram method, presumably due to the optical thickness of the observed transitions with low energy levels. Therefore we determined its abundance by the χ² method, with the initial column density of 1.0 × 10¹⁷ cm⁻², initial excitation temperature of 118 K, and initial source size of 1′′1 from Beltrán et al. (2005). Since the number of observed transitions were not enough for CH₂CHCN and (CH₃)₂CO, their source sizes were fixed to be the continuum size of 1′′7. Although the excitation temperature of CH₃CH₂CN would be a good indicator for those of CH₂CHCN and (CH₃)₂CO, the
<table><caption>**Table 8**
Important Gas Phase Reactions for COMs of Interest</caption><thead><tr><th>Reaction</th><th>α</th><th>β</th><th>γ</th></tr></thead><tbody><tr><td>CH<sub>3</sub>OH<sub>2</sub><sup>+</sup> + e<sup>-</sup> → H+H<sub>2</sub> + H<sub>2</sub>CO</td><td>9.1 (-8)</td><td>-6.7 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>OH<sub>2</sub><sup>+</sup> + e<sup>-</sup> → H<sub>2</sub>O + CH<sub>3</sub></td><td>8.19 (-8)</td><td>-6.7 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>OH<sub>2</sub><sup>+</sup> + e<sup>-</sup> → H + OH + CH<sub>3</sub></td><td>4.64 (-7)</td><td>-6.7 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>OH<sub>2</sub><sup>+</sup> + e<sup>-</sup> → H + CH<sub>2</sub> + H<sub>2</sub>O</td><td>1.91 (-7)</td><td>-6.7 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>OH<sub>2</sub><sup>+</sup> + e<sup>-</sup> → H + CH<sub>3</sub>OH</td><td>2.73 (-8)</td><td>-6.7 (-1)</td><td>0</td></tr><tr><td>HC(OH)OCH<sub>3</sub><sup>+</sup> + e<sup>-</sup> → HCOOCH<sub>3</sub> + CH<sub>3</sub>OH</td><td>1.5 (-7)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>HC(OH)OCH<sub>3</sub><sup>+</sup> + e<sup>-</sup> → HCOOCH<sub>3</sub> + H</td><td>1.5 (-7)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>OCH<sub>4</sub><sup>+</sup> + e<sup>-</sup> → O+CH<sub>3</sub> + CH<sub>4</sub></td><td>7.48 (-7)</td><td>-7 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>OCH<sub>4</sub><sup>+</sup> + e<sup>-</sup> → CH<sub>3</sub> + CH<sub>3</sub>OH</td><td>8.33 (-7)</td><td>-7 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>OCH<sub>4</sub><sup>+</sup> + e<sup>-</sup> → H + CH<sub>3</sub>OCH<sub>3</sub>+</td><td>1.19 (-7)</td><td>-7 (-1)</td><td>0</td></tr><tr><td>C<sub>2</sub>H<sub>4</sub> + CN → H + CH<sub>2</sub>CHCN</td><td>2.67 (-10)</td><td>-6.9 (-1)</td><td>3.1 (1)</td></tr><tr><td>C<sub>2</sub>H<sub>4</sub> + CN → HCN + C<sub>2</sub>H<sub>3</sub></td><td>2.14 (-10)</td><td>-6.9 (-1)</td><td>3.1 (1)</td></tr><tr><td>C<sub>2</sub>H<sub>4</sub>CN<sup>+</sup> + e<sup>-</sup> → H<sub>2</sub> + H<sub>2</sub></td><td>1.5 (-7)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>C<sub>2</sub>H<sub>4</sub>CN<sup>+</sup> + e<sup>-</sup> → H+H<sub>2</sub></td><td>1 (-6)</td><td>-3 (-1)</td><td>0</td></tr><tr><td>C<sub>2</sub>H<sub>4</sub>CN<sup>+</sup> + e<sup>-</sup> → H + CH<sub>2</sub>CHCN</td><td>1 (-6)</td><td>-3 (-1)</td><td>0</td></tr><tr><td>C<sub>3</sub>H<sub>6</sub>OH<sup>+</sup> + e<sup>-</sup> → CH<sub>3</sub> + CH<sub>3</sub>CHO</td><td>1.5 (-7)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>C<sub>3</sub>H<sub>6</sub>OH<sup>+</sup> + e<sup>-</sup> → H + (CH<sub>3</sub>)<sub>2</sub>CO</td><td>1.5 (-7)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>COCH<sub>4</sub><sup>+</sup> + e<sup>-</sup> → CH<sub>3</sub>CO + CH<sub>3</sub> + H</td><td>6.75 (-8)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>COCH<sub>4</sub><sup>+</sup> + e<sup>-</sup> → H<sub>2</sub>CCO + CH<sub>4</sub> + H</td><td>6.75 (-8)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>COCH<sub>4</sub><sup>+</sup> + e<sup>-</sup> → CH<sub>3</sub>CO + CH<sub>4</sub></td><td>1.5 (-8)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>COCH<sub>4</sub><sup>+</sup> + e<sup>-</sup> → (CH<sub>3</sub>)<sub>2</sub>CO + H</td><td>1.5 (-8)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>COCH<sub>4</sub><sup>+</sup> + e<sup>-</sup> → CH<sub>3</sub> + CO + CH<sub>4</sub></td><td>6.75 (-8)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>H<sub>2</sub>CO + NH<sub>2</sub> → H + NH<sub>2</sub>CHO</td><td>2.6 (-12)</td><td>-2.1 (0)</td><td>2.69 (1)</td></tr><tr><td>NH + CH<sub>3</sub> → CH<sub>2</sub>NH + H</td><td>1.3 (-10)</td><td>1.7 (-1)</td><td>0</td></tr><tr><td>CH + NH<sub>3</sub> → CH<sub>2</sub>NH + H</td><td>1.52 (-10)</td><td>-5 (-2)</td><td>0</td></tr><tr><td>CH<sub>2</sub>NH<sub>2</sub><sup>+</sup> + e<sup>-</sup> → CH<sub>2</sub>NH + H</td><td>1.5 (-7)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>NH<sub>3</sub><sup>+</sup> + e<sup>-</sup> → CH<sub>2</sub>NH + H<sub>2</sub> + H</td><td>1.5 (-7)</td><td>-5 (-1)</td><td>0</td></tr><tr><td>CH<sub>3</sub>NH<sub>2</sub><sup>+</sup> + e<sup>-</sup> → CH<sub>2</sub>NH + H<sub>2</sub></td><td>1.5 (-7)</td><td>-5 (-1)</td><td>0</td></tr></tbody></table>

Note. a (b) means $a \times 10^b$. Here, α, β, and γ represent the coefficients for the Arrhenius equation.

excitation temperature of CH<sub>3</sub>CH<sub>2</sub>CN has a large error. An excitation temperature of 100 K was assumed for CH<sub>2</sub>CHCN and (CH<sub>3</sub>)<sub>2</sub>CO, considering the higher excitation temperature of CH<sub>3</sub>CH<sub>2</sub>CN reported in Beltrán et al. (2005). An excitation temperature of 10 K was assumed for CH<sub>3</sub>CHO.

The least squares method was applied for CH<sub>3</sub>CH<sub>2</sub>CN, HCOOCH<sub>3</sub>, and CH<sub>3</sub>CH<sub>2</sub>CN, while this method was not applied for CH<sub>2</sub>CHCN and CH<sub>3</sub>OCH<sub>3</sub>, due to a lack of observed transitions. In Table 4, abundances under compact source sizes for (CH<sub>3</sub>)<sub>2</sub>CO, CH<sub>3</sub>OCH<sub>3</sub>, NH<sub>2</sub>CHO, and CH<sub>2</sub>CHCHN were simply derived by compensating for an effect of beam dilution.

### 3.3.6. G34.3+0.2

The observed column densities of CH<sub>3</sub>OH, CH<sub>3</sub>CH<sub>2</sub>CN, and CH<sub>2</sub>CHCN agreed with Ikeda et al. (2001). Although the column density of HCOOCH<sub>3</sub> agreed with Fontani et al. (2007), our column density of HCOOCH<sub>3</sub> was higher than Ikeda et al. (2001) by an order of magnitude.

In this source, the average radial velocities for CH<sub>3</sub>OH, CH<sub>2</sub>CHCN, CH<sub>3</sub>CH<sub>2</sub>CN, and NH<sub>2</sub>CHO fell into 97.5 ± 0.4 km s<sup>-1</sup>. This difference would not be enough to claim the different spatial distributions with our velocity resolution of 0.35 km s<sup>-1</sup>. HCOOCH<sub>3</sub> showed a slightly higher radial velocity of 98.5 ± 1.2 km s<sup>-1</sup>; however, its standard deviation is not enough to distinguish it from other species.

The excitation temperature of HCOOCH<sub>3</sub> was not determined from a rotation diagram. This would be because some transitions are optically thick and led to the scattering of plots in the rotation diagram. (CH<sub>3</sub>)<sub>2</sub>CO and NH<sub>2</sub>CHO abundances were derived under the excitation temperature of 60 K, considering that the excitation temperatures of CH<sub>3</sub>CH<sub>2</sub>CN and HCOOCH<sub>3</sub> derived with the least squares method are not so high, as described in the latter part of this section.

### 3.3.7. G19.61-0.23

Our column densities of CH<sub>3</sub>OH, NH<sub>2</sub>CHO, and CH<sub>3</sub>CH<sub>2</sub>CN are consistent with the interferometric observations by Qin et al. (2010). However, we note that the column density of CH<sub>3</sub>CH<sub>2</sub>CN was an order of magnitude higher than that of Fontani et al. (2007).

The spectrum obtained for this source was limited from 103 to 105 GHz. Despite this limitation, some CH<sub>2</sub>CHCN, CH<sub>3</sub>CH<sub>2</sub>CN, and CH<sub>3</sub>OH lines were detected. CH<sub>3</sub>OH and NH<sub>2</sub>CHO showed average radial velocities of ~37.5 ± 0.3 and ~37.5 ± 0.7 km s<sup>-1</sup>, while CH<sub>2</sub>CHCN showed ~38.5 ± 1.1 km s<sup>-1</sup>. The line width for CH<sub>3</sub>OH of 5.9 km s<sup>-1</sup> was narrower than that of CH<sub>2</sub>CHCN and CH<sub>3</sub>CH<sub>2</sub>CN, which showed line widths of 7.8 and 7.3 km s<sup>-1</sup>, respectively.

For the assumption of compact source size, molecular abundances for this source were calculated assuming a continuum source size of 2.5 due to the lack of enough observed transitions. The excitation temperatures of CH<sub>2</sub>CHCN and CH<sub>3</sub>CH<sub>2</sub>CN were fixed at 60 K from the relatively lower excitation temperature of NH<sub>2</sub>CHO for this source.
<table><caption>**Table 9**

Dust Surface Reactions Related to COMs of Interest</caption><thead><tr><th>Reaction</th><th>E<sub>A</sub><br>(K)</th></tr></thead><tbody><tr><td>CO + H → HCO</td><td>2.5 (3)</td></tr><tr><td>HCO + H → H<sub>2</sub>CO</td><td>0</td></tr><tr><td>H<sub>2</sub>CO + H → CH<sub>3</sub>O</td><td>2.2 (3)</td></tr><tr><td>H<sub>2</sub>CO + H → CH<sub>2</sub>OH</td><td>5.4 (3)</td></tr><tr><td>CH<sub>3</sub>O + H → CH<sub>3</sub>OH</td><td>0</td></tr><tr><td>CH<sub>2</sub>OH + H → CH<sub>3</sub>OH</td><td>0</td></tr><tr><td>CH + OH → CH<sub>3</sub>OH</td><td>0</td></tr><tr><td>CH<sub>3</sub>O + CH + CH<sub>3</sub> → CH<sub>3</sub>OCH<sub>3</sub></td><td>0</td></tr><tr><td>HCO + CH<sub>3</sub>O → HCOOCH<sub>3</sub></td><td>0</td></tr><tr><td>HC<sub>3</sub>N + H → CH<sub>2</sub>CCN</td><td>0</td></tr><tr><td>CH<sub>2</sub>CCN + H → CH<sub>2</sub>CHCN</td><td>0</td></tr><tr><td>CH<sub>2</sub>CHCN + H → CH<sub>3</sub>CHCN</td><td>0</td></tr><tr><td>CH<sub>3</sub>CHCN + H → CH<sub>3</sub>CH<sub>2</sub>CN</td><td>0</td></tr><tr><td>CH<sub>2</sub> + CHCN → CH<sub>2</sub>CHCN</td><td>0</td></tr><tr><td>C<sub>2</sub>H<sub>5</sub> + CN → CH<sub>3</sub>CH<sub>2</sub>CN</td><td>0</td></tr><tr><td>CH<sub>3</sub> + CH<sub>2</sub>CN → CH<sub>3</sub>CH<sub>2</sub>CN</td><td>0</td></tr><tr><td>CH<sub>3</sub>CO + CH<sub>3</sub> → (CH<sub>3</sub>)<sub>2</sub>CO</td><td>0</td></tr><tr><td>H + NH<sub>2</sub>CHO → H<sub>2</sub> + H<sub>2</sub>NCO</td><td>0</td></tr><tr><td>H + H<sub>2</sub>NCO → NH<sub>2</sub>CHO</td><td>0</td></tr><tr><td>NH<sub>2</sub> + CHO → NH<sub>2</sub>CHO</td><td>0</td></tr><tr><td>HCN + H → HCNH</td><td>6.44 (3)</td></tr><tr><td>HCN + H → H<sub>2</sub>CN</td><td>3.65 (3)</td></tr><tr><td>HCNH + H → CH<sub>2</sub>NH</td><td>0</td></tr><tr><td>H<sub>2</sub>CN + H → CH<sub>2</sub>NH</td><td>0</td></tr><tr><td>CH<sub>2</sub>NH + H → CH<sub>3</sub>NH</td><td>2.13 (3)</td></tr><tr><td>CH<sub>2</sub>NH + H → CH<sub>2</sub>NH<sub>2</sub></td><td>3.17 (3)</td></tr><tr><td>CH<sub>3</sub>NH + H → CH<sub>3</sub>NH<sub>2</sub></td><td>0</td></tr><tr><td>CH<sub>2</sub>NH<sub>2</sub> + H → CH<sub>3</sub>NH<sub>2</sub></td><td>0</td></tr><tr><td>N + CH<sub>3</sub> → CH<sub>2</sub>NH</td><td>0</td></tr><tr><td>NH + CH<sub>2</sub> → CH<sub>2</sub>NH</td><td>0</td></tr><tr><td>NH<sub>2</sub> + CH → CH<sub>2</sub>NH</td><td>0</td></tr><tr><td>NH<sub>2</sub> + CH<sub>3</sub> → CH<sub>3</sub>NH<sub>2</sub></td><td>0</td></tr></tbody></table>

Note. Dust surface reactions related to CH₂NH are shown. Here, Eₐ represents the value of the activation barrier. Since radical species are so reactive, radical–radical reactions would have no activation barriers. The activation barriers for HCN and CH₂NH were cited in the theoretical study by Woon (2002).

### 3.3.8. DR21(OH)

Although the spectrum obtained for this source was limited from 103 to 105 GHz, CH₃OH and HCOOCH₃ were detected. We avoid discussing the spatial structure of this source from line parameters, since only three lines were available in total and their signal-to-noise ratios (S/N) were not low. Their abundances were obtained by assuming an excitation temperature of 150 K, based on Ikeda et al. (2001).

## 4. Evaluation by Chemical Modeling

### 4.1. The Chemical Model

To simulate the abundance of various COMs in hot cores, the NAUTILUS gas–grain chemical model (Ruaud et al. 2016) was used with the fast warm-up model presented in Garrod (2013). This chemical model computes the time evolution of species in three phases: gas phase, grain surface, and grain mantle. All of the physicochemical processes included in the model can be found with their corresponding equations in Ruaud et al. (2016). The gas-phase chemistry is described by the public network kida.uva.2014 (Wakelam et al. 2015). We incorporated reactions regarding CH₂NH and CH₃NH₂ from

Suzuki et al. (2016) and reactions for COMs from Garrod (2013). The binding energies for the species of interest are shown in Table 7. The important chemical reactions, cited from kida.uva.2014, Suzuki et al. (2016), and Garrod (2013) for the species of interest, are summarized in Tables 8 and 9.

For the initial composition, we used the initial abundances from Ruaud et al. (2016) assuming that the chemical evolution started from atomic form, except for H₂. Elements with an ionization potential below 13.6 eV, or hydrogen, C, S, Si, Fe, Na, Mg, Cl, and P, were initially singly ionized.

### 4.2. Physical Model

The physical evolution starts from a diffuse cloud phase, where gas density is increased by gravitational collapse. This phase is called the collapsing phase. The initial gas density, *n*, was increased up to the peak density as a function of time, *t*, along with the modified free-fall differential equation shown below (Nejad et al. 1990):

$$ \frac{dn}{dt} = B \left(\frac{n^4}{n_i}\right)^{1/3} \left\{ 24\pi G m_H n_i \left[\left(\frac{n}{n_i}\right)^{1/3} - 1\right] \right\}^{1/2}, \quad (8) $$

where $n_i$ is the initial density, $m_H$ is the mass of the hydrogen atom, and G is the gravitational constant. However, the actual gravitational collapse would be somewhat slowed down from a free-fall process by the resistance of turbulence, thermal motion, or a magnetic field. Thus, the collapse speed is adjusted by a parameter B. The factor B = 1 corresponds to the usual free-fall case. Values of B smaller than unity are used to assume the situation of non-free-fall cases, as Garrod (2013) employed B = 0.7 assuming that internal physical processes would be working against a free-fall process. While the gas kinetic temperature was fixed at 10 K in this collapsing phase, the dust temperature, T_dust, decreased from 19 to 8 K, as was presented in Garrod & Pauly (2011).

Once the peak density was achieved, we fixed the density, and the gas and dust temperatures were raised to their peak temperatures. After that, chemical evolution continued while fixing the temperature and density to their peak values.

In Section 4.3, we will discuss potentially important parameters in our modeling, by changing the initial density, *n*ᵢ, the parameter *B*, the peak density, the timescale of the warm-up phase, and the peak temperature. If one of these factors largely contributes to differences in the chemical compositions of hot cores, they may be keys to explaining the observed chemical differences.

### 4.3. Parameter Dependence of the Chemical Network
Simulations

#### 4.3.1. Methodology

To discuss the difference in modeling results under different conditions, we computed the “degree of proximity” (DoP) at each time step using the following formula:

$$ \text{DoP}(t) = \frac{1}{N_{\text{total}}} \sum_{i} |\log_{10} \frac{n_{A}(X)_{i}(t)}{n_{B}(X)_{i}(t)}|, \quad (9) $$

where $n_A(X)_i(t)$ and $n_B(X)_i(t)$ are the calculated abundances of species *i* at a certain time step *t*, with different models A and B,
and $N_{total}$ is the total number of species involved in the comparison. This formula will also be used to evaluate the distance from observational results to our modeling, by replacing $n_B(X)_i$ with observed fractional abundances. DoP is similar to the distance of disagreement: a smaller value of DoP means a better agreement between predicted abundances by modelings or observed abundances. Since the simulated fractional abundances range up to $10^{-5}$ to less than $10^{-10}$, the comparison using the squares of the difference tends to underestimate the importance of less abundant species. The comparison using a logarithm in the above formula has an advantage in giving the same weight for both overestimated and underestimated by a factor of $k (|\log_{10} k| = |\log_{10} k^{-1}|)$. This method has been employed by many authors since it was suggested by Wakelam et al. (2006). The observed species except for CH$_3$CHO were used to calculate DoPs since CH$_3$CHO would be in a low-temperature envelope considering its low excitation temperature (~20 K). We will use the derived abundances of observed COMs from Table 4 and CH$_2$NH from Suzuki et al. (2016).

The parameters to test their importance are the following: (1) initial densities of 0.1, 1, and 10 cm$^{-3}$; (2) warm-up timescales of 7.1 × 10$^2$, 7.1 × 10$^3$, and 7.1 × 10$^4$ years; (3) peak densities of 1 × 10$^6$, 1 × 10$^7$, and 1 × 10$^8$ cm$^{-3}$; (4) degree of resistance to gravitational collapse, B, of 1, 0.7, 0.2, and 0.1; and (5) peak temperatures of 30, 60, 90, 120, 150, and 200 K. We calculated DoPs compared to a standard simulation, which employed an initial density of 1 cm$^{-3}$, B = 0.7, peak density of 1 × 10$^7$ cm$^{-3}$, warm-up timescale of 7.1 × 10$^4$ years, and peak temperature of 200 K. The calculated DoPs are shown in Figure 5. A timescale longer than 1 × 10$^6$ years is doubtful for the lifetime of hot cores (Wilner et al. 2001). Within this timescale, DoPs are small at any time in Figures 5 (1)–(4). By contrast, DoPs were quite large under the different temperatures in Figure 5 (5), suggesting that the peak temperature would be a key parameter to change the chemical compositions of hot cores.

In Figure 6, the simulated abundances of COMs were compared under the different temperatures ranging from 30 K to 200 K. The different degree of depletion of each species can be explained by the following:

1. Each species has different binding energies, resulting in different evaporation rates.

2. Some COMs were nonthermally liberated from grains with the formation heat (Garrod et al. 2007). For instance, radicals such as OH, CH$_3$, and HCO were not evaporated if the temperature was low (~60 K), leading to the formation of some kinds of COMs like CH$_3$OCH$_3$ and HCOOCH$_3$ through thermal hopping, and some of the products were released at that time due to the reaction heat.

3. If species were susceptible to hydrogenation processes, they were converted on grain surfaces to more complex molecules when the temperature is low. Such species, CH$_2$CHCN, NH$_2$CHO, and CH$_2$NH, tend to decrease through the following hydrogenation processes (Theule et al. 2011 and Suzuki et al. 2016 for CH$_2$NH, Caselli et al. 1993 for CH$_2$CHCN, and Noble et al. 2015 for NH$_2$CHO):

$$ \begin{aligned} \mathrm{CH_2NH} + \mathrm{H} &\rightarrow \mathrm{CH_2NH_2} \\ \mathrm{CH_2CHCN} + \mathrm{H} &\rightarrow \mathrm{CH_2CH_2CN} \\ \mathrm{NH_2CHO} + \mathrm{H} &\rightarrow \mathrm{HNCHO} + \mathrm{H_2}. \end{aligned} $$

### 4.4. Comparison with Observed Data

In this section, we will discuss if observed abundances can be explained with the different structures of the temperature inside the hot cores. For comparison, we selected two representative hot cores, G10.47+0.03 and NGC 6334F. G10.47+0.03 is rich in N-bearing species compared to NGC 6334F, providing us with preferable samples to discuss chemical differences. In addition to the observed abundances of CH$_3$OH, HCOOCH$_3$, CH$_3$OCH$_3$, (CH$_3$)$_2$CO, CH$_2$CHCN, and NH$_2$CHO in our survey, we will use the abundances of CH$_2$NH for these sources from Suzuki et al. (2016), where CH$_2$NH abundances of G10.47+0.03 and NGC 6334F were reported to be $3.1 \times 10^{-8}$ and $2.4 \times 10^{-9}$. Although CH$_2$CH$_2$CN is observed, this species is not included in the calculation of DoP since further discussion would be needed of CH$_2$CH$_2$CN chemistry.

In actual hot cores, there would be a temperature gradient from the inner hot region to the outer warm region. We approximately represented this temperature gradient in hot cores with a two-layer model, where the temperature of the inner core is fixed at 200 K and a warm region with lower temperature surrounds the inner core. Although this hot core would be further surrounded by the cold envelope, we did not consider the contribution of the envelope in this model. The temperature and volume of the warm region were free parameters in this model. The temperatures of the warm region, $T_{warm}$, were set to be 30, 60, 90, 120, and 150 K. The volume ratio of the 200 K and warm regions, $V_{warm}/V_{200 K}$, was assumed to be 1, 10, 100, and 1000, to represent the different temperature structures of hot cores. Then the chemical compositions are calculated as $\frac{X_{200 K} V_{200 K} + X_{warm} V_{warm}}{V_{200 K} + V_{warm}}$, where $X_{warm}$ and $X_{200 K}$ respectively represent the simulated fractional abundances under temperatures of $T_{warm}$ and 200 K. In this calculation, the ratio of $V_{warm}/V_{200 K}$ does not depend on the distance to the sources from the Earth, since both volumes $V_{warm}$ and $V_{200 K}$ will proportionally decrease with the distance.

With these simulated abundances, the DoPs for G10.47+0.03 and NGC 6334F under the different $T_{warm}$ and $V_{warm}/V_{200 K}$ were calculated along with the physical evolution of the core. In Figure 7, the time evolution of DoPs under $T_{warm} = 120$ K was compared by assuming the different volume ratios of $V_{warm}/V_{200 K}$. While DoPs of G10.47+0.03 showed minimum values at $8.0 \times 10^5$ years and $V_{warm}/V_{200 K}$ of 100, the minimum of DoP for NGC 6334F was achieved at $6.5 \times 10^5$ years and $V_{warm}/V_{200 K}$ of 1000. The values of DoP and its best age are associated with an error due to the uncertainties in observed abundance. While chemical reactions in our models also contain uncertainties with their reaction coefficients, we neglect such error of chemistry to determine the best model since we have employed the identical chemical data set for all models and the uncertainties of DoP among models are determined only by the error of observed abundances. Then the propagation of the error in Figure 4 associated with the abundances of species gives us an error of DoP of 0.04 for G10.47+0.03 and 0.05 for NGC 6334F. With these errors, we summarize the minimum values of DoPs achieved under other combinations of $T_{warm}$ and $V_{warm}/V_{200 K}$ in Tables 10 and 11. Finally, we found that ($T_{warm}$,
<figure><img src="image_9.png" /><figcaption>**Figure 5.** We calculated DoPs compared to a standard model, which employed an initial density of 1 cm⁻³, *B* = 0.7, peak density of 1 × 10⁷ cm⁻³, warm-up timescale of 7.1 × 10⁴ years, and peak temperature of 200 K. Time zero corresponds to the beginning of the warm-up phase. The calculated DoPs are shown for cases of (1) initial densities of 0.1 and 10 cm⁻³; (2) warm-up timescales of 7.1 × 10² and 7.1 × 10⁵ years; (3) peak densities of 1 × 10⁶ and 1 × 10⁸ cm⁻³; (4) degree of resistance to gravitational collapse, *B*, of 1, 0.2, and 0.1; and (5) peak temperatures of 30, 60, 90, 120 and 150 K. The DoPs for the 30, 60, and 90 K models in (3) were higher than 3.0.</figcaption></figure>

$V_{\text{warm}}/V_{200\,\text{K}}$) = (120 K, 1000) for NGC 6334F was the best combination of the parameters to explain the observed abundances. For G10.47+0.03, both ($T_{\text{warm}}$, $V_{\text{warm}}/V_{200\,\text{K}}$) = (120 K, 100) and (120 K, 10) were appropriate under the error of 0.05. The combinations of these best values are shown in boldface in Tables 10 and 11. The temperature of 120 K decreased the abundances of CH₂NH, CH₂CHCN, and NH₂CHO more than CH₃OH and CH₃OCH₃ through the absorption of these species and grain surface reactions. For the age of the core, our results indicated that G10.47+0.03 is more evolved than NGC 6334F, whereas a hot region would be larger than NGC 6334F. The abundances of CH₃OH, HCOOCH₃, and CH₃OCH₃ decrease via destruction reactions

in the gas phase, whereas those of CH₂NH, CH₂CHCN, and NH₂CHO increase through formation processes in the gas phase. Therefore, observed N-bearing species tend to be rich in the evolved hot cores.

The best simulated abundances were compared with our observed abundances in Table 12. The letters “S” and “o” respectively represent simulated abundance and observed abundance. Observed abundances are presented in boldface if the difference from the simulated one is within a factor of 10. We found that the observed abundances for most of the species can be explained by our chemical model, except for underestimation of HCOOCH₃ and overestimation of NH₂CHO in NGC 6334F. These discrepancies would come from the
<figure><img src="image_10.png" /><figcaption>**Figure 6.** Comparison of abundances of COMs simulated under the different peak temperatures of 30, 60, 90, 120, 150, and 200 K. We added the time evolution of CH<sub>2</sub>NH to compare with the observational results of Suzuki et al. (2016).</figcaption></figure>
<figure><img src="image_11.png" /><figcaption>**Figure 7.** DoPs under $V_{120\text{K}}/V_{200\text{K}} = 1, 10, 100$, and $1000$ were calculated for $G10.47+0.03$ and NGC 6334F. A smaller $V_{120\text{K}}/V_{200\text{K}}$ represents a core where a high-temperature region is dominant.</figcaption></figure>

<table><caption>**Table 10**
DoPs for $G10.47+0.03$</caption><thead><tr><th rowspan="2">T<sub>warm</sub></th><th colspan="4">V<sub>warm</sub>/V<sub>200 K</sub></th></tr><tr><th>1</th><th>10</th><th>100</th><th>1000</th></tr></thead><tbody><tr><td>30 K</td><td>1.05</td><td>0.83</td><td>0.76</td><td>1.27</td></tr><tr><td>60 K</td><td>1.05</td><td>0.83</td><td>0.73</td><td>1.10</td></tr><tr><td>90 K</td><td>1.05</td><td>0.83</td><td>0.75</td><td>1.09</td></tr><tr><td>120 K</td><td>0.99</td><td><strong>0.68</strong></td><td><strong>0.66</strong></td><td>0.81</td></tr><tr><td>150 K</td><td>1.04</td><td>0.95</td><td>1.05</td><td>1.18</td></tr></tbody></table>

**Note.** The temperature gradient inside the hot core was represented by 200 K and warmer regions. DoPs for $G10.47+0.03$ under the different volume ratios $V_{\text{warm}}/V_{200\text{K}}$ and the different temperatures for the warm region, $T_{\text{warm}}$. The combination of the best temperature and volume ratio is shown in boldface.

<table><caption>**Table 11**
DoPs for NGC 6334F</caption><thead><tr><th rowspan="2">T<sub>warm</sub></th><th colspan="4">V<sub>warm</sub>/V<sub>200 K</sub></th></tr><tr><th>1</th><th>10</th><th>100</th><th>1000</th></tr></thead><tbody><tr><td>30 K</td><td>1.25</td><td>1.10</td><td>1.20</td><td>1.56</td></tr><tr><td>60 K</td><td>1.24</td><td>1.10</td><td>1.16</td><td>1.39</td></tr><tr><td>90 K</td><td>1.24</td><td>1.21</td><td>1.06</td><td>1.24</td></tr><tr><td>120 K</td><td>1.26</td><td>1.24</td><td>1.03</td><td><strong>0.86</strong></td></tr><tr><td>150 K</td><td>1.25</td><td>1.15</td><td>1.17</td><td>1.19</td></tr></tbody></table>

**Note.** The temperature gradient inside the hot core was represented by 200 K and warmer regions. DoPs for NGC 6334F under the different volume ratios $V_{\text{warm}}/V_{200\text{K}}$ and the different temperatures for the warm region, $T_{\text{warm}}$. The combination of the best temperature and volume ratio is shown in boldface.

uncertainties that are associated with the desorption energies and a very simplified physical structure.

Are the observed correlations in Table 5 explained by our model by assuming the different temperature structures inside hot cores or their different ages? In this paper, we reported the interesting correlation between CH$_3$OH, HCOOCH$_3$, and CH$_3$OCH$_3$, and between CH$_2$NH, CH$_2$CHCN, and NH$_2$CHO, respectively. With the two-layer model, if we change the ratio of $V_{\text{warm}}/V_{200\text{K}}$ by fixing the age of the core to $8.0 \times 10^5$ years and $T_{\text{warm}}$ to 120 K, the fractional abundances of CH$_2$NH, CH$_2$CHCNs, and NH$_2$CHO are almost linearly decreased, leading the correlation coefficients among these

<table><caption>**Table 12**
Comparison of Simulated Abundances with Observed Abundances</caption><thead><tr><th>Species</th><th>G10 (s)</th><th>G10 (o)</th><th>N63 (s)</th><th>N63 (o)</th></tr></thead><tbody><tr><td>CH<sub>3</sub>OH</td><td>3.0 (-7)</td><td><strong>3.5</strong> (-7)</td><td>9.6 (-7)</td><td><strong>9.0</strong> (-7)</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>2.0 (-8)</td><td><strong>2.3</strong> (-8)</td><td>5.0 (-10)</td><td>4.7 (-7)</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>7.3 (-8)</td><td><strong>1.3</strong> (-8)</td><td>1.7 (-7)</td><td><strong>4.3</strong> (-8)</td></tr><tr><td>(CH<sub>3</sub>)<sub>2</sub>CO</td><td>4.1 (-9)</td><td><strong>2.5</strong> (-8)</td><td>9.2 (-9)</td><td><strong>2.1</strong> (-9)</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>2.8 (-8)</td><td><strong>1.0</strong> (-8)</td><td>9.6 (-9)</td><td>7.0 (-10)</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>1.6 (-9)</td><td><strong>1.1</strong> (-8)</td><td>3.9 (-10)</td><td><strong>2.9</strong> (-10)</td></tr><tr><td>CH<sub>2</sub>NH</td><td>3.9 (-8)</td><td><strong>1.8</strong> (-8)</td><td>8.4 (-9)</td><td><strong>1.2</strong> (-9)</td></tr></tbody></table>

**Note.** We searched for the best time (DoP is minimum) to explain the observed abundances toward $G10.47+0.03$ (denoted as G10) and NGC 6334F (denoted as N63) under the $V_{120\text{K}}/V_{200\text{K}}$ values of 1, 10, 100, and 1000. The simulated abundances and the observed abundances are compared under the best time and $V_{120\text{K}}/V_{200\text{K}}$ ratio, that is, $8.7 \times 10^5$ years and $V_{120\text{K}}/V_{200\text{K}} = 100$ for $G10.47+0.03$, and $8.2 \times 10^5$ years and $V_{120\text{K}}/V_{200\text{K}} = 1000$ for $G10.47+0.03$. Letters “s” and “o” respectively represent simulated abundance and observed abundance. A factor of 0.5 was multiplied by the observed fractional abundance to compare with simulated values. Observed abundances are presented in boldface if the difference from the simulated one is within a factor of 10.

species to be unity. While high correlation coefficients between N-bearing species are consistent with our observations, the different $V_{\text{warm}}/V_{200\text{K}}$ ratios could not explain the negative correlation coefficients between O- and N-bearing species. Another important factor for the correlations of molecular abundances would be the age of the core. In Table 13, we show the correlation coefficients between CH$_3$OH, HCOOCH$_3$, CH$_3$OCH$_3$, CH$_2$NH, CH$_2$CHCN, and NH$_2$CHO using the simulated abundances by the two-layer model in different ages, fixing $V_{\text{warm}}/V_{200\text{K}}$ at 100 and $T_{\text{warm}}$ at 120 K. In the calculation of correlation coefficients, we used the chemical compositions of different ages ranging from $1.0 \times 10^5$ to $1.0 \times 10^6$ years since the beginning of the warm-up phase by the interval of $5.0 \times 10^4$ years. While CH$_3$OH, HCOOCH$_3$, and CH$_3$OCH$_3$ showed high correlation coefficients, these O-bearing species have negative correlation coefficients with CH$_2$NH and CH$_2$CHCN. These results are consistent with our observational results. However, the correlation coefficients between CH$_3$OH and CH$_2$NH and CH$_2$CHCN are too low compared to our observations. In addition, NH$_2$CHO shows the correlation with CH$_3$OH and HCOOCH$_3$ rather than CH$_2$NH
<table><caption>**Table 13**
Predicted Correlation Coefficients between Observed Molecules</caption><thead><tr><th></th><th>HCOOCH<sub>3</sub></th><th>CH<sub>3</sub>OCH<sub>3</sub></th><th>NH<sub>2</sub>CHO</th><th>CH<sub>2</sub>CHCN</th><th>CH<sub>2</sub>NH</th></tr></thead><tbody><tr><td>CH<sub>3</sub>OH</td><td>0.48</td><td>0.74</td><td>0.22</td><td>-0.89</td><td>-0.79</td></tr><tr><td>HCOOCH<sub>3</sub></td><td>...</td><td>0.89</td><td>0.89</td><td>-0.78</td><td>-0.05</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>...</td><td>...</td><td>0.81</td><td>-0.90</td><td>-0.23</td></tr><tr><td>NH<sub>2</sub>CHO</td><td>...</td><td>...</td><td>...</td><td>-0.54</td><td>0.34</td></tr><tr><td>CH<sub>2</sub>CHCN</td><td>...</td><td>...</td><td>...</td><td>...</td><td>0.60</td></tr></tbody></table>

Note. We calculated the correlation coefficients with our chemical model under the different ages, fixing $V_{120 K}/V_{200 K}$ at 100 and $T_{\text{warm}}$ at 120 K. In the calculation of the correlation coefficients, the simulated abundances in the gas phase were employed in the different ages of the core, starting from $1 \times 10^5$ up to $1 \times 10^6$ years by the time interval of $1 \times 10^5$ years.

and CH$_2$CHCN, contradicting the observation. Therefore, the age of the core could only partly explain the observed correlations. We suggest that both the different ages of the cores and the $V_{\text{warm}}/V_{200 K}$ ratios would contribute to the observed correlations between CH$_3$OH, HCOOCH$_3$, CH$_3$OCH$_3$, CH$_2$NH, CH$_2$CHCN, and NH$_2$CHO.

Although our model successfully explains the observed abundances, the temperature of 120 K seems higher considering the observed excitation temperatures. Since our physical structure and its time evolution would be oversimplified, a revision of physical structure would also be key to improving our knowledge regarding the evolution of COMs. In addition, giving an older age to G10.47+0.03 than to NGC 6334F does not agree with Suzuki et al. (2016), where we suggested the possibility that G10.47+0.03 is more evolved than NGC 6334F based on the very weak hydrogen recombination line in G10.47+0.03. One possibility to explain this discrepancy would be that the distributions of molecules and hydrogen recombination do not overlap each other, and we have observed the different components simultaneously. Toward G10.47+0.03, Cesaroni et al. (2010) detected two HCHII regions indicative of the very early evolutionary phase of star formation. NGC 6334F is known to have a UCHII region and hot cores associated with molecular emission (SMA 3 and SMA 1 and 2, respectively, in Hunter et al. 2006). Considering the nondetection of the free-free emission in Hunter et al. (2006), the hot cores, SMA 1 and 2, are thought to be younger than SMA 3. However, a detailed comparison of the ages of hot cores in G10.47+0.03 and NGC 6334F is difficult with currently available data. Mapping observations of molecular emission and hydrogen recombination lines with ALMA will be helpful to resolving the detailed molecular distributions and their evolutionary phases for further discussion.

### 4.5. Comparison with Caselli et al. (1993)

It is worth discussing the difference between this work and the previous study by Caselli et al. (1993). They investigated the chemical differences between the Orion Hot Core and the Compact Ridge, where N- and O-bearing species are abundant, respectively. They prepared a Hot Core and a Compact Ridge model, where chemical evolution starts from 40 and 20 K, followed by a sudden increase of temperature to 200 K and 100 K, respectively. For the initial gas densities, densities of $1 \times 10^5$ and $2 \times 10^4 \text{ cm}^{-3}$ were employed for the Hot Core and Compact Ridge models. They found that N-bearing species such as CH$_2$CHCN and CH$_3$CH$_2$CN are more abundant in the Hot Core model than in the Compact Ridge model, since the higher temperature enables radicals to efficiently move to form C$_3$N, followed by successive hydrogenation to form

CH$_2$CHCN and CH$_3$CH$_2$CN. On the other hand, the abundance of CH$_3$OH was much higher in the Compact Ridge model, due to efficient hydrogenation processes. Other O-bearing species like CH$_3$OCH$_3$ and HCOOCH$_3$ were produced using the liberated CH$_3$OH after the warm-up phase.

While our result that the chemical difference between the Hot Core and Compact Ridge might be reconciled by temperature is consistent with Caselli et al. (1993), we emphasize the importance of temperature in a different way than Caselli et al. (1993). We assumed that the evolution of the cloud starts from the diffuse cloud phase, where the temperature and the density are as low as $1 \text{ cm}^{-3}$. This assumption would be more reasonable than the one in Caselli et al. (1993) as the initial condition for the evolution of the cores. In this case, CH$_3$OH is produced equally during the collapsing phase independent of the peak temperature in the subsequent warm-up phase, inconsistent with Caselli et al. (1993). Furthermore, in contrast to Caselli et al. (1993), the origins of CH$_3$OCH$_3$ and HCOOCH$_3$ in our model were not in the gas phase, due to the update of the rate coefficients of gas-phase reactions based on the current understanding that gas-phase recombination processes of positive ions are inefficient in producing COMs (Geppert et al. 2006).

In our model, the higher abundances of O-bearing species in the hot regions were simply due to their binding energies. For N-bearing species, our model suggests that the differences in the abundances were not due to the formation processes before the warm-up phase, as suggested by Caselli et al. (1993), but due to the evaporation rates after the warm-up. In this work, the difference in the chemical compositions is explained by the different temperatures after the warm-up phase. More N-bearing species, such as CH$_2$CHCN, NH$_2$CHO, and CH$_2$NH, are formed in the gas phase with an updated gas-phase chemical reaction data set than in Caselli et al. (1993). However, if the temperature is not high enough, some of the desorbed molecules are converted to more complex molecules on the grains. Therefore, the depletion of N-bearing species in the Compact Ridge can be explained by adsorption and the subsequent destruction process on grains under a lower temperature than in the Hot Core.

### 4.6. Chemistry in Hot Core Envelopes

We found the very low excitation temperature (~20 K) of CH$_3$CHO. In addition, NH$_2$CHO in W51 e1/e2 and CH$_2$CHCN in G34.3+0.2 clearly showed an excitation temperature lower than 40 K. These species would mainly exist in the envelope.

We performed chemical modeling assuming the condition of an envelope to see if we can explain the observed abundances of these species. We assumed a peak temperature of 30 K
and a peak density of $1 \times 10^6 \text{ cm}^{-3}$, and the other physical conditions and chemical reactions were fixed with our standard model. In Figure 8(a), we showed the simulated fractional abundances of CH$_3$CHO, CH$_2$CHCN, and NH$_2$CHO with the envelope model. We lowered the binding energies of these species by 500 and 1000 K, respectively, in Figures 8(b) and (c). Since thermal evaporation processes are negligible at 30 K, chemical desorption processes and photoevaporation by ultraviolet photons contribute to the liberation of frozen species on grains. We used the equations of nonthermal desorption processes from Garrod et al. (2007).

In Figure 8(a), the peak abundances of CH$_3$CHO and NH$_2$CHO were respectively $2.6 \times 10^{-10}$ and $1.9 \times 10^{-11}$, which are more than 10 times less than our observed abundances. Therefore, for these species, their observed fractional abundances were not explained at all. Their fractional abundances change only slightly even if we changed the binding energies in Figures 8(b) and (c), suggesting that their discrepancies would not be due to the uncertainties of the desorption energies.

We found that the peak of simulated fractional abundance of CH$_2$CHCN was $6.4 \times 10^{-10}$. Although the fractional abundance of CH$_2$CHCN was enhanced by a chemical desorption process in this case, we have to be careful regarding its efficiency since the latest modeling by Wakelam et al. (2017) claims that chemical desorption processes would be less effective than previously thought. It is obvious that further detailed studies are required on the chemistry in the envelope of hot cores.

## 5. Conclusion

The main results of this paper can be summarized as follows:

1. We conducted survey observations of COMs toward high-mass star-forming regions. We reported more than 1000 transitions of CH$_3$OH, HCOOCH$_3$, CH$_3$OCH$_3$, CH$_3$CHO, (CH$_3$)$_2$CO, NH$_2$CHO, CH$_2$CHCN, and CH$_3$CH$_2$CN. Their abundances and excitation temperatures were analyzed using the rotation diagram method and the least squares method.

2. In this work, we aimed to test whether different spatial distributions of N- versus O-bearing COMs could be probed by spatially unresolved data, as previous work (Blake et al. 1987) indicated a shift in radial velocities between N- and O-bearing species. Our results indicate that any existing velocity shifts are generally smaller than the uncertainties on the measured velocities and hence do not allow us to draw any conclusions on different spatial distributions of O- and N-bearing COMs from single-dish data. Future spatially resolved observations are therefore crucial to investigating the origin of the emission from N- and O-bearing COMs in hot cores.

3. Among our sources, NGC 6334F and W51 e1/e2 are richer in N-bearing species than O-bearing species. In addition, we found the possible correlations among N-bearing species based on our data. However, their significance levels were not high enough, except for “CH$_2$CHCN and NH$_2$CHO” and “CH$_3$CH$_2$CN and CH$_2$NH,” due to the limited number of sources. It would be very important to increase the number of sources to

confirm if such correlations are general in star-forming regions.

4. With our chemical modeling study, we searched for essential parameters of star-forming regions that may dramatically change the chemical evolution. Through simulations under different physical conditions, that is, initial densities, warm-up speed, peak density, timescale of collapsing phase, and peak temperatures, we found that different temperatures had a significant impact on the chemistry, while the effects from other parameters were small. With observed chemical compositions of G10.47 +0.03, and NGC 6334F, where N-bearing species are rich and not so rich, respectively, we discussed if the observed chemical difference can be explained by assuming different temperature structures and ages of the cores. As a result, by assuming that the high-temperature region (~200 K) is more dominant in G10.47 +0.03 than in NGC 6334F and G10.47+0.03 is more evolved than NGC 6334F, we succeeded in reproducing their observed abundances very well.

5. NH$_2$CHO, CH$_2$NH, and CH$_2$CHCN would be enhanced if the hot region inside the hot core is large since these species are susceptible to hydrogenation processes if the temperature is low. In addition, our modeling suggests that NH$_2$CHO, CH$_2$NH, and CH$_2$CHCN are produced after the completion of the warm-up phase, when CH$_3$OH, HCOOCH$_3$, and CH$_3$OCH$_3$ start to decrease. Therefore, the different ages of cores would also lead to the correlations and anticorrelations between observed O- and N-bearing species. We suggest that both the different temperature structures inside the core and their evolutionary phase contribute to the observed molecular correlations.

6. Our calculations suggest the importance of both gas-phase and grain surface chemistry of CH$_3$CH$_2$CN. We found that the current model tends to increase CH$_3$CH$_2$CN abundance under 120 K, which does not match with the observation. In addition, the possibility of a gas-phase formation process of C$_2$H$_6$ + CN → CH$_3$CH$_2$CN + H should be investigated.

7. CH$_3$CHO typically showed an excitation temperature of ~20 K, and NH$_2$CHO in W51 e1/e2 and CH$_2$CHCN in G34.3+0.2 showed an excitation temperature of ~30 K. The low excitation temperature of some COMs suggests that they exist in hot core envelopes. While our chemical model for envelopes suggests that CH$_2$CHCN can be nonthermally liberated from the envelope, our model could not reproduce the observed NH$_2$CHO and CH$_3$CHO at all. Further detailed studies would be required on the chemistry of hot core envelopes.

We are grateful to all of the staff members of the Nobeyama Radio Observatory, the National Astronomical Observatory of Japan (NAOJ), and the Arizona Radio Observatory for their support throughout our observations. We thank to Dr. Hideko Nomura and the staff at Bordeaux University for fruitful discussions. Part of the data analysis was made at the Astronomy Data Center, NAOJ. This research has made use of NASA's Astrophysics Data System. This study was supported by the Astrobiology Program of National Institutes of Natural Sciences (NINS) and by JSPS Kakenhi grants
<figure><img src="image_12.png" /><figcaption>**Figure 8.** Chemical modeling of NH<sub>2</sub>CHO, CH<sub>3</sub>CHO, and CH<sub>2</sub>CHCN for envelopes of hot cores. We assumed a peak temperature of 30 K and a peak density of 1 × 10<sup>6</sup> cm<sup>-2</sup>. In (b) and (c), we lowered the binding energies of these species by 500 K and 1000 K, respectively.</figcaption></figure>

15H03646 and 14J03618. Valentine Wakelam acknowledge the European Research Council (3DICE, grant agreement 336474) and the CNRS program "Physique et Chimie du Milieu Interstellaire" (PCMI) cofunded by the Centre National d'Etudes Spatiales (CNES). Liton Majumdar acknowledges support from the NASA postdoctoral program. A portion of this research was carried out at the Jet Propulsion Laboratory,

California Institute of Technology, under a contract with the National Aeronautics and Space Administration.

## Appendix

In this appendix, we summarize the line parameters of COMs from Tables 14 to 21.
<table><caption>Table 14
Observed Lines toward G10.47+0.03</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δν (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td rowspan="20">CH<sub>3</sub>OH</td><td>80.99371</td><td>80.99324</td><td>7(2)-8(1) A<sup>-</sup></td><td>103</td><td>2.5</td><td>488</td><td>9.9</td><td>66.3</td><td>9</td></tr><tr><td>81.65344</td><td>81.65293</td><td>18(4)-19(3) E</td><td>493</td><td>5.9</td><td>228</td><td>9.9</td><td>66.1</td><td>8</td></tr><tr><td>84.42421</td><td>84.42378</td><td>13(-3)-14(-2) E</td><td>274</td><td>4.3</td><td>262</td><td>9.7</td><td>66.5</td><td>6</td></tr><tr><td>84.52160</td><td>84.52117</td><td>5(1)-4(0) E</td><td>40</td><td>3.1</td><td>1022</td><td>8.0</td><td>66.5</td><td>16</td></tr><tr><td>84.74446</td><td>84.74390</td><td>19(4)-18(5) E</td><td>537</td><td>5.2</td><td>111</td><td>13.0</td><td>66.0</td><td>11</td></tr><tr><td>86.61607</td><td>86.61560</td><td>7(2)-6(3) A<sup>-</sup></td><td>103</td><td>1.4</td><td>515</td><td>9.8</td><td>66.4</td><td>15</td></tr><tr><td>86.90346</td><td>86.90295</td><td>7(2)-6(3) A<sup>+</sup></td><td>103</td><td>1.4</td><td>560</td><td>9.8</td><td>66.2</td><td>14</td></tr><tr><td>88.94051</td><td>88.93999</td><td>15(3,12)-14(4) A<sup>-</sup></td><td>328</td><td>4.2</td><td>404</td><td>9.5</td><td>66.3</td><td>13</td></tr><tr><td>89.50643</td><td>89.50581</td><td>8(-4)-9(-3) E</td><td>171</td><td>1.6</td><td>514</td><td>10.2</td><td>65.9</td><td>10</td></tr><tr><td>95.91483</td><td>95.91431</td><td>2(1)-1(1) A<sup>+</sup></td><td>21</td><td>1.2</td><td>682</td><td>8.3</td><td>66.4</td><td>13</td></tr><tr><td>96.74019</td><td>96.73936</td><td>2(-1)-1(-1) E</td><td>13</td><td>1.2</td><td>1690</td><td>9.0</td><td>65.4</td><td>16</td></tr><tr><td>96.74222</td><td>96.74138</td><td>2(0)-1(0) A<sup>+</sup></td><td>7</td><td>1.6</td><td>1264</td><td>5.5</td><td>65.4</td><td>12</td></tr><tr><td>96.74507</td><td>96.74455</td><td>2(0)-1(0) E</td><td>20</td><td>1.6</td><td>992</td><td>7.8</td><td>66.4</td><td>18</td></tr><tr><td>96.75602</td><td>96.75551</td><td>2(1)-1(1) E</td><td>28</td><td>1.2</td><td>707</td><td>8.8</td><td>66.4</td><td>16</td></tr><tr><td>100.63947</td><td>100.63890</td><td>13(2)-12(3) E</td><td>234</td><td>3.8</td><td>552</td><td>9.8</td><td>66.3</td><td>13</td></tr><tr><td>103.38174</td><td>103.38115</td><td>12(2)-12(1) E</td><td>207</td><td>0.8</td><td>279</td><td>10.7</td><td>66.3</td><td>18</td></tr><tr><td>104.06116</td><td>104.06066</td><td>13(-3)-12(-4) E</td><td>274</td><td>3.3</td><td>378</td><td>10.1</td><td>66.5</td><td>15</td></tr><tr><td>104.33701</td><td>104.33656</td><td>13(-2)-13(1) E</td><td>237</td><td>1.2</td><td>329</td><td>10.2</td><td>66.7</td><td>19</td></tr><tr><td>104.35542</td><td>104.35482</td><td>10(-4)-11(3) A<sup>-</sup></td><td>208</td><td>2.5</td><td>446</td><td>10.5</td><td>66.3</td><td>17</td></tr><tr><td>105.06433</td><td>105.06369</td><td>13(1)-12(2) A<sup>+</sup></td><td>224</td><td>4.3</td><td>491</td><td>10.0</td><td>66.2</td><td>15</td></tr><tr><td>105.57686</td><td>105.57629</td><td>14(-2)-14(1) E</td><td>270</td><td>1.8</td><td>361</td><td>9.0</td><td>66.4</td><td>15</td></tr><tr><td rowspan="20">HCOOCH<sub>3</sub></td><td>79.78208</td><td>79.78227</td><td>7(0,7)-6(0,6)E</td><td>16</td><td>18.4</td><td>114</td><td>8.7</td><td>68.7</td><td>7</td></tr><tr><td>79.78432</td><td>79.78391</td><td>7(0,7)-6(0,6)A</td><td>16</td><td>18.4</td><td>95</td><td>7.1</td><td>66.5</td><td>5</td></tr><tr><td>86.02165</td><td>86.02165</td><td>7(5,2)-6(5,1)E</td><td>33</td><td>9.2</td><td>41</td><td>9.5</td><td>68.0</td><td>5</td></tr><tr><td>86.02965</td><td>86.02966</td><td>7(5,2)-6(5,1)A</td><td>33</td><td>9.2</td><td>79</td><td>11.9</td><td>68.1</td><td>7</td></tr><tr><td>blend</td><td>86.03021</td><td>7(5,3)-6(5,2)A</td><td>33</td><td>9.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>88.84352</td><td>88.84349</td><td>7(1,6)-6(1,5)E</td><td>18</td><td>18.2</td><td>108</td><td>10.6</td><td>67.9</td><td>9</td></tr><tr><td>88.85214</td><td>88.85208</td><td>7(1,6)-6(1,5)A</td><td>18</td><td>18.2</td><td>114</td><td>8.8</td><td>67.8</td><td>10</td></tr><tr><td>blend</td><td>89.31459</td><td>8(1,8)-7(1,7)E</td><td>20</td><td>21.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>89.31643</td><td>89.31667</td><td>8(1,8)-7(1,7)A</td><td>20</td><td>21.0</td><td>268</td><td>13.1</td><td>68.8</td><td>11</td></tr><tr><td>96.07718</td><td>96.07726</td><td>8(2,7)-7(2,6)A</td><td>24</td><td>20.0</td><td>92</td><td>9.9</td><td>68.2</td><td>10</td></tr><tr><td>100.29514</td><td>100.29514</td><td>8(3,5)-7(3,4)E</td><td>27</td><td>18.4</td><td>137</td><td>8.8</td><td>68.0</td><td>9</td></tr><tr><td>100.30879</td><td>100.30879</td><td>8(3,5)-7(3,4)A</td><td>27</td><td>18.4</td><td>142</td><td>9.0</td><td>68.0</td><td>9</td></tr><tr><td>100.48265</td><td>100.48265</td><td>8(1,7)-7(1,6)E</td><td>23</td><td>20.8</td><td>206</td><td>8.9</td><td>68.0</td><td>10</td></tr><tr><td>100.49149</td><td>100.49150</td><td>8(1,7)-7(1,6)A</td><td>23</td><td>20.8</td><td>193</td><td>8.4</td><td>68.0</td><td>7</td></tr><tr><td>blend</td><td>100.68148</td><td>9(0,9)-8(0,8)A</td><td>25</td><td>23.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>100.68295</td><td>100.68339</td><td>9(0,9)-8(0,8)E</td><td>25</td><td>23.7</td><td>239</td><td>11.6</td><td>69.3</td><td>11</td></tr><tr><td>103.46729</td><td>103.46729</td><td>8(2,6)-7(2,5)E</td><td>25</td><td>20.2</td><td>152</td><td>7.5</td><td>68.0</td><td>13</td></tr><tr><td>103.47927</td><td>103.47927</td><td>8(2,6)-7(2,5)A</td><td>25</td><td>20.2</td><td>141</td><td>8.8</td><td>68.0</td><td>16</td></tr><tr><td rowspan="20">CH<sub>3</sub>OCH<sub>3</sub></td><td>blend</td><td>78.85627</td><td>13(2,11)-13(1,12)EA</td><td>90</td><td>73.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>78.85627</td><td>13(2,11)-13(1,12)AE</td><td>90</td><td>109.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>78.85820</td><td>78.85782</td><td>13(2,11)-13(1,12)EE</td><td>90</td><td>293.0</td><td>155</td><td>15.9</td><td>66.5</td><td>7</td></tr><tr><td>blend</td><td>78.85937</td><td>13(2,11)-13(1,12)AA</td><td>90</td><td>183.1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>81.36897</td><td>21(5,16)-20(6,15)AA</td><td>246</td><td>47.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>81.37050</td><td>81.37051</td><td>21(5,16)-20(6,15)EE</td><td>246</td><td>75.6</td><td>26</td><td>4.5</td><td>68.0</td><td>7</td></tr><tr><td>81.37255</td><td>81.37191</td><td>21(5,16)-20(6,15)AE</td><td>246</td><td>28.4</td><td>15</td><td>6.8</td><td>65.7</td><td>7</td></tr><tr><td>blend</td><td>81.37217</td><td>21(5,16)-20(6,15)EA</td><td>246</td><td>18.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>81.46762</td><td>18(4,15)-17(5,12)AA</td><td>178</td><td>41.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>81.46997</td><td>81.46992</td><td>18(4,15)-17(5,12)EE</td><td>178</td><td>66.4</td><td>18</td><td>8.5</td><td>67.8</td><td>6</td></tr><tr><td>81.47159</td><td>81.47207</td><td>18(4,15)-17(5,12)EA</td><td>178</td><td>16.5</td><td>16</td><td>8.6</td><td>69.8</td><td>5</td></tr><tr><td>blend</td><td>81.47239</td><td>18(4,15)-17(5,12)AE</td><td>178</td><td>24.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>84.52710</td><td>18(4,14)-17(5,13)AA</td><td>179</td><td>25.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>84.53055</td><td>84.52959</td><td>18(4,14)-17(5,13)EE</td><td>179</td><td>66.6</td><td>19</td><td>17.0</td><td>64.6</td><td>9</td></tr><tr><td>blend</td><td>84.53193</td><td>18(4,14)-17(5,13)AE</td><td>179</td><td>8.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>84.53225</td><td>18(4,14)-17(5,13)EA</td><td>179</td><td>16.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>84.63190</td><td>3(2,1)-3(1,2)AE</td><td>11</td><td>16.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>84.63227</td><td>3(2,1)-3(1,2)EA</td><td>11</td><td>10.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>84.63472</td><td>84.63441</td><td>3(2,1)-3(1,2)EE</td><td>11</td><td>43.7</td><td>45</td><td>16.7</td><td>66.9</td><td>5</td></tr><tr><td>blend</td><td>84.63674</td><td>3(2,1)-3(1,2)AA</td><td>11</td><td>27.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>90.93751</td><td>6(0,6)-5(1,5)AA</td><td>19</td><td>32.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>90.93867</td><td>90.93810</td><td>6(0,6)-5(1,5)EE</td><td>19</td><td>86.2</td><td>198</td><td>10.4</td><td>66.1</td><td>10</td></tr><tr><td>blend</td><td>90.93870</td><td>6(0,6)-5(1,5)AE</td><td>19</td><td>10.8</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>90.93870</td><td>6(0,6)-5(1,5)EA</td><td>19</td><td>21.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δν (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td rowspan="25">(CH<sub>3</sub>)<sub>2</sub>CO</td><td>blend</td><td>92.69614</td><td>8(5,4)-9(4,5)AE</td><td>68</td><td>5.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>92.69897</td><td>8(5,3)-9(4,5)EA</td><td>68</td><td>3.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>92.70196</td><td>8(5,3)-9(4,5)EE</td><td>68</td><td>12.0</td><td>27</td><td>11.0</td><td>67.1</td><td>4</td></tr><tr><td>blend</td><td>92.70307</td><td>8(5,4)-9(4,5)AA</td><td>68</td><td>9.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>96.84724</td><td>5(2,4)-5(1,5)EA</td><td>19</td><td>16.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>96.84729</td><td>5(2,4)-5(1,5)AE</td><td>19</td><td>8.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>96.85040</td><td>96.84988</td><td>5(2,4)-5(1,5)EE</td><td>19</td><td>65.6</td><td>72</td><td>16.8</td><td>66.4</td><td>5</td></tr><tr><td>blend</td><td>96.85250</td><td>5(2,4)-5(1,5)AA</td><td>19</td><td>24.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>96.92805</td><td>17(8,10)-18(7,12)EE</td><td>229</td><td>40.7</td><td>...</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>96.92934</td><td>17(8,10)-18(7,11)AA</td><td>229</td><td>15.7</td><td>20</td><td>9.9</td><td>67.8</td><td>11</td></tr><tr><td>blend</td><td>96.92937</td><td>17(8,9)-18(7,12)AA</td><td>229</td><td>26.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>96.92979</td><td>17(8,10)-18(7,11)AE</td><td>229</td><td>5.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>96.92989</td><td>17(8,9)-18(7,12)AE</td><td>229</td><td>15.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>96.93111</td><td>17(8,9)-18(7,11)EE</td><td>229</td><td>40.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>96.93291</td><td>17(8,9)-18(7,11)EA</td><td>229</td><td>10.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>99.32436</td><td>4(1,4)-3(0,3)EA</td><td>10</td><td>17.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>99.32436</td><td>4(1,4)-3(0,3)AE</td><td>10</td><td>26.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>99.32577</td><td>99.32521</td><td>4(1,4)-3(0,3)EE</td><td>10</td><td>69.8</td><td>241</td><td>10.9</td><td>66.3</td><td>7</td></tr><tr><td>blend</td><td>99.32606</td><td>4(1,4)-3(0,3)AA</td><td>10</td><td>43.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>100.46041</td><td>6(2,5)-6(1,6)EA</td><td>25</td><td>19.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>100.46044</td><td>6(2,5)-6(1,6)AE</td><td>25</td><td>28.8</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>100.46361</td><td>100.46307</td><td>6(2,5)-6(1,6)EE</td><td>25</td><td>76.9</td><td>146</td><td>14.1</td><td>66.4</td><td>10</td></tr><tr><td>blend</td><td>100.46571</td><td>6(2,5)-6(1,6)AA</td><td>25</td><td>48.1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>100.94684</td><td>19(4,16)-18(5,13)AA</td><td>196</td><td>27.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>100.94935</td><td>100.94900</td><td>19(4,16)-18(5,13)EE</td><td>196</td><td>71.9</td><td>35</td><td>11.8</td><td>67.0</td><td>7</td></tr><tr><td>blend</td><td>100.95109</td><td>19(4,16)-18(5,13)EA</td><td>196</td><td>18.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>100.95125</td><td>19(4,16)-18(5,13)AE</td><td>196</td><td>9.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>104.17791</td><td>104.17587</td><td>17(2,15)-17(1,16)EA</td><td>148</td><td>79.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>104.17587</td><td>17(2,15)-17(1,16)AE</td><td>148</td><td>119.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>104.17791</td><td>104.17738</td><td>17(2,15)-17(1,16)EE</td><td>148</td><td>318.3</td><td>216</td><td>13.7</td><td>66.5</td><td>16</td></tr><tr><td>blend</td><td>104.17889</td><td>17(2,15)-17(1,16)AA</td><td>148</td><td>198.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>105.76828</td><td>13(1,12)-13(0,13)EA</td><td>86</td><td>36.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>105.76828</td><td>13(1,12)-13(0,13)AE</td><td>86</td><td>55.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>105.77078</td><td>105.77034</td><td>13(1,12)-13(0,13)EE</td><td>86</td><td>146.7</td><td>146</td><td>14.6</td><td>66.8</td><td>18</td></tr><tr><td>blend</td><td>105.77240</td><td>13(1,12)-13(0,13)AA</td><td>86</td><td>91.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td rowspan="15">NH<sub>2</sub>CHO</td><td>92.72787</td><td>92.72790</td><td>9(0,9)-8(1,8)AE</td><td>23</td><td>72.0</td><td>34</td><td>12.5</td><td>68.1</td><td>5</td></tr><tr><td>blend</td><td>92.72791</td><td>9(1,9)-8(0,8)AE</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>92.72795</td><td>9(0,9)-8(1,8)EA</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>92.72795</td><td>9(1,9)-8(0,8)EA</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>92.73603</td><td>92.73567</td><td>9(0,9)-8(1,8)EE</td><td>23</td><td>72.0</td><td>54</td><td>9.7</td><td>66.8</td><td>10</td></tr><tr><td>blend</td><td>92.73567</td><td>9(1,9)-8(0,8)EE</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>92.74398</td><td>92.74336</td><td>9(0,9)-8(1,8)AA</td><td>23</td><td>72.0</td><td>50</td><td>7.3</td><td>66.0</td><td>6</td></tr><tr><td>99.26684</td><td>99.26643</td><td>5(5,0)-4(4,1)AA</td><td>14</td><td>34.3</td><td>19</td><td>7.5</td><td>66.8</td><td>6</td></tr><tr><td>100.35044</td><td>100.35030</td><td>8(2,6)-7(3,5)EE</td><td>25</td><td>43.4</td><td>37</td><td>10</td><td>67.6</td><td>10</td></tr><tr><td>81.69384</td><td>81.69345</td><td>4(1,4)-3(1,3)</td><td>13</td><td>49.0</td><td>249</td><td>10.2</td><td>66.5</td><td>6</td></tr><tr><td>84.54279</td><td>84.54233</td><td>4(0,4)-3(0,3)</td><td>10</td><td>52.3</td><td>153</td><td>8.9</td><td>66.4</td><td>8</td></tr><tr><td>84.80825</td><td>84.80779</td><td>4(2,3)-3(2,2)</td><td>22</td><td>39.2</td><td>150</td><td>8.5</td><td>66.4</td><td>6</td></tr><tr><td>84.89041</td><td>84.88899</td><td>4(3,2)-3(3,1)</td><td>37</td><td>22.9</td><td>129</td><td>13.9</td><td>63.0</td><td>7</td></tr><tr><td>blend</td><td>84.89098</td><td>4(3,1)-3(3,0)</td><td>37</td><td>22.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>87.84931</td><td>87.84887</td><td>4(1,3)-3(1,2)</td><td>14</td><td>49.0</td><td>241</td><td>8.6</td><td>66.5</td><td>12</td></tr><tr><td>105.46468</td><td>105.46422</td><td>5(0,5)-4(0,4)</td><td>15</td><td>65.3</td><td>333</td><td>11.5</td><td>66.7</td><td>16</td></tr><tr><td>105.97343</td><td>105.97260</td><td>5(2,4)-4(2,3)</td><td>27</td><td>54.9</td><td>280</td><td>10.1</td><td>65.6</td><td>16</td></tr><tr><td>106.10827</td><td>106.10786</td><td>5(4,2)-4(4,1)</td><td>63</td><td>23.5</td><td>240</td><td>8.7</td><td>66.8</td><td>17</td></tr><tr><td>blend</td><td>106.10788</td><td>5(4,1)-4(4,0)</td><td>63</td><td>23.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>106.13511</td><td>106.13442</td><td>5(3,3)-4(3,2)</td><td>42</td><td>41.8</td><td>209</td><td>9.8</td><td>66.1</td><td>15</td></tr><tr><td>106.14198</td><td>106.14139</td><td>5(3,2)-4(3,1)</td><td>42</td><td>41.8</td><td>189</td><td>9.0</td><td>66.3</td><td>17</td></tr><tr><td rowspan="10">CH<sub>2</sub>CHCN</td><td>84.94625</td><td>84.94625</td><td>9(0,9)-8(0,8)</td><td>20</td><td>130.9</td><td>143</td><td>8.5</td><td>68.0</td><td>6</td></tr><tr><td>85.71571</td><td>85.71570</td><td>9(2,7)-8(2,6)</td><td>29</td><td>124.5</td><td>116</td><td>8.5</td><td>68.0</td><td>6</td></tr><tr><td>96.98244</td><td>96.98244</td><td>10(1,9)-9(1,8)</td><td>25</td><td>145.5</td><td>206</td><td>9.1</td><td>68.0</td><td>7</td></tr><tr><td>103.57570</td><td>103.57570</td><td>11(0 11)-10(0 10)</td><td>30</td><td>160.0</td><td>241</td><td>9.0</td><td>68.0</td><td>17</td></tr><tr><td>104.21291</td><td>104.21291</td><td>11(2 10)-10(2 9)</td><td>39</td><td>154.8</td><td>234</td><td>7.9</td><td>68.0</td><td>20</td></tr><tr><td>104.41963</td><td>104.41928</td><td>11(6,5)-10(6,4)</td><td>108</td><td>112.5</td><td>220</td><td>8.6</td><td>67.0</td><td>15</td></tr><tr><td>blend</td><td>104.41928</td><td>11(6,6)-10(6,5)</td><td>108</td><td>112.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr></tbody></table>
<table><caption>**Table 14**
(Continued)</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δν (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td rowspan="20">CH<sub>3</sub>CH<sub>2</sub>CN</td><td>104.43302</td><td>104.43302</td><td>11(3.9)-10(3.8)</td><td>50</td><td>148.2</td><td>197</td><td>8.6</td><td>68.0</td><td>9</td></tr><tr><td>104.43784</td><td>104.43748</td><td>11(7.4)-10(7.3)</td><td>136</td><td>95.3</td><td>178</td><td>8.6</td><td>67.0</td><td>10</td></tr><tr><td>blend</td><td>104.43748</td><td>11(7.5)-10(7.4)</td><td>136</td><td>95.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>104.45423</td><td>104.45423</td><td>11(3.8)-10(3.7)</td><td>50</td><td>148.2</td><td>224</td><td>10.3</td><td>68.0</td><td>16</td></tr><tr><td>104.46177</td><td>104.46147</td><td>11(8.4)-10(8.3)</td><td>168</td><td>75.4</td><td>160</td><td>10.5</td><td>67.1</td><td>12</td></tr><tr><td>blend</td><td>104.46147</td><td>11(8.3)-10(8.2)</td><td>168</td><td>75.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>104.52381</td><td>104.52351</td><td>11(10.2)-10(10.1)</td><td>245</td><td>27.8</td><td>79</td><td>5.9</td><td>67.2</td><td>13</td></tr><tr><td>blend</td><td>104.52351</td><td>11(10.1)-10(10.0)</td><td>245</td><td>27.8</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>104.96147</td><td>104.96147</td><td>11(2.9)-10(2.8)</td><td>39</td><td>154.8</td><td>149</td><td>12.0</td><td>68.0</td><td>26</td></tr><tr><td>79.44246</td><td>79.44216</td><td>7(1.7)-6(0.6)</td><td>13</td><td>6.5</td><td>35</td><td>5.3</td><td>66.9</td><td>6</td></tr><tr><td>79.67780</td><td>79.67751</td><td>9(0.9)-8(0.8)</td><td>19</td><td>133.1</td><td>233</td><td>8.8</td><td>66.9</td><td>7</td></tr><tr><td>81.26173</td><td>81.26133</td><td>9(2.7)-8(2.6)</td><td>24</td><td>126.8</td><td>259</td><td>7.9</td><td>66.5</td><td>5</td></tr><tr><td>84.15223</td><td>84.15184</td><td>11(0.11)-10(1.10)</td><td>28</td><td>10.3</td><td>40</td><td>7.4</td><td>66.6</td><td>6</td></tr><tr><td>86.82016</td><td>86.81985</td><td>10(1.10)-9(1.9)</td><td>24</td><td>146.7</td><td>352</td><td>8.5</td><td>66.9</td><td>10</td></tr><tr><td>88.89511</td><td>88.89485</td><td>19(1.18)-19(0.19)</td><td>84</td><td>11.2</td><td>52</td><td>5.5</td><td>67.1</td><td>8</td></tr><tr><td>89.00957</td><td>89.00931</td><td>25(2.23)-25(1.24)</td><td>147</td><td>24.4</td><td>77</td><td>7.3</td><td>67.1</td><td>8</td></tr><tr><td>89.29798</td><td>89.29766</td><td>10(2.9)-9(2.8)</td><td>28</td><td>142.3</td><td>310</td><td>8.3</td><td>66.9</td><td>9</td></tr><tr><td>89.41584</td><td>89.41539</td><td>24(3.21)-24(2.22)</td><td>140</td><td>27.8</td><td>91</td><td>6.7</td><td>66.5</td><td>8</td></tr><tr><td>89.56272</td><td>89.56231</td><td>10(6.4)-9(6.3)</td><td>64</td><td>94.9</td><td>337</td><td>9.0</td><td>66.6</td><td>6</td></tr><tr><td>blend</td><td>89.56231</td><td>10(6.5)-9(6.4)</td><td>64</td><td>94.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>89.56544</td><td>89.56503</td><td>10(7.3)-9(7.2)</td><td>78</td><td>75.6</td><td>294</td><td>7.2</td><td>66.6</td><td>7</td></tr><tr><td>blend</td><td>89.56503</td><td>10(7.4)-9(7.3)</td><td>78</td><td>75.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>89.56845</td><td>89.56809</td><td>10(5.6)-9(5.5)</td><td>51</td><td>111.2</td><td>345</td><td>8.8</td><td>66.8</td><td>6</td></tr><tr><td>blend</td><td>89.56810</td><td>10(5.5)-9(5.4)</td><td>51</td><td>111.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>89.57341</td><td>89.57305</td><td>10(8.2)-9(8.1)</td><td>95</td><td>53.4</td><td>247</td><td>8.1</td><td>66.8</td><td>9</td></tr><tr><td>blend</td><td>89.57305</td><td>10(8.3)-9(8.2)</td><td>95</td><td>53.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>89.58524</td><td>89.58491</td><td>10(9.1)-9(9.0)</td><td>114</td><td>28.2</td><td>173</td><td>8.0</td><td>66.9</td><td>5</td></tr><tr><td>blend</td><td>89.58491</td><td>10(9.2)-9(9.1)</td><td>114</td><td>28.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>89.59003</td><td>10(4.7)-9(4.6)</td><td>41</td><td>124.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>89.59098</td><td>89.59101</td><td>10(4.6)-9(4.5)</td><td>41</td><td>124.5</td><td>400</td><td>11.0</td><td>68.1</td><td>15</td></tr><tr><td>89.62876</td><td>89.62848</td><td>10(3.8)-9(3.7)</td><td>34</td><td>134.9</td><td>314</td><td>8.2</td><td>67.1</td><td>9</td></tr><tr><td>89.68500</td><td>89.68471</td><td>10(3.7)-9(3.6)</td><td>34</td><td>134.9</td><td>318</td><td>7.9</td><td>67.0</td><td>6</td></tr><tr><td>90.41925</td><td>90.41893</td><td>15(1.14)-14(2.13)</td><td>54</td><td>6.8</td><td>34</td><td>5.3</td><td>66.9</td><td>5</td></tr><tr><td>90.45368</td><td>90.45335</td><td>10(2.8)-9(2.7)</td><td>28</td><td>142.3</td><td>270</td><td>8.1</td><td>66.9</td><td>6</td></tr><tr><td>90.53132</td><td>90.53097</td><td>23(3.20)-23(2.21)</td><td>129</td><td>26.0</td><td>81</td><td>7.0</td><td>66.8</td><td>5</td></tr><tr><td>93.06001</td><td>93.05981</td><td>30(3.27)-30(2.28)</td><td>212</td><td>36.2</td><td>64</td><td>6.0</td><td>67.4</td><td>3</td></tr><tr><td>96.92010</td><td>96.91976</td><td>11(0.11)-10(0.10)</td><td>28</td><td>162.6</td><td>211</td><td>8.0</td><td>66.9</td><td>7</td></tr><tr><td>99.07084</td><td>99.07060</td><td>32(3.29)-32(2.30)</td><td>240</td><td>37.3</td><td>75</td><td>7.1</td><td>67.3</td><td>10</td></tr><tr><td>99.68190</td><td>99.68146</td><td>11(2.9)-10(2.8)</td><td>33</td><td>157.6</td><td>360</td><td>8.5</td><td>66.7</td><td>8</td></tr><tr><td>100.61463</td><td>100.61420</td><td>11(1.10)-10(1.9)</td><td>30</td><td>161.6</td><td>341</td><td>8.0</td><td>66.7</td><td>10</td></tr><tr><td>103.05920</td><td>103.05935</td><td>33(3.30)-33(2.31)</td><td>254</td><td>37.5</td><td>88</td><td>9.9</td><td>68.4</td><td>12</td></tr><tr><td>104.10603</td><td>104.10563</td><td>13(0.13)-12(1.12)</td><td>39</td><td>13.2</td><td>76</td><td>5.5</td><td>66.8</td><td>16</td></tr><tr><td>105.46983</td><td>105.46930</td><td>12(0.12)-11(0.11)</td><td>33</td><td>177.4</td><td>446</td><td>9.0</td><td>66.5</td><td>16</td></tr></tbody></table>
<table><caption>Table 15
Observed Lines toward Orion KL</caption><thead><tr><th>Species</th><th>Obs. freq.<br>(GHz)</th><th>Rest freq.<br>(GHz)</th><th>Transition</th><th>Eu<br>(K)</th><th>μ<sup>2</sup>S<br>(D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup><br>(mK)</th><th>Δv<br>(km s<sup>-1</sup>)</th><th>V<sub>LSR</sub><br>(km s<sup>-1</sup>)</th><th>rms Noise<br>(mK)</th></tr></thead><tbody><tr><td rowspan="21">CH<sub>3</sub>OH</td><td>80.99277</td><td>80.99326</td><td>7(2)-8(1) A<sup>-</sup></td><td>103</td><td>2.5</td><td>2450</td><td>4.3</td><td>7.8</td><td>15</td></tr><tr><td>81.65268</td><td>81.65293</td><td>18(4)-19(3) E</td><td>493</td><td>5.9</td><td>439</td><td>4.2</td><td>6.9</td><td>20</td></tr><tr><td>84.42337</td><td>84.42371</td><td>13(-3)-14(-2) E</td><td>274</td><td>4.3</td><td>888</td><td>5.8</td><td>7.2</td><td>24</td></tr><tr><td>84.52058</td><td>84.52121</td><td>5(-1)-4(0) E</td><td>40</td><td>3.1</td><td>6136</td><td>2.5</td><td>8.2</td><td>14</td></tr><tr><td>84.57350</td><td>84.57402</td><td>19(2)-18(-3) E</td><td>463</td><td>0.4</td><td>48</td><td>3.0</td><td>7.8</td><td>12</td></tr><tr><td>84.74384</td><td>84.74390</td><td>19(4)-18(5) E</td><td>537</td><td>5.2</td><td>409</td><td>9.8</td><td>6.2</td><td>24</td></tr><tr><td>86.61514</td><td>86.61560</td><td>7(2)-6(3) A<sup>-</sup></td><td>103</td><td>1.4</td><td>1606</td><td>5.0</td><td>7.6</td><td>21</td></tr><tr><td>86.90250</td><td>86.90295</td><td>7(2)-6(3) A<sup>+</sup></td><td>103</td><td>1.4</td><td>1787</td><td>4.9</td><td>7.6</td><td>18</td></tr><tr><td>88.59442</td><td>88.59481</td><td>15(3)-14(4) A<sup>+</sup></td><td>328</td><td>4.2</td><td>711</td><td>4.4</td><td>7.3</td><td>13</td></tr><tr><td>88.93962</td><td>88.93999</td><td>15(3)-14(4) A<sup>-</sup></td><td>328</td><td>4.2</td><td>877</td><td>5.0</td><td>7.3</td><td>13</td></tr><tr><td>89.50534</td><td>89.50578</td><td>8(-4)-9(-3) E</td><td>171</td><td>1.6</td><td>1073</td><td>3.9</td><td>7.5</td><td>12</td></tr><tr><td>94.54129</td><td>94.54181</td><td>8(3)-9(2) E</td><td>131</td><td>2.2</td><td>2325</td><td>5.2</td><td>7.7</td><td>13</td></tr><tr><td>94.81459</td><td>94.81507</td><td>19(7)-20(6) A<sup>+</sup></td><td>685</td><td>4.6</td><td>309</td><td>4.0</td><td>7.5</td><td>14</td></tr><tr><td>blend</td><td>94.81508</td><td>19(7)-20(6) A<sup>-</sup></td><td>685</td><td>4.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>95.16877</td><td>95.16952</td><td>8(0)-7(1) A<sup>+</sup></td><td>84</td><td>7.2</td><td>8569</td><td>3.0</td><td>8.4</td><td>13</td></tr><tr><td>95.91365</td><td>95.91431</td><td>2(1)-1(1) A<sup>+</sup></td><td>21</td><td>1.2</td><td>3986</td><td>2.7</td><td>8.1</td><td>14</td></tr><tr><td>96.73871</td><td>96.73936</td><td>2(-1)-1(-1) E</td><td>13</td><td>1.2</td><td>4067</td><td>2.9</td><td>8.0</td><td>15</td></tr><tr><td>96.74070</td><td>96.74138</td><td>2(0)-1(0) A<sup>+</sup></td><td>7</td><td>1.6</td><td>4518</td><td>3.1</td><td>8.1</td><td>15</td></tr><tr><td>96.74389</td><td>96.74455</td><td>2(0)-1(0) E</td><td>20</td><td>1.6</td><td>4235</td><td>3.0</td><td>8.0</td><td>15</td></tr><tr><td>96.75484</td><td>96.75551</td><td>2(1)-1(1) E</td><td>28</td><td>1.2</td><td>3418</td><td>2.8</td><td>8.1</td><td>16</td></tr><tr><td>99.60153</td><td>99.60195</td><td>15(1)-15(1) A</td><td>295</td><td>0.09</td><td>75</td><td>2.6</td><td>7.3</td><td>8</td></tr><tr><td>100.63845</td><td>100.63887</td><td>13(2)-12(3) E</td><td>234</td><td>3.8</td><td>1847</td><td>4.8</td><td>7.3</td><td>14</td></tr><tr><td>101.12623</td><td>101.12677</td><td>5(-2)-5(1) E</td><td>61</td><td>0.01</td><td>44</td><td>4.0</td><td>7.6</td><td>5</td></tr><tr><td>101.18483</td><td>101.18537</td><td>6(-2)-6(1) E</td><td>75</td><td>0.02</td><td>88</td><td>2.9</td><td>7.6</td><td>7</td></tr><tr><td>102.12211</td><td>102.12270</td><td>10(-2)-10(1) E</td><td>154</td><td>0.3</td><td>354</td><td>3.6</td><td>7.7</td><td>20</td></tr><tr><td>103.32452</td><td>103.32525</td><td>12(3)-13(0) E</td><td>229</td><td>0.04</td><td>51</td><td>2.5</td><td>8.1</td><td>5</td></tr><tr><td>103.38059</td><td>103.38121</td><td>12(-2)-12(1) E</td><td>207</td><td>0.8</td><td>512</td><td>3.5</td><td>7.8</td><td>14</td></tr><tr><td>105.57579</td><td>105.57638</td><td>14(-2)-14(1) E</td><td>270</td><td>1.8</td><td>1386</td><td>4.8</td><td>7.7</td><td>12</td></tr><tr><td>107.01313</td><td>107.01377</td><td>3(1)-4(0) A<sup>+</sup></td><td>28</td><td>3.0</td><td>8145</td><td>3.3</td><td>7.8</td><td>15</td></tr><tr><td>107.15932</td><td>107.15991</td><td>15(-2)-15(1) E</td><td>305</td><td>2.6</td><td>1244</td><td>4.7</td><td>7.7</td><td>12</td></tr><tr><td rowspan="21">HCOOCH<sub>3</sub></td><td>79.40120</td><td>79.40177</td><td>9(3,7)-9(2,8)E</td><td>33</td><td>2.1</td><td>96</td><td>3.1</td><td>8.1</td><td>11</td></tr><tr><td>79.43210</td><td>79.43272</td><td>9(3,7)-9(2,8)A</td><td>33</td><td>2.1</td><td>175</td><td>3.7</td><td>8.3</td><td>10</td></tr><tr><td>79.44927</td><td>79.44981</td><td>9(2,8)-9(1,9)E</td><td>29</td><td>1.3</td><td>67</td><td>2.9</td><td>8.1</td><td>12</td></tr><tr><td>79.48779</td><td>79.48829</td><td>9(2,8)-9(1,9)A</td><td>29</td><td>1.3</td><td>80</td><td>3.2</td><td>7.9</td><td>8</td></tr><tr><td>79.78123</td><td>79.78165</td><td>7(0,7)-6(0,6)E</td><td>16</td><td>18.4</td><td>579</td><td>3.4</td><td>7.6</td><td>15</td></tr><tr><td>79.78336</td><td>79.78391</td><td>7(0,7)-6(0,6)A</td><td>16</td><td>18.4</td><td>583</td><td>3.6</td><td>8.1</td><td>15</td></tr><tr><td>81.16729</td><td>81.16769</td><td>13(2,11)-13(1,12)E</td><td>59</td><td>2.8</td><td>76</td><td>2.3</td><td>7.5</td><td>10</td></tr><tr><td>81.21731</td><td>81.21781</td><td>13(2,11)-13(1,12)A</td><td>59</td><td>2.8</td><td>83</td><td>2.9</td><td>7.9</td><td>6</td></tr><tr><td>81.31373</td><td>81.31410</td><td>16(3,13)-16(2,14)E</td><td>89</td><td>4.6</td><td>78</td><td>2.6</td><td>7.3</td><td>6</td></tr><tr><td>81.36188</td><td>81.36230</td><td>16(3,13)-16(2,14)A</td><td>89</td><td>4.6</td><td>75</td><td>2.5</td><td>7.5</td><td>7</td></tr><tr><td>81.38003</td><td>81.38058</td><td>3(2,1)-2(1,2)E</td><td>6</td><td>0.6</td><td>23</td><td>1.6</td><td>8.0</td><td>7</td></tr><tr><td>81.39162</td><td>81.39228</td><td>3(2,1)-2(1,2)A</td><td>6</td><td>0.6</td><td>26</td><td>4.0</td><td>8.4</td><td>7</td></tr><tr><td>84.22411</td><td>84.22480</td><td>11(4,7)-11(3,8)E</td><td>50</td><td>3.0</td><td>76</td><td>3.7</td><td>8.5</td><td>12</td></tr><tr><td>84.23282</td><td>84.23326</td><td>11(4,7)-11(3,8)A</td><td>50</td><td>3.0</td><td>72</td><td>3.5</td><td>7.6</td><td>12</td></tr><tr><td>84.44863</td><td>84.44910</td><td>7(2,6)-6(2,5)E</td><td>19</td><td>17.2</td><td>453</td><td>3.9</td><td>7.7</td><td>10</td></tr><tr><td>84.45423</td><td>84.45479</td><td>7(2,6)-6(2,5)A</td><td>19</td><td>17.2</td><td>465</td><td>3.9</td><td>8.0</td><td>11</td></tr><tr><td>85.91865</td><td>85.91909</td><td>7(6,1)-6(6,0)E</td><td>40</td><td>5.0</td><td>146</td><td>3.7</td><td>7.5</td><td>5</td></tr><tr><td>85.92630</td><td>85.92651</td><td>7(6,2)-6(6,1)E</td><td>40</td><td>5.0</td><td>546</td><td>7.5</td><td>6.7</td><td>8</td></tr><tr><td>blend</td><td>85.92723</td><td>7(6,2)-6(6,1)A</td><td>40</td><td>5.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>85.92724</td><td>7(6,1)-6(6,0)A</td><td>40</td><td>5.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>86.02058</td><td>86.02101</td><td>7(5,2)-6(5,1)E</td><td>33</td><td>9.2</td><td>263</td><td>3.6</td><td>7.5</td><td>8</td></tr><tr><td>86.02718</td><td>86.02767</td><td>7(5,3)-6(5,2)E</td><td>33</td><td>9.2</td><td>271</td><td>3.5</td><td>7.7</td><td>7</td></tr><tr><td>86.02926</td><td>86.02945</td><td>7(5,3)-6(5,2)A</td><td>33</td><td>9.2</td><td>373</td><td>5.5</td><td>6.7</td><td>14</td></tr><tr><td>blend</td><td>86.03021</td><td>7(5,2)-6(5,1)A</td><td>33</td><td>9.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>87.55188</td><td>87.55242</td><td>10(2,9)-10(1,10)A</td><td>34</td><td>1.3</td><td>72</td><td>1.6</td><td>7.9</td><td>6</td></tr><tr><td>87.76589</td><td>87.76630</td><td>8(0,8)-7(1,7)E</td><td>20</td><td>2.8</td><td>126</td><td>2.5</td><td>7.4</td><td>6</td></tr><tr><td>87.76854</td><td>87.76907</td><td>8(0,8)-7(1,7)A</td><td>20</td><td>2.8</td><td>115</td><td>2.7</td><td>7.8</td><td>10</td></tr><tr><td>88.68634</td><td>88.68691</td><td>11(3,9)-11(2,10)E</td><td>45</td><td>2.4</td><td>60</td><td>1.9</td><td>7.9</td><td>5</td></tr><tr><td>88.84264</td><td>88.84312</td><td>7(1,6)-6(1,5)E</td><td>18</td><td>18.2</td><td>518</td><td>3.1</td><td>7.6</td><td>14</td></tr><tr><td>88.85107</td><td>88.85164</td><td>7(1,6)-6(1,5)A</td><td>18</td><td>18.2</td><td>507</td><td>3.0</td><td>7.9</td><td>19</td></tr><tr><td>89.31413</td><td>89.31459</td><td>8(1,8)-7(1,7)E</td><td>20</td><td>21.0</td><td>587</td><td>3.3</td><td>7.5</td><td>14</td></tr><tr><td>89.31606</td><td>89.31667</td><td>8(1,8)-7(1,7)A</td><td>20</td><td>21.0</td><td>636</td><td>3.7</td><td>8.0</td><td>14</td></tr><tr><td>89.74516</td><td>89.74566</td><td>11(1,10)-11(0,11)E</td><td>40</td><td>1.3</td><td>40</td><td>1.4</td><td>7.7</td><td>6</td></tr></tbody></table>
<table><caption>**Table 15**
(Continued)</caption><thead><tr><th>Species</th><th>Obs. freq.<br>(GHz)</th><th>Rest freq.<br>(GHz)</th><th>Transition</th><th>Eu<br>(K)</th><th>μ<sup>2</sup>S<br>(D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup><br>(mK)</th><th>Δν<br>(km s<sup>-1</sup>)</th><th>V<sub>LSR</sub><br>(km s<sup>-1</sup>)</th><th>rms Noise<br>(mK)</th></tr></thead><tbody><tr><td></td><td>89.79648</td><td>89.79699</td><td>11(1,10)-11(0,11)A</td><td>40</td><td>1.3</td><td>39</td><td>1.6</td><td>7.7</td><td>7</td></tr><tr><td></td><td>90.14518</td><td>90.14563</td><td>7(2,5)-6(2,4)E</td><td>20</td><td>17.3</td><td>394</td><td>2.9</td><td>7.5</td><td>14</td></tr><tr><td></td><td>90.15593</td><td>90.15651</td><td>7(2,5)-6(2,4)A</td><td>20</td><td>17.3</td><td>391</td><td>3.0</td><td>7.9</td><td>17</td></tr><tr><td></td><td>90.22714</td><td>90.22760</td><td>8(0,8)-7(0,7)E</td><td>20</td><td>21.1</td><td>437</td><td>3.4</td><td>7.5</td><td>12</td></tr><tr><td></td><td>90.22906</td><td>90.22965</td><td>8(0,8)-7(0,7)A</td><td>20</td><td>21.0</td><td>431</td><td>3.2</td><td>8.0</td><td>12</td></tr><tr><td></td><td>91.77540</td><td>91.77588</td><td>8(1,8)-7(0,7)E</td><td>20</td><td>2.9</td><td>156</td><td>2.3</td><td>7.6</td><td>6</td></tr><tr><td></td><td>91.77656</td><td>91.77725</td><td>8(1,8)-7(0,7)A</td><td>20</td><td>2.9</td><td>212</td><td>3.1</td><td>8.2</td><td>7</td></tr><tr><td></td><td>92.88371</td><td>92.88412</td><td>17(3,14)-17(2,15)E</td><td>100</td><td>4.4</td><td>185</td><td>2.3</td><td>7.3</td><td>10</td></tr><tr><td></td><td>92.93981</td><td>92.94028</td><td>17(3,14)-17(2,15)A</td><td>100</td><td>4.4</td><td>197</td><td>2.3</td><td>7.5</td><td>12</td></tr><tr><td></td><td>93.20521</td><td>93.20566</td><td>14(2,12)-14(1,13)E</td><td>67</td><td>2.8</td><td>66</td><td>2.6</td><td>7.4</td><td>8</td></tr><tr><td></td><td>93.26127</td><td>93.26176</td><td>14(2,12)-14(1,13)A</td><td>67</td><td>2.8</td><td>82</td><td>2.1</td><td>7.6</td><td>8</td></tr><tr><td></td><td>93.65952</td><td>93.66003</td><td>8(4,4)-8(3,5)A</td><td>32</td><td>1.8</td><td>146</td><td>2.3</td><td>7.6</td><td>9</td></tr><tr><td></td><td>93.70065</td><td>93.70128</td><td>8(4,4)-8(3,5)E</td><td>32</td><td>1.4</td><td>133</td><td>2.2</td><td>8.0</td><td>17</td></tr><tr><td></td><td>94.37810</td><td>94.37849</td><td>9(1,8)-8(2,7)E</td><td>28</td><td>1.7</td><td>137</td><td>2.7</td><td>7.2</td><td>11</td></tr><tr><td></td><td>94.38708</td><td>94.38765</td><td>9(1,8)-8(2,7)A</td><td>28</td><td>1.7</td><td>134</td><td>2.0</td><td>7.8</td><td>9</td></tr><tr><td></td><td>94.62630</td><td>94.62687</td><td>12(3,10)-12(2,11)E</td><td>52</td><td>2.5</td><td>170</td><td>2.4</td><td>7.8</td><td>11</td></tr><tr><td></td><td>94.63216</td><td>94.63272</td><td>5(2,4)-4(1,3)E</td><td>11</td><td>1.0</td><td>120</td><td>2.0</td><td>7.8</td><td>6</td></tr><tr><td></td><td>94.64673</td><td>94.64732</td><td>5(2,4)-4(1,3)A</td><td>11</td><td>1.0</td><td>91</td><td>2.2</td><td>7.9</td><td>7</td></tr><tr><td></td><td>94.66641</td><td>94.66693</td><td>12(3,10)-12(2,11)A</td><td>52</td><td>2.5</td><td>168</td><td>2.7</td><td>7.7</td><td>15</td></tr><tr><td></td><td>95.17539</td><td>95.17592</td><td>7(4,3)-7(3,4)A</td><td>27</td><td>1.5</td><td>152</td><td>2.5</td><td>7.7</td><td>13</td></tr><tr><td></td><td>96.05836</td><td>96.05907</td><td>11(2,10)-11(1,11)E</td><td>41</td><td>1.3</td><td>58</td><td>6.5</td><td>8.2</td><td>6</td></tr><tr><td></td><td>96.07018</td><td>96.07065</td><td>8(2,7)-7(2,6)E</td><td>24</td><td>20.0</td><td>544</td><td>4.1</td><td>7.5</td><td>13</td></tr><tr><td></td><td>96.07627</td><td>96.07688</td><td>8(2,7)-7(2,6)A</td><td>24</td><td>20.0</td><td>573</td><td>4.4</td><td>7.9</td><td>18</td></tr><tr><td></td><td>96.08642</td><td>96.08666</td><td>6(4,2)-6(3,3)A</td><td>23</td><td>1.1</td><td>55</td><td>5.4</td><td>6.7</td><td>6</td></tr><tr><td></td><td>96.10670</td><td>96.10722</td><td>11(2,10)-11(1,11)A</td><td>41</td><td>1.3</td><td>50</td><td>3.3</td><td>7.6</td><td>14</td></tr><tr><td></td><td>96.16716</td><td>96.16764</td><td>6(4,2)-6(3,3)E</td><td>23</td><td>0.8</td><td>38</td><td>4.6</td><td>7.5</td><td>9</td></tr><tr><td></td><td>96.50741</td><td>96.50799</td><td>7(4,4)-7(3,5)E</td><td>27</td><td>1.0</td><td>41</td><td>2.8</td><td>7.8</td><td>8</td></tr><tr><td></td><td>96.55208</td><td>96.55255</td><td>6(4,3)-6(3,4)E</td><td>23</td><td>0.8</td><td>32</td><td>7.7</td><td>7.5</td><td>5</td></tr><tr><td></td><td>96.61255</td><td>96.61316</td><td>8(4,5)-8(3,6)E</td><td>32</td><td>1.4</td><td>62</td><td>3.1</td><td>7.9</td><td>14</td></tr><tr><td></td><td>96.63743</td><td>96.63777</td><td>7(4,4)-7(3,5)A</td><td>27</td><td>1.5</td><td>61</td><td>3.5</td><td>7.1</td><td>15</td></tr><tr><td></td><td>96.64746</td><td>96.64810</td><td>5(4,1)-5(3,2)E</td><td>19</td><td>0.7</td><td>32</td><td>3.5</td><td>8.0</td><td>14</td></tr><tr><td></td><td>96.67035</td><td>96.67090</td><td>5(4,2)-5(3,3)E</td><td>19</td><td>0.7</td><td>26</td><td>2.6</td><td>7.7</td><td>8</td></tr><tr><td></td><td>96.69290</td><td>96.69352</td><td>6(4,3)-6(3,4)A</td><td>23</td><td>1.1</td><td>37</td><td>3.2</td><td>7.9</td><td>8</td></tr><tr><td></td><td>96.70911</td><td>96.70921</td><td>8(4,5)-8(3,6)A</td><td>32</td><td>1.8</td><td>119</td><td>6.0</td><td>6.3</td><td>12</td></tr><tr><td></td><td>96.79359</td><td>96.79409</td><td>5(4,2)-5(3,3)A</td><td>19</td><td>0.8</td><td>28</td><td>2.5</td><td>7.5</td><td>8</td></tr><tr><td></td><td>96.95627</td><td>96.95687</td><td>9(4,6)-9(3,7)E</td><td>37</td><td>2.0</td><td>84</td><td>3.3</td><td>7.8</td><td>14</td></tr><tr><td></td><td>97.01759</td><td>97.01807</td><td>9(4,6)-9(3,7)A</td><td>37</td><td>2.1</td><td>79</td><td>3.1</td><td>7.5</td><td>5</td></tr><tr><td></td><td>97.19862</td><td>97.19913</td><td>17(5,12)-17(4,13)A</td><td>108</td><td>5.2</td><td>162</td><td>3.7</td><td>7.6</td><td>5</td></tr><tr><td></td><td>97.19922</td><td>97.19922</td><td>17(5,12)-17(4,13)E</td><td>108</td><td>5.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td></td><td>99.13272</td><td>99.13319</td><td>9(0,9)-8(1,8)E</td><td>25</td><td>3.3</td><td>155</td><td>2.5</td><td>7.4</td><td>12</td></tr><tr><td></td><td>99.13518</td><td>99.13579</td><td>9(0,9)-8(1,8)A</td><td>25</td><td>3.3</td><td>153</td><td>2.5</td><td>7.8</td><td>13</td></tr><tr><td></td><td>99.16626</td><td>99.16652</td><td>11(2,9)-10(3,8)E</td><td>43</td><td>1.1</td><td>60</td><td>2.3</td><td>6.8</td><td>6</td></tr><tr><td></td><td>99.17866</td><td>99.17936</td><td>11(2,9)-10(3,8)A</td><td>43</td><td>1.2</td><td>71</td><td>2.3</td><td>8.1</td><td>9</td></tr><tr><td></td><td>100.29401</td><td>100.29451</td><td>8(3,5)-7(3,4)E</td><td>27</td><td>18.4</td><td>631</td><td>3.1</td><td>7.5</td><td>12</td></tr><tr><td></td><td>100.30756</td><td>100.30821</td><td>8(3,5)-7(3,4)A</td><td>27</td><td>18.4</td><td>628</td><td>3.2</td><td>7.9</td><td>12</td></tr><tr><td></td><td>100.48163</td><td>100.48217</td><td>8(1,7)-7(1,6)E</td><td>23</td><td>20.8</td><td>654</td><td>3.1</td><td>7.6</td><td>13</td></tr><tr><td></td><td>100.49007</td><td>100.49071</td><td>8(1,7)-7(1,6)A</td><td>23</td><td>20.8</td><td>673</td><td>3.2</td><td>7.9</td><td>13</td></tr><tr><td></td><td>100.65938</td><td>100.65969</td><td>12(4,9)-12(3,10)E</td><td>57</td><td>3.0</td><td>152</td><td>5.5</td><td>6.9</td><td>17</td></tr><tr><td></td><td>100.68095</td><td>100.68148</td><td>9(0,9)-8(0,8)E</td><td>25</td><td>23.7</td><td>680</td><td>3.2</td><td>7.6</td><td>17</td></tr><tr><td></td><td>100.68339</td><td>100.68339</td><td>9(0,9)-8(0,8)A</td><td>25</td><td>23.7</td><td>...</td><td>...</td><td>...</td><td>17</td></tr><tr><td></td><td>100.69258</td><td>100.69305</td><td>12(4,9)-12(3,10)A</td><td>57</td><td>3.0</td><td>106</td><td>2.0</td><td>7.4</td><td>17</td></tr><tr><td></td><td>100.73416</td><td>100.73477</td><td>12(1,11)-12(0,12)E</td><td>47</td><td>1.4</td><td>84</td><td>2.6</td><td>7.8</td><td>17</td></tr><tr><td></td><td>100.79015</td><td>100.79077</td><td>12(1,11)-12(0,12)A</td><td>47</td><td>1.4</td><td>75</td><td>1.6</td><td>7.9</td><td>13</td></tr><tr><td></td><td>103.22784</td><td>103.22841</td><td>13(4,10)-13(3,11)E</td><td>65</td><td>3.2</td><td>55</td><td>2.2</td><td>7.7</td><td>8</td></tr><tr><td></td><td>103.26144</td><td>103.26201</td><td>13(4,10)-13(3,11)A</td><td>65</td><td>3.2</td><td>60</td><td>2.4</td><td>7.7</td><td>8</td></tr><tr><td></td><td>103.46598</td><td>103.46648</td><td>8(2,6)-7(2,5)E</td><td>25</td><td>20.2</td><td>429</td><td>3.2</td><td>7.5</td><td>11</td></tr><tr><td></td><td>103.47803</td><td>103.47870</td><td>8(2,6)-7(2,5)A</td><td>25</td><td>20.2</td><td>431</td><td>3.3</td><td>7.9</td><td>11</td></tr><tr><td></td><td>105.42404</td><td>105.42464</td><td>15(2,13)-15(1,14)A</td><td>76</td><td>2.8</td><td>185</td><td>2.3</td><td>7.7</td><td>11</td></tr><tr><td></td><td>105.45846</td><td>105.45897</td><td>18(3,15)-18(2,16)E</td><td>111</td><td>4.3</td><td>243</td><td>2.7</td><td>7.4</td><td>15</td></tr><tr><td></td><td>105.52120</td><td>105.52175</td><td>18(3,15)-18(2,16)A</td><td>111</td><td>4.3</td><td>197</td><td>2.4</td><td>7.6</td><td>14</td></tr><tr><td></td><td>107.53662</td><td>107.53719</td><td>9(2,8)-8(2,7)E</td><td>29</td><td>22.8</td><td>1141</td><td>2.8</td><td>7.6</td><td>9</td></tr><tr><td></td><td>107.54312</td><td>107.54375</td><td>9(2,8)-8(2,7)A</td><td>29</td><td>22.8</td><td>952</td><td>2.8</td><td>7.8</td><td>9</td></tr><tr><td>CH<sub>3</sub>OCH<sub>3</sub></td><td>78.85586</td><td>78.85627</td><td>13(2,11)-13(1,12)AE</td><td>90</td><td>109.9</td><td>441</td><td>3.2</td><td>7.6</td><td>12</td></tr></tbody></table>
<table><caption>Table 15
(Continued)</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δν (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td>blend</td><td>78.85627</td><td>78.85627</td><td>13(2,11)-13(1,12)EA</td><td>90</td><td>73.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>78.85737</td><td>78.85782</td><td>78.85782</td><td>13(2,11)-13(1,12)EE</td><td>90</td><td>293.0</td><td>667</td><td>3.1</td><td>7.7</td><td>12</td></tr><tr><td>78.85892</td><td>78.85937</td><td>78.85937</td><td>13(2,11)-13(1,12)AA</td><td>90</td><td>183.1</td><td>458</td><td>3.5</td><td>7.7</td><td>12</td></tr><tr><td>79.75310</td><td>79.75370</td><td>79.75370</td><td>15(3,13)-14(4,10)AA</td><td>122</td><td>21.1</td><td>38</td><td>2.5</td><td>8.2</td><td>5</td></tr><tr><td>79.75617</td><td>79.75661</td><td>79.75661</td><td>15(3,13)-14(4,10)EE</td><td>122</td><td>56.2</td><td>109</td><td>1.9</td><td>7.6</td><td>6</td></tr><tr><td>79.75905</td><td>79.75945</td><td>79.75945</td><td>15(3,13)-14(4,10)EA</td><td>122</td><td>14.0</td><td>55</td><td>4.9</td><td>7.5</td><td>7</td></tr><tr><td>81.46711</td><td>81.46762</td><td>81.46762</td><td>18(4,15)-17(5,12)AA</td><td>178</td><td>41.5</td><td>39</td><td>2.4</td><td>7.9</td><td>5</td></tr><tr><td>81.46941</td><td>81.46992</td><td>81.46992</td><td>18(4,15)-17(5,12)EE</td><td>178</td><td>66.4</td><td>59</td><td>3.0</td><td>7.9</td><td>5</td></tr><tr><td>84.52910</td><td>84.52959</td><td>84.52959</td><td>18(4,14)-17(5,13)EE</td><td>179</td><td>66.6</td><td>56</td><td>3.4</td><td>7.7</td><td>14</td></tr><tr><td>84.63156</td><td>84.63190</td><td>84.63190</td><td>3(2,1)-3(1,2)AE</td><td>11</td><td>16.4</td><td>146</td><td>3.9</td><td>7.2</td><td>5</td></tr><tr><td>blend</td><td>84.63227</td><td>84.63227</td><td>3(2,1)-3(1,2)AE</td><td>11</td><td>10.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>84.63389</td><td>84.63441</td><td>84.63441</td><td>3(2,1)-3(1,2)EE</td><td>11</td><td>43.7</td><td>260</td><td>3.5</td><td>7.8</td><td>7</td></tr><tr><td>84.63621</td><td>84.63674</td><td>84.63674</td><td>3(2,1)-3(1,2)AA</td><td>11</td><td>27.3</td><td>169</td><td>3.5</td><td>7.9</td><td>5</td></tr><tr><td>85.97270</td><td>85.97325</td><td>85.97325</td><td>13(2,12)-12(3,9)AA</td><td>88</td><td>16.8</td><td>36</td><td>5.7</td><td>7.9</td><td>12</td></tr><tr><td>85.97562</td><td>85.97613</td><td>85.97613</td><td>13(2,12)-12(3,9)EE</td><td>88</td><td>44.9</td><td>111</td><td>3.4</td><td>7.8</td><td>12</td></tr><tr><td>85.97850</td><td>85.97900</td><td>85.97900</td><td>13(2,12)-12(3,9)EA</td><td>88</td><td>11.2</td><td>46</td><td>2.6</td><td>7.7</td><td>5</td></tr><tr><td>89.69763</td><td>89.69774</td><td>89.69774</td><td>2(2,1)-2(1,2)AE</td><td>8</td><td>8.5</td><td>86</td><td>5.9</td><td>6.4</td><td>15</td></tr><tr><td>89.69930</td><td>89.69980</td><td>89.69980</td><td>2(2,1)-2(1,2)EE</td><td>8</td><td>22.3</td><td>186</td><td>3.1</td><td>7.7</td><td>12</td></tr><tr><td>89.70245</td><td>89.70281</td><td>89.70281</td><td>2(2,1)-2(1,2)AA</td><td>8</td><td>14.1</td><td>94</td><td>4.9</td><td>7.2</td><td>13</td></tr><tr><td>90.88871</td><td>90.88925</td><td>90.88925</td><td>15(3,12)-14(4,11)AA</td><td>123</td><td>36.2</td><td>48</td><td>3.3</td><td>7.8</td><td>7</td></tr><tr><td>90.89177</td><td>90.89225</td><td>90.89225</td><td>15(3,12)-14(4,11)EE</td><td>123</td><td>57.9</td><td>99</td><td>2.1</td><td>7.6</td><td>7</td></tr><tr><td>90.89471</td><td>90.89518</td><td>90.89518</td><td>15(3,12)-14(4,11)AE</td><td>123</td><td>21.7</td><td>57</td><td>2.6</td><td>7.5</td><td>7</td></tr><tr><td>blend</td><td>90.89533</td><td>90.89533</td><td>15(3,12)-14(4,11)EA</td><td>123</td><td>14.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>90.93751</td><td>90.93751</td><td>6(0,6)-5(1,5)AA</td><td>19</td><td>32.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>90.93755</td><td>90.93810</td><td>90.93810</td><td>6(0,6)-5(1,5)EE</td><td>19</td><td>86.1</td><td>409</td><td>4.9</td><td>7.8</td><td>14</td></tr><tr><td>blend</td><td>90.93870</td><td>90.93870</td><td>6(0,6)-5(1,5)AE</td><td>19</td><td>10.8</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>90.93870</td><td>90.93870</td><td>6(0,6)-5(1,5)EA</td><td>19</td><td>21.5</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>91.47334</td><td>91.47376</td><td>91.47376</td><td>3(2,2)-3(1,3)EA</td><td>11</td><td>9.7</td><td>105</td><td>3.5</td><td>7.4</td><td>9</td></tr><tr><td>blend</td><td>91.47414</td><td>91.47414</td><td>3(2,2)-3(1,3)AE</td><td>11</td><td>4.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>91.47608</td><td>91.47660</td><td>91.47660</td><td>3(2,2)-3(1,3)EE</td><td>11</td><td>38.9</td><td>317</td><td>2.6</td><td>7.7</td><td>15</td></tr><tr><td>91.47873</td><td>91.47924</td><td>91.47924</td><td>3(2,2)-3(1,3)AA</td><td>11</td><td>14.6</td><td>141</td><td>2.4</td><td>7.7</td><td>7</td></tr><tr><td>92.70142</td><td>92.70196</td><td>92.70196</td><td>8(5,3)-9(4,5)EE</td><td>68</td><td>12.0</td><td>105</td><td>2.4</td><td>7.7</td><td>10</td></tr><tr><td>92.70247</td><td>92.70307</td><td>92.70307</td><td>8(5,4)-9(4,5)AA</td><td>68</td><td>9.6</td><td>92</td><td>2.0</td><td>7.9</td><td>6</td></tr><tr><td>92.70977</td><td>92.71029</td><td>92.71029</td><td>8(5,4)-9(4,6)EE</td><td>68</td><td>12.0</td><td>126</td><td>2.0</td><td>7.7</td><td>7</td></tr><tr><td>93.66408</td><td>93.66460</td><td>93.66460</td><td>12(1,11)-12(0,12)EA</td><td>74</td><td>37.6</td><td>400</td><td>2.7</td><td>7.7</td><td>12</td></tr><tr><td>blend</td><td>93.66460</td><td>93.66460</td><td>12(1,11)-12(0,12)AE</td><td>74</td><td>18.8</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>93.66590</td><td>93.66646</td><td>93.66646</td><td>12(1,11)-12(0,12)EE</td><td>74</td><td>150.2</td><td>905</td><td>2.5</td><td>7.8</td><td>12</td></tr><tr><td>93.66772</td><td>93.66832</td><td>93.66832</td><td>12(1,11)-12(0,12)AA</td><td>74</td><td>56.3</td><td>452</td><td>3.0</td><td>7.9</td><td>12</td></tr><tr><td>93.85395</td><td>93.85444</td><td>93.85444</td><td>4(2,3)-4(1,4)EA</td><td>15</td><td>13.3</td><td>471</td><td>2.4</td><td>7.6</td><td>10</td></tr><tr><td>blend</td><td>93.85456</td><td>93.85456</td><td>4(2,3)-4(1,4)AE</td><td>15</td><td>19.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>93.85654</td><td>93.85710</td><td>93.85710</td><td>4(2,3)-4(1,4)EE</td><td>15</td><td>53.1</td><td>670</td><td>2.4</td><td>7.8</td><td>10</td></tr><tr><td>93.85913</td><td>93.85971</td><td>93.85971</td><td>4(2,3)-4(1,4)AA</td><td>15</td><td>33.2</td><td>452</td><td>2.2</td><td>7.8</td><td>19</td></tr><tr><td>94.14797</td><td>94.14845</td><td>94.14845</td><td>11(6,5)-12(5,7)EE</td><td>111</td><td>23.2</td><td>120</td><td>2.2</td><td>7.5</td><td>7</td></tr><tr><td>96.84679</td><td>96.84724</td><td>96.84724</td><td>5(2,4)-5(1,5)EA</td><td>19</td><td>16.4</td><td>169</td><td>3.7</td><td>7.4</td><td>17</td></tr><tr><td>blend</td><td>96.84729</td><td>96.84729</td><td>5(2,4)-5(1,5)AE</td><td>19</td><td>8.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>96.84936</td><td>96.84988</td><td>96.84988</td><td>5(2,4)-5(1,5)EE</td><td>19</td><td>65.6</td><td>409</td><td>3.4</td><td>7.6</td><td>17</td></tr><tr><td>96.85195</td><td>96.85250</td><td>96.85250</td><td>5(2,4)-5(1,5)AA</td><td>19</td><td>24.6</td><td>170</td><td>3.4</td><td>7.7</td><td>17</td></tr><tr><td>96.93120</td><td>96.93111</td><td>96.93111</td><td>17(8,9)-18(7,11)EE</td><td>229</td><td>40.7</td><td>24</td><td>4.3</td><td>5.7</td><td>14</td></tr><tr><td>99.32384</td><td>99.32436</td><td>99.32436</td><td>4(1,4)-3(0,3)EA</td><td>10</td><td>17.5</td><td>449</td><td>2.4</td><td>7.6</td><td>10</td></tr><tr><td>blend</td><td>99.32436</td><td>99.32436</td><td>4(1,4)-3(0,3)AE</td><td>10</td><td>26.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>99.32466</td><td>99.32521</td><td>99.32521</td><td>4(1,4)-3(0,3)EE</td><td>10</td><td>69.8</td><td>585</td><td>1.8</td><td>7.7</td><td>5</td></tr><tr><td>99.32546</td><td>99.32606</td><td>99.32606</td><td>4(1,4)-3(0,3)AA</td><td>10</td><td>43.6</td><td>421</td><td>2.4</td><td>7.8</td><td>15</td></tr><tr><td>99.83309</td><td>99.83366</td><td>99.83366</td><td>14(2,13)-13(3,10)AA</td><td>101</td><td>28.9</td><td>97</td><td>2.0</td><td>7.7</td><td>7</td></tr><tr><td>99.83589</td><td>99.83645</td><td>99.83645</td><td>14(2,13)-13(3,10)EE</td><td>101</td><td>46.2</td><td>173</td><td>2.0</td><td>7.7</td><td>9</td></tr><tr><td>99.83869</td><td>99.83924</td><td>99.83924</td><td>14(2,13)-13(3,10)EA</td><td>101</td><td>11.5</td><td>111</td><td>2.2</td><td>7.7</td><td>7</td></tr><tr><td>blend</td><td>99.83925</td><td>99.83925</td><td>14(2,13)-13(3,10)AE</td><td>101</td><td>17.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>100.45988</td><td>100.46041</td><td>100.46041</td><td>6(2,5)-6(1,6)EA</td><td>25</td><td>19.2</td><td>372</td><td>2.7</td><td>7.6</td><td>16</td></tr><tr><td>blend</td><td>100.46044</td><td>100.46044</td><td>6(2,5)-6(1,6)AE</td><td>25</td><td>28.8</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>100.46245</td><td>100.46307</td><td>100.46307</td><td>6(2,5)-6(1,6)EE</td><td>25</td><td>76.9</td><td>532</td><td>2.7</td><td>7.9</td><td>16</td></tr><tr><td>100.46517</td><td>100.46571</td><td>100.46571</td><td>6(2,5)-6(1,6)AA</td><td>25</td><td>48.1</td><td>242</td><td>1.6</td><td>7.6</td><td>17</td></tr><tr><td>100.94845</td><td>100.94900</td><td>100.94900</td><td>19(4,16)-18(5,13)EE</td><td>196</td><td>71.9</td><td>44</td><td>2.7</td><td>7.6</td><td>5</td></tr><tr><td>105.55919</td><td>105.55979</td><td>105.55979</td><td>19(4,15)-18(5,14)AA</td><td>196</td><td>45.2</td><td>128</td><td>4.0</td><td>7.7</td><td>14</td></tr><tr><td>105.56150</td><td>105.56207</td><td>105.56207</td><td>19(4,15)-18(5,14)EE</td><td>196</td><td>72.3</td><td>214</td><td>3.4</td><td>7.6</td><td>11</td></tr></tbody></table>
<table><caption>Table 15
(Continued)</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δν (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td rowspan="10">(CH<sub>3</sub>)<sub>2</sub>CO</td><td>105.56371</td><td>105.56427</td><td>19(4,15)-18(5,14)AE</td><td>196</td><td>27.1</td><td>113</td><td>4.1</td><td>7.6</td><td>8</td></tr><tr><td>105.76769</td><td>105.76828</td><td>13(1,12)-13(0,13)AE</td><td>86</td><td>55.0</td><td>665</td><td>2.7</td><td>7.7</td><td>12</td></tr><tr><td>blend</td><td>105.76828</td><td>13(1,12)-13(0,13)EA</td><td>86</td><td>36.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>105.76972</td><td>105.77034</td><td>13(1,12)-13(0,13)EE</td><td>86</td><td>146.7</td><td>981</td><td>2.7</td><td>7.8</td><td>12</td></tr><tr><td>105.77178</td><td>105.77240</td><td>13(1,12)-13(0,13)AA</td><td>86</td><td>91.7</td><td>701</td><td>2.5</td><td>7.8</td><td>12</td></tr><tr><td>81.78887</td><td>81.78900</td><td>7(1,6)-6(2,5)AE</td><td>18</td><td>44.8</td><td>24</td><td>4.3</td><td>6.5</td><td>10</td></tr><tr><td>blend</td><td>81.78927</td><td>7(1,6)-6(2,5)EA</td><td>18</td><td>44.8</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>81.81309</td><td>81.81373</td><td>7(1,6)-6(2,5)EE</td><td>17</td><td>44.8</td><td>31</td><td>2.7</td><td>8.3</td><td>9</td></tr><tr><td>81.83269</td><td>81.83305</td><td>7(2,6)-6(1,5)EE</td><td>17</td><td>44.8</td><td>38</td><td>3.3</td><td>7.3</td><td>6</td></tr><tr><td>81.83782</td><td>81.83824</td><td>7(1,6)-6(2,5)AA</td><td>17</td><td>44.8</td><td>23</td><td>1.8</td><td>7.5</td><td>9</td></tr><tr><td>91.63413</td><td>91.63464</td><td>8(1,7)-7(2,6)EE</td><td>22</td><td>53.4</td><td>45</td><td>2.8</td><td>7.7</td><td>8</td></tr><tr><td>91.63722</td><td>91.63746</td><td>8(2,7)-7(1,6)EE</td><td>22</td><td>53.4</td><td>34</td><td>5.0</td><td>6.8</td><td>7</td></tr><tr><td>91.65876</td><td>91.65911</td><td>8(1,7)-7(2,6)AA</td><td>22</td><td>53.3</td><td>39</td><td>3.4</td><td>7.2</td><td>5</td></tr><tr><td>92.72744</td><td>92.72790</td><td>9(0,9)-8(1,8)AE</td><td>23</td><td>72.0</td><td>97</td><td>2.5</td><td>7.5</td><td>5</td></tr><tr><td>blend</td><td>92.72791</td><td>9(1,9)-8(0,8)AE</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>92.72795</td><td>9(0,9)-8(1,8)EA</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>92.72795</td><td>9(1,9)-8(0,8)EA</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>92.73531</td><td>92.73567</td><td>9(0,9)-8(1,8)EE</td><td>23</td><td>72.0</td><td>171</td><td>4.4</td><td>7.2</td><td>14</td></tr><tr><td>blend</td><td>92.73567</td><td>9(1,9)-8(0,8)EE</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>92.74299</td><td>92.74336</td><td>9(0,9)-8(1,8)AA</td><td>23</td><td>72.0</td><td>87</td><td>3.8</td><td>7.2</td><td>10</td></tr><tr><td>blend</td><td>92.74336</td><td>9(1,9)-8(0,8)AA</td><td>23</td><td>72.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>100.35006</td><td>100.35030</td><td>8(2,6)-7(3,5)EE</td><td>25</td><td>43.4</td><td>45</td><td>4.7</td><td>6.7</td><td>9</td></tr><tr><td>108.38706</td><td>108.38759</td><td>8(3,5)-7(4,4)EE</td><td>27</td><td>32.5</td><td>53</td><td>4.0</td><td>7.5</td><td>12</td></tr><tr><td rowspan="10">NH<sub>2</sub>CHO</td><td>81.69326</td><td>81.69345</td><td>4(1,4)-3(1,3)</td><td>13</td><td>49.0</td><td>62</td><td>5.1</td><td>6.7</td><td>9</td></tr><tr><td>84.54213</td><td>84.54233</td><td>4(0,4)-3(0,3)</td><td>10</td><td>52.3</td><td>35</td><td>4.4</td><td>6.7</td><td>11</td></tr><tr><td>84.80731</td><td>84.80779</td><td>4(2,3)-3(2,2)</td><td>22</td><td>39.2</td><td>32</td><td>4.1</td><td>7.7</td><td>11</td></tr><tr><td>87.84847</td><td>87.84887</td><td>4(1,3)-3(1,2)</td><td>14</td><td>49.0</td><td>43</td><td>4.1</td><td>7.4</td><td>6</td></tr><tr><td>102.06409</td><td>102.06427</td><td>5(1,5)-4(1,4)</td><td>18</td><td>62.8</td><td>69</td><td>7.0</td><td>6.5</td><td>8</td></tr><tr><td>105.46416</td><td>105.46422</td><td>5(0,5)-4(0,4)</td><td>15</td><td>65.3</td><td>229</td><td>6.3</td><td>6.2</td><td>15</td></tr><tr><td>84.94625</td><td>84.94600</td><td>9(0,9)-8(0,8)</td><td>20</td><td>130.9</td><td>143</td><td>8.5</td><td>5.1</td><td>6</td></tr><tr><td>85.71570</td><td>85.71542</td><td>9(2,7)-8(2,6)</td><td>29</td><td>124.5</td><td>116</td><td>8.5</td><td>5.0</td><td>8</td></tr><tr><td>92.42667</td><td>92.42625</td><td>10(1,10)-9(1,9)</td><td>27</td><td>144.1</td><td>167</td><td>9.4</td><td>4.6</td><td>20</td></tr><tr><td>94.27727</td><td>94.27663</td><td>10(0,10)-9(0,9)</td><td>25</td><td>145.5</td><td>204</td><td>8.6</td><td>4.0</td><td>13</td></tr><tr><td>94.76119</td><td>94.76078</td><td>10(2,9)-9(2,8)</td><td>34</td><td>139.7</td><td>158</td><td>9.4</td><td>4.7</td><td>13</td></tr><tr><td>blend</td><td>94.91312</td><td>10(4,7)-9(4,6)</td><td>60</td><td>122.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>94.91323</td><td>10(4,6)-9(4,5)</td><td>60</td><td>122.3</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>94.91399</td><td>94.91396</td><td>10(5,5)-9(5,4)</td><td>79</td><td>109.2</td><td>333</td><td>10.0</td><td>5.9</td><td>17</td></tr><tr><td>blend</td><td>94.91396</td><td>10(5,6)-9(5,5)</td><td>79</td><td>109.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>94.92508</td><td>94.92501</td><td>10(6,5)-9(6,4)</td><td>103</td><td>93.1</td><td>176</td><td>7.2</td><td>5.8</td><td>8</td></tr><tr><td>blend</td><td>94.92501</td><td>10(6,4)-9(6,3)</td><td>103</td><td>93.1</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>94.92874</td><td>94.92861</td><td>10(3,8)-9(3,7)</td><td>45</td><td>132.4</td><td>173</td><td>9.0</td><td>5.6</td><td>11</td></tr><tr><td>94.94241</td><td>94.94163</td><td>10(3,7)-9(3,6)</td><td>45</td><td>132.4</td><td>198</td><td>9.3</td><td>3.5</td><td>10</td></tr><tr><td>94.96523</td><td>94.96491</td><td>10(8,3)-9(8,2)</td><td>163</td><td>52.4</td><td>46</td><td>7.2</td><td>5.0</td><td>8</td></tr><tr><td>blend</td><td>94.96491</td><td>10(8,2)-9(8,1)</td><td>163</td><td>52.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>94.99163</td><td>94.99155</td><td>10(9,2)-9(9,1)</td><td>200</td><td>27.7</td><td>29</td><td>3.1</td><td>5.7</td><td>6</td></tr><tr><td>blend</td><td>94.99155</td><td>10(9,1)-9(9,0)</td><td>200</td><td>27.7</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>96.98320</td><td>96.98244</td><td>10(1,9)-9(1,8)</td><td>28</td><td>144.1</td><td>207</td><td>9.1</td><td>3.6</td><td>7</td></tr><tr><td>103.57574</td><td>103.57540</td><td>11(0,11)-10(0,10)</td><td>30</td><td>160.0</td><td>136</td><td>7.5</td><td>5.0</td><td>9</td></tr><tr><td rowspan="10">CH<sub>2</sub>CHCN</td><td>79.67784</td><td>79.67750</td><td>9(0,9)-8(0,8)</td><td>19</td><td>133.1</td><td>690</td><td>8.5</td><td>4.7</td><td>15</td></tr><tr><td>81.26172</td><td>81.26143</td><td>9(2,7)-8(2,6)</td><td>24</td><td>126.8</td><td>389</td><td>7.9</td><td>4.9</td><td>10</td></tr><tr><td>81.74705</td><td>81.74648</td><td>18(1,17)-18(0,18)</td><td>76</td><td>11.4</td><td>57</td><td>10.2</td><td>3.9</td><td>5</td></tr><tr><td>84.15244</td><td>84.15184</td><td>11(0,11)-10(1,10)</td><td>28</td><td>10.3</td><td>33</td><td>12.2</td><td>3.9</td><td>9</td></tr><tr><td>86.74552</td><td>86.74531</td><td>8(1,8)-7(0,7)</td><td>16</td><td>7.5</td><td>60</td><td>12.8</td><td>5.3</td><td>10</td></tr><tr><td>86.82017</td><td>86.81984</td><td>10(1,10)-9(1,9)</td><td>24</td><td>146.7</td><td>566</td><td>8.4</td><td>4.9</td><td>16</td></tr><tr><td>88.32406</td><td>88.32375</td><td>10(0,10)-9(0,9)</td><td>23</td><td>147.9</td><td>388</td><td>8.3</td><td>5.0</td><td>15</td></tr><tr><td>89.00948</td><td>89.00930</td><td>25(2,23)-25(1,24)</td><td>147</td><td>24.4</td><td>56</td><td>4.7</td><td>5.4</td><td>13</td></tr><tr><td>89.29796</td><td>89.29764</td><td>10(2,9)-9(2,8)</td><td>28</td><td>142.3</td><td>460</td><td>8.5</td><td>4.9</td><td>14</td></tr><tr><td>89.41532</td><td>89.41537</td><td>24(3,21)-24(2,22)</td><td>140</td><td>27.8</td><td>66</td><td>7.6</td><td>6.2</td><td>7</td></tr><tr><td>89.56279</td><td>89.56231</td><td>10(6,4)-9(6,3)</td><td>64</td><td>94.9</td><td>589</td><td>10.5</td><td>4.4</td><td>16</td></tr><tr><td>89.56540</td><td>89.56503</td><td>10(7,3)-9(7,2)</td><td>78</td><td>75.6</td><td>551</td><td>6.9</td><td>4.8</td><td>18</td></tr><tr><td>89.56831</td><td>89.56809</td><td>10(5,6)-9(5,5)</td><td>51</td><td>111.2</td><td>728</td><td>9.6</td><td>5.3</td><td>13</td></tr><tr><td>89.57309</td><td>89.57305</td><td>10(8,2)-9(8,1)</td><td>95</td><td>53.4</td><td>299</td><td>12.4</td><td>5.9</td><td>12</td></tr><tr><td>89.58582</td><td>89.58491</td><td>10(9,1)-9(9,0)</td><td>114</td><td>28.2</td><td>158</td><td>13.1</td><td>3.0</td><td>12</td></tr></tbody></table>
<table><caption>**Table 15**
(Continued)</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δν (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td>89.62879</td><td>89.62844</td><td>10(3,8)-9(3,7)</td><td>34</td><td>134.9</td><td>481</td><td>8.3</td><td>4.8</td><td>16</td><td></td></tr><tr><td>89.68501</td><td>89.68471</td><td>10(3,7)-9(3,6)</td><td>34</td><td>134.9</td><td>484</td><td>8.8</td><td>5.0</td><td>16</td><td></td></tr><tr><td>90.45363</td><td>90.45335</td><td>10(2,8)-9(2,7)</td><td>28</td><td>142.3</td><td>401</td><td>8.4</td><td>5.1</td><td>18</td><td></td></tr><tr><td>90.53156</td><td>90.53095</td><td>23(3,20)-23(2,21)</td><td>129</td><td>26.0</td><td>38</td><td>7.7</td><td>4.0</td><td>8</td><td></td></tr><tr><td>91.01877</td><td>91.01826</td><td>29(3,26)-29(2,27)</td><td>199</td><td>35.3</td><td>52</td><td>5.6</td><td>4.3</td><td>5</td><td></td></tr><tr><td>91.55011</td><td>91.54911</td><td>10(1,9)-9(1,8)</td><td>25</td><td>146.7</td><td>1601</td><td>14.7</td><td>2.7</td><td>15</td><td></td></tr><tr><td>93.06026</td><td>93.05981</td><td>30(3,27)-30(2,28)</td><td>212</td><td>36.2</td><td>86</td><td>8.0</td><td>4.6</td><td>9</td><td></td></tr><tr><td>93.75563</td><td>93.75508</td><td>21(3,18)-21(2,19)</td><td>110</td><td>22.3</td><td>101</td><td>14.1</td><td>4.3</td><td>9</td><td></td></tr><tr><td>93.94993</td><td>93.94931</td><td>9(1,9)-8(0,8)</td><td>20</td><td>8.6</td><td>60</td><td>9.7</td><td>4.0</td><td>5</td><td></td></tr><tr><td>95.10428</td><td>95.10405</td><td>26(2,24)-26(1,25)</td><td>158</td><td>24.1</td><td>80</td><td>5.5</td><td>5.3</td><td>8</td><td></td></tr><tr><td>96.92002</td><td>96.91975</td><td>11(0,11)-10(0,10)</td><td>28</td><td>162.6</td><td>396</td><td>9.9</td><td>5.2</td><td>6</td><td></td></tr><tr><td>99.68198</td><td>99.68150</td><td>11(2,9)-10(2,8)</td><td>33</td><td>157.6</td><td>542</td><td>10.3</td><td>4.6</td><td>15</td><td></td></tr><tr><td>100.61463</td><td>100.61428</td><td>11(1,10)-10(1,9)</td><td>30</td><td>161.6</td><td>571</td><td>8.6</td><td>5.0</td><td>19</td><td></td></tr><tr><td>101.09135</td><td>101.09166</td><td>10(1,10)-9(0,9)</td><td>24</td><td>9.8</td><td>33</td><td>6.8</td><td>6.9</td><td>6</td><td></td></tr><tr><td>102.22785</td><td>102.22741</td><td>17(3,14)-17(2,15)</td><td>76</td><td>15.9</td><td>45</td><td>9.2</td><td>4.7</td><td>6</td><td></td></tr><tr><td>103.86766</td><td>103.86725</td><td>21(1,20)-21(0,21)</td><td>102</td><td>10.9</td><td>38</td><td>6.9</td><td>4.8</td><td>7</td><td></td></tr><tr><td>107.04385</td><td>107.04351</td><td>12(2,11)-11(2,10)</td><td>38</td><td>172.9</td><td>800</td><td>9.6</td><td>5.0</td><td>22</td><td></td></tr><tr><td>107.49199</td><td>107.49157</td><td>12(8,4)-11(8,3)</td><td>105</td><td>98.8</td><td>653</td><td>10.9</td><td>4.8</td><td>13</td><td></td></tr><tr><td>107.52086</td><td>107.51994</td><td>12(10,2)-11(10,1)</td><td>145</td><td>54.4</td><td>353</td><td>11.3</td><td>3.4</td><td>13</td><td></td></tr><tr><td>107.54761</td><td>107.54759</td><td>12(4,8)-11(4,7)</td><td>51</td><td>158.1</td><td>819</td><td>11.6</td><td>5.9</td><td>13</td><td></td></tr><tr><td>107.59458</td><td>107.59404</td><td>12(3,10)-11(3,9)</td><td>44</td><td>166.7</td><td>748</td><td>10.5</td><td>4.5</td><td>13</td><td></td></tr><tr><td>107.70327</td><td>107.70217</td><td>34(3,31)-34(2,32)</td><td>269</td><td>37.5</td><td>44</td><td>9.4</td><td>2.9</td><td>8</td><td></td></tr><tr><td>107.73525</td><td>107.73473</td><td>12(3,9)-11(3,8)</td><td>44</td><td>166.7</td><td>713</td><td>10.8</td><td>4.6</td><td>15</td><td></td></tr><tr><td>108.21091</td><td>108.21038</td><td>11(1,11)-10(0,10)</td><td>29</td><td>11.0</td><td>93</td><td>11.2</td><td>4.5</td><td>12</td><td></td></tr><tr><td>108.22752</td><td>108.22711</td><td>14(3,11)-14(2,12)</td><td>55</td><td>12.1</td><td>91</td><td>7.6</td><td>4.9</td><td>9</td><td></td></tr></tbody></table>

<table><caption>**Table 16**
Observed Lines toward NGC 6334F</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δν (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td>CH<sub>3</sub>OH</td><td>80.99346</td><td>80.99326</td><td>7(2)-8(1) A<sup>-</sup></td><td>103</td><td>2.5</td><td>1086</td><td>5.9</td><td>-7.7</td><td>7</td></tr><tr><td></td><td>81.65317</td><td>81.65293</td><td>18(4)-19(3) E</td><td>493</td><td>5.9</td><td>506</td><td>5.2</td><td>-7.9</td><td>21</td></tr><tr><td></td><td>83.79289</td><td>83.79265</td><td>18(-2)-18(2) E</td><td>423</td><td>0.2</td><td>54</td><td>4.9</td><td>-7.9</td><td>7</td></tr><tr><td></td><td>84.42402</td><td>84.42371</td><td>13(-3)-14(-2) E</td><td>274</td><td>4.3</td><td>522</td><td>5.4</td><td>-8.1</td><td>15</td></tr><tr><td></td><td>84.52163</td><td>84.52121</td><td>5(-1)-4(0) E</td><td>40</td><td>3.1</td><td>4014</td><td>4.3</td><td>-8.5</td><td>8</td></tr><tr><td></td><td>84.57398</td><td>84.57402</td><td>19(2)-18(-3) E</td><td>463</td><td>0.4</td><td>80</td><td>4.7</td><td>-6.9</td><td>6</td></tr><tr><td></td><td>84.74419</td><td>84.74390</td><td>19(4)-18(5) E</td><td>537</td><td>5.2</td><td>204</td><td>6.4</td><td>-8.0</td><td>9</td></tr><tr><td></td><td>85.56844</td><td>85.56807</td><td>6(-2)-7(-1) E</td><td>75</td><td>2.0</td><td>974</td><td>5.5</td><td>-8.3</td><td>18</td></tr><tr><td></td><td>86.61591</td><td>86.61560</td><td>7(2)-6(3) A<sup>-</sup></td><td>103</td><td>1.4</td><td>549</td><td>5.7</td><td>-8.1</td><td>19</td></tr><tr><td></td><td>86.90334</td><td>86.90295</td><td>7(2)-6(3) A<sup>+</sup></td><td>103</td><td>1.4</td><td>571</td><td>5.3</td><td>-8.3</td><td>17</td></tr><tr><td></td><td>88.59515</td><td>88.59481</td><td>15(3)-14(4) A<sup>+</sup></td><td>328</td><td>4.2</td><td>794</td><td>5.0</td><td>-8.1</td><td>17</td></tr><tr><td></td><td>88.94029</td><td>88.93999</td><td>15(3)-14(4) A<sup>-</sup></td><td>328</td><td>4.2</td><td>390</td><td>5.3</td><td>-8.0</td><td>12</td></tr><tr><td></td><td>89.50609</td><td>89.50578</td><td>8(-4)-9(-3) E</td><td>171</td><td>1.6</td><td>619</td><td>5.3</td><td>-8.1</td><td>33</td></tr><tr><td></td><td>94.54212</td><td>94.54181</td><td>8(3)-9(2) E</td><td>131</td><td>2.2</td><td>1036</td><td>5.5</td><td>-8.0</td><td>16</td></tr><tr><td></td><td>94.81507</td><td>94.81507</td><td>19(7)-20(6) A<sup>+</sup></td><td>685</td><td>4.6</td><td>180</td><td>5.5</td><td>-7.0</td><td>11</td></tr><tr><td></td><td>blend</td><td>94.81508</td><td>19(7)-20(6) A<sup>-</sup></td><td>685</td><td>4.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td></td><td>95.16963</td><td>95.16952</td><td>8(0)-7(1) A<sup>+</sup></td><td>84</td><td>7.2</td><td>1787</td><td>5.7</td><td>-7.4</td><td>15</td></tr><tr><td></td><td>95.91472</td><td>95.91431</td><td>2(1)-1(1) A<sup>+</sup></td><td>21</td><td>1.2</td><td>1685</td><td>5.0</td><td>-8.3</td><td>7</td></tr><tr><td></td><td>96.44680</td><td>96.44660</td><td>21(-2)-21(2) E</td><td>563</td><td>0.3</td><td>57</td><td>3.2</td><td>-7.6</td><td>8</td></tr><tr><td></td><td>96.73986</td><td>96.73936</td><td>2(-1)-1(-1) E</td><td>13</td><td>1.2</td><td>3270</td><td>5.4</td><td>-8.5</td><td>8</td></tr><tr><td></td><td>96.74188</td><td>96.74138</td><td>2(0,2)-1(0,1) A<sup>+</sup></td><td>7</td><td>1.6</td><td>3867</td><td>4.6</td><td>-8.6</td><td>8</td></tr><tr><td></td><td>96.74498</td><td>96.74455</td><td>2(0)-1(0) E</td><td>20</td><td>1.6</td><td>2244</td><td>5.4</td><td>-8.3</td><td>8</td></tr><tr><td></td><td>96.75591</td><td>96.75551</td><td>2(1)-1(1) E</td><td>28</td><td>1.2</td><td>1520</td><td>5.0</td><td>-8.3</td><td>9</td></tr><tr><td></td><td>99.60220</td><td>99.60195</td><td>15(1)-15(1) A</td><td>295</td><td>0.09</td><td>51</td><td>3.4</td><td>-7.8</td><td>9</td></tr><tr><td></td><td>100.63927</td><td>100.63887</td><td>13(2)-12(3) E</td><td>234</td><td>3.8</td><td>868</td><td>5.2</td><td>-8.2</td><td>14</td></tr><tr><td></td><td>101.18563</td><td>101.18537</td><td>6(-2)-6(1) E</td><td>75</td><td>0.02</td><td>73</td><td>3.7</td><td>-7.8</td><td>12</td></tr><tr><td></td><td>103.32483</td><td>103.32525</td><td>12(3)-13(0) E</td><td>229</td><td>0.04</td><td>129</td><td>1.7</td><td>-5.8</td><td>30</td></tr><tr><td></td><td>103.38133</td><td>103.38121</td><td>12(-2)-12(1) E</td><td>207</td><td>0.8</td><td>362</td><td>5.4</td><td>-7.3</td><td>36</td></tr><tr><td></td><td>105.57650</td><td>105.57638</td><td>14(-2)-14(1) E</td><td>270</td><td>1.8</td><td>472</td><td>5.5</td><td>-7.3</td><td>17</td></tr><tr><td></td><td>107.01407</td><td>107.01377</td><td>3(1)-4(0) A<sup>+</sup></td><td>28</td><td>3.0</td><td>1310</td><td>5.7</td><td>-7.8</td><td>13</td></tr></tbody></table>
<table><caption>**Table 16**
(Continued)</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δv (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td rowspan="20">HCOOCH<sub>3</sub></td><td>107.16006</td><td>107.15991</td><td>15(-2)-15(1) E</td><td>305</td><td>2.6</td><td>423</td><td>5.0</td><td>-7.4</td><td>12</td></tr><tr><td>79.40195</td><td>79.40177</td><td>9(3,7)-9(2,8)E</td><td>33</td><td>2.1</td><td>115</td><td>4.3</td><td>-7.7</td><td>12</td></tr><tr><td>79.43270</td><td>79.43272</td><td>9(3,7)-9(2,8)A</td><td>33</td><td>2.1</td><td>277</td><td>4.0</td><td>-6.9</td><td>17</td></tr><tr><td>79.45003</td><td>79.44981</td><td>9(2,8)-9(1,9)E</td><td>29</td><td>1.3</td><td>92</td><td>4.1</td><td>-7.8</td><td>10</td></tr><tr><td>79.48834</td><td>79.48829</td><td>9(2,8)-9(1,9)A</td><td>29</td><td>1.3</td><td>97</td><td>2.3</td><td>-7.2</td><td>14</td></tr><tr><td>79.78191</td><td>79.78165</td><td>7(0,7)-6(0,6)E</td><td>16</td><td>18.4</td><td>523</td><td>4.6</td><td>-8.0</td><td>19</td></tr><tr><td>79.78405</td><td>79.78391</td><td>7(0,7)-6(0,6)A</td><td>16</td><td>18.4</td><td>516</td><td>4.2</td><td>-7.5</td><td>14</td></tr><tr><td>80.56526</td><td>80.56497</td><td>10(2,8)-9(3,7)E</td><td>36</td><td>0.9</td><td>51</td><td>2.4</td><td>-8.1</td><td>8</td></tr><tr><td>80.57267</td><td>80.57268</td><td>10(2,8)-9(3,7)A</td><td>36</td><td>0.9</td><td>56</td><td>3.6</td><td>-7.0</td><td>11</td></tr><tr><td>81.16795</td><td>81.16769</td><td>13(2,11)-13(1,12)E</td><td>59</td><td>2.8</td><td>119</td><td>3.5</td><td>-7.9</td><td>5</td></tr><tr><td>81.21802</td><td>81.21781</td><td>13(2,11)-13(1,12)A</td><td>59</td><td>2.8</td><td>108</td><td>5.0</td><td>-7.8</td><td>9</td></tr><tr><td>81.31431</td><td>81.31410</td><td>16(3,13)-16(2,14)E</td><td>89</td><td>4.6</td><td>145</td><td>4.0</td><td>-7.8</td><td>9</td></tr><tr><td>81.36249</td><td>81.36230</td><td>16(3,13)-16(2,14)A</td><td>89</td><td>4.6</td><td>126</td><td>3.6</td><td>-7.7</td><td>8</td></tr><tr><td>81.38070</td><td>81.38058</td><td>3(2,1)-2(1,2)E</td><td>6</td><td>0.6</td><td>61</td><td>2.8</td><td>-7.5</td><td>5</td></tr><tr><td>81.39219</td><td>81.39228</td><td>3(2,1)-2(1,2)A</td><td>6</td><td>0.6</td><td>40</td><td>6.9</td><td>-6.7</td><td>6</td></tr><tr><td>84.22483</td><td>84.22480</td><td>11(4,7)-11(3,8)E</td><td>50</td><td>3.0</td><td>85</td><td>3.7</td><td>-7.1</td><td>6</td></tr><tr><td>84.23358</td><td>84.23326</td><td>11(4,7)-11(3,8)A</td><td>50</td><td>3.0</td><td>74</td><td>3.8</td><td>-8.1</td><td>6</td></tr><tr><td>84.44942</td><td>84.44910</td><td>7(2,6)-6(2,5)E</td><td>19</td><td>17.2</td><td>338</td><td>4.5</td><td>-8.1</td><td>8</td></tr><tr><td>84.45498</td><td>84.45479</td><td>7(2,6)-6(2,5)A</td><td>19</td><td>17.2</td><td>332</td><td>4.4</td><td>-7.7</td><td>7</td></tr><tr><td>85.63848</td><td>85.63835</td><td>4(2,3)-3(1,2)E</td><td>9</td><td>0.8</td><td>71</td><td>1.8</td><td>-7.5</td><td>8</td></tr><tr><td>85.65604</td><td>85.65580</td><td>4(2,3)-3(1,2)A</td><td>9</td><td>0.8</td><td>84</td><td>3.8</td><td>-7.8</td><td>11</td></tr><tr><td>85.76211</td><td>85.76188</td><td>21(5,16)-21(4,17)E</td><td>156</td><td>7.9</td><td>147</td><td>4.2</td><td>-7.8</td><td>14</td></tr><tr><td>85.77360</td><td>85.77332</td><td>21(5,16)-21(4,17)A</td><td>156</td><td>7.9</td><td>115</td><td>3.6</td><td>-8.0</td><td>7</td></tr><tr><td>85.78086</td><td>85.78070</td><td>20(5,15)-20(4,16)E</td><td>143</td><td>7.3</td><td>160</td><td>3.7</td><td>-7.6</td><td>6</td></tr><tr><td>85.78548</td><td>85.78526</td><td>20(5,15)-20(4,16)A</td><td>143</td><td>7.3</td><td>151</td><td>3.5</td><td>-7.8</td><td>8</td></tr><tr><td>85.91937</td><td>85.91909</td><td>7(6,1)-6(6,0)E</td><td>40</td><td>5.0</td><td>224</td><td>3.9</td><td>-8.0</td><td>13</td></tr><tr><td>85.92704</td><td>85.92651</td><td>7(6,2)-6(6,1)E</td><td>40</td><td>5.0</td><td>500</td><td>6.0</td><td>-8.8</td><td>19</td></tr><tr><td>blend</td><td>85.92723</td><td>7(6,2)-6(6,1)A</td><td>40</td><td>5.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>85.92724</td><td>7(6,1)-6(6,0)A</td><td>40</td><td>5.0</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>86.02129</td><td>86.02101</td><td>7(5,2)-6(5,1)E</td><td>33</td><td>9.2</td><td>311</td><td>4.2</td><td>-8.0</td><td>11</td></tr><tr><td>86.02786</td><td>86.02767</td><td>7(5,3)-6(5,2)E</td><td>33</td><td>9.2</td><td>317</td><td>3.5</td><td>-7.7</td><td>13</td></tr><tr><td>86.02995</td><td>86.02945</td><td>7(5,3)-6(5,2)A</td><td>33</td><td>9.2</td><td>426</td><td>5.9</td><td>-8.8</td><td>13</td></tr><tr><td>blend</td><td>86.03021</td><td>7(5,2)-6(5,1)A</td><td>33</td><td>9.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>86.21024</td><td>86.21008</td><td>7(4,4)-6(4,3)A</td><td>27</td><td>12.7</td><td>390</td><td>4.2</td><td>-7.6</td><td>18</td></tr><tr><td>86.22413</td><td>86.22355</td><td>7(4,3)-6(4,2)E</td><td>27</td><td>12.6</td><td>613</td><td>5.1</td><td>-9.0</td><td>13</td></tr><tr><td>blend</td><td>86.22411</td><td>7(4,4)-6(4,3)E</td><td>27</td><td>12.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>86.25074</td><td>86.25058</td><td>7(4,3)-6(4,2)A</td><td>27</td><td>12.7</td><td>418</td><td>3.9</td><td>-7.6</td><td>18</td></tr><tr><td>86.26600</td><td>86.26583</td><td>7(3,5)-6(3,4)A</td><td>23</td><td>15.3</td><td>432</td><td>4.4</td><td>-7.6</td><td>13</td></tr><tr><td>86.26896</td><td>86.26866</td><td>7(3,5)-6(3,4)E</td><td>23</td><td>15.2</td><td>451</td><td>4.1</td><td>-8.0</td><td>18</td></tr><tr><td>87.76653</td><td>87.76630</td><td>8(0,8)-7(1,7)E</td><td>20</td><td>2.8</td><td>171</td><td>3.8</td><td>-7.8</td><td>5</td></tr><tr><td>87.76909</td><td>87.76907</td><td>8(0,8)-7(1,7)A</td><td>20</td><td>2.8</td><td>144</td><td>3.4</td><td>-7.1</td><td>9</td></tr><tr><td>88.05443</td><td>88.05403</td><td>19(5,14)-19(4,15)E</td><td>130</td><td>6.6</td><td>216</td><td>3.7</td><td>-8.4</td><td>8</td></tr><tr><td>blend</td><td>88.05437</td><td>19(5,14)-19(4,15)A</td><td>130</td><td>6.6</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>88.17566</td><td>88.17563</td><td>10(4,6)-10(3,7)E</td><td>43</td><td>2.5</td><td>149</td><td>3.9</td><td>-7.1</td><td>11</td></tr><tr><td>88.18063</td><td>88.18036</td><td>10(4,6)-10(3,7)A</td><td>43</td><td>2.5</td><td>139</td><td>3.5</td><td>-7.9</td><td>9</td></tr><tr><td>88.68704</td><td>88.68691</td><td>11(3,9)-11(2,10)E</td><td>45</td><td>2.4</td><td>144</td><td>3.1</td><td>-7.4</td><td>6</td></tr><tr><td>88.72344</td><td>88.72324</td><td>11(3,9)-11(2,10)A</td><td>45</td><td>2.4</td><td>115</td><td>3.8</td><td>-7.7</td><td>6</td></tr><tr><td>88.84342</td><td>88.84312</td><td>7(1,6)-6(1,5)E</td><td>18</td><td>18.2</td><td>247</td><td>4.4</td><td>-8.0</td><td>9</td></tr><tr><td>88.85181</td><td>88.85164</td><td>7(1,6)-6(1,5)A</td><td>18</td><td>18.2</td><td>238</td><td>4.5</td><td>-7.6</td><td>8</td></tr><tr><td>89.31491</td><td>89.31459</td><td>8(1,8)-7(1,7)E</td><td>20</td><td>21.0</td><td>272</td><td>4.6</td><td>-8.1</td><td>10</td></tr><tr><td>89.31693</td><td>89.31667</td><td>8(1,8)-7(1,7)A</td><td>20</td><td>21.0</td><td>286</td><td>4.2</td><td>-7.9</td><td>6</td></tr><tr><td>90.14579</td><td>90.14563</td><td>7(2,5)-6(2,4)E</td><td>20</td><td>17.3</td><td>270</td><td>4.7</td><td>-7.5</td><td>24</td></tr><tr><td>90.15668</td><td>90.15651</td><td>7(2,5)-6(2,4)A</td><td>20</td><td>17.3</td><td>301</td><td>3.6</td><td>-7.6</td><td>24</td></tr><tr><td>90.22783</td><td>90.22760</td><td>8(0,8)-7(0,7)E</td><td>20</td><td>21.1</td><td>364</td><td>4.7</td><td>-7.8</td><td>25</td></tr><tr><td>90.22980</td><td>90.22965</td><td>8(0,8)-7(0,7)A</td><td>20</td><td>21.0</td><td>344</td><td>4.5</td><td>-7.5</td><td>20</td></tr><tr><td>91.77605</td><td>91.77588</td><td>8(1,8)-7(0,7)E</td><td>20</td><td>2.9</td><td>202</td><td>2.9</td><td>-7.5</td><td>7</td></tr><tr><td>91.77727</td><td>91.77679</td><td>20(4,16)-20(3,17)E</td><td>139</td><td>6.4</td><td>315</td><td>3.9</td><td>-8.6</td><td>10</td></tr><tr><td>blend</td><td>91.77725</td><td>8(1,8)-7(0,7)A</td><td>20</td><td>2.9</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>91.82536</td><td>91.82518</td><td>20(4,16)-20(3,17)A</td><td>139</td><td>6.4</td><td>145</td><td>3.1</td><td>-7.6</td><td>7</td></tr><tr><td>92.88439</td><td>92.88412</td><td>17(3,14)-17(2,15)E</td><td>100</td><td>4.4</td><td>143</td><td>3.6</td><td>-7.9</td><td>9</td></tr><tr><td>92.94048</td><td>92.94028</td><td>17(3,14)-17(2,15)A</td><td>100</td><td>4.4</td><td>108</td><td>3.7</td><td>-7.6</td><td>8</td></tr><tr><td>93.20590</td><td>93.20566</td><td>14(2,12)-14(1,13)E</td><td>67</td><td>2.8</td><td>118</td><td>3.9</td><td>-7.8</td><td>6</td></tr><tr><td>93.26191</td><td>93.26176</td><td>14(2,12)-14(1,13)A</td><td>67</td><td>2.8</td><td>122</td><td>3.2</td><td>-7.5</td><td>8</td></tr></tbody></table>
<table><caption>Table 16
(Continued)</caption><thead><tr><th>Species</th><th>Obs. freq. (GHz)</th><th>Rest freq. (GHz)</th><th>Transition</th><th>Eu (K)</th><th>μ<sup>2</sup>S (D<sup>2</sup>)</th><th>T<sub>A</sub><sup>*</sup> (mK)</th><th>Δν (km s<sup>-1</sup>)</th><th>V<sub>LSR</sub> (km s<sup>-1</sup>)</th><th>rms Noise (mK)</th></tr></thead><tbody><tr><td>93.66019</td><td>93.66003</td><td></td><td>8(4,4)-8(3,5)A</td><td>32</td><td>1.8</td><td>99</td><td>2.8</td><td>-7.5</td><td>5</td></tr><tr><td>93.70138</td><td>93.70128</td><td></td><td>8(4,4)-8(3,5)E</td><td>32</td><td>1.4</td><td>89</td><td>3.1</td><td>-7.3</td><td>7</td></tr><tr><td>94.37880</td><td>94.37849</td><td></td><td>9(1,8)-8(2,7)E</td><td>28</td><td>1.7</td><td>113</td><td>4.2</td><td>-8.0</td><td>17</td></tr><tr><td>94.38786</td><td>94.38765</td><td></td><td>9(1,8)-8(2,7)A</td><td>28</td><td>1.7</td><td>137</td><td>4.0</td><td>-7.7</td><td>13</td></tr><tr><td>94.62706</td><td>94.62687</td><td></td><td>12(3,10)-12(2,11)E</td><td>52</td><td>2.5</td><td>154</td><td>4.0</td><td>-7.6</td><td>8</td></tr><tr><td>94.63298</td><td>94.63272</td><td></td><td>5(2,4)-4(1,3)E</td><td>11</td><td>1.0</td><td>90</td><td>3.2</td><td>-7.8</td><td>8</td></tr><tr><td>94.64753</td><td>94.64732</td><td></td><td>5(2,4)-4(1,3)A</td><td>11</td><td>1.0</td><td>87</td><td>4.0</td><td>-7.7</td><td>9</td></tr><tr><td>94.66712</td><td>94.66693</td><td></td><td>12(3,10)-12(2,11)A</td><td>52</td><td>2.5</td><td>141</td><td>2.8</td><td>-7.6</td><td>14</td></tr><tr><td>95.17615</td><td>95.17592</td><td></td><td>7(4,3)-7(3,4)A</td><td>27</td><td>1.5</td><td>102</td><td>2.9</td><td>-7.7</td><td>6</td></tr><tr><td>96.05927</td><td>96.05907</td><td></td><td>11(2,10)-11(1,11)E</td><td>41</td><td>1.3</td><td>55</td><td>3.6</td><td>-7.6</td><td>7</td></tr><tr><td>96.07099</td><td>96.07065</td><td></td><td>8(2,7)-7(2,6)E</td><td>24</td><td>20.0</td><td>410</td><td>4.2</td><td>-8.1</td><td>7</td></tr><tr><td>96.07705</td><td>96.07688</td><td></td><td>8(2,7)-7(2,6)A</td><td>24</td><td>20.0</td><td>396</td><td>4.9</td><td>-7.5</td><td>13</td></tr><tr><td>96.08724</td><td>96.08666</td><td></td><td>6(4,2)-6(3,3)A</td><td>23</td><td>1.1</td><td>58</td><td>4.7</td><td>-8.8</td><td>6</td></tr><tr><td>96.10746</td><td>96.10722</td><td></td><td>11(2,10)-11(1,11)A</td><td>41</td><td>1.3</td><td>42</td><td>3.8</td><td>-7.8</td><td>6</td></tr><tr><td>96.16775</td><td>96.16764</td><td></td><td>6(4,2)-6(3,3)E</td><td>23</td><td>0.8</td><td>49</td><td>3.2</td><td>-7.3</td><td>7</td></tr><tr><td>96.50803</td><td>96.50799</td><td></td><td>7(4,4)-7(3,5)E</td><td>27</td><td>1.0</td><td>64</td><td>3.3</td><td>-7.1</td><td>7</td></tr><tr><td>96.61325</td><td>96.61316</td><td></td><td>8(4,5)-8(3,6)E</td><td>32</td><td>1.4</td><td>72</td><td>3.2</td><td>-7.3</td><td>5</td></tr><tr><td>96.63799</td><td>96.63777</td><td></td><td>7(4,4)-7(3,5)A</td><td>27</td><td>1.5</td><td>58</td><td>3.7</td><td>-7.7</td><td>4</td></tr><tr><td>96.64809</td><td>96.64810</td><td></td><td>5(4,1)-5(3,2)E</td><td>19</td><td>0.7</td><td>37</td><td>2.8</td><td>-7.0</td><td>5</td></tr><tr><td>96.67098</td><td>96.67090</td><td></td><td>5(4,2)-5(3,3)E</td><td>19</td><td>0.7</td><td>35</td><td>2.2</td><td>-7.3</td><td>9</td></tr><tr><td>96.69378</td><td>96.69352</td><td></td><td>6(4,3)-6(3,4)A</td><td>23</td><td>1.1</td><td>58</td><td>3.8</td><td>-7.8</td><td>7</td></tr><tr><td>96.70961</td><td>96.70921</td><td></td><td>8(4,5)-8(3,6)A</td><td>32</td><td>1.8</td><td>101</td><td>4.5</td><td>-8.2</td><td>8</td></tr><tr><td>96.77688</td><td>96.77676</td><td></td><td>7(4,3)-7(3,5)E</td><td>24</td><td>0.5</td><td>39</td><td>3.4</td><td>-7.4</td><td>5</td></tr><tr><td>96.79433</td><td>96.79409</td><td></td><td>5(4,2)-5(3,3)A</td><td>19</td><td>0.8</td><td>54</td><td>2.6</td><td>-7.7</td><td>6</td></tr><tr><td>96.83545</td><td>96.83528</td><td></td><td>4(4,0)-4(3,1)A</td><td>17</td><td>0.4</td><td>38</td><td>2.9</td><td>-7.5</td><td>9</td></tr><tr><td>96.85933</td><td>96.85939</td><td></td><td>4(4,0)-4(3,1)E</td><td>17</td><td>0.4</td><td>27</td><td>2.7</td><td>-6.8</td><td>8</td></tr><tr><td>96.95700</td><td>96.95687</td><td></td><td>9(4,6)-9(3,7)E</td><td>37</td><td>2.0</td><td>89</td><td>3.3</td><td>-7.4</td><td>5</td></tr><tr><td>97.01839</td><td>97.01807</td><td></td><td>9(4,6)-9(3,7)A</td><td>37</td><td>2.1</td><td>89</td><td>3.3</td><td>-8.0</td><td>7</td></tr><tr><td>97.19943</td><td>97.19913</td><td></td><td>17(5,12)-17(4,13)A</td><td>108</td><td>5.2</td><td>183</td><td>4.1</td><td>-7.9</td><td>9</td></tr><tr><td>blend</td><td>97.19922</td><td></td><td>17(5,12)-17(4,13)E</td><td>108</td><td>5.2</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>98.27076</td><td>98.27037</td><td></td><td>8(6,2)-7(6,1)E</td><td>45</td><td>9.4</td><td>372</td><td>3.8</td><td>-8.2</td><td>18</td></tr><tr><td>98.27970</td><td>98.27887</td><td></td><td>8(6,3)-7(6,2)E</td><td>45</td><td>9.4</td><td>626</td><td>5.7</td><td>-9.5</td><td>15</td></tr><tr><td>blend</td><td>98.27975</td><td></td><td>8(6,3)-7(6,2)A</td><td>45</td><td>9.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>blend</td><td>98.27979</td><td></td><td>8(6,2)-7(6,1)A</td><td>45</td><td>9.4</td><td>...</td><td>...</td><td>...</td><td>...</td></tr><tr><td>98.42442</td><td>98.42408</td><td></td><td>8(5,3)-7(5,2)E</td><td>38</td><td>13.1</td><td>430</td><td>4.0</td><td>-8.0</td><td>15</td></tr><tr><td>98.43183</td><td>98.43175</td><td></td><td>8(5,4)-7(5,3)E</td><td>38</td><td>13.1</td><td>334</td><td>3.7</td><td>-7.2</td><td>16</td></tr><tr><td>98.43288</td><td>98.43277</td><td></td><td>8(5,4)-7(5,3)A</td><td>38</td><td>13.1</td><td>450</td><td>4.9</td><td>-7.3</td><td>19</td></tr><tr><td>98.43603</td><td>98.43582</td><td></td><td>8(5,3)-7(5,2)A</td><td>38</td><td>13.1</td><td>449</td><td>4.0</td><td>-7.6</td><td>17</td></tr><tr><td>98.60709</td><td>98.60677</td><td></td><td>8(3,6)-7(3,5)E</td><td>27</td><td>18.4</td><td>497</td><td>4.3</td><td>-8.0</td><td>16</td></tr><tr><td>98.61133</td><td>98.61120</td><td></td><td>8(3,6)-7(3,5)A</td><td>27</td><td>18.4</td><td>500</td><td>5.1</td><td>-7.4</td><td>16</td></tr><tr><td>98.68281</td><td>98.68263</td><td></td><td>8(4,5)-7(4,4)A</td><td>32</td><td>16.1</td><td>545</td><td>4.2</td><td>-7.6</td><td>16</td></tr><tr><td>98.71228</td><td>98.71193</td><td></td><td>8(4,5)-7(4,4)E</td><td>32</td><td>15.6</td><td>483</td><td>4.4</td><td>-8.1</td><td>20</td></tr><tr><td>99.13338</td><td>99.13319</td><td></td><td>9(0,9)-8(1,8)E</td><td>25</td><td>3.3</td><td>78</td><td>2.9</td><td>-7.6</td><td>5</td></tr><tr><td>99.13595</td><td>99.13579</td><td></td><td>9(0,9)-8(1,8)A</td><td>25</td><td>3.3</td><td>74</td><td>4.0</td><td>-7.5</td><td>5</td></tr><tr><td>100.07879</td><td>100.07853</td><td></td><td>9(1,9)-8(1,8)E</td><td>25</td><td>23.6</td><td>684</td><td>4.6</td><td>-7.8</td><td>13</td></tr><tr><td>100.08080</td><td>100.08057</td><td></td><td>9(1,9)-8(1,8)A</td><td>25</td><td>23.6</td><td>612</td><td>4.8</td><td>-7.7</td><td>18</td></tr><tr><td>100.29486</td><td>100.29451</td><td></td><td>8(3,5)-7(3,4)E</td><td>27</td><td>18.4</td><td>250</td><td>4.4</td><td>-8.0</td><td>13</td></tr><tr><td>100.30848</td><td>100.30821</td><td></td><td>8(3,5)-7(3,4)A</td><td>27</td><td>18.4</td><td>275</td><td>4.2</td><td>-7.8</td><td>10</td></tr><tr><td>100.48252</td><td>100.48217</td><td></td><td>8(1,7)-7(1,6)E</td><td>23</td><td>20.8</td><td>574</td><td>4.4</td><td>-8.1</td><td>20</td></tr><tr><td>100.49095</td><td>100.49071</td><td></td><td>8(1,7)-7(1,6)A</td><td>23</td><td>20.8</td><td>572</td><td>4.4</td><td>-7.7</td><td>17</td></tr><tr><td>100.54375</td><td>100.54378</td><td></td><td>12(1,11)-12(1,12)E</td><td>47</td><td>0.8</td><td>60</td><td>2.5</td><td>-6.9</td><td>14</td></tr><tr><td>100.60018</td><td>100.60000</td><td></td><td>12(1,11)-12(1,12)A</td><td>47</td><td>0.8</td><td>71</td><td>2.7</td><td>-7.5</td><td>9</td></tr><tr><td>100.65963</td><td>100.65969</td><td></td><td>12(4,9)-12(3,10)E</td><td>57</td><td>3.0</td><td>256</td><td>4.9</td><td>-6.8</td><td>19</td></tr><tr><td>100.68183</td><td>100.68148</td><td></td><td>9(0,9)-8(0,8)E</td><td>25</td><td>23.7</td><td>544</td><td>4.7</td><td>-8.0</td><td>7</td></tr><tr><td>100.68370</td><td>100.68339</td><td></td><td>9(0,9)-8(0,8)A</td><td>25</td><td>23.7</td><td>537</td><td>4.1</td><td>-7.9</td><td>13</td></tr><tr><td>100.69341</td><td>100.69305</td><td></td><td>12(4,9)-12(3,10)A</td><td>57</td><td>3.0</td><td>131</td><td>3.7</td><td>-8.1</td><td>9</td></tr><tr><td>100.73506</td><td>100.73477</td><td></td><td>12(1,11)-12(0,12)E</td><td>47</td><td>1.4</td><td>114</td><td>3.2</td><td>-7.8</td><td>11</td></tr><tr><td>100.79081</td><td>100.79077</td><td></td><td>12(1,11)-12(0,12)A</td><td>47</td><td>1.4</td><td>105</td><td>2.1</td><td>-7.1</td><td>9</td></tr><tr><td>103.26241</td><td>103.26201</td><td></td><td>13(4,10)-13(3,11)A</td><td>65</td><td>3.2</td><td>115</td><td>3.3</td><td>-8.2</td><td>19</td></tr><tr><td>103.46674</td><td>103.46648</td><td></td><td>8(2,6)-7(2,5)E</td><td>25</td><td>20.2</td><td>326</td><td>4.1</td><td>-7.8</td><td>27</td></tr><tr><td>103.47879</td><td>103.47870</td><td></td><td>8(2,6)-7(2,5)A</td><td>25</td><td>20.2</td><td>328</td><td>3.9</td><td>-7.3</td><td>27</td></tr><tr><td>107.53752</td><td>107.53719</td><td></td><td>9(2,8)-8(2,7)E</td><td>29</td><td>22.8</td><td>399</td><td>4.6</td><td>-7.9</td><td>16</td></tr><tr><td>107.54397</td><td>107.54375</td><td></td><td>9(2,8)-8(2,7)A</td><td>29</td><td>22.8</td><td>414</td><td>4.8</td><td>-7.6</td><td>12</td></tr></tbody></table>