<figure><img src="image_1.png" /></figure>

# Erratum: ATOMS: ALMA three-millimeter observations of massive star-forming regions – III. Catalogues of candidate hot molecular cores and hyper/ultra compact H II regions

by Hong-Li Liu<sup>1,2,3★</sup> Tie Liu,<sup>3,4★</sup> Neal J. Evans II,<sup>5,6</sup> Ke Wang,<sup>7</sup> Guido Garay,<sup>8</sup> Sheng-Li Qin,<sup>1</sup>

Shanghuo Li<sup>6</sup>, Amelia Stutz,<sup>2,9</sup> Paul F. Goldsmith,<sup>10</sup> Sheng-Yuan Liu,<sup>11</sup> Anandmayee Tej<sup>5,12</sup>

Qizhou Zhang,<sup>13</sup> Mika Juvela,<sup>14</sup> Di Li<sup>15,16,17</sup> Jun-Zhi Wang,<sup>3,18</sup> Leonardo Bronfman,<sup>8</sup> Zhiyuan Ren<sup>10</sup>,<sup>15</sup>

Yue-Fang Wu,<sup>19</sup> Kee-Tae Kim,<sup>6,20</sup> Chang-Won Lee,<sup>6,20</sup> Ken'ichi Tatematsu<sup>10</sup>,<sup>21</sup> Maria R. Cunningham,<sup>22</sup>

Xun-Chuan Liu,<sup>19</sup> Jing-Wen Wu,<sup>15</sup> Tomoya Hirota,<sup>21</sup> Jeong-Eun Lee,<sup>23</sup> Pak-Shing Li,<sup>24</sup> Sung-Ju Kang,<sup>6</sup>

Diego Mardones,<sup>8</sup> Isabelle Ristorcelli,<sup>25</sup> Yong Zhang<sup>10</sup>,<sup>26</sup> Qiu-Yi Luo,<sup>3</sup> L. Viktor Toth<sup>10</sup>,<sup>27</sup>

Hee-weon Yi,<sup>23</sup> Hyeong-Sik Yun,<sup>23</sup> Ya-Ping Peng,<sup>28</sup> Juan Li<sup>10</sup>,<sup>3,18</sup> Feng-Yao Zhu,<sup>3</sup> Zhi-Qiang Shen,<sup>3,18</sup>

Tapas Baug,<sup>7,29</sup> L. K. Dewangan<sup>10</sup>,<sup>30</sup> Eswaraiah Chakali,<sup>15</sup> Rong Liu,<sup>15</sup> Feng-Wei Xu,<sup>7,19</sup> Yu Wang,<sup>19</sup>

Chao Zhang,<sup>15,31</sup> Jinzeng Li,<sup>15</sup> Chao Zhang,<sup>1</sup> Jianwen Zhou,<sup>15</sup> Mengyao Tang<sup>10</sup>,<sup>1</sup> Qiaowei Xue,<sup>1</sup>

Namitha Issac,<sup>12</sup> Archana Soam<sup>10,32</sup> and Rodrigo H. Álvarez-Gutiérrez<sup>2</sup>

**Key words:** errata, addenda – stars: formation – stars: kinematics and dynamics – ISM: clouds – H II regions.

<footnote n="1"><sup>1</sup>Department of Astronomy, Yunnan University, Kunming 650091, People's Republic of China</footnote>

<footnote n="2"><sup>2</sup>Departamento de Astronomía, Universidad de Concepción, Casilla 160-C, Concepción 4030000, Chile</footnote>

<footnote n="3"><sup>3</sup>Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People's Republic of China</footnote>

<footnote n="4"><sup>4</sup>Key Laboratory for Research in Galaxies and Cosmology, Shanghai Astronomical Observatory, Chinese Academy of Sciences, 80 Nandan Road, Shanghai 200030, People's Republic of China</footnote>

<footnote n="5"><sup>5</sup>Department of Astronomy, The University of Texas at Austin, 2515 Speedway, Stop C1400, Austin, TX 78712-1205, USA</footnote>

<footnote n="6"><sup>6</sup>Korea Astronomy and Space Science Institute, 776 Daedeokdaero, Yuseong-gu, Daejeon 34055, Republic of Korea</footnote>

<footnote n="7"><sup>7</sup>Kavli Institute for Astronomy and Astrophysics, Peking University, 5 Yiheyuan Road, Haidian District, Beijing 100871, People's Republic of China</footnote>

<footnote n="8"><sup>8</sup>Departamento de Astronomía, Universidad de Chile, Las Condes, Santiago, Chile</footnote>

<footnote n="9"><sup>9</sup>Max-Planck-Institute for Astronomy, Königstuhl 17, D-69117 Heidelberg, Germany</footnote>

<footnote n="10"><sup>10</sup>Jet Propulsion Laboratory, California Institute of Technology, 4800 Oak Grove Drive, Pasadena, CA 91109, USA</footnote>

<footnote n="11"><sup>11</sup>Institute of Astronomy and Astrophysics, Academia Sinica, 11F of Astronomy-Mathematics Building, AS/NTU No. 1, Section 4, Roosevelt Rd., Taipei 10617, Taiwan</footnote>

<footnote n="12"><sup>12</sup>Indian Institute of Space Science and Technology, Thiruvananthapuram 695 547, Kerala, India</footnote>

<footnote n="13"><sup>13</sup>Center for Astrophysics | Harvard & Smithsonian, 60 Garden Street, Cambridge, MA 02138, USA</footnote>

<footnote n="14"><sup>14</sup>Department of Physics, University of Helsinki, P.O. Box 64, FI-00014, Helsinki, Finland</footnote>

<footnote n="15"><sup>15</sup>National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100101, People's Republic of China</footnote>

<footnote n="16"><sup>16</sup>University of Chinese Academy of Sciences, Beijing 100049, People's Republic of China</footnote>

<footnote n="17"><sup>17</sup>NAOC-UKZN Computational Astrophysics Centre, University of KwaZulu-Natal, Durban 4000, South Africa</footnote>

<footnote n="18"><sup>18</sup>Key Laboratory of Radio Astronomy, Chinese Academy of Sciences, Nanjing 210008, People's Republic of China</footnote>

<footnote n="19"><sup>19</sup>Department of Astronomy, Peking University, Beijing 100871, People's Republic of China</footnote>

<footnote n="20"><sup>20</sup>University of Science and Technology, Korea (UST), 217 Gajeong-ro, Yuseong-gu, Daejeon 34113, Republic of Korea</footnote>

<footnote n="21"><sup>21</sup>National Astronomical Observatory of Japan, National Institutes of Natural Sciences, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan</footnote>

<footnote n="22"><sup>22</sup>School of Physics, University of New South Wales, Sydney, NSW 2052, Australia</footnote>

<footnote n="23"><sup>23</sup>School of Space Research, Kyung Hee University, Yongin-Si, Gyeonggi-Do 17104, Republic of Korea</footnote>

<footnote n="24"><sup>24</sup>Astronomy Department, University of California, Berkeley, CA 94720, USA</footnote>

<footnote n="25"><sup>25</sup>IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France</footnote>

<footnote n="26"><sup>26</sup>School of Physics and Astronomy, Sun Yat-sen University, 2 Daxue Road, Zhuhai, Guangdong 519082, People's Republic of China</footnote>

<footnote n="27"><sup>27</sup>Department of Astronomy, Eötvös Loránd University, Pázmány Péter sétány 1/A, H-1117, Budapest, Hungary</footnote>

<footnote n="28"><sup>28</sup>College of Science, Yunnan Agricultural University, Kunming, 650201, People's Republic of China</footnote>

<footnote n="29"><sup>29</sup>Satyendra Nath Bose National Centre for Basic Sciences, Block-JD, Sector-III, Salt Lake, Kolkata 700 106, India</footnote>

<footnote n="30"><sup>30</sup>Physical Research Laboratory, Navrangpura, Ahmedabad 380 009, India</footnote>

<footnote n="31"><sup>31</sup>Department of Physics, Taiyuan Normal University, Jinzhong 030619, People's Republic of China</footnote>

<footnote n="32"><sup>32</sup>SOFIA Science Centre, USRA, NASA Ames Research Centre, MS-12, N232, Moffett Field, CA 94035, USA</footnote>
<figure><img src="image_2.png" /><figcaption>**Figure 5.** Venn diagram showing the relation between 135 COM-containing and 91 H/UC-H II cores. The 135 COM-containing cores consist of 51 pure and 30 H/UC-H II-associated w-cHMCs and 31 pure and 23 H/UC-H II-associated s-cHMCs.</figcaption></figure>

This is an erratum to the paper 'ALMA three-millimeter observations of massive star-forming regions – III. Catalogues of candidate hot molecular cores and hyper/ultra compact H II regions', which was published in Liu et al. (2021). In that paper, 453 compact cores extracted from 3 mm continuum data are compiled into four catalogues, including the H/UC-H II, pure s-cHMC/w-cHMC, and 'unknown' catalogues. In section 3.2.1, 'Search for COM-containing cores', there were small errors on the number statistics of the cores in both pure s-cHMC and pure w-cHMC catalogues due to the mistake made at the final stage of arranging the results. The number for these two catalogues should be corrected to be 31 and 51 from 32 and 58, respectively. As a consequence, the number of cores in other two catalogues will change slightly since the total number of all continuum cores remains 453. That is, the number of cores in the H/UC-H II ('unknown') catalogue should change from 89 (274) to 91 (280).

In section 3.3, a fixed temperature of 100 K was used in calculating the parameters of the ‘unknown’ cores. However, the temperature should be corrected as the clump-average one as described in the paper. This correction will increase by a factor of 3–4 the temperature-related parameters (i.e. mass, mass surface density, and number density of gas). This increase slightly affects the results in section 3.3 only. In summary, the small change of the number of cores in each catalogue and the miscalculation of the temperature-related parameters for the ‘unknown’ cores do not affect the conclusion of the paper.

In the following, the details on where to update the specific numbers or values are listed in the order in which they appear in the paper.

(i) in Abstract, the numbers of cores in the H/UC-H II, pure s-cHMC, and pure w-cHMC catalogues should be updated as 91, 31, 51 instead of the reported values 89, 32, and 58, respectively.

(ii) in section 3.2.1, the number of the H/UC-H II cores should change from 89 to 91.

(iii) in section 3.2.2, the numbers of the pure s-cHMC/w-cHMC cores should change from 32/58 to 31/51. Accordingly, the total number of the COM-containing cores is reduced from 138 to 135.

(iv) in section 3.3, the number of the ‘unknown’ cores should be 280 instead of the reported value 274. In addition, these cores have the updated temperature-related parameters, including a median mass of 63 $M_\odot$ in an IQR of [20, 310] $M_\odot$, a median number density of $0.9 \times 10^7 \text{ cm}^{-3}$ in an IQR of [0.4, 1.7] $\times 10^7 \text{ cm}^{-3}$, and a median mass surface density of $7.2 \text{ g cm}^{-2}$ in an IQR of [4.3, 14.2] g cm$^{-2}$.

(v) in section 4.2, the number of the COM-containing but not H/UC-H II-associated cores is updated from 90 to 82. The numbers of the pure s-cHMC/w-cHMC cores should be 31/51.

(vi) in section 4.3, the number of all COM-containing cores should change from 138 to 135 while the number of the pure s-cHMC cores goes from 56 to 51.

(vii) in section 4.4 the numbers of the w-cHMC, s-cHMC, and ‘unknown’ clumps should be 25, 18, and 29 instead of 28, 17, and 28, respectively.

(viii) in section 5, the number of the H/UC-H II cores should updated from 89 to 91. Accordingly, the number of the UC-H II cores is increased to 81 from the quoted value 79.

(ix) in Conclusion, the numbers of cores in the H/UC-H II, pure s-cHMC, pure w-cHMC, and ‘unknown’ catalogues should be updated as 91, 31, 51, and 280, respectively (see above). The number of the UC-H II should be 81 (see above).

(x) in appendix B, the number of the COM-containing but not H/UC-H II-associated cores should change from 90 to 82. The numbers of the pure s-cHMC/w-cHMC cores should be 31/51 (see above).

In addition, five figures (i.e. Figs 5–9) and three tables (i.e. Tables 1–3) and four online tables as the supplementary data) have been slightly modified due to the updated numbers of the sources in the four catalogues. Except for Figs 5 and 8, none of the figures change enough to notice. Fig. 5 changes in correspondence to the number update of cores in all of the four catalogues while Fig. 7 does only due to the number update of the pure COM-containing cores (i.e. in s-cHMC and w-cHMC catalogues).

<figure><img src="image_3.png" /><figcaption>**Figure 6.** (a) Radius versus distance for w-cHMC, s-cHMC, and H/UC-H II cores. The p value of the KS test 0.03 suggests that the size distributions of w-cHMC and s-cHMC come from an identical distribution. (b) Mass versus distance for w-cHMC and s-cHMC cores. H/UC-H II cores are not shown here since their masses cannot be estimated from 3 mm continuum due to free-free contamination (see text in section 3.2.2). The curve is the mass sensitivity distribution as a function of the distance.</figcaption></figure>
<figure><img src="image_4.png" /><figcaption>**Figure 7.** Distance distribution of the four groups of clumps. (a) Cumulative distribution function. (b)–(d) Histograms of all clumps against w-cHMC group, s-cHMC group, and H/UC-H II group of clumps, respectively.</figcaption></figure>

<figure><img src="image_5.png" /><figcaption>**Figure 8.** Distributions of the mass and mass surface density of the 80 COM-containing cores that are not associated with the H/UC-H II signature. The two parameters were calculated assuming a temperature of 100 K typical of HMCs (see appendix B). The dashed vertical line indicates a stringent theoretical threshold of 1 g cm⁻² above which the cores most likely form high-mass stars. The red dots highlight the cores associated with the Class II CH₃OH masers, showing that they are widely distributed, but above the 1 g cm⁻² line.</figcaption></figure>
<figure><img src="image_6.png" /><figcaption>**Figure 9.** Box and whisker plot showing four groups of clumps the distribution of the L/M ratio (panel a), dust temperature $T_d$ (panel b). The numbers associated with the boxes from the top to bottom represent the upper quartile, median (inside the box), and lower quartile, respectively. The red crosses indicate the outliers outside 1.5 times the interquartile range either above the upper quartile or below the lower quartile.</figcaption></figure>

<table><caption>**Table 1.** Parameters of the H/UC-H II cores from the ATOMS survey's clumps.</caption><thead><tr><th>Name clump</th><th>Gal. name core</th><th>D kpc</th><th>FWHM maj(°) × min(°)</th><th>PA deg</th><th>FWHM<sub>dec</sub> maj(°) × min(°)</th><th>F<sup>int</sup><sub>3mm</sub> mJy</th><th>F<sup>P</sup><sub>3mm</sub> mJy beam<sup>-1</sup></th><th>R<sub>core</sub><sup>0.8</sup></th><th>F<sup>P</sup><sub>H40u</sub> mJy beam<sup>-1</sup></th><th>V<sub>100, H40u</sub> km s<sup>-1</sup></th><th>ΔV<sub>H40u</sub> km s<sup>-1</sup></th><th>FWHM<sup>M340u</sup> maj(°) × min(°)</th><th>R<sup>H40u</sup><sub>core</sub> 10<sup>-2</sup> pc</th></tr></thead><tbody><tr><td>109002–4732</td><td>G268.4225–00.8491</td><td>2.0<sup>+0.7</sup><sub>-0.8</sub></td><td>4.6 × 4.0</td><td>15.8</td><td>4.5 × 3.6</td><td>3058.0 ± 29.0</td><td>329.7 ± 2.9</td><td>2.0<sup>+0.6</sup><sub>-0.8</sub></td><td>242.7 ± 1.5</td><td>-2.0 ± 1.6</td><td>34.5 ± 1.6</td><td>4.4 ± 3.3</td><td>1.9<sup>+0.6</sup><sub>-0.7</sub></td></tr><tr><td>112320–6122</td><td>G300.9688+01.1475*</td><td>3.1<sup>+0.6</sup><sub>-0.5</sub></td><td>2.6 × 2.4</td><td>11.2</td><td>1.6 × 0.9</td><td>477.4 ± 9.5</td><td>333.5 ± 4.3</td><td>0.9<sup>+0.2</sup><sub>-0.1</sub></td><td>191.6 ± 2.0</td><td>-41.4 ± 1.6</td><td>37.3 ± 1.6</td><td>1.5 ± 0.7</td><td>0.8<sup>+0.2</sup><sub>-0.1</sub></td></tr><tr><td>112326–6245</td><td>G301.1364–00.2257*</td><td>5.6<sup>+0.5</sup><sub>-0.8</sub></td><td>2.9 × 2.2</td><td>172.0</td><td>1.8 × 1.0</td><td>2003.0 ± 49.0</td><td>1351.0 ± 21.0</td><td>1.8<sup>+0.1</sup><sub>-0.3</sub></td><td>526.5 ± 3.2</td><td>-63.8 ± 1.6</td><td>55.0 ± 1.6</td><td>1.6 ± 0.8</td><td>1.6<sup>+0.1</sup><sub>-0.2</sub></td></tr><tr><td>112326–6245</td><td>G301.1363–00.2235*</td><td>5.6<sup>+0.5</sup><sub>-0.8</sub></td><td>3.4 × 2.1</td><td>178.0</td><td>2.3 × 1.1</td><td>212.0 ± 52.0</td><td>130.0 ± 21.0</td><td>2.2<sup>+0.2</sup><sub>-0.3</sub></td><td>94.8 ± 0.0</td><td>-38.6 ± 1.6</td><td>25.3 ± 0.1</td><td>2.3 ± 1.1</td><td>2.2<sup>+0.2</sup><sub>-0.3</sub></td></tr><tr><td>112383–6128</td><td>G301.7314+01.033</td><td>2.8<sup>+0.7</sup><sub>-0.6</sub></td><td>4.1 × 3.7</td><td>17.0</td><td>3.3 × 3.2</td><td>96.7 ± 2.2</td><td>27.4 ± 0.5</td><td>2.2<sup>+0.5</sup><sub>-0.5</sub></td><td>32.8 ± 0.9</td><td>-38.3 ± 1.6</td><td>24.7 ± 1.6</td><td>3.2 ± 2.3</td><td>1.9<sup>+0.4</sup><sub>-0.4</sub></td></tr><tr><td>112572–6316</td><td>G303.9302–00.6879*</td><td>11.5<sup>+0.3</sup><sub>-0.3</sub></td><td>2.8 × 2.3</td><td>7.3</td><td>1.5 × 1.3</td><td>48.2 ± 1.0</td><td>32.3 ± 0.5</td><td>3.9<sup>+0.1</sup><sub>-0.1</sub></td><td>17.9 ± 0.8</td><td>24.0 ± 1.6</td><td>24.5 ± 1.6</td><td>1.4 ± 1.0</td><td>3.2<sup>+0.1</sup><sub>-0.1</sub></td></tr><tr><td>113080–6229</td><td>G305.1961+00.0331*</td><td>2.3<sup>+0.6</sup><sub>-0.6</sub></td><td>12.6 × 8.9</td><td>78.0</td><td>12.5 × 8.6</td><td>2014.0 ± 46.0</td><td>76.6 ± 1.7</td><td>5.8<sup>+1.4</sup><sub>-1.4</sub></td><td>70.0 ± 1.8</td><td>-35.8 ± 1.6</td><td>28.0 ± 1.6</td><td>9.3 ± 5.2</td><td>3.9<sup>+1.0</sup><sub>-1.0</sub></td></tr><tr><td>113291–6249</td><td>G307.5605–00.5870</td><td>7.8<sup>+0.5</sup><sub>-0.5</sub></td><td>7.6 × 5.9</td><td>24.2</td><td>7.3 × 5.6</td><td>562.4 ± 9.3</td><td>53.1 ± 0.8</td><td>12.1<sup>+0.7</sup><sub>-0.7</sub></td><td>51.0 ± 1.5</td><td>-38.2 ± 1.6</td><td>28.6 ± 1.6</td><td>4.4 ± 3.2</td><td>7.1<sup>+0.4</sup><sub>-0.4</sub></td></tr><tr><td>113471–6120</td><td>G309.9206+00.4788*</td><td>6.6<sup>+0.6</sup><sub>-0.6</sub></td><td>2.4 × 1.9</td><td>71.9</td><td>1.0 × 1.0</td><td>848.0 ± 21.0</td><td>648.0 ± 10.0</td><td>1.6<sup>+0.1</sup><sub>-0.1</sub></td><td>347.8 ± 1.8</td><td>-57.0 ± 1.6</td><td>34.1 ± 1.6</td><td>1.1 ± 1.0</td><td>1.6<sup>+0.1</sup><sub>-0.1</sub></td></tr><tr><td>114013–6105</td><td>G311.6273+00.2902</td><td>3.5<sup>+0.7</sup><sub>-0.5</sub></td><td>5.0 × 4.8</td><td>155.0</td><td>4.8 × 4.3</td><td>1198.0 ± 34.0</td><td>171.0 ± 4.3</td><td>3.9<sup>+0.8</sup><sub>-0.5</sub></td><td>133.1 ± 1.5</td><td>-58.3 ± 1.6</td><td>37.6 ± 1.6</td><td>4.1 ± 3.0</td><td>3.0<sup>+0.6</sup><sub>-0.4</sub></td></tr></tbody></table>

*Note.* The * symbol after the core name indicates that this core is associated with a COM-containing core or COM-containing cores. FWHM is the measured core size while FWHM<sub>dec</sub> is the corresponding deconvolved size. R<sub>core</sub> follows the form of R<sub>eff</sub>/3600 × π/180 × D, where R<sub>eff</sub> is the effective radius equal to √FWHM<sub>dec</sub>/2, and D is the distance of the core. The errors on R<sub>core</sub> and R<sup>H40u</sup><sub>core</sub> mainly result from the distance uncertainties and those on the fluxes arise from the 2D Gaussian fitting in the core extraction. Only a small portion of the data is provided here and the full table will be available as supplementary material.

<table><caption>**Table 2.** Parameters of the COM-containing core but not H/UC-H II-associated cores with $N_{line} \ge 20$ (or pure s-cHMC).</caption><thead><tr><th>Name clump</th><th>Gal. name core</th><th>D kpc</th><th>FWHM maj(°) × min(°)</th><th>PA deg</th><th>FWHM<sub>dec</sub> maj(°) × min(°)</th><th>F<sup>int</sup><sub>3mm</sub> mJy</th><th>F<sup>P</sup><sub>3mm</sub> mJy beam<sup>-1</sup></th><th>R<sub>core</sub></th><th>N<sub>line</sub></th><th>log(M<sub>☉</sub>)</th><th>log(n<sub>core</sub>)</th><th>Σ<sub>core</sub></th></tr></thead><tbody><tr><td>108303–4303</td><td>G261.6444–02.0890</td><td>2.4<sup>+0.5</sup><sub>-0.6</sub></td><td>2.3 × 2.1</td><td>58.0</td><td>1.9 × 1.5</td><td>18.2 ± 0.8</td><td>7.0 ± 0.2</td><td>1.0<sup>+0.2</sup><sub>-0.2</sub></td><td>24</td><td>1.0<sup>+0.7</sup><sub>-0.7</sub></td><td>7.2<sup>+4.5</sup><sub>-4.5</sub></td><td>7.3</td></tr><tr><td>108470–4243</td><td>G263.2500+00.5137</td><td>2.4<sup>+0.6</sup><sub>-0.6</sub></td><td>2.6 × 2.1</td><td>147.6</td><td>2.1 × 1.5</td><td>38.0 ± 0.9</td><td>13.5 ± 0.2</td><td>1.0<sup>+0.2</sup><sub>-0.3</sub></td><td>81</td><td>1.3<sup>+1.0</sup><sub>-1.0</sub></td><td>7.4<sup>+4.8</sup><sub>-4.8</sub></td><td>13.8</td></tr><tr><td>113079–6218</td><td>G305.2084+00.2060</td><td>3.0<sup>+0.6</sup><sub>-0.7</sub></td><td>3.5 × 3.0</td><td>22.8</td><td>2.8 × 2.2</td><td>97.0 ± 2.6</td><td>39.1 ± 0.8</td><td>1.8<sup>+0.4</sup><sub>-0.4</sub></td><td>80</td><td>1.9<sup>+1.5</sup><sub>-1.6</sub></td><td>7.3<sup>+4.8</sup><sub>-4.9</sub></td><td>18.1</td></tr><tr><td>113134–6242</td><td>G305.7992–00.2447</td><td>2.0<sup>+0.6</sup><sub>-0.4</sub></td><td>3.4 × 2.7</td><td>171.5</td><td>2.4 × 2.1</td><td>103.8 ± 2.4</td><td>47.2 ± 0.8</td><td>1.1<sup>+0.3</sup><sub>-0.2</sub></td><td>61</td><td>1.6<sup>+1.4</sup><sub>-1.3</sub></td><td>7.6<sup>+4.9</sup><sub>-4.7</sub></td><td>23.6</td></tr><tr><td>113484–6100</td><td>G310.1436+00.7598</td><td>6.9<sup>+0.5</sup><sub>-0.7</sub></td><td>3.5 × 3.2</td><td>77.0</td><td>2.8 × 2.7</td><td>41.1 ± 1.7</td><td>13.0 ± 0.4</td><td>4.6<sup>+0.3</sup><sub>-0.5</sub></td><td>33</td><td>2.3<sup>+1.5</sup><sub>-1.6</sub></td><td>6.5<sup>+4.5</sup><sub>-4.6</sub></td><td>6.2</td></tr><tr><td>114498–5856</td><td>G318.0497+00.0868</td><td>2.9<sup>+0.4</sup><sub>-0.3</sub></td><td>3.9 × 3.0</td><td>63.4</td><td>3.5 × 2.4</td><td>60.7 ± 1.4</td><td>15.9 ± 0.3</td><td>2.0<sup>+0.3</sup><sub>-0.2</sub></td><td>39</td><td>1.7<sup>+1.1</sup><sub>-1.1</sub></td><td>7.0<sup>+4.3</sup><sub>-4.2</sub></td><td>8.3</td></tr><tr><td>115394–5358</td><td>G326.4747+00.7030</td><td>2.4<sup>+0.3</sup><sub>-0.2</sub></td><td>5.2 × 4.4</td><td>140.9</td><td>4.9 × 4.0</td><td>226.7 ± 5.4</td><td>28.4 ± 0.6</td><td>2.5<sup>+0.3</sup><sub>-0.2</sub></td><td>33</td><td>2.1<sup>+1.5</sup><sub>-1.4</sub></td><td>7.2<sup>+4.2</sup><sub>-4.1</sub></td><td>13.3</td></tr></tbody></table>

*Note.* The parameters FWHM, FWHM<sub>dec</sub>, and R<sub>core</sub> are derived in the same way as in Table 1. The errors on R<sub>core</sub>, M<sub>☉</sub>, and n<sub>core</sub> mainly result from the distance uncertainties, and those on the fluxes from the 2D Gaussian fitting in the core extraction. Only a small portion of the data is provided here and the full table will be available as supplementary material.

<table><caption>**Table 3.** Parameters of the COM-containing core but not H/UC-H II-associated cores with $5 \le N_{line} < 20$ (or pure w-cHMC).</caption><thead><tr><th>Name clump</th><th>Gal. name core</th><th>D kpc</th><th>FWHM maj(°) × min(°)</th><th>PA deg</th><th>FWHM<sub>dec</sub> maj(°) × min(°)</th><th>F<sup>int</sup><sub>3mm</sub> mJy</th><th>F<sup>P</sup><sub>3mm</sub> mJy beam<sup>-1</sup></th><th>R<sub>core</sub></th><th>N<sub>line</sub></th><th>log(M<sub>☉</sub>)</th><th>log(n<sub>core</sub>)</th><th>Σ<sub>core</sub></th></tr></thead><tbody><tr><td>108448–4343</td><td>G263.7737–00.4326</td><td>1.4<sup>+0.6</sup><sub>-0.8</sub></td><td>3.5 × 2.3</td><td>113.0</td><td>3.1 × 2.0</td><td>5.6 ± 1.2</td><td>1.3 ± 0.2</td><td>0.9<sup>+0.4</sup><sub>-0.5</sub></td><td>5</td><td>0.1<sup>+0.0</sup><sub>-0.1</sub></td><td>6.5<sup>+3.5</sup><sub>-3.6</sub></td><td>1.0</td></tr><tr><td>109018–4816</td><td>G269.1523–01.1279</td><td>2.8<sup>+0.6</sup><sub>-0.7</sub></td><td>4.3 × 2.7</td><td>178.5</td><td>4.1 × 2.2</td><td>51.9 ± 2.1</td><td>8.6 ± 0.3</td><td>2.1<sup>+0.4</sup><sub>-0.5</sub></td><td>12</td><td>1.6<sup>+1.3</sup><sub>-1.3</sub></td><td>6.9<sup>+4.4</sup><sub>-4.4</sub></td><td>6.6</td></tr><tr><td>109018–4816</td><td>G269.1506–01.1279</td><td>2.8<sup>+0.6</sup><sub>-0.7</sub></td><td>3.2 × 2.2</td><td>85.9</td><td>2.8 × 1.8</td><td>25.1 ± 1.5</td><td>7.0 ± 0.3</td><td>1.5<sup>+0.3</sup><sub>-0.4</sub></td><td>6</td><td>1.3<sup>+0.9</sup><sub>-1.0</sub></td><td>7.0<sup>+4.4</sup><sub>-4.5</sub></td><td>5.7</td></tr><tr><td>110365–5803</td><td>G286.2074+00.1698</td><td>3.4<sup>+0.6</sup><sub>-0.6</sub></td><td>3.6 × 3.0</td><td>81.9</td><td>3.1 × 2.5</td><td>31.7 ± 1.0</td><td>9.2 ± 0.2</td><td>2.3<sup>+0.4</sup><sub>-0.4</sub></td><td>10</td><td>1.6<sup>+1.1</sup><sub>-1.2</sub></td><td>6.7<sup>+4.3</sup><sub>-4.3</sub></td><td>4.7</td></tr><tr><td>111298–6155</td><td>G293.8274–00.7461</td><td>9.4<sup>+0.4</sup><sub>-0.3</sub></td><td>4.0 × 3.0</td><td>92.8</td><td>3.6 × 2.3</td><td>41.8 ± 1.9</td><td>11.8 ± 0.4</td><td>6.6<sup>+0.3</sup><sub>-0.2</sub></td><td>10</td><td>2.6<sup>+1.5</sup><sub>-1.4</sub></td><td>6.3<sup>+4.4</sup><sub>-4.3</sub></td><td>5.8</td></tr><tr><td>111332–6258</td><td>G294.5115–01.6213</td><td>1.1<sup>+0.7</sup><sub>-0.6</sub></td><td>5.9 × 4.7</td><td>81.2</td><td>5.6 × 4.2</td><td>30.5 ± 2.0</td><td>3.8 ± 0.2</td><td>1.3<sup>+0.8</sup><sub>-0.7</sub></td><td>6</td><td>0.6<sup>+0.7</sup><sub>-0.6</sub></td><td>6.5<sup>+3.5</sup><sub>-3.4</sub></td><td>1.5</td></tr><tr><td>113079–6218</td><td>G305.2022+00.2072</td><td>3.0<sup>+0.6</sup><sub>-0.7</sub></td><td>3.5 × 3.2</td><td>105.0</td><td>3.0 × 2.0</td><td>20.5 ± 2.8</td><td>7.8 ± 0.8</td><td>1.8<sup>+0.4</sup><sub>-0.4</sub></td><td>11</td><td>1.3<sup>+0.9</sup><sub>-0.9</sub></td><td>6.6<sup>+4.1</sup><sub>-4.2</sub></td><td>3.9</td></tr></tbody></table>

*Note.* The parameters FWHM, FWHM<sub>dec</sub>, and R<sub>core</sub> are derived in the same way as in Table 1. The errors on R<sub>core</sub>, M<sub>☉</sub>, and n<sub>core</sub> mainly result from the distance uncertainties, and those on the fluxes from the 2D Gaussian fitting in the core extraction. Only a small portion of the data is provided here and the full table will be available as supplementary material.
<table><caption>**Table 4.** Parameters of the ‘unknown’ cores (i.e. no signature of H/UC-H II nor cHMC).</caption><thead><tr><th>Name<br>clump</th><th>Gal. name<br>core</th><th>D<br>kpc</th><th>FWHM<br>maj(′′) × min(′′)</th><th>PA<br>deg</th><th>FWHM<sub>dec</sub><br>maj(′′) × min(′′)</th><th>F<sup>int.</sup><sub>3mm</sub><br>mJy</th><th>F<sup>p</sup><sub>3mm</sub><br>mJy beam<sup>-1</sup></th><th>R<sub>core</sub><br>10<sup>-2</sup> pc</th><th>log(M<sub>core</sub>)<br>M<sub>☉</sub></th><th>log(n<sub>core</sub>)<br>cm<sup>-3</sup></th><th>Σ<sub>core</sub><br>g cm<sup>-2</sup></th></tr></thead><tbody><tr><td>I08076-3556</td><td>G253.2971-01.6156</td><td>1.0<sup>+0.5</sup><sub>-0.5</sub></td><td>5.1 × 3.3</td><td>86.4</td><td>4.9 × 3.0</td><td>11.6 ± 1.2</td><td>1.3 ± 0.1</td><td>0.9<sup>+0.4</sup><sub>-0.5</sub></td><td>0.9<sup>+0.8</sup><sub>-0.9</sub></td><td>7.3<sup>+3.9</sup><sub>-4.0</sub></td><td>5.5</td></tr><tr><td>I08076-3556</td><td>G253.2930-01.6113</td><td>1.0<sup>+0.5</sup><sub>-0.5</sub></td><td>2.2 × 1.6</td><td>99.3</td><td>1.6 × 1.1</td><td>18.8 ± 0.5</td><td>9.8 ± 0.2</td><td>0.3<sup>+0.1</sup><sub>-0.2</sub></td><td>1.1<sup>+1.1</sup><sub>-1.1</sub></td><td>8.6<sup>+5.3</sup><sub>-5.4</sub></td><td>80.1</td></tr><tr><td>I08303-4303</td><td>G261.6446-02.0899</td><td>2.4<sup>+0.5</sup><sub>-0.6</sub></td><td>4.9 × 2.5</td><td>6.9</td><td>4.7 × 2.0</td><td>23.7 ± 1.4</td><td>3.6 ± 0.2</td><td>1.8<sup>+0.4</sup><sub>-0.4</sub></td><td>1.7<sup>+1.3</sup><sub>-1.4</sub></td><td>7.2<sup>+4.5</sup><sub>-4.5</sub></td><td>10.2</td></tr><tr><td>I08303-4303</td><td>G261.6444-02.0876</td><td>2.4<sup>+0.5</sup><sub>-0.6</sub></td><td>4.0 × 3.8</td><td>40.0</td><td>3.8 × 3.5</td><td>15.2 ± 1.6</td><td>1.8 ± 0.2</td><td>2.1<sup>+0.5</sup><sub>-0.5</sub></td><td>1.5<sup>+1.1</sup><sub>-1.2</sub></td><td>6.8<sup>+4.1</sup><sub>-4.1</sub></td><td>4.6</td></tr><tr><td>I08448-4343</td><td>G263.7776-00.4332</td><td>1.4<sup>+0.6</sup><sub>-0.8</sub></td><td>5.2 × 3.0</td><td>116.0</td><td>5.0 × 2.8</td><td>8.8 ± 1.7</td><td>1.1 ± 0.2</td><td>1.3<sup>+0.6</sup><sub>-0.7</sub></td><td>0.9<sup>+0.8</sup><sub>-0.9</sub></td><td>6.9<sup>+3.9</sup><sub>-4.0</sub></td><td>3.1</td></tr><tr><td>I08448-4343</td><td>G263.7729-00.4364</td><td>1.4<sup>+0.6</sup><sub>-0.8</sub></td><td>2.5 × 1.8</td><td>72.0</td><td>2.1 × 1.1</td><td>2.1 ± 0.8</td><td>0.9 ± 0.2</td><td>0.5<sup>+0.2</sup><sub>-0.3</sub></td><td>0.3<sup>+0.2</sup><sub>-0.3</sub></td><td>7.2<sup>+4.2</sup><sub>-4.3</sub></td><td>4.5</td></tr><tr><td>I08448-4343</td><td>G263.7724-00.4366</td><td>1.4<sup>+0.6</sup><sub>-0.8</sub></td><td>2.2 × 1.8</td><td>103.0</td><td>1.5 × 1.3</td><td>1.9 ± 0.7</td><td>0.9 ± 0.2</td><td>0.5<sup>+0.2</sup><sub>-0.3</sub></td><td>0.2<sup>+0.2</sup><sub>-0.3</sub></td><td>7.2<sup>+4.3</sup><sub>-4.3</sub></td><td>4.7</td></tr><tr><td>I08448-4343</td><td>G263.7723-00.4350</td><td>1.4<sup>+0.6</sup><sub>-0.8</sub></td><td>4.4 × 2.2</td><td>80.6</td><td>3.6 × 1.8</td><td>7.3 ± 0.0</td><td>5.8 ± 0.2</td><td>0.9<sup>+0.4</sup><sub>-0.5</sub></td><td>0.8<sup>+0.7</sup><sub>-0.8</sub></td><td>7.8<sup>+4.8</sup><sub>-4.9</sub></td><td>5.5</td></tr><tr><td>I08448-4343</td><td>G263.7744-00.4328</td><td>1.4<sup>+0.6</sup><sub>-0.8</sub></td><td>2.5 × 2.2</td><td>18.0</td><td>2.1 × 1.6</td><td>11.5 ± 0.9</td><td>3.9 ± 0.2</td><td>0.6<sup>+0.3</sup><sub>-0.3</sub></td><td>1.0<sup>+0.9</sup><sub>-1.0</sub></td><td>7.7<sup>+4.8</sup><sub>-4.9</sub></td><td>16.5</td></tr><tr><td>I08448-4343</td><td>G263.7712-00.4363</td><td>1.4<sup>+0.6</sup><sub>-0.8</sub></td><td>3.2 × 1.8</td><td>157.0</td><td>2.9 × 1.1</td><td>2.4 ± 0.9</td><td>0.8 ± 0.2</td><td>0.6<sup>+0.3</sup><sub>-0.3</sub></td><td>0.3<sup>+0.3</sup><sub>-0.4</sub></td><td>7.1<sup>+4.1</sup><sub>-4.2</sub></td><td>3.7</td></tr></tbody></table>

Note. The parameters FWHM, FWHM<sub>dec</sub>, and R<sub>core</sub> are derived in the same way as in Table 1. The errors on R<sub>core</sub>, M<sub>core</sub>, and n<sub>core</sub> mainly come from the distance uncertainties, those on the fluxes from the 2D Gaussian fitting in the core extraction. Only a small portion of the data is provided here, and the full table will be available as supplementary material.

## REFERENCE

Liu H.-L. et al., 2021, MNRAS, 505, 2801

## SUPPORTING INFORMATION

Supplementary data are available at MNRAS online.

**Table S1.** Parameters of 91 H/UC-H II cores.

**Table S2.** Parameters of 31 COM-containing cores with $N_{line} \ge 20$ (or pure s-cHMC).

**Table S3.** Parameters of 51 COM-containing cores with $5 \le N_{line} < 20$ (or pure w-cHMC).

**Table S4.** Parameters of 280 ‘unknown’ cores (i.e., no signature of H/UC-H II nor cHMC).

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