# Erratum: "Molecules with ALMA at Planet-forming Scales (MAPS). III. Characteristics of Radial Chemical Substructures" (2021, ApJS, 257, 3)

Charles J. Law, Ryan A. Loomis, Richard Teague, Karin I. Öberg, Ian Czekala, Sean M. Andrews, Jane Huang, Yuri Aikawa, Felipe Alarcón, Jaehan Bae, et al.

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Charles J. Law, Ryan A. Loomis, Richard Teague, Karin I. Öberg, Ian Czekala, et al. Erratum: "Molecules with ALMA at Planet-forming Scales (MAPS). III. Characteristics of Radial Chemical Substructures" (2021, ApJS, 257, 3). 2022, 10.3847/1538-4365/ac69e9. insu-03705348

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# Erratum: “Molecules with ALMA at Planet-forming Scales (MAPS). III. Characteristics of Radial Chemical Substructures” (2021, ApJS, 257, 3)

Charles J. Law<fnref n="1" />, Ryan A. Loomis<fnref n="2" />, Richard Teague<fnref n="1" />, Karin I. Öberg<fnref n="1" />, Ian Czekala<fnref n="3" />,<fnref n="4" />,<fnref n="5" />,<fnref n="6" />,<fnref n="7" />,<fnref n="24" />, Sean M. Andrews<fnref n="1" />, Jane Huang<fnref n="1" />,<fnref n="8" />,<fnref n="24" />, Yuri Aikawa<fnref n="9" />, Felipe Alarcón<fnref n="8" />, Jaehan Bae<fnref n="10" />,<fnref n="11" />,<fnref n="24" />, Edwin A. Bergin<fnref n="8" />, Jennifer B. Bergner<fnref n="12" />,<fnref n="24" />, Yann Boehler<fnref n="13" />, Alice S. Booth<fnref n="14" />,<fnref n="15" />, Arthur D. Bosman<fnref n="8" />, Jenny K. Calahan<fnref n="8" />, Gianni Cataldi<fnref n="9" />,<fnref n="16" />, L. Ilsedore Cleeves<fnref n="17" />, Kenji Furuya<fnref n="16" />, Viviana V. Guzmán<fnref n="18" />, John D. Ilee<fnref n="15" />, Romane Le Gal<fnref n="1" />,<fnref n="13" />,<fnref n="19" />,<fnref n="20" />, Yao Liu<fnref n="21" />, Feng Long<fnref n="1" />, François Ménard<fnref n="13" />, Hideko Nomura<fnref n="16" />, Chunhua Qi<fnref n="1" />, Kamber R. Schwarz<fnref n="22" />,<fnref n="24" />, Anibal Sierra<fnref n="23" />, Takashi Tsukagoshi<fnref n="16" />, Yoshihide Yamato<fnref n="9" />, Merel L. R. van 't Hoff<fnref n="8" />, Catherine Walsh<fnref n="15" />, David J. Wilner<fnref n="1" />, and Ke Zhang<fnref n="8" />,<fnref n="25" />

Received 2022 April 22; published 2022 May 13

In the published article, we computed the disk size in 18 molecular emission lines and the 90 and 260 GHz continuum for all sources (Section 3.5). We defined $R_{\text{gas}}$ as the radius which encloses 90% of the total line emission or continuum flux. However, we omitted the necessary factor of $2\pi r$ when computing the cumulative sums, i.e., the integral of a radial function has an areal element of $2\pi r dr$.

Table 2 is revised and lists the updated gas and continuum disk sizes, and Figures 15 and 16 are also updated. For all sources, the disk size of each line increases in nearly all cases, with mean increases of 45% (IM Lup), 47% (GM Aur), 22% (AS 209), 44% (HD 163296), and 43% (MWC 480). The most notable changes are ≥100% increases in the continuum sizes of the IM Lup and MWC 480 disks. The continuum emission in the AS 209 disk is no longer smaller than the majority of lines, and instead it is slightly larger than the complex nitriles and comparable to that of C$_{2}$H 3–2 and CS 2–1.

Overall, the relative ordering of disk sizes among lines remains approximately the same, as shown in Figures 15 and 16, and all subsequent discussion and conclusions presented in the published article remain unchanged.

## ORCID iDs

Charles J. Law https://orcid.org/0000-0001-1413-1776

Ryan A. Loomis https://orcid.org/0000-0002-8932-1219

Richard Teague https://orcid.org/0000-0003-1534-5186

Karin I. Öberg https://orcid.org/0000-0001-8798-1347

Ian Czekala https://orcid.org/0000-0002-1483-8811

Sean M. Andrews https://orcid.org/0000-0003-2253-2270

Jane Huang https://orcid.org/0000-0001-6947-6072

Yuri Aikawa https://orcid.org/0000-0003-3283-6884

Felipe Alarcón https://orcid.org/0000-0002-2692-7862

Jaehan Bae https://orcid.org/0000-0001-7258-770X

Edwin A. Bergin https://orcid.org/0000-0003-4179-6394

Jennifer B. Bergner https://orcid.org/0000-0002-8716-0482

Yann Boehler https://orcid.org/0000-0002-8692-8744

Alice S. Booth https://orcid.org/0000-0003-2014-2121

Arthur D. Bosman https://orcid.org/0000-0003-4001-3589

Jenny K. Calahan https://orcid.org/0000-0002-0150-0125

Gianni Cataldi https://orcid.org/0000-0002-2700-9676

L. Ilsedore Cleeves https://orcid.org/0000-0003-2076-8001

Kenji Furuya https://orcid.org/0000-0002-2026-8157

Viviana V. Guzmán https://orcid.org/0000-0003-4784-3040

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Original content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further

distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.

<footnote n="1">¹Center for Astrophysics | Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA; charles.law@cfa.harvard.edu</footnote>

<footnote n="2">²National Radio Astronomy Observatory, 520 Edgemont Rd., Charlottesville, VA 22903, USA</footnote>

<footnote n="3">³Department of Astronomy and Astrophysics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA</footnote>

<footnote n="4">⁴Center for Exoplanets and Habitable Worlds, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA</footnote>

<footnote n="5">⁵Center for Astrostatistics, 525 Davey Laboratory, The Pennsylvania State University, University Park, PA 16802, USA</footnote>

<footnote n="6">⁶Institute for Computational & Data Sciences, The Pennsylvania State University, University Park, PA 16802, USA</footnote>

<footnote n="7">⁷Department of Astronomy, 501 Campbell Hall, University of California, Berkeley, CA 94720-3411, USA</footnote>

<footnote n="8">⁸Department of Astronomy, University of Michigan, 323 West Hall, 1085 S. University Avenue, Ann Arbor, MI 48109, USA</footnote>

<footnote n="9">⁹Department of Astronomy, Graduate School of Science, The University of Tokyo, Tokyo 113-0033, Japan</footnote>

<footnote n="10">¹⁰Earth and Planets Laboratory, Carnegie Institution for Science, 5241 Broad Branch Road NW, Washington, DC 20015, USA</footnote>

<footnote n="11">¹¹Department of Astronomy, University of Florida, Gainesville, FL 32611, USA</footnote>

<footnote n="12">¹²University of Chicago, Department of the Geophysical Sciences, Chicago, IL 60637, USA</footnote>

<footnote n="13">¹³Univ. Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France</footnote>

<footnote n="14">¹⁴Leiden Observatory, Leiden University, 2300 RA Leiden, The Netherlands</footnote>

<footnote n="15">¹⁵School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK</footnote>

<footnote n="16">¹⁶National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan</footnote>

<footnote n="17">¹⁷Department of Astronomy, University of Virginia, Charlottesville, VA 22904, USA</footnote>

<footnote n="18">¹⁸Instituto de Astrofísica, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, 7820436 Macul, Santiago, Chile</footnote>

<footnote n="19">¹⁹IRAP, Université de Toulouse, CNRS, CNES, UT3, F-31400 Toulouse, France</footnote>

<footnote n="20">²⁰IRAM, 300 rue de la piscine, F-38406 Saint-Martin d'Hères, France</footnote>

<footnote n="21">²¹Purple Mountain Observatory & Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, Nanjing 210023, People's Republic of China</footnote>

<footnote n="22">²²Lunar and Planetary Laboratory, University of Arizona, 1629 E. University Blvd., Tucson, AZ 85721, USA</footnote>

<footnote n="23">²³Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile</footnote>

<footnote n="24">²⁴ NASA Hubble Fellowship Program Sagan Fellow.</footnote>

<footnote n="25">²⁵ NASA Hubble Fellow.</footnote>
<figure><img src="image_5.png" /><figcaption>**Figure 15.** Gas disk size for all lines organized by increasing sizes within each disk. Sizes are color coded by species, as described in Section 3.5. The size of the 90 and 260 GHz continuum disks are shown as gray hatched bars for comparison. The aggregate panel shows mean sizes of each line across the MAPS disks with error bars showing the standard deviation. Disk sizes are defined as the radius containing 90% of total flux.</figcaption></figure>

<table><caption>**Table 2**
Gas Disk Sizes</caption><thead><tr><th rowspan="2">Line</th><th colspan="5">Disk Size (au)</th></tr><tr><th>IM Lup</th><th>GM Aur</th><th>AS 209</th><th>HD 163296</th><th>MWC 480</th></tr></thead><tbody><tr><td>CO 2-1</td><td>753 ± 6</td><td>616 ± 9</td><td>272 ± 4</td><td>459 ± 4</td><td>573 ± 7</td></tr><tr><td><sup>13</sup>CO 2-1</td><td>540 ± 7</td><td>427 ± 9</td><td>196 ± 5</td><td>364 ± 4</td><td>419 ± 7</td></tr><tr><td><sup>13</sup>CO 1-0</td><td>543 ± 16</td><td>410 ± 16</td><td>190 ± 10</td><td>340 ± 8</td><td>392 ± 17</td></tr><tr><td>C<sup>18</sup>O 2-1</td><td>404 ± 14</td><td>297 ± 24</td><td>176 ± 5</td><td>301 ± 4</td><td>326 ± 11</td></tr><tr><td>C<sup>18</sup>O 1-0</td><td>436 ± 45</td><td>219 ± 26</td><td>160 ± 9</td><td>275 ± 11</td><td>312 ± 40</td></tr><tr><td>C<sub>2</sub>H 3-2</td><td>478 ± 18</td><td>200 ± 12</td><td>115 ± 5</td><td>352 ± 8</td><td>120 ± 7</td></tr><tr><td>C<sub>2</sub>H 1-0</td><td>114 ± 15</td><td>56 ± 17</td><td>110 ± 9</td><td>153 ± 55</td><td>113 ± 14</td></tr><tr><td>c-C<sub>3</sub>H<sub>2</sub> 7-6</td><td>...</td><td>169 ± 16</td><td>112 ± 8</td><td>162 ± 20</td><td>122 ± 13</td></tr><tr><td>H<sub>2</sub>CO 3-2</td><td>474 ± 15</td><td>366 ± 13</td><td>202 ± 7</td><td>404 ± 9</td><td>375 ± 29</td></tr><tr><td>HCO<sup>+</sup> 1-0</td><td>492 ± 50</td><td>389 ± 25</td><td>199 ± 15</td><td>385 ± 13</td><td>408 ± 26</td></tr><tr><td>CS 2-1</td><td>592 ± 21</td><td>197 ± 13</td><td>124 ± 10</td><td>177 ± 11</td><td>114 ± 31</td></tr><tr><td>HCN 3-2</td><td>418 ± 9</td><td>295 ± 13</td><td>159 ± 5</td><td>361 ± 4</td><td>176 ± 24</td></tr><tr><td>HCN 1-0</td><td>638 ± 45</td><td>306 ± 100</td><td>115 ± 9</td><td>447 ± 9</td><td>92 ± 47</td></tr><tr><td>DCN 3-2</td><td>397 ± 17</td><td>76 ± 10</td><td>112 ± 6</td><td>161 ± 37</td><td>126 ± 12</td></tr><tr><td>HC<sub>3</sub>N 29-28</td><td>...</td><td>77 ± 11</td><td>93 ± 5</td><td>86 ± 6</td><td>98 ± 8</td></tr><tr><td>HC<sub>3</sub>N 11-10</td><td>...</td><td>71 ± 26</td><td>108 ± 10</td><td>126 ± 16</td><td>126 ± 15</td></tr><tr><td>CN 1-0</td><td>594 ± 18</td><td>412 ± 16</td><td>231 ± 9</td><td>482 ± 9</td><td>530 ± 16</td></tr><tr><td>CH<sub>3</sub>CN 12-11</td><td>90 ± 12</td><td>100 ± 21</td><td>98 ± 10</td><td>54 ± 5</td><td>114 ± 14</td></tr><tr><td>90 GHz continuum</td><td>222 ± 10</td><td>171 ± 14</td><td>123 ± 8</td><td>111 ± 6</td><td>105 ± 13</td></tr><tr><td>260 GHz continuum</td><td>242 ± 4</td><td>194 ± 5</td><td>128 ± 3</td><td>139 ± 3</td><td>111 ± 5</td></tr></tbody></table>

**Note.** Disk size was computed as the radius which encloses 90% of the total disk flux (see Section 3.5). Note that this is often smaller than the total radial extent of an emission line due to the presence of diffuse, low flux emission at large radii.

John D. Ilee https://orcid.org/0000-0003-1008-1142

Romane Le Gal https://orcid.org/0000-0003-1837-3772

Yao Liu https://orcid.org/0000-0002-7616-666X

Feng Long https://orcid.org/0000-0002-7607-719X

François Ménard https://orcid.org/0000-0002-1637-7393

Hideko Nomura https://orcid.org/0000-0002-7058-7682
<figure><img src="image_6.png" /><figcaption>**Figure 16.** Gas disk size of chemical species in astronomical units for each disk plotted against one another. Spearman correlation coefficients are displayed in the upper left corners of each scatter plot. A one-to-one size ratio is shown as a gray dashed line. Sizes are color coded by species according to the legend. In general, the distribution of sizes in different species is quite consistent among disks.</figcaption></figure>

Chunhua Qi https://orcid.org/0000-0001-8642-1786

Kamber R. Schwarz https://orcid.org/0000-0002-6429-9457

Anibal Sierra https://orcid.org/0000-0002-5991-8073

Takashi Tsukagoshi https://orcid.org/0000-0002-6034-2892

Yoshihide Yamato https://orcid.org/0000-0003-4099-6941

Merel L. R. van 't Hoff https://orcid.org/0000-0002-2555-9869

Catherine Walsh https://orcid.org/0000-0001-6078-786X

David J. Wilner https://orcid.org/0000-0003-1526-7587

Ke Zhang https://orcid.org/0000-0002-0661-7517