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Molecules with ALMA at Planet-forming Scales (MAPS). VIII. CO Gap in AS 209—Gas Depletion or Chemical Processing?

Authors: Felipe Alarcón, Arthur D. Bosman, Edwin A. Bergin, Ke Zhang, Richard Teague, Jaehan Bae, Yuri Aikawa, Sean M. Andrews, Alice S. Booth, Jenny K. Calahan, Gianni Cataldi, Ian Czekala, Jane Huang, John D. Ilee, Charles J. Law, Romane Le Gal, Yao Liu, Feng Long, Ryan A. Loomis, François Ménard, Karin I. Öberg, Kamber R. Schwarz, Merel L. R. van 't Hoff, Catherine Walsh, David J. Wilner

Felipe Alarcón et al 2021 The Astrophysical Journal Supplement Series 257 .

Provider: AAS Journals

Caption: Figure 15.

C₂H 2D abundance structure in each set of simulations. Top row: C₂H abundance structure for Model A. Bottom row: C₂H abundance structure for Model B. In the regions where the small dust is depleted, C₂H can be produced closer to the midplane. This causes the slight increases in C₂H column density observed in Figure 9.

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