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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 14.

CO abundance structure for both model sets, A and B, with different localized depletion factors of small grains from left to right. Top row: CO abundance structure for Model A, where CO has been depleted and the gas surface density has a smooth profile. Bottom row: CO abundance structure for Model B, where CO is considered to trace the gas surface density by a constant scaling or CO/H2 ratio. In both models, there are not significant changes with different degrees of small-grains depletion. However, we observe that in Model A, CO has a more uniform vertical distribution than in Model B.

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