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Primordial or Secondary? Testing Models of Debris Disk Gas with ALMA*
Gianni Cataldi (National Astronomical Observatory of Japan, The University of Tokyo), Yuri Aikawa (The University of Tokyo), Kazunari Iwasaki (National Astronomical Observatory of Japan), Sebastián Marino (University of Exeter), A. Brandeker (Stockholm University, AlbaNova), Antonio S. Hales (National Radio Astronomy Observatory, Atacama Large Millimeter Submillimeter Array), Thomas K. Henning (Max Planck Institute for Astronomy), Aya E. Higuchi (Tokyo Denki University), A. Meredith Hughes (Wesleyan University), M. Janson (Stockholm University, AlbaNova), Quentin Kral (Centre National de la Recherche Scientifique, Université Paris Sciences et Lettres), Luca Matrà (Trinity College Dublin), A. Moór (Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences), Göran Olofsson (Stockholm University, AlbaNova), Seth Redfield (Wesleyan University), Aki Roberge (Goddard Space Flight Center)
Abstract: Abstract The origin and evolution of gas in debris disks are still not well understood. Secondary gas production from cometary material or a primordial origin have been proposed. So far, observations have mostly concentrated on CO, with only a few C observations available. We overview the C and CO content of debris disk gas and test state-of-the-art models. We use new and archival Atacama Large Millimeter/submillimeter Array (ALMA) observations of CO and C i emission, complemented by C ii data from Herschel, for a sample of 14 debris disks. This expands the number of disks with ALMA measurements of both CO and C i by 10 disks. We present new detections of C i emission toward three disks: HD 21997, HD 121191, and HD 121617. We use a simple disk model to derive gas masses and column densities. We find that current state-of-the-art models of secondary gas production overpredict the C0 content of debris disk gas. This does not rule out a secondary origin, but might indicate that the models require an additional C removal process. Alternatively, the gas might be produced in transient events rather than a steady-state collisional cascade. We also test a primordial gas origin by comparing our results to a simplified thermochemical model. This yields promising results, but more detailed work is required before a conclusion can be reached. Our work demonstrates that the combination of C and CO data is a powerful tool to advance our understanding of debris disk gas.