Observational Diagnostics of Gas in Protoplanetary Disks
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Protoplanetary disks are composed primarily of gas (99% of the mass). Nevertheless, relatively few observational constraints exist for the gas in disks. In this review, I discuss several observational diagnostics in the UV, optical, near-IR, mid-IR, and (sub)-mm wavelengths that have been employed to study the gas in the disks of young stellar objects. I concentrate in diagnostics that probe the inner 20 AU of the disk, the region where planets are expected to form. I discuss the potential and limitations of each gas tracer and present prospects for future research.
KeywordsProtoplanetary disks Observations Gas Spectroscopy
I would like to thank the organizers of the Ascona planet formation meeting for inviting me to give the observations of gas in disks talk, and to R. Nelson, C.P. Dullemond, C. Clarke and S. Fromang for kindly accepting that I present my talk as in individual contribution in this volume. I am grateful for the detailed suggestions in the manuscript provided by M. Audard, C. Baldovin-Saavedra and F. Fontani. I would like to warmly thank M. van den Ancker, Y. Pavluychenkov, M. Goto, C.P. Dullemond, Th. Henning, C. Martin-Zaïdi, G. van der Plas and D. Fedele for all the discussions about gas in disks during the last years. Part of this work is supported by a Swiss National Science Fundation grant to M. Audard.
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