Measuring the icy content of protoplanetary disks with JWST J.A. Sturm 1 , M.K. McClure 1 , J.B. Bergner 2 , D. Harsono 3 , E. Dartois 4 , M.N. Drozdovskaya 5 , S. Ioppolo 6 , K.I. Öberg 7 , C.J. Law 7 , M.E. Palumbo 8 , Y.J. Pendleton 9 , W.R.M. Rocha 1,10 , H. Terada 11,12 and R.G. Urso 8 , Ice Age collaboration 1 Leiden Observatory, Leiden University, P.O. Box 9513, NL-2300 RA Leiden, The Netherlands, 2 Department of Chemistry, University of California, Berkeley, California 94720-1460, United States. 3 Institute of Astronomy and Astrophysics, Academia Sinica, No. 1, Sec. 4, Roosevelt Road, Taipei 10617, Taiwan, R. O. C. 4 Institut des Sciences Moléculaires d’Orsay, CNRS, Univ. Paris-Saclay, 91405 Orsay, France. 5 Center for Space and Habitability, Universität Bern, Gesellschaftsstrasse 6, 3012, Bern, Switzerland. 6 Center for Interstellar Catalysis, Department of Physics and Astronomy, Aarhus University, Ny Munkegade 120, Aarhus C 8000, Denmark. 7 Center for Astrophysics | Harvard & Smithsonian, 60 Garden St., Cambridge, MA 02138, USA. 8 INAF – Osservatorio Astrofisico di Catania, via Santa Sofia 78, 95123 Catania, Italy 9 Department of Physics, University of Central Florida, Orlando, FL 32816, USA. 10 Laboratory for Astrophysics, Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden, The Netherlands. 11 TMT International Observatory, 100 W Walnut St, Suite 300, Pasadena, CA USA. 12 National Astronomical Observatory of Japan, National Institutes of Natural Sciences (NINS), 2-21-1 Osawa, Mitaka, Tokyo 181- 8588, Japan. Ices constitute the bulk reservoir of volatiles like C, N, and O in cold protoplanetary disks, and are thought to be the carriers and precursors of the complex organic molecules seen in Solar System comets. Protoplanetary disk ices can be observed in absorption against the continuum of the warm inner regions in edge-on disks, with features all across the mid-infrared. With the advent of JWST, we can spatially resolve the icy content in comet forming regions for the first time, with unprecedented sensitivity. However, inferring abundances from the spatially resolved ice features in the mid-infrared is non-trivial due to strong radiative transfer effects on the absorption feature strength and shape. I will present the very first resolved JWST/NIRSpec observations of ices in an edge- on disk, as part of the Ice Age ERS program, and show the first steps towards understanding JWST ice features in protoplanetary disks using radiative transfer models. References 1. Sturm et al. (resubm.) The edge-on HH 48 NE protoplanetary disk I. Modeling the geometry and stellar parameters
2. Sturm et al. (resubm.) The edge-on HH 48 NE protoplanetary disk II. Modeling the ices and silicates 3. Sturm et al. (in prep.) The edge-on HH 48 NE protoplanetary disk III. NIRSpec observations
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