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Unveiling the physical and chemical conditions in the young disk around L1527
van 't Hoff, M. L. R.; Tobin, J. J.; Harsono, D.; van Dishoeck, E. F.
AA(Leiden Observatory, Leiden University, PO box 9513, NL-2300 RA, Leiden, the Netherlands ), AB(Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, 440 W. Brooks Street, Norman, OK 73019, USA), AC(Leiden Observatory, Leiden University, PO box 9513, NL-2300 RA, Leiden, the Netherlands ), AD(Leiden Observatory, Leiden University, PO box 9513, NL-2300 RA, Leiden, the Netherlands ; Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany)
Astrochemistry VII: Through the Cosmos from Galaxies to Planets, Proceedings of the International Astronomical Union, IAU Symposium, Volume 332, pp. 121-123
Publication Date:
stars: individual (L1527 IRS), stars: formation, astrochemistry
Abstract Copyright:
(c) 2018: Copyright © International Astronomical Union 2018
Bibliographic Code:


Planets form in disks around young stars. The planet formation process may start when the protostar and disk are still deeply embedded within their infalling envelope. However, unlike more evolved protoplanetary disks, the physical and chemical structure of these young embedded disks are still poorly constrained. We have analyzed ALMA data for 13CO, C18O and N2D+ to constrain the temperature structure, one of the critical unknowns, in the disk around L1527. The spatial distribution of 13CO and C18O, together with the kinetic temperature derived from the optically thick 13CO emission and the non-detection of N2D+, suggest that this disk is warm enough (>~ 20 K) to prevent CO freeze-out.
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