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The TW Hya Rosetta Stone Project. I. Radial and Vertical Distributions of DCN and DCO⁺

Öberg, Karin I. and Cleeves, L. Ilsedore and Bergner, Jennifer B. and Cavanaro, Joseph and Teague, Richard and Huang, Jane and Loomis, Ryan A. and Bergin, Edwin A. and Blake, Geoffrey A. and Calahan, Jenny and Cazzoletti, Paolo and Guzmán, Viviana Veloso and Hogerheijde, Michiel R. and Kama, Mihkel and Terwisscha van Scheltinga, Jeroen and Qi, Chunhua and van Dishoeck, Ewine F. and Walsh, Catherine and Wilner, David J. (2021) The TW Hya Rosetta Stone Project. I. Radial and Vertical Distributions of DCN and DCO⁺. Astronomical Journal, 161 (1). Art. No. 38. ISSN 1538-3881. https://resolver.caltech.edu/CaltechAUTHORS:20201224-085806513

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Abstract

Molecular D/H ratios are frequently used to probe the chemical past of solar system volatiles. Yet it is unclear which parts of the solar nebula hosted an active deuterium fractionation chemistry. To address this question, we present 0farcs2–0farcs4 Atacama Large Millimeter/submillimeter Array (ALMA) observations of DCO⁺ and DCN 2–1, 3–2, and 4–3 toward the nearby protoplanetary disk around TW Hya, taken as part of the TW Hya Rosetta Stone project, augmented with archival data. DCO⁺ is characterized by an excitation temperature of ~40 K across the 70 au radius pebble disk, indicative of emission from a warm, elevated molecular layer. Tentatively, DCN is present at even higher temperatures. Both DCO⁺ and DCN present substantial emission cavities in the inner disk, while in the outer disk the DCO⁺ and DCN morphologies diverge: most DCN emission originates from a narrow ring peaking around 30 au, with some additional diffuse DCN emission present at larger radii, while DCO⁺ is present in a broad structured ring that extends past the pebble disk. Based on a set of simple parametric disk abundance models, these emission patterns can be explained by a near-constant DCN abundance exterior to the cavity, and an increasing DCO⁺ abundance with radius. In conclusion, the ALMA observations reveal an active deuterium fractionation chemistry in multiple disk regions around TW Hya, but not in the cold planetesimal-forming midplane and in the inner disk. More observations are needed to explore whether deuterium fractionation is actually absent in these latter regions, and if its absence is a common feature or something peculiar to the old TW Hya disk.


Item Type:Article
Related URLs:
URLURL TypeDescription
https://doi.org/10.3847/1538-3881/abc74dDOIArticle
https://arxiv.org/abs/2011.06774arXivDiscussion Paper
ORCID:
AuthorORCID
Öberg, Karin I.0000-0001-8798-1347
Cleeves, L. Ilsedore0000-0003-2076-8001
Bergner, Jennifer B.0000-0002-8716-0482
Teague, Richard0000-0003-1534-5186
Huang, Jane0000-0001-6947-6072
Loomis, Ryan A.0000-0002-8932-1219
Bergin, Edwin A.0000-0003-4179-6394
Blake, Geoffrey A.0000-0003-0787-1610
Calahan, Jenny0000-0002-0150-0125
Cazzoletti, Paolo0000-0002-1917-7370
Guzmán, Viviana Veloso0000-0003-4784-3040
Hogerheijde, Michiel R.0000-0001-5217-537X
Kama, Mihkel0000-0003-0065-7267
Terwisscha van Scheltinga, Jeroen0000-0002-3800-9639
Qi, Chunhua0000-0001-8642-1786
van Dishoeck, Ewine F.0000-0001-7591-1907
Walsh, Catherine0000-0001-6078-786X
Wilner, David J.0000-0003-1526-7587
Alternate Title:TW Hya Rosetta Stone Project. I. Radial and Vertical Distributions of DCN and DCO+, The TW Hya Rosetta Stone Project I: Radial and vertical distributions of DCN and DCO+
Additional Information:© 2020. The American Astronomical Society. Received 2020 July 31; revised 2020 October 11; accepted 2020 November 2; published 2020 December 22. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2016.1.00311.S and ADS/JAO.ALMA#2016.1.00440.S. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), MOST and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. This work is supported by the National Radio Astronomy Observatory (NRAO). NRAO is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This work was supported by an award from the Simons Foundation (SCOL # 321183, KÖ). K.I.Ö. also gratefully acknowledges support from the David and Lucille Packard Foundation. L.I.C. gratefully acknowledges support from the David and Lucille Packard Foundation and the Johnson & Johnson WISTEM2D Award. J.B.B. acknowledges support from NASA through the NASA Hubble Fellowship grant #HST-HF2-51429.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-26555. J.T.v.S. and M.R.H. are supported by the Dutch Astrochemistry II program of the Netherlands Organization for Scientific Research (648.000.025). J.H. acknowledges that support for this work was provided by NASA through the NASA Hubble Fellowship grant #HST-HF2-51460.001-A awarded by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS5-26555. C.W acknowledges financial support from the University of Leeds and from the Science and Technology Facilities Council (grant Nos. ST/R000549/1 and ST/T000287/1). J.K.C. acknowledges support from the National Science Foundation Graduate Research Fellowship under Grant No. DGE 1256260 and the National Aeronautics and Space Administration FINESST grant, under Grant No. 80NSSC19K1534. Facility: ALMA - Atacama Large Millimeter Array. Software: CASA (McMullin et al. 2007), Astropy (Astropy Collaboration et al. 2013, 2018), RADMC-3D (Dullemond 2012).
Funders:
Funding AgencyGrant Number
National Radio Astronomy ObservatoryUNSPECIFIED
Simons Foundation321183
David and Lucile Packard FoundationUNSPECIFIED
Johnson & JohnsonWISTEM2D
NASA Hubble FellowshipHST-HF2-51429.001-A
NASANAS5-26555
Nederlandse Organisatie voor Wetenschappelijk Onderzoek (NWO)648.000.025
NASA Hubble FellowshipHST-HF2-51460.001-A
University of LeedsUNSPECIFIED
Science and Technology Facilities Council (STFC)ST/R000549/1
Science and Technology Facilities Council (STFC)ST/T000287/1
NSF Graduate Research FellowshipDGE-1256260
NASA80NSSC19K1534
Subject Keywords:Planet formation ; Protoplanetary disks ; Millimeter astronomy ; Astrochemistry ; Submillimeter astronomy ; Interstellar molecules ; Solar system formation
Issue or Number:1
Classification Code:Unified Astronomy Thesaurus concepts: Planet formation (1241); Protoplanetary disks (1300); Millimeter astronomy (1061); Astrochemistry (75); Submillimeter astronomy (1647); Interstellar molecules (849); Solar system formation (1530)
Record Number:CaltechAUTHORS:20201224-085806513
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20201224-085806513
Official Citation:Karin I. Öberg et al 2021 AJ 161 38
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:107271
Collection:CaltechAUTHORS
Deposited By: George Porter
Deposited On:04 Jan 2021 16:38
Last Modified:04 Jan 2021 16:42

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