The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones
Mid-infrared spectroscopy of protoplanetary disks provides a chemical inventory of gas within a few astronomical unit, where planets are readily detected around older stars. With the James Webb Space Telescope (JWST) Disk Infrared Spectral Chemistry Survey, we explore demographic trends among 31 dis...
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2025-01-01
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| author | Nicole Arulanantham Colette Salyk Klaus Pontoppidan Andrea Banzatti Ke Zhang Karin Öberg Feng Long John Carr Joan Najita Ilaria Pascucci María José Colmenares Chengyan Xie Jane Huang Joel Green Sean M. Andrews Geoffrey A. Blake Edwin A. Bergin Paola Pinilla Miguel Vioque Emma Dahl Eshan Raul Sebastiaan Krijt The JDISCS Collaboration |
| author_facet | Nicole Arulanantham Colette Salyk Klaus Pontoppidan Andrea Banzatti Ke Zhang Karin Öberg Feng Long John Carr Joan Najita Ilaria Pascucci María José Colmenares Chengyan Xie Jane Huang Joel Green Sean M. Andrews Geoffrey A. Blake Edwin A. Bergin Paola Pinilla Miguel Vioque Emma Dahl Eshan Raul Sebastiaan Krijt The JDISCS Collaboration |
| author_sort | Nicole Arulanantham |
| collection | DOAJ |
| description | Mid-infrared spectroscopy of protoplanetary disks provides a chemical inventory of gas within a few astronomical unit, where planets are readily detected around older stars. With the James Webb Space Telescope (JWST) Disk Infrared Spectral Chemistry Survey, we explore demographic trends among 31 disks observed with MIRI (MRS) and with previous Atacama Large Millimeter/submillimeter Array millimeter continuum imaging at high angular resolution (5–10 au). With these signal-to-noise ratio of ∼200–450 spectra, we report emission from H _2 O, OH, CO, C _2 H _2 , HCN, CO _2 , [Ne ii ], [Ne iii ], and [Ar ii ]. Emission from H _2 O, OH, and CO is nearly ubiquitous for low-mass stars, and detection rates of all molecules are higher than for similar disks observed with Spitzer-IRS. Slab model fits to the molecular emission lines demonstrate that emission from C _2 H _2 , HCN, and possibly CO _2 is optically thin; thus since column densities and emitting radii are degenerate, observations are actually sensitive to the total molecular mass. C _2 H _2 and HCN emission also typically originate in a hotter region ( $92{0}_{-130}^{+70}$ , $82{0}_{-130}^{+70}$ K, respectively) than CO _2 ( $60{0}_{-160}^{+200}$ K). The HCN to cold H _2 O luminosity ratios are generally smaller in smooth disks, consistent with more efficient water delivery via icy pebbles in the absence of large dust substructures. The molecular emission-line luminosities are also correlated with mass accretion rates and infrared spectral indices, similar to trends reported from Spitzer - IRS surveys. This work demonstrates the power of combining multiwavelength observations to explore inner disk chemistry as a function of outer disk and stellar properties, which will continue to grow as the sample of observed Class II systems expands in the coming JWST observation cycles. |
| format | Article |
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| institution | Kabale University |
| issn | 1538-3881 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-e27517cf7a7b4c0ea4cdb9ea7151e1f02025-08-20T03:30:20ZengIOP PublishingThe Astronomical Journal1538-38812025-01-0117026710.3847/1538-3881/addd01The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk ZonesNicole Arulanantham0https://orcid.org/0000-0003-2631-5265Colette Salyk1https://orcid.org/0000-0003-3682-6632Klaus Pontoppidan2https://orcid.org/0000-0001-7552-1562Andrea Banzatti3https://orcid.org/0000-0003-4335-0900Ke Zhang4https://orcid.org/0000-0002-0661-7517Karin Öberg5https://orcid.org/0000-0001-8798-1347Feng Long6https://orcid.org/0000-0002-7607-719XJohn Carr7https://orcid.org/0000-0002-6695-3977Joan Najita8https://orcid.org/0000-0002-5758-150XIlaria Pascucci9https://orcid.org/0000-0001-7962-1683María José Colmenares10https://orcid.org/0000-0002-5296-6232Chengyan Xie11https://orcid.org/0000-0001-8184-5547Jane Huang12https://orcid.org/0000-0001-6947-6072Joel Green13https://orcid.org/0000-0003-1665-5709Sean M. Andrews14https://orcid.org/0000-0003-2253-2270Geoffrey A. Blake15https://orcid.org/0000-0003-0787-1610Edwin A. Bergin16https://orcid.org/0000-0003-4179-6394Paola Pinilla17https://orcid.org/0000-0001-8764-1780Miguel Vioque18https://orcid.org/0000-0002-4147-3846Emma Dahl19https://orcid.org/0000-0003-2985-1514Eshan Raul20https://orcid.org/0009-0002-2380-6683Sebastiaan Krijt21https://orcid.org/0000-0002-3291-6887The JDISCS CollaborationAstrophysics & Space Institute , Schmidt Sciences, New York, NY 10011, USAVassar College , 124 Raymond Avenue, Poughkeepsie, NY 12604, USAJet Propulsion Laboratory, California Institute of Technology , 4800 Oak Grove Drive, Pasadena, CA 91109, USADepartment of Physics, Texas State University , 749 N Comanche Street, San Marcos, TX 78666, USADepartment of Astronomy, University of Wisconsin-Madison , Madison, WI 53706, USACenter for Astrophysics—Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USALunar and Planetary Laboratory, University of Arizona , Tucson, AZ 85721, USADepartment of Astronomy, University of Maryland , College Park, MD 20742, USANSF’s NOIRLab , 950 N. Cherry Avenue, Tucson, AZ 85719, USADepartment of Planetary Sciences, University of Arizona , 1629 East University Boulevard, Tucson, AZ 85721, USADepartment of Astronomy, University of Michigan , 1085 S. University, Ann Arbor, MI 48109, USALunar and Planetary Laboratory, University of Arizona , Tucson, AZ 85721, USADepartment of Astronomy, Columbia University , 538 W. 120th Street, Pupin Hall, New York, NY 10027, USASpace Telescope Science Institute , 3700 San Martin Drive, Baltimore, MD 21218, USACenter for Astrophysics—Harvard & Smithsonian , 60 Garden Street, Cambridge, MA 02138, USADivision of Geological and Planetary Sciences, California Institute of Technology , MC 150-21, Pasadena, CA 91125, USADepartment of Astronomy, University of Michigan , 1085 S. University, Ann Arbor, MI 48109, USAMullard Space Science Laboratory, University College London , Holmbury St Mary, Dorking, Surrey RH5 6NT, UKEuropean Southern Observatory , Karl-Schwarzschild-Str. 2, 85748 Garching bei München, GermanyDivision of Geological and Planetary Sciences, California Institute of Technology , MC 150-21, Pasadena, CA 91125, USADepartment of Astronomy, University of Wisconsin-Madison , Madison, WI 53706, USADepartment of Physics and Astronomy, University of Exeter , Exeter, EX4 4QL, UKMid-infrared spectroscopy of protoplanetary disks provides a chemical inventory of gas within a few astronomical unit, where planets are readily detected around older stars. With the James Webb Space Telescope (JWST) Disk Infrared Spectral Chemistry Survey, we explore demographic trends among 31 disks observed with MIRI (MRS) and with previous Atacama Large Millimeter/submillimeter Array millimeter continuum imaging at high angular resolution (5–10 au). With these signal-to-noise ratio of ∼200–450 spectra, we report emission from H _2 O, OH, CO, C _2 H _2 , HCN, CO _2 , [Ne ii ], [Ne iii ], and [Ar ii ]. Emission from H _2 O, OH, and CO is nearly ubiquitous for low-mass stars, and detection rates of all molecules are higher than for similar disks observed with Spitzer-IRS. Slab model fits to the molecular emission lines demonstrate that emission from C _2 H _2 , HCN, and possibly CO _2 is optically thin; thus since column densities and emitting radii are degenerate, observations are actually sensitive to the total molecular mass. C _2 H _2 and HCN emission also typically originate in a hotter region ( $92{0}_{-130}^{+70}$ , $82{0}_{-130}^{+70}$ K, respectively) than CO _2 ( $60{0}_{-160}^{+200}$ K). The HCN to cold H _2 O luminosity ratios are generally smaller in smooth disks, consistent with more efficient water delivery via icy pebbles in the absence of large dust substructures. The molecular emission-line luminosities are also correlated with mass accretion rates and infrared spectral indices, similar to trends reported from Spitzer - IRS surveys. This work demonstrates the power of combining multiwavelength observations to explore inner disk chemistry as a function of outer disk and stellar properties, which will continue to grow as the sample of observed Class II systems expands in the coming JWST observation cycles.https://doi.org/10.3847/1538-3881/addd01Planetary system formationProtoplanetary disksJames Webb Space TelescopeInfrared spectroscopySmall molecules |
| spellingShingle | Nicole Arulanantham Colette Salyk Klaus Pontoppidan Andrea Banzatti Ke Zhang Karin Öberg Feng Long John Carr Joan Najita Ilaria Pascucci María José Colmenares Chengyan Xie Jane Huang Joel Green Sean M. Andrews Geoffrey A. Blake Edwin A. Bergin Paola Pinilla Miguel Vioque Emma Dahl Eshan Raul Sebastiaan Krijt The JDISCS Collaboration The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones The Astronomical Journal Planetary system formation Protoplanetary disks James Webb Space Telescope Infrared spectroscopy Small molecules |
| title | The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones |
| title_full | The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones |
| title_fullStr | The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones |
| title_full_unstemmed | The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones |
| title_short | The JDISC Survey: Linking the Physics and Chemistry of Inner and Outer Protoplanetary Disk Zones |
| title_sort | jdisc survey linking the physics and chemistry of inner and outer protoplanetary disk zones |
| topic | Planetary system formation Protoplanetary disks James Webb Space Telescope Infrared spectroscopy Small molecules |
| url | https://doi.org/10.3847/1538-3881/addd01 |
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