The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). III. Dust and Gas Disk Properties in the Lupus Star-forming Region
We present Band 6 and Band 7 observations of 10 Lupus disks around M3-K6 stars from the Atacama Large Millimeter/submillimeter Array survey of Gas Evolution in PROtoplanetary disks (AGE-PRO) Large Program. In addition to continuum emission in both bands, our Band 6 setup covers the ^12 CO, ^13 CO, a...
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2025-01-01
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| author | Dingshan Deng Miguel Vioque Ilaria Pascucci Laura M. Pérez Ke Zhang Nicolás Kurtovic Leon Trapman Estephani E. TorresVillanueva Carolina Agurto-Gangas John Carpenter Paola Pinilla Uma Gorti Benoît Tabone Anibal Sierra Giovanni P. Rosotti Lucas A. Cieza Rossella Anania Camilo González-Ruilova Michiel R. Hogerheijde James Miley Dary A. Ruiz-Rodriguez Maxime Ruaud Kamber Schwarz |
| author_facet | Dingshan Deng Miguel Vioque Ilaria Pascucci Laura M. Pérez Ke Zhang Nicolás Kurtovic Leon Trapman Estephani E. TorresVillanueva Carolina Agurto-Gangas John Carpenter Paola Pinilla Uma Gorti Benoît Tabone Anibal Sierra Giovanni P. Rosotti Lucas A. Cieza Rossella Anania Camilo González-Ruilova Michiel R. Hogerheijde James Miley Dary A. Ruiz-Rodriguez Maxime Ruaud Kamber Schwarz |
| author_sort | Dingshan Deng |
| collection | DOAJ |
| description | We present Band 6 and Band 7 observations of 10 Lupus disks around M3-K6 stars from the Atacama Large Millimeter/submillimeter Array survey of Gas Evolution in PROtoplanetary disks (AGE-PRO) Large Program. In addition to continuum emission in both bands, our Band 6 setup covers the ^12 CO, ^13 CO, and C ^18 O J = 2–1 lines, while our Band 7 setup covers the N _2 H ^+ J = 3–2 line. All of our sources are detected in ^12 CO and ^13 CO; seven out of ten are detected in C ^18 O; and three are detected in N _2 H ^+ . We find strong correlations between the CO isotopologue line fluxes and the continuum flux densities. With the exception of one disk, we also identify a strong correlation between the C ^18 O J = 2–1 and N _2 H ^+ J = 3–2 fluxes, indicating similar CO abundances across this sample. For the two sources with well-resolved continuum and ^12 CO J = 2–1 images, we find that their gas-to-dust size ratio is consistent with the median value of ∼2 inferred from a larger sample of Lupus disks. We derive dust disk masses from continuum flux densities. We estimate gas disk masses by comparing C ^18 O J = 2–1 line fluxes with those predicted by the limited grid of self-consistent disk models of M. Ruaud et al. A comparison of these mass estimates with those derived by L. Trapman et al., using a combination of CO isotopologue and N _2 H ^+ line emission, shows that the masses are consistent with each other. Some discrepancies appear for small and faint disks, but they are still within the uncertainties. Both methods find gas disk masses increase with dust disk masses, and gas-to-dust mass ratios are between 10 and 100 in the AGE-PRO Lupus sample. |
| format | Article |
| id | doaj-art-f6c77cd6680a4f0daed0fe1cab217ccd |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
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| spelling | doaj-art-f6c77cd6680a4f0daed0fe1cab217ccd2025-08-20T03:39:19ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-019891310.3847/1538-4357/add43aThe ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). III. Dust and Gas Disk Properties in the Lupus Star-forming RegionDingshan Deng0https://orcid.org/0000-0003-0777-7392Miguel Vioque1https://orcid.org/0000-0002-4147-3846Ilaria Pascucci2https://orcid.org/0000-0001-7962-1683Laura M. Pérez3https://orcid.org/0000-0002-1199-9564Ke Zhang4https://orcid.org/0000-0002-0661-7517Nicolás Kurtovic5https://orcid.org/0000-0002-2358-4796Leon Trapman6https://orcid.org/0000-0002-8623-9703Estephani E. TorresVillanueva7https://orcid.org/0000-0001-9961-8203Carolina Agurto-Gangas8https://orcid.org/0000-0002-7238-2306John Carpenter9https://orcid.org/0000-0003-2251-0602Paola Pinilla10https://orcid.org/0000-0001-8764-1780Uma Gorti11https://orcid.org/0000-0002-3311-5918Benoît Tabone12https://orcid.org/0000-0002-1103-3225Anibal Sierra13https://orcid.org/0000-0002-5991-8073Giovanni P. Rosotti14https://orcid.org/0000-0003-4853-5736Lucas A. Cieza15https://orcid.org/0000-0002-2828-1153Rossella Anania16https://orcid.org/0009-0004-8091-5055Camilo González-Ruilova17https://orcid.org/0000-0003-4907-189XMichiel R. Hogerheijde18https://orcid.org/0000-0001-5217-537XJames Miley19https://orcid.org/0000-0002-1575-680XDary A. Ruiz-Rodriguez20https://orcid.org/0000-0003-3573-8163Maxime Ruaud21https://orcid.org/0000-0003-0522-5789Kamber Schwarz22https://orcid.org/0000-0002-6429-9457Lunar and Planetary Laboratory, the University of Arizona , Tucson, AZ 85721, USA ; dingshandeng@arizona.eduEuropean Southern Observatory , Karl-Schwarzschild-Str. 2, 85748 Garching bei München, Germany; Joint ALMA Observatory , Alonso de Córdova 3107, Vitacura, Santiago 763-0355, ChileLunar and Planetary Laboratory, the University of Arizona , Tucson, AZ 85721, USA ; dingshandeng@arizona.eduDepartamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, ChileDepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USAMax-Planck-Institut für Extraterrestrische Physik , Giessenbachstrasse 1, D-85748 Garching, Germany; Max-Planck-Institut für Astronomie (MPIA) , Konigstuhl 17, 69117 Heidelberg, GermanyDepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USADepartment of Astronomy, University of Wisconsin-Madison , 475 N Charter Street, Madison, WI 53706, USADepartamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, ChileInstituto de Estudios Astrofísicos, Universidad Diego Portales , Av. Ejercito 441, Santiago, Chile; Millennium Nucleus on Young Exoplanets and their Moons (YEMS) , Chile; Center for Interdisciplinary Research in Astrophysics and Space Exploration (CIRAS), Universidad de Santiago de Chile , ChileMullard Space Science Laboratory, University College London , Holmbury St Mary, Dorking, Surrey RH5 6NT, UKNASA Ames Research Center , Moffett Field, CA 94035, USA; Carl Sagan Center , SETI Institute, Mountain View, CA 94043, USAUniversité Paris-Saclay , CNRS, Institut d'Astrophysique Spatiale, 91405, Orsay, FranceDepartamento de Astronomía, Universidad de Chile , Camino El Observatorio 1515, Las Condes, Santiago, Chile; Mullard Space Science Laboratory, University College London , Holmbury St Mary, Dorking, Surrey RH5 6NT, UKDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, I-20133 Milano, ItalyInstituto de Estudios Astrofísicos, Universidad Diego Portales , Av. Ejercito 441, Santiago, Chile; Millennium Nucleus on Young Exoplanets and their Moons (YEMS) , ChileDipartimento di Fisica, Università degli Studi di Milano , Via Celoria 16, I-20133 Milano, ItalyInstituto de Estudios Astrofísicos, Universidad Diego Portales , Av. Ejercito 441, Santiago, Chile; Millennium Nucleus on Young Exoplanets and their Moons (YEMS) , Chile; Center for Interdisciplinary Research in Astrophysics and Space Exploration (CIRAS), Universidad de Santiago de Chile , ChileLeiden Observatory, Leiden University , PO Box 9513, 2300 RA Leiden, The Netherlands; Anton Pannekoek Institute for Astronomy, University of Amsterdam , The NetherlandsMillennium Nucleus on Young Exoplanets and their Moons (YEMS) , Chile; Center for Interdisciplinary Research in Astrophysics and Space Exploration (CIRAS), Universidad de Santiago de Chile , Chile; Departamento de Física, Universidad de Santiago de Chile , Av. Victor Jara 3659, Santiago, ChileNational Radio Astronomy Observatory , 520 Edgemont Road, Charlottesville, VA 22903, USA; Joint ALMA Observatory , Avenida Alonso de Córdova 3107, Vitacura, Santiago, ChileCarl Sagan Center , SETI Institute, Mountain View, CA 94043, USAMax-Planck-Institut für Astronomie (MPIA) , Konigstuhl 17, 69117 Heidelberg, GermanyWe present Band 6 and Band 7 observations of 10 Lupus disks around M3-K6 stars from the Atacama Large Millimeter/submillimeter Array survey of Gas Evolution in PROtoplanetary disks (AGE-PRO) Large Program. In addition to continuum emission in both bands, our Band 6 setup covers the ^12 CO, ^13 CO, and C ^18 O J = 2–1 lines, while our Band 7 setup covers the N _2 H ^+ J = 3–2 line. All of our sources are detected in ^12 CO and ^13 CO; seven out of ten are detected in C ^18 O; and three are detected in N _2 H ^+ . We find strong correlations between the CO isotopologue line fluxes and the continuum flux densities. With the exception of one disk, we also identify a strong correlation between the C ^18 O J = 2–1 and N _2 H ^+ J = 3–2 fluxes, indicating similar CO abundances across this sample. For the two sources with well-resolved continuum and ^12 CO J = 2–1 images, we find that their gas-to-dust size ratio is consistent with the median value of ∼2 inferred from a larger sample of Lupus disks. We derive dust disk masses from continuum flux densities. We estimate gas disk masses by comparing C ^18 O J = 2–1 line fluxes with those predicted by the limited grid of self-consistent disk models of M. Ruaud et al. A comparison of these mass estimates with those derived by L. Trapman et al., using a combination of CO isotopologue and N _2 H ^+ line emission, shows that the masses are consistent with each other. Some discrepancies appear for small and faint disks, but they are still within the uncertainties. Both methods find gas disk masses increase with dust disk masses, and gas-to-dust mass ratios are between 10 and 100 in the AGE-PRO Lupus sample.https://doi.org/10.3847/1538-4357/add43aProtoplanetary disksAstrochemistryPlanet formationMillimeter astronomySubmillimeter astronomy |
| spellingShingle | Dingshan Deng Miguel Vioque Ilaria Pascucci Laura M. Pérez Ke Zhang Nicolás Kurtovic Leon Trapman Estephani E. TorresVillanueva Carolina Agurto-Gangas John Carpenter Paola Pinilla Uma Gorti Benoît Tabone Anibal Sierra Giovanni P. Rosotti Lucas A. Cieza Rossella Anania Camilo González-Ruilova Michiel R. Hogerheijde James Miley Dary A. Ruiz-Rodriguez Maxime Ruaud Kamber Schwarz The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). III. Dust and Gas Disk Properties in the Lupus Star-forming Region The Astrophysical Journal Protoplanetary disks Astrochemistry Planet formation Millimeter astronomy Submillimeter astronomy |
| title | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). III. Dust and Gas Disk Properties in the Lupus Star-forming Region |
| title_full | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). III. Dust and Gas Disk Properties in the Lupus Star-forming Region |
| title_fullStr | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). III. Dust and Gas Disk Properties in the Lupus Star-forming Region |
| title_full_unstemmed | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). III. Dust and Gas Disk Properties in the Lupus Star-forming Region |
| title_short | The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). III. Dust and Gas Disk Properties in the Lupus Star-forming Region |
| title_sort | alma survey of gas evolution of protoplanetary disks age pro iii dust and gas disk properties in the lupus star forming region |
| topic | Protoplanetary disks Astrochemistry Planet formation Millimeter astronomy Submillimeter astronomy |
| url | https://doi.org/10.3847/1538-4357/add43a |
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