The ALMA Survey of Gas Evolution of PROtoplanetary Disks (AGE-PRO). II. Dust and Gas Disk Properties in the Ophiuchus Star-forming Region
Dary Ruíz-Rodríguez, Camilo González-Ruilova, Lucas A. Cieza, Ke Zhang, Leon Trapman, Anibal Sierra, Paola Pinilla, Ilaria Pascucci, Laura M. Pérez, Dingshan Deng, Carolina Agurto-Gangas, John M. Carpenter, Benoît Tabone, Giovanni Rosotti, Rossella Anania, James Miley, Kamber R. Schwarz, Aleksandra Kuznetsova, Miguel Vioque, N. T. Kurtovic
Abstract
Abstract The ALMA survey of Gas Evolution in PROtoplanetary disks (AGE-PRO) Large Program aims to trace the evolution of gas disk mass and size throughout the lifetime of protoplanetary disks by using the Atacama Large Millimeter/submillimeter Array (ALMA). This paper presents Band-6 ALMA observations of 10 embedded (Class I and Flat Spectrum) sources in the Ophiuchus molecular cloud, with spectral types ranging from M3 to K6 stars, which serve as the evolutionary starting point in the AGE-PRO sample. While we find four nearly edge-on disks (≥70°), and three highly inclined disks (≥60 ° ) in our sample, we show that, as a population, embedded disks in Ophiuchus are not significantly contaminated by more-evolved, but highly inclined sources. We derived dust disk masses from the Band-6 continuum and estimated gas disk masses from the C 18 O J = 2−1 and C 17 O J = 2−1 lines. The mass estimates from the C 17 O line are slightly higher, suggesting C 18 O emission might be partially optically thick. While the 12 CO and 13 CO lines are severely contaminated by extended emission and self-absorption, the C 18 O and C 17 O lines are allowed to trace the radial extent of the gaseous disks. From these measurements, we found that the C 18 O J = 2−1 and C 17 O J = 2−1 fluxes correlate well with each other and with the continuum fluxes. Furthermore, the C 18 O and C 17 O lines present a larger radial extension than disk dust sizes by factors ranging from ∼1.5 to ∼2.5, as is found for Class II disks using the radial extension of the 12 CO. In addition, we have detected outflows in three disks from 12 CO observations.