TY - JOUR
T1 - Probing protoplanetary disk evolution in the Chamaeleon II region
AU - Villenave, M.
AU - Ménard, F.
AU - Dent, W. R.F.
AU - Benisty, M.
AU - Van Der Plas, G.
AU - Williams, J. P.
AU - Ansdell, M.
AU - Ribas, A
AU - Caceres, C.
AU - Canovas, H.
AU - Cieza, L.
AU - Hales, A.
AU - Kamp, I.
AU - Pinte, C.
AU - Principe, D. A.
AU - Schreiber, M. R.
N1 - Funding Information:
cA knolw edgements. The authors thank the referee for their constructive report and useful suggestions that have significantly improved the paper. We also thank P. Galli for sharing the membership tables for the Chamaeleon sources and S. van Terwisga for interesting discussions. This paper makes use of the following ALMA data: ADS/JAO.ALMA#2013.1.00708.S. ALMA is a partnership of ESO (representing its member states), NSF (USA), and NINS (Japan), together with NRC (Canada), NSC 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. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc. M.V., F.M., M.B., and G.vd.P. acknowledge funding from ANR of France under contract number ANR-16-CE31-0013 (Planet Forming Disks). M.V. research was supported by an appointment to the NASA Postdoctoral Program at the NASA Jet Propulsion Laboratory, administered by Universities Space Research Association under contract with NASA. C.C. acknowledges support from DGI-UNAB project DI-11-19/R and ANID – Millennium Science Initiative Program – NCN19_171. L.C. acknowledges support from ANID FONDECYT grant 1211656. C.P. acknowledges funding from the Australian Research Council via FT170100040 and DP180104235. J.P.W. acknowledges support from NSF grant AST-1907486.
Publisher Copyright:
© M. Villenave et al. 2021.
Copyright:
Copyright 2021 Elsevier B.V., All rights reserved.
PY - 2021/9/1
Y1 - 2021/9/1
N2 - Context. Characterizing the evolution of protoplanetary disks is necessary to improve our understanding of planet formation. Constraints on both dust and gas are needed to determine the dominant disk dissipation mechanisms. Aims. We aim to compare the disk dust masses in the Chamaeleon II (Cha II) star-forming region with other regions with ages between 1 and 10 Myr. Methods. We use ALMA band 6 observations (1.3 mm) to survey 29 protoplanetary disks in Cha II. Dust mass estimates are derived from the continuum data. Results. Out of our initial sample of 29 disks, we detect 22 sources in the continuum, 10 in 12CO, 3 in 13CO, and none in C18O (J = 2-1). Additionally, we detect two companion candidates in the continuum and 12CO emission. Most disk dust masses are lower than 10 M⊕ , assuming thermal emission from optically thin dust. Including non-detections, we derive a median dust mass of 4.5 ± 1.5 M⊕ from survival analysis. We compare consistent estimations of the distributions of the disk dust mass and the disk-to-stellar mass ratios in Cha II with six other low mass and isolated star-forming regions in the age range of 1-10 Myr: Upper Sco, CrA, IC 348, Cha I, Lupus, and Taurus. When comparing the dust-to-stellar mass ratio, we find that the masses of disks in Cha II are statistically different from those in Upper Sco and Taurus, and we confirm that disks in Upper Sco, the oldest region of the sample, are statistically less massive than in all other regions. Performing a second statistical test of the dust mass distributions from similar mass bins, we find no statistical differences between these regions and Cha II. Conclusions. We interpret these trends, most simply, as a sign of decline in the disk dust masses with time or dust evolution. Different global initial conditions in star-forming regions may also play a role, but their impact on the properties of a disk population is difficult to isolate in star-forming regions lacking nearby massive stars.
AB - Context. Characterizing the evolution of protoplanetary disks is necessary to improve our understanding of planet formation. Constraints on both dust and gas are needed to determine the dominant disk dissipation mechanisms. Aims. We aim to compare the disk dust masses in the Chamaeleon II (Cha II) star-forming region with other regions with ages between 1 and 10 Myr. Methods. We use ALMA band 6 observations (1.3 mm) to survey 29 protoplanetary disks in Cha II. Dust mass estimates are derived from the continuum data. Results. Out of our initial sample of 29 disks, we detect 22 sources in the continuum, 10 in 12CO, 3 in 13CO, and none in C18O (J = 2-1). Additionally, we detect two companion candidates in the continuum and 12CO emission. Most disk dust masses are lower than 10 M⊕ , assuming thermal emission from optically thin dust. Including non-detections, we derive a median dust mass of 4.5 ± 1.5 M⊕ from survival analysis. We compare consistent estimations of the distributions of the disk dust mass and the disk-to-stellar mass ratios in Cha II with six other low mass and isolated star-forming regions in the age range of 1-10 Myr: Upper Sco, CrA, IC 348, Cha I, Lupus, and Taurus. When comparing the dust-to-stellar mass ratio, we find that the masses of disks in Cha II are statistically different from those in Upper Sco and Taurus, and we confirm that disks in Upper Sco, the oldest region of the sample, are statistically less massive than in all other regions. Performing a second statistical test of the dust mass distributions from similar mass bins, we find no statistical differences between these regions and Cha II. Conclusions. We interpret these trends, most simply, as a sign of decline in the disk dust masses with time or dust evolution. Different global initial conditions in star-forming regions may also play a role, but their impact on the properties of a disk population is difficult to isolate in star-forming regions lacking nearby massive stars.
KW - Circumstellar matter
KW - Protoplanetary disks
KW - Stars: formation
KW - Stars: variables: T Tauri, Herbig Ae/Be
UR - http://www.scopus.com/inward/record.url?scp=85114555171&partnerID=8YFLogxK
U2 - 10.1051/0004-6361/202140496
DO - 10.1051/0004-6361/202140496
M3 - Article
AN - SCOPUS:85114555171
VL - 653
JO - Astronomy & Astrophysics
JF - Astronomy & Astrophysics
SN - 0004-6361
M1 - A46
ER -