Observational Constraints on The Evolution of Dust in ...

164 From Protoplanetary Disks to Planetary Systems
ID Oli/Pyr a % Ens % For % Sil % Oli/Pyr a % Sil %
(1.5 µm) (1.5 µm) (1.5 µm) (1.5 µm) (6.0 µm) (6.0 µm)
PBB2002 J161420.2 67.7 +7.9
−7.8 0.6 +0.9
−0.0 0.8 +1.2
−0.0 0.0 +0.4
−0.0 15.2 +2.8
−1.5 7.9 +1.3
−1.3
PZ99 J160357.6 6.1 +9.2
−0.0 3.8 +2.9
−0.0 0.2 +2.2
−0.0 0.0 +2.6
−0.0 87.1 +19.9
−46.7 0.0 +5.1
−0.0
PZ99 J161411.0 8.8 +4.7
−0.0 3.9 +3.5
−0.0 0.0 +1.4
−0.0 0.0 +4.1
−0.0 84.8 +8.6
−55.2 0.0 +3.0
−0.0
ScoPMS31 72.4 +39.8
−61.0 4.6 +10.7
−3.7 0.0 +9.0
−1.9 1.9 +9.2
−1.4 6.6 +4.2
−6.2 0.0 +1.5
−0.0
η Chamaeleontis
J0843 44.6 +19.9
−21.9 5.9 +7.6
−0.0 0.0 +10.2
−0.0 1.6 +11.6
−0.0 13.6 +19.2
−0.0 0.0 +3.9
−0.0
RECX-5 12.3 +15.6
−3.5 23.9 +13.9
−0.0 0.0 +8.0
−0.0 8.0 +6.9
−3.3 7.1 +18.9
−0.0 0.0 +10.0
−0.0
RECX-9 31.6 +15.8
−24.2 0.9 +7.0
−0.0 5.4 +5.8
−3.2 4.6 +10.8
−2.1 3.3 +3.0
−1.1 0.8 +8.3
−0.0
RECX-11 26.8 +15.7
−14.4 8.0 +10.5
−0.0 0.0 +2.7
−0.0 3.4 +3.7
−1.9 17.6 +8.1
−6.6 0.0 +1.9
−0.0
Table A.2 – Intermediate and large dust composition derived using the “B2C” procedure. b
a Amorphous olivine and pyroxene combined.
b For each object, the first line corresponds to the warm component abundances,
while the second line corresponds to the cold component abundances, when
available.