Observations of edge-on protoplanetary disks with ALMA I. Results from continuum data

被引:126
|
作者
Villenave, M. [1 ,2 ]
Menard, F. [1 ]
Dent, W. R. F. [3 ]
Duchene, G. [1 ,4 ]
Stapelfeldt, K. R. [5 ]
Benisty, M. [1 ,6 ]
Boehler, Y. [1 ]
van der Plas, G. [1 ]
Pinte, C. [1 ,7 ,8 ]
Telkamp, Z. [4 ]
Wolff, S. [9 ]
Flores, C. [10 ]
Lesur, G. [1 ]
Louvet, F. [11 ]
Riols, A. [1 ]
Dougados, C. [1 ]
Williams, H. [4 ,12 ]
Padgett, D. [5 ]
机构
[1] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France
[2] European Southern Observ, Alonso Cordova 3107,Casilla 19001, Santiago 19, Chile
[3] Joint ALMA Observ, Alonso de Cordova 3107, Santiago 7630355, Chile
[4] Univ Calif Berkeley, Astron Dept, Berkeley, CA 94720 USA
[5] CALTECH, Jet Prop Lab, 4800 Oak Grove Dr, Pasadena, CA 91109 USA
[6] Univ Chile, Dept Astron, CNRS, Unidad Mixta Int Francochilena Astron,UMI 3386, Camino Observ 1515, Santiago, Chile
[7] Monash Univ, Monash Ctr Astrophys MoCA, Clayton, Vic 3800, Australia
[8] Monash Univ, Sch Phys & Astron, Clayton, Vic 3800, Australia
[9] Leiden Univ, Leiden Observ, NL-2300 RA Leiden, Netherlands
[10] Univ Hawaii, Inst Astron, 640 N Aohoku Pl, Hilo, HI 96720 USA
[11] Univ Paris Diderot, CEA Saclay, CNRS, AIM Paris Saclay,Dept Astrophys,CEA, F-91191 Gif Sur Yvette, France
[12] Univ Minnesota, Sch Phys & Astron, 116 Church St SE, Minneapolis, MN 55455 USA
基金
澳大利亚研究理事会;
关键词
protoplanetary disks; stars: formation; circumstellar matter; stars: variables: T Tauri; Herbig Ae/Be; CIRCUMSTELLAR DISK; RADIATIVE-TRANSFER; TAURUS-AURIGA; DUST; STAR; POPULATION; SIMULATIONS; ENVELOPES; OPACITY; SYSTEMS;
D O I
10.1051/0004-6361/202038087
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Aims. We aim to study vertical settling and radial drift of dust in protoplanetary disks from a different perspective: an edge-on view. An estimation of the amplitude of settling and drift is highly relevant to understanding planet formation. Methods. We analyze a sample of 12 HST-selected edge-on protoplanetary disks (i.e., seen with high inclinations) for which the vertical extent of the emission layers can be constrained directly. We present ALMA high angular resolution continuum images (similar to 0.1 '') of these disks at two wavelengths, 0.89 and 2.06 mm (respectively ALMA bands 7 and 4), supplemented with archival band 6 data (1.33 mm) where available. Results. Several sources show constant brightness profiles along their major axis with a steep drop at the outer edges. Two disks have central holes with additional compact continuum emission at the location of the central star. For most sources, the millimeter continuum emission is more compact than the scattered light, both in the vertical and radial directions. Six sources are resolved along their minor axis in at least one millimetric band, providing direct information on the vertical distribution of the millimeter grains. For the second largest disk of the sample, Tau 042021, the significant difference in vertical extent between band 7 and band 4 suggests efficient size-selective vertical settling of large grains. Furthermore, the only Class I object in our sample shows evidence of flaring in the millimeter. Along the major axis, all disks are well resolved. Four of them are larger in band 7 than in band 4 in the radial direction, and three have a similar radial extent in all bands. These three disks are also the ones with the sharpest apparent edges (between 80% and 20% of the peak flux, Delta r/r similar to 0.3), and two of them are binaries. For all disks, we also derive the millimeter brightness temperature and spectral index maps. We find that all edge-on disks in our sample are likely optically thick and that the dust emission reveals low brightness temperatures in most cases (brightness temperatures <= 10 K). The integrated spectral indices are similar to those of disks at lower inclination. Conclusions. The comparison of a generic radiative transfer disk model with our data shows that at least three disks are consistent with a small millimeter dust scale height, of a few au (measured at r = 100 au). This is in contrast with the more classical value of h(g) similar to 10 au derived from scattered light images and from gas line measurements. These results confirm, by direct observations, that large (millimeter) grains are subject to significant vertical settling in protoplanetary disks.
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页数:22
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