2016A&A...588A..53T


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.17CEST00:55:01

2016A&A...588A..53T - Astronomy and Astrophysics, volume 588A, 53-53 (2016/4-1)

Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks.

TAZZARI M., TESTI L., ERCOLANO B., NATTA A., ISELLA A., CHANDLER C.J., PEREZ L.M., ANDREWS S., WILNER D.J., RICCI L., HENNING T., LINZ H., KWON W., CORDER S.A., DULLEMOND C.P., CARPENTER J.M., SARGENT A.I., MUNDY L., STORM S., CALVET N., GREAVES J.A., LAZIO J. and DELLER A.T.

Abstract (from CDS):

Context. The growth of dust grains from sub-µm to mm and cm sizes is the first step towards the formation of planetesimals. Theoretical models of grain growth predict that dust properties change as a function of disk radius, mass, age, and other physical conditions. High angular resolution observations at several (sub-)mm wavelengths constitute the ideal tool with which to directly probe the bulk of dust grains and to investigate the radial distribution of their properties.
Aims. We lay down the methodology for a multiwavelength analysis of (sub-)mm and cm continuum interferometric observations to self-consistently constrain the disk structure and the radial variation of the dust properties. The computational architecture is massively parallel and highly modular.
Methods. The analysis is based on the simultaneous fit in the uv-plane of observations at several wavelengths with a model for the disk thermal emission and for the dust opacity. The observed flux density at the different wavelengths is fitted by posing constraints on the disk structure and on the radial variation of the grain size distribution.
Results. We apply the analysis to observations of three protoplanetary disks (AS 209, FT tau, DR tau) for which a combination of spatially resolved observations in the range ∼0.88mm to ∼10mm is available from SMA, CARMA, and VLA. In these disks we find evidence of a decrease in the maximum dust grain size, amax, with radius. We derive large amax values up to 1cm in the inner disk 15AU<=R<=30AU and smaller grains with amax∼1mm in the outer disk (R>= 80AU). Our analysis of the AS 209 protoplanetary disk confirms previous literature results showing amax decreasing with radius.
Conclusions. Theoretical studies of planetary formation through grain growth are plagued by the lack of direct information on the radial distribution of the dust grain size. In this paper we develop a multiwavelength analysis that will allow this missing quantity to be constrained for statistically relevant samples of disks and to investigate possible correlations with disk or stellar parameters.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: formation - planetary systems - protoplanetary disks

Simbad objects: 15

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Number of rows : 15

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 3C 84 Sy2 03 19 48.1597607660 +41 30 42.114155434   13.10 12.48 11.09   ~ 3459 3
2 V* CY Tau TT* 04 17 33.7281514373 +28 20 46.809969664 14.52 14.68 13.40 12.59   M1.5 221 0
3 3C 111 Sy1 04 18 21.2773655604 +38 01 35.801523843   19.75 18.05     ~ 839 1
4 V* FT Tau TT* 04 23 39.193 +24 56 14.11       14.37   M2.8 103 0
5 PKS 0428+205 rG 04 31 03.76136151 +20 37 34.2649550   22.174   19.085   ~ 163 1
6 V* HL Tau TT* 04 31 38.437 +18 13 57.65   16.02 15.10 14.21   K5 1122 0
7 QSO J0431+1731 BLL 04 31 57.37922 +17 31 35.7762       21.3   ~ 31 1
8 V* DR Tau TT* 04 47 06.2152696011 +16 58 42.814250257 12.03 11.86 10.50 12.19   K5Ve 462 0
9 QSO B0446+113 BLL 04 49 07.67110088 +11 21 28.5964577     20 18.58   ~ 218 1
10 QSO J0530+13 QSO 05 30 56.41672 +13 31 55.1495     20.0 19.35   ~ 871 1
11 V* CQ Tau Ae* 05 35 58.4671238887 +24 44 54.086375712 11.290 10.780 10.000   8.33 F5IVe 245 0
12 ICRF J054236.1+495107 Sy1 05 42 36.13789843 +49 51 07.2337251   18.45 17.80 17.210   ~ 1230 1
13 3C 273 BLL 12 29 06.6996828061 +02 03 08.598846466   13.05 14.830 14.11   ~ 5241 1
14 DoAr 25 TT* 16 26 23.6911216715 -24 43 13.886717283       12.65   K5 116 0
15 EM* AS 209 TT* 16 49 15.3035547820 -14 22 08.642015783   12.62 11.28     K4Ve 202 0

    Equat.    Gal    SGal    Ecl

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2019.10.17-00:55:01

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