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J/A+A/610/A24           AS 209 ALMA image                        (Fedele+, 2018)

ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet. Fedele D., Tazzari M., Booth R., Testi L., Clarke C.J., Pascucci I., Kospal A., Semenov D., Bruderer S., Henning T., Teague R. <Astron. Astrophys. 610, A24 (2018)> =2018A&A...610A..24F (SIMBAD/NED BibCode)
ADC_Keywords: YSOs ; Exoplanets ; Radio continuum Keywords: protoplanetary disks - planet-disk interactions Abstract: This paper presents new high angular resolution ALMA 1.3mm dust continuum observations of the protoplanetary system AS 209 in the Ophiuchus star forming region. The dust continuum emission is characterized by a main central core and two prominent rings at r=75au and r=130au intervaled by two gaps at at r=62au and r=103au. The two gaps have different widths and depths, with the inner one being narrower and shallower. We determined the surface density of the millimeter dust grains using the 3D radiative transfer disk code dali. According to our fiducial model the inner gap is partially filled with millimeter grains while the outer gap is largely devoid of dust. The inferred surface density is compared to 3D hydrodynamical simulations (FARGO-3D) of planet-disk interaction. The outer dust gap is consistent with the presence of a giant planet (Mplanet∼0.8MSaturn); the planet is responsible for the gap opening and for the pile-up of dust at the outer edge of the planet orbit. The simulations also show that the same planet could be the origin of the inner gap at r=62au. The relative position of the two dust gaps is close to the 2:1 resonance and we have investigated the possibility of a second planet inside the inner gap. The resulting surface density (including location, width and depth of the two dust gaps) are in agreement with the observations. The properties of the inner gap pose a strong constraint to the mass of the inner planet (Mplanet<0.1MJ). In both scenarios (single or pair of planets), the hydrodynamical simulations suggest a very low disk viscosity (α<10-4). Given the young age of the system (0.5-1Myr), this result implies that the formation of giant planets occurs on a timescale of ≲1Myr. Description: The ALMA observations of AS 209 (J2000: RA=16:49:15.296, DE=-14:22:09.02) have been performed on 2016 September 22 (with 38 antennas) and 26 (41 antennas) in band 6 (211-275GHz) as part of the project ID 2015.1.00486.S (PI: D. Fedele). The correlator setup includes a broad (2GHz bandwidth) spectral window centered at 230GHz. Objects: --------------------------------------------------- RA (2000) DE Designation(s) --------------------------------------------------- 16 49 15.30 -14 22 08.6 AS 209 = V* V1121 Oph --------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file list.dat 127 1 Information on fits image fits/* 0 1 Fits image
Byte-by-byte Description of file: list.dat
Bytes Format Units Label Explanations
1- 9 F9.5 deg RAdeg Right Ascension of center (J2000) 10- 18 F9.5 deg DEdeg Declination of center (J2000) 20- 23 I4 --- Nx Number of pixels along X-axis 25- 28 I4 --- Ny Number of pixels along Y-axis 30- 55 A26 --- Obs.Date Observation date (YYYY-MM-DDThh:mm:ss.ssssss) 57- 63 F7.3 GHz Freq Observed frequency 65- 68 I4 Kibyte size Size of FITS file 70-115 A46 --- FileName Name of FITS file, in subdirectory fits 117-127 A11 --- Title Title of the FITS file
Acknowledgements: Davide Fedele, fedele(at)arcetri.astro.it
(End) Patricia Vannier [CDS] 14-Feb-2018
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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