J/A+A/622/A75 MWC 480 ALMA image (Liu+, 2019)
Ring structure in the MWC 480 disk revealed by ALMA.
Liu Y., Dipierro G., Ragusa E., Lodato G., Herczeg G.J., Long F.,
Harsono D., Boehler Y., Menard F., Johnstone D., Pascucci I., Pinilla P.,
Salyk C., van der Plas G., Cabrit S., Fischer W.J., Hendler N., Manara C.F.,
Nisini B., Rigliaco E., Avenhaus H., Banzatti A., Gully-Santiago M.
<Astron. Astrophys. 622, A75 (2019)>
=2019A&A...622A..75L 2019A&A...622A..75L (SIMBAD/NED BibCode)
ADC_Keywords: Stars, emission ; Stars, radio
Keywords: protoplanetary disks - planet-disk interactions - radiative transfer -
stars: formation - stars: individual: MWC 480
Abstract:
Gap-like structures in protoplanetary disks are likely related to
planet formation processes. In this work, we present and analyze
high-resolution 1.3mm ALMA continuum observations of the
protoplanetary disk around the Herbig Ae star MWC 480. Our
observations show for the first time a gap centered at ∼74AU with a
width of ∼23AU, surrounded by a bright ring centered at ∼98AU from the
central star. Detailed radiative transfer modeling of the ALMA image
and the broadband spectral energy distribution is used to constrain
the surface density profile and structural parameters of the disk. If
the width of the gap corresponds to 4-8 times the Hill radius of a
single forming planet, then the putative planet would have a mass of
0.4∼3MJ. We test this prediction by performing global
three-dimensional smoothed particle hydrodynamic gas/dust simulations
of disks hosting a migrating and accreting planet. We find that the
dust emission across the disk is consistent with the presence of an
embedded planet with a mass of ∼2.3MJ at an orbital radius of ∼78AU.
Given the surface density of the best-fit radiative transfer model,
the amount of depleted mass in the gap is higher than the mass of the
putative planet, which satisfies the basic condition for the formation
of such a planet.
Description:
Continuum ALMA data at 1.3mm (Band 6) of the MWC 480 disk. The data
is a part of the Cycle 4 program (ID: 2016.1.01164.S; PI: G. Herczeg).
The observation was conducted on August 27, 2017, using 47 12m
antennas with baselines ranging from 21 to 3638m. The on-source time
was 4 minutes and the precipitable water vapor (PWV) was 0.5mm during
the integration.
More details as well as the data reduction are described in the paper.
Objects:
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RA (2000) DE Designation(s)
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04 58 46.27 +29 50 37.0 MWC 480 = BD+29 774
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
list.dat 131 1 Information on fits image
fits/* . 1 Fits image
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Byte-by-byte Description of file: list.dat
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Bytes Format Units Label Explanations
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1- 9 F9.5 deg RAdeg Right Ascension of center (J2000)
10- 18 F9.5 deg DEdeg Declination of center (J2000)
20- 22 I3 --- Nx Number of pixels along X-axis
24- 26 I3 --- Ny Number of pixels along Y-axis
28- 50 A23 "datime" Obs.Date Observation date (YYYY-MM-DDThh:mm:ss.sss)
52- 58 F7.3 GHz Obs.Freq Observed frequency
60- 62 I3 Kibyte size Size of FITS file
64- 73 A10 --- FileName Name of FITS file, in subdirectory fits
75-131 A57 --- Title Title of the FITS file
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Acknowledgements:
Yao Liu, yliu(at)mpia.de
(End) Yao Liu [PMO], Patricia Vannier [CDS] 04-Dec-2018