2019MNRAS.483.3278C


C.D.S. - SIMBAD4 rel 1.7 - 2020.10.29CET22:09:15

2019MNRAS.483.3278C - Mon. Not. R. Astron. Soc., 483, 3278-3287 (2019/March-1)

Cm-wavelength observations of MWC 758: resolved dust trapping in a vortex.

CASASSUS S., MARINO S., LYRA W., BARUTEAU C., VIDAL M., WOOTTEN A., PEREZ S., ALARCON F., BARRAZA M., CARCAMO M., DONG R., SIERRA A., ZHU Z., RICCI L., CHRISTIAENS V. and CIEZA L.

Abstract (from CDS):

The large crescents imaged by ALMA in transition discs suggest that azimuthal dust trapping concentrates the larger grains, but centimetre-wavelengths continuum observations are required to map the distribution of the largest observable grains. A previous detection at ∼1 cm of an unresolved clump along the outer ring of MWC 758 (Clump 1), and buried inside more extended sub-mm continuum, motivates followup VLA observations. Deep multiconfiguration integrations reveal the morphology of Clump 1 and additional cm-wave components that we characterize via comparison with a deconvolution of recent 342 GHz data (∼1 mm). Clump 1, which concentrates ∼1/3 of the whole disc flux density at ∼1 cm, is resolved as a narrow arc with a deprojected aspect ratio χ > 5.6, and with half the azimuthal width than at 342 GHz. The spectral trends in the morphology of Clump 1 are quantitatively consistent with the Lyra-Lin prescriptions for dust trapping in an anticyclonic vortex, provided with porous grains (f ∼ 0.2 ± 0.2) in a very elongated (χ ∼ 14 ± 3) and cold (T∼23±2K) vortex. The same prescriptions constrain the turbulence parameter α and the gas surface density Σg through log10(α×Σg/_g cm_–2) ∼-2.3±0.4, thus requiring values for Σg larger than a factor of a few compared to that reported in the literature from the CO isotopologues, if α <= 10–3. Such physical conditions imply an appreciably optically thick continuum even at cm-wavelengths (τ_33 GHz_∼0.2). A secondary and shallower peak at 342 GHz is about twice fainter relative to Clump 1 at 33 GHz. Clump 2 appears to be less efficient at trapping large grains.

Abstract Copyright: © 2018 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society

Journal keyword(s): accretion, accretion discs - planet-disc interactions - protoplanetary discs

Status at CDS : Examining the need for a new acronym.

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 3C 48 QSO 01 37 41.2995845985 +33 09 35.079126038   16.62 16.20     ~ 2526 2
2 EM* LkHA 330 TT* 03 45 48.2804487421 +32 24 11.851014679   12.30 10.97     F7 121 0
3 V* HL Tau Or* 04 31 38.471952 +18 13 58.08504   15.89 14.49 14.39   K5 1223 0
4 EM* LkCa 15 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 560 1
5 V* V1366 Ori Ae* 05 16 00.4764811920 -09 48 35.394685295 10.19 10.16 9.84 9.77 9.63 B9.5V 165 0
6 ICRF J052109.8+163822 Sy1 05 21 09.88592749 +16 38 22.0517668   19.37 18.84 18.480   ~ 757 1
7 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 364 0
8 NVSS J055932+235354 Rad 05 59 32.03313165 +23 53 53.9267683           ~ 41 1
9 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 361 1
10 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 480 1
11 EM* SR 21A TT* 16 27 10.2776332501 -24 19 12.620553212   16.08 14.10     G1 234 1
12 IRAS 16245-2423 TT* 16 27 37.1911764648 -24 30 35.031583716       16.66 14.67 B5-F2 237 0
13 Haro 1-16 Or* 16 31 33.4638378966 -24 27 37.158295501   14.02 12.80     K3e 178 0
14 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 342 2

    Equat.    Gal    SGal    Ecl

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2020.10.29-22:09:15

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