2019A&A...625A.118K


C.D.S. - SIMBAD4 rel 1.7 - 2020.01.22CET11:34:32

2019A&A...625A.118K - Astronomy and Astrophysics, volume 625A, 118-118 (2019/5-1)

Highly structured disk around the planet host PDS 70 revealed by high-angular resolution observations with ALMA.

KEPPLER M., TEAGUE R., BAE J., BENISTY M., HENNING T., VAN BOEKEL R., CHAPILLON E., PINILLA P., WILLIAMS J.P., BERTRANG G.H.-M., FACCHINI S., FLOCK M., GINSKI C., JUHASZ A., KLAHR H., LIU Y., MULLER A., PEREZ L.M., POHL A., ROSOTTI G., SAMLAND M. and SEMENOV D.

Abstract (from CDS):


Context. Imaged in the gap of a transition disk and found at a separation of about 195mas (∼22au) from its host star at a position angle of about 155°, PDS 70 b is the most robustly detected young planet to date. This system is therefore a unique laboratory for characterizing the properties of young planetary systems at the stage of their formation.
Aims. We aim to trace direct and indirect imprints of PDS 70 b on the gas and dust emission of the circumstellar disk in order to study the properties of this ∼5Myr young planetary system.
Methods. We obtained ALMA band 7 observations of PDS 70 in dust continuum and 12CO (3-2) and combined them with archival data. This resulted in an unprecedented angular resolution of about 70mas (∼8au).
Results. We derive an upper limit on circumplanetary material at the location of PDS 70 b of ∼0.01M and find a highly structured circumstellar disk in both dust and gas. The outer dust ring peaks at 0.65'' (74au) and reveals a possible second unresolved peak at about 0.53'' (60au). The integrated intensity of CO also shows evidence of a depletion of emission at ∼0.2'' (23au) with a width of ∼0.1'' (11au). The gas kinematics show evidence of a deviation from Keplerian rotation inside ≤0.8'' (91au). This implies a pressure gradient that can account for the location of the dust ring well beyond the location of PDS 70 b. Farther in, we detect an inner disk that appears to be connected to the outer disk by a possible bridge feature in the northwest region in both gas and dust. We compare the observations to hydrodynamical simulations that include a planet with different masses that cover the estimated mass range that was previously derived from near-infrared photometry (∼5-9MJup). We find that even a planet with a mass of 10MJup may not be sufficient to explain the extent of the wide gap, and an additional low-mass companion may be needed to account for the observed disk morphology.

Abstract Copyright: © M. Keppler et al. 2019

Journal keyword(s): stars: individual: PDS 70 - techniques: interferometric - hydrodynamics - planet-disk interactions - protoplanetary disks

Simbad objects: 11

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Number of rows : 11

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 EM* LkCa 15 TT* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 534 1
2 HD 36112 Ae* 05 30 27.5286772598 +25 19 57.082162439   8.57 8.27     A8Ve 334 0
3 V* TW Hya TT* 11 01 51.9054298616 -34 42 17.031550898   11.94 10.50 10.626 9.18 K6Ve 1471 1
4 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 627 1
5 QSO B1334-127 QSO 13 37 39.78277768 -12 57 24.6932620   18.5 18.5 16.22   ~ 418 1
6 PDS 70b Pl? 14 08 10.1545137760 -41 23 52.576649494           ~ 25 0
7 V* V1032 Cen TT* 14 08 10.1545137760 -41 23 52.576649494     12.199   10.506 K7IVe 80 0
8 QSO B1424-41 QSO 14 27 56.29756536 -42 06 19.4375991   18.48 17.7 16.30   ~ 331 1
9 QSO B1514-24 BLL 15 17 41.8135246339 -24 22 19.482167214   15.13 14.00 13.95   ~ 628 3
10 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 751 0
11 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 313 2

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2020.01.22-11:34:32

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