2017A&A...598A..43C


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST04:07:08

2017A&A...598A..43C - Astronomy and Astrophysics, volume 598A, 43-43 (2017/2-1)

Constraining the mass of the planet(s) sculpting a disk cavity The intriguing case of 2MASS J16042165-2130284.

CANOVAS H., HARDY A., ZURLO A., WAHHAJ Z., SCHREIBER M.R., VIGAN A., VILLAVER E., OLOFSSON J., MEEUS G., MENARD F., CACERES C., CIEZA L.A. and GARUFI A.

Abstract (from CDS):

Context. The large cavities observed in the dust and gas distributions of transition disks may be explained by planet-disk interactions. At ∼145pc, 2MASS J16042165-2130284 (J1604) is a 5-12Myr old transitional disk with different gap sizes in the mm- and µm-sized dust distributions (outer edges at ∼79 and at ∼63au, respectively). Its 12CO emission shows a ∼30au cavity. This radial structure suggests that giant planets are sculpting this disk.
Aims. We aim to constrain the masses and locations of plausible giant planets around J1604.
Methods. We observed J1604 with the Spectro-Polarimetric High-contrast Exoplanet REsearch (SPHERE) at the Very Large Telescope (VLT), in IRDIFS_EXT, pupil-stabilized mode, obtaining YJH-band images with the integral field spectrograph (IFS) and K1K2-band images with the Infra-Red Dual-beam Imager and Spectrograph (IRDIS). The dataset was processed exploiting the angular differential imaging (ADI) technique with high-contrast algorithms.
Results. Our observations reach a contrast of ΔK,ΔYH ∼12mag from 0".15 to 0".80 (∼22 to 115au), but no planet candidate is detected. The disk is directly imaged in scattered light at all bands from Y to K, and it shows a red color. This indicates that the dust particles in the disk surface are mainly ≥0.3µm-sized grains. We confirm the sharp dip/decrement in scattered light in agreement with polarized light observations. Comparing our images with a radiative transfer model we argue that the southern side of the disk is most likely the nearest.
Conclusions. This work represents the deepest search yet for companions around J1604. We reach a mass sensitivity of ≥2-3MJup from ∼22 to ∼115au according to a hot start scenario. We propose that a brown dwarf orbiting inside of ∼15au and additional Jovian planets at larger radii could account for the observed properties of J1604 while explaining our lack of detection.

Abstract Copyright: © ESO, 2017

Journal keyword(s): protoplanetary disks - planet-disk interactions - stars: variables: T Tauri, Herbig Ae/Be - techniques: high angular resolution - stars: individual: 2MASS J16042165-2130284

VizieR on-line data: <Available at CDS (J/A+A/598/A43): list.dat fits/*>

Simbad objects: 8

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Number of rows : 8

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 Or* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 552 1
2 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 651 1
3 CPD-36 6759 Y*O 15 15 48.4459023859 -37 09 16.026315179   9.21 8.708     F8V 357 1
4 HD 142527 Ae* 15 56 41.8888096574 -42 19 23.245384377   9.04 8.34     F6III 467 1
5 RX J160421-21307 TT* 16 04 20.9770687478 -21 30 41.699585480   16.6     11.99 M2 21 0
6 2MASS J16042165-2130284 pr* 16 04 21.6546714640 -21 30 28.549578725   13.3       K2 91 0
7 NAME Upper Sco Association As* 16 12 -23.4           ~ 1021 1
8 HD 169142 Ae* 18 24 29.7799676975 -29 46 49.328597698   8.42 8.16     F1VekA3mA3_lB? 335 2

    Equat.    Gal    SGal    Ecl

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2020.07.08-04:07:08

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