2019A&A...621A...7W


Query : 2019A&A...621A...7W

2019A&A...621A...7W - Astronomy and Astrophysics, volume 621A, 7-7 (2019/1-1)

Imaging the disc rim and a moving close-in companion candidate in the pre-transitional disc of V1247 Orionis.

WILLSON M., KRAUS S., KLUSKA J., MONNIER J.D., CURE M., SITKO M., AARNIO A., IRELAND M.J., RIZZUTO A., HONE E., KREPLIN A., ANDREWS S., CALVET N., ESPAILLAT C., FUKAGAWA M., HARRIES T.J., HINKLEY S., KANAAN S., MUTO T. and WILNER D.J.

Abstract (from CDS):


Context. V1247 Orionis harbours a pre-transitional disc with a partially cleared gap. Earlier interferometric and polarimetric observations revealed strong asymmetries both in the gap region and in the outer disc. The presence of a companion was inferred to explain these asymmetric structures and the ongoing disc clearing.
Aims. Using an extensive set of multi-wavelength and multi-epoch observations we aimed to identify the origin of the previously detected asymmetries.
Methods. We have observed V1247 Ori at three epochs spanning ∼678 days using sparse aperture masking interferometry with Keck/NIRC2 and VLT/NACO. In addition, we search for signs of accretion through VLT/SPHERE-ZIMPOL spectral differential imaging in Hα and R-band continuum. Our SMA sub-millimetre interferometry in 880 µm continuum and in the CO(3-2) line allows us to constrain the orientation and direction of rotation of the outer disc.
Results. We find the L'-band emission to be dominated by static features which trace forward-scattered dust emission from the inner edge of the outer disc located to the north-east. In H- and K-bands, we see evidence for a companion candidate that moved systematically by 45° within the first ∼345 days. The separation of the companion candidate is not well constrained, but the observed position angle change is consistent with Keplerian motion of a body located on a 6au orbit. From the SMA CO moment map, the location of the disc rim, and the detected orbital motion, we deduced the three-dimensional orientation of the disc. We see no indication of accretion in Hα and set upper limits for an accreting companion.
Conclusions. The measured contrast of the companion candidate in H and K is consistent with an actively accreting protoplanet. Hence, we identify V1247 Ori as a unique laboratory for studying companion-disc interactions and disc clearing.

Abstract Copyright: © ESO 2018

Journal keyword(s): planets and satellites: detection - planets and satellites: formation - protoplanetary disks - stars: pre-main sequence - infrared: planetary systems - stars: individual: V1247 Orionis

Simbad objects: 25

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Number of rows : 25
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024
#notes
1 3C 84 Sy2 03 19 48.1599902040 +41 30 42.108850836   13.10 12.48 11.09   ~ 4017 3
2 EM* LkHA 330 TT* 03 45 48.2805122064 +32 24 11.850978276   12.30 10.97     F7 142 0
3 V* FP Tau Or* 04 14 47.3033083488 +26 46 26.414391720 17.21 16.14 15.02     M4Ve 170 0
4 V* DM Tau Or* 04 33 48.7336763736 +18 10 09.973460280 14.30 14.82 14.00     M2Ve 635 0
5 EM* LkCa 15b Pl 04 39 17.7911622816 +22 21 03.390090984           ~ 87 1
6 QSO B0529+075 QSO 05 32 38.9985483000 +07 32 43.344156480   19.0 19.00 17.50   ~ 225 1
7 HD 36696 * 05 33 30.6601153104 -03 06 34.240326984   9.30 8.30     K0/1III 14 0
8 Ass Ori OB 1b As* 05 34.0 -01 30           ~ 266 0
9 HD 36811 SB* 05 34 09.7403451960 -01 54 06.662865492 7.37 7.26 7.08 6.95 6.85 A0V 50 0
10 HD 290679 * 05 35 36.3894356856 -01 34 32.716032132   11.25 10.13     K2 5 0
11 HD 290685 * 05 36 28.0764666048 -01 45 15.522226200   10.58 9.46     K0 4 0
12 HD 37295 * 05 37 23.3923836497 -02 05 01.185008607   8.45 8.14     F0IV/V 8 0
13 HD 37331 * 05 37 50.2544039952 +00 19 02.320621860   8.10 7.82     A9V 19 0
14 V* V1247 Ori dS* 05 38 05.2519466880 -01 15 21.698856468   10.18 9.82     F0V 115 0
15 HD 290735 * 05 39 14.4591356856 -00 25 09.348027816   11.860 10.564     K7 8 0
16 HD 37634 PM* 05 39 44.2525498644 -05 03 02.588808148   9.53 8.89     G5V 43 0
17 HD 38406 PM* 05 45 28.7949099456 -01 36 54.405700308   8.82 8.19     G1/2V 30 0
18 QSO B0605-0834 BLL 06 07 59.69924014 -08 34 49.9783246     17.60 17.70   ~ 461 1
19 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1898 1
20 NAME TW Hya b Pl? 11 01 51.9053285064 -34 42 17.033218380           ~ 9 1
21 Ass Cha T 1-20 Or* 11 08 39.0261275112 -77 16 04.163889324   18.44 16.28 15.822 13.17 K5Ve 88 0
22 V* T Cha Or* 11 57 13.5245085552 -79 21 31.530508884   10.00 11.86     K0e 272 1
23 3C 279 Bla 12 56 11.16657958 -05 47 21.5251510   18.01 17.75 15.87   ~ 3057 2
24 HD 142527b Pl? 15 56 41.8882637904 -42 19 23.248281828           ~ 27 0
25 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 643 1

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