2016A&A...595A...9W


Query : 2016A&A...595A...9W

2016A&A...595A...9W - Astronomy and Astrophysics, volume 595A, 9-9 (2016/11-1)

Sparse aperture masking interferometry survey of transitional discs. Search for substellar-mass companions and asymmetries in their parent discs.

WILLSON M., KRAUS S., KLUSKA J., MONNIER J.D., IRELAND M., AARNIO A., SITKO M.L., CALVET N., ESPAILLAT C. and WILNER D.J.

Abstract (from CDS):

Context. Transitional discs are a class of circumstellar discs around young stars with extensive clearing of dusty material within their inner regions on 10s of au scales. One of the primary candidates for this kind of clearing is the formation of planet(s) within the disc that then accrete or clear their immediate area as they migrate through the disc.
Aims. The goal of this survey was to search for asymmetries in the brightness distribution around a selection of transitional disc targets. We then aimed to determine whether these asymmetries trace dynamically-induced structures in the disc or the gap-opening planets themselves.
Methods. Our sample included eight transitional discs. Using the Keck/NIRC2 instrument we utilised the Sparse Aperture Masking (SAM) interferometry technique to search for asymmetries indicative of ongoing planet formation. We searched for close-in companions using both model fitting and interferometric image reconstruction techniques. Using simulated data, we derived diagnostics that helped us to distinguish between point sources and extended asymmetric disc emission. In addition, we investigated the degeneracy between the contrast and separation that appear for marginally resolved companions.
Results. We found FP Tau to contain a previously unseen disc wall, and DM Tau, LkHα330, and TW Hya to contain an asymmetric signal indicative of point source-like emission. We placed upper limits on the contrast of a companion in RXJ 1842.9-3532 and V2246 Oph. We ruled the asymmetry signal in RXJ 1615.3-3255 and V2062 Oph to be false positives. In the cases where our data indicated a potential companion we computed estimates for the value of McMc and found values in the range of 10–5-10–3M2J/yr.
Conclusions. We found significant asymmetries in four targets. Of these, three were consistent with companions. We resolved a previously unseen gap in the disc of FP Tau extending inwards from approximately 10au.

Abstract Copyright: © ESO, 2016

Journal keyword(s): protoplanetary disks - planets and satellites: formation - planets and satellites: detection - techniques: interferometric - stars: pre-main sequence

Simbad objects: 34

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Number of rows : 34
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2023
#notes
1 HD 22781 PM* 03 40 49.5243423552 +31 49 34.652692848   9.628 8.766 8.45   K0 45 1
2 EM* LkHA 330 TT* 03 45 48.2805122064 +32 24 11.850978276   12.30 10.97     F7 135 0
3 HD 23849 PM* 03 49 25.3403965248 +28 38 09.891799872       8.0   G5 17 0
4 HD 281309 * 03 53 35.5284238632 +30 46 24.406357836   9.77 9.17     G0 21 0
5 HD 283420 * 04 10 35.8731543672 +25 21 45.049724028 9.540 9.580 9.140     F8 21 0
6 HD 283477 * 04 14 47.0174078040 +26 28 15.078143424   10.37 9.84     F8 12 0
7 V* FP Tau Or* 04 14 47.3033083488 +26 46 26.414391720 17.21 16.14 15.02     M4Ve 160 0
8 V* DM Tau Or* 04 33 48.7336763736 +18 10 09.973460280 14.30 14.82 14.00     M2Ve 596 0
9 EM* LkCa 15 Or* 04 39 17.7911622816 +22 21 03.390090984   13.01 12.03 11.61   K5:Ve 634 1
10 HD 285938 * 04 39 22.7035612944 +19 07 06.758466960   10.15 9.58     G0 10 0
11 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 4099 0
12 HD 94542 PM* 10 54 16.9756556328 -34 57 49.956539112   9.16 8.58     G0/1V 18 0
13 HD 95105 * 10 58 17.5718841336 -37 09 05.094065520   10.07 9.10     K1IV 13 0
14 V* TW Hya TT* 11 01 51.9053285064 -34 42 17.033218380   11.94 10.50 10.626 9.18 K6Ve 1791 1
15 Ass Cha T 1-20 Or* 11 08 39.0261275112 -77 16 04.163889324   18.44 16.28 15.822 13.17 K5Ve 81 0
16 HD 97507 PM* 11 12 54.0496506360 -34 24 24.283154448   9.21 8.59     G3V 38 0
17 V* T Cha Or* 11 57 13.5245085552 -79 21 31.530508884   10.00 11.86     K0e 261 1
18 HD 142527 Ae* 15 56 41.8882637904 -42 19 23.248281828   9.04 8.34     F6III 584 1
19 WRAY 15-1443 TT* 16 15 20.2341630672 -32 55 05.097631872 13.88 13.22 12.00 11.21 10.50 K5 85 0
20 HD 146369 * 16 17 47.5563563160 -42 20 08.758404636   10.88 9.72     G(6/8p) 6 0
21 HD 146569 * 16 18 05.4709303584 -31 39 06.288546888   8.36 8.25     A0V 28 0
22 HD 146593 * 16 18 20.3587751112 -32 57 35.958653136   8.67 8.26     F3V 21 0
23 HD 147681 PM* 16 24 12.9292086720 -23 30 01.418973264   9.35 8.82 8.5   G1V 28 0
24 HD 147742 * 16 24 25.1036870592 -22 39 17.534566908   8.49 8.00     F6V 27 0
25 Haro 1-6 Or* 16 26 03.0276684144 -24 23 36.188140848   14.15 14.01 12.38 10.80 K0 213 2
26 HD 148212 PM* 16 27 31.3998635208 -25 09 02.212620768   10.28 9.65     G2V 20 0
27 HD 148352 Y*O 16 28 25.1695251528 -24 45 01.016932824   7.89 7.55     F2V 49 0
28 HD 148562 TT* 16 29 54.5953266552 -24 58 46.075015272 8.08 7.99 7.81     A2V 61 0
29 Haro 1-16 Or* 16 31 33.4634997336 -24 27 37.158728076   14.02 12.80     K3e 210 0
30 HD 148806 * 16 31 45.7871542032 -29 38 42.491519448   10.09 9.53     G0V 12 0
31 HD 171450 * 18 36 27.3706537848 -34 42 17.707277988   9.89 9.52     F0V 11 0
32 HD 171574 * 18 37 11.2632646824 -36 03 25.691586048   9.03 8.54     F3IV/V 11 0
33 WRAY 15-1880 TT* 18 42 57.9813628512 -35 32 42.826760736   12.91 11.77     K2 49 0
34 HD 176999 * 19 04 15.3725907936 -35 21 48.844692000   9.86 9.43     F3/5V 12 0

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2023.02.04-10:13:57

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