2019A&A...626A..95P


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.10CEST03:22:24

2019A&A...626A..95P - Astronomy and Astrophysics, volume 626A, 95-95 (2019/6-1)

First resolved observations of a highly asymmetric debris disc around HD 160305 with VLT/SPHERE.

PERROT C., THEBAULT P., LAGRANGE A.-M., BOCCALETTI A., VIGAN A., DESIDERA S., AUGEREAU J.-C., BONNEFOY M., CHOQUET E., KRAL Q., LOH A., MAIRE A.-L., MENARD F., MESSINA S., OLOFSSON J., GRATTON R., BILLER B., BRANDNER W., BUENZLI E., CHAUVIN G., CHEETHAM A., DAEMGEN S., DELORME P., FELDT M., LAGADEC E., LANGLOIS M., LANNIER J., MESA D., MOUILLET D., PERETTI S., JANIN-POTIRON P., SALTER G., SISSA E., ROUX A., LLORED M., BUEY J.-T., PAVLOV A., WEBER L. and PETIT C.

Abstract (from CDS):


Context. Direct imaging of debris discs gives important information about their nature, their global morphology, and allows us to identify specific structures possibly in connection with the presence of gravitational perturbers. It is the most straightforward technique to observe planetary systems as a whole.
Aims. We present the first resolved images of the debris disc around the young F-type star HD 160305, detected in scattered light using the VLT/SPHERE instrument in the near infrared.
Methods. We used a post-processing method based on angular differential imaging and synthetic images of debris discs produced with a disc modelling code (GRaTer) to constrain the main characteristics of the disc around HD 160305. All of the point sources in the field of the IRDIS camera were analysed with an astrometric tool to determine whether they are bound objects or background stars.
Results. We detect a very inclined (∼82°) ring-like debris disc located at a stellocentric distance of about 86au (deprojected width ∼27au). The disc displays a brightness asymmetry between the two sides of the major axis, as can be expected from scattering properties of dust grains. We derive an anisotropic scattering factor g>0.5. A second right-left asymmetry is also observed with respect to the minor axis. We measure a surface brightness ratio of 0.73±0.18 between the bright and the faint sides. Because of the low signal-to-noise ratio (S/N) of the images we cannot easily discriminate between several possible explanations for this left-right asymmetry, such as perturbations by an unseen planet, the aftermath of the breakup of a massive planetesimal, or the pericenter glow effect due to an eccentric ring. Two epochs of observations allow us to reject the companionship hypothesis for the 15 point sources present in the field.

Abstract Copyright: © P. Clément et al. 2019

Journal keyword(s): scattering - stars: individual: HD160305 - methods: observational - techniques: high angular resolution - planet-disk interactions - techniques: image processing

VizieR on-line data: <Available at CDS (J/A+A/626/A95): list.dat fits/*>

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 HD 61005 PM* 07 35 47.4624262763 -32 12 14.042600581   8.96 8.22     G8Vk 171 0
2 NGC 3603 OpC 11 15 18.6 -61 15 26           ~ 942 1
3 HD 106906 * 12 17 53.1914296570 -55 58 31.890430864   8.95 8.89 8.46   F5V 98 0
4 HD 131835 * 14 56 54.4676957121 -35 41 43.659216390   8.05 7.86     A2IV 80 0
5 HD 141569 pr* 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 471 0
6 NAME ASSOC II SCO As* 16 15 -24.2           ~ 1120 1
7 NGC 6380 GlC 17 34 28.00 -39 04 09.0           ~ 97 0
8 HD 160305 Em* 17 41 49.0383861184 -50 43 28.042296041   8.91 8.405   7.736 F8/G0V 27 1
9 GSC 07396-00759 Em* 18 14 22.0738917529 -32 46 10.133784566   14.14 12.78 12.13 10.380 M1Ve 32 0
10 V* AU Mic BY* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 893 0
11 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1115 3

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2020.07.10-03:22:25

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