2010A&A...524L...1B


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.17CET15:07:43

2010A&A...524L...1B - Astronomy and Astrophysics, volume 524, L1-1 (2010/12-1)

Dissecting the Moth: discovery of an off-centered ring in the HD 61005 debris disk with high-resolution imaging.

BUENZLI E., THALMANN C., VIGAN A., BOCCALETTI A., CHAUVIN G., AUGEREAU J.-C., MEYER M.R., MENARD F., DESIDERA S., MESSINA S., HENNING T., CARSON J., MONTAGNIER G., BEUZIT J.L., BONAVITA M., EGGENBERGER A., LAGRANGE A.M., MESA D., MOUILLET D. and QUANZ S.P.

Abstract (from CDS):

The debris disk known as ``The Moth'' is named after its unusually asymmetric surface brightness distribution. It is located around the ∼90Myr old G8V star HD 61005 at 34.5pc and has previously been imaged by the HST at 1.1 and 0.6µm. Polarimetric observations suggested that the circumstellar material consists of two distinct components, a nearly edge-on disk or ring, and a swept-back feature, the result of interaction with the interstellar medium. We resolve both components at unprecedented resolution with VLT/NACO H-band imaging. Using optimized angular differential imaging techniques to remove the light of the star, we reveal the disk component as a distinct narrow ring at inclination i=84.3±1.0°. We determine a semi-major axis of a=61.25±0.85AU and an eccentricity of e=0.045±0.015, assuming that periastron is located along the apparent disk major axis. Therefore, the ring center is offset from the star by at least 2.75±0.85AU. The offset, together with a relatively steep inner rim, could indicate a planetary companion that perturbs the remnant planetesimal belt. From our imaging data we set upper mass limits for companions that exclude any object above the deuterium-burning limit for separations down to 0.3". The ring shows a strong brightness asymmetry along both the major and minor axis. A brighter front side could indicate forward-scattering grains, while the brightness difference between the NE and SW components can be only partly explained by the ring center offset, suggesting additional density enhancements on one side of the ring. The swept-back component appears as two streamers originating near the NE and SW edges of the debris ring.

Abstract Copyright:

Journal keyword(s): techniques: high angular resolution - circumstellar matter - protoplanetary disks - stars: individual: HD 61005

Simbad objects: 10

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Number of rows : 10

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 15115 PM* 02 26 16.2457708887 +06 17 33.187984874   7.15 6.80   6.33 F4IV 143 0
2 EM* LkCa 15 TT* 04 39 17.7912813350 +22 21 03.387667491   13.01 12.03 11.61   K5:Ve 525 1
3 HD 32297 * 05 02 27.4357771761 +07 27 39.682335894   8.32 8.14     A0V 138 0
4 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1602 1
5 HD 61005 PM* 07 35 47.4624262763 -32 12 14.042600581   8.96 8.22     G8Vk 161 0
6 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 454 2
7 GSC 07188-00571 * 10 24 28.4387527499 -32 20 45.148332606   14.97 14.17 14.16   ~ 1 0
8 * alf PsA b Pl 22 57 39.04625 -29 37 20.0533           ~ 176 1
9 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1101 3
10 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 859 1

    Equat.    Gal    SGal    Ecl

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2019.11.17-15:07:43

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