2016A&A...596L...4W


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.16CEST19:24:24

2016A&A...596L...4W - Astronomy and Astrophysics, volume 596, L4-4 (2016/12-1)

The SHARDDS survey: First resolved image of the HD 114082 debris disk in the Lower Centaurus Crux with SPHERE.

WAHHAJ Z., MILLI J., KENNEDY G., ERTEL S., MATRA L., BOCCALETTI A., DEL BURGO C., WYATT M., PINTE C., LAGRANGE A.-M., ABSIL O., CHOQUET E., GOMEZ GONZALEZ C.A., KOBAYASHI H., MAWET D., MOUILLET D., PUEYO L., DENT W.R.F., AUGEREAU J.-C. and GIRARD J.

Abstract (from CDS):

We present the first resolved image of the debris disk around the 16±8Myr old star, HD 114082. The observation was made in the H-band using the SPHERE instrument. The star is at a distance of 92±6pc in the Lower Centaurus Crux association. Using a Markov chain Monte Carlo analysis, we determined that the debris is likely in the form of a dust ring with an inner edge of 27.7+2.8–3.5au, position angle -74.3°+0.5–1.5, and an inclination with respect to the line of sight of 6.7°+3.8–0.4. The disk imaged in scattered light has a surface density that is declining with radius of ∼r–4, which is steeper than expected for grain blowout by radiation pressure. We find only marginal evidence (2σ) of eccentricity and rule out planets more massive than 1.0MJup orbiting within 1 au of the inner edge of the ring, since such a planet would have disrupted the disk. The disk has roughly the same fractional disk luminosity (Ldisk/L*=3.3x10–3) as HR 4796 A and β Pictoris, however it was not detected by previous instrument facilities most likely because of its small angular size (radius ∼0.4''), low albedo (∼0.2), and low scattering efficiency far from the star due to high scattering anisotropy. With the arrival of extreme adaptive optics systems, such as SPHERE and GPI, the morphology of smaller, fainter, and more distant debris disks are being revealed, providing clues to planet-disk interactions in young protoplanetary systems.

Abstract Copyright: © ESO, 2016

Journal keyword(s): stars: individual: HD 114082 - techniques: high angular resolution - planetary systems

Simbad objects: 21

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Number of rows : 21

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 105 PM* 00 05 52.5449273706 -41 45 11.046016405   8.13 7.53     G0V 149 0
2 HD 377 PM* 00 08 25.7456097412 +06 37 00.488182642   8.22 7.59   6.90 G2V 115 0
3 HD 10472 PM* 01 40 24.0660166953 -60 59 56.623736611   8.01 7.61   7.13 F2IV/V 49 0
4 HD 25457 TT* 04 02 36.7451443573 -00 16 08.118566607   5.88 5.38     F7V 237 0
5 HD 38207 * 05 43 20.9562637826 -20 11 21.439223613   8.83 8.47     F2V 31 0
6 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1655 1
7 HD 69830 PM* 08 18 23.9469692487 -12 37 55.810202572   6.74 5.95     G8:V 464 2
8 NAME TW Hya Association As* 11 01.9 -34 42           ~ 819 0
9 HD 106906 * 12 17 53.1914296570 -55 58 31.890430864   8.95 8.89 8.46   F5V 98 0
10 NAME Lower Centaurus Crux As* 12 19 -57.1           ~ 354 1
11 HD 109573 PM* 12 36 01.0317721349 -39 52 10.222698506   5.786 5.774 7.25 5.81 A0V 551 1
12 HD 114082 * 13 09 16.1923187430 -60 18 30.052893109   8.64 8.21     F3V 54 1
13 NAME beta Pic Moving Group MGr 14 30 -42.0           ~ 557 0
14 HD 141569 pr* 15 49 57.7484743862 -03 55 16.344023102 7.22 7.20 7.12 7.00 7.04 A2VekB9mB9(_lB) 472 0
15 HD 181327 PM* 19 22 58.9434412361 -54 32 16.979671096   7.50 7.04   6.49 F6V 225 0
16 V* AU Mic BY* 20 45 09.5323695486 -31 20 27.241710746   10.05 8.627 9.078 6.593 M1VeBa1 894 0
17 HD 202628 PM* 21 18 27.2693236958 -43 20 04.746121764   7.39 6.742     G5V 141 0
18 HD 206893 PM* 21 45 21.9056012837 -12 47 00.068065895   7.11 6.67     F5V 60 0
19 HD 207129 PM* 21 48 15.7510673466 -47 18 13.020109072   6.18 5.58     G2V 288 0
20 * alf PsA ** 22 57 39.04625 -29 37 20.0533 1.31 1.25 1.16 1.11 1.09 A4V 1116 3
21 HD 218396 El* 23 07 28.7156905667 +21 08 03.302133882   6.21 5.953     F0+VkA5mA5 896 0

    Equat.    Gal    SGal    Ecl

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2020.07.16-19:24:24

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