2013A&A...559A.111H


C.D.S. - SIMBAD4 rel 1.7 - 2019.07.20CEST01:58:00

2013A&A...559A.111H - Astronomy and Astrophysics, volume 559A, 111-111 (2013/11-1)

An interferometric study of the post-AGB binary 89 Herculis. I. Spatially resolving the continuum circumstellar environment at optical and near-IR wavelengths with the VLTI, NPOI, IOTA, PTI, and the CHARA Array.

HILLEN M., VERHOELST T., VAN WINCKEL H., CHESNEAU O., HUMMEL C.A., MONNIER J.D., FARRINGTON C., TYCNER C., MOURARD D., TEN BRUMMELAAR T., BANERJEE D.P.K. and ZAVALA R.T.

Abstract (from CDS):

Binary post-asymptotic giant branch (post-AGB) stars are interesting laboratories to study both the evolution of binaries as well as the structure of circumstellar disks. A multiwavelength high angular resolution study of the prototypical object 89Herculis is performed with the aim of identifying and locating the different emission components seen in the spectral energy distribution. A large interferometric data set, collected over the past decade and covering optical and near-infrared wavelengths, is analyzed in combination with the spectral energy distribution and flux-calibrated optical spectra. In this first paper only simple geometric models are applied to fit the interferometric data. Combining the interferometric constraints with the photometry and the optical spectra, we re-assess the energy budget of the post-AGB star and its circumstellar environment. We report the first (direct) detection of a large (35-40%) optical circumstellar flux contribution and spatially resolve its emission region. Given this large amount of reprocessed and/or redistributed optical light, the fitted size of the emission region is rather compact and fits with(in) the inner rim of the circumbinary dust disk. This rim dominates our K band data through thermal emission and is rather compact, emitting significantly already at a radius of twice the orbital separation. We interpret the circumstellar optical flux as due to a scattering process, with the scatterers located in the extremely puffed-up inner rim of the disk and possibly also in a bipolar outflow seen pole-on. A non-local thermodynamic equilibrium gaseous origin in an inner disk cannot be excluded but is considered highly unlikely. This direct detection of a significant amount of circumbinary light at optical wavelengths poses several significant questions regarding our understanding of both post-AGB binaries and the physics in their circumbinary disks. Although the identification of the source of emission/scattering remains inconclusive without further study on this and similar objects, the implications are manifold.

Abstract Copyright:

Journal keyword(s): stars: AGB and post-AGB - circumstellar matter - binaries: general - techniques: interferometric - scattering - ISM: jets and outflows

VizieR on-line data: <Available at CDS (J/A+A/559/A111): list.dat fits/*>

Simbad objects: 22

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Number of rows : 22

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2019
#notes
1 BD+46 442 * 01 45 47.0309135946 +46 49 00.940007737   10.02 9.46     F2III 15 0
2 V* AB Aur Ae* 04 55 45.8459978418 +30 33 04.293281305 7.20 7.16 7.05 6.96 6.70 A0Ve 892 2
3 NAME LMC G 05 23 34.6 -69 45 22     0.4     ~ 14185 1
4 HD 44179 pA* 06 19 58.2185496 -10 38 14.706068 9.51 9.33 9.02     B9Ib/II 699 0
5 HD 89353 pA* 10 18 07.5892879413 -28 59 31.194541133   5.76 5.53     B9.5Ib/II 282 0
6 * iot Oph PM* 16 54 00.4715122 +10 09 55.298255 3.98 4.30 4.38     B8V 96 0
7 * 84 Her PM* 17 43 21.5646072179 +24 19 40.157353689   6.394 5.729     G2IIIb 130 0
8 HD 162828 * 17 52 02.5684024789 +24 18 16.062363369   8.27 6.98     K2 6 0
9 * 89 Her pA* 17 55 25.1884459710 +26 02 59.970100296 5.36 5.70 5.36 5.06 4.94 F2Ibp 383 0
10 HD 163296 Ae* 17 56 21.2882188601 -21 57 21.872343282 7.00 6.93 6.85 6.86 6.67 A1Vep 718 0
11 HD 163948 * 17 57 24.3103683187 +33 24 03.008833104 8.380 7.790 6.880     K0 11 0
12 HD 164730 * 18 01 29.3040912555 +24 14 59.821706482   8.23 7.02     K0 7 0
13 HD 165524 * 18 05 30.1367482327 +21 38 47.832235454   7.425 6.179     K3III: 17 0
14 * omi Her Be* 18 07 32.5507266 +28 45 44.967843 3.74 3.802 3.827     B9.5III 140 0
15 * 102 Her * 18 08 45.4914189 +20 48 52.407870 3.38 4.177 4.347     B2IV 173 0
16 * 101 Her * 18 08 52.8635204306 +20 02 42.838708227   5.259 5.099     A8III 40 0
17 * t Her * 18 21 01.0202651422 +28 52 11.821053982   5.322 5.115     A8Vn 44 0
18 HD 169981 SB* 18 25 58.7870959144 +29 49 44.146965856 5.99 5.90 5.83 5.75 5.71 A2IV 65 0
19 * ups Sgr Be* 19 21 43.6228354 -15 57 18.062473 4.18 4.71 4.61 4.34 4.21 F2p 281 0
20 * iot Cyg PM* 19 29 42.3587204 +51 43 47.205830   3.899 3.755     A5V 122 0
21 * tet Cyg PM* 19 36 26.5343563 +50 13 15.964573 4.83 4.86 4.48 4.13 3.92 F3+V 319 1
22 V* QY Sge LP* 20 07 54.6188178294 +18 42 54.520818409   12.57       G0Ie 47 0

    Equat.    Gal    SGal    Ecl

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2019.07.20-01:58:00

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