2010A&A...522A..17F


C.D.S. - SIMBAD4 rel 1.7 - 2019.10.19CEST20:54:23

2010A&A...522A..17F - Astronomy and Astrophysics, volume 522, A17-17 (2010/11-1)

Mid-infrared interferometry of massive young stellar objects. II. Evidence for a circumstellar disk surrounding the Kleinmann-Wright object.

FOLLERT R., LINZ H., STECKLUM B., VAN BOEKEL R., HENNING T., FELDT M., HERBST T.M. and LEINERT C.

Abstract (from CDS):

The formation scenario for massive stars is still under discussion. To further constrain current theories, it is vital to spatially resolve the structures from which material accretes onto massive young stellar objects (MYSOs). Due to the small angular extent of MYSOs, one needs to overcome the limitations of conventional thermal infrared imaging, regarding spatial resolution, in order to get observational access to the inner structure of these objects. We employed mid-infrared interferometry, using the MIDI instrument on the ESO/VLTI, to investigate the Kleinmann-Wright Object, a massive young stellar object previously identified as a Herbig Be star precursor. Dispersed visibility curves in the N-band (8-13µm) have been obtained at 5 interferometric baselines. We show that the mid-infrared emission region is resolved. A qualitative analysis of the data indicates a non-rotationally symmetric structure, e.g. the projection of an inclined disk. We employed extensive radiative transfer simulations based on spectral energy distribution fitting. Since SED-only fitting usually yields degenerate results, we first employed a statistical analysis of the parameters provided by the radiative transfer models. In addition, we compared the ten best-fitting self-consistent models to the interferometric observations. Our analysis of the Kleinmann-Wright Object suggests the existence of a circumstellar disk of 0.1M at an intermediate inclination of 76°, while an additional dusty envelope is not necessary for fitting the data. Furthermore, we demonstrate that the combination of IR interferometry with radiative transfer simulations has the potential to resolve ambiguities arising from the analysis of spectral energy distributions alone.

Abstract Copyright:

Journal keyword(s): techniques: interferometric -stars: formation - ISM: individuel objects: Kleinmann-Wright object - stars: protostars

Simbad objects: 17

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Number of rows : 17

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 * alf Crt PM* 10 59 46.4648602 -18 17 55.617244 6.14 5.16 4.07 3.27 2.72 K0IIIb 197 0
2 HD 101666 * 11 41 43.9467327788 -32 29 57.843983672   6.675 5.200     K5III 30 0
3 * eps Cru PM* 12 21 21.6093625 -60 24 04.129070   5.01 3.59     K3III 81 0
4 HD 120404 * 13 51 47.4342248812 -69 24 04.515687153   7.459 5.727     K5/M0III 22 0
5 * del TrA * 16 15 26.2697841 -63 41 08.449198   4.943 3.839     G2Ib-IIa 97 0
6 * alf TrA * 16 48 39.89508 -69 01 39.7626   3.36 1.92     K2III_Ba1 227 0
7 NAME M 8E IR Y*O 18 04 53.9 -24 26 41           ~ 81 0
8 W 33a Y*O 18 14 39.0 -17 52 03           ~ 570 0
9 HD 168415 PM* 18 20 08.7916221688 -15 49 54.108217037   6.867 5.371     K3III 28 0
10 MSX5C G014.9957-00.6735 IR 18 20 19.7 -16 13 31           ~ 36 2
11 NAME M 17 SW SFR 18 20 23.1 -16 11 43           ~ 241 0
12 NGC 6618 OpC 18 20 47 -16 10.3           ~ 1455 0
13 * del Sgr * 18 20 59.6435424 -29 49 41.165919   4.069 2.668     K2.5IIIaCN0.5 160 0
14 * lam Sgr PM* 18 27 58.2407185 -25 25 18.114589 4.75 3.85 2.81 2.06 1.50 K1IIIb 255 0
15 * tau Sgr PM* 19 06 56.4052936935 -27 40 13.609432896 5.65 4.51 3.31 2.44 1.85 K1.5IIIb 142 0
16 * eps Peg LP* 21 44 11.1561394 +09 52 30.031152 5.61 3.91 2.39 1.34 0.58 K2Ib-II 428 0
17 * alf Tuc SB* 22 18 30.0947834 -60 15 34.526307 5.75 4.18 2.82 1.76 1.02 K3III 120 0

    Equat.    Gal    SGal    Ecl

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2019.10.19-20:54:23

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