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The GRAVITY young stellar object survey. II. First spatially resolved observations of the CO bandhead emission in a high-mass YSO | | GRAVITY Collaboration
; A. Caratti o Garatti
; R. Fedriani
; R. Garcia Lopez
; M. Koutoulaki
; K. Perraut
; H. Linz
; W. Brandner
; P. Garcia
; L. Klarmann
; T. Henning
; L. Labadie
; J. Sanchez-Bermudez
; B. Lazareff
; E.F. van Dishoeck
; P. Caselli
; P.T. de Zeeuw
; A. Bik
; M. Benisty
; C. Dougados
; T.P. Ray
; A. Amorim
; J.-P. Berger
; Y. Clénet
; V. Coudé du Foresto
; G. Duvert
; A. Eckart
; F. Eisenhauer
; F. Gao
; E. Gendron
; R. Genzel
; S. Gillessen
; P. Gordo
; L. Jocou
; M. Horrobin
; P. Kervella
; S. Lacour
; J.-B. Le Bouquin
; P. Léna
; R. Grellmann
; T. Ott
; T. Paumard
; G. Perrin
; G. Rousset
; S. Scheithauer
; J. Shangguan
; J. Stadler
; O. Straub
; C. Straubmeier
; E. Sturm
; W.F. Thi
; F.H. Vincent
; F. Widmann
; | | Date: |
11 Mar 2020 | | Abstract: | The inner regions of the discs of high-mass young stellar objects (HMYSOs)
are still poorly known due to the small angular scales and the high visual
extinction involved. We deploy near-infrared (NIR) spectro-interferometry to
probe the inner gaseous disc in HMYSOs and investigate the origin and physical
characteristics of the CO bandhead emission (2.3-2.4 $mu$m). We present the
first GRAVITY/VLTI observations at high spectral (R=4000) and spatial (mas)
resolution of the CO overtone transitions in NGC 2024 IRS2. The continuum
emission is resolved in all baselines and is slightly asymmetric, displaying
small closure phases ($leq$8$^{circ}$). Our best ellipsoid model provides a
disc inclination of 34$^{circ}$$pm$1$^{circ}$, a disc major axis position
angle of 166$^{circ}$$pm$1$^{circ}$, and a disc diameter of 3.99$pm$0.09
mas (or 1.69$pm$0.04 au, at a distance of 423 pc). The small closure phase
signals in the continuum are modelled with a skewed rim, originating from a
pure inclination effect. For the first time, our observations spatially and
spectrally resolve the first four CO bandheads. Changes in visibility, as well
as differential and closure phases across the bandheads are detected. Both the
size and geometry of the CO-emitting region are determined by fitting a
bidimensional Gaussian to the continuum-compensated CO bandhead visibilities.
The CO-emitting region has a diameter of 2.74$pm^{0.08}_{0.07}$ mas
(1.16$pm$0.03 au), and is located in the inner gaseous disc, well within the
dusty rim, with inclination and $PA$ matching the dusty disc geometry, which
indicates that both dusty and gaseous discs are coplanar. Physical and
dynamical gas conditions are inferred by modelling the CO spectrum. Finally, we
derive a direct measurement of the stellar mass of $M_*sim$14.7$^{+2}_{-3.6}$
M$_{odot}$ by combining our interferometric and spectral modelling results. | | Source: | arXiv, 2003.5404 | | Services: | Forum | Review | PDF | Favorites | |
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