The GRAVITY young stellar object survey: II. First spatially resolved observations of the CO bandhead emission in a high-mass YSO

被引：14

作者：

Garatti, A. Caratti O. ^{[1
,2
,3
]}

Fedriani, R. ^{[1
,3
,4
]}

Lopez, R. Garcia ^{[1
,2
,3
]}

Koutoulaki, M. ^{[1
,3
,5
]}

Perraut, K. ^{[6
]}

Linz, H. ^{[2
]}

Brandner, W. ^{[2
]}

Garcia, P. ^{[7
,8
,9
]}

Klarmann, L. ^{[2
]}

Henning, T. ^{[2
]}

Labadie, L. ^{[10
]}

Sanchez-Bermudez, J. ^{[2
,11
]}

Lazareff, B. ^{[6
]}

van Dishoeck, E. F. ^{[12
,14
]}

Caselli, P. ^{[12
]}

de Zeeuw, P. T. ^{[12
,14
]}

Bik, A. ^{[13
]}

Benisty, M. ^{[6
,9
]}

Dougados, C. ^{[6
]}

Ray, T. P. ^{[1
]}

Amorim, A. ^{[8
]}

Berger, J-P ^{[6
]}

Clenet, Y. ^{[15
]}

du Foresto, V. Coude ^{[15
]}

Duvert, G. ^{[6
]}

Eckart, A. ^{[10
]}

Eisenhauer, F. ^{[12
]}

Gao, F. ^{[12
]}

Gendron, E. ^{[15
]}

Genzel, R. ^{[12
,16
]}

Gillessen, S. ^{[12
]}

Gordo, P. ^{[8
]}

Jocou, L. ^{[6
]}

Horrobin, M. ^{[10
]}

Kervella, P. ^{[15
]}

Lacour, S. ^{[15
]}

Le Bouquin, J-B ^{[6
]}

Lena, P. ^{[15
]}

Grellmann, R. ^{[10
]}

Ott, T. ^{[12
]}

Paumard, T. ^{[15
]}

Perrin, G. ^{[15
]}

Rousset, G. ^{[15
]}

Scheithauer, S. ^{[2
]}

Shangguan, J. ^{[12
]}

Stadler, J. ^{[12
]}

Straub, O. ^{[12
]}

Straubmeier, C. ^{[10
]}

Sturm, E. ^{[12
]}

Thi, W. F. ^{[12
]}

机构：

[1] Dublin Inst Adv Studies, 31 Fitzwilliam Pl, Dublin D02 XF86, Ireland

[2] Max Planck Inst Astron, Konigstuhl 17, D-69117 Heidelberg, Germany

[3] Univ Coll Dublin, Sch Phys, Dublin 4, Ireland

[4] Chalmers Univ Technol, Dept Space Earth & Environm, S-41293 Gothenburg, Sweden

[5] European Southern Observ, Karl Schwarzschild Str 2, D-85748 Garching, Germany

[6] Univ Grenoble Alpes, CNRS, IPAG, F-38000 Grenoble, France

[7] Univ Porto, Fac Engn, Rua Dr Roberto Frias, P-4200465 Porto, Portugal

[8] Inst Super Tecn, CENTRA, Av Rovisco Pais, P-1049001 Lisbon, Portugal

[9] European Southern Observ, 19001 Casilla, Santiago 19, Chile

[10] Univ Cologne, Phys Inst 1, Zulpicher Str 77, D-50937 Cologne, Germany

[11] Univ Nacl Autonoma Mexico, Inst Astron, Apdo Postal 70264, Mexico City 04510, DF, Mexico

[12] Max Planck Inst Extraterr Phys, Giessenbachstr, D-85741 Garching, Germany

[13] Stockholm Univ, Oskar Klein Ctr, Dept Astron, S-10691 Stockholm, Sweden

[14] Leiden Univ, Leiden Observ, Pob 9513, NL-2300 RA Leiden, Netherlands

[15] PSL Res Univ, Sorbonne Univ, Observ Paris,Sorbonne Paris Cite, LESIA,CNRS,UPMC Univ Paris 06,Univ Paris Diderot, Paris, France

[16] Univ Calif Berkeley, Dept Phys, Le Conte Hall, Berkeley, CA 94720 USA

来源：

ASTRONOMY & ASTROPHYSICS | 2020年 / 635卷

基金：

欧洲研究理事会; 爱尔兰科学基金会;

关键词：

stars: formation; stars: massive; infrared: stars; techniques: interferometric; techniques: spectroscopic; methods: observational;

D O I：

10.1051/0004-6361/202037583

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Context. 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.Aims. We deploy near-infrared 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).Methods. We present the first GRAVITY/VLTI observations at high spectral (R=4000) and spatial (mas) resolution of the CO overtone transitions in NGC 2024 IRS 2.Results. The continuum emission is resolved in all baselines and is slightly asymmetric, displaying small closure phases (<= 8 degrees). Our best ellipsoid model provides a disc inclination of 34 degrees +/- 1 degrees, a disc major axis position angle (PA) of 166 degrees +/- 1 degrees, and a disc diameter of 3.99 +/- 0.09 mas (or 1.69 +/- 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 +/-(0.08)(0.07) +/- 0.07 0.08 </mml:msubsup> mas (1.16 +/- 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-* similar to 14.7(-3.6)(+2)M(circle dot) M * similar to 14 . 7 - 3.6 + 2 M circle dot by combining our interferometric and spectral modelling results.

引用

页数：9

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