Volume 589, May 2016
|Number of page(s)||5|
|Published online||06 April 2016|
Tracing jet emission at the base of a high-mass YSO
First AMBER/VLTI observations of the Brγ emission in IRAS 13481-6124⋆
1 Dublin Institute for Advanced Studies, School of Cosmic
Physics, Astronomy & Astrophysics Section, 31 Fitzwilliam Place, Dublin 2, Ireland
2 Thüringer Landessternwarte Tautenburg, Sternwarte 5, 07778 Tautenburg, Germany
3 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
4 University of Exeter, School of Physics, Stocker Road, Exeter, EX4 4QL, UK
5 School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK
6 ESO-European Organisation for Astronomical Research in the Southern Hemisphere, Alonso de Cordova 3107, Vitacura, Santiago de Chile, Chile
Received: 27 January 2016
Accepted: 17 March 2016
Aims. To probe the circumstellar environment of IRAS 13481-6124, a 20 M⊙ high-mass young stellar object (HMYSO) with a collimated parsec-scale jet and an accretion disc, we investigate the origin of its Brγ emission line through near-infrared (NIR) interferometry.
Methods. We present the first AMBER/VLTI observations of the Brγ emitting region in an HMYSO at medium spectral resolution (R = 1500).
Results. Our AMBER/VLTI observations reveal a spatially and spectrally resolved Brγ line in emission with a strong P Cygni profile, indicating outflowing matter with a terminal velocity of ~500 km s-1. Visibilities, differential phases, and closure phases are detected in our observations within the spectral line and in the adjacent continuum. Both total visibilities (continuum plus line emitting region) and pure-line visibilities indicate that the Brγ-emitting region is more compact (2–4 mas in diameter or ~6–13 au at 3.2 kpc) than the continuum-emitting region (~5.4 mas or ~17 au). The absorption feature is also spatially resolved at the longest baselines (81 and 85 m) and has a visibility that is slightly smaller than the continuum-emitting region. The differential phases at the four longest baselines display an “S”-shaped structure across the line, peaking in the blue- and red-shifted high-velocity components. The calibrated photocentre shifts are aligned with the known jet axis, i.e they are probably tracing an ionised jet. The high-velocity components (vr ~ 100−500 km s-1) are located far from the source, whereas the low-velocity components (0–100 km s-1) are observed to be closer, indicating a strong acceleration of the gas flow in the inner 10 au. Finally, a non-zero closure phase along the continuum is detected. By comparing our observations with the synthetic images of the continuum around 2.16 μm, we confirm that this feature originates from the asymmetric brightness distribution of the continuum owing to the inclination of the inner disc.
Key words: stars: formation / circumstellar matter / stars: protostars / stars: massive / techniques: interferometric / techniques: high angular resolution
© ESO, 2016
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