Publications of the MPIfR Optical & Infrared Interferometry Group


AMBER/VLTI interferometric observations of the recurrent Nova RS Oph 5.5 days after outburst

O. Chesneau, N. Nardetto, F. Millour, C. Hummel, A. Domiciano de Souza, D. Bonneau, M. Vannier, F. Rantakyrö, A. Spang, F. Malbet, D. Mourard, M.F. Bode, T.J. OBrien, G. Skinner, R.G. Petrov, P. Stee,
E. Tatulli, and F. Vakili

Astronomy & Astrophysics, vol. 464, pg.119-126 (2007)

Abstract
Aims.We report on spectrally dispersed interferometric AMBER/VLTI observations of the recurrent nova RS Oph five days after the discovery of its outburst on 2006 Feb. 12.
Methods.Using three baselines ranging from 44 to 86 m, and a spectral resolution of $\lambda/\delta\lambda=1500$, we measured the extension of the milliarcsecond-scale emission in the K band continuum and in the Br$\gamma$ and He I $2.06~\mu$m lines, allowing us to get an insight into the kinematics of the line forming regions. The continuum visibilities were interpreted by fitting simple geometric models consisting of uniform and Gaussian ellipses, ring and binary models. The visibilities and differential phases in the Br$\gamma$ line were interpreted using skewed ring models aiming to perform a limited parametric reconstruction of the extension and kinematics of the line forming region.
Results.The limited uv coverage does not allow discrimination between filled models (uniform or Gaussian ellipses) and rings. Binary models are discarded because the measured closure phase in the continuum is close to zero. The visibilities in the lines are at a low level compared to their nearby continuum, consistent with a more extended line forming region for He I $2.06~\mu$m than Br$\gamma$. The ellipse models for the continuum and for the lines are highly flattened ( $b/a\sim0.6$) and share the same position angle ( ${\rm PA}\sim140^{\circ}$). Their typical Gaussian extensions are $3.1\times1.9~{\rm mas}$, $4.9\times2.9~{\rm mas}$ and $6.3\times3.6~{\rm mas}$ for the continuum, Br$\gamma$ and He I $2.06~\mu$m lines, respectively. Two radial velocity fields are apparent in the Br$\gamma$ line: a slow expanding ring-like structure ( $v_{\rm rad}\leq1800~{\rm km\,s}^{-1}$), and a fast structure extended in the E-W direction ( $v_{\rm rad}\sim 2500{-}3000~{\rm km\,s}^{-1}$), a direction that coincides with the jet-like structure seen in the radio. These results confirm the basic fireball model, contrary to the conclusions of other interferometric observations conducted by Monnier et al. (2006a, ApJ, 647, L127).

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