IRAS 04158+2805 has long been thought to be a very low mass T-Tauri star (VLMS) surrounded by a nearly edge-on, extremely large disc. Recent observations revealed that this source hosts a binary surrounded by an extended circumbinary disc with a central dust cavity. In this paper, we combine ALMA multi-wavelength observations of continuum and 12CO line emission, with Hα imaging and Keck astrometric measures of the binary to develop a coherent dynamical model of this system. The system features an azimuthal asymmetry detected at the western edge of the cavity in Band 7 observations and a wiggling outflow. Dust emission in ALMA Band 4 from the proximity of the individual stars suggests the presence of marginally resolved circumstellar discs. We estimate the binary orbital parameters from the measured arc of the orbit from Keck and ALMA astrometry. We further constrain these estimates using considerations from binary-disc interaction theory. We finally perform three SPH gas + dust simulations based on the theoretical constraints; we post-process the hydrodynamic output using radiative transfer Monte Carlo methods and directly compare the models with observations. Our results suggest that a highly eccentric e ∼ 0.5–0.7 equal mass binary, with a semi-major axis of ∼55 au, and small/moderate orbital plane versus circumbinary disc inclination θ ≲ 30○ provides a good match with observations. A dust mass of ∼1.5 × 10−4 M⊙ best reproduces the flux in Band 7 continuum observations. Synthetic CO line emission maps qualitatively capture both the emission from the central region and the non-Keplerian nature of the gas motion in the binary proximity.
Wakeflow is a Python package for generating semi-analytic models of the perturbations induced by planets embedded in gaseous circumstellar disks. These perturbations take the form of a spiral shock wave (Ogilvie & Lubow, 2002), and are often called a "planet wake" in analogy with that produced by a boat in a lake. Using Wakeflow, users may calculate the perturbed density and velocity fields of the gas in the disk. These may be used with radiation transfer codes to generate synthetic observations that map both the gas distribution and the gas kinematics. Comparison with real observations, such as from molecular line emission taken with the Attacama Large Millimetre Array, allows researchers to infer the properties of potential planets as well as the disk itself.
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