Feeding a Protostar with 10 000 au Scale Streamers
1 Max-Planck-Institut für extraterrestrische Physik (MPE), Gießenbachstr. 1, 85748 Garching, Germany
2 Department of Astronomy, The University of Texas at Austin, 2500 Speedway, Austin, TX 78712, USA
3 Institut de Radioastronomie Millimétrique (IRAM), 300 rue de la Piscine, 38406 Saint-Martin d’Hères, France
* e-mail: email@example.com
Published online: 7 September 2022
Dense cores are the places where stars are formed within the supersonic Molecular Clouds. These dense regions (n ∼ 105 cc) are cold (T ∼10 K) and display subsonic levels of turbulence (Mach ∼ 0.5), and represent the initial conditions for both star and disk formation. However, the influence of the parental core properties on the disk formation process is still not well constrained, and it is therefore crucial to study dense cores with interferometers to better understand the dense core and disk connection. We present NOEMA observations of a Class 0 object, which has been suggested to present a disk under gravitational instability (GI) (asymmetrical features in ALMA high resolution dust continuum emission). Our new data reveal a previously unseen large scale (∼10,000 au, or 33′′) streamer of fresh gas from the surrounding dense core down to the disk scales. This streamer is almost perpendicular to the outflow, and it contains material with subsonic levels of turbulence, and therefore unperturbed by the outflow. Based on the total mass in the streamer and the free-fall timescale, we estimate infall rates to the disk scales, which clearly show that accretion via streamer can have an important role in the disk formation. Moreover, these results show that previously observed disk asymmetries could also be driven by large scale asymmetric flows instead of GI. This result shows the power and importance of studying dense cores with interferometers to provide a complete and proper picture of star and disk formation.
© The Authors, Published by EDP Sciences, 2022
This is an Open Access article distributed under the terms of the Creative Commons Attribution License 4.0 (http://creativecommons.org/licenses/by/4.0/).