Gas infall via accretion disk feeding Cepheus A HW2

• Published in: Astronomy and astrophysics (Berlin) Vol. 697; p. A206
• Main Authors: Sanna, A., Oliva, A., Moscadelli, L., Carrasco-González, C., Giannetti, A., Sabatini, G., Beltrán, M., Brogan, C., Hunter, T., Torrelles, J. M., Rodríguez-Kamenetzky, A., Caratti o Garatti, A., Kuiper, R.
• Format: Journal Article
• Language: English
• Published: 01.05.2025
• ISSN: 0004-6361; 1432-0746
• DOI: 10.1051/0004-6361/202450330

The star-forming region Cepheus A hosts a very young star, called HW2, that is the second closest to us growing a dozen times more massive than our Sun. The circumstellar environment surrounding HW2 has been the subject of extensive debate on the possible presence of an accretion disk, whose existence is at the foundation of our current paradigm of star formation. Here, we look to answer this long-standing question by resolving the gaseous disk component and its kinematics through sensitive observations at centrimetre (cm) wavelengths of hot ammonia (NH 3 ) with the Jansky Very Large Array. We mapped the accretion disk surrounding HW2 at radii between 200 and 700 au, showing how fast circumstellar gas collapses and slowly orbits to pile up near the young star at very high rates of 2 × 10 −3 M ⊙ yr −1 . These results, corroborated by state-of-the-art simulations, show that an accretion disk is still efficient in terms of focusing huge mass-infall rates near the young star, even after this star had already achieved a large mass of 16 M ⊙ .