Volume 603, July 2017
|Number of page(s)||9|
|Section||Interstellar and circumstellar matter|
|Published online||11 July 2017|
Planar infall of CH3OH gas around Cepheus A HW2
1 Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
2 INAF, Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
3 INAF, Osservatorio Astronomico di Cagliari, via della Scienza 5, 09047 Selargius, Italy
4 JIVE, Joint Institute for VLBI in Europe, Postbus 2, 7990 AA Dwingeloo, The Netherlands
5 European Southern Observatory, Alonso de Cordova 3107, Casilla 19001, Santiago 19, Chile
6 Ural Federal University, 51 Lenin Str., 620000 Ekaterinburg, Russia
Received: 13 March 2017
Accepted: 7 April 2017
Aims. In order to test the nature of an (accretion) disk in the vicinity of Cepheus A HW2, we measured the three-dimensional velocity field of the CH3OH maser spots, which are projected within 1000 au of the HW2 object, with an accuracy on the order of 0.1 km s-1.
Methods. We made use of the European VLBI Network (EVN) to image the 6.7 GHz CH3OH maser emission toward Cepheus A HW2 with 4.5 milliarcsec resolution (3 au). We observed at three epochs spaced by one year between 2013 and 2015. During the last epoch, in mid-March 2015, we benefited from the newly deployed Sardinia Radio Telescope.
Results. We show that the CH3OH velocity vectors lie on a preferential plane for the gas motion with only small deviations of 12° ± 9° away from the plane. This plane is oriented at a position angle of 134° east of north, and inclined by 26° with the line of sight, closely matching the orientation of the previously reported disk-like structure. Knowing the orientation of the equatorial plane, we can reconstruct a face-on view of the CH3OH gas kinematics onto the plane. CH3OH maser emission is detected within a radius of 900 au from HW2, and down to a radius of about 300 au, the latter coincident with the extent of the dust emission at 0.9 mm. The velocity field is dominated by an infall component of about 2 km s-1 down to a radius of 300 au, where a rotational component of 4 km s-1 becomes dominant. We discuss the nature of this velocity field and the implications for the enclosed mass.
Conclusions. These findings directly support the interpretation that the high-density gas and dust emission that surrounds Cepheus A HW2 traces an accretion disk.
Key words: ISM: kinematics and dynamics / masers / stars: formation / stars: individual: Cepheus A HW2
© ESO, 2017
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