A revised distance to IRAS 16293-2422 from VLBA astrometry of associated water masers

¹ Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany
e-mail: sdzib@mpifr-bonn.mpg.de
² Humboldt Fellow, Berlin, Germany
e-mail: gortiz@mpifr-bonn.mpg.de
³ Instituto de Radioastronomía y Astrofísica, Universidad Nacional Autónoma de México, Morelia 58089, Mexico
e-mail: a.hernandez@irya.unam.mx
⁴ IRAP, Université de Toulouse, CNRS, UPS, CNES, Toulouse, France
⁵ Instituto de Astronomía, Universidad Nacional Autónoma de México, Apartado Postal 70-264, CdMx C.P. 04510, Mexico
⁶ National Radio Astronomy Observatory, PO Box 0, Socorro, NM 87801, USA

Received: 12 October 2017
Accepted: 8 February 2018

Abstract

IRAS 16293-2422 is a very well-studied young stellar system seen in projection towards the L1689N cloud in the Ophiuchus complex. However, its distance is still uncertain; there is a range of values from 120 pc to 180 pc. Our goal is to measure the trigonometric parallax of this young star by means of H₂O maser emission. We use archival data from 15 epochs of VLBA observations of the 22.2 GHz water maser line. By modeling the displacement on the sky of the H₂O maser spots, we derived a trigonometric parallax of 7.1 ± 1.3 mas, corresponding to a distance of 141₋₂₁⁺³⁰ pc. This new distance is in good agreement with recent values obtained for other magnetically active young stars in the L1689 cloud. We relate the kinematics of these masers with the outflows and the recent ejections powered by source A in the system.