Volume 539, March 2012
|Number of page(s)||12|
|Section||Galactic structure, stellar clusters and populations|
|Published online||24 February 2012|
Parallaxes and proper motions of interstellar masers toward the Cygnus X star-forming complex
I. Membership of the Cygnus X region
1 Istituto di Fisica dello Spazio Interplanetario (INAF–IFSI), via del fosso del cavaliere 100, 00133 Roma, Italy
2 Max-Planck-Institut für Radioastronomie (MPIfR), Auf dem Hügel 69, 53121 Bonn, Germany
e-mail: firstname.lastname@example.org; email@example.com; firstname.lastname@example.org;
3 National Radio Astronomy Observatory, 1003 Lopezville Road, Socorro 87801, USA
4 Harvard Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
5 Joint Institute for VLBI in Europe, Postbus 2, 7990 AA Dwingeloo, The Netherlands
6 Sterrewacht Leiden, Leiden University, Postbus 9513, 2300 RA Leiden, The Netherlands
7 Mizusawa VLBI Observatory, National Astronomical Observatory of Japan, 2-21-1 Osawa, Mitaka, 181-8588 Tokyo, Japan
8 Faculty of Science, Yamaguchi University, 1677-1 Yoshida, 753-8512 Yamaguchi, Japan
Received: 5 October 2011
Accepted: 30 November 2011
Context. Whether the Cygnus X complex consists of one physically connected region of star formation or of multiple independent regions projected close together on the sky has been debated for decades. The main reason for this puzzling scenario is the lack of trustworthy distance measurements.
Aims. We aim to understand the structure and dynamics of the star-forming regions toward Cygnus X by accurate distance and proper motion measurements.
Methods. To measure trigonometric parallaxes, we observed 6.7 GHz methanol and 22 GHz water masers with the European VLBI Network and the Very Long Baseline Array.
Results. We measured the trigonometric parallaxes and proper motions of five massive star-forming regions toward the Cygnus X complex and report the following distances within a 10% accuracy: 1.30+0.07-0.07 kpc for W 75N, 1.46+0.09-0.08 kpc for DR 20, 1.50+0.08-0.07 kpc for DR 21, 1.36+0.12-0.11 kpc for IRAS 20290+4052, and 3.33+0.11-0.11 kpc for AFGL 2591. While the distances of W 75N, DR 20, DR 21, and IRAS 20290+4052 are consistent with a single distance of 1.40 ± 0.08 kpc for the Cygnus X complex, AFGL 2591 is located at a much greater distance than previously assumed. The space velocities of the four star-forming regions in the Cygnus X complex do not suggest an expanding Strömgren sphere.
Key words: stars: formation / astrometry / techniques: interferometric / ISM: general / masers / ISM: kinematics and dynamics
© ESO, 2012
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