| Issue |
A&A
Volume 567, July 2014
|
|
|---|---|---|
| Article Number | L5 | |
| Number of page(s) | 6 | |
| Section | Letters | |
| DOI | https://doi.org/10.1051/0004-6361/201423855 | |
| Published online | 11 July 2014 | |
High angular resolution 7 mm images toward the UC HII region W3(OH)⋆,⋆⋆
1 Max-Planck-Institut für Radioastronomie, auf dem Hügel 69, 53121 Bonn, Germany
e-mail: sdzib@mpifr-bonn.mpg.de
2 Centro de Radiostronomía y Astrofísica, Universidad Nacional Autónoma de México, 58089 Morelia, Mexico
3 Astronomy Department, Faculty of Science, King Abdulaziz University, PO Box 80203, 21589 Jeddah, Saudi Arabia
4 School of Astronomy and Space Science, Nanjing University, 22 Hankou Road, 210093 Nanjing, PR China
5 Key Laboratory of Modern Astronomy and Astrophysics (Nanjing University), Ministry of Education, 210093 Nanjing, PR China
Received: 20 March 2014
Accepted: 20 June 2014
Context. Recent high angular resolution radio observations of the ultracompact H ii region W3(OH) confirm the presence of an extremely compact (0.′′05), time-variable source near its center.
Aims. We use new, sensitive high angular resolution observations of radio continuum and recombination lines to study the compact source in W3(OH) and the ultracompact H ii region itself.
Methods. We reduced and analyzed extensive Jansky Very Large Array observations of W3(OH) in the continuum at 41.0 GHz and in the H54α and He54α lines.
Results. Our images confirm there is the compact source and show that it is connected by a linear filament to the brightest part of W3(OH). We discuss several possible explanations for this structure and propose future observations that may clarify its nature.
Key words: ISM: jets and outflows / stars: formation / accretion, accretion disks / ISM: individual objects: W3(OH) / HII regions
Appendices are available in electronic form at http://www.aanda.org
Reduced VLA FITS cubes are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/567/L5
© ESO, 2014
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