Volume 566, June 2014
|Number of page(s)||5|
|Section||Interstellar and circumstellar matter|
|Published online||25 June 2014|
CRIRES-VLT high-resolution spectro-astrometry as a tool in the search for disks inside the cores of planetary nebulae⋆
1 Instituto de Astrofísica de Andalucía (IAA-CSIC), Glorieta de la Astronomía s/n, 18008 Granada, Spain
e-mail: firstname.lastname@example.org; email@example.com
2 European Southern Observatory (ESO), Karl Schwarzschild Str. 2, 85748 Garching bei München, Germany
3 Universidad de Vigo, Departamento de Física Aplicada, Facultad de Ciencias, Campus Lagoas-Marcosende s/n, 36310 Vigo, Spain
4 Consejo Superior de Investigaciones Científicas (CSIC), C/ Serrano 117, 28006 Madrid, Spain
5 Department of Astronomy and Astrophysics, University of Chicago, Chicago, IL 60637, USA
Received: 29 August 2013
Accepted: 15 May 2014
The onset of asymmetry in planetary nebulae (PNe) occurs during the short transition between the end of the asymptotic giant branch (AGB) phase and the beginning of the PN phase. Sources in this transition phase are compact and emit intensely in infrared wavelengths, making high spatial resolution observations in the infrared mandatory to investigate the shaping process of PNe. Interferometric VLTI IR observations have revealed compelling evidence of disks at the cores of PNe, but the limited sensitivity, strong observational constraints, and limited spatial coverage place severe limits on a universal use of this technique. Inspired by the successful detection of proto-planetary disks using spectro-astrometric observations, we apply this technique here for the first time to search for subarcsecond structures in PNe. Our exploratory study using CRyogenic high-resolution Infra-Red Echelle Spectrograph (CRIRES) commissioning data of the proto-PN IRAS 17516−2525 and the young PN SwSt 1 has revealed small-sized structures after the spectro-astrometric analysis of the two sources. In IRAS 17516−2525, the spectro-astrometric signal has a size of only 12 ± 5 mas, as detected in the Brγ line, whereas the structures found in SwSt 1 have sizes of 230 ± 29 mas in the [Fe iii] line and 130 ± 21 mas in the Brγ line. The spectroscopic observations required to perform spectro-astrometry of sources in the transition towards the PN phase are less time-consuming and much more sensitive than VLTI IR observations. The results presented here open a new window in the search for the small-sized collimating agents that shape the complex morphologies of extremely axisymmetric PNe.
Key words: techniques: spectroscopic / techniques: high angular resolution / ISM: jets and outflows / planetary nebulae: general / planetary nebulae: individual: IRAS 17516 / 2525 / planetary nebulae: individual: SwSt 1
© ESO, 2014
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