EDP Sciences
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Issue A&A
Volume 484, Number 1, June II 2008
Page(s) 281 - 291
Section Stellar structure and evolution
DOI http://dx.doi.org/10.1051/0004-6361:20078493
Published online 17 January 2008



A&A 484, 281-291 (2008)
DOI: 10.1051/0004-6361:20078493

Astrometric and photometric monitoring of GQ Lupi and its sub-stellar companion

R. Neuhäuser1, M. Mugrauer1, A. Seifahrt1, T. O. B. Schmidt1, and N. Vogt2, 3

1  Astrophysikalisches Institut, Universität Jena, Schillergässchen 2-3, 07745 Jena, Germany
    e-mail: rne@astro.uni-jena.de
2  Departamento de Física y Astronomía, Universidad de Valparaíso, Avenida Gran Bretaña 1111, Valparaíso, Chile
3  Instituto de Astronomía, Universidad Catolica del Norte, Avda. Angamos 0610, Antofagasta, Chile

Received 16 August 2007 / Accepted 4 December 2007

Abstract
Context. Neuhäuser et al. (2005, A&A, 435, L13) presented direct imaging evidence for a sub-stellar companion to the young T Tauri star GQ Lupi. Common proper motion was highly significant, but no orbital motion was detected. Faint luminosity, low gravity, and a late-M/early-L spectral type indicated that the companion is either a planet or a brown dwarf.
Aims. We have monitored GQ Lupi and its companion in order to detect orbital and parallactic motion and variability in its brightness. We also search for closer and fainter companions.
Methods. We have taken six more images with the VLT Adaptive Optics instrument NACO from May 2005 to Feb. 2007, always with the same calibration binary from Hipparcos for both astrometric and photometric calibration. By adding up all the images taken so far, we search for additional companions.
Results. The position of GQ Lupi A and its companion compared to a nearby non-moving background object varies as expected for parallactic motion by about one pixel ( $2 \cdot \pi$ with parallax $\pi$). We could not find evidence for variability of the GQ Lupi companion in the $K_{\rm s}$-band (standard deviation being $\pm$0.08 mag), which may be due to large error bars. No additional companions are found with deep imaging.
Conclusions. There is now exceedingly high significance for common proper motion of GQ Lupi A and its companion. In addition, we see for the first time an indication for orbital motion (~2 to 3 mas/yr decrease in separation, but no significant change in the position angle), consistent with a near edge-on or highly eccentric orbit. We measured the parallax for GQ Lupi A to be $\pi = 6.4 \pm 1.9$ mas (i.e. $156 \pm 50$ pc) and for the GQ Lupi companion to be $7.2 \pm 2.1$ mas (i.e. $139 \pm 45$ pc), both consistent with being in the Lupus I cloud and bound to each other.


Key words: astrometry -- stars: binaries: visual -- stars: distances -- stars: formation -- stars: individual: GQ Lupi -- stars: pre-main sequence



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Editor-in-Chief: T. Forveille
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ISSN: 0004-6361 ; e-ISSN: 1432-0746
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Published by: EDP Sciences

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