Deep infrared imaging and spectroscopy of the nearby late M-dwarf DENIS-P J104814-395606

Details Deep infrared imaging and spectroscopy of the nearby late M-dwarf DENIS-P J104814-395606 Deep infrared imaging and spectroscopy of the nearby late M-dwarf DENIS-P J104814-395606

Jul 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002an....323..447n&link_type=abstract

Astronomische Nachrichten, vol. 323, no. 5, p. 447-452

Other

7

Stars: Individual (M Dwarf Denis-P J104814-395606), Technique: Infrared Imaging, Technique: Spectroscopic

Scientific paper

We obtained deep H- and K-band images of DENIS-P J104814-395606 using SofI and the speckle camera SHARP-I at the ESO-3.5m-NTT as well as QUIRC at the Mauna Kea 2.2m telescope between December 2000 and June 2001. The target was recently discovered as nearby M9-dwarf among DENIS sources (Delfosse et al. 2001). We detect parallactic motion on our images and determine the distance to be 4.6 +/- 0.3 pc, more precise than previously known. From the available colors, the distance, and the spectral type, we conclude from theoretical models that the star has a mass of ~ 0.075 to 0.09 Msun and an age of ~ 1 to 2 Gyrs. We also obtained H- and K-band spectra of this star with ISAAC at the VLT. A faint companion candidate is detected 6'' NNW of the star, which is 6.4 +/- 0.5 mag fainter in H. However, according to another image taken several month later, the companion candidate is not co-moving with the M9-dwarf. Instead, it is a non-moving background object. Limits for undetected companion candidates are such that we can exclude any stellar companions outside of ~ 0.25'' (1 AU), any brown dwarf companions (above the deuterium burning mass limit) outside of ~ 2'' (9 AU), and also any companion down to ~ 40 M_jup with >= 0.15'' (0.7 AU) separation, all calculated for an age of 2 Gyrs. Our observations show that direct imaging of sub-stellar companions near the deuterium burning mass limit in orbit around nearby ultra-cool dwarfs is possible, even with separations that are smaller than the semi-major axis of the outermost planet in our solar system, namely a few tens of AU.

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