Volume 568, August 2014
|Number of page(s)||8|
|Published online||25 August 2014|
Long-term Ks-band photometric monitoring of L dwarfs
1 Centro de Astrobiología (INTA-CSIC), PO Box 78, 28261 Villanueva de la Cañada, Madrid, Spain
2 Saint Louis University – Madrid Campus, Division of Science, Engineering and Nursing, Avenida del Valle 34, 28003 Madrid, Spain
3 Centro de Astrobiología (INTA-CSIC), Carretera de Ajalvir km. 4, 28850 Torrejón de Ardoz, Spain
Received: 6 May 2014
Accepted: 29 July 2014
Context. Ultracool dwarfs (≲2500 K) are known to display photometric variability in short timescales (hours to days), which has usually been related to rotation-modulated dust cloud patterns, or to unresolved companions.
Aims. We perform photometric time-series analysis of a sample of ten early to mid-L dwarfs in the field over three years of Ks-band observations with the OMEGA 2000 infrared camera of the 3.5 m telescope on Calar Alto Observatory between January 2010 and December 2012. This study represents the first systematic long-term photometric monitoring of this kind of object to date.
Methods. We perform Ks-band differential photometry of our targets (with typical errors of ±15−30 mmag at the 1σ level) by subtracting a reference flux from each photometric measurement. This reference flux is computed using three nearby, probably constant stars in the target’s field-of-view. We then construct and visually inspect the light curves to search for variability, and use four different periodogram algorithms to look for possible periods in our photometric data.
Results. Our targets do not display long-term variability over 1σ compared to other nearby stars of similar brightness, nor do the periodograms unveil any possible periodicity for these objects, with two exceptions: 2MASS J02411151-0326587 and G196-3B. In the case of 2MASS J02411151-0326587 (L0), our data suggest a tentative period of 307±21 days, at 40% confidence level, which seems to be associated with peak-to-peak variability of 44±10 mmag. This object may also display variability in timescales of years, as suggested by the comparison of our Ks-band photometry with 2MASS. For G196-3B (L3), we find peak-to-peak variations of 42±10 mmag, with a possible photometric period of 442±7 days, at 95% confidence level. This is roughly the double of the astrometric period reported by Zapatero Osorio et al. (2014, A&A, 568, A6). Given the significance of these results, further photometric data are required to confirm the long-term variability.
Conclusions. Our results suggest that early- to mid-L dwarfs are fairly stable in the Ks-band within ±90 mmag at the 3σ level over months to years, which covers hundreds to tens of thousands of rotation cycles. Two out of ten targets show periodic photometric variability at 2.2 μm with peak-to-peak variations of about 40 mmag and tentative periods of ~300 and ~450 d.
Key words: stars: low-mass / brown dwarfs / techniques: photometric / stars: general
© ESO, 2014
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