Loading…

Long-term photometry of IC 348 with the Young Exoplanet Transit Initiative network

We present long-term photometric observations of the young open cluster IC 348 with a baseline time-scale of 2.4 yr. Our study was conducted with several telescopes from the Young Exoplanet Transit Initiative (YETI) network in the Bessel R band to find periodic variability of young stars. We identif...

Full description

Saved in:
Bibliographic Details
Published in:Monthly notices of the Royal Astronomical Society 2016-11, Vol.462 (3), p.2396-2417
Main Authors: Fritzewski, D. J., Kitze, M., Mugrauer, M., Neuhäuser, R., Adam, C., Briceño, C., Buder, S., Butterley, T., Chen, W.-P., Dinçel, B., Dhillon, V. S., Errmann, R., Garai, Z., Gilbert, H. F. W., Ginski, C., Greif, J., Hardy, L. K., Hernández, J., Huang, P. C., Kellerer, A., Kundra, E., Littlefair, S. P., Mallonn, M., Marka, C., Pannicke, A., Pribulla, T., Raetz, St, Schmidt, J. G., Schmidt, T. O. B., Seeliger, M., Wilson, R. W., Wolf, V.
Format: Article
Language:English
Subjects:
Citations: Items that this one cites
Items that cite this one
Online Access:Get full text
Tags: Add Tag
No Tags, Be the first to tag this record!
Description
Summary:We present long-term photometric observations of the young open cluster IC 348 with a baseline time-scale of 2.4 yr. Our study was conducted with several telescopes from the Young Exoplanet Transit Initiative (YETI) network in the Bessel R band to find periodic variability of young stars. We identified 87 stars in IC 348 to be periodically variable; 33 of them were unreported before. Additionally, we detected 61 periodic non-members of which 41 are new discoveries. Our wide field of view was the key to those numerous newly found variable stars. The distribution of rotation periods in IC 348 has always been of special interest. We investigate it further with our newly detected periods but we cannot find a statistically significant bimodality. We also report the detection of a close eclipsing binary in IC 348 composed of a low-mass stellar component (M ≳ 0.09 M⊙) and a K0 pre-main-sequence star (M ≈ 2.7 M⊙). Furthermore, we discovered three detached binaries among the background stars in our field of view and confirmed the period of a fourth one.
ISSN:0035-8711
1365-2966
DOI:10.1093/mnras/stw1797