The β Pictoris association: Catalog of photometric rotational periods of low-mass members and candidate members⋆,⋆⋆,⋆⋆⋆
1 INAF-Catania Astrophysical Observatory, via S. Sofia, 78, 95123 Catania, Italy
2 York Creek Observatory, Georgetown, 7253 Tasmania, Australia
3 Instituto de Astronomía y Física del Espacio (IAFE-CONICET), Buenos Aires, Argentina
4 Departamento de Física, FCEN-Universidad de Buenos Aires, Buenos Aires, Argentina
5 Department of Physics, College of Science, Guizhou University, 550025 Guiyang, PR China
6 Aryabhatta Research Institute of Observational Sciences, Manora Peak, 263129 Nainital, India
7 Observatorio Astrónomico de Córdoba, Laprida 854, X5000BGR, Córdoba, Argentina
8 Consejo National de Investigaciones Científicas y Técnicas (CONICET), Argentina
9 Remote Observatory Atacama Desert (ROAD), Vereniging Voor Sterrenkunde (VVS), Oude Bleken 12, 2400 Mol, Belgium
10 American Association of Variable Star Observers (AAVSO), Cambridge, MA 02138, USA
11 Harlingten Atacama Observatory, San Pedro de Atacama, Chile
12 Research Institute Crimean Astrophysical Observatory, 298409 Nauchny, Crimea
13 IAU Minor Planet Center code D79, 2 Yandra Street, Vale Park, 5081 South Australia, Australia
14 Taurus Hill Observatory, 79480 Kangslanpi, Varkaus, Finland
15 Canada-France-Hawaii Telescope, 65-1238 Mamalahoa Hwy, Kamuela, HI 96743, USA
16 Klein Karoo Observatory, 6620 Western Cape, South Africa
17 Zeta UMa Observatory, 28008 Madrid, Spain
18 Montcabrer Observatory, C/Jaume Balmes, 24, Cabrils, Spain
19 Southern Stars Observatory, Pamatai, Tahiti, French Polynesia, France
20 Perth Exoplanet Survey Telescope, Western Australia, Australia
Received: 20 June 2016
Accepted: 9 September 2016
Aims. We intended to compile the most complete catalog of bona fide members and candidate members of the β Pictoris association, and to measure their rotation periods and basic properties from our own observations, public archives, and exploring the literature.
Methods. We carried out a multi-observatories campaign to get our own photometric time series and collected all archived public photometric data time series for the stars in our catalog. Each time series was analyzed with the Lomb-Scargle and CLEAN periodograms to search for the stellar rotation periods. We complemented the measured rotational properties with detailed information on multiplicity, membership, and projected rotational velocity available in the literature and discussed star by star.
Results. We measured the rotation periods of 112 out of 117 among bona fide members and candidate members of the β Pictoris association and, whenever possible, we also measured the luminosity, radius, and inclination of the stellar rotation axis. This represents to date the largest catalog of rotation periods of any young loose stellar association.
Conclusions. We provided an extensive catalog of rotation periods together with other relevant basic properties useful to explore a number of open issues, such as the causes of spread of rotation periods among coeval stars, evolution of angular momentum, and lithium-rotation connection.
Key words: stars: activity / stars: late-type / starspots / open clusters and associations: individual:βPictoris association / binaries: close / stars: rotation
Tables 1 and 2 are also available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (22.214.171.124) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/600/A83
Table 3 is only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (126.96.36.199) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/600/A83
Based on observations obtained at the Canada-France-Hawaii Telescope (CFHT) which is operated by the National Research Council of Canada, the Institut National des Sciences de l’Univers of the Centre National de la Recherche Scientique of France, and the University of Hawaii.
© ESO, 2017