Article (Scientific journals)
A census of variability in globular cluster M 68 (NGC 4590)
Kains, N.; Arellano Ferro, A.; Figuera Jaimes, R. et al.
2015In Astronomy and Astrophysics, 578
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Keywords :
Globular clusters: individual: M 68; Stars: variables: general; Stars: variables: RR Lyrae; Astrophysics; Image analysis; Surveys; Telescopes; Time series analysis; Electron multiplying ccds; Empirical relations; Fourier decomposition; Globular clusters; Globular clusters: individual; Spatial resolution; Stars
Abstract :
[en] Aims. We analyse 20 nights of CCD observations in the V and I bands of the globular cluster M 68 (NGC 4590) and use them to detect variable objects. We also obtained electron-multiplying CCD (EMCCD) observations for this cluster in order to explore its core with unprecedented spatial resolution from the ground. Methods. We reduced our data using difference image analysis to achieve the best possible photometry in the crowded field of the cluster. In doing so, we show that when dealing with identical networked telescopes, a reference image from any telescope may be used to reduce data from any other telescope, which facilitates the analysis significantly. We then used our light curves to estimate the properties of the RR Lyrae (RRL) stars in M 68 through Fourier decomposition and empirical relations. The variable star properties then allowed us to derive the cluster's metallicity and distance. Results. M 68 had 45 previously confirmed variables, including 42 RRL and 2 SX Phoenicis (SX Phe) stars. In this paper we determine new periods and search for new variables, especially in the core of the cluster where our method performs particularly well. We detect 4 additional SX Phe stars and confirm the variability of another star, bringing the total number of confirmed variable stars in this cluster to 50. We also used archival data stretching back to 1951 to derive period changes for some of the single-mode RRL stars, and analyse the significant number of double-mode RRL stars in M 68. Furthermore, we find evidence for double-mode pulsation in one of the SX Phe stars in this cluster. Using the different classes of variables, we derived values for the metallicity of the cluster of [Fe/H] = -2.07 ± 0.06 on the ZW scale, or -2.20 ± 0.10 on the UVES scale, and found true distance moduli μ<inf>0</inf> = 15.00 ± 0.11 mag (using RR0 stars), 15.00 ± 0.05 mag (using RR1 stars), 14.97 ± 0.11 mag (using SX Phe stars), and 15.00 ± 0.07 mag (using the M<inf>V</inf> -[Fe/H] relation for RRL stars), corresponding to physical distances of 10.00 ± 0.49, 9.99 ± 0.21, 9.84 ± 0.50, and 10.00 ± 0.30 kpc, respectively. Thanks to the first use of difference image analysis on time-series observations of M 68, we are now confident that we have a complete census of the RRL stars in this cluster. © ESO, 2015.
Disciplines :
Space science, astronomy & astrophysics
Author, co-author :
Kains, N.;  Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD, United States, European Southern Observatory, Karl-Schwarzschild Straße 2, Garching bei München, Germany
Arellano Ferro, A.;  Instituto de Astronomía, Universidad Nacional Autónoma de Mexico, Coyoácan, Mexico
Figuera Jaimes, R.;  European Southern Observatory, Karl-Schwarzschild Straße 2, Garching bei München, Germany, SUPA School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, United Kingdom
Bramich, D. M.;  Qatar Environment and Energy Research Institute, Qatar Foundation, PO Box 5825, Doha, Qatar
Skottfelt, J.;  Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, Copenhagen, Denmark, Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5, Copenhagen, Denmark
Jørgensen, U. G.;  Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, Copenhagen, Denmark, Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5, Copenhagen, Denmark
Tsapras, Y.;  Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Goleta, CA, United States, School of Mathematical Sciences, Queen Mary, University of London, Mile End Road, London, United Kingdom
Street, R. A.;  Las Cumbres Observatory Global Telescope Network, 6740 Cortona Drive, Goleta, CA, United States
Browne, P.;  SUPA School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, United Kingdom
Dominik, M.;  SUPA School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, United Kingdom
Horne, K.;  SUPA School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, United Kingdom
Hundertmark, M.;  SUPA School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, United Kingdom
Ipatov, S.;  Qatar Foundation, PO Box 5825, Doha, Qatar
Snodgrass, C.;  Max Planck Institute for Solar System Research, Justus-von-Liebig-Weg 3, Göttingen, Germany
Steele, I. A.;  Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead, Wirral, United Kingdom
Alsubai, K. A.;  Qatar Foundation, PO Box 5825, Doha, Qatar
Bozza, V.;  Dipartimento di Fisica E.R. Caianiello, Università degli Studi di Salerno, via Giovanni Paolo II 132, Fisciano, Italy, Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Italy
Calchi Novati, S.;  Dipartimento di Fisica E.R. Caianiello, Università degli Studi di Salerno, via Giovanni Paolo II 132, Fisciano, Italy, Istituto Internazionale per gli Alti Studi Scientifici (IIASS), via Giuseppe Pellegrino, 19, Vietri Sul Mare Salerno, Italy
Ciceri, S.;  Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, Germany
D'ago, G.;  Dipartimento di Fisica E.R. Caianiello, Università degli Studi di Salerno, via Giovanni Paolo II 132, Fisciano, Italy, Istituto Nazionale di Fisica Nucleare, Sezione di Napoli, Italy
Galianni, P.;  SUPA School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, United Kingdom
Gu, S.-H.;  Yunnan Observatories, Chinese Academy of Sciences, Kunming, China, Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China
Harpsøe, K.;  Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, Copenhagen, Denmark, Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5, Copenhagen, Denmark
Hinse, T. C.;  Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, Copenhagen, Denmark, Korea Astronomy and Space Science Institute, Daejeon, South Korea
Juncher, D.;  Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, Copenhagen, Denmark, Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5, Copenhagen, Denmark
Korhonen, H.;  Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, Copenhagen, Denmark, Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5, Copenhagen, Denmark, Finnish Centre for Astronomy with ESO (FINCA), University of Turku, Väisäläntie 20, Piikkiö, Finland
Mancini, L.;  Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, Germany
Popovas, A.;  Niels Bohr Institute, University of Copenhagen, Juliane Maries vej 30, Copenhagen, Denmark, Centre for Star and Planet Formation, Geological Museum, Øster Voldgade 5, Copenhagen, Denmark
Rabus, M.;  Max Planck Institute for Astronomy, Königstuhl 17, Heidelberg, Germany, Instituto de Astrofísica, Facultad de Física, Pontificia Universidad Católica de Chile, Av. Vicuña Mackenna 4860, Macul, Santiago, Chile
Rahvar, S.;  Department of Physics, Sharif University of Technology, PO Box 11155-9161, Tehran, Iran, Perimeter Institute for Theoretical Physics, 31 Caroline St. N., Waterloo, ON, Canada
Southworth, J.;  Astrophysics Group, Keele University, Staffordshire, United Kingdom
Surdej, Jean  ;  Université de Liège - ULiège > Département d'astrophys., géophysique et océanographie (AGO) > Département d'astrophys., géophysique et océanographie (AGO)
Vilela, C.;  Astrophysics Group, Keele University, Staffordshire, United Kingdom
Wang, X.-B.;  Yunnan Observatories, Chinese Academy of Sciences, Kunming, China, Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming, China
Wertz, O.;  Institut d'Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août 17, Liège, Belgium
More authors (25 more) Less
Language :
English
Title :
A census of variability in globular cluster M 68 (NGC 4590)
Publication date :
2015
Journal title :
Astronomy and Astrophysics
ISSN :
0004-6361
eISSN :
1432-0746
Publisher :
EDP Sciences
Volume :
578
Peer reviewed :
Peer Reviewed verified by ORBi
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