The M 4 Core Project with HST: I. Overview and first epoch

Authors

  • L.R. Bedin,

    Corresponding author
    1. Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
    • Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy

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  • J. Anderson,

    1. Space Telescope Science Institute, 3800 San Martin Drive, Baltimore, MD 21218, USA
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  • D.C. Heggie,

    1. School of Mathematics and Maxwell Institute for Mathematical Sciences, University of Edinburgh, Kings Buildings, Edinburgh, EH9-3JZ, UK
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  • G. Piotto,

    1. Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
    2. Dipartimento di Fisica e Astronomia “Galileo Galilei”, Univ. di Padova, Vicolo dell'Osservatorio 3, Padova, I-35122, Italy
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  • A.P. Milone,

    1. Instituto de Astrof`ısica de Canarias, La Laguna, Tenerife, Canary Islands, E-38200, Spain
    2. Department of Astrophysics, University of La Laguna, La Laguna, Tenerife, Canary Islands, E-38200, Spain
    3. Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston, ACT, 2611, Australia
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  • M. Giersz,

    1. Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, ul. Bartycka 18, 00-716, Warsaw, Poland
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  • V. Nascimbeni,

    1. Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
    2. Dipartimento di Fisica e Astronomia “Galileo Galilei”, Univ. di Padova, Vicolo dell'Osservatorio 3, Padova, I-35122, Italy
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  • A. Bellini,

    1. Space Telescope Science Institute, 3800 San Martin Drive, Baltimore, MD 21218, USA
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  • R.M. Rich,

    1. Department of Physics and Astronomy, University of California, Los Angeles, CA 90095, USA
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  • M. van den Berg,

    1. Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Science Park 904, 1098 XH Amsterdam, The Netherlands
    2. Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, 02138 MA, USA
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  • D. Pooley,

    1. School of Mathematics and Maxwell Institute for Mathematical Sciences, University of Edinburgh, Kings Buildings, Edinburgh, EH9-3JZ, UK
    2. Department of Physics, Sam Houston State University, Huntsville, TX 77341, USA
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  • K. Brogaard,

    1. Department of Physics and Astronomy, Aarhus University, Ny Munkegade, 8000 Aarhus C, Denmark
    2. Department of Physics and Astronomy, University of Victoria, PO Box 3055, Victoria, B.C., V8W 3P6, Canada
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  • S. Ortolani,

    1. Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
    2. Dipartimento di Fisica e Astronomia “Galileo Galilei”, Univ. di Padova, Vicolo dell'Osservatorio 3, Padova, I-35122, Italy
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  • L. Malavolta,

    1. Istituto Nazionale di Astrofisica – Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova, I-35122, Italy
    2. Dipartimento di Fisica e Astronomia “Galileo Galilei”, Univ. di Padova, Vicolo dell'Osservatorio 3, Padova, I-35122, Italy
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  • L. Ubeda,

    1. Space Telescope Science Institute, 3800 San Martin Drive, Baltimore, MD 21218, USA
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  • A.F. Marino

    1. Research School of Astronomy and Astrophysics, The Australian National University, Cotter Road, Weston, ACT, 2611, Australia
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  • Based on observations collected with the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope Science Institute, which is operated by AURA, Inc., under NASA contract NAS 5-26555, under large program GO-12911.

Abstract

We present an overview of the ongoing Hubble Space Telescope large program GO-12911. The program is focused on the core of M 4, the nearest Galactic globular cluster, and the observations are designed to constrain the number of binaries with massive companions (black holes, neutron stars, or white dwarfs) by measuring the “wobble” of the luminous (mainsequence) companion around the center of mass of the pair, with an astrometric precision of ∼50 µas. The high spatial resolution and stable medium-band PSFs of WFC3/UVIS will make these measurements possible. In this work we describe (i) the motivation behind this study, (ii) our observing strategy, (iii) the many other investigations enabled by this unique data set, and which of those our team is conducting, and (iv) a preliminary reduction of the first-epoch dataset collected on 2012 October 10. (© 2013 WILEY-VCH Verlag GmbH & Co. KGaA, Weinheim)

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