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A SINFONI integral field spectroscopy survey for galaxy counterparts to damped Lyman α systems – III. Three additional detections

Authors

  • Céline Péroux,

    Corresponding author
    1. Laboratoire d’Astrophysique de Marseille, OAMP, Université Aix-Marseille & CNRS, 38 rue Frédéric Joliot Curie, 13388 Marseille Cedex 13, France
      E-mail: celine.peroux@gmail.com
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  • Nicolas Bouché,

    Corresponding author
    1. Department of Physics, University of California, Santa Barbara, CA 93106, USA
    2. CNRS, Institut de Recherche en Astrophysique et Planétologie [IRAP] de Toulouse, 14 Avenue E. Belin, F-31400 Toulouse, France
    3. Université de Toulouse, UPS-OMP, IRAP, F-31400 Toulouse, France
      Marie Curie fellow.
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  • Varsha P. Kulkarni,

    1. Department of Physics and Astronomy, University of South Carolina, Columbia, SC 29208, USA
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  • Donald G. York,

    1. Department of Astronomy and Astrophysics and The Enrico Fermi Institute, University of Chicago, 5640 S. Ellis Ave, Chicago, IL 60637, USA
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  • Giovanni Vladilo

    1. Osservatorio Astronomico di Trieste – INAF, Via Tiepolo 11, 34143 Trieste, Italy
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  • Based on observations collected during programmes ESO 83.A-0699 and 85.A-0708 at the European Southern Observatory with SINFONI on the 8.2-m YEPUN telescope operated at the Paranal Observatory, Chile.

E-mail: celine.peroux@gmail.com

Marie Curie fellow.

ABSTRACT

We report three additional Spectrograph for Integral Field Observations in the Near Infrared (SINFONI) detections of Hα emission line from quasar absorbers, two of which are new identifications. These were targeted among a sample of systems with inline image and metallicities measured from high-resolution spectroscopy. The detected galaxies are at impact parameters ranging from 6 to 12 kpc from the quasar’s line of sight. We derive star formation rates (SFRs) of a few M yr−1 for the two absorbers at zabs∼ 1 and SFR = 17 M yr−1 for the damped Lyman α system (DLA) at zabs∼ 2. These three detections are found among a sample of 16 DLAs and sub-DLAs (five at zabs∼ 1 and seven at zabs∼ 2). For the remaining undetected galaxies, we derive flux limits corresponding to SFR < 0.1–11.0 M yr−1 depending on redshift of the absorber and depth of the data. When combined with previous results from our survey for galaxy counterparts to H i-selected absorbers, we find a higher probability of detecting systems with higher metallicity as traced by dust-free [Zn/H] metallicity. We also report a higher detection rate with SINFONI for host galaxies at zabs∼ 1 than for systems at zabs∼ 2. Using the [N ii]/Hα ratio, we can thus compare absorption and emission metallicities in the same high-redshift objects, more than doubling the number of systems for which such measures are possible.

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