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The Hubble Space Telescope Advanced Camera for Surveys Coma Cluster Survey. I. Survey Objectives and Design*

, , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , , and

© 2008. The American Astronomical Society. All rights reserved. Printed in U.S.A.
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Author affiliations

1 Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1LD, UK

2 Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218

3 Dominion Astrophysical Observatory, Herzberg Institute of Astrophysics, National Research Council of Canada, 5071 West Saanich Road, Victoria, BC V9E 2E7, Canada

4 Instituto de Astrofísica de Canarias, C/Vía Lactea s/n, 38200 La Laguna, Tenerife, Spain

5 Department of Physics, Rochester Institute of Technology, 85 Lomb Memorial Drive, Rochester, NY 14623

6 Department of Physics, Engineering Physics and Astronomy, Queen's University, Kingston, ON K7L 3N6, Canada

7 School of Physics and Astronomy, Cardiff University, The Parade, Cardiff CF24 3YB, UK

8 Max-Planck-Institut für Extraterrestrische Physik, Giessenbachstrasse, D-85748 Garching, Germany

9 Universitäts-Sternwarte München, Scheinerstrasse 1, D-81679 München, Germany

10 Centre for Astrophysics and Supercomputing, Swinburne University of Technology, Hawthorn, VIC 3122, Australia

11 Department of Astronomy, University of Florida, P.O. Box 112055, Gainesville, FL 32611

12 Department of Physics and Astronomy, Johns Hopkins University, 3400 North Charles Street, Baltimore, MD 21218

13 Laboratory for X-Ray Astrophysics, NASA Goddard Space Flight Center, Code 662.0, Greenbelt, MD 20771

14 Departamento de Física Teórica, Universidad Autónoma de Madrid, Carretera de Colmenar Viejo km 15.600, 28049 Madrid, Spain

15 Department of Physics and Astronomy, University of Waterloo, 200 University Avenue West, Waterloo, ON N2L 3G1, Canada

16 Astrophysics Group, H. H. Wills Physics Laboratory, University of Bristol, Tyndall Avenue, Bristol BS8 1TL, UK

17 Department of Astronomy, University of Texas at Austin, 1 University Station C1400, Austin, TX 78712

18 Subaru Telescope, National Astronomical Observatory of Japan, 650 North A'ohoku Place, Hilo, HI 96720

19 Leo Goldberg Fellow, National Optical Astronomy Observatory, 950 North Cherry Avenue, Tucson, AZ 85719

20 Department of Physics, University of Durham, South Road, Durham DH1 3LE, UK

21 Department of Physics and Astronomy, San Francisco State University, San Francisco, CA 94132-4163

22 Gemini Observatory, Casilla 603, La Serena, Chile

23 Jansky Fellow of the National Radio Astronomy Observatory. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc

24 Department of Astronomy, University of Tokyo, 7-3-1 Hongo, Bunkyo, Tokyo 113-0033, Japan

25 Kapteyn Astronomical Institute, University of Groningen, P.O. Box 800, 9700 AV Groningen, The Netherlands

26 INAF-Osservatorio Astronomico di Padova, Vicolo dell'Osservatorio 5, Padova I-35122, Italy

27 Institute of Astronomy, Madingley Road, Cambridge CB3 0HA, UK

28 Institute for Astronomy, University of Hawaii, 2680 Woodlawn Drive, Honolulu, HI 96822

Dates

Received 2007 September 1
Accepted 2008 January 21

Citation

David Carter et al 2008 ApJS 176 424

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DOI

https://doi.org/10.1086/533439

Keywords

galaxies: clusters: individual (Abell 1656) ; galaxies: fundamental parameters; galaxies: luminosity function, mass function; galaxies: photometry; galaxies: stellar content; galaxies: structure

Journal RSS feed

0067-0049/176/2/424

Abstract

We describe the HST ACS Coma Cluster Treasury survey, a deep two-passband imaging survey of one of the nearest rich clusters of galaxies, the Coma Cluster (Abell 1656). The survey was designed to cover an area of 740 arcmin2 in regions of different density of both galaxies and intergalactic medium within the cluster. The ACS failure of 2007 January 27 leaves the survey 28% complete, with 21 ACS pointings (230 arcmin2) complete, and partial data for a further four pointings (44 arcmin2). The predicted survey depth for 10 σ detections for optimal photometry of point sources is g' = 27.6 in the F475W filter and IC = 26.8 mag in F814 (AB magnitudes). Initial simulations with artificially injected point sources show 90% recovered at magnitude limits of g' = 27.55 and IC = 26.65. For extended sources, the predicted 10 σ limits for a 1 arcsec2 region are g' = 25.8 mag arcsec−2 and IC = 25.0 mag arcsec−2. We highlight several motivating science goals of the survey, including study of the faint end of the cluster galaxy luminosity function, structural parameters of dwarf galaxies, stellar populations and their effect on colors and color gradients, evolution of morphological components in a dense environment, the nature of ultracompact dwarf galaxies, and globular cluster populations of cluster galaxies of a range of luminosities and types. This survey will also provide a local rich cluster benchmark for various well-known global scaling relations and explore new relations pertaining to the nuclear properties of galaxies.

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Footnotes

  • * 

    Based on observations with the NASA/ESA Hubble Space Telescope obtained at the Space Telescope Science Institute, which is operated by the association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. These observations are associated with program GO10861.

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