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Reionization and the Cosmic Dawn with the Square Kilometre Array

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Abstract

The Square Kilometre Array (SKA) will have a low frequency component (SKA-low) which has as one of its main science goals the study of the redshifted 21 cm line from the earliest phases of star and galaxy formation in the Universe. This 21 cm signal provides a new and unique window both on the time of the formation of the first stars and accreting black holes and the subsequent period of substantial ionization of the intergalactic medium. The signal will teach us fundamental new things about the earliest phases of structure formation, cosmology and even has the potential to lead to the discovery of new physical phenomena. Here we present a white paper with an overview of the science questions that SKA-low can address, how we plan to tackle these questions and what this implies for the basic design of the telescope.

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Notes

  1. We will use both names throughoutcthe White Paper, mostly indicating the very low frequency (≲ 250 MHz) part of the SKA array interesting for HI studies at redshift z ≳ 5.

  2. These baselines exceed the imprint of the station beam on the ionosphere and larger beam-sizes therefore require longer baselines, somewhat counterintuitively.

  3. This first draft of this white paper was written during a three day workshop at the Oskar Klein Centre in Stockholm, January 18–20, 2012.

  4. Sometimes this period is called the Late Dark Ages but this is confusing as the Universe at those times did contain sources of radiation and therefore was no longer truly dark.

  5. We will use cMpc for comoving Mpc and pMpc for proper Mpc; without any prefix Mpc means cMpc.

  6. The physical distance of a deviation of the wave-vector from the straight line it would follow without the ionosphere, is smaller than the dominant scales that cause phase distortions of the plane wave.

  7. This section is based on a memo written by two of the co-authors (LVEK and BS) as part of the SKA Science Working Group to inform the SKA Project Office on the optimal frequency range(s) for high-redshift HI studies.

  8. We note that these redshifts are not as precisely determined as quoted here from either observations or theory, but we would like to be precise in corresponding redshifts and frequencies.

  9. We note that this assumes that the collecting area (or \(A_{\mathrm eff}\) per antenna) that can be purchased per dollar is a function of \(\nu _{\mathrm opt}\). We suspect, however, that it will not be a strong function and that \(A_{\mathrm eff}\) goes up with \(\nu _{\mathrm opt}\) going down, for fixed costs, because dipoles do not linearly grow in cost with their effective collecting area. Hence, one might consider the extreme case where dipole size is not a cost factor. In that case \(A_{\mathrm eff}\) grows with \((\nu /\nu _{\mathrm opt})^{-2}\) and offsets the loss in collecting area due to sparseness at frequencies greater than \(\nu _{\mathrm opt}\). In that case, choosing a very low value of \(\nu _{\mathrm opt}\) makes more sense, but could be limited by other factors such as land use, etc. A final choice of \(\nu _{\mathrm opt}\) should therefore factor this cost in.

  10. This equation is not given in this form in [148], but has been derived using the same method as outlined there. In this form is gives the important scaling relations with array parameters useful to understand power-spectrum measurements.

  11. We note that somewhat larger beams might be ok (station size perhaps up to 70 m) with multi-beaming and uv-plane dithering but this will require careful thinking about how to connect these multi-beamed data into a single power spectrum in overlapping areas. It can best be done in the uv-plane by combining the visibilities brought to a common phase-center. Also a hybrid system where only a sub-set of receiver elements inside stations are beam-formed and correlated could be considered.

  12. We recognize that more details need to be worked out especially on costs and calibratability of the array, but as far as we are aware this array design does not have major show stoppers and could be used as a starting point for a more detailed design.

  13. These ranges have been argued for as well in the Memo “Is There an Optimum Frequency Range for SKA1-lo? Question 1 of the Magnicent Memoranda II” by Huynh et al.

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Authors and Affiliations

  1. Department of Astronomy & Oskar Klein Center, Stockholm University, Stockholm, Sweden

    Garrelt Mellema, Kanan K. Datta & Hannes Jensen

  2. Kapteyn Astronomical Institute, University of Groningen, Groningen, The Netherlands

    Léon V. E. Koopmans, Soobash Daiboo, A. G. de Bruyn, Ronniy Joseph, André R. Offringa, Harish Vedantham & Saleem Zaroubi

  3. Department of Physics and Astronomy, University College London, London, UK

    Filipe A. Abdalla

  4. Center for Astrophysics, Harvard University, Cambridge, USA

    Gianni Bernardi

  5. Max Plank Institute for Astrophysics, Garching, Germany

    Benedetta Ciardi

  6. ASTRON, Dwingeloo, The Netherlands

    Vibor Jelić, Panos Labroupoulos, V. N. Pandey & Sarod Yatawatta

  7. Department of Astronomy, Radboud University, Nijmegen, Netherlands

    Heino Falcke

  8. Scuola Normale Superiore, Pisa, Italy

    Andrea Ferrara & Andrei Mesinger

  9. Department of Physics and Astronomy, Sussex University, Sussex, UK

    Ilian T. Iliev

  10. Department of Physics and Oskar Klein Center, Stockholm University, Stockholm, Sweden

    Fabio Iocco

  11. Institute for Astronomy, University of Edinburgh, Edinburgh, UK

    Avery Meiksin

  12. Department of Physics, Imperial College, London, UK

    Jonathan R. Pritchard

  13. CENTRA, Instituto Superior Tecnico, Technical University of Lisbon, Lisbon, Portugal

    Mario G. Santos

  14. Faculty of Physics, Bielefeld University, Bielefeld, Germany

    Dominik J. Schwarz

  15. Observatoire de Paris, Paris, France

    Benoit Semelin

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  1. Garrelt Mellema
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Correspondence to Garrelt Mellema.

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Mellema, G., Koopmans, L.V.E., Abdalla, F.A. et al. Reionization and the Cosmic Dawn with the Square Kilometre Array. Exp Astron 36, 235–318 (2013). https://doi.org/10.1007/s10686-013-9334-5

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