filaments in the field with a S/N of the order of 10 to $\sim150$ for the most pessimistic model considered here. Some of the brighter filaments can be detected with an integration time of a few minutes with SKA1-mid and a few seconds with SKA2. Therefore, SKA2 will be capable of not only detecting but also mapping a large part of the IGM in these filaments.'
author:
- |
    Robin Kooistra$^{1,2}$, Marta B. Silva$^{2,3}$, Saleem Zaroubi$^{2,4,5}$, Marc A. W. Verheijen$^{2,6}$Elmo Tempel$^{7,8}$ and Kelley M. Hess$^{2,9}$\
    $^1$Kavli IPMU (WPI), UTIAS, The University of Tokyo, Kashiwa, Chiba 277-8583, Japan\
    $^2$Kapteyn Astronomical Institute, University of Groningen, Landleven 12, 9747 AD Groningen, the Netherlands\
    $^3$Institute of Theoretical Astrophysics, University of Oslo,P.O. Box 1029 Blindern, N-0315 Oslo, Norway\
    $^4$Department of Natural Sciences, Open University of Israel, 1 University Road, PO Box 808, Ra’anana 4353701, Israel\
    $^5$Department of Physics, The Technion, Haifa 32000, Israel\
    $^6$Adjunct Faculty, National Centre for Radio Astrophysics, TIFR, Ganeshkhind, Pune 411007, India\
    $^7$Leibniz-Institut für Astrophysik Potsdam (AIP), An der Sternwarte 16, 14482 Potsdam, Germany\
    $^8$Tartu Observatory, University of Tartu, Observatooriumi 1, 61602 Tõravere, Estonia\
    $^9$ASTRON, Netherlands Institute for Radio Astronomy, PO 2, 7990 AA, Dwingeloo, The Netherlands
bibliography:
- 'skafils.bib'
title: Detecting 