  This chapter describes the prospects for detecting the first black holes in
our Universe, with a specific focus on instruments/telescopes that will come
online within the next decade, including e.g. the SKA, WFIRST, EUCLID, JWST,
and large ground-based facilities such as E-ELTs, GMT and TMT. This chapter
focusses on: (1) the indirect detectability of the first generations of stellar
mass black holes through their imprint on various Cosmic Background Radiation
fields including the 21-cm and X-ray backgrounds; (2) direct detectability of
line and continuum emission by more massive black holes (M_BH ~ 1e4-1e6 M_sun)
that formed via channels other than `ordinary' stellar evolution.
