  The rare intermittent pulsars pose some of the most challenging questions
surrounding the pulsar emission mechanism, but typically have relatively
minimal low-frequency ($\lesssim$ 300 MHz) coverage. We present the first
low-frequency detection of the intermittent pulsar J1107-5907 with the
Murchison Widefield Array (MWA) at 154 MHz and the simultaneous detection from
the recently upgraded Molonglo Observatory Synthesis Telescope (UTMOST) at 835
MHz, as part of an on-going observing campaign. During a 30-minute simultaneous
observation, we detected the pulsar in its bright emission state for
approximately 15 minutes, where 86 and 283 pulses were detected above a
signal-to-noise threshold of 6 with the MWA and UTMOST, respectively. Of the
detected pulses, 51 had counterparts at both frequencies and exhibited steep
spectral indices for both the bright main pulse component and the precursor
component. We find that the bright state pulse energy distribution is best
parameterised by a log-normal distribution at both frequencies, contrary to
previous results which suggested a power law distribution. Further
low-frequency observations are required in order to explore in detail aspects
such as pulse-to-pulse variability, intensity modulations and to better
constrain the signal propagation effects due to the interstellar medium and
intermittency characteristics at these frequencies. The spectral index,
extended profile emission covering a large fraction of pulse longitude, and the
broadband intermittency of PSR J1107-5907 suggests that future low-frequency
pulsar searches, for instance those planned with SKA-Low, will be in an
excellent position to find and investigate new pulsars of this type.
