  The presence of black holes (BHs) at the centers of dwarf elliptical galaxies
(dEs) has been argued both theoretically and observationally. Using archival
HST/WFPC2 data, we found the Virgo cluster dwarf elliptical galaxy VCC128 to
harbor a binary nucleus, a feature that is usually interpreted as the
observable signature of a stellar disk orbiting a central massive black hole.
Debattista et al. 2006 estimated its mass M sim 6 10^6 - 5 10^7 Msun. One of
the most robust means of verifying the existence of a BH is radio continuum
and/or X-ray emission, however because of the deficiency of gas in dEs, radio
continuum emission forms the best option here. We have tried to detect the
X-band radio emission coming from the putative black hole in VCC128 when it
accretes gas from the surrounding ISM. While we made a positive 4 sigma
detection of a point source 4.63'' south-west of the binary nucleus, no
statistically significant evidence for emission associated with the nuclei
themselves was detected.
  This implies either that VCC128 has no massive central black hole, which
makes the nature of the binary nucleus hard to explain, or, if it has a central
black hole, that the physical conditions of the ISM (predominantly its density
and temperature) and/or of the surrounding accretion disk do not allow for
efficient gas accretion onto the black hole, making the quiescent black hole
very hard to detect at radio wavelengths.
