  Nowhere is black hole feedback seen in sharper relief than in the Perseus
cluster of galaxies. Owing to a combination of astrophysical and instrumental
challenges, however, it can be difficult to study the black hole accretion that
powers feedback into clusters of galaxies. Recent observations with Hitomi have
resolved the narrow Fe K-alpha line associated with accretion onto the black
hole in NGC 1275 (3C 84), the active galaxy at the center of Perseus. The width
of that line indicates the fluorescing material is located 6-45 pc from the
black hole. Here, we report on a specialized Chandra imaging observation of NGC
1275 that offers a complementary angle. Using a sub-array, sub-pixel event
repositioning, and an X-ray "lucky imaging" technique, Chandra imaging suggests
an upper limit of about 0.3 arc seconds on the size of the Fe K-alpha emission
region, corresponding to 98 pc. Both spectroscopy and direct imaging now point
to an emission region consistent with an extended molecular torus or disk,
potentially available to fuel the black hole. A low X-ray continuum flux was
likely measured from NGC 1275; contemporaneously, radio flaring and record-high
GeV fluxes were measured. This may be an example of the correlation between
X-ray flux dips and jet activity that is observed in other classes of accreting
black holes across the mass scale.
