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Nowhere is black hole feedback seen in sharper relief than in the Perseuscluster of galaxies. Owing to a combination of astrophysical and instrumentalchallenges, however, it can be difficult to study the black hole accretion thatpowers feedback into clusters of galaxies. Recent observations with Hitomi haveresolved the narrow Fe K-alpha line associated with accretion onto the blackhole in NGC 1275 (3C 84), the active galaxy at the center of Perseus. The widthof that line indicates the fluorescing material is located 6-45 pc from theblack hole. Here, we report on a specialized Chandra imaging observation of NGC1275 that offers a complementary angle. Using a sub-array, sub-pixel eventrepositioning, and an X-ray "lucky imaging" technique, Chandra imaging suggestsan upper limit of about 0.3 arc seconds on the size of the Fe K-alpha emissionregion, corresponding to 98 pc. Both spectroscopy and direct imaging now pointto an emission region consistent with an extended molecular torus or disk,potentially available to fuel the black hole. A low X-ray continuum flux waslikely measured from NGC 1275; contemporaneously, radio flaring and record-highGeV fluxes were measured. This may be an example of the correlation betweenX-ray flux dips and jet activity that is observed in other classes of accretingblack holes across the mass scale.

Chandra Imaging of the Outer Accretion Flow onto the Black Hole at the Center of the Perseus Cluster