Constraining Black Hole Spin based on the Absence of Lense-Thirring Precession of Megamaser Clumps. (arXiv:2104.05084v2 [astro-ph.HE] UPDATED)

Constraining Black Hole Spin based on the Absence of Lense-Thirring Precession of Megamaser Clumps. (arXiv:2104.05084v2 [astro-ph.HE] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Giner_S/0/1/0/all/0/1">Santiago Giner</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Loeb_A/0/1/0/all/0/1">Abraham Loeb</a>

We make use of the absence of Lense-Thirring precession of the innermost
megamaser clumps around black holes in order to place upper limits on the spin
amplitude of seven black holes at the center of megamaser galaxies: NGC 4258,
NGC 2273, UGC 3789, NGC 3393, NGC 5495, NGC 5765b, and UGC 6093. The
constraints are derived by requiring that the associated precession time-scale
be longer than the age of the megamaser clumps, in order to preserve the
single-plane geometry of the megamasers.

We make use of the absence of Lense-Thirring precession of the innermost
megamaser clumps around black holes in order to place upper limits on the spin
amplitude of seven black holes at the center of megamaser galaxies: NGC 4258,
NGC 2273, UGC 3789, NGC 3393, NGC 5495, NGC 5765b, and UGC 6093. The
constraints are derived by requiring that the associated precession time-scale
be longer than the age of the megamaser clumps, in order to preserve the
single-plane geometry of the megamasers.

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