We combine nulling interferometry at 10 {\mu}m using the MMT and Keck Telescopes with spectroscopy, imaging, and photometry from 3 to 100 {\mu}m using Spitzer to study the debris disk around {\beta} Leo over a broad range of spatial scales, corresponding to radii of 0.1 to ~100 AU. We have also measured the close binary star o Leo with both Keck and MMT interferometers to verify our procedures with these instruments. The {\beta} Leo debris system has a complex structure: 1.) relatively little material within 1 AU; 2.) an inner component with a color temperature of ~600 K, fitted by a dusty ring from about 2 to 3 AU; and 3.) a second component with a color temperature of ~120 K fitted by a broad dusty emission zone extending from about ~5 AU to ~55 AU. Unlike many other A-type stars with debris disks, {\beta} Leo lacks a dominant outer belt near 100 AU.
@article{arxiv.1010.0003,
title = {The Structure of the {\beta} Leonis Debris Disk},
author = {Nathan D. Stock and Kate Y. L. Su and Wilson Liu and Phil M. Hinz and George H. Rieke and Massimo Marengo and Karl R. Stapelfeldt and Dean C. Hines and David E. Trilling},
journal= {arXiv preprint arXiv:1010.0003},
year = {2015}
}