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We present the first systematic investigation of the existence, spatialdistribution, and kinematics of warm ionized gas as traced by the [O II] 3727AAemission line in 74 of the most massive galaxies in the local Universe. All ofour galaxies have deep integral field spectroscopy from the volume- andmagnitude-limited MASSIVE survey of early-type galaxies with stellar masslog(M_*/M_sun) > 11.5 (M_K < -25.3 mag) and distance D < 108 Mpc. Of the 74galaxies in our sample, we detect warm ionized gas in 28, which yields a globaldetection fraction of 38\pm6% down to a typical [O II] equivalent width limitof 2AA. MASSIVE fast rotators are more likely to have gas than MASSIVE slowrotators with detection fractions of 80\pm10% and 28\pm6%, respectively. Thespatial extents span a wide range of radii (0.6 - 18.2 kpc; 0.1 - 4R_e), andthe gas morphologies are diverse, with 17/28 = 61\pm9% being centrallyconcentrated, 8/28 = 29\pm9% exhibiting clear rotation out to several kpc, and3/28 = 11\pm6% being extended but patchy. Three out of four fast rotators showkinematic alignment between the stars and gas, whereas the two slow rotatorswith robust kinematic measurements available exhibit kinematic misalignment.Our inferred warm ionized gas masses are roughly ~10^5M_sun. The emission lineratios and radial equivalent width profiles are generally consistent withexcitation of the gas by the old underlying stellar population. We exploredifferent gas origin scenarios for MASSIVE galaxies and find that a variety ofphysical processes are likely at play, including internal gas recycling,cooling out of the hot gaseous halo, and gas acquired via mergers.

The MASSIVE Survey VI: The Spatial Distribution and Kinematics of Warm Ionized Gas in the Most Massive Local Early-type Galaxies