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We have conducted a study of extra-planar diffuse ionized gas using the firstyear data from the MaNGA IFU survey. We have stacked spectra from 49 edge-on,late-type galaxies as a function of distance from the midplane of the galaxy.With this technique we can detect the bright emission lines Halpha, Hbeta,[OII]3726, 3729, [OIII]5007, [NII]6549, 6584, and [SII]6717, 6731 out to about4 kpc above the midplane. With 16 galaxies we can extend this analysis out toabout 9 kpc, i.e. a distance of ~2R_e, vertically from the midplane. In thehalo, the surface brightnesses of the [OII] and Halpha emission lines arecomparable, unlike in the disk where Halpha dominates. When we split the sampleby specific star formation rate, concentration index, and stellar mass, eachsubsample's emission line surface brightness profiles and ratios differ,indicating that extra-planar gas properties can vary. The emission line surfacebrightnesses of the gas around high specific star formation rate galaxies arehigher at all distances, and the line ratios are closer to ratioscharacteristic of HII regions compared with low specific star formation rategalaxies. The less concentrated and lower stellar mass samples exhibit lineratios that are more like HII regions at larger distances than their moreconcentrated and higher stellar mass counterparts. The largest differencebetween different subsamples occurs when the galaxies are split by stellarmass. We additionally infer that gas far from the midplane in more massivegalaxies has the highest temperatures and steepest radial temperature gradientsbased on their [NII]/Halpha and [OII]/Halpha ratios between the disk and thehalo.

SDSS IV MaNGA: Deep observations of extra-planar, diffuse ionized gas around late-type galaxies from stacked IFU spectra