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tokens: in the vicinity. Details of the array configurations are given in Table 2 . Observations were reduced following standard procedures in Miriad (Sault et al. 1995 ), with the flux density scale set by observations of calibrators PKS 1934−638 and/or PKS 0823−500. Initially, observations were made covering the nominal position of the 3FGL source, and the positions of radio sources cataloged by Schinzel et al. ( 2017 ) and candidate X-ray sources. Observations differed in length, hour-angle coverage, angular resolution, and sensitivity to extended radio emission in the vicinity, resulting in a heterogeneous data set. Schinzel et al. ( 2017 ), who observed with the ATCA in the relatively compact H168 and H214 array configurations, detected four sources within the 3 σ error region around 4FGL J1405.1−6119, all of which were brighter than 15 mJy, and are resolved out on longer ATCA baselines. Schinzel et al. ( 2017 ) also list a further 60 objects in the field detected outside the 3 σ region, which appear to be associated with the H ii region cataloged by Caswell Haynes ( 1987 ) at ( l , b ) = (311.627, +0.27). Observations of the candidate X-ray sources in more extended ATCA array configurations revealed the fainter (∼2 mJy), variable radio counterpart. The final observations of the series were conducted as targeted observations, with the phase calibrator PKS 1420−679 used throughout. 3.4. Near-infrared Observations and Analysis We observed the candidate near-IR counterpart to 4FGL J1405.1−6119 (2MASS J14051441−6118282, allWISE J140514.40−611827.7; Landi et al. 2017 ) with FLAMINGOS-2 (Eikenberry et al. 2004 ) on Gemini South on 2018 June 7 through Program ID GS-2018A-Q-412. We used the R3K grism and a 4 pixel slit, giving a resolution of R ∼ 1800 across the K -band. The target was observed with 10 separate 120 s exposures in a standard ABBA nod, giving 1200 s of exposure time total. We also observed the nearby A0V star HD 119942 as a telluric standard immediately before our science observations. The data were reduced using standard near-IR procedures, with optimal extraction of the spectra from subtracted, flat-fielded nodded pairs. The final combined spectrum has a signal-to-noise of about 140 per resolution element in the continuum. After interpolating over the intrinsic Br γ feature in the telluric standard, we corrected the 4FGL J1405.1−6119 spectrum for telluric absorption by scaling the telluric spectrum to minimize the residuals in the regions of strong telluric lines. 4. Results 4.1. Gamma-Ray Results The power spectra of the light curves of all 3033 3FGL and 5523 FL8Y sources were examined for indications of periodic modulation that could arise from previously unknown binary systems. For candidate new binaries our usual threshold for further investigation has been for a source to have a peak power ≥18× mean power level (FAP 5 × 10 −4 ) and for the period not to coincide with a known artifact. We also exclude very long periods that are