We report secondary eclipse photometry of the hot Jupiter HAT-P-32Ab , taken with Hale/WIRC in H and K _ { S } bands and with Spitzer /IRAC at 3.6 and 4.5 µm .
We carried out adaptive optics imaging of the planet host star HAT-P-32A and its companion HAT-P-32B in the near-IR and the visible .
We clearly resolve the two stars from each other and find a separation of 2 \farcs 923 \pm 0 \farcs 004 and a position angle 110 \fdg 64 \pm 0 \fdg 12 .
We measure the flux ratios of the binary in g ^ { \prime } r ^ { \prime } i ^ { \prime } z ^ { \prime } and H & K _ { S } bands , and determine T _ { \text { eff } } = 3565 \pm 82 K for the companion star , corresponding to an M1.5 dwarf .
We use PHOENIX stellar atmosphere models to correct the dilution of the secondary eclipse depths of the hot Jupiter due to the presence of the M1.5 companion .
We also improve the secondary eclipse photometry by accounting for the non-classical , flux-dependent nonlinearity of the WIRC IR detector in the H band .
We measure planet-to-star flux ratios of 0.090 \pm 0.033 % , 0.178 \pm 0.057 % , 0.364 \pm 0.016 % , and 0.438 \pm 0.020 % in the H , K _ { S } , 3.6 and 4.5 µm bands , respectively .
We compare these with planetary atmospheric models , and find they prefer an atmosphere with a temperature inversion and inefficient heat redistribution .
However , we also find that the data are equally well-described by a blackbody model for the planet with T _ { p } = 2042 \pm 50 K. Finally , we measure a secondary eclipse timing offset of 0.3 \pm 1.3 min from the predicted mid-eclipse time , which constrains e = 0.0072 ^ { +0.0700 } _ { -0.0064 } when combined with RV data and is more consistent with a circular orbit .