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We analyze all existing secondary eclipse time series spectroscopy of hotJupiter HD189733b acquired with the now defunct Spitzer/IRS instrument. Wedescribe the novel approaches we develop to remove the systematic effects andextract accurate secondary eclipse depths as a function of wavelength in orderto construct the emission spectrum of the exoplanet. We compare our results toa previous study by Grillmair et al. that did not examine all data setsavailable to us. We are able to confirm the detection of a water feature near6{\mu}m claimed by Grillmair et al. We compare the planetary emission spectrumto three model families -- based on isothermal atmosphere, gray atmosphere, andtwo realizations of the complex radiative transfer model by Burrows et al.,adopted in Grillmair et al.'s study. While we are able to reject the simpleisothermal and gray models based on the data at the 97% level just from the IRSdata, these rejections hinge on eclipses measured within relatively narrowwavelength range, between 5.5 and 7{\mu}m. This underscores the need forobservational studies with broad wavelength coverage and high spectralresolution, in order to obtain robust information on exoplanet atmospheres.

Updated Spitzer Emission Spectroscopy of Bright Transiting Hot Jupiter HD189733b