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We present UV through NIR broad-band photometry, and optical and NIRspectroscopy of Type Iax supernova 2012Z. The data set consists of both earlyand late-time observations, including the first late phase NIR spectrumobtained for a spectroscopically classified SN Iax. Simple model calculationsof its bolometric light curve suggest SN 2012Z produced ~0.3 M_sun of (56)Ni,ejected about a Chandrasekhar mass of material, and had an explosion energy of~10^51 erg, making it one of the brightest and most energetic SN Iax yetobserved. The late phase NIR spectrum of SN 2012Z is found to broadly resemblesimilar epoch spectra of normal SNe Ia; however, like other SNe Iax,corresponding visual-wavelength spectra differ substantially compared to allsupernova types. Constraints from the distribution of IMEs, e.g. silicon andmagnesium, indicate that the outer ejecta did not experience significant mixingduring or after burning, and the late phase NIR line profiles suggests most ofthe (56)Ni is produced during high density burning. The various observationalproperties of SN 2012Z are found to be consistent with the theoreticalexpectations of a Chandrasekhar mass white dwarf progenitor that experiences apulsational delayed detonation, which produced several tenths of a solar massof (56)Ni during the deflagration burning phase and little (or no) (56)Niduring the detonation phase. Within this scenario only a moderate amount ofRayleigh-Taylor mixing occurs both during the deflagration and fallback phaseof the pulsation, and the layered structure of the IMEs is a product of thesubsequent denotation phase. The fact that the SNe Iax population does notfollow a tight brightness-decline relation similar to SNe Ia can then beunderstood in the framework of variable amounts of mixing during pulsationalrebound and variable amounts of (56)Ni production during the early subsonicphase of expansion.

Comprehensive Observations of the Bright and Energetic Type Iax SN 2012Z: Interpretation as a Chandrasekhar Mass White Dwarf Explosion