Photometric data from the literature are combined with triaxial mass models to derive the variation in the intrinsic shapes of the light distribution of elliptical galaxies NGC 720, 2768 and 3605. The inferred shape variation is given by a Bayesian probability distribution, assuming a uniform prior. The likelihood of obtaining the data is calculated by using an ensemble of triaxial models. We apply the method to infer the shape variation of a galaxy, using the ellipticities and the difference in the position angles at two suitably chosen points from the profiles of the photometric data. The best‐constrained shape parameters are found to be the short‐to‐long axial ratios at small and large radii, and the absolute values of the triaxiality difference between these radii. The elliptical galaxies of our present investigation are very flat, with ellipticity typically around 0.3 or more. We find that the expectation values of the short‐to‐long axial ratio of these galaxies are around 0.5.

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We determine the orientations of the light distribution of individual elliptical galaxies by combining the profiles of photometric data from the literature with triaxial models. The orientation is given by a Bayesian probability distribution.The likelihood of obtaining the data from a model is a function of the parameters describing the intrinsic shape and the orientation. Integrating the likelihood over the shape parameters, we obtain the estimates of the orientation. We find that the position angle difference between the two suitably chosen points from the profiles of the photometric data plays a key role in constraining the orientation of the galaxy. We apply the methodology to a sample of ten galaxies. The alignment of the intrinsic principle axes of the NGC 3379, 4486 and NGC 5638 are studied.

Determination of the orientation of the elliptical galaxies is an important problem. We determine the orientation of the light distribution of individual elliptical galaxies by combining the profiles of photometric data from the literature with triaxial models. The likelihood of obtaining the data from a model is a function of the parameters describing the intrinsic shape and the orientation. Integrating the likelihood over the shape parameters, we obtain the estimates of the orientation. Apply the methodology to determine the orientation of the galaxy NGC 741.

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