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Recent N-body simulations have shown that the assembly history of galactichalos depend on the density of large-scale environment. It implies that thegalaxy properties like age and size of bulge may also vary with the surroundinglarge-scale structures, which are characterized by the tidal shear as well asthe density. By using a sample of 15,882 well-resolved nearby galaxies from theTully Catalog and the real space tidal field reconstructed from the 2MassRedshift Survey (2MRS), we investigate the dependence of galaxy morphologicaltype on the shear of large-scale environment where the galaxies are embedded.We first calculate the large scale dimensionless overdensities (d) and thelarge-scale ellipticities (e) of the regions where the Tully galaxies arelocated and classify the Tully galaxies according to their morphological typesand create subsamples selected at similar value of d but span different rangesin e. We calculate the mean ellipticity, <e>, averaged over each subsample andfind a signal of variation of <e> with galaxy morphological type: For the caseof 0.5<=d<=1.0, the ellipticals are found to be preferentially located in theregions with low ellipticity. For the case of -0.3<=d<=0.1, the latest-typespirals are found to be preferentially located in the regions with highellipticity. The null hypothesis that the mean ellipticities of the regionswhere the ellipticals and the latest type spirals are located are same as theglobal mean ellipticity averaged over all types is rejected at 3 sigma levelwhen -0.3<=d<=0.1. Yet, no signal of galaxy-shear correlation is found in thehighly overdense/underdense regions. The observed trend suggests that theformation epochs of galactic halos might be a function not only of halo massand large-scale density but also of large-scale shear.

The Variation of Galaxy Morphological Type with the Shear of Environment