Drawing on the descriptive representation literature, we argue that religious identity is a social identity similar to gender or race, which leads a person to feel represented by someone who shares their religious identity. We argue that religious identity motivates approbation for public officials that is distinct from partisanship. We find that constituents who share the religious identity of their congressional representatives are significantly more likely to approve of their representative's performance in office. In addition, those who share a religious identity with President Obama are more trusting of him; particularly among those for whom religion is important. Finally, we find that shared religious identity moderates the relationship between partisanship and trust in the President. All else equal, Republicans who share a religious identity with President Obama are 500% more likely to trust him than a Republican who does not.

We investigate the evolution of the Hα equivalent width, EW(Hα), with redshift and its dependence on stellar mass, using the first data from the 3D-HST survey, a large spectroscopic Treasury program with the HST-WFC3. Combining our Hα measurements of 854 galaxies at 0.8<z<1.5 with those of ground based surveys at lower and higher redshift, we can consistently determine the evolution of the EW(Hα) distribution from z=0 to z=2.2. We find that at all masses the characteristic EW(Hα) is decreasing towards the present epoch, and that at each redshift the EW(Hα) is lower for high-mass galaxies. We find EW(Hα) ~ (1+z)1.8 with little mass dependence. Qualitatively, this measurement is a model-independent confirmation of the evolution of star forming galaxies with redshift. A quantitative conversion of EW(Hα) to sSFR (specific star-formation rate) is model dependent, because of differential reddening corrections between the continuum and the Balmer lines. The observed EW(Hα) can be reproduced with the characteristic evolutionary history for galaxies, whose star formation rises with cosmic time to z ~ 2.5 and then decreases to z = 0. This implies that EW(Hα) rises to 400 Å at z = 8. The sSFR evolves faster than EW(Hα), as the mass-to-light ratio also evolves with redshift. We find that the sSFR evolves as (1+z)3.2, nearly independent of mass, consistent with previous reddening insensitive estimates. We confirm previous results that the observed slope of the sSFR-z relation is steeper than the one predicted by models, but models and observations agree in finding little mass dependence.

We demonstrate that quantifying the intrinsic variability of quasars by fitting individual structure function data pairs with a 2-parameter power law model separates quasars from contaminating variable and non-variable point sources with a completeness of 93% and a purity of 99%. This approach can be used to select quasar samples in surveys like that being performed by Pan-STARRS1, where the usual color selection of quasars is not possible due to a filter system that is too red.

Molecular order and morphological order are two characteristics of feather fiber that make it unique. The fiber is highly microcrystalline and is very durable, i.e., resistant to both mechanical and thermal stress. Feather structure at the microscopic level is a complicated mixture of straight and branched fibers held together by a central fiber to form specific macroscopic structures. The proper design of processes to incorporate feathers into composite products 1) preserves the fiber's molecular properties and 2) alters its micro-/macroscopic morphology to conform to existing composite process requirements.