Those who heard it first: The political implications of the sermon on the mount to Jesus’ Jewish audience

This dissertation examines the Sermon on the Mount (in the Gospel of Matthew) from the perspective of politics and peace. It investigates not what Jesus meant, but what his audience heard and were likely to have understood. It does this in order to ascertain the novelty or otherwise of Jesus’ teachings on peace with regard to Jewish thought and political understandings of his time. His audience was primarily Jewish, and the political implications they drew from Jesus’ teachings would have been influenced by established Jewish thought on ethics and governance. This dissertation researches specifically this: how would Jesus’ Jewish listeners have interpreted the peace sayings of the Sermon on the Mount? This dissertation finds that the Jewish intellectual framework within which Jesus’ first audience heard the Sermon on the Mount contained many specific sayings found in Pirkei Avot, and also a history of practice of non-violent action found in Jewish tradition, and that the oral law and the Sermon on the Mount both reflect Jewish ethical ideologies of non-violent resistance. This dissertation argues that, in the Sermon on the Mount, a very Jewish Jesus – a man true to the religio-political views of his day – reaffirms a Jewish ethical form of non-violent resistance. The most important evidence available is the Gospel of Matthew itself, Jewish ethical writings such as Pirkei Avot, other Mishna writings, and writings on the lex talionis. The evidence points to an audience that would have perceived Jesus as teaching non-violence in a context of resistance rather than completely passive submission. The overall finding of this dissertation will be that the writer of Matthew depicts a Jesus who, in style, form, and content, builds on a Jewish ethical foundation to promote non-violent assertion of equality and human dignity in the widely known and oft-cited Sermon on the Mount

Planetary camera observations of the central parsec of M32

Analysis of V band HST Planetary Camera images of the elliptical galaxy M32 shows that its nucleus is extremely dense and remains unresolved at even the HST diffraction limit. A combined approach of image deconvolution and model fitting is used to investigate the starlight distribution into limiting radii of 0".04 (0.14 pc at 700 kpc). The logarithmic slope of the brightness profile smoothly flattens from y= -1.2 at 3.4 pc to y= -0.5 at 0.34 pc; interior to this radius the profile is equally consistent with a singular µ(r)∝ r,^(-1/2) cusp or a small nonisothermal core with r_c<0.37 pc. The isophotes maintain constant ellipticity into tlle center, and there is no evidence for a central point source, disk, dust, or any other substructures. The cusp model implies central mass densities p_0 > 3 X 10^7 M_☉ pc^(-3) at the resolution limit and is consistent with a central M_• = 3 X 10^6 M_☉ black hole; the core model implies p_0≈4 X 10^6 M_☉ pc^(-3). From the viewpoint of long-term stability, we argue that a starlight cusp surrounding a central black hole is the more plausible interpretation of the observations. A core at the implied density and size without a black hole has a relaxation time of only ~7 X 10^7 yr and a short stellar oollision timescale implying wholesale stellar merging over the age of the universe. The core would be strongly vulnerable to collapse and concomitant runaway stellar merging. Collapse may lead to formation of a massive black hole in any case if it cannot be reversed by formation of a binary from high-mass merger products. Regardless of the ultimate fate of the core, however, structural evolution of the core will always be accompanied by strong evolution of the core population-the constant isophote shape and absence of a central color gradient appear to show that such evolution has not occurred. In contrast, the high velocities around a black hole imply long relaxation and stellar collision times for the cusp population compared to the age of the universe

Imaging of the gravitational lens system PG 1115+080 with the Hubble Space Telescope

This paper is the first of a series presenting observations of gravitational lenses and lens candidates, taken with the Wide Field/Planetary Camera (WFPC) of the Hubble Space Telescope (HST). We have resolved the gravitational lens system PG 1115 + 080 into four point sources and a red, extended object that is presumably the lens galaxy; we present accurate relative intensities, colors, and positions of the four images, and lower accuracy intensity and position of the lens galaxy, all at the epoch 1991.2. Comparison with earlier data shows no compelling evidence for relative intensity variations between the QSO components having so far been observed. The new data agree with earlier conclusions that the system is rather simple, and can be produced by the single observed galaxy. The absence of asymmetry in the HST images implies that the emitting region of the quasar itself has an angular radius smaller than about 10 milliarcsec (100 pc for H_0=50, q_0=0.5)

The Postcollapse core of M15 imaged with the HST planetary camera

We have obtained U-band images of the M15 core with the Planetary Camera of the Hubble Space Telescope. We are able to resolve stars down to the main-sequence turnoff (m_v≈ 19.4) into the cluster center. We use crowded field photometry techniques to decompose M15 into bright resolved stars and a residual component consisting of stars at turnoff brightness or fainter. The residual component comprises 59% of the cluster light and follows a y = -0.71 power-law distribution for r > 1". The residual component flattens off interior to this radius and has a large core with r_c = 2".2 = 0.13 pc. The core size may reflect postcollapse core expansion. The resolved stars have a slightly shallower distribution (y = - 0.53) but have an abrupt overdensity for r < 1".5, which accounts for the unresolved surface brightness cusp at ground resolution. The bright stars do not become more highly concentrated at still smaller radii, however; neither the bright stars nor the residual component form a cusp at subarcsecond resolution. The total central density of light in all components is 8 x 10^5 L_☉ pc^(-3) (U-band). The Peterson, Seitzer, and Cudworth central velocity dispersion implies a high core M/L ≈ 8 (U-band). The existence of a core rather than a cusp at the 0.1 pc scale may imply that the centrally deduced dark matter is in a diffuse form rather than a massive black hole

Molecular Dynamics Simulations of Temperature Equilibration in Dense Hydrogen

The temperature equilibration rate in dense hydrogen (for both T_{i}>T_{e} and T_i<T_e) has been calculated with molecular dynamics simulations for temperatures between 10 and 600 eV and densities between 10^{20}/cc to 10^{24}/cc. Careful attention has been devoted to convergence of the simulations, including the role of semiclassical potentials. We find that for Coulomb logarithms L>1, a model by Gericke-Murillo-Schlanges (GMS) [Gericke et al., PRE 65, 036418 (2002)] based on a T-matrix method and the approach by Brown-Preston-Singleton [Brown et al., Phys. Rep. 410, 237 (2005)] agrees with the simulation data to within the error bars of the simulation. For smaller Coulomb logarithms, the GMS model is consistent with the simulation results. Landau-Spitzer models are consistent with the simulation data for L>4