We propose to produce definitive Color-Magnitude Diagrams (CMDs) for a small, but carefully chosen sample of galactic globular clusters, using the Mosaic Camera on the Blanco telescope. The large field size will enable us to efficiently cover to beyond the published tidal radius for even the larger clusters in our sample. We will combine with

If the gas in filaments and halos shares the same velocity field as the luminous matter, it will generate measurable temperature anisotropies due to the kinematic Sunyaev-Zel'dovich effect. We compute the distribution function of the KSZ signal produced by a typical filament and show it is highly non-Gaussian. The combined contribution of the

Recent observations of coronal hole areas with the XRT and EIS instruments on board the Hinode satellite have shown with unprecedented detail the launching of fast, hot jets away from the solar surface. In some cases these events coincide with episodes of flux emergence from beneath the photosphere. In this Letter we show results of a three

Globular clusters (GCs) provide crucial constraints on galaxy formation models and structure in the Universe, as well as the amount and distribution of galactic dark matter (DM). We request time to double the existing sample of GC velocities for the Virgo elliptical galaxy NGC 4649 from 120 to 250. This increased GC sample will allow the use of the

Finding distances in astronomy is notoriously difficult. With accurate optical spectroscopy, both the distance to and extinction (reddening) of normal stars can be found, but this is not possible for X-ray sources. It is possible, however, to measure the extincting column from an X-ray spectrum from photoelectric ionisation edges. It is also

The line-of-sight velocities and [O III] 5007 Å expansion velocities are measured for 11 planetary nebulae (PNs) in the Virgo Cluster core, at 15 Mpc distance, with the FLAMES spectrograph on the ESO VLT. These PNs are located about halfway between the two giant elliptical galaxies M87 and M86. From the [O III] 5007 Å line profile widths, the