’ reserve holdings in the context of IMF surveillance activities. The paper concludes that IMF economists were generally at the forefront of research during the 2000s, notably in empirical applications of theoretical models, in quantifying the effects of growing exposures to financial crises on reserve

and the solar wind/IMF conditions. The selection funnels were shifted within ±10 ◦ of SM latitude around the model cusp location, and linear regression parameters were calcu-lated for each sliding subset, further divided into 10 bins of distance in the range 2≤R≤12RE, with the following re-sults. (1

We present an investigation about the shape of the initial mass function (IMF) of early-type galaxies (ETGs), based on a joint lensing and dynamical analysis, and on stellar population synthesis models, for a sample of 55 lens ETGs identified by the Sloan Lens ACS (SLACS) Survey. We construct

what characteristics of the internally generated field of Mercury can be inferred from the MESSENGER observations, and to what extent they will be able to constrain various models of Mercury's magnetic field generation. Based on the results of our simulations, we argue that it should be possible

have constructed an H-R diagram and used it and other arguments to infer masses and ages. To allow comparison with the results of our previous studies of IC 348 and ρ Oph, we first use the models of D’Antona & Mazzitelli. With these models, the distributions of ages of comparable samples of stars

with low-resolution (R ∼ 1,200) infrared CTIO spectroscopy and optical/near-infrared HST imaging. Extinction, measured from [Fe II] lines, is estimated at AV = 17.7±2.6. The age of the cluster is estimated at 5.7 Myr, based on Brγ equivalent width for an instantaneous burst using Starburst99 modeling

. This paper circumvents those challenges and infers macro-economic policy using the actual record of the macro-economy in a specification based on Alesina’s rational partisan theory (Alesina, 1987). The testing strategy relies upon the variation we see in party control of different cabinet ministries under

< 2.0, with 202-h of exposure at the ESO Very Large Telescope. We constructed detailed axisymmetric dynamical models for the objects, based on the Jeans equations, taking the observed surface brightness (from deep HST/ACS observations), PSF and slit effects into account. Our dynamical masses MJeans

.0, with 202-h of exposure at the ESO Very Large Telescope. We constructed detailed axisymmetric dynamical models for the objects, based on the Jeans equations, taking the observed surface brightness (from deep HST/ACS observations), PSF and slit effects into account. Our dynamical masses MJeans agree within

for the cooling flow sample. For 2/3 of this sample it is possible to equate Chandra/XMM cooling flow mass deposition rates with UV inferred star formation rates, for a combination of starburst lifetime and IMF slope. This is a pilot study of the well populated XMM UV cluster archive and a more extensive follow