We present a morphological analysis of the feature-rich 2MASS LMC colormagnitude diagram, identifying Galactic and LMC populations and estimating the density of LMC populations alone. We also present the projected spatial distributions of various stellar populations. The conditions that prevailed when 2MASS observed the LMC provided 10σ limiting sensitivity for J <∼ 16.3, H <∼ 15.3, Ks <∼ 14.7....

We describe BeppoSAX observations of the black hole candidates LMC X–1 and LMC X–3 performed in Oct. 1997. Both sources can be modelled by a multicolor accretion disk spectrum, with temperature ∼ 1 keV. However, there is some evidence that a thin emitting component coexists with the thick disk at these temperatures. In the direction of LMC X–1, we detected a significant emission above 10 keV, w...

The superb phase resolution and quality of the OGLE data on LMC and SMC Cepheids, together with existing data on Galactic Cepheids, are combined to study the period-colour (PC) and amplitude-colour (AC) relations as a function of pulsation phase. Our results confirm earlier work that the LMC PC relation (at mean light) is more consistent with two lines of differing slopes, separated at a period...

We identify a vertical extension of the red clump stars in the color magnitude diagram (CMD) of a section of the Large Magellanic Cloud (LMC). The distribution of stars in this extension is indistinguishable in the U , B, V , and I bands — confirming that the detection is real and placing a strong constraint on models of this stellar population. After subtracting the principal red clump compone...

Aims. We used the red clump stars from the VI photometric data of the Optical Gravitational Lensing Experiment (OGLE III) survey and from the Magellanic Cloud Photometric Survey (MCPS) to estimate the structural parameters of the LMC disk, such as the inclination, i and the position angle of the line of nodes (PAlon), φ. Methods. The observed disk region is divided into sub-regions. The deredde...

We identify a vertical extension of the red clump stars in the color magnitude diagram (CMD) of a section of the Large Magellanic Cloud (LMC). The distribution of stars in this extension is indistinguishable in the U , B, V , and I bands — confirming that the detection is real and placing a strong constraint on models of this stellar population. After subtracting the principal red clump compone...

The LMC paradigm is not a recent approach to teaching computer architecture: it has been presented, tested and used since 1965, first by its authors, Madnick and Donovan, and their MIT students, and since then in many other universities around the world. The main purpose of the LMC paradigm is to explain, using a very simple model, the main components of a real computer system, and to learn how...

Aims. The distribution of RR Lyrae stars (RRLS) in the inner Large Magellanic Cloud (LMC), and the structure of the halo of the LMC delineated by these stars are studied here. Methods. RRLS identified by the OGLE II survey are used to estimate their number density distribution in the bar region of the LMC. To find their location, I estimated the scale-height of their distribution in the LMC usi...

We present an analysis of the deepest pure-UV observations with the highest angular resolution ever performed, a set of 12 exposures with the HST WFPC2 and F160BW filter obtained in parallel observing mode, which cover ∼12 square arcminutes in the LMC, North of the bar and in the “general field” regime of the LMC. The 341 independent measurements of 198 objects represent an accumulated exposure...

In the first of two studies on teat-seeking behavior of newborn pigs, latencies from birth to first mammary contact (LMC) and to first suckle (LS) were recorded by live observation (n = 66). LMC accounted for 66% of LS and variances were similar between these two measures, suggesting that LMC is a good predictor of time to first suckle. In a second experiment, 32 litters of pigs were farrowed i...