We demonstrate that single and binary star clusters can be formed during cloud-cloud collisions triggered by the tidal interaction between the Large and Small Magellanic clouds. We run two different sets of self-consistent numerical simulations that show that compact, bound star clusters can be formed within the centers of two colliding clouds as a

We report on a Chandra observation of the transient low-mass X-ray binary and type-I X-ray burst source 2S 1711-339 (Carpenter et al. 1977,MNRAS,179,270; Wilson et al. 2003,ApJ,596,1220). The 2S 1711-339 region was observed with the Chandra ACIS-S3 CCD array for 25 ks on 2003 February 07. A total of 64 counts were detected from a source at R.A. =

The experimental study of laser beam propagation in turbulence is relevant to fields such as adaptive optics and optical communications. Turbulence sensing for astronomical purposes requires a convergent laser beam adequately focused on the sodium mesospheric layer. Free Optical communications ground-to-satellite usually are based on divergent

The observed masses of the most massive stars do not surpass about 150 Msolar. This may either be a fundamental upper mass limit which is defined by the physics of massive stars and/or their formation, or it may simply reflect the increasing sparsity of such very massive stars, so that the observation of even higher mass stars becomes unlikely in

As a result of an error in processing proof corrections, the feature labels in the bottom panel of Figure 1 are incorrect. The correct Figure 1 is given here. The press sincerely regrets this error.

2S 1711-339: In ATEL #233 the absorbed X-ray flux of 2S 1711-339 was incorrectly given as 2e-15 ergs cm-2 s-1 (0.3-7.0 keV). The correct value obtained by using a blackbody model with kT = 0.24 +/- 0.03 keV or a neutron-star hydrogen-atmosphere model with kT = 0.07 +/- 0.03 keV is 1.0e-14 ergs cm-2 s-1 (0.5-10.0 keV). This flux is a factor of 10