Spectroscopy of new Pleiades brown dwarfs

Follow-up spectroscopy of the four brown dwarf candidates discovered in an 850 arcmin² optical/near-infrared survey of the Pleiades cluster is presented. All four candidates show spectra consistent with Pleiades membership and should be considered to be very probable members, as the possibility of their being field stars has been shown to be small. At l  = 20.55 and I  −  J  = 3.40 our faintest candidate, NPL40, is the lowest mass brown dwarf spectroscopically identified in the Pleiades at present. Its mass was estimated to be 0.040 M⊙.     

The Coma Berenices star cluster and its moving group

We report on the analysis of astrometric and photometric data from Hipparcos, Tycho and the ACT catalogue in a 1200 sq. degree field around the nearby open star cluster in Coma Berenices and infer the characteristic features of this cluster. From a sample of 51 kinematic members we derive the cluster's distance, size and spatial structure as well as its stellar content, mass and age. We find that the cluster consists of an elliptical core-halo system with major axis parallel to the direction of galactic motion, and of a moving group of extratidal stars. The latter have tangential distances ≥10 pc from the cluster center, but have the same distance from the Sun, the same motion and the same age as the stars in the core and halo. The luminosity function of the core-halo system steeply declines beyond absolute magnitude M_V=4.5, but that of the moving group rises towards fainter magnitudes and suggests the existence of further low-mass members below the current magnitude limit. The cloud of extratidal stars witnesses the process of dissolution of the cluster.     

The impact of membership in communal property associations on livelihoods in the Northern Province, South Africa

This paper investigates the impacts of Communal Property Associations on rural livelihoods in the Northern Province, South Africa. After a brief review of livelihoods and a short background to land reform in South Africa the paper details findings regarding the impact of land reform in the province. Quantitative and qualitative interviews were conducted from July 1999 until May 2000 and in January 2001 to identify and explain any change in livelihoods resulting from land transfer. Change in livelihoods as a result of land reform was found to be minimal largely due to general disorganization, farm size problems, lack of capital, lack of skills and labor, gender bias, and skewed age distribution.     

Environmental reconstructions of a late devensian terrace sequence. Some preliminary findings

Facies analysis of Severn Main terrace sediments at Eardington, Shropshire is instructive in determining aspects of the sedimentary environment at a ‘proximal’ location in the terrace. Evaluation of the structural and directional properties of the gravels indicates that the terrace is a composite feature comprising two units. The lower unit is notable for the widespread occurrence of large sandy facies, a near absence of massive gravel facies, and the presence of large, locally derived, lithoclasts in excess of 1 m in diameter. Facies associations observed indicate the existence of in-channel bars and large channels with bedforms at the dune-plane bed transition. The directional properties of the unit indicate flows parallel to the main valley axis and although the unit is unlike previously reported examples it is interpreted as being the product of a proximal low sinuosity environment. The upper unit is composed mainly of multistorey, coarse, massive gravel units with limited interbedded sand facies. Fabric analysis indicates progradation of the unit from the west. The facies sequence is similar to those encompassed by facies models proposed for proximal alluvial fan deposits and therefore, on structural and directional grounds, the upper unit is interpreted as an alluvial fan deposit which prograded into the main Severn valley from the adjacent Mor Brook tributary. The implications of the composite nature of the terrace at this point are considered both in terms of terrace correlation and palaeohyrological estimation.     

The formation of higher order hierarchical systems in star clusters

We simulate open clusters containing up to 182 stars initially in the form of singles, binaries and triples. Due to the high interaction rate a large number of stable quadruples, quintuples, sextuples and higher order hierarchies form during the course of the simulations. For our choice of initial conditions, the formation rate of quadruple systems after about 2 Myr is roughly constant with time at ∼0.008 per cluster per Myr. The formation rates of quintuple and sextuple systems are about half and one-quarter, respectively, of the quadruple formation rate, and both rates are also approximately constant with time. We present reaction channels and relative probabilities for the formation of persistent systems containing up to six stars. The reaction networks for the formation and destruction of quintuple and sextuple systems can become quite complicated, although the branching ratios remain largely unchanged during the course of the cluster evolution. The total number of quadruples is about a factor of 3 smaller than observed in the solar neighbourhood.     

Captured older stars as the reason for apparently prolonged star formation in young star clusters

The existence of older stars within a young star cluster can be interpreted to imply that star formation occurs on time-scales longer than a free-fall time of a pre-cluster cloud core. Here, the idea is explored that these older stars are not related to the star formation process forming the young star cluster but rather that the orbits of older field stars are focused by the collapsing pre-cluster cloud core. Two effects appear: the focusing of stellar orbits leads to an enhancement of the density of field stars in the vicinity of the centre of the young star cluster; and due to the time-dependent potential of the forming cluster some of these stars can get bound gravitationally to the cluster. These stars exhibit similar kinematical properties to the newly formed stars and cannot be distinguished from them on the basis of radial velocity or proper motion surveys. Such contaminations may lead to a wrong apparent star formation history of a young cluster. In the case of the ONC, the theoretical number of gravitationally bound older low-mass field stars agrees with the number of observed older low-mass stars.     

Multisite campaign on the open cluster M67 – II. Evidence for solar-like oscillations in red giant stars

Measuring solar-like oscillations in an ensemble of stars in a cluster, holds promise for testing stellar structure and evolution more stringently than just fitting parameters to single field stars. The most-ambitious attempt to pursue these prospects was by Gilliland et al. who targeted 11 turn-off stars in the open cluster M67 (NGC 2682), but the oscillation amplitudes were too small (<20 μmag) to obtain unambiguous detections. Like Gilliland et al. we also aim at detecting solar-like oscillations in M67, but we target red giant stars with expected amplitudes in the range 50–  500 μmag  and periods of 1 to 8 h. We analyse our recently published photometry measurements, obtained during a six-week multisite campaign using nine telescopes around the world. The observations are compared with simulations and with estimated properties of the stellar oscillations. Noise levels in the Fourier spectra as low as  27 μmag  are obtained for single sites, while the combined data reach  19 μmag  , making this the best photometric time series of an ensemble of red giant stars. These data enable us to make the first test of the scaling relations (used to estimate frequency and amplitude) with an homogeneous ensemble of stars. The detected excess power is consistent with the expected signal from stellar oscillations, both in terms of its frequency range and amplitude. However, our results are limited by apparent high levels of non-white noise, which cannot be clearly separated from the stellar signal.