Photometric study of 9 doubtful open clusters

We present results of a photometric investigation of 9 poorly studied apparent open clusters. While the aim of our survey was to determine structural and astrophysical parameters for these objects, they were found not to be physical groups of stars. BV wide‐field CCD photometry combined with the near‐infrared JHK_S data from the 2MASS and proper motions were used to study their nature. Detailed analysis of radial density profiles, morphology of decontaminated colourmagnitude diagrams, and proper motion distributions indicate that these stellar ensembles are projective chance alignments of physically unrelated stars. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

The binary population in OB associations

I describe the outlines of a project aimed at characterising the binary population in the nearby OB Associations. The goal is to obtain an accurate picture of the ‘primordial§ binary population, thus allowing firm constraints to be set on our understanding of the process of star and cluster formation.     

Integrated spectral properties of four previously unstudied small angular size galactic open clusters

We have derived fundamental parameters for the previously unstudied concentrated Galactic open clusters Berkeley 77, NGC2587, BH58 and ESO324‐SC15 by means of integrated spectroscopy in the range 3800–6800 Å. The cluster integrated spectra are compared with those of solar metallicity template spectra of Galactic open clusters with known parameters. The spectra were obtained at CASLEO (San Juan, Argentina) with a resolution of 14 Å.We estimated simultaneously age and foreground interstellar reddening by comparing the continuum distribution and line strengths of the cluster spectra with those of template spectra. Berkeley 77 was found to be an old cluster of 3–4 Gyr, while the remaining three clusters are between 400 and 1000 Myr old. The derived foreground reddening values range from E (B – V) = 0.0 in NGC2587 and ESO324‐SC15 to approximately 0.30 in Berkeley 77. (© 2008 WILEY‐VCH Verlag GmbH & Co. KGaA, Weinheim)     

Lower delta plain interdistributary deposits — An example from the Westphalian of the Lancashire Coalfield,northwest England

A large quarry at Billinge Beacon in Lancashire, northwest England, has provided an excellent exposure of part of the Lower Westphalian A (Upper Carboniferous) Coal Measures sequence which was deposited in a lower delta plain setting. The main horizon exposed, known as the Dyneley Knoll Flags, is interpreted as the proximal reaches of two crevasse-initiated minor delta complexes, into the lower of which has been incised a sinuous minor distributary channel. The channel, which was approximately 120 m wide, built a 160 m wide channel belt by limited lateral accretion with time; vertical accretion appears to have been the dominant infilling mechanism. This produced a stacked series of epsilon cross-strata, made up of rhythmically interbedded sandstone and silty claystone. The peculiar style of infilling of the channel is ascribed to deep incision of the channel into minor delta deposits, and possibly the influence of a seasonal climate.     

ROSAT PSPC observations of the Orion Trapezium area II. Source variability and revised source list

A deep ROSAT PSPC image centred on the Orion Trapezium has been reduceda second time using an improved version of the PSF to fit the data. The outer rim of the field of view was also included. The new catalogue contains 316 X‐ray sources which are easily identified with pre‐main sequence stars of the Ori OB1 Ic and Id association. All 316 sources were tested for variability. No variations were found inside the single exposures of about 45 minutes length each. Between the 4 exposures spaced over 5 days about 1/3 of the sources show signs of activities of various forms. As above 25% of these have somewhat regular lights curves (monotonically rising or falling or hill‐shaped) we infer that at least some outbursts with time scales longer than a day are present and that past searches for X‐ray flares of pre‐main sequence stars were biased towards shorter time scales.