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Search for associations containing young stars (SACY). I. Sample and searching method
We report results from a high-resolution optical spectroscopic surveyaimed to search for nearby young associations and young stars amongoptical counterparts of ROSAT All-Sky Survey X-ray sources in theSouthern Hemisphere. We selected 1953 late-type (B-V~≥~0.6),potentially young, optical counterparts out of a total of 9574 1RXSsources for follow-up observations. At least one high-resolutionspectrum was obtained for each of 1511 targets. This paper is the firstin a series presenting the results of the SACY survey. Here we describeour sample and our observations. We describe a convergence method in the(UVW) velocity space to find associations. As an example, we discuss thevalidity of this method in the framework of the β Pic Association.
| Mature and Fresh Surfaces on the Newborn Asteroid Karin
Here we report a near-infrared (J, H, and K bands) spectroscopy of 832Karin, the brightest asteroid among the Karin cluster group, which isthought to be the remnants of a collisional breakup only 5.8 millionyears ago. The spectroscopic observation was performed by the Subarutelescope with the Cooled Infrared Spectrograph and Camera for OHS on2003 September 14. For different rotational phases of Karin, we deriveddifferent spectra such as a reddened spectrum like that of an S-typeasteroid and an unreddened spectrum like that of ordinary chondrite.Karin could be an impact fragment preserving an old surface and isprobably one of the cone-shaped fragments at the low-velocity impactthat formed the Karin cluster group. Our result supports the idea thatS-type asteroids are parent bodies of ordinary chondrites.
| Five-colour photometry of OB-stars in the Southern Hemisphere
Observations of OB-stars, made in 1959 and 1960 at the Leiden SouthernStation near Hartebeespoortdam, South Africa, with the VBLUW photometerattached to the 90 cm light-collector, are given in this paper. They arecompared with photometry obtained by \cite[Graham (1968),]{gra68}\cite[Walraven & Walraven (1977),]{wal77} \cite[Lub & Pel(1977)]{lub77} and \cite[Van Genderen et al. (1984).]{gen84} Formulaefor the transformation of the present observations to those of\cite[Walraven & Walraven (1977)]{wal77} and \cite[Lub & Pel(1977)]{lub77} are given. Table 4 is only available in electronic format the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) orvia http://cdsweb.u-strasbg.fr/Abstract.html
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