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The distance to NGC 5904 (M 5) via the subdwarf main sequence fitting method
We present a determination of the distance modulus of the globularcluster NGC 5904 (M 5), obtained by means of the subdwarf main-sequencefitting on the (V,V-I) color-magnitude diagram. The subdwarf sample hasbeen selected from the HIPPARCOS catalog in a metallicity rangehomogeneous with the cluster ([Fe/H] ≃ -1.1). Both the cluster andthe subdwarfs have been observed with the sametelescope+instrument+filters setup (namely, ESO-NTT equipped with theSUSI2 camera), in order to preserve homogeneity and reduce systematicuncertainties. A set of archival HST data has then been used to obtain adeep and precise ridge line. These have been accurately calibrated inthe ground photometric system by using the NTT data and used to fit thecluster distance modulus. By adopting the most commonly accepted valuesfor the reddening, E(B-V) = 0.035 and 0.03, we obtain respectivelyμ0 = 14.44 ± 0.09 ± 0.07 andμ0 = 14.41 ± 0.09 ± 0.07, in agreement withrecent determinations.Based on data collected at ESO-La Silla, Chile, (GTO 63.L-0717) and fromHST archival data (GO 8310).
| Improved Astrometry and Photometry for the Luyten Catalog. II. Faint Stars and the Revised Catalog
We complete construction of a catalog containing improved astrometry andnew optical/infrared photometry for the vast majority of NLTT starslying in the overlap of regions covered by POSS I and by the secondincremental Two Micron All Sky Survey (2MASS) release, approximately 44%of the sky. The epoch 2000 positions are typically accurate to 130 mas,the proper motions to 5.5 mas yr-1, and the V-J colors to0.25 mag. Relative proper motions of binary components are measured to 3mas yr-1. The false-identification rate is ~1% for11<~V<~18 and substantially less at brighter magnitudes. Theseimprovements permit the construction of a reduced proper-motion diagramthat, for the first time, allows one to classify NLTT stars intomain-sequence (MS) stars, subdwarfs (SDs), and white dwarfs (WDs). We inturn use this diagram to analyze the properties of both our catalog andthe NLTT catalog on which it is based. In sharp contrast to popularbelief, we find that NLTT incompleteness in the plane is almostcompletely concentrated in MS stars, and that SDs and WDs are detectedalmost uniformly over the sky δ>-33deg. Our catalogwill therefore provide a powerful tool to probe these populationsstatistically, as well as to reliably identify individual SDs and WDs.
| A search for previously unrecognized metal-poor subdwarfs in the Hipparcos astrometric catalogue
We have identified 317 stars included in the Hipparcos astrometriccatalogue that have parallaxes measured to a precision of better than 15per cent, and the location of which in the(MV,(B-V)T) diagram implies a metallicitycomparable to or less than that of the intermediate-abundance globularcluster M5. We have undertaken an extensive literature search to locateStrömgren, Johnson/Cousins and Walraven photometry for over 120stars. In addition, we present new UBV(RI)C photometry of 201of these candidate halo stars, together with similar data for a further14 known metal-poor subdwarfs. These observations provide the firstextensive data set of RCIC photometry ofmetal-poor, main-sequence stars with well-determined trigonometricparallaxes. Finally, we have obtained intermediate-resolution opticalspectroscopy of 175 stars. 47 stars still lack sufficient supplementaryobservations for population classification; however, we are able toestimate abundances for 270 stars, or over 80 per cent of the sample.The overwhelming majority have near-solar abundance, with theirinclusion in the present sample stemming from errors in the colourslisted in the Hipparcos catalogue. Only 44 stars show consistentevidence of abundances below [Fe/H]=-1.0. Nine are additions to thesmall sample of metal-poor subdwarfs with accurate photometry. Weconsider briefly the implication of these results for clustermain-sequence fitting.
| The proper-motion approach to counterparts of gamma-ray burst sources and high-latitude X-ray transient sources
Reasons to expect association of high-energy activity with nearby starsare outlined. The need to resort to proper-motion data to identify thesestars is explained. Results of a search for proper-motion stars in, orvery near, the error boxes of four high-latitude X-ray transient sourcesare given. The transients are 4U 0336+01, 2A 1102+384, Cen XR-4, and MX2346-65.
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| Сазвежђа: | Вук |
| Ректацензија: | 15h04m58.20s |
| Deклинација: | -32°50'52.3" |
| Apparent магнитуда: | 10.003 |
| Proper motion RA: | -184.9 |
| Proper motion Dec: | -176.6 |
| B-T magnitude: | 10.659 |
| V-T magnitude: | 10.058 |
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