Comprehensive analysis of RGU photometry in the direction to M5

The RGU-photographic investigation of an intermediate latitude field in the direction to the Galactic center is presented. 164 extra-galactic objects, identified by comparison of Minnesota and Basel charts, are excluded from the program. Also, a region with size 0.104 square-degrees, contaminated by cluster (M5) stars and affected by background light of the bright star HD 136202 is omitted. Contrary to previous investigations, a reddening of $E(B-V)=0.046$, corresponding to E(G-R)=0.07 mag is adopted. The separation of dwarfs and evolved stars is carried out by an empirical method, already applied in some of our works. A new calibration for the metallicity determination is used for dwarfs, while the absolute magnitude determination for stars of all categories is performed using the procedures given in the literature. There is good agreement between the observed logarithmic space density histograms and the galactic model gradients. Also, the local luminosity function agrees with Gliese's (1969) and Hipparcos' (Jahreiss & Wielen 1997) luminosity functions, for stars with $2<M(G)\leq8$ mag. For giants, we obtained two different local space densities from comparison with two Galactic models, i.e. $D^{*}(0)=6.63$, close to that of Gliese (1969), and $D^{*}(0)=6.79$. A metallicity gradient, $d[Fe/H]/dz= -0.20$ dex/kpc, is detected for dwarfs (only) with absolute magnitudes $4<M(G)\leq6$, corresponding to a spectral type interval F5-K0.Comment: 17 pages, including 13 figures and 3 tables, accepted for publication in PAS

New colour-transformations for the Sloan photometry and revised metallicity calibration and equations for photometric parallax estimation

We evaluated new colour-transformations for the Sloan photometry by 224 standards and used them to revise both the equations for photometric parallax estimation and metallicity calibration cited by Karaali et al. (2003). This process improves the metallicity and absolute magnitude estimations by [Fe/H]<=0.3 dex and M^{H}_{g} <= 0.1 mag respectively. There is a high correlation for metallicities and absolute magnitudes derived for two systems, UBV and Sloan, by means of the revised calibrations.Comment: 11 pages, including 7 figures and 2 tables, accepted for publication in PAS

Volume limited dependent Galactic model parameters

We estimated 34 sets of Galactic model parameters for three intermediate latitude fields with Galactic longitudes l=60, l=90, and l=180, and we discussed their dependence on the volume. Also, we confirmed the variation of these parameters with absolute magnitude and Galactic longitude. The star samples in two fields are restricted with bright and unit absolute magnitude intervals, (4,5], and (5,6], whereas for the third field a larger absolute magnitude interval is adopted, (4,10]. The limiting apparent magnitudes of star samples are g=15 and g=22.5 mag which provide space densities within distances in the line of sight 0.9 and 25 kpc. The Galactic model parameters for the thin disc are not volume dependent. However, the ones for thick disc and halo do show spectacular trends in their variations with volume, except for the scalelength of the thick disc. The local space density of the thick disc increases, whereas the scaleheight of the same Galactic component decreases monotonically. However, both model parameters approach asymptotic values at large distances. The axial ratio of the halo increases abruptly for the volumes where thick disc is dominant, whereas it approaches an asymptotic value gradually for larger volumes, indicating a continuous transition from disclike structure to a spherical one at the outermost region of the Galaxy. The variation of the Galactic model parameters with absolute magnitude can be explained by their dependence on the stellar luminosity, whereas the variation with volume and Galactic longitude at short distances is a bias in analysis.Comment: 12 pages, including 8 figures and 5 tables, accepted for publication in PAS

Transformations between the theoretical and observational planes in the HST-NICMOS and WFPC2 photometric systems

Color-temperature relations and bolometric corrections in the HST-NICMOS F1110W, F160W and F222M and in the WFPC2 F439W, F555W and F814W photometric systems, using two different sets of model atmospheres, have been derived. This database of homogeneous, self-consistent transformations between the theoretical and observational planes also allows combinations of visual and infrared quantities, without any further transformation between the two different photometric systems. The behavior of the inferred quantities with varying the stellar parameters, the adopted model atmospheres and the instrumental configurations are investigated. Suitable relations to transform colors and bolometric corrections from HST to ground-based photometric systems are also provided.Comment: 22 pages, 14 figure

Comprehensive Analysis of RGU Photometry in the Direction to M5

The RGU-photographic investigation of an intermediate latitude field in the direction to the Galactic centre is presented. 164 extra-galactic objects, identified by comparison of Minnesota and Basel charts, are excluded from the program. Also, a region with size 0.104 square-degrees, contaminated by cluster (M5) stars and affected by background light of the bright star HD 136202 is omitted. Contrary to previous investigations, a reddening of E(B - V) = 0.046, corresponding to E(G - R) = 0.07 mag is adopted. The separation of dwarfs and evolved stars is carried out by an empirical method, already applied in some of our works. A new calibration for the metallicity determination is used for dwarfs, while the absolute magnitude determination for stars of all categories is performed using the procedures given in the literature. There is good agreement between the observed logarithmic space density histograms and the galactic model gradients. Also, the local luminosity function agrees with Gliese's (1969) and Hipparcos (Jahreiss & Wielen 1997) luminosity functions, for stars with 2 < M(G) ≤ 8 mag. For giants, we obtained two different local space densities from comparison with two Galactic models, i.e. D*(0) = 6.63, close to that of Gliese (1969), and D*(0) = 6.79. A metallicity gradient, d[Fe/H]/dz = -0.20 dex kpc-1, is detected for dwarfs (only) with absolute magnitudes 4 < M(G) ≤ 6, corresponding to a spectral type interval F5-K

Placement of a temporary pacemaker electrode through a persistent left superior vena cava

Perioperative temporary pacing was needed in a patient with congenital skeletal malformations and a cardiac conduction disturbance with incomplete trifascicular block. We report the successful placement of the pacemaker electrode through a persistent left superior vena cava (SVC

Stable Isotope Event Markers Near the Permo-Triassic Boundary in the Karavanke Mountains (Slovenia)

Stable isotope analyses of carbonates and organic matter from the Permo-Triassic boundary section in the Karavanke Mountains, Slovenia, indicate a further example of the “light carbon” event across the boundary. In this section the changes in carbon isotope values were a direct result of the culmination of the marine regression and associated events at the end of the Permian, which caused a drop in primary productivity, as well as related local environmental changes, with no evidence of any considerable diagenetic overprint

New metallicity calibration down to [Fe/H] = -2.75 dex

88 dwarfs, covering the colour index interval 0.37 <(B-V)o <= 1.07 mag, with metallicities -2.70 <= [Fe/H] <= +0.26 dex have been taken from three different sources for new metallicity calibration. The catalogue of Cayrel de Stroble et al. (2001) which includes 65% of the stars in our sample supplies detailed information on abundances for stars with determination based on high resolution spectroscopy. 77 stars which supplies at least one of the following conditions have been used as "corner stones" for constructing the new calibration: (i) the parallax is larger than 10 mas (distance relative to the Sun less than 100 pc) and the galactic latitude is absolutely higher than 30 degrees, (ii) the parallax is rather large, if the galactic latitude is absolutely low and vice versa. Contrary to the previous investigations, a third-degree polynomial fitted for the new calibration: [Fe/H] = 0.10-2.76d-24.04d^2+30.00d^3. The coefficients were evaluated by the least-square method, without regarding the metallicity of Hyades. However, the constant term is in the range of metallicity determined for this cluster i.e.: 0.08 <= [Fe/H] <= 0.11 dex. The mean deviation and the mean error in our work are equal to those of Carney (1979), for [Fe/H] >= -1.75 dex where Carney's calibration is valid.Comment: 22 pages, 5 figures. accepted for PASA, Vol 20, No