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The main aim of this paper is to classify mental functions by the Wechsler Adult Intelligence Scale-Revised tests with a mixed method based on wavelets and partial correlation. The Wechsler Adult Intelligence Scale-Revised is a widely used test designed and applied for the classification of the adults cognitive skills in a comprehensive manner. In this paper, many different intellectual profiles have been taken into consideration to measure the relationship between the mental functioning and psychological disorder. We propose a method based on wavelets and correlation analysis for classifying mental functioning, by the analysis of some selected parameters measured by the Wechsler Adult Intelligence Scale-Revised tests. In particular, 1-D Continuous Wavelet Analysis, 1-D Wavelet Coefficient Method and Partial Correlation Method have been analyzed on some Wechsler Adult Intelligence Scale-Revised parameters such as School Education, Gender, Age, Performance Information Verbal and Full Scale Intelligence Quotient. In particular, we will show that gender variable has a negative but a significant role on age and Performance Information Verbal factors. The age parameters also has a significant relation in its role on Performance Information Verbal and Full Scale Intelligence Quotient change. [ABSTRACT FROM AUTHOR]

The kinematics of M-type (O-rich) giant semi-regular (SR) variable stars were examined. They were grouped with respect to their relative parallax errors (??/?) in order to study the stars having relatively better parallax, and with the period limit (70 d). The spatial and velocity distributions were examined and the results were compared with the results of irregular (L) and Mira-type variables. It was found that M-type giant SR variables are distributed similarly to thin-disc stars and form a kinematically homogeneous group. When the kinematic properties of M-type giant SR variables were compared with those of L- and Mira-type variables, it was estimated that M-type giant SR variables behave as old-disc objects and their kinematic ages vary approximately between 2 and 9 Gyr. [ABSTRACT FROM AUTHOR]

Abstract: Granitic intrusions in Eocene and post-Eocene volcanic rocks outcrop in the Northern and Southern Zones of the Eastern Pontides, NE Turkey. Intrusions in the Northern Zone extend NW–SE whereas those in the Southern Zone are nearly E–W orientated. The contacts of the intrusions with the volcanic rocks are sharp, epidotized and include volcanic xenoliths. The margins of Southern Zone intrusions often contain abundant angular mafic microgranular enclaves of diorite to quartz diorite composition. The rocks also show evidence of mingling and mixing between coeval mafic and felsic magmas. Field observations suggest a stopping type of ascent and emplacement style for the intrusions. Petrographically, intrusions show variations in both colour and mineralogy with fine to medium granular, monzonitic, poikilitic, rapakivi, anti-rapakivi and graphic textures. Based on modal mineralogy, the Northern rocks are monzonite, quartz monzonite, monzodiorite and quartz monzodiorite whereas the Southern samples are monzogranite and granodiorite. The rocks are generally calc-alkaline to mildly alkaline transitional and metaluminous, and show a CAFEMIC trend. The Northern Zone intrusions form a post-collisional, A-type, alkaline monzonitic association and Southern Zone intrusions form a post-collisional, I-type, granodioritic calc-alkaline-transitional association. Whole-rock compositional data indicate that differentiation occurred via fractional crystallisation with or without magma mixing. Incompatible and rare earth element patterns indicate that both the Northern and the Southern Zone intrusions were derived from melting of a mantle region enriched by subduction-related fluids but evolved differently during ascent and emplacement. U–Pb zircon dating in the Southern Zone yields an intrusion age of 44.4±0.3Ma. Regional geodynamics indicates post-collisional extensional tectonics in the region. Crustal involvement and the level of emplacement may have been important for magmatic evolution, especially for the Southern Zone intrusions, after the cessation of subduction and subsequent crustal thickening. [Copyright &y& Elsevier]

We have studied the period–luminosity (P–L) relationships of oxygen-rich semiregular (SR) variables in several wavelength bands usingHipparcosparallaxes with an accuracy of better than 10 per cent. We have shown that there is a clear dependence on period of absolute magnitude in theU, B, V, R, IC, J, H, K, L, M, N,[12],[25],[60] and[100] bands, and that the slope of the linearrelation is a smooth function of wavelength. We point out that this relation can in principle be used to derive absolute bolometric magnitude as a function of period.The behaviour of the second periods of SR variables in the P–L relation in theVandKbands is also discussed. [ABSTRACT FROM AUTHOR]

Different meteorological parameters and atmospheric circulations are known as one of the sources of excitement of gravity waves (GWs). The main purpose of this paper is to analyze the GWs and seasonal variations over Istanbul by wavelet-based computer simulations. Turbulent structures of pressure, height, and air temperature have been analyzed in this paper. These waves are in the meso-scale wave-form and, generally, are observed in spring, autumn, and winter. The FAWAV Wavelet software and the latest version of MATLAB wavelet packet are applied to analyze meteorological parameters for the north-western part of Turkey. Wavelet based computer simulation of data is generally close to the real data under consideration for the Daubechies wavelet series. [ABSTRACT FROM AUTHOR]

The AZT-22 telescope installed in Turkey (Antalia) was aligned and tested on stars by the Hartmann method. The rms normal deviation of an equivalent optical system is 0.040 ± 0.016 µm;. The circle of confusion is 0.40 ± 0.04 arcsec in diameter at a 50% energy level. [ABSTRACT FROM AUTHOR]

Abstract: A scientific collaboration between TÜBİTAK National Observatory (Turkey), Kazan State University (Russia) and Nikolaev Astronomical Observatory (Ukraine) involves observations of minor planets and near-Earth asteroids (NEAs) with the 1.5m Russian–Turkish telescope (RTT150). Regular observations of selected asteroids in the range of 11–18 magnitudes began in 2004 with the view of determining masses of selected asteroids, improving the orbits of the NEAs, and studying physical characteristics of selected asteroids from photometric observations. More than 3000 positions of 53 selected asteroids and 11 NEAs have been obtained with an internal error in the range of 30–300mas for a single determination. Photometric reductions of more than 4000 CCD frames are in progress. Masses of 21 asteroids were estimated through dynamical method using the ground-based optical observations, mainly from the RTT150 and Minor Planet Center. A comparison of the observational results from the RTT150 in 2004–2005 with observations of the same objects at other observatories allows us to conclude that RTT150 can be used for ground-based support in astrometry for the space mission GAIA. [Copyright &y& Elsevier]

Context. The photometry of mutual occultations and eclipses of natural planetary satellites can be used to infer very accurate astrometric data. This can be achieved by processing the light curves of the satellites observed during international campaigns of photometric observations of these mutual events. Aims. This work focuses on processing the complete database of photometric observations of the mutual occultations and eclipses of the Uranian satellites made during the international campaign in 2007. The final goal is to derive new accurate astrometric data. Methods. We used an accurate photometric model of mutual events that explicitly depends on parameters that these accurate observations should be sensitive to, including the albedos of the satellites. Our original method is applied to derive astrometric data in relative positions from photometric observations of mutual occultations and eclipses of the Uranian satellites. Results. We process the 41 light-curves obtained during the international campaign of photometric observations of the Uranian satellites in 2007. The root-mean-square (rms) of the residuals "observations minus calculations" (O-C) with respect to theory for the best 34 observations are equal to 10.3 and 17.7 mas in right ascension and declination, respectively. For five observations only the position angle was derived. Topocentric or heliocentric angular differences for satellites pairs were obtained from 25 central instant offsets between observation and theory during the time period from May 4, 2007 to January 4, 2008. Conclusions. The rms of the residuals is from 10 to 20 mas that corresponds in situ to 10 to 20 km. These mutual event observations appear to be the most accurate astrometric ground-based observations of the major Uranian satellites to-date and should be used for dynamical purposes. [ABSTRACT FROM AUTHOR]

We present here the optical CCD observations and long slit spectra of the galactic supernova remnants G59.5+0.1, G84.9+0.5 and G67.7+1.8, the first two being observed for the first time. The observations were carried out with the 1.5 m Russian-Turkish joint Telescope (RTT150) at TÜBİTAK National Observatory (TUG). The images were taken with H α, [SII] and their continuum filters. After subtracting the continuum from H α and [SII], [SII]/H α ratio is obtained. The average ratio is found to be 0.41 for G59.5+0.1 and 0.44 for G84.9+0.5, in a very good agreement with the ratios obtained from the optical spectra, namely 0.46 and 0.40, respectively, indicating that these remnants are close to, or interacting with, HII regions. G59.5+0.1 and G84.9+0.5 remnants show diffuse-shell morphology while G67.7+1.8 shows arc-shell morphology. From the emission lines of the spectra, the electron density N e , pre-shock density n c , explosion energy E, interstellar extinction E(B-V), and neutral hydrogen column density N(HI) are calculated and shock velocity V s is estimated for these remnants. [ABSTRACT FROM AUTHOR]

We present the R c-band light curves for components A and B of the gravitationally lensed quasar SBS 1520+530 obtained during 2001–2005 with the 1.5-m Russian-Turkish Telescope (RTT-150) at the TUBITAK National Observatory (Turkey). Based on an analysis of the data for the period 2001–2002, we have estimated the time delay of the brightness fluctuations between components A and B of the quasar to be 128 days. This time delay agrees with its previously published values for the periods 1999–2001 and 2003–2004. Using all of the published data on the brightnesses of components A and B of SBS 1520+530 for the 6-year period, we have found at least two microlensing events. One event has the pattern of a long-term linear trend; the duration of the other event is several hundred days. [ABSTRACT FROM AUTHOR]

We report the results of analysis of the data volume containing 13834 topocentric positions of 231 asteroids obtained from observations at the Russian-Turkish RTT-150 telescope (TÜBITAK (Scientific and Technological Research Council of Turkey), Turkey) in 2004-2013. The positions of asteroids were calculated with the differential reduction method in the ICRS system with the use of the reference catalogs of the UCAC series. The observational program covered the main-belt asteroids closely encountering the other asteroids and the near-Earth asteroids (NEA). For the main belt asteroids, the mean-square error of one position was 84 and 68 mas in right ascension and declination, respectively, while it was 160 and 120 mas, respectively, for NEAs. The obtained volume of the asteroid positions widens the arc of groundbased observations of these bodies, which is important for evaluating their orbital elements with a higher accuracy. Moreover, observations of the main-belt asteroids in the periods of close encounters yield valuable material to solve the problem on accurate estimation of the masses of asteroids with a dynamic method. It has been shown that the supplementing of the input dataset with the here-reported observational volume decreases the error in the estimates of the perturbing asteroid mass and the orbital parameters of perturbed bodies. [ABSTRACT FROM AUTHOR]

A site selection of potential observatory locations in Turkey have been carried out by using Multi-Criteria Decision Analysis (MCDA) coupled with Geographical Information Systems (GIS) and satellite imagery which in turn reduced cost and time and increased the accuracy of the final outcome. The layers of cloud cover, digital elevation model, artificial lights, precipitable water vapor, aerosol optical thickness and wind speed were studied in the GIS system. In conclusion of MCDA, the most suitable regions were found to be located in a strip crossing from southwest to northeast including also a diverted region in southeast of Turkey. These regions are thus our prime candidate locations for future on-site testing. In addition to this major outcome, this study has also been applied to locations of major observatories sites. Since no goal is set for the best, the results of this study is limited with a list of positions. Therefore, the list has to be further confirmed with on-site tests. A national funding has been awarded to produce a prototype of an on-site test unit (to measure both astronomical and meteorological parameters) which might be used in this list of locations. [ABSTRACT FROM AUTHOR]

Multicolor photometric observations of the optical afterglow from GRB 060526 with the Russian-Turkish 1.5-m RTT-150 telescope (Mount Bakyrlytepe, Turkey) are presented. The afterglow light curve was measured in detail starting from about 5 h after the GRB and over five ensuing nights. In addition, upper limits were obtained on the rapid variability of the afterglow on the first night of observations and the history of afterglow color variations was measured in detail. In the time interval from 6 to 16 h after the burst, the flux gradually decreased approximately as a power law with a slope of −1.14 ± 0.02. Subsequently, variability was observed on a time scale δt < t and the afterglow began to decay much faster. The afterglow color was approximately constant ( V−R ≈ 0.5) throughout the observations, despite the flux variability. Variability time scales up to δt/t ≈ 0.0055 were observed at ΔF ν/ F ν ≈ 0.3, which violates many constraints on the variability of the observed emission from an ultrarelativistic jet obtained by Ioka et al. (2005). We suggest explaining this variability by the fact that the shell motion is no longer ultrarelativistic at this time. [ABSTRACT FROM AUTHOR]

Our observations with the 1.5-m Russian-Turkish Telescope (RTT150) in October 2005 as part of the program for identifying ROSAT X-ray sources revealed deep eclipses in the cataclysmic variable 1RXS J020929.0+283243 in Triangulum. We determined the orbital period of the binary (96.26 min) and the range of its magnitude variations [Figure not available: see fulltext.]. Due to the favorable geometry (the orbital inclination is close to 90°), the light curve exhibits eclipses of the white dwarf by the secondary component and eclipses of the hot spot by the white dwarf itself. [ABSTRACT FROM AUTHOR]

The results of optical (the RTT-150 telescope) and X-ray (the RXTE observatory) observations of the burster GS 1826–24 are presented. Emphasis was placed on analyzing the emissions during thermonuclear bursts. The results obtained allowed the size of the accretion disk in GS 1826–24 and the inclination of this binary to be estimated.© 2004 MAIK “Nauka / Interperiodica”. [ABSTRACT FROM AUTHOR]

We present the photometric observations of the old nova V603 Aql with the RTT 150 Russian-Turkish telescope during eleven nights of 2001–2002. We show that the star at this time was in a state with positive superhumps and its photometric period of 0d.144–0d.145 was longer than the orbital period. We found night-to-night variations in the mean brightness of the system that are consistent with disk precession periods of 3d.3 and 3d.0 in 2001 and 2002, respectively. Analysis of the results and their comparison with the results of other authors using current theoretical models for disk precession lead us to suggest that the change in the disk precession period was caused by a change in the accretion rate in the system. V603 Aql in a state with negative superhumps was found to be brighter than it is in a state with positive superhumps by 0m.2–0m.3. We hypothesize that the transition between these states could also be caused by a change in the accretion rate. Quasi-periodic oscillations (QPOs) of the brightness with typical time scales of 9–70 min were detected on each observing night. These time scales were found to change from night to night. The detection of QPOs with a period of about 0.05 of the orbital period and its multiples on certain nights provides evidence for the model of QPO generation through accretion-rate modulation by ionization-front oscillations on the surface of the donor star near the inner Lagrangian point. [ABSTRACT FROM AUTHOR]

We describe the first results of our observations of the exceptionally bright optical afterglow from the cosmic gamma-ray burst (GRB) of March 29, 2003 (030329), with the 1.5-m Russian–Turkish telescope (RTT150) installed at the TUBITAK National Observatory (Turkey) at Mount Bakyrlytepe. RTT150 was one of the first medium-class telescopes pointed at the afterglow. The observations began as early as about six hours after the GRB. During the first five hours of our observations, the BVRI flux fell off exactly as a power law with the same slope –1.19 ± 0.01. Subsequently, in all of the BVRI bands, we observed the same increase in the power-law slope of the light curve to a value that was later recorded during the observations at observatories in the western hemisphere. The break in the power-law light curve occurs at t–t0 ≈ 0.57 days (13.5 h) and lasts for about 0.2 days. Apart from this smooth decrease in the flux, the afterglow exhibited no flux variability. The upper limits on the variability are 10–1% on time scales of 0.1–1000 s, respectively. The BVRI spectral flux distribution during the first night of our observations closely corresponds to a power-law spectrum with a spectral index α = 0.66 ± 0.01. The change in the power-law slope of the light curve at the end of our observations is probably attributable to the deceleration of the ultrarelativistic jet to a gamma factor when its structural features begin to show up in the light curve. The radio, optical, and X-ray broadband spectrum is consistent with the assumption about the synchrotron radiation of the ultrarelativistic jet. This unique object continues to be observed with RTT150.© 2003 MAIK “Nauka / Interperiodica”. [ABSTRACT FROM AUTHOR]