Vertical and radial metallicity gradients in high latitude galactic fields with SDSS

Güçtekin, S. Tunçel; Bilir, S.; Karaali, S.; Plevne, O.; Ak, S.

doi:10.1016/j.asr.2018.10.041

Cited by 11 publications

(3 citation statements)

References 45 publications

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“…Chemical abundances of stars changes drastically in Galaxy-wide distances so that various metallicity gradients were obtained in various radial and vertical directions from the Galactic centre and the Galactic plane, respectively (Coşkunoglu et al 2012;Plevne et al 2015;Onal Tas , et al 2016Tunçel Güçtekin et al 2019). Up until the Gaia era, our RC knowledge was gathered from the stars within the Solar neighbourhood with different radii (5 < R < 10 kpc and −2 < |Z| < 2 kpc).…”

Section: Introductionmentioning

confidence: 99%

“…Chemical abundances of stars changes drastically in Galaxy-wide distances so that various metallicity gradients were obtained in various radial and vertical directions from the Galactic centre and the Galactic plane, respectively (Coşkunoglu et al 2012;Plevne et al 2015;Önal Tas , et al 2016Önal Tas , et al , 2018Tunçel Güçtekin et al 2019).…”

Section: Introductionmentioning

confidence: 99%

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Multiwavelength Absolute Magnitudes and Colors of Red Clump Stars in the Gaia Era

Plevne

Taş

Bilir

et al. 2020

ApJ

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This study presents the multi-wavelength investigation of the absolute magnitudes and colours of the red clump (RC) stars selected from APOGEE and GALAH DR2 combined catalogue which is complemented with Gaia DR2 astrometric data and multi-wavelength photometric data of GALEX GR6/7, SDSS DR7, Gaia DR2, 2MASS and WISE sky surveys. The analyses are centred on the different distance estimation methods using Gaia trigonometric parallaxes, (1/ ) and Bayes statistics, and chemically defined Galactic disc populations on [α/Fe]×[Fe/H] plane. Such investigation questions the long studied problem of the population effects on RC luminosity. Using two different distance estimation approach, (i) chemical thin and chemical thick disc RC stars are shown to have different absolute magnitudes, while colours remain the same in all photometric bands. Absolute magnitudes vary between -0.12 and +0.13 mag for the 1/ with the change of the Galactic population. This variation in absolute magnitudes is found to be larger for the other method. (ii) The Besançon population synthesis model of Galaxy for 2MASS photometry, in which the absolute magnitude difference between chemical populations were found between -0.35 and -0.40 mag from thin disc to thick disc. When results compared with each other, differences of absolute magnitudes are about three times larger in the model than observations. We confirm that the RC absolute magnitudes depend on α-element abundances of Galactic populations.

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Section: Introductionmentioning

confidence: 99%

“…Chemical abundances of stars changes drastically in Galaxy-wide distances so that various metallicity gradients were obtained in various radial and vertical directions from the Galactic centre and the Galactic plane, respectively (Coşkunoglu et al 2012;Plevne et al 2015;Önal Tas , et al 2016Önal Tas , et al , 2018Tunçel Güçtekin et al 2019).…”

Section: Introductionmentioning

confidence: 99%

Multiwavelength Absolute Magnitudes and Colors of Red Clump Stars in the Gaia Era

Plevne

Taş

Bilir

et al. 2020

ApJ

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“…Similar calibrations have been developed for the SDSS photometric system and applied to faint stars (Karaali et al 2005;Bilir et al 2005;Tunçel Güçtekin et al 2017). These calibrations were used to calculate metal abundances (Ak et al 2007;Ivezic et al 2008;Tunçel Güçtekin et al 2019) and estimation of the Galactic model parameters…”

Section: Introductionmentioning

confidence: 99%

Bridging the ultraviolet and optical regions: Transformation equations between GALEX and UBV photometric systems

Bilir

Alan

Güçtekin

et al. 2020

Publ. Astron. Soc. Aust.

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We derive transformation equations between GALEX and UBV colours by using the reliable data of 556 stars. We present two sets of equations: as a function of (only) luminosity class and as a function of both luminosity class and metallicity. The metallicities are provided from the literature, while the luminosity classes are determined by using the PARSEC mass tracks in this study. Small colour residuals and high squared correlation coefficients promise accurate derived colours. The application of the transformation equations to 70 stars with reliable data shows that the metallicity plays an important role in estimation of more accurate colours.

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Updated absolute parameters and kinematics of IS CMa

Evcil,

Adalalı,

Alan

et al. 2024

Astron Nachr

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Eclipsing binary systems are significant objects for astrophysics in that direct observations can determine the fundamental parameters of stars. In this study, we precisely determined the fundamental parameters of the binary component stars obtained by simultaneous analysis of radial velocities and the TESS light curve using the Wilson and Devinney code. Following the analysis, the masses and radii of the primary and secondary components were determined as , , and , , respectively. Furthermore, the distance of IS CMa is calculated as pc. On the basis of the analysis of the mid‐eclipse times, it was found that the variation in the orbital period is represented by an upward parabola. It has an increasing rate of = 1.09 10 day year. Using PARSEC stellar evolutionary tracks and isochrones with solar metallicity estimated the age of IS CMa as Gyr. Kinematic and Galactic orbital parameters of IS CMa were obtained from the astrometric and spectroscopic data of the system. The Galactic orbit analysis reveals that IS CMa formed inside the solar circle and it is a member of the young thin‐disc population.

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Vertical and radial metallicity gradients in high latitude galactic fields with SDSS

Cited by 11 publications

References 45 publications

Multiwavelength Absolute Magnitudes and Colors of Red Clump Stars in the Gaia Era

Multiwavelength Absolute Magnitudes and Colors of Red Clump Stars in the Gaia Era

Bridging the ultraviolet and optical regions: Transformation equations between GALEX and UBV photometric systems

Updated absolute parameters and kinematics of IS CMa

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