Local Stellar Kinematics from RAVE data—VII. Metallicity Gradients from Red Clump Stars

Taş, Özgecan Önal; Bilir, S.; Seabroke, G. M.; Karaali, S.; Ak, S.; Ak, T.; Bostancı, Z. F.

doi:10.1017/pasa.2016.33

Cited by 12 publications

(1 citation statement)

References 76 publications

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“…had shown that the modes of the intrinsic (dereddened) colours and absolute magnitudes of such a sample are completely defined by the clump giants 1 . The intrinsic colours and absolute magnitudes of the clump vary only with age and metallic-★ E-mail: georgegontcharov@yahoo.com 1 To obtain the modes, we follow , who rounds the observables up to 0.01 mag and finds the tops of their histograms in each ity and can be presented in the space under consideration as some simple functions of | | (Girardi 2016;Önal Taş et al 2016). Therefore, we assumed for our sample that the spatial variations of the modes of the observables BP − RP , RP − 3, G BP + G BP , G RP + G RP , and W3 + W3 reflect the spatial variations of the reddenings ( BP − RP ) and ( RP − 3), extinctions G BP , G RP , and W3 in a combination with some linear gradients of the dereddened colours ( BP − RP ) 0 and ( RP − 3) 0 and absolute magnitudes G BP , G RP , and W3 with | |.…”

Section: Introductionmentioning

confidence: 99%

Gaia DR2 giants in the Galactic dust – II. Application of the reddening maps and models

Gontcharov

Mosenkov

2020

Monthly Notices of the Royal Astronomical Society

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We exploit a complete sample of 101 810 Gaia DR2 giants, selected in Paper I in the space cylinder with a radius of 700 pc around the Sun and a height of |Z| = 1800 pc, using the Gaia DR2 parallaxes, GBP and GRP photometry, and WISE W3 photometry. We explain the spatial variations of the modes of the observables GBP − GRP and GRP − W3 by the spatial variations of the corresponding reddenings described in the GM20 3D dust distribution model. Presented in the current paper, GM20 is an advanced version of the model introduced by Gontcharov in 2009. GM20 proposes two intersecting dust layers, along the Galactic mid-plane and in the Gould Belt, with exponential vertical and sinusoidal longitudinal variations of the dust spatial density in each layer. The Belt layer is an ellipse, oriented nearly between the centre and anti-centre of the Galaxy, and with a semi-major and -minor axes of 600 and 146 pc, respectively. GBP − GRP and GRP − W3 give similar solutions, but different equatorial layer scale heights of 150 ± 15 and 180 ± 15 pc, respectively, and (GBP − GRP)0 = (1.14 ± 0.01) − (0.022 ± 0.010) |Z|, (GRP − W3)0 = (1.44 ± 0.01) − (0.015 ± 0.010) |Z|, where Z is in kpc. We compare GM20 with several 3D reddening models and maps in their ability to predict the observed colour modes. GM20 and the 3D map by Gontcharov appear to be the best among the models and maps, respectively. However, the most reliable models and maps mainly disagree only in their estimates of low reddening, including the reddening across the whole dust layer.

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Section: Introductionmentioning

confidence: 99%

Gaia DR2 giants in the Galactic dust – II. Application of the reddening maps and models

Gontcharov

Mosenkov

2020

Monthly Notices of the Royal Astronomical Society

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Radial Metallicity Gradients for the Chemically Selected Galactic Thin Disc Main‐Sequence Stars

Akbaba,

Ak,

Bilir

et al. 2024

Astron Nachr

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We present the radial metallicity gradients within the Galactic thin disc population through main‐sequence stars selected on the chemical plane using GALAH DR3 accompanied with Gaia DR3 astrometric data. The [Fe/H], [/Fe] and [Mg/H] radial gradients are estimated for guiding radius as , , dex kpc and for the traceback early orbital radius as , , dex kpc for 66,545 thin‐disc stars, respectively. Alteration of the chemical structure within the Galactic disc caused by the radial orbital variations complicates results for the radial metallicity gradient. The effect of radial orbital variations on the metallicity gradients as a function on time indicates the following results: (i) The presence of a gradient along the disc throughout the time for which the model provides similar prediction, (ii) the radial orbital variations becomes more pronounced with the age of the stellar population and (iii) the effect of radial orbital variations on the metallicity gradients is minimal. The effect of radial orbital variations is found to be at most 6% which does not statistically affect the radial gradient results. These findings contribute to a better understanding of the chemical evolution within the Galactic disc and provide an important basis for further research.

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Local stellar kinematics from RAVE data—VIII. Effects of the Galactic disc perturbations on stellar orbits of red clump stars

Taş

Bilir

Plevne

2018

Astrophys Space Sci

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We aim to probe the dynamic structure of the extended Solar neighbourhood by calculating the radial metallicity gradients from orbit properties, which are obtained for axisymmetric and non-axisymmetric potential models, of red clump (RC) stars selected from the RAdial Velocity Experiment's Fourth Data Release. Distances are obtained by assuming a single absolute magnitude value in near-infrared, i.e. M Ks = −1.54±0.04 mag, for each RC star. Stellar orbit parameters are calculated by using the potential functions: (i) for the MWPotential2014 potential, (ii) for the same potential with perturbation functions of the Galactic bar and transient spiral arms. The stellar age is calculated with a method based on Bayesian statistics. The radial metallicity gradients are evaluated based on the maximum vertical distance (z max ) from the Galactic plane and the planar eccentricity (e p ) of RC stars for both of the potential models. The largest radial metallicity gradient in the 0 < z max ≤ 0.5 kpc distance interval is −0.065 ± 0.005 dex kpc −1 for a subsample with e p ≤ 0.1, while the lowest value is −0.014 ± 0.006 dex kpc −1 for the subsample with e p ≤ 0.5. We find that at z max > 1 kpc, the radial metallicity gradients have zero or positive values and they do not depend on e p subsamples. There is a large radial metallicity gradient for thin disc, but no radial gradient found for thick

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Local Stellar Kinematics from RAVE data—VII. Metallicity Gradients from Red Clump Stars

Cited by 12 publications

References 76 publications

Gaia DR2 giants in the Galactic dust – II. Application of the reddening maps and models

Gaia DR2 giants in the Galactic dust – II. Application of the reddening maps and models

Radial Metallicity Gradients for the Chemically Selected Galactic Thin Disc Main‐Sequence Stars

Local stellar kinematics from RAVE data—VIII. Effects of the Galactic disc perturbations on stellar orbits of red clump stars

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