Luminosity-colour relations for thin-disc main-sequence stars

Bilir, S.; Karaali, S.; Ak, S.; Yaz, E.; Cabrera-Lavers, A.; Coşkunoğlu, K.B.

doi:10.1111/j.1365-2966.2008.13839.x

Cited by 24 publications

(52 citation statements)

References 32 publications

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“…In Karaali et al (2003), we presented a procedure for the photometric parallax estimation of dwarf stars which depends on the absolute magnitude offset from the main sequence of the Hyades cluster. Bilir et al (2008) obtained the absolute magnitude calibrations of the thin disc main-sequence stars in the optical M V and in the NIR M J bands using the recent reduced Hipparcos astrometric data (van Leeuwen 2007). Bilir et al (2009) derived a new luminosity colour relation based on trigonometric parallaxes for the thin disc main-sequence stars with Sloan Digital Sky Survey (SDSS) photometry.…”

Section: Introductionmentioning

confidence: 99%

Absolute Magnitude Calibration for Red Giants Based on the Colour–Magnitude Diagrams of Galactic Clusters. III. Calibration with 2MASS

Karaali

Bilir²,

Gökçe³

2013

Publ. Astron. Soc. Aust.

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We present two absolute magnitude calibrations, M J and M K s , for red giants with the colour-magnitude diagrams of five Galactic clusters with different metallicities, i.e. M92, M13, M71, M67, and NGC 6791. The combination of the absolute magnitudes of the red giant sequences with the corresponding metallicities provides calibration for absolute magnitude estimation for red giants for a given colour

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Section: Introductionmentioning

confidence: 99%

Absolute Magnitude Calibration for Red Giants Based on the Colour–Magnitude Diagrams of Galactic Clusters. III. Calibration with 2MASS

Karaali

Bilir²,

Gökçe³

2013

Publ. Astron. Soc. Aust.

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“…Bilir et al (2008) obtained the absolute magnitude calibrations of the thin disc main-sequence stars in the optical (M V ) and the near-infrared (M J ) bands using the recent reduced Hipparcos astrometric data (van Leeuwen 2007). Bilir et al (2009) derived a new luminosity colour relation based on trigonometric parallaxes for the thin disc main-sequence stars with the Sloan Digital Sky Survey (SDSS) photometry.…”

Section: Introductionmentioning

confidence: 99%

Absolute Magnitude Calibration for Giants Based on the Colour–Magnitude Diagrams of Galactic Clusters. II. Calibration with SDSS

Karaali¹,

Bilir²,

Gökçe³

2013

Publ. Astron. Soc. Aust.

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We present an absolute magnitude calibration for red giants with the colour-magnitude diagrams of six Galactic clusters with different metallicities, i.e. M92, M13, M3, M71, NGC 6791, and NGC 2158. The combination of the absolute magnitudes of the red giant sequences with the corresponding metallicities provides calibration for absolute magnitude estimation for red giants for a given (g − r) 0 colour. The calibration is defined in the colour interval 0.45 ࣘ (g − r) 0 ࣘ 1.30 mag and it covers the metallicity interval −2.15 ≤ [Fe/H] ≤ +0.37 dex. The absolute magnitude residuals obtained by the application of the procedure to another set of Galactic clusters lie in the interval −0.28 < M ࣘ +0.43 mag. However, the range of 94% of the residuals is shorter, −0.1 < M ࣘ +0.4 mag. The mean and the standard deviation of (all) residuals are 0.169 and 0.140 mag, respectively. The derived relations are applicable to stars older than 2 Gyr, the age of the youngest calibrating cluster.

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“…Photometric parallax of a star can be provided by combination of its apparent and absolute magnitudes (cf. Bilir et al 2008bBilir et al , 2009). However, estimation of the absolute magnitude of a star is another problem.…”

Section: Introductionmentioning

confidence: 99%

Metallicity calibration and photometric parallax estimation: II. SDSS photometry

Güçtekin

Bilir

Karaali

et al. 2016

Astrophys Space Sci

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We used the updated [Fe/H] abundances of 168 F-G type dwarfs and calibrated them to a third order polynomial in terms of reduced ultraviolet excess, δ 0.41 defined with ugr data in the SDSS. We estimated the M g absolute magnitudes for the same stars via the re-reduced Hipparcos parallaxes and calibrated the absolute magnitude offsets, ∆M g , relative to the intrinsic sequence of Hyades to a third order polynomial in terms of δ 0.41 . mean of the residuals and the corresponding standard deviation for the metallicity calibration are 0 and 0.137 mag; while, for the absolute magnitude calibration they are 0 and 0.179 mag, respectively. We applied our procedures to 23,414 dwarf stars in the Galactic field with the Galactic coordinates 85• and size 78 deg 2 . We estimated absolute magnitude M g dependent vertical metallicity gradients as a function of vertical distance Z. The gradients are deep in the range of 0 < Z ≤ 5 kpc, while they are very small positive numbers beyond Z = 5 kpc. All dwarfs with 5 < M g ≤ 6 mag are thin-disc stars and their distribution shows a mode at (g − r) 0 ≈ 0.38 mag, while the absolute magnitudes 4 < M g ≤ 5 are dominated by thick disc and halo stars, i.e. the apparently bright ones (g 0 ≤ 18 mag) are thick-disc stars with a mode at (g − r) 0 ∼ 0.38 mag, while the halo population is significant in the faint stars (g 0 > 18 mag).

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Luminosity-colour relations for thin-disc main-sequence stars

Cited by 24 publications

References 32 publications

Absolute Magnitude Calibration for Red Giants Based on the Colour–Magnitude Diagrams of Galactic Clusters. III. Calibration with 2MASS

Absolute Magnitude Calibration for Red Giants Based on the Colour–Magnitude Diagrams of Galactic Clusters. III. Calibration with 2MASS

Absolute Magnitude Calibration for Giants Based on the Colour–Magnitude Diagrams of Galactic Clusters. II. Calibration with SDSS

Metallicity calibration and photometric parallax estimation: II. SDSS photometry

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