Absolute magnitude calibration for red clump stars

Abstract

We combined the (K s , J − K s ) data in Laney et al. (2012) with the V apparent magnitudes and trigonometric parallaxes taken from the Hipparcos catalogue and used them to fit the M Ks absolute magnitude to a linear polynomial in terms of V − K s colour. The mean and standard deviation of the absolute magnitude residuals,−0.001 and 0.195 mag, respectively, estimated for 224 red clump stars in Laney et al. (2012) are (absolutely) smaller than the corresponding ones estimated by the procedure which adopts a mean M Ks = −1.613 mag absolute magnitude for all red clump stars, −0.053 and 0.218 mag, respectively. The statistics estimated by applying the linear equation to the data of 282 red clump stars in Alves (2000) are larger, ∆M Ks = 0.209 and σ = 0.524 mag, which can be explained by a different absolute magnitude trend, i.e. condensation along a horizontal distribution.

Solar Space Density of the Red Clump Stars and the Scale-Length of the Thin Disc

“…Laney , Joner, & Pietrzyski (2012) determined the absolute magnitude M K s = −1.613 ± 0.015 mag for RC stars in the solar neighbourhood and applied it to estimate the distance of the Large Magellanic Cloud. Karaali, Bilir & Yaz Gökçe (2013) fitted the M K s absolute magnitudes of the RC stars to a linear polynomial in terms of V − K s colour, and Bilir et al (2013a) calibrated the M K s , M V , M J and M g absolute magnitudes in terms of colours corresponding to the photometric systems where the K s , V, J and g bands are defined. Finally, we quote the paper of Bilir et al (2013b) where the M V absolute magnitude had been calibrated in terms of metallicity and B − V colour.…”

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

“…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. In Karaali et al (2012, hereafter Paper I), we used a similar procedure for the absolute magnitude estimation of red giants by using the V 0 , ( B − V ) 0 apparent magnitude–colour diagrams of Galactic clusters with different metallicities. Here, we will estimate absolute magnitudes for red giants with g 0 , ( g − r ) 0 colour–magnitude diagrams.…”

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

“…In Karaali, Bilir, & Yaz Gökçe (2012a, 2012b; hereafter Paper I and Paper II, respectively), we used a procedure for the absolute magnitude estimation of red giants by using the V 0 ×( B − V ) 0 and g 0 ×( g − r ) 0 apparent magnitude–colour diagrams of Galactic clusters with different metallicities. Here, we extend our procedure to Two Micron All Sky Survey (2MASS; Skrutskie et al 2006) photometry.…”