Transformations from <i>WISE</i> to 2MASS, SDSS and <i>BVI</i> Photometric Systems: II. Transformation Equations for Red-Clump Stars

Bilir, S.; Karaali, S.; Dağtekin, N. D.; Önal, Ö.; Ak, S.; Ak, T.; Cabrera-Lavers, A.

doi:10.1071/as11078

Cited by 5 publications

(9 citation statements)

References 24 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…3 Identification of the RC stars in WISE Bilir et al (2012) showed that the RC stars can be effectively detectable in W 1, W 2 and W 3 bands of the WISE photometry while dwarfs can be found using W 1 and W 2 (Bilir et al, 2011). We preferred W 1 and W 3 bands in order to identify the RC stars in WISE.…”

Section: The Datamentioning

confidence: 99%

“…We tested the adopted absolute magnitudes and colours of the RC stars es-Table 3 Modes of distributions for the absolute magnitudes and a colour in WISE for the RC stars with σ π /π ≤ 0.15 (see Table 1). The evaluated values from the transformation equations (TEs; Bilir et al, 2012) are also given. Differences between two sets of the data are in the last column.…”

Section: Mode (Mag)mentioning

confidence: 99%

See 1 more Smart Citation

First identification and absolute magnitudes of the red clump stars in the Solar neighbourhood for WISE

et al. 2013

Self Cite

View full text Add to dashboard Cite

We present the first determination of absolute magnitudes for the red clump (RC) stars with the Wide-field Infrared Survey Explorer (WISE). We used recently reduced parallaxes taken from the Hipparcos catalogue and identified 3889 RC stars with the WISE photometry in the Solar neighbourhood. Mode values estimated from the distributions of absolute magnitudes and a colour of the RC stars in WISE photometry are M W 1 = −1.635 ± 0.026, M W 3 = −1.606 ± 0.024 and (W 1 − W 3) 0 = −0.028 ± 0.001 mag. These values are consistent with those obtained from the transformation formulae using 2MASS data. Distances of the RC stars estimated by using their M W 1 and M W 3 absolute magnitudes are in agreement with the ones calculated by the spectrophotometric method, as well. These WISE absolute magnitudes can be used in astrophysical researches where distance plays an important role.

show abstract

Section: The Datamentioning

confidence: 99%

Section: Mode (Mag)mentioning

confidence: 99%

First identification and absolute magnitudes of the red clump stars in the Solar neighbourhood for WISE

et al. 2013

Self Cite

View full text Add to dashboard Cite

show abstract

“…A mean value for the M K s absolute magnitude with weak metallicity dependence can be used for distance estimation which is rather useful for the Galactic structure and interstellar extinction. Examples can be found in López-Corredoira et al (2002, Cabrera-Lavers, Garzón, & Hammersley (2005);Cabrera-Lavers et al (2007a, 2007b, 2008 and Bilir et al (2012) and references therein.…”

Section: Scale-length Of the Thin Discmentioning

confidence: 99%

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

Gökçe

Karaali

Duran

et al. 2015

Publ. Astron. Soc. Aust.

Self Cite

View full text Add to dashboard Cite

We estimated the scale-length of the thin disc with the J and W1 magnitudes of the most probable red clump stars in the Galactic plane, −0• .5 ≤ b ≤ +0• .5, in 19 equal sized fields with consecutive Galactic longitudes which cover the interval 90Our results are constrained with respect to the solar space density (D * = 5.95), which indicates that the radial variation of the density is lower for higher Galactocentric distances. The scale-length of the thin disc is 2 kpc for the fields in the Galactic anticentre direction or close to this direction, while it decreases continuously in the second and third quadrants reaching to a lower limit of h = 1.6 kpc at the Galactic longitudes l = 90• and l = 270• . The distribution of the scale-length in 19 fields is consistent with the predictions from the Galaxia model and its variation with longitude is probably due to the inhomogeneity structure of the disc caused by the accreted material or other features such as warp and flare.

show abstract

“…Yaz et al (2010) obtained transformation between optical and NIR bands for red giants. Bilir et al (2012) extended this study to mid-infrared bands by using Radial Velocity Experiment (RAVE) Third Data Release (DR3) data (Siebert et al 2011). Both works provide absolute magnitudes for a given photometry from another one.…”

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.

Self Cite

View full text Add to dashboard Cite

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

show abstract

Transformations from WISE to 2MASS, SDSS and BVI Photometric Systems: II. Transformation Equations for Red-Clump Stars

Cited by 5 publications

References 24 publications

First identification and absolute magnitudes of the red clump stars in the Solar neighbourhood for WISE

First identification and absolute magnitudes of the red clump stars in the Solar neighbourhood for WISE

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

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

Contact Info

Product

Resources

About