Fine structure of the red giant clump from Hipparcos data, and distance determinations based on its mean magnitude

  title={Fine structure of the red giant clump from Hipparcos data, and distance determinations based on its mean magnitude},
  author={L{\'e}o Girardi and Martin A. T. Groenewegen and Achim Weiss and Maurizio Salaris},
  journal={Monthly Notices of the Royal Astronomical Society},
The I-band brightness MI of clump stars is a possible distance indicator for stellar populations. Investigations have shown that MI is almost insensitive to the V − I colour within the clump. Based on this, it was assumed that MI was insensitive to age and composition of the stellar population and therefore an ideal standard candle, which could be calibrated with local clump stars whose absolute brightness is known from Hipparcos parallaxes. This resulted in a distance to the Large Magellanic… 
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We present a sample of about 120,000 red clump candidates selected from the LAMOST DR2 catalog based on the empirical distribution model in the effective temperature vs. surface gravity plane.
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The red giant clump has been recently argued to be a reliable distance indicator for the galaxies in the Local Group. The accuracy of distance determinations based on this method, however, depends on
An empirical test of the theoretical population corrections to the red clump absolute magnitude
The mean absolute magnitude of the local red clump (RC), M R C λ, is a very well-determined quantity owing to the availability of accurate Hipparcos parallaxes for several hundred RC stars,
Population effects on the red giant clump absolute magnitude: The K-band
We present a detailed analysis of the behaviour of the red clump K-band absolute magnitude (MRCK) in simple and composite stellar populations, in light of its use as a standard candle for distance
Red Clump Stars
Low-mass stars in their core-helium-burning stage define the sharpest feature present in the color-magnitude diagrams of nearby galaxy systems: the red clump (RC). This feature has given rise to a
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The range of metallicity of the Hipparcos sample partially overlaps with met allicity of field giants in the LMC, thus making it possible to determine the distance to the L MC by almost direct comparison of brightness of the local Hipparco red clump giants with that of LMC stars.
WIYN Open Cluster Study. III. The Observed Variation of the Red Clump Luminosity and Color with Metallicity and Age
The recent controversy regarding the variation of the I-band red clump (RC) luminosity (M) with metallicity and age has prompted us to examine this question, using precise photometry of Galactic open
A secondary clump of red giant stars: why and where
Based on the results of detailed population synthesis models, Girardi et al. recently claimed that the clump of red giants in the colour–magnitude diagram (CMD) of composite stellar populations
K-band calibration of the red clump luminosity
The average near-infrared (K-band) luminosity of 238 Hipparcos red clump giants is derived and then used to measure the distance to the Galactic center. These Hipparcos red clump giants have been
Absolute Magnitudes of Seismic Red Clumps in the Kepler Field and SAGA: the age dependency of the distance scale
Red clump stars are fundamental distance indicators in astrophysics, although theoretical stellar models predict a dependence of absolute magnitudes with ages. This effect is particularly strong


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