# Absolute Magnitudes of Seismic Red Clumps in the Kepler Field and SAGA: the age dependency of the distance scale

## TL;DR

This study investigates how the absolute magnitudes of red clump stars depend on age, using seismic data from Kepler and SAGA, revealing a measurable age-related variation that impacts distance measurements.

## Contribution

It provides new calibrations of red clump absolute magnitudes across multiple photometric systems, accounting for age dependence, based on seismic and age data from Kepler and SAGA.

## Key findings

- Detected a 0.020 mag/Gyr slope in infrared absolute magnitudes.
- Distance calibrations can be off by up to 0.2 mag if ages are unknown.
- Results are consistent with local Hipparcos-based calibrations within uncertainties.

## Abstract

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 below 2 Gyr, but even above this limit a mild age dependence is still expected. We use seismically identified red clump stars in the Kepler field for which we have reliable distances, masses and ages from the SAGA survey to first explore this effect. By excluding red clump stars with masses larger than 1.6 Msun (corresponding to ages younger than 2 Gyr), we derive robust calibrations linking intrinsic colors to absolute magnitudes in the following photometric systems: Str\"omgren $by$, Johnson $BV$, Sloan $griz$, 2MASS $JHK_s$ and WISE $W1W2W3$. With the precision achieved we also detect a slope of absolute magnitudes 0.020(0.003) mag per Gyrin the infrared, implying that distance calibrations of clump stars can be off by up to 0.2 mag in the infrared (over the range from 2 Gyr to 12 Gyr) if their ages are unknown. Even larger uncertainties affect optical bands, because of the stronger interdependency of absolute magnitudes on colors and age. Our distance calibrations are ultimately based on asteroseismology, and we show how the distance scale can be used to test the accuracy of seismic scaling relations. Within the uncertainties our calibrations are in agreement with those built upon local red clump with Hipparcos} parallaxes, although we find a tension which if confirmed would imply that scaling relations overestimate radii of red clump stars by 2(+-20%. Data-releases post Gaia DR1 will provide an important testbed for our results.