English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Tools annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

We analyse Gaia EDR3 parallax systematics as a function of magnitude and skylocation using a recently published catalogue of 12,500 asteroseismic red-giantstar distances. We selected ~ 3500 red clump (RC) stars of similar chemicalcomposition as the optimal subsample for this purpose. We perform a detailedassessment of systematic uncertainties relevant for parallax offset estimationbased on the asteroseismic distances. Following this assessment, we adopt forour baseline analysis the asteroseismic parameters measured as in Elsworth etal. (2020), spectroscopy from APOGEE (DR17), and we further restrict the sampleto low-extinction RC stars with quality astrometric solutions from Gaia EDR3.We then investigated both the parallax offset relative to the published GaiaEDR3 parallaxes and the residual parallax offset after correcting Gaia EDR3parallaxes following Lindegren et al. (2021).  We find residual parallax offsets very close to zero (-1.6 +/- 0.5 (stat.)+/- 10 (syst.) muas) for stars fainter than G > 11 mag in the initial Keplerfield. For 17 K2 campaigns in the same magnitude range, the residual parallaxoffset is +16.5 +/- 1.7 (stat.) +/- 10 (syst.) muas. At brighter magnitudes (G<= 11 mag), we find inconsistent residual parallax offsets between the Keplerfield, 17 K2 campaigns, and the TESS southern continuous viewing zone, withdifferences of up to 60 muas. This suggests a significant dependence on skylocation at bright magnitudes due to the lack of bright physical pairsavailable for determining the parallax offset corrections. Finally, we estimatethe absolute magnitude of the RC and obtain M_Ks^RC = -1.650 +/- 0.025 mag inthe 2MASS Ks-band and M_G^RC = (0.432 +/- 0.004) - (0.821 +/- 0.033) (Teff [K]- 4800K)/1000K [mag] in the Gaia G-band.

astronomy and astrophysics

Investigating Gaia EDR3 parallax systematics using asteroseismology of  Cool Giant Stars observed by Kepler, K2, and TESS II. Deciphering Gaia  parallax systematics using red clump stars