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 Tools annual

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 monthly

Global: Zendy Plus monthly

Presents the access of premium content as premium feature

Premium Content

Global: Zendy Plus annual

Global: Zendy Free Plan

The putative association between the 10.8 d classical Cepheid TW Nor and theopen cluster Lynga 6 has generated considerable debate in the literature. NewJHKs photometry in tandem with existing radial velocities for Lynga 6 starsimply cluster membership for TW Nor, and establish the variable as ahigh-weight calibrator for classical Cepheid relations. Fundamental meanparameters determined for Lynga 6 are: d=1.91+-0.10 kpc, E(J-H)=0.38+-0.02, andlog(t)=7.9+-0.1. The Benedict et al.(2007)/Turner (2010) Galactic VIc Wesenheitfunction was revised using TW Nor's new parameters:W_VI,0=(-3.37+-0.08)log(P_0)-2.48+-0.08. TW Nor/Lynga 6 lie beyond theSagittarius-Carina spiral arm and occupy the Centaurus arm, along withinnumerable young Cepheids and clusters (e.g., VW Cen & VVV CL070).

New Evidence Supporting Membership for TW Nor in Lynga 6 and the Centaurus Spiral Arm