NEW EVIDENCE SUPPORTING MEMBERSHIP FOR TW NOR IN LYNGA 6 AND THE CENTAURUS SPIRAL ARM
- Department of Astronomy and Physics, Saint Mary's University, Halifax, Nova Scotia (Canada)
- Departamento de Astronomia, Universidad de Concepcion, Concepcion (Chile)
- Departamento Astronomia y Astrofisica, Pontificia Universidad Catolica de Chile, Santiago (Chile)
- Centre for Astrophysics Research, University of Hertfordshire, Hatfield (United Kingdom)
- Departamento de Fisica y Astronomia, Facultad de Ciencias, Universidad de Valparaiso, Valparaiso (Chile)
- Konkoly Observatory, Budapest (Hungary)
The putative association between the 10{sub .}{sup d}8 classical Cepheid TW Nor and the open cluster Lynga 6 has generated considerable debate in the literature. New JHK{sub s} photometry in tandem with existing radial velocities for Lynga 6 stars implies cluster membership for TW Nor and establishes the variable as a high-weight calibrator for classical Cepheid relations. Fundamental mean parameters determined for Lynga 6 are: d = 1.91 {+-} 0.10 kpc, E(J - H) = 0.38 {+-} 0.02, and log {tau} = 7.9 {+-} 0.1. The Benedict et al./Turner Galactic VI{sub c} Wesenheit function was revised using TW Nor's new parameters: W{sub VI,0} (- 3.37 {+-} 0.08)log P{sub 0} - 2.48 {+-} 0.08. TW Nor/Lynga 6 lie beyond the Sagittarius-Carina spiral arm and occupy the Centaurus arm, along with innumerable young Cepheids and clusters (e.g., VW Cen and VVV CL070).
- OSTI ID:
- 22047378
- Journal Information:
- Astrophysical Journal Letters, Vol. 741, Issue 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); ISSN 2041-8205
- Country of Publication:
- United States
- Language:
- English
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