# Detection of a White Dwarf companion to a Blue Straggler Star in the   outskirts of globular cluster NGC 5466 with the Ultraviolet Imaging Telescope   (UVIT)

**Authors:** Snehalata Sahu, Annapurni Subramaniam, Mirko Simunovic, J. Postma,, Patrick C\^ot\'e, N.Kameswera Rao, Aaron M. Geller, Nathan Leigh, Michael, Shara, Thomas H. Puzia, and Peter B. Stetson

arXiv: 1903.08212 · 2019-05-08

## TL;DR

This study reports the discovery of a white dwarf companion to a blue straggler star in the globular cluster NGC 5466, using ultraviolet and optical observations, providing insights into BSS formation mechanisms in low-density environments.

## Contribution

First detection of a BSS-WD companion in the outskirts of a low-density globular cluster, supporting the mass-transfer formation pathway.

## Key findings

- White dwarf companion confirmed through SED fitting.
- BSS and WD parameters consistent with theoretical models.
- Supports mass-transfer origin for BSS in low-density clusters.

## Abstract

We report the discovery of a hot white dwarf (WD) companion to a blue straggler star (BSS) in the globular cluster (GC) NGC 5466, based on observations from the Ultra-Violet Imaging Telescope (UVIT) on board AstroSat. The Spectral Energy Distribution (SED) of the Far-UV detected BSS NH 84 was constructed by combining the flux measurements from 4 filters of UVIT, with GALEX, GAIA and other ground-based observations. The SED of NH 84 reveals the presence of a hot companion to the BSS. The temperature and radius of the BSS (T$_{\mathrm{eff}} = 8000^{+1000}_{-250}$ K, R/R$_\odot = 1.44 \pm 0.05$) derived from Gemini spectra and SED fitting using Kurucz atmospheric models are consistent with each other. The temperature and radius of the hotter companion of NH 84 (T$_{\mathrm{eff}} = 32,000 \pm 2000$ K, R/R$_\odot = 0.021 \pm 0.007$) derived by fitting Koester WD models to the SED suggest that it is likely to be a hot WD. The radial velocity derived from the spectra along with the proper motion from GAIA DR2 confirms NH 84 to be a kinematic member of the cluster. This is the second detection of a BSS-WD candidate in a GC, and the first in the outskirts of a low density GC. The location of this BSS in NGC 5466 along with its dynamical age supports the mass-transfer pathway for BSS formation in low density environments.

## Full text

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## Figures

24 figures with captions in the complete paper: https://tomesphere.com/paper/1903.08212/full.md

## References

65 references — full list in the complete paper: https://tomesphere.com/paper/1903.08212/full.md

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Source: https://tomesphere.com/paper/1903.08212