Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7038
Title: A hot companion to a blue straggler in NGC 188 as revealed by the Ultra-Violet Imaging Telescope (UVIT) on ASTROSAT
Authors: Subramaniam, A
Sindhu, N
Tandon, S. N
Kameswara Rao, N
Postma, J
Cote, Patrick
Hutchings, J. B
Ghosh, S. K
George, K
Girish, V
Mohan, Rekhesh
Murthy, J
Sankarasubramanian, K
Stalin, C. S
Sutaria, F. K
Mondal, Chayan
Snehalata Sahu
Keywords: Binaries: general;Blue stragglers;Open clusters and associations: individual (NGC 188)
Issue Date: 20-Dec-2016
Publisher: IOP Publishing
Citation: The Astrophysical Journal Letters, Vol. 833, No. 2, L27
Abstract: We present early results from the Ultra-Violet Imaging Telescope (UVIT) on board the ASTROSAT observatory. We report the discovery of a hot companion associated with one of the blue straggler stars (BSSs) in the old open cluster, NGC 188. Using fluxes measured in four filters in UVIT's far-UV (FUV) channel, and two filters in the near-UV (NUV) channel, we have constructed the spectral energy distribution (SED) of the star WOCS-5885, after combining with flux measurements from GALEX, Ultraviolet Imaging Telescope, Ultraviolet Optical Telescope, SPITZER, WISE, and several ground-based facilities. The resulting SED spans a wavelength range of 0.15 μm to 7.8 μm. This object is found to be one of the brightest FUV sources in the cluster. An analysis of the SED reveals the presence of two components. The cooler component is found to have a temperature of 6000 ± 150 K, confirming that it is a BSS. Assuming it to be a main-sequence star, we estimate its mass to be ~1.1–1.2 M ⊙. The hotter component, with an estimated temperature of 17,000 ± 500 K, has a radius of ~ 0.6 R ⊙ and L ~30 L ⊙. Bigger and more luminous than a white dwarf, yet cooler than a sub-dwarf, we speculate that it is a post-AGB/HB star that has recently transferred its mass to the BSS, which is known to be a rapid rotator. This binary system, which is the first BSS with a post-AGB/HB companion identified in an open cluster, is an ideal laboratory to study the process of BSS formation via mass transfer.
Description: Restricted Access
URI: http://hdl.handle.net/2248/7038
ISSN: 2041-8205
???metadata.dc.rights???: © The American Astronomical Society
???metadata.dc.relation.uri???: http://dx.doi.org/10.3847/2041-8213/833/2/L27
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