Please use this identifier to cite or link to this item: http://hdl.handle.net/2248/7398
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dc.contributor.authorSnehalata Sahu-
dc.contributor.authorSubramaniam, A-
dc.contributor.authorCote, Patrick-
dc.contributor.authorKameswara Rao, N-
dc.contributor.authorStetson, Peter B-
dc.date.accessioned2019-02-21T04:09:58Z-
dc.date.available2019-02-21T04:09:58Z-
dc.date.issued2019-01-
dc.identifier.citationMonthly Notices of the Royal Astronomical Society, Vol. 482, No. 1, pp.1080–1095en_US
dc.identifier.issn1365-2966-
dc.identifier.urihttp://hdl.handle.net/2248/7398-
dc.descriptionRestricted Accessen_US
dc.description.abstractA complete census of the blue horizontal branch (BHB) and blue straggler star (BSS) population within a 10′ radius from the centre of the globular cluster NGC 288 is presented, based on images from the Ultraviolet Imaging Telescope (UVIT). The UV and UV−optical colour–magnitude diagrams (CMDs) are constructed by combining the UVIT, HST-ACS and ground data and are compared with the Bag of Stellar Tracks and Isochrones (BaSTI) isochrones generated for UVIT filters. We used stellar proper motion data from GAIA DR2 to select the cluster members. Our estimations of the temperature distribution of 110 BHB stars reveal two peaks, with the main peak at Teff ∼ 10 300 K, and with the distribution extending up to Teff ∼ 18 000 K. We identify the well-known photometric gaps, including the Grundahl jump (G-jump) in the BHB distribution, which are located between the peaks. We detect a plateau in the far-ultraviolet (FUV) magnitude for stars hotter than Teff ∼ 11 500 K (G-jump), which could be caused by atomic diffusion. We detect two extreme horizontal branch (EHB) candidates, with temperatures ranging from 29 000 to 32 000 K. The radial distribution of 68 BSSs suggests that the bright BSSs are more centrally concentrated than the faint BSSs and the BHB stars. We find that the BSSs have a mass range of 0.86–1.25 M⊙ and an age range of 2–10 Gyr, with peaks at 1 M⊙ and 4 Gyr respectively. This study showcases the importance of combining UVIT with HST, ground and GAIA data in deriving HB and BSS properties.en_US
dc.language.isoenen_US
dc.publisherOxford University Press on behalf of the Royal Astronomical Societyen_US
dc.relation.urihttps://doi.org/10.1093/mnras/sty2679-
dc.rights© Royal Astronomical Society-
dc.subjectStars: blue stragglersen_US
dc.subjectStars: horizontal branchen_US
dc.subjectStars: Hertzsprung–Russell and colour–magnitude diagramsen_US
dc.subjectGlobular clusters: individual: NGC 288en_US
dc.subjectUltraviolet: starsen_US
dc.subjectStars: imagingen_US
dc.subjectCataloguesen_US
dc.titleUVIT–HST–GAIA view of NGC 288: a census of the hot stellar population and its properties from UVen_US
dc.typeArticleen_US
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