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 Plus annual

Presents the access of premium content as premium feature

Premium Content

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 annual

Global: Zendy Free Plan

Global: Zendy Tools monthly

Global: Zendy Plus monthly

GALEX, the first all sky imaging UV satellite, has imaged a large part of thesky providing an excellent opportunity for studying UV star counts. The aim ofour study is to investigate in detail the observed UV star counts obtained byGALEX vis-a-vis the model simulated catalogs produced by the Besancon model ofstellar population synthesis in various Galactic directions, and to explore thepotential for studying the structure of our Galaxy from images in multiple NUVand FUV filters of the forthcoming Ultraviolet Imaging Telescope (UVIT) to beflown onboard ASTROSAT. We have upgraded the Besancon model of stellarpopulation synthesis to include the UV bands of GALEX and UVIT. Depending onthe availability of contiguous GALEX, SDSS, WISE and 2MASS overlapping regions,we have chosen a set of 19 GALEX fields which spread over a range of Galacticdirections. We cross-matched GALEX sources with the WISE+2MASS and SDSScatalogs and UV stars in the GALEX catalog are identified by choosing asuitable IR colour, J - W1 (W1 is a WISE band at 3.4 microns). The IR colourcut method, which is used for the first time for separation of stars, isdiscussed in comparison with the GALEX+SDSS star counts method. We present theresults of the UV star counts analysis carried out using the data from GALEX.We find that the Besancon model simulations represent the observed star countsof both the GALEX AIS and MIS well within the error bars in various Galacticdirections. Based on the model analysis, we separated out white dwarfs of thedisc and blue horizontal branch stars of the halo from the observed sample byselecting a suitable FUV - NUV colour. The Besancon model is now ready forfurther comparisons in the UV domain and will be used for prospective studiesfor the UVIT instrument to be flown onboard ASTROSAT.

A Stellar Population Synthesis Model for the Study of Ultraviolet Star Counts of the Galaxy