/ftp/cats/J_other/PASA/37.22



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J/other/PASA/37.22  Calibration sample UBV and GALEX photometry   (Bilir+, 2020)
The following files can be converted to FITS (extension .fit or fit.gz)
	table2.dat
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Query from: http://vizier.u-strasbg.fr/viz-bin/VizieR?-source=J/other/PASA/37.22
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drwxr-xr-x 26 cats archive 4096 Dec 2 10:10 [Up] drwxr-xr-x 3 cats archive 298 Sep 8 22:57 [TAR file] -rw-r--r-- 1 cats archive 471 Aug 4 2020 .message -r--r--r-- 1 cats archive 5233 Aug 4 2020 ReadMe -rw-r--r-- 1 cats archive 696 Aug 4 2020 +footg5.gif -rw-r--r-- 1 cats archive 6204 Aug 4 2020 +footg8.gif -r--r--r-- 1 cats archive 75060 Aug 3 2020 table2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/other/PASA/37.22 Calibration sample UBV and GALEX photometry (Bilir+, 2020) ================================================================================ Bridging the ultraviolet and optical regions: Transformation equations between GALEX and UBV photometric systems. Bilir S., Alan N., Guctekin Tuncel S., Celebi M., Yontan T., Plevne O., Ak S., Ak T., Karaali S. <Publ. Astron. Soc. Australia, 37, 22 (2020)> =2020PASA...37...22B (SIMBAD/NED BibCode) ================================================================================ ADC_Keywords: Stars, fundamental ; Photometry, UBV ; Photometry, ultraviolet ; Abundances, [Fe/H] Keywords: techniques: photometric - catalogue - surveys Abstract: We derive transformation equations between GALEX and UBV colours by using the reliable data of 556 stars. We present two sets of equations: as a function of (only) luminosity class and as a function of both luminosity class and metallicity. The metallicities are provided from the literature, while the luminosity classes are determined by using the PARSEC mass tracks in this study. Small colour residuals and high squared correlation coefficients promise accurate derived colours. The application of the transformation equations to 70 stars with reliable data shows that the metallicity plays an important role in estimation of more accurate colours. Description: We used 556 stars with accurate spectroscopic, photometric and astrometric data and derived transformation equations between GALEX and UBV colours.

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