/ftp/cats/aliases/O/OGLE_34_



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J/AcA/60/91         VI light curves of SMC Cepheids          (Soszynski+, 2010)
The following files can be converted to FITS (extension .fit or fit.gz)
	table1.dat table2.dat remarks.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/AcA/60/91
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drwxr-xr-x 9 cats archive 167 Jan 29 2012 [Up] drwxr-xr-x 3 cats archive 331 Jan 13 2023 [TAR file] -rw-r--r-- 1 cats archive 488 Dec 19 2022 .message -r--r--r-- 1 cats archive 7049 May 22 2012 ReadMe -rw-r--r-- 1 cats archive 405 Mar 26 2012 +footg5.gif -rw-r--r-- 1 cats archive 2135 Jun 10 2011 +footg8.gif -r--r--r-- 1 cats archive 579 Dec 24 2010 remarks.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 3458 Dec 24 2010 table1.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 4042 Dec 24 2010 table2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/AcA/60/91 VI light curves of SMC type II Cepheids (Soszynski+, 2010) ================================================================================ The Optical Gravitational Lensing Experiment. The OGLE-III catalog of variable stars. VIII. Type II Cepheids in the Small Magellanic Cloud. Soszynski I., Udalski A., Szymanski M.K., Kubiak M., Pietrzynski G., Wyrzykowski L., Ulaczyk K., Poleski R. <Acta Astron., 60, 91-107 (2010)> =2010AcA....60...91S ================================================================================ ADC_Keywords: Magellanic Clouds ; Stars, variable ; Magnitudes Keywords: stars: variables: Cepheids - stars: oscillations - stars: Population II - Magellanic Clouds Abstract: The eighth part of the OGLE-III Catalog of Variable Stars (OIII-CVS) contains type II Cepheids in the Small Magellanic Cloud (SMC). The sample consists of 43 objects, including 17 BL Her, 17 W Vir and 9 RV Tau stars (first examples ever found in the SMC). Seven stars have been classified as peculiar W Vir stars - a recently identified subclass of type II Cepheids. These stars have distinctive light curves, are brighter and bluer than the ordinary W Vir variables. We confirm that a large fraction of the peculiar W Vir stars are members of binary systems.