/ftp/cats/aliases/M//MYStIX_4_



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J/ApJS/209/30         MYStIX project: Bayesian matching         (Naylor+, 2013)
The following files can be converted to FITS (extension .fit or fit.gz)
	table2a.dat table2b.dat table2.dat refs.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/ApJS/209/30
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drwxr-xr-x 21 cats archive 4096 Feb 21 2020 [Up] drwxr-xr-x 3 cats archive 4096 Jan 13 2023 [TAR file] -rw-r--r-- 1 cats archive 500 Dec 19 2022 .message -r--r--r-- 1 cats archive 14998 Feb 10 2014 ReadMe -rw-r--r-- 1 cats archive 1109 May 30 2018 +footg5.gif -rw-r--r-- 1 cats archive 3837 May 30 2018 +footg8.gif -r--r--r-- 1 cats archive 3935 Jan 23 2014 refs.dat [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 1460 Jan 23 2014 table2.dat [txt] [txt.gz] [fits] [fits.gz] [html] -rw-r--r-- 1 cats archive 188 Feb 9 2014 table2.sim -r--r--r-- 1 cats archive 349118 Jan 9 2014 table2a.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html] -r--r--r-- 1 cats archive 320953 Jan 9 2014 table2b.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe : J/ApJS/209/30 MYStIX project: Bayesian matching (Naylor+, 2013) ================================================================================ Bayesian matching for X-ray and infrared sources in the MYStIX project. Naylor T., Broos P.S., Feigelson E.D. <Astrophys. J. Suppl. Ser., 209, 30 (2013)> =2013ApJS..209...30N ================================================================================ ADC_Keywords: X-ray sources ; Infrared sources ; Cross identifications Keywords: methods: data analysis - methods: statistical - stars: formation - stars: pre-main sequence Abstract: Identifying the infrared counterparts of X-ray sources in Galactic plane fields such as those of the MYStIX project presents particular difficulties due to the high density of infrared sources. This high stellar density makes it inevitable that a large fraction of X-ray positions will have a faint field star close to them, which standard matching techniques may incorrectly take to be the counterpart. Instead we use the infrared data to create a model of both the field star and counterpart magnitude distributions, which we then combine with a Bayesian technique to yield a probability that any star is the counterpart of an X-ray source. In our more crowded fields, between 10% and 20% of counterparts that would be identified on the grounds of being the closest star to an X-ray position within a 99% confidence error circle are instead identified by the Bayesian technique as field stars. These stars are preferentially concentrated at faint magnitudes. Equally importantly the technique also gives a probability that the true counterpart to the X-ray source falls beneath the magnitude limit of the infrared catalog. In deriving our method, we place it in the context of other procedures for matching astronomical catalogs.