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J/ApJ/652/1133 BVI photometry of NGC 4258 Cepheids (Macri+, 2006)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
table1.dat table2.dat table[45].dat table6.dat table7.dat
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Query from: http://vizier.cds.unistra.fr/viz-bin/VizieR?-source=J/ApJ/652/1133
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-r--r--r-- 1 cats archive 10823 Jul 30 2008 table2.dat [txt] [txt.gz] [fits] [fits.gz] [html]
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-r--r--r-- 1 cats archive 17422 Jul 30 2008 table6.dat [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 368835 Oct 21 2008 table7.dat [txt] [txt.gz] [fits] [fits.gz] [html]
Beginning of ReadMe :J/ApJ/652/1133 BVI photometry of NGC 4258 Cepheids (Macri+, 2006)
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A new Cepheid distance to the maser-host galaxy NGC 4258 and its implications
for the Hubble constant.
Macri L.M., Stanek K.Z., Bersier D., Greenhill L.J., Reid M.J.
<Astrophys. J., 652, 1133-1149 (2006)>
=2006ApJ...652.1133M
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ADC_Keywords: Galaxies, nearby ; Stars, variable ; Photometry, UBVRI
Keywords: Cepheids - distance scale - galaxies: individual (NGC 4258)
Abstract:
We present initial results from a time series BVI survey of two fields
in NGC 4258 using the HST ACS. This galaxy was selected because of its
accurate maser-based distance, which is anticipated to have a total
uncertainty of 3%. The goal of the HST observations is to provide an
absolute calibration of the Cepheid distance scale and to measure its
dependence on chemical abundance (the so-called metallicity effect).
We carried out observations of two fields at different galactocentric
distances with a mean abundance difference of 0.5dex. We discovered a
total of 281 Cepheids with periods ranging from 4 to 45 days (the
duration of our observing window).
Description:
We used the HST (GO program 9810) to observe two fields located at
widely different galactocentric radii within the disk of NGC 4258
(M106). The fields were observed on 12 separate epochs between 2003
December 5 and 2004 January 19.