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J/PASP/111/335 CaII-M_v_ Correlation (Wilson-Bappu Effect) (Wallerstein+ 1999)
The following files can be converted to FITS (extension .fit .fgz or .fiZ)
table1a.dat table1b.dat, table1c.dat
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Query from: http://vizier.cds.unistra.fr/cgi-bin/VizieR?-source=J/PASP/111/335
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-rw-r--r-- 1 cats archive 213 Sep 19 2007 +footg5.gif
-rw-r--r-- 1 cats archive 2047 Mar 5 2008 +footg8.gif
-r--r--r-- 1 cats archive 65587 Aug 3 1999 fig1.gif
-r--r--r-- 1 cats archive 49152 Aug 3 1999 fig2.gif
-r--r--r-- 1 cats archive 51575 Aug 3 1999 fig3.gif
-r--r--r-- 1 cats archive 102442 Aug 3 1999 fig4.gif
-r--r--r-- 1 cats archive 109958 Aug 3 1999 fig5.gif
-r--r--r-- 1 cats archive 7470 Aug 3 1999 table1a.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
-r--r--r-- 1 cats archive 4675 Aug 3 1999 table1b.dat.gz [txt] [txt.gz] [fits] [fits.gz] [html]
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Beginning of ReadMe :J/PASP/111/335 CaII-M_v_ Correlation (Wilson-Bappu Effect) (Wallerstein+ 1999)
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The Ca II-Mv Correlation (Wilson-Bappu Effect) Calibrated by Hipparcos
Parallaxes
Wallerstein G., Machado-Palaez L., Gonzalez G.
<Publ. Astron. Soc. Pac. 111, 335 (1999)>
=1999PASP..111..335W
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ADC_Keywords: Parallaxes, trigonometric; Magnitudes, absolute;
Photometry, K-line; Stars, late-type
Description:
Hipparcos parallaxes were used to derive absolute visual magnitudes of
G, K, and M stars with Ca II emission line widths previously measured
by O.C. Wilson. A linear relationship similar to the one derived
originally by Wilson & Bappu and improved by Lutz & Kelker was found
from M_v_=+7 to -2. For stars brighter than M_v_=-2 a substantial
number of stars show Ca II emission lines that are broader than
expected from the linear fit. Most of those stars are bright giants
and supergiants of type G.
Introduction:
In 1957 O. C. Wilson and M. K. V. Bappu reported on the remarkable
correlation between the measured width of the emission feature at the
center of the Ca II K line and the absolute visual magnitude of the
star. The correlation is independent of spectral type and applicable
to stars of type G, K, and M. Their original calibration was based on
the Sun and the four K giants in the Hyades. Except for the
main-sequence stars there were not many additional calibrating stars
with sufficiently accurate parallaxes to evaluate the dispersion about
the mean relation or to extend the calibration to stars brighter than
about M_v_ = 0.
The paucity of accurate parallaxes for luminous red giants has been
largely overcome by the Hipparcos program (Kovalevsky
1998ARA&A..36...99K) in which parallaxes with uncertainties of near 1
mas were obtained for numerous stars. Hence, we now have 10 sigma
parallaxes out to 100 pc and 5 sigma data to 200 pc, providing
M_v_-values with uncertainties of 0.21 and 0.42 mag, respectively.
Therefore, the large database provided by Wilson (1976ApJ...205..823W)
can be combined with Hipparcos parallaxes to recalibrate the M_v_ -
log W_0_ relation, where W_0_ is the measured width corrected for the
instrumental width. In addition, stars that appear to deviate from the
Wilson-Bappu relation may be investigated in order to understand the
anomalies of their chromospheres.
We have limited ourselves to stars with parallaxes that are at least 5
times their probable error and whose log W_0_-values are listed by
Wilson (1967PASP...79...46W, 1976ApJ...205..823W). Other databases are
available, e.g., Warner (1967MNRAS.137..119W) and Zarro & Rogers
(1983ApJS...53..815Z), but the Wilson data are so much larger than the
others that we decided to base our discussion on these data alone. For
each star we have extracted the parallax, its probable error, V
magnitude, spectral type, B-V color, and V-I color from the Hipparcos
Catalogue (ESA 1997, Cat. I/239). These quantities are listed in
Table 1 along with Wilson's intensity index (1-5), log W_0_, and the
M_v_-value derived from the apparent magnitude and parallax.
Table 1 is divided into three sections: Table1a.dat contains stars
with Ca II emission index 2 from Wilson (1976ApJ...205..823W);
Table1b.dat contains stars of index 1 from the same source; and
Table1c.dat contains stars in Wilson (1967PASP...79...46W). The
complete data set has been used to plot fig1.gif, where we show M_v_
plotted against log W_0_, the same coordinates used by Wilson & Bappu
(1957ApJ...126...46W). Because of the crowding we do not show the
probable errors of each point in this plot.