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J/PASP/111/335 Ca II-M_v Correlation (Wilson-Bappu Effect) (Wallerstein+ 1999)
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The Ca II-M_v 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 1998) 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 (1976) 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 (1967,
1976). Other databases are available, e.g., Warner (1967) and Zarro & Rogers
(1983), 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). 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 (1976); Table1b.dat contains stars of index
1 from the same source; and Table1c.dat contains stars in Wilson (1967).
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 (1957).
Because of the crowding we do not show the probable errors of each point
in this plot.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1a.dat 54 390 Stars with Ca II Emission of Intensity Index
>=2 and Hipparcos Parallaxes (Wilson 1976)
table1b.dat 53 250 Stars with Ca II Emission of Intensity Index
1 and Hipparcos Parallaxes (Wilson 1976)
table1c.dat 53 32 Mostly Lower Luminosity Stars with Ca II
Emission and Hipparcos Parallaxes
(Wilson 1967)
fig1.gif - - *695 x 639 GIF image of Dependence of M_v as
derived from Hipparcos parallaxes on log W_0
fig2.gif - - 695 x 639 GIF image of Dependence of the
deviation from the mean line, delta log W_0,
on Wilson's estimated intensity of Ca II
emission
fig3.gif - - 695 x 639 GIF image of Dependence of delta log
W_0 on spectral type
fig4.gif - - 653 x 853 GIF image of Sample profiles of the
Ca II K line. Note the apparent emission
features at 3936.0 and 3938.3 angstroms due
to Fe II in some stars
fig5.gif - - 653 x 853 GIF image of Sample profiles of the
Ca II H line and Hepsilon
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Note on fig1.gif:
An unweighted least-squares fit to the data is shown as a solid line. The
dashed line shows a least-squares fit with the points weighted by
parallax/probable error. Circles represent stars with parallax >
(10xprobable error); triangles represent stars with (10xprobable error) >
parallax > (5xprobable error). Stars within the parallelogram are described
in Table 2. The symbols have the same meaning in fig2.gif and fig3.gif.
Table 2
Stars within the Box in fig1.gif
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Star (HD) Spectral Type log W_0 M_v Trig.
-----------------------------------------------
16901 G0 Ib 2.15 -1.20
20123 G5 III 2.10 -2.00
26630 G0 Ib 2.15 -2.61
74395 G1 Ib 2.12 -1.71
92125 G3 Ib-II 2.07 -1.13
159181 G2 II 2.19 -2.43
173764 G4 II 2.11 -2.41
204075 G4 Ibp* 2.07 -1.66
204867 G0 Ib 2.16 -3.47
209750 G2 Ib 2.20 -3.88
210745 K1 Ib 2.16 -3.35
222574 G0 Ib 2.09 -1.65
* A well-known Ba II star.
Table A1
Properties of Stars Whose Spectra are Displayed in fig4.gif and fig5.gif
------------------------------------------------------------------------
Spectral
Region Spectral
Star (angstroms) Type M_v log W_0 Observatory
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Boo 3933,68 K2 IIIp -0.31 1.83 DAO
UMa 3933,68 K0 III -1.08 1.84 DAO
Leo A 3933 K1 III -0.92 1.82 DAO
Dra 3968 K2 +0.81 1.75 DAO
Vir 3968 M1 III -0.87 1.86 McD
Cyg 3933,68 K5 Ib-II -4.07 1.83 McD
Aqr 3933,68 G2 Ib -3.88 2.20 McD
56 Leo 3933 M5 II +0.92 1.93 McD
Table A2
Measured Wavelengths of Suspected Emission Lines Other than the
Ca II, H and K Lines
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Star HD H 3970.05 Fe II 3935.94 Fe II 3938.27
-----------------------------------------------------------
89484** 69.90 37.81
94705* 71.63 35.96
95689** 70.11 37.82
102212* 70.38 35.94
121299* 70.47
124897* 70.14
124897** 70.18 35.80 37.88
133165* 69.73 35.55
137759** 69.99
200905* 69.31 35.60 37.75
209750* 35.70 38.20
* Spectrum obtained at Dominion Astrophysical Observatory.
** Spectrum obtained at McDonald Observatory.
Byte-by-byte Description of file: table1a.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HD HD number
8- 12 F5.2 mas plx Parallax
14- 17 F4.2 mas e_plx Parallax probable error
19- 21 F3.1 mag Vmag V magnitude
23- 31 A9 --- SpType Spectral Type
33- 36 F4.2 mag B-V B-V color
38- 41 F4.2 mag V-I V-I color
43 I1 --- Int_idx [2-5] Intensity index
45- 48 F4.2 --- logW log W_0
50- 54 F5.2 mag Mv M_v-value derived from the apparent
magnitude and parallax
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Byte-by-byte Description of file: table1b.dat, table1c.dat
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Bytes Format Units Label Explanations
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1- 6 I6 --- HD HD number
8- 13 F6.2 mas plx Parallax
15- 18 F4.2 mas e_plx Parallax probable error
20- 22 F3.1 mag Vmag V magnitude
24- 32 A9 --- SpType Spectral Type
34- 37 F4.2 mag B-V B-V color
39- 42 F4.2 mag V-I V-I color
44- 47 F4.2 --- logW log W_0
49- 53 F5.2 mag Mv M_v-value derived from the apparent
magnitude and parallax
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Acknowledgements:
Dr. George Wallerstein
Department of Astronomy
University of Washington
Seattle, WA 98195
wall@astro.washington.edu
References:
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Griffin, R. F. 1998, Observatory, 118, 145 =1998Obs...118..145G
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(End) Gail L. Schneider [SSDOO/ADC] 18-July-1999