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J/PASP/111/335  CaII-Mv Correlation (Wilson-Bappu Effect) (Wallerstein+ 1999)

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
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 Mv=+7 to -2. For stars brighter than Mv=-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 Mv = 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 Mv-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 Mv - log W0 relation, where W0 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 W0-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 W0, and the Mv-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 Mv plotted against log W0, 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. File Summary:
FileName Lrecl Records Explanations
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 30 Mostly Lower Luminosity Stars with Ca II Emission and Hipparcos Parallaxes (Wilson 1967) fig1.gif 1 65587 *695 x 639 GIF image of Dependence of Mv as derived from Hipparcos parallaxes on log W0 fig2.gif 1 49152 695 x 639 GIF image of Dependence of the deviation from the mean line, delta log W0, on Wilson's estimated intensity of Ca II emission fig3.gif 1 51575 695 x 639 GIF image of Dependence of delta log W0 on spectral type fig4.gif 1 102442 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 1 109958 653 x 853 GIF image of Sample profiles of the Ca II H line and Hepsilon
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 ----------------------------------------------- Star (HD) Spectral Type log W0 Mv 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 Mv log W0 Observatory ------------------------------------------------------------------------ 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 ----------------------------------------------------------- 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
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD number 8- 12 F5.2 mas plx Trigonometric 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 W0 50- 54 F5.2 mag Mv Mv-value derived from the apparent magnitude and parallax
See also: I/239 : The Hipparcos and Tycho Catalogues (ESA 1997) Byte-by-byte Description of file: table1b.dat, table1c.dat
Bytes Format Units Label Explanations
1- 6 I6 --- HD HD number 8- 13 F6.2 mas plx Trigonometric 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 W0 49- 53 F5.2 mag Mv Mv-value derived from the apparent magnitude and parallax
Acknowledgements: Dr. George Wallerstein Department of Astronomy University of Washington Seattle, WA 98195 References: Burstein, D., & Heiles, C. 1982, AJ, 87, 1165 =1982AJ.....87.1165B Dupree, A. K. 1986, ARA&A, 24, 377 =1986ARA&A..24..377D ESA. 1997, The Hipparcos and Tycho Catalogues (ESA SP-1200) Griffin, R. F. 1968, A Photometric Atlas of the Spectrum of Arcturus (Cambridge: Cambridge Philos. Soc.) Griffin, R. F. 1998, Observatory, 118, 145 =1998Obs...118..145G Kovalevsky, J. 1998, ARA&A, 36, 99 =1998ARA&A..36...99K Lutz, T. E., & Kelker, D. H. 1973, PASP, 85, 573 (L-K) =1973PASP...85..573L Lutz, T. E., & Kelker, D. H. 1975, PASP, 87, 617 =1975PASP...87..617L Neckel, Th., Klare, G., & Sarcander, M. 1980, A&AS, 42, 251 =1980A&AS...42..251N Scoville, F., & Mena-Werth, J. 1998, PASP, 110, 794 (SM-W) =1998PASP..110..794S Warner, B. 1967, MNRAS, 137, 119 =1967MNRAS.137..119W Wilson, O. C. 1957, ApJ, 126, 46 =1957ApJ...126...46W Wilson, O. C. 1959, ApJ, 130, 499 =1959ApJ...130..499W Wilson, O. C. 1967, PASP, 79, 46 =1967PASP...79...46W Wilson, O. C. 1976, ApJ, 205, 823 =1976ApJ...205..823W Wilson, O. C., & Bappu, M. K. V. 1957, ApJ, 125, 661 =1957ApJ...125..661W Zarro, D. M., & Rogers, A. W. 1983, ApJS, 53, 815 =1983ApJS...53..815Z
(End) Gail L. Schneider [SSDOO/ADC] 18-July-1999
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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