H gamma and h delta Absorption Features in Stars and Stellar Populations Guy Worthey, & D. L. Ottaviani 1997, Astrophysical Journal Supplement Series, in press The catalog consists of 2 files. This is File 1



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H gamma and H delta Absorption Features in Stars and Stellar Populations Guy Worthey, & D. L. Ottaviani 1997, Astrophysical Journal Supplement Series, in press The catalog consists of 2 files. This is File 1. File 2 contains average index measurements and atmospheric parameters. Please copy both of these files when duplicating the catalog. This computer-readable distribution is meant to summarize ALL of the data on stellar absorption features published in the "Old Stellar Populations" series (Faber et al. 1985, Burstein et al. 1986, Gorgas et al. 1993, hereafter G93, and Worthey et al. 1994), as well as the current Worthey & Ottaviani paper, which deals with 4 additional Balmer absorption indices. The main body of data consists of 21+4 absorption feature indices measured in 460 stars. Additional entries give temperatures, gravities, and metal abundances for most stars, along with notes on the literature cited or method used for parameter estimation. The strength of absorption features in stellar spectra are measured in terms of "indices" in which a "feature" bandpass is defined centered on the feature of interest, flanked to the blue and the red by "pseudocontinuum" bandpasses. The average flux (in wavelength units) is found for the flanking pseudocontinua, and a straight line is drawn between the centers of the pseudocontinua. The portion of this line which lies over the "feature" bandpass is the "continuum" from which the index is measured by integrating the ratio of feature/continuum flux over the feature bandpass. The indices are expressed in two ways. For narrow features primarily due to atomic species, the index is given as an equivalent width (EW) in Angstroms. For broader features which measure molecular line absorption, the index is expressed a flux ratio in magnitudes. The table below summarizes the 25 index definitions. Note that the wavelength definitions have been revised from Worthey et al. 1994 through comparison with spectra with better wavelength calibrations. The listed wavelength definitions are accurate to 0.4 Angstroms. The CN2 index duplicates the CN1 index too closely to be useful, except possibly for the study of starburst galaxies. For early-type galaxies the authors prefer CN1 over CN2, and will adopt the CN1 definition in the future to measure this feature. Table 1: Index Definitions ------------------------------------------------------------------------- Name Feature Bandpass Pseudocontinua Units IDS Error ------------------------------------------------------------------------- 01 CN 1 4142.125-4177.125 4080.125-4117.625 mag 0.021 4244.125-4284.125 02 CN 2 4142.125-4177.125 4083.875-4096.375 mag 0.023 4244.125-4284.125 03 Ca4227 4222.250-4234.750 4211.000-4219.750 Ang 0.27 4241.000-4251.000 04 G4300 4281.375-4316.375 4266.375-4282.625 Ang 0.39 4318.875-4335.125 05 Fe4383 4369.125-4420.375 4359.125-4370.375 Ang 0.53 4442.875-4455.375 06 Ca4455 4452.125-4474.625 4445.875-4454.625 Ang 0.25 4477.125-4492.125 07 Fe4531 4514.250-4559.250 4504.250-4514.250 Ang 0.42 4560.500-4579.250 08 Fe4668 4634.000-4720.250 4611.500-4630.250 Ang 0.64 4742.750-4756.500 09 H beta 4847.875-4876.625 4827.875-4847.875 Ang 0.22 4876.625-4891.625 10 Fe5015 4977.750-5054.000 4946.500-4977.750 Ang 0.46 5054.000-5065.250 11 Mg 1 5069.125-5134.125 4895.125-4957.625 mag 0.007 5301.125-5366.125 12 Mg 2 5154.125-5196.625 4895.125-4957.625 mag 0.008 5301.125-5366.125 13 Mg b 5160.125-5192.625 5142.625-5161.375 Ang 0.23 5191.375-5206.375 14 Fe5270 5245.650-5285.650 5233.150-5248.150 Ang 0.28 5285.650-5318.150 15 Fe5335 5312.125-5352.125 5304.625-5315.875 Ang 0.26 5353.375-5363.375 16 Fe5406 5387.500-5415.000 5376.250-5387.500 Ang 0.20 5415.000-5425.000 17 Fe5709 5696.625-5720.375 5672.875-5696.625 Ang 0.18 5722.875-5736.625 18 Fe5782 5776.625-5796.625 5765.375-5775.375 Ang 0.20 5797.875-5811.625 19 Na D 5876.875-5909.375 5860.625-5875.625 Ang 0.24 5922.125-5948.125 20 TiO 1 5936.625-5994.125 5816.625-5849.125 mag 0.007 6038.625-6103.625 21 TiO 2 6189.625-6272.125 6066.625-6141.625 mag 0.006 6372.625-6415.125 22 H del_A 4083.500-4122.250 4041.600-4079.750 Ang 0.64 4128.500-4161.000 23 H gam_A 4319.750-4363.500 4283.500-4319.750 Ang 0.48 4367.250-4419.750 24 H del_F 4091.000-4112.250 4057.250-4088.500 Ang 0.40 4114.750-4137.250 25 H gam_F 4331.250-4352.250 4283.500-4319.750 Ang 0.33 4354.750-4384.750 ------------------------------------------------------------------------- File 2 of this distribution, which contains average index measurements and atmospheric parameters is organized as follows: Table 2: File 2 Format ------------------------------------------------------------------------- col. bytes format ------------------------------------------------------------------------- 1 1-10 A10 HD (Henry Draper Catalog) number, if any. 2 11-25 A15 Alternate names for the star. These could be "HR" 3 26-39 A14 numbers (Bright Star Catalog; Hoffleit 1982), "BD" (Bonner Durchmusterung) numbers, "Gl" numbers (Nearby Stars; Gleise 1969), cluster names (see the Appendix of this work), or common names. This is not a complete cross-reference list. 4-28 40-239 25(F8) Index values, units indicated in the above table. 29 240-249 I10 Effective temperature (source in column 29). 30 250-257 F8 Logarithm of the surface gravity in cm/s^2 (source in column 30). 31 258-265 F8 [Fe/H] (source in column 31). 32 266-269 I4 Number of observations. This number is the upper limit to the actual number of measurements which went into the index averages, as some portions of some spectra were missing or otherwise unusable. 33-35 270-281 3(I4) Sources for effective temperature, gravity, and [Fe/H], respectively. 36 282-360 A79 Spectral type and comment, if any. --------------------------------------------------------------------------- Here is a sample line, which can be used as a header for File 2: HD name1 name2 CN 1 CN 2 Ca4227 G 4300 Fe4383 Ca4455 Fe4531 Fe4668 HB4681 Fe5015 Mg 1 Mg 2 Mg b Fe5270 Fe5335 Fe5406 Fe5709 Fe5782 Na5895 TiO 1 TiO 2 H del_A H gam_A H del_F H gam_F Te log g [Fe/H] NObs ---notes--- Spectral type and comments --------------------------------------------------------------------------- Notes on temperature, gravity, and [Fe/H] (columns 33-35): The first several are from Table 2 of G93: 1. Laird (1985) 2. Cayrel de Strobel et al. (1980) 3. Wallerstein (1961) 4. Peterson & Carney (1979) 5. Johnson et al. (1968) 6. Peterson (1981) 7. Yale Bright Star Catalog 4th ed. (Hoffleit 1982) 8. Dickow et al. (1970) 10. Clegg et al. (1981) 13. Cayrel de Strobel et al. (1985) 16. Gliese (1969) 17. Computed in G93 using log g from theoretical models (VandenBerg 1983) versus Te (Veeder 1974) and/or Mbol (Mv from Gliese (1969); BC from Johnson (1966) versus spectral type). 18. Hearnshaw (1974a,b; 1976a,b) Most cluster parameters are from Table 4 of G93: 19. [Fe/H] for NGC 188 VandenBerg (1985) 20. [Fe/H] for NGC 7789 [Fe/H]hyades = -0.25, Twarog & Tyson (1985) 21. [Fe/H] for M67,M71 Burstein et al. (1986) 22. [Fe/H] for Hyades Boesgaard & Friel, (1990) 23. [Fe/H] for M3,M5,M10,M13,M92 Kraft (1979) 24. [Fe/H] for Coma cluster Boesgaard (1987) 25. Gravities estimated using VandenBerg (1983;1985) isochrones, as in G93 26. [Fe/H]o taken from from Faber et al. (1985) 27. Te, log g, [Fe/H] from Gilroy et al. (1988) 28. Te, log g, [Fe/H] from Danford & Lea (1981) 29. Te derived from the relation given by Saxner & Hammarback (1985): Te = 8065 - 3580(B-V)(1 - 0.196[Fe/H]) 0.30 0.05, and 3 for hotter stars. Log g was then calculated from fundamental parameters. Mass assumed 0.65 Mo, distance moduli from Table 4 of G93 or Table A3 of this work. 76. Metallicity of NGC 6171 = M101 from Zinn & West (1984). 77. Temperature of cool supergiant HR 8752 assigned on the basis of spectral type. Johnson (1966). Spectral type is apparently varying with time. 78. Temperatures from Veeder (1974). 79. [Fe/H] an average of Brown et al. (1989) and McWilliam (1990). 80. Parameters from Gratton & Sneden (1991). 81. HR 4365: [Fe/H] and log g from Helfer & Wallerstein (1968). Hyades [Fe/H] assumed +0.13 (Boesgaard & Friel 1990). Temperature is an average of that of Helfer & Wallerstein (1968) from 6-color photometry (4253 K) and that deduced from B-V via Johnson (1966) and Ridgway et al. (1980) (4450 K). Note that the V-K value quoted for this star in Faber et al. (1985) is fictitious (though close to correct), as the star does not appear in the quoted source (Johnson et al. 1966). Also note that the temperature for this star quoted in Cayrel de Strobel et al. (1992) is too low, and should be THETA = 1.185 (not 1.32). --------------------------------------------------------------------------- References: Adelman, S.J., & Hill, G. 1987, MNRAS, 226,581 Boesgaard, A.M. 1987, ApJ, 321,967 Boesgaard, A.M., & Friel, E.D., 1990, ApJ, 351,467 Bohm-Vitense, E. 1981, ARAA, 19,295 Brown, J.A., Sneden, C., Lambert, D.L., & Dutchover, E.Jr. 1989, ApJS, 71,293 Burstein, D., Faber, S.M., & Gonzalez, J.J. 1986, AJ, 91,1130 Carney, B.W. 1983, AJ, 88,623 Cayrel de Strobel, G., Bentolila, C., Hauck, B., & Curchod, A. 1980, A&AS, 41,405 Cayrel de Strobel, G., Knowles, N., Hernandez, G., & Bentolila, C. 1981, A&A, 94,1 Cayrel de Strobel, G., Bentolila, C., Hauck, B., & Duquennoy, A. 1985, A&AS, 59,145 Cayrel de Strobel, G., Hauck, B., Francois, P., Thevenin, F., Friel, E.D., Mermilliod, M., & Borde, S. 1992, A&AS, 95,273 Clegg, R.E.S., Lambert, D.C., & Tomkin, J. 1981, ApJ, 250,262 Danford, S.C., & Lea, S.M. 1981, AJ, 86,1909 de Jagar, C., Nieuwenhuijzen, H., & van der Hucht, K.A. 1988, A&AS, 72,259 Dickow, P., Gyldenkerne, K., Hansen, L., Jacobsen, P.-U., Johansen, K.T., Kjaergaard, P., & Olsen, E.H. 1970, A&AS, 2,1 Eggen, O.J. 1991, AJ, 102,1826 Faber, S.M., Friel, E.D., Burstein, D., & Gaskell, C.M. 1985, ApJS, 57,711 Fernley, J.A., Skillen, I., & Jameson, R.F. 1989, MNRAS, 237,947 Ferro, A.A., Parrao, L., & Giridhar, S. 1988, PASP, 100,993 Gleise, W. 1969, Catalogue of Nearby Stars, Veroff. 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L. 1997, ApJS, in press Zinn, R., & West, M. 1984, ApJS, 55,45 ---------------------------------------------------------------------------

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