Old Stellar Populations V.
Absorption Feature Indices for the Complete Lick/IDS Sample of Stars

Guy Worthey, S.M. Faber, J. Jesus Gonzalez, & D. Burstein
Astrophysical Journal Supplement Series 1994, v. 94 p. 687

   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, and
Gorgas et al. 1993, hereafter G93, and Worthey et al. 1994). The main
body of data consists of 21 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 21 index definitions.

   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      4143.375-4178.375   4081.375-4118.875   mag     0.021
                                 4245.375-4285.375
02 CN 2      4143.375-4178.375   4085.125-4097.625   mag     0.023  new
                                 4245.375-4285.375
03 Ca4227    4223.500-4236.000   4212.250-4221.000   Ang     0.27   new
                                 4242.250-4252.250
04 G4300     4282.625-4317.625   4267.625-4283.875   Ang     0.39
                                 4320.125-4336.375
05 Fe4383    4370.375-4421.625   4360.375-4371.625   Ang     0.53   new
                                 4444.125-4456.625
06 Ca4455    4453.375-4475.875   4447.125-4455.875   Ang     0.25   new
                                 4478.375-4493.375
07 Fe4531    4515.500-4560.500   4505.500-4515.500   Ang     0.42   new
                                 4561.750-4580.500
08 Fe4668    4635.250-4721.500   4612.750-4631.500   Ang     0.64   new
                                 4744.000-4757.750
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   new
                                 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   new
                                 5415.000-5425.000
17 Fe5709    5698.375-5722.125   5674.625-5698.375   Ang     0.18   new
                                 5724.625-5738.375
18 Fe5782    5778.375-5798.375   5767.125-5777.125   Ang     0.20   new
                                 5799.625-5813.375
19 Na D      5878.625-5911.125   5862.375-5877.375   Ang     0.24 
                                 5923.875-5949.875
20 TiO 1     5938.375-5995.875   5818.375-5850.875   mag     0.007
                                 6040.375-6105.375
21 TiO 2     6191.375-6273.875   6068.375-6143.375   mag     0.006
                                 6374.375-6416.875
-------------------------------------------------------------------------

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.
4-24  40-207  21(F8) Index values, units indicated in the above table.
25    208-217 I10    Effective temperature (source in column 29).
26    218-225 F8     Logarithm of the surface gravity in cm/s^2 (source 
                     in column 30).
27    226-233 F8     [Fe/H] (source in column 31).
28    234-237 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.
29-31 238-249 3(I4)  Sources for effective temperature, gravity, and [Fe/H], 
                     respectively.
32    250-328 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       Te   log g  [Fe/H] NObs ---notes---  Spectral type and comments



---------------------------------------------------------------------------
Notes on temperature, gravity, and [Fe/H] (columns 29-31):

    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<B-V<0.63
30. Te an average from linear interpolation in Johnson (1966). Both
    B-V and R-I were averaged, B-V given twice the weight. For Hyads
    vB 64, and vB 73, V-K was used instead of B-V.
31. Te from linear interpolation in Table 3 of Bohm-Vitense (1981),
    using the lower temperature scale where appropriate because
    it agrees with that of Saxner and Hammarback (1985).
32. Gravities estimated from fundamental parameters Te, M, L. Bolometric
    corrections from Johnson (1966), adjusted to VandenBerg's solar BC
    of -0.12. Masses estimated using VandenBerg isochrones of ages 0.4 (Coma),
    0.7 (Hyades) Gyr.
33. Temperature from the Carney (1983) calibration of THETA-effective
    versus V-K. Valid for dwarfs of any metallicity and 4500<Te<7000:
    The  relation is THETAe = 0.245(V-K) + 0.514. We have found that
    this scale doesn't agree at the hot end with Saxner & Hammarback (1985) or
    Bohm-Vitense (1981). We therefore do not use this calibration for stars 
    hotter than V-K=1.00. It does agree with Johnson (1966) at the cool end.
34. Te, log g, [Fe/H] from Adelman & Hill (1987).
35. log g from Stromgren c1 photometry (calibration of Laird 1985).
    Mean photometry from the ubvyBeta Photoelectric Photometric Catalog
    of Hauck and Mermilliod (1990), computer readable version.
36. Te from fitting functions for (R-I)j in Carney (1983, Appendix I).
37. Straight mean from Cayrel de Strobel et al. (1992).
38. Te from fitting functions for (b-y) in Carney (1983, Appendix I).
40. log g as a function of spectral type, Landolt-Bornstein (1982).
41. Te from linear B-V interpolation in Table 4 of Bohm-Vitense (1981).
42. Te, log g, [Fe/H] from Luck and Bond (1982).
43. log g estimated from color-log g relations defined by Hyades and 
    Coma clusters
45. For HR 2135, Te is from Underhill et al. (1979). With a
    BCv = 0.13 - 0.12 = 0.01 (from Johnson 1966 corrected to
    BC(solar)=-0.12), we have V=4.62. With a true distance modulus of 10.57
    (1300 pc - Underhill et al.) and an visual extinction = 3*E(B-V) = 
    3*0.51 = 1.53 (E(B-V) from Greenberg and Chlewicki (1983)),
    we have an absolute magnitude of -7.48. Reading from
    Figure 1 of Schaller et al. (1992), we estimate a mass of 17
    solar masses for this star. The gravity from fundamental relations
    is then 2.70.
46. [Fe/H] estimated as in Laird (1985), using the Stromgren m1 index.
47. Average of methods 36 and 38.
48. Te and log g from Ferro, Parrao, and Giridhar (1988).
49. Te and log g estimated from c1 and Beta, from the graphs of Moon and 
    Dworetsky (1985). For stars later than A0, if the Te obtained 
    by this method differed by more than 200 K from Bohm-Vitense's 
    (1981, Table 3) value, the latter was adopted, and log g rederived.
50. [Fe/H] from Cayrel de Strobel et al. (1981).
51. [Fe/H] from Herbig & Wolff (1966).
52. Te and log g from Malagnini & Morossi (1990).
53. [Fe/H] from Gustafsson & Nissen (1972).
54. Te from Gray & Johanson (1991).
55. Parameters from Luck, Bond, & Lambert (1990). Te and log g are 
    photometrically determined.
56. Te determined by Gulati, Malagnini, & Morossi (1989).
57. Average Te, Mbol, M(evolutionary) and R from Fernley, Skillen, & 
    Jameson (1989).
58. [Fe/H] from Klochkova & Panchuk (1991). [Fe/H] is solar within the 
    uncertainties in transforming from the metallicity scale they employed.
59. [Fe/H] from Hearnshaw (1974a).
60. Te and log L from de Jager et al. (1988). M estimated from
    the tracks of Schaller et al. (1992) to derive log g. 
    (Derived values: HR7678, M=40; HR7977, M=22; HR825, M=18)
61. From Eggen (1991). Te estimated using [c1] and Beta 
    and the grid of Moon & Dworetsky (1985). log g and P[Fe/H] are
    derived by Eggen.
62. Te and log g from Leitherer & Wolf (1984).
63. Te from (B-V)o as a function a spectral type from Landolt-Bornstein (1982),
    converted to Te via Bohm-Vitense (1981).
64. [Fe/H] from Kuroczkin & Wiszniewski (1977).
65. Te from the spectral-type-vs.-Te relation of Ridgway, Joyce, White
    and Wing (1980, hereafter RJWW) for M giants.
66. Te from V-K. For giants, calibration is RJWW's, plus one point at 5010 K
    from Johnson (1966), plus hotter points from the same reference, but
    from the dwarf table. Interpolation was linear. For dwarfs and subgiants, 
    Johnson (1966) calibration was used. Input V-K is, in some cases, a 
    transformation from B-V (see G93 for details).
67. The red dwarfs BD +19 5116 A and B were assigned temperatures according
    to their spectral types from Johnson (1966).
68. Te from Tsuji (1986) based on angular diameters
    from Ridgway et al. (1982). [C/H] from the Tsuji analysis. log g = 0 is a
    reasonable guess, good to plus or minus 0.5 dex.
69. Gravity estimated in G93 from the Mg2 index.
70. Leep & Wallerstein (1981).
71. Brown et al. (1989).
72. Smith & Lambert (1985).
73. Gravity for supergiant HR 8752 was taken to be near its evolutionary
    value of 0.0, taken from Luck (1975).
74. Some late M giants were assumed to have gravities near 0, which is a 
    typical value.
75. Effective temperature and bolometric correction from B-V via the 
    Kurucz (1992) color grids. For the Te/BC derivation
    log g was assumed to be 2 for B-V > 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. Astr. Rechen-Inst. 
   Heidelberg No. 22
Gilroy, K.K., Sneden, C., Pilachowski, C.A., & Cowan, J.J. 1988, ApJ, 327,298
Gorgas, J., Faber, S.M., Burstein, D., Gonzalez, J.J., Courteau, S., & 
   Prosser, C. 1993, ApJS, 86,153 (G93)
Gratton, R.G. & Sneden, C. 1991, A&A, 241,501
Gray, D.F. & Johanson, H.L. 1991, PASP, 103,439
Greenberg, J.M., & Chlewicki, G. 1983, ApJ, 272,563
Gulati, R.K., Malagnini, M.L., & Morossi, C. 1989, A&AS, 80,73
Gustafsson, B., & Nissen, P.E. 1972, A&A, 19,261
Hauck, B., & Mermilliod, M. 1990, A&AS, 86,107
Hearnshaw, J.B. 1974a, A&A, 34,263
Hearnshaw, J.B. 1974b, A&A, 36,191
Hearnshaw, J.B. 1976a, A&A, 51,71
Hearnshaw, J.B. 1976b, A&A, 51,85
Helfer, H.L., & Wallerstein, G. 1968, ApJS, 16,1
Herbig, G.H., & Wolff, R.J. 1966, Ann. Astrophys., 29,593
Hoffleit, D. 1982, The Bright Star Catalog, 4th ed., (New Haven:Yale 
   University Observatory)
Johnson, H.L. 1966, ARA&A, 4,193
Johnson, H.L., MacArthur, J.W., & Mitchell, R.I., 1968, ApJ, 152,465
Johnson, H.L., Mitchell, R.I., Iriarte, B., & Wisniewski, W.Z. 1966, Comm.
   Lunar Planet. Lab., 4,99
Klochkova, V.G., & Panchuk, V.E. 1991, Soviet Astronomy Letters, 17,229
Kraft, R.P., 1979, ARA&A, 17,309
Kuroczkin, D., & Wiszniewski, A., 1977, Acta. Astron., 27,145
Kurucz, R.L. 1992, private communication
Laird, J.B. 1985, ApJS, 57,389
Landolt-Bornstein 1982, Numerical Data and Functional Relationships in 
   Science and Technology, Vol. 2b, eds. K. Scaifers & H.H. Voigt, 
   (Springer-Verlag)
Leep, E.M., & Wallerstein, G. 1981, MNRAS, 196,543
Leitherer, C., & Wolf, B. 1984, A&A, 132,151
Luck, R.E. 1975, ApJ, 202,743
Luck, R.E., & Bond, H.E. 1982, ApJ, 263,215
Luck, R.E., Bond, H.E., & Lambert, D.L. 1990, ApJ, 357,188
Malagnini, M.L., & Morossi, C., 1990, A&AS 85,1015
McWilliam, A. 1990, ApJS, 74,1075
Moon, T.T., & Dworetsky, M.M. 1985, MNRAS 217,305
Peterson, R.C. 1981, ApJS, 45,421
Peterson, R.C., & Carney, B.W. 1979, ApJ, 231,762
Ridgway, S.T., Joyce, R.R., White, N.M., & Wing, R.F. 1980, ApJ, 235,126 (RJWW)
Ridgway, S.T., Jacoby, G.H., Joyce, R.R., Siegel, M.J., & Wells, D.C. 1982, 
   AJ, 87,808
Saxner, M., & Hammarback, G. 1985, A&A, 151,372
Schaller, G., Schaerer, D., Meynet, G., & Maeder, A. 1992, A&AS, 96,269
Smith, V.V., & Lambert, D.L. 1985, ApJ, 294,326
Tsuji, T. 1986, A&A, 156,8
Twarog, B.A., & Tyson, N. 1985, AJ, 90,1247
Underhill, A.B., Divan, L., Prevot-Burnichon, M.-L., & Doazan, V. 1979, 
   MNRAS, 189,601
VandenBerg, D.A. 1983, ApJS, 51,29
VandenBerg, D.A. 1985, ApJS, 58,711
Veeder, G.J. 1974, AJ, 79,1056
Wallerstein, G. 1961, ApJS, 6,407
Worthey, G., Faber, S.M., Gonzalez, J.J., & Burstein, D. 1994, ApJS, ---,---
Zinn, R.,  & West, M. 1984, ApJS, 55,45
---------------------------------------------------------------------------