Spectroscopic Studies of Extremely Metal-Poor Stars with the Subaru High Dispersion Spectrograph. I. Observational Data

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SPECTROSCOPIC STUDIES OF EXTREMELY METAL-POOR STARS WITH THE SUBARU HIGH
DISPERSION SPECTROGRAPH. I. OBSERVATIONAL DATA1
Satoshi Honda,2,3Wako Aoki,2,3Hiroyasu Ando,2Hideyuki Izumiura,4Toshitaka Kajino,2,3Eiji Kambe,5
Satoshi Kawanomoto,2Kunio Noguchi,2,3Kiichi Okita,4Kozo Sadakane,6Bun’ei Sato,2,7
Masahide Takada-Hidai,8Yoichi Takeda,2,9Etsuji Watanabe,4Timothy C. Beers,10
John E. Norris,11and Sean G. Ryan12
Received 2003 July 10; accepted 2004 January 27
ABSTRACT
We have obtained high-resolution (R ’ 50;000 or 90,000), high-quality (S=N k100) spectra of 22 very metal-
poor stars ([Fe/H?P ? 2:5) with the High Dispersion Spectrograph fabricated for the 8.2 m Subaru Telescope.
The spectra cover the wavelength range from 3500 to 5100 8; equivalent widths are measured for isolated lines
of numerous elemental species, including the ?-elements, the iron-peak elements, and the light and heavy
neutron-capture elements. Errors in the measurements and comparisons with previous studies are discussed.
These data will be used to perform detailed abundance analyses in the following papers of this series. Radial
velocities are also reported and are compared with previous studies. At least one moderately r-process–enhanced
metal-poor star, HD 186478, exhibits evidence of a small-amplitude radial velocity variation, confirming the
binary status noted previously. During the course of this initial program, we have discovered a new moderately
r-process–enhanced, very metal-poor star, CS 30306?132 ([Fe/H? ¼ ?2:4; [Eu/Fe? ¼ þ0:85), which is discussed
in detail in the companion paper.
Subject headings: nuclear reactions, nucleosynthesis, abundances — stars: abundances — stars: Population II
On-line material: machine-readable table
1. INTRODUCTION
Very metal-poor stars ([Fe/H? P ? 2:5)13are believed to
have been born in the early Galaxy; their chemical composi-
tions are living records of the nucleosynthesis processes that
preceded their formation. As a result of considerable efforts
by many astronomers, a large list of candidate stars with
[Fe/H? < ?2:5 have been provided by wide-field objective-
prism surveys in the past two decades (e.g., the HK survey:
Beers, Preston, & Shectman 1985, 1992, Beers 1999; and the
Hamburg/ESO Survey: Christlieb & Beers 2000, Christlieb
et al. 2001, Christlieb 2003). Over the past several years, high-
resolution spectroscopic studies have enabled the measure-
ment of elemental abundances for many of the metal-poor
stars found by these surveys (e.g., McWilliam et al. 1995a;
Ryan, Norris, & Beers 1996; Burris et al. 2000; Carretta et al.
2002; Cayrel et al. 2004), including detailed studies of the
lowest metallicity stars yet identified (e.g., Norris, Ryan, &
Beers 2001; Christlieb et al. 2002). These observational
studies, which continue at present, are providing strong con-
straints on models of the dominant nucleosynthesis processes
in the earliest epochs of star formation in our Galaxy, in
particular those associated with massive stars and Type II
supernovae.
Remarkable progress has been made, in particular, through
studies of the neutron-capture elements in very metal-poor
stars. High-resolution spectroscopic studies of very metal-
poor stars have revealed, for example, that a small fraction
(presently estimated to be on the order of 2%–3%, T. C. Beers
2003, private communication) of giants with ½Fe=H? < ?2:5
exhibit large overabundances (e.g., ½r-process=Fe? > þ1:0) of
neutron-capture elements associated with the r-process (e.g.,
[r-process/Fe? > þ1:0 ; McWilliam et al. 1995a; Sneden et al.
2000, 2003; Cayrel et al. 2001; Hill et al. 2002). These, along
with a handful of other metal-poor stars with moderately en-
hanced r-process elements (þ0:5 ? ½r-process/Fe? ? þ1:0,
e.g., Westin et al. 2000; Johnson & Bolte 2001; Cowan et al.
2002), display remarkably similar abundance patterns in the
range 56 ? Z < 76, all apparently in good agreement with
the solar-system r-process component. In addition, some of
1Based on data collected at Subaru Telescope, which is operated by the
National Astronomical Observatory of Japan.
2National Astronomical Observatory, Mitaka, Tokyo 181-8588, Japan;
honda@optik.mtk.nao.ac.jp,aoki.wako@nao.ac.jp,ando@optik.mtk.nao.ac.jp,
kajino@nao.ac.jp, kawanomo@optik.mtk.nao.ac.jp, knoguchi@optik.mtk.nao
.ac.jp.
3Department of Astronomy, Graduate University for Advanced Studies,
Mitaka, Tokyo 181-8588, Japan.
4Okayama Astrophysical Observatory, National Astronomical Observa-
tory of Japan, Kamogata-cho, Okayama 719-0232, Japan; izumiura@oao.nao
.ac.jp, okita@oao.nao.ac.jp, watanabe@oao.nao.ac.jp.
5Department of Earth and Ocean Sciences, National Defense Academy,
Hashirimizu 1-10-20, Yokosuka, Kanagawa 239-8686, Japan; kambe@nda
.ac.jp.
6Astronomical Institute, Osaka Kyoiku University, Kashiwara-shi, Osaka
582-8582, Japan; sadakane@cc.osaka-kyoiku.ac.jp.
7Department of Astronomy, School of Science, University of Tokyo,
Bunkyo-ku, Tokyo 113-0033, Japan; satobn@oao.nao.ac.jp.
8Liberal Arts Education Center, Tokai University, 1117 Kitakaname,
Hiratsuka-shi, Kanagawa 259-1292, Japan; hidai@apus.rh.u-tokai.ac.jp.
9Komazawa University, Komazawa, Setagaya, Tokyo 154-8525, Japan;
takedayi@cc.nao.ac.jp.
10Department of Physics and Astronomy, Michigan State University, East
Lansing, MI 48824–1116; beers@pa.msu.edu.
11Reseach School of Astronomy and Astrophysics, Australian National
University, Private Bag, Ewston Creek Post Office, Canberra, ACT 2611,
Australia; jen@mso.anu.edu.au.
12Department of Physics and Astronomy, Open University, Walton Hall,
Milton Keynes MK7 6AA, UK; s.g.ryan@open.ac.uk.
13We use the usual notation ½A=B? ? log10ðNA=NBÞ?? log10ðNA=NBÞ?
and log?ðAÞ ? log10ðNA=NHÞ þ 12:0, for elements A and B. Also, the term
‘‘metallicity’’ will be assumed here to be equivalent to the stellar [Fe/H] value.
A
113
The Astrophysical Journal Supplement Series, 152:113–128, 2004 May
# 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A.

Page 2

TABLE 1
Program Stars and Observation Log
NumberStar
VB?VR
S/Na
S/Nb
Exposure
(s)
1.................................
2.................................
3.................................
4.................................
5.................................
6.................................
7.................................
8.................................
9.................................
10...............................
11...............................
12...............................
13...............................
14...............................
15...............................
16...............................
17...............................
18...............................
19...............................
20...............................
21...............................
22...............................
HD 4306
HD 6268
HD 88609
HD 110184
HD 115444
HD 122563
HD 126587
HD 140283
HD 186478
BS 16082?129
BS 16085?050
BS 16469?075
BS 16920?017
BS 16928?053
BS 16929?005
BS 17583?100
CS 22169?035
CS 22183?031
CS 22892?052
CS 22952?015
CS 30306?132
CS 31082?001
9.08
8.10
8.59
8.31
8.97
6.20
9.15
7.21
9.18
13.55
12.15
13.42
13.88
13.47
13.61
12.37
12.88
13.62
13.18
13.27
12.81
11.67
0.63
0.79
0.93
1.17
0.78
0.91
0.73
0.49
0.90
0.67
0.74
0.77
0.76
0.85
0.62
0.51
0.92
0.65
0.78
0.78
0.80
0.77
90000
90000
90000
90000
90000
90000
90000
90000
100000
50000
50000
50000
50000
50000
50000
50000
50000
50000
90000
50000
50000
50000
272
158
62
221
255
374
187
458
158
55
100
59
41
49
56
79
49
47
60
59
85
100
497
288
113
403
466
683
341
836
274
135
245
145
100
120
137
194
120
115
147
145
208
122
1800
1800
2110
900
3900
1200
4500
3600
2400
5400
5100
5400
5400
5400
5400
3600
5400
9751
7200
9000
4493
1200
aS/N ratio per pixel at 4000 8.
bS/N ratio per resolution element at 4000 8.
TABLE 2
Coordinates and Radial Velocity
Number Star R.A. (J2000.0)Decl. (J2000.0)Observation Date
Vra
1...............................
2...............................
3...............................
4...............................
5...............................
5...............................
6...............................
6...............................
7...............................
7...............................
8...............................
8...............................
9...............................
10.............................
11.............................
12.............................
13.............................
14.............................
15.............................
16.............................
16.............................
17.............................
18.............................
18.............................
19.............................
20.............................
21.............................
22.............................
HD 4306
HD 6268
HD 88609
HD 110184
HD 115444
HD 115444
HD 122563
HD 122563
HD 126587
HD 126587
HD 140283
HD 140283
HD 186478
BS 16082?129
BS 16085?050
BS 16469?075
BS 16920?017
BS 16928?053
BS 16929?005
BS 17583?100
BS 17583?100
CS 22169?035
CS 22183?031
CS 22183?031
CS 22892?052
CS 22952?015
CS 30306?132
CS 31082?001
00 45 27.2
01 03 18.2
10 14 29.0
12 40 14.1
13 16 42.5
?09 32 40
?27 52 50
+53 33 39
+08 31 38
+36 22 53
2000 Aug 19
2000 Aug 18
2000 Nov 11
2001 Jan 29
2000 Jul 4
2001 Jan 28
2000 Jul 4
2001 Jan 29
2001 Jan 27
2001 Jan 31
2000 Jul 4
2000 Aug 17
2000 Aug 20
2001 Jan 30
2001 Jan 31
2001 Jan 28
2001 Jan 27
2001 Jan 28
2001 Jan 30
2000 Aug 19
2000 Aug 20
2000 Nov 11
2000 Nov 10
2000 Nov 11
2001 Jul 22
2000 Nov 11
2001 Jul 26
2001 Jul 30
?69.69 ? 0.29
39.20 ? 0.27
?37.28 ? 0.43
138.89 ? 0.27
?27.30 ? 0.34
?27.58 ? 0.25
?27.20 ? 0.33
?26.52 ? 0.34
148.72 ? 0.72
149.10 ? 0.24
?171.17 ? 0.29
?170.23 ? 0.19
30.52 ? 0.31
?92.16 ? 0.30
?75.06 ? 0.28
332.88 ? 0.74
?206.53 ? 0.84
?81.00 ? 0.35
?51.29 ? 0.43
?107.96 ? 0.32
?108.76 ? 0.42
17.72 ? 0.73
11.67 ? 0.67
11.97 ? 0.56
12.72 ? 0.49
?20.07 ? 0.71
109.01 ? 0.31
138.91 ? 0.30
14 02 31.9 +09 41 10
14 27 00.4
?22 14 39
15 43 03.1
?10 56 01
19 45 14.1
13 47 11.5
12 37 46.7
10 15 10.1
12 07 17.1
12 22 28.1
13 03 29.4
21 42 27.8
?17 29 27
+28 57 46
+19 22 44
+42 53 19
+41 39 35
+34 11 24
+33 51 06
+26 40 34
04 12 13.9
01 09 04.9
?12 05 05
?04 43 25
22 17 01.5
23 37 28.6
15 14 18.6
01 29 31.2
?16 39 26
?05 47 56
+07 27 02
?16 00 48
Note.—Units of right ascension are hours, minutes, and seconds, and units of declination are degrees, arcminutes, and arcseconds.
aHeliocentric radial velocity (km s?1).

Page 3

the neutron-capture–enhanced, metal-poor stars exhibit abun-
dance patterns associated with s-process nucleosynthesis (e.g.,
Norris, Ryan, & Beers 1997; Van Eck et al. 2001; Aoki et al.
2002; Lucatello et al. 2003).
These efforts are having a large collective impact on studies
on the origin of the neutron-capture elements in the Galaxy
(e.g., Ishimaru & Wanajo 1999; Fields, Truran, & Cowan
2002; Qian & Wasserburg 2002), and on the underlying
physics and astrophysical sites of the r- and s-processes (e.g.,
Gallino et al. 1998; Wanajo et al. 2002, 2003; Schatz et al.
2002; Truran et al. 2002). Furthermore, detailed studies of the
r-process–enhanced, very metal-poor stars have provided
new, potentially quite powerful, methods for obtaining hard
lower limits on the age of the Galaxy and the universe, from
the application of cosmo-chronometry based on the observed
(present-day) abundance ratios of radioactive nuclei (Th and
U), as compared with one another, and with stable elements
originating in the r-process, (e.g., Eu, Sneden et al. 1996;
Westin et al. 2000; Cayrel et al. 2001; Schatz et al. 2002;
Wanajo et al. 2002, 2003; Sneden et al. 2003).
In order to develop a more clear understanding of the in-
dividual nucleosynthetic processes that were operating in the
early Galaxy, further abundance studies are required, based on
high-quality spectra, for much larger samples of very metal-
poor stars than have been examined to date. We have initiated
such a set of investigations with the Subaru Telescope High
Dispersion Spectrograph (HDS, Noguchi et al. 2002). In this
paper we present observations of 22 very metal-poor stars
observed during the commissioning phase of this instrument.
In x 2 we discuss the selection of targets and details of the
observations that have been carried out. Our spectra cover the
wavelength range from 3500 to 5100 8 with high spectral
resolution (a resolving power of R ¼ 50;000 or 90,000) and
high signal-to-noise (S=N k100 per resolution element). We
report the equivalent widths measured for the spectra in x 3,
where we also discuss the random errors of our measurements
and make comparisons with previous studies of stars in
common. Radial velocity measurements for our program stars
are presented in x 4, along with a comparison with previous
measurements for a number of stars. These data will be used in
the detailed abundance analyses that will follow in additional
papers of this series.
2. OBSERVATIONS
2.1. Selection of Targets
The present work is focused primarily on the observed
abundance patterns of r-process elements in very metal-poor
stars. Accordingly, our sample was selected to include stars
that fall into one of several categories: (1) very metal-poor
stars that were previously known to exhibit extremely large
enhancements of their r-process elements (CS 22892?052 and
CS 31082?001: Sneden et al. 1996; Cayrel et al. 2001);
(2) bright metal-poor stars that were studied by previous
authors (e.g., McWilliam et al. 1995a; Burris et al. 2000) and
shown to be moderately r-process-element–rich; and (3) can-
didate very metal-poor giants discovered in the course of
the HK survey of Beers and colleagues (Beers et al. 1992;
Fig. 1.—Examples of spectra for nine stars in our sample over the wave-
length range 4000–4040 8. The star names and [Fe/H] values reported in
Paper II are presented in the figure. This spectral region includes the line of
Th ii at 4019 8; detections are indicated with a vertical arrow. The apparent
emission lines seen in some of the spectra result from imperfect cosmic-ray
cleaning.
Fig. 2.—Same as Fig. 1, but for the spectral range 4100–4140 8. This
region includes lines of H? (from which one may ascertain that the effective
temperatures of these stars are quite similar to one another) and the Eu ii
4129 8 line; detections are indicated with a vertical arrow.
OBSERVATIONS WITH SUBARU HDS
115

Page 4

TABLE 3
Equivalent Widths for Program Stars
Equivalent Width (m8)a
Wavelength
(8)
Species
L.E.P.
(eV) log gf
12345678910 11 12131415 161718 19202122
3829.35.......
3832.31.......
3838.30.......
4571.10.......
4703.00.......
5172.70.......
5183.62.......
3961.53.......
4102.94.......
4226.73.......
4283.01.......
4318.66.......
4425.44.......
4454.79.......
4455.89.......
4400.40.......
4415.56.......
5031.02.......
3998.64.......
4533.25.......
4534.78.......
4535.58.......
4981.74.......
4991.07.......
4999.51.......
5039.96.......
5064.66.......
5173.75.......
5192.98.......
4028.35.......
4337.93.......
4394.07.......
4395.85.......
4399.78.......
4417.72.......
4443.81.......
4450.49.......
4464.46.......
4468.50.......
4470.86.......
4501.28.......
4571.98.......
4589.95.......
4865.62.......
Mg i
Mg i
Mg i
Mg i
Mg i
Mg i
Mg i
Al i
Si i
Ca i
Ca i
Ca i
Ca i
Ca i
Ca i
Sc ii
Sc ii
Sc ii
Ti i
Ti i
Ti i
Ti i
Ti i
Ti i
Ti i
Ti i
Ti i
Ti i
Ti i
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
Ti ii
2.71
2.71
2.72
0.00
4.35
2.71
2.72
0.01
1.91
0.00
1.89
1.90
1.88
1.90
1.90
0.60
0.59
1.36
0.05
0.85
0.84
0.83
0.85
0.84
0.83
0.02
0.05
0.00
0.02
1.89
1.08
1.22
1.24
1.24
1.17
1.08
1.08
1.16
1.13
1.17
1.12
1.57
1.24
1.12
?0.480
0.145
0.414
?5.569
?0.377
?0.381
?0.158
?0.336
?3.100
0.240
?0.220
?0.210
?0.358
0.260
?0.510
?0.540
?0.670
?0.400
?0.056
0.476
0.280
0.130
0.504
0.380
0.250
?1.130
?0.991
?1.118
?1.006
?1.000
?1.130
?1.590
?2.170
?1.270
?1.430
?0.700
?1.450
?2.080
?0.600
?2.280
?0.750
?0.530
?1.790
?2.610
157.6
190.1
237.7
45.5
...
...
...
106.9
63
...
...
47.4
42.7
70.3
...
56.2
48.9
20.3
54.8
38.6
...
...
44.5
40.7
35.8
17.3
20.5
...
...
38.4
84.5
42.3
30.6
74.5
73.9
96.8
64.7
44.8
98.4
28.1
93.9
85.8
48.4
11.3
198.5
213.5
261.9
77.4
...
...
...
139.5
91.4
...
...
64.1
55
95.4
...
86.6
78.1
46
...
...
...
...
66.7
...
57.3
...
...
...
...
...
119
70
57.8
96.6
105
128.2
96.6
...
132.5
56.8
...
...
...
29.7
156.4
160.4
194.9
76.5
...
...
...
118.1
76.6
...
...
43.9
39.9
69.5
35.4
67
61.7
30.2
...
...
36.5
...
51
...
40.4
22.7
29.9
...
...
...
80.4
55
122.6
81.4
88.6
116
75.6
...
112.8
38.1
109.8
...
61.5
20.9
...
263.1
...
132.6
...
...
...
174.3
114.5
...
...
81.4
71.6
...
...
...
103
64.7
108.8
84.6
71.8
...
97.5
...
86.1
72.1
78.9
76.3
...
82.2
145.1
...
...
...
129.5
160.1
124.7
...
163.8
74.9
156.1
154.6
102.4
51.8
...
181.6
205.4
51.7
54.6
...
...
112.4
57.4
...
46.5
40.9
34.4
64.9
...
58.2
52.2
22.3
56.5
40.9
31.1
24.2
47.2
42.1
36.3
18.9
22.5
...
...
42.1
92.8
48.1
36.2
75.4
81.1
104
71.5
50.2
107.1
34.1
101.7
92.6
54.3
15.1
...
230
262
85
72
209
232
146
82
...
65.6
55.4
49.1
79.9
...
78.3
76
42
70.2
52.2
42.6
35.6
61.6
57.8
49.1
30.2
35.9
34
39.2
52.5
...
...
46.6
89
95.1
119.3
87.4
67
121.4
48.6
117.2
109.9
71.7
25.2
...
174.9
202
43.8
52.6
168.4
187.1
104.6
60.5
...
52.2
40.6
35.7
64.6
...
...
47.7
18.5
52.3
35.5
95.5
21.2
39.8
37.7
31.6
15.9
18
16.6
19.7
35.4
78
...
...
...
70.6
95.7
63.8
42.9
98.1
26.6
93.1
84.5
46.4
11.5
125.3
153.2
173.5
7.7
41
...
...
68.4
19.4
...
29.6
27.2
22.2
48.5
...
17.5
14.7
4.8
24.2
14.4
...
...
19.1
16.4
12
3.3
5
...
...
13.4
40.9
11.5
6.7
30.5
32.3
60.8
23.8
11.7
63.1
5.4
57.2
52.6
13.9
2
...
231.7
288.8
95.7
90.7
...
...
145.3
89
...
84
69.9
63.5
97.1
...
79.6
80.9
47
81.5
63.4
54.7
49
73.3
71
64.3
45.3
49.3
...
...
70.9
110.1
74.9
58.1
102.5
104.1
126.7
92.5
76.5
130.6
59.3
125.3
117
78.9
32.3
131.5
143.4
166.2
32.2
45
150.4
169.6
88
46.8
...
...
37.2
33.9
57.9
24.2
...
37.4
17.3
43.3
29.1
23.4
18.8
36.9
34.1
23.2
13.8
10.8
...
17.9
27.7
...
...
...
...
62.2
85.4
...
35.9
83.7
22.4
82.7
74
40
12
158
177
198
42.2
56.5
176.8
192.4
105
73.2
...
39.5
36.8
31.4
60.7
...
...
51.4
27.1
38.3
24.8
17.6
12.4
31
24.5
21.7
10.5
11.1
8.8
11.5
25.2
...
...
...
...
60.2
90.2
54.3
32.6
90.6
18.9
86.3
80.5
34.3
9.8
131.2
137.9
163.7
24.1
...
...
...
85.5
40
...
35.5
24.9
29.2
42.6
...
...
29.1
12.3
28
20.6
16.1
...
25
22.4
16.4
10.5
11.3
8.1
10.7
21.8
...
...
...
...
52.6
76.3
43.2
22.7
78.3
16.6
70.7
64.4
26.2
...
110.3
103.6
137.1
17.5
...
131.6
149.7
85.1
22.9
...
12.8
25.2
11.2
30.8
...
...
29.2
8.4
...
30
19.3
14.7
39.2
17.8
25.3
12.8
...
14.8
15.5
26.8
70.2
...
...
...
63.4
87.7
58.1
38.5
89.3
24.5
83
76.8
41.6
...
151.6
142.5
171
49
...
...
...
97.5
56.1
...
44.2
40.1
41.8
61.7
...
...
41.1
21.9
53
36
30.9
29.9
...
39.7
31
14.9
22.3
20.2
18.7
33.5
...
...
...
...
69.4
100.8
65.8
45.8
101
27.3
95
87.9
48.5
22
109.4
120
127.9
15.4
...
...
...
64.2
18.2
...
30
18.8
20.7
35.1
...
...
3.7
...
26.2
...
14.1
10.5
16.7
16
13.6
...
...
...
7
12
...
...
...
...
29.4
55.3
23.8
18.3
59.6
...
55.6
44.7
10.2
...
125.2
142.2
164.7
10.9
39.9
...
...
67.1
15.5
134.9
28
26.7
22.4
43.9
17.5
13.5
13.1
...
23.3
...
10.6
...
19.4
...
15.1
...
...
...
...
11.3
37.4
12.2
...
29
28.8
57.7
21.6
12.7
60.3
...
54.2
49.2
12.5
...
154
124.4
156.6
49.7
...
...
...
101.6
68.3
...
...
...
...
...
...
...
46.6
20.3
...
...
36
...
36.7
36.6
...
...
...
...
...
...
69.6
...
103.4
53.7
67.6
91.6
52.3
...
88.6
...
92.5
85
47.9
...
131.5
122.6
143.7
21.6
38.2
...
...
81.4
40.1
...
16.5
19.3
19
49.9
...
30.5
22.8
...
32.8
54.3
...
...
22.5
16.1
16.7
...
...
...
...
16.8
47.5
...
64.8
42.4
34.4
61.1
34.7
...
57.8
...
60.7
49.1
18.4
...
140.6
158.7
176.2
27.4
41.5
154.5
177.4
107
44.6
Syn
...
32
35.2
...
25
...
41.4
15.3
37.7
25.3
21.6
15.1
31.5
29.1
...
9.7
12.4
...
...
...
...
...
...
...
65.7
84.7
50.9
30.5
93.3
...
83.2
77.2
34
11.1
96.5
103.9
120.5
17.1
23.7
...
...
93.2
45.6
...
18.3
26.8
...
...
...
32.3
23.5
...
33.2
23
...
...
15.9
...
12.8
...
...
...
...
22.4
50
...
...
35.9
41.4
73.3
33.9
...
70.9
...
69.9
62.1
...
...
172.5
208.8
265.3
59.2
74.3
193
231.7
119.1
68.5
...
...
54.4
52
81
...
...
50.7
26.2
59.4
47.5
38.1
30.7
54.7
49.5
42.2
20
27.9
22.1
28.8
45.8
81
...
...
...
86.5
100.6
68.5
50.5
102.4
34.6
97.9
92.2
52.4
14.7
...
191
...
55.3
61.9
187.3
...
110.2
66.9
...
...
48.7
...
...
...
...
...
21.8
59.2
104.4
32
27.2
48.9
44.8
47.3
20.6
...
...
...
...
...
...
...
...
...
101.9
68.9
47.1
...
...
98.5
92.3
55.4
...
116

Page 5

TABLE 3—Continued
Equivalent Width (m8)a
Wavelength
(8)
Species
L.E.P.
(eV)loggf
123456789 10 1112131415161718 1920 2122
5129.16.......
5185.91.......
5188.70.......
4379.24.......
4389.99.......
3951.96.......
4005.71.......
4254.35.......
4274.81.......
4289.73.......
4554.99.......
4558.65.......
4588.20.......
4030.76.......
4033.07.......
4034.49.......
4041.37.......
4754.04.......
4823.51.......
3763.80.......
3767.20.......
3787.89.......
3805.35.......
3815.85.......
3820.44.......
3825.89.......
3827.83.......
3840.45.......
3849.98.......
3856.38.......
3859.92.......
3865.53.......
3886.29.......
3899.72.......
3902.96.......
3920.27.......
3922.92.......
3949.96.......
4005.25.......
4063.61.......
4071.75.......
4076.64.......
4114.45.......
4132.91.......
4134.69.......
4143.88.......
Ti ii
Ti ii
Ti ii
V i
V i
V ii
V ii
Cr i
Cr i
Cr i
Cr ii
Cr ii
Cr ii
Mn i
Mn i
Mn i
Mn i
Mn i
Mn i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
Fe i
1.89
1.89
1.58
0.30
0.28
1.48
1.82
0.00
0.00
0.00
4.07
4.07
4.07
0.00
0.00
0.00
2.11
2.28
2.32
0.99
1.01
1.01
3.30
1.49
0.86
0.92
1.56
0.99
1.01
0.05
0.00
1.01
0.05
0.09
1.56
0.12
0.05
2.18
1.56
1.56
1.61
3.21
2.83
2.85
2.83
1.56
?1.390
?1.350
?1.210
0.565
0.235
?0.784
?0.522
?0.114
?0.231
?0.361
?1.380
?0.660
?0.630
?0.470
?0.618
?0.811
0.285
?0.086
0.144
?0.221
?0.382
?0.838
0.313
0.237
0.157
?0.024
0.094
?0.497
?0.863
?1.280
?0.698
?0.950
?1.055
?1.515
?0.442
?1.734
?1.626
?1.251
?0.583
0.062
?0.008
?0.528
?1.303
?1.005
?0.649
?0.511
...
...
...
14.2
...
17.7
18.1
...
...
85.9
...
10.2
8.4
91
77.4
79.1
16.6
6.3
8.8
139
125.9
112
46.8
137.2
188.2
165.1
124.3
123.9
110.6
137.6
184
111.2
115.4
127.7
103.8
121.8
128.9
45.5
101.5
128.4
120.6
26.7
12.8
23.1
36.3
104
...
...
...
28.9
...
44.6
46
...
...
109.8
...
30.2
19.8
138.2
124.4
105.8
45.7
18.1
26.2
209.9
175.7
148.2
78.8
191.1
287.4
234.8
177.5
171.5
149.7
180.7
234.7
144.8
208.5
165.9
138.9
161.7
171.7
68.5
142.7
186.3
168.7
...
33.3
47.2
66
134.7
...
...
...
...
...
34.9
38.6
...
...
92.1
...
13.4
6.8
105.5
95.8
89.3
37.2
11.6
12.8
...
...
116
...
...
252.6
198.3
117
138.8
...
160.6
203.7
115.9
161.7
150.1
118.5
142.5
148.1
61
110.1
147.7
150
25.8
16.8
119.5
48
123.9
72.6
65.6
...
...
...
...
...
...
...
135.1
...
...
23.5
...
179.3
164.8
67.7
40.6
...
...
...
222.8
81.6
...
...
...
...
...
...
...
...
194.6
...
...
...
...
253.8
95
...
...
...
...
52.8
184.4
...
...
...
...
...
14
8.7
21.6
19.3
45.1
37.1
90
28
21.7
35.4
36.3
113.7
112.8
109.1
4.8
20.7
13.3
140.8
125.2
119.8
43.9
19.9
25.7
171.7
151.7
129.7
59.3
165.6
279.7
222.2
159
154.4
142.2
173.6
238.2
136.1
184.7
162.5
131.4
157.7
168.4
66.9
131.7
166.3
153.7
45.1
28.8
42.2
58.3
134.5
22.8
19
59.8
...
...
17.4
18.4
88
88.1
82
4.8
20.7
13.3
97.2
83.6
75.2
15.7
5.9
8.6
138.7
127.3
110.3
48.9
138.1
193.3
165.8
124.5
126.7
111.9
140.3
185.3
111.7
156
129.6
105.5
123.1
132
44.9
103.1
129.6
120.8
27.2
13
102.7
38
104.8
...
...
...
4.9
...
5.2
5.2
66.3
63.5
57.2
1.5
8.7
5
66.8
55.2
45.9
13.3
5.2
7.3
107.8
96.9
84.5
40.4
114.6
148.5
129.4
102
96.1
87.3
106.1
137.5
84.1
109
96.7
82.2
89.3
96.1
28.3
78.8
106.7
...
18.5
8.7
15.3
28.2
83.7
...
...
...
38.6
...
42.5
43.5
23.2
16.5
...
...
...
36.1
16.9
84.2
82.2
76.8
...
9.8
5.2
84.8
75.1
77.1
23.2
6.5
11.3
113.9
106.1
89.4
52.1
119.6
168.2
151.6
112.5
109.9
103.7
117.6
151.9
100.7
127.6
121
98.2
119.8
124.2
37.2
98.8
118.6
109.6
...
19.6
90.2
37.1
100.1
17.2
15.4
...
...
...
18.2
17.6
83.7
79.4
72.6
...
11.2
5
106.1
91.6
80.9
26.6
9.7
14.9
131.3
120.7
108.4
42.3
131.5
172.2
152.4
122.1
121.7
111.7
139.6
168.5
110.3
141.4
133.8
103.5
122.6
132.4
36.1
99.4
127.5
117.3
21.9
10.7
...
...
105.5
12.9
11.1
34
...
...
11.6
7.1
70.7
69.1
67.2
...
...
...
75.5
61.3
57.7
7.7
...
...
116.6
110.8
100.5
42.7
121.5
159.9
134.5
97.8
111.7
101.2
117.5
156
100.9
144.7
122.7
89.1
115.9
120.6
30.8
87
115.9
107.4
...
...
87.2
21.4
94.4
20.6
17.9
49
...
...
...
17.6
82.9
79.6
72.9
...
8.9
4.1
98.7
86.7
80.8
31.8
13.5
13.3
98
90.8
85.3
...
96.9
149.9
131
107.9
92.1
99.5
123.1
142.5
90.4
125.8
118
92.4
114.1
114.2
26.8
85
110.3
72.6
...
...
...
...
102.3
24.9
22.6
...
...
...
16.2
21.1
95.6
92.5
88.3
...
12.2
7.9
97.1
91.9
86.7
26.6
13.2
14.3
137.2
128.9
115.7
47.8
138.2
210.2
180
137.8
130
124.7
148.7
195.6
117.7
150.4
140.5
111.8
137.1
148.2
48.1
112
137.6
115.7
...
16.7
24.7
37.8
117.5
...
...
19.2
...
...
...
...
52.4
52.9
47.6
...
...
...
39.5
35.6
...
...
...
...
...
83.8
72
19.2
91.8
122
107
84.4
82.2
82.3
96
116.1
72.5
103.5
93.8
68.8
88.4
95.1
16.5
67.2
88.3
80.9
16
...
...
15.7
75.9
...
...
...
...
...
6.2
...
60.1
53.6
49.6
...
...
...
50.4
38.9
33
...
...
...
103
86.4
80.9
34.3
109
134.8
119
...
91.7
80.3
98
126.6
78.7
105.5
93.3
...
84.6
91.4
23.2
71.5
96.5
91.7
15.5
...
17.3
21.3
81.9
...
...
...
...
...
...
...
...
...
...
...
...
17.1
...
18.4
11.8
...
...
...
15.7
...
87.4
...
...
...
...
...
93.6
92.2
...
18.7
5.5
...
134.5
127.6
109
65.3
138.7
183.2
171.2
127.6
121.1
117.3
138.1
179
111.1
193.4
130.7
105.9
125.8
128
42.9
100.4
135.7
117.3
34.6
10.2
101.6
34.6
104.2
...
...
...
11.6
...
...
...
31.6
27.1
...
...
...
23.3
23.2
96.8
...
96.1
...
17.9
9
109.8
97.8
108.1
30.8
12.3
20.1
155
137.8
114.8
63.6
156.6
234
193.3
140
139
119.1
146.4
215.2
115.8
179.6
132.7
111.3
121.8
135.7
55.9
104.7
144.9
130.9
39.4
18.8
33.8
53.6
111.1
...
22
...
...
...
29.4
33.5
95.7
96.7
...
...
...
...
109
96.2
91.8
19.8
7.3
...
140.4
...
109
...
164
210
...
...
129.4
119.9
149
191.1
118.7
173.3
139.3
108.1
126.2
133.5
50.7
107.5
...
128.7
...
16.6
...
48.9
50.4
...
86
2.8
11.1
7.1
97.2
83.6
75.2
15.7
5.9
8.6
152.4
137.6
131.1
58.1
150.9
210.3
182.3
136
136.6
125.2
155.8
190.7
119.6
165.3
140.5
112.1
137
142.5
47.7
110.4
139.4
130.1
29.4
14.3
22.7
43.8
113.2
...
...
...
28.2
18.6
138.8
124.9
121.3
47.1
21
28.4
217.1
180.3
145.9
76.9
195.1
331.7
272.9
185.9
182.8
156.4
189.3
292.4
148.2
221.3
168.2
123.5
161.7
173.5
73.8
142.4
179.9
171.2
59.8
38.9
143.8
68.6
135.3
...
88.1
...
...
...
130.3
112.2
...
...
...
...
...
...
130.3
...
...
...
...
...
...
...
155.9
182.3
128.6
174.1
158.4
...
...
164.3
59.4
...
...
...
...
...
...
...
...
51.3
53.1
...
...
...
65.1
46.3
36.4
...
...
...
102.5
84.4
63.7
31.2
111.1
143.3
125.5
89.7
88.9
78.6
101.5
121
82.2
104.8
91
76.3
99.5
93.6
36.9
81.8
110.1
76.9
...
...
67.3
18.5
72.5
...
66.4
...
...
...
91.6
73.2
57.4
...
...
...
53.9
109.2
51.2
47.4
102.5
149.6
135.5
101.5
109.8
105.2
138.9
144.1
102
132.8
133.3
11.3
118.2
130.3
30.1
102.5
123.7
113.8
...
17.4
95.4
33.8
101.3
117