Pushing Automated Abundance Derivations Into the Cool Star Regime: A Test Using Three G and Two K Stars in Praesepe

TL;DR

This study demonstrates that automated spectral analysis methods can reliably derive stellar abundances for G and K stars in open clusters, supporting their use in chemical tagging across diverse stellar types.

Contribution

The paper introduces an automated approach for abundance analysis of cooler stars, extending the applicability of chemical tagging techniques to a broader temperature range.

Findings

Automated routines yield consistent abundances for G and K stars within 0.1 dex.

G and K stars in Praesepe show chemical homogeneity within measurement uncertainties.

Results support the feasibility of automated abundance analysis for chemical tagging across main-sequence stars.

Abstract

We present the results of an abundance analysis of three G and two K dwarfs in the Praesepe open cluster based on high-resolution, moderate signal-to-noise-ratio spectra obtained with the ARC 3.5-m Telescope at Apache Point Observatory. Using a Principle Component Analysis and the BACCHUS automated spectral analysis code, we determined stellar parameters and abundances of up to 24 elements for each of our targets, which range in temperature from 6000 to 4600 K. The average derived iron abundance for the three G stars is 0.17+/-0.07 dex, consistent with the 0.12+/-0.04 dex derived by Boesgaard et al. (2013) for their sample of 11 solar-type Praesepe members, which included these G stars. To investigate the efficacy of using automated routines to derive the abundances of cooler main-sequence stars, we compared the abundances of the K dwarfs to those of the G dwarfs. Our abundances are consistent to <=0.1~dex for 13 of the 18 elements we report for all five of the stars, providing more evidence that G and K stars in a given open cluster are chemically homogeneous. The median difference between the mean G and K stars abundances is 0.08+/-0.05 dex, despite serious challenges with the noisier data for the fainter K dwarfs. Our results are encouraging for chemical tagging, as they indicate that it may be possible to use automated abundance determination techniques to identify chemically related main-sequence stars across larger temperature ranges than are usually considered in these experiments.

Figures

Tables

Table 1. Table 1: APO observations

Star	RA, Dec	$V$	Date	Exposure time
	(J2000)	(mag)		(s)
JS 482	08 42 20.09 $+$19 09 05.67	13.52	11/28/2017	7200
JS 552	08 43 56.72 $+$19 43 32.29	13.26	12/29/2017	8400
KW23	08 37 11.49 $+$19 48 13.25	11.29	03/30/2018	1800
KW30	08 37 22.23 $+$20 10 37.24	11.40	03/30/2018	1800
KW208	08 39 45.75 $+$19 22 01.15	10.66	03/30/2018	1800

Table 2. Table 2: Parameter ranges of the learning database used for the PCA analysis

	Range	Step
$T_{\mathrm{eff}}$	4000$-$6000 K	100 K
$\log g$	4.00$-$5.00 dex	0.10 dex
[M/H]	-0.50$-$0.5 dex	0.10 dex
${\xi }_t$	1.0 $\text{km}{\text{s}}^{-1}$	–
$v\sin i$	0$-$15 $\text{km}{\text{s}}^{-1}$	1 $\text{km}{\text{s}}^{-1}$
Resolution	31,500	–
$\lambda$	5000$-$6000 Å	0.15 Å

Table 3. Table 3: Stellar parameters derived from the different techniques

	PCA				BACCHUS (adopted)				Gaia
	$T_{\mathrm{eff}}$	$\log g$	[M/H]	$v\sin i$	$T_{\mathrm{eff}}$	$\log g$	[Fe/H]	${\xi }_t$	$T_{\mathrm{eff}}$
	(K)	(dex)	(dex)	($\text{km}{\text{s}}^{-1}$)	(K)	(dex)	(dex)	($\text{km}{\text{s}}^{-1}$)	(K)
JS 482	4650$\pm$100	4.30$\pm$0.15	0.11$\pm$0.10	7.0$\pm$2.0	4658$\pm$110	4.55$\pm$0.50	0.13$\pm$0.15	0.69$\pm$0.07	4685
JS 552	4750$\pm$100	4.40$\pm$0.15	0.10$\pm$0.10	8.0$\pm$2.0	4749$\pm$87	4.34$\pm$0.22	0.12$\pm$0.15	1.13$\pm$0.06	4921
KW23	5650$\pm$100	4.40$\pm$0.15	0.12$\pm$0.10	5.5$\pm$2.0	5773$\pm$53	4.56$\pm$0.24	0.20$\pm$0.11	1.20$\pm$0.04	5601
KW30	5700$\pm$100	4.45$\pm$0.15	0.10$\pm$0.10	6.0$\pm$2.0	5716$\pm$45	4.57$\pm$0.42	0.12$\pm$0.12	1.18$\pm$0.04	5597
KW208	5950$\pm$100	4.35$\pm$0.15	0.12$\pm$0.10	9.0$\pm$2.0	6005$\pm$19	4.46$\pm$0.21	0.18$\pm$0.12	1.05$\pm$0.04	6230

Table 4. Table 4: Elemental abundances for our five targets. Columns 7, 8, and 9 give the mean abundances for each element for the three G stars, the two K stars, and their differences, respectively.

	KW23	KW30	KW208	JS 552	JS 482	Mean G	Mean K	$\Delta$(GK)
[Fe/H]	0.20$\pm$0.04	0.12$\pm$0.04	0.18$\pm$0.03	0.12$\pm$0.03	0.13$\pm$0.03	0.17$\pm$0.04	0.12$\pm$0.01	0.04$\pm$0.03
A(Li)	2.06$\pm$0.02	2.12$\pm$0.02	2.75$\pm$0.02	$\cdots$	$\cdots$	2.31$\pm$0.40	$\cdots$	$\cdots$
[C/Fe]	-0.13$\pm$0.04	-0.09$\pm$0.22	-0.15$\pm$0.13	-0.15$\pm$0.03	-0.20$\pm$0.09	-0.12$\pm$0.03	-0.17$\pm$0.04	0.05$\pm$0.03
[O/Fe]	-0.08$\pm$0.10	-0.12$\pm$0.16	-0.02$\pm$0.09	$\cdots$	$\cdots$	-0.08$\pm$0.05	$\cdots$	$\cdots$
[Na/Fe]	0.04$\pm$0.08	-0.02$\pm$0.05	-0.35$\pm$0.16	-0.02$\pm$0.25	-0.07$\pm$0.38	-0.11$\pm$0.21	-0.05$\pm$0.04	-0.07$\pm$0.05
[Mg/Fe]	-0.07$\pm$0.10	-0.04$\pm$0.05	-0.08$\pm$0.06	-0.17$\pm$0.04	-0.20$\pm$0.09	-0.06$\pm$0.02	-0.19$\pm$0.02	0.13$\pm$0.09
[Al/Fe]	-0.02$\pm$0.10	-0.08$\pm$0.10	-0.15$\pm$0.02	0.05$\pm$0.11	-0.05$\pm$0.12	-0.08$\pm$0.07	0.00$\pm$0.07	-0.09$\pm$0.06
[Si/Fe]	-0.03$\pm$0.03	-0.03$\pm$0.04	-0.06$\pm$0.05	-0.13$\pm$0.11	0.23$\pm$0.38	-0.04$\pm$0.02	0.05$\pm$0.26	-0.09$\pm$0.07
[Ca/Fe]	-0.01$\pm$0.08	0.00$\pm$0.19	0.01$\pm$0.09	0.15$\pm$0.10	0.12$\pm$0.26	0.00$\pm$0.01	0.13$\pm$0.02	-0.13$\pm$0.09
[Sc/Fe]	-0.01$\pm$0.10	0.02$\pm$0.18	-0.03$\pm$0.13	-0.17$\pm$0.13	0.10$\pm$0.31	-0.01$\pm$0.02	-0.04$\pm$0.20	0.03 $\pm$0.02
[Ti/Fe]	-0.01$\pm$0.05	-0.03$\pm$0.06	-0.04$\pm$0.07	0.06$\pm$0.09	0.06$\pm$0.16	-0.03$\pm$0.01	0.06$\pm$0.01	-0.09$\pm$0.06
[V/Fe]	0.09$\pm$0.06	0.07$\pm$0.08	-0.04$\pm$0.03	0.27$\pm$0.12	0.27$\pm$0.13	0.04$\pm$0.08	0.27$\pm$0.01	-0.23$\pm$0.16
[Cr/Fe]	0.02$\pm$0.06	-0.05$\pm$0.11	-0.04$\pm$0.04	-0.08$\pm$0.09	-0.05$\pm$0.18	-0.02$\pm$0.04	-0.07$\pm$0.02	0.05 $\pm$0.03
[Mn/Fe]	0.04$\pm$0.05	0.06$\pm$0.05	0.01$\pm$0.03	0.06$\pm$0.10	0.06$\pm$0.24	0.04$\pm$0.02	0.06$\pm$0.01	-0.02$\pm$0.02
[Co/Fe]	0.00$\pm$0.05	0.02$\pm$0.06	-0.13$\pm$0.05	-0.10$\pm$0.07	0.06$\pm$0.24	-0.04$\pm$0.09	-0.02$\pm$0.11	-0.02$\pm$0.01
[Ni/Fe]	-0.03$\pm$0.04	-0.08$\pm$0.04	-0.10$\pm$0.02	-0.09$\pm$0.06	-0.03$\pm$0.09	-0.07$\pm$0.04	-0.06$\pm$0.04	-0.01$\pm$0.01
[Cu/Fe]	0.02$\pm$0.06	0.07$\pm$0.09	0.02$\pm$0.03	0.19$\pm$0.11	-0.08$\pm$0.52	0.04$\pm$0.03	0.06$\pm$0.19	-0.02$\pm$0.01
[Zn/Fe]	-0.23$\pm$0.12	-0.01$\pm$0.12	-0.02$\pm$0.10	$\cdots$	$\cdots$	-0.09$\pm$0.13	$\cdots$	$\cdots$
[Sr/Fe]	0.00$\pm$0.12	-0.13$\pm$0.12	$\cdots$	$\cdots$	$\cdots$	-0.06$\pm$0.09	$\cdots$	$\cdots$
[Y/Fe]	-0.09$\pm$0.12	0.12$\pm$0.20	0.01$\pm$0.11	$\cdots$	0.08$\pm$0.45	0.02$\pm$0.11	0.08$\pm$0.45	-0.07$\pm$0.05
[Zr/Fe]	-0.19$\pm$0.13	-0.22$\pm$0.25	-0.18$\pm$0.20	-0.04$\pm$0.14	0.09$\pm$0.17	-0.20$\pm$0.02	0.02$\pm$0.09	-0.22$\pm$0.16
[Ba/Fe]	0.05$\pm$0.14	0.00$\pm$0.10	0.17$\pm$0.12	-0.10$\pm$0.11	-0.17$\pm$0.24	0.07$\pm$0.09	-0.14$\pm$0.13	0.21$\pm$0.15
[La/Fe]	-0.10$\pm$0.07	0.05$\pm$0.28	-0.25$\pm$0.14	0.16$\pm$0.66	-0.02$\pm$0.20	-0.10$\pm$0.15	0.07$\pm$0.13	-0.17$\pm$0.12
[Nd/Fe]	0.00$\pm$0.15	0.02$\pm$0.21	-0.20$\pm$0.31	$\cdots$	0.17$\pm$0.36	-0.06$\pm$0.12	0.17$\pm$0.36	-0.23$\pm$0.16

Table 5. Table 5: Previous determinations of Praesepe’s metallicity

Authors	Sample	[Fe/H]
		(dex)
Boesgaard (1989)	three F stars	0.09$\pm$0.07
Friel & Boesgaard (1992)	six F stars	0.04$\pm$0.06
An et al. (2007)	four G stars	0.11$\pm$0.03
Pace et al. (2008)	six G stars	0.27$\pm$0.10
Fossati et al. (2008)	six F stars	0.11$\pm$0.03
Carrera & Pancino (2011)	three giants	0.16$\pm$0.05
Boesgaard et al. (2013)	11 G stars	0.12$\pm$0.04
Yang, Chen, & Zhao (2015)	four giants	0.16$\pm$0.06

Table 6. Table 6: Comparison of the mean elemental abundances derived from our five targets and those obtained for a sample of 11 Praesepe solar-type stars studied by Boesgaard et al. ( 2013 ) , which included our three G stars.

	Mean	Boesgaard et al. (2013)
[Fe/H]	0.15$\pm$0.08	0.12$\pm$0.04
A(Li)	2.31$\pm$0.40	$\cdots$
[C/Fe]	-0.14$\pm$0.27	-0.09$\pm$0.05
[O/Fe]	-0.08$\pm$0.05	-0.15$\pm$0.09
[Na/Fe]	-0.08$\pm$0.43	-0.01$\pm$0.03
[Mg/Fe]	-0.11$\pm$0.16	0.00$\pm$0.04
[Al/Fe]	-0.05$\pm$0.21	0.00$\pm$0.04
[Si/Fe]	0.00$\pm$0.40	0.00$\pm$0.03
[Ca/Fe]	0.05$\pm$0.35	-0.01$\pm$0.05
[Sc/Fe]	-0.02$\pm$0.41	0.04$\pm$0.02
[Ti/Fe]	0.01$\pm$0.21	-0.03$\pm$0.06
[V/Fe]	0.13$\pm$0.20	0.04$\pm$0.04
[Cr/Fe]	-0.04$\pm$0.24	0.00$\pm$0.03
[Mn/Fe]	0.05$\pm$0.27	$\cdots$
[Co/Fe]	-0.03$\pm$0.26	$\cdots$
[Ni/Fe]	-0.07$\pm$0.12	-0.03$\pm$0.03
[Cu/Fe]	0.04$\pm$0.53	$\cdots$
[Zn/Fe]	-0.09$\pm$0.13	$\cdots$
[Sr/Fe]	-0.06$\pm$0.09	$\cdots$
[Y/Fe]	0.03$\pm$0.51	0.01$\pm$0.08
[Zr/Fe]	-0.11$\pm$0.40	$\cdots$
[Ba/Fe]	-0.01$\pm$0.33	0.11$\pm$0.03
[La/Fe]	-0.03$\pm$0.75	$\cdots$
[Nd/Fe]	0.00$\pm$0.54	$\cdots$

Table 7. Table 7: Abundance determination sensitivity to the stellar parameters. The maximum value of the sensitivity, in dex, is included in this table.

$\Delta$[X/H]	$T_{\mathrm{eff}}$$\pm$100 K	$\log g$$\pm$0.30 dex	${\xi }_t$$\pm$0.05 $\text{km}{\text{s}}^{-1}$
KW23
Li	…	…	…
C	0.06	0.02	0.02
O	0.10	0.09	0.01
Na	0.10	0.07	0.01
Mg	0.08	0.11	0.01
Al	0.05	0.01	0.01
Si	0.01	0.03	0.01
Ca	0.08	0.08	0.02
Sc	0.02	0.12	0.03
Ti	0.08	0.03	0.01
V	0.11	0.01	0.00
Cr	0.09	0.03	0.03
Mn	0.09	0.02	0.01
Co	0.07	0.04	0.01
Ni	0.06	0.02	0.00
Cu	0.10	0.04	0.01
Fe	0.07	0.01	0.01
Zn	0.06	0.06	0.02
Sr	0.10	0.02	0.03
Y	0.05	0.13	0.04
Zr	0.09	0.14	0.05
Ba	0.05	0.10	0.05
La	0.04	0.08	0.01
Nd	0.15	0.15	0.05
KW30
Li	…	…	…
C	0.15	0.13	0.13
O	0.12	0.11	0.01
Na	0.09	0.08	0.04
Mg	0.04	0.03	0.01
Al	0.04	0.01	0.00
Si	0.03	0.02	0.02
Ca	0.10	0.13	0.03
Sc	0.03	0.11	0.02
Ti	0.08	0.03	0.01
V	0.13	0.03	0.03
Cr	0.11	0.06	0.04
Mn	0.11	0.01	0.01
Co	0.08	0.03	0.02
Ni	0.09	0.00	0.02
Cu	0.09	0.04	0.01
Fe	0.07	0.02	0.01
Zn	0.01	0.04	0.02
Sr	0.10	0.03	0.03
Y	0.05	0.12	0.04
Zr	0.20	0.13	0.09
Ba	0.03	0.01	0.03
La	0.12	0.19	0.10
Nd	0.10	0.13	0.11
KW208
Li	…	…	…
C	0.13	0.13	0.12
O	0.14	0.10	0.07
Na	0.07	0.04	0.01
Mg	0.08	0.05	0.01
Al	0.06	0.01	0.01
Si	0.03	0.06	0.00
Ca	0.08	0.10	0.01
Sc	0.03	0.12	0.01
Ti	0.09	0.06	0.02
V	0.11	0.01	0.01
Cr	0.07	0.03	0.02
Mn	0.08	0.02	0.00
Co	0.10	0.05	0.04
Ni	0.09	0.02	0.02
Cu	0.09	0.01	0.00
Fe	0.07	0.04	0.01
Zn	0.06	0.02	0.03
Sr	$\dots$	$\dots$	$\dots$
Y	0.05	0.14	0.05
Zr	0.05	0.09	0.02
Ba	0.08	0.03	0.08
La	0.09	0.16	0.05
Nd	0.30	0.31	0.27
JS 482
Li	…	…	…
C	0.03	0.01	0.01
O	$\dots$	$\dots$	$\dots$
Na	0.15	0.19	0.00
Mg	0.04	0.04	0.00
Al	0.05	0.02	0.00
Si	0.08	0.17	0.00
Ca	0.12	0.11	0.01
Sc	0.06	0.14	0.00
Ti	0.11	0.05	0.02
V	0.12	0.01	0.01
Cr	0.09	0.07	0.01
Mn	0.13	0.07	0.00
Co	0.01	0.11	0.00
Ni	0.02	0.04	0.01
Cu	0.07	0.23	0.00
Fe	0.02	0.01	0.01
Zn	$\dots$	$\dots$	$\dots$
Sr	$\dots$	$\dots$	$\dots$
Y	0.39	0.06	0.01
Zr	0.13	0.02	0.02
Ba	0.08	0.09	0.01
La	0.03	0.06	0.01
Nd	0.01	0.16	0.00
JS 552
Li	…	…	…
C	0.00	0.02	0.02
O	$\dots$	$\dots$	$\dots$
Na	0.21	0.20	0.00
Mg	0.01	0.04	0.00
Al	0.06	0.02	0.00
Si	0.09	0.10	0.00
Ca	0.09	0.08	0.00
Sc	0.02	0.17	0.01
Ti	0.10	0.04	0.02
V	0.13	0.01	0.02
Cr	0.09	0.06	0.01
Mn	0.09	0.07	0.01
Co	0.03	0.08	0.01
Ni	0.02	0.07	0.02
Cu	0.08	0.10	0.01
Fe	0.01	0.02	0.01
Zn	$\dots$	$\dots$	$\dots$
Sr	$\dots$	$\dots$	$\dots$
Y	$\dots$	$\dots$	$\dots$
Zr	0.16	0.01	0.01
Ba	0.04	0.01	0.02
La	0.01	0.02	0.55
Nd	$\dots$	$\dots$	$\dots$

Table 8. Table 8: Line-by-line abundances for each element and each of our targets. Column 1 is the star, column 2 is the element, and columns 3, 4, and 5 are the atomic data: line wavelength in Å, oscillator strength log ⁡ ( g ​ f ) 𝑔 𝑓 \log(gf) , and excitation potential in eV. The derived absolute elemental abundance is tabulated in column 6.

Star	Element	$\lambda$ (Å)	$\log \left(gf\right)$	EP ($\mathrm{eV}$)	$\log ϵ$
KW23	Cr I	5272.00	-0.42	3.449	5.430
KW23	Cr I	5287.17	-0.87	3.438	5.780
KW23	Cr I	5296.69	-1.36	0.983	5.830
KW23	Cr I	5300.74	-2.0	0.983	5.630
KW23	Cr I	5304.18	-0.67	3.464	5.760
KW23	Cr I	5312.85	-0.55	3.449	5.860
KW23	Cr I	5318.77	-0.67	3.438	5.780
KW23	Cr I	5345.79	-0.95	1.004	5.780
KW23	Cr I	5348.31	-1.21	1.004	5.840
KW23	Cr I	5628.64	-0.74	3.422	5.810
KW23	Cr I	5719.81	-1.58	3.013	5.430
KW23	Cr II	5788.41	-9.975	8.718	5.780
JS 552	Cr I	4936.33	-0.25	3.113	5.880
JS 552	Cr I	4964.92	-2.526	0.941	5.420
JS 552	Cr II	5239.01	-6.462	6.641	5.540
JS 552	Cr I	5241.45	-1.92	2.71	6.090
JS 552	Cr I	5272.00	-0.42	3.449	5.450
JS 552	Cr I	5300.74	-2.0	0.983	5.292
JS 552	Cr I	5304.18	-0.67	3.464	5.978
JS 552	Cr I	5312.85	-0.55	3.449	5.568
JS 552	Cr I	5318.77	-0.67	3.438	5.676
JS 552	Cr I	5628.64	-0.74	3.422	5.564
JS 552	Cr I	5719.81	-1.58	3.013	5.717
JS 552	Cr II	5788.41	-9.975	8.718	5.696
JS 552	Cr I	5844.59	-1.77	3.013	5.874
JS 482	Cr II	4588.19	-0.627	4.071	5.531
JS 482	Cr I	4936.33	-0.25	3.113	6.100
JS 482	Cr I	4964.92	-2.526	0.941	5.330
JS 482	Cr I	5241.45	-1.92	2.71	5.837
JS 482	Cr II	5246.76	-2.466	3.714	5.407
JS 482	Cr I	5287.17	-0.87	3.438	5.385
JS 482	Cr I	5300.74	-2.0	0.983	5.391
JS 482	Cr I	5304.18	-0.67	3.464	5.929
JS 482	Cr I	5312.85	-0.55	3.449	5.433
JS 482	Cr I	5318.77	-0.67	3.438	5.695
JS 482	Cr I	5628.64	-0.74	3.422	5.610
JS 482	Cr I	5719.81	-1.58	3.013	5.865
JS 482	Cr II	5788.41	-9.975	8.718	5.628
JS 482	Cr I	5844.59	-1.77	3.013	5.867
KW208	Co I	5176.09	-2.658	2.08	4.605
KW208	Co I	5212.70	-1.134	3.514	4.757
KW208	Co I	5331.41	-2.461	1.785	4.888
KW208	Co I	5351.99	-1.459	3.576	4.913
KW208	Co I	5590.73	-2.424	2.042	4.871
KW208	Co I	5647.20	-2.127	2.28	4.904
KW208	Co I	6093.09	-3.458	1.74	4.821
KW208	Co I	6189.00	-3.375	1.71	4.887
KW208	Co I	6429.91	-2.596	2.137	4.786
KW208	Co I	6455.01	-0.924	3.632	4.827
KW208	Co I	6632.40	-2.568	2.28	5.066
KW208	Co I	6770.99	-2.997	1.883	4.968
KW208	Co I	6814.91	-1.957	1.956	4.754
KW30	Co I	5176.09	-2.658	2.08	4.744
KW30	Co I	5212.70	-1.134	3.514	4.905
KW30	Co I	5331.41	-2.461	1.785	5.004
KW30	Co I	5351.99	-1.459	3.576	4.880
KW30	Co I	5483.91	-1.258	3.632	5.082
KW30	Co I	5530.80	-3.214	1.71	5.225
KW30	Co I	5647.20	-2.127	2.28	4.889
KW30	Co I	6093.09	-3.458	1.74	4.998
KW30	Co I	6189.0	-3.375	1.71	5.103
KW30	Co I	6429.91	-2.596	2.137	5.141
KW30	Co I	6455.01	-0.924	3.632	4.648
KW30	Co I	6632.40	-2.568	2.28	5.069
KW30	Co I	6770.99	-2.997	1.883	5.032
KW30	Co I	6814.91	-1.957	1.956	4.683
KW23	Co I	5176.09	-2.658	2.08	4.819
KW23	Co I	5212.70	-1.134	3.514	4.911
KW23	Co I	5331.41	-2.461	1.785	5.033
KW23	Co I	5351.99	-1.459	3.576	4.995
KW23	Co I	5483.31	-2.04	1.71	4.835
KW23	Co I	5483.91	-1.258	3.632	4.979
KW23	Co I	5530.80	-3.214	1.71	5.245
KW23	Co I	5590.73	-2.424	2.042	4.877
KW23	Co I	5647.20	-2.127	2.28	4.989
KW23	Co I	6093.09	-3.458	1.74	5.166
KW23	Co I	6116.99	-2.695	1.785	5.177
KW23	Co I	6189.00	-3.375	1.71	5.018
KW23	Co I	6429.91	-2.596	2.137	4.995
KW23	Co I	6455.01	-0.924	3.632	4.907
KW23	Co I	6632.40	-2.568	2.28	5.172
KW23	Co I	6770.99	-2.997	1.883	5.151
KW23	Co I	6814.91	-1.957	1.956	4.825
JS 552	Co I	5331.41	-2.461	1.785	4.883
JS 552	Co I	5351.99	-1.459	3.576	4.560
JS 552	Co I	5369.61	-2.293	1.74	4.988
JS 552	Co I	5483.31	-2.04	1.71	4.554
JS 552	Co I	5530.80	-3.214	1.71	5.146
JS 552	Co I	5590.73	-2.424	2.042	4.625
JS 552	Co I	5647.20	-2.127	2.28	4.983
JS 552	Co I	5915.60	-3.41	2.137	4.448
JS 552	Co I	6116.99	-2.695	1.785	5.230
JS 552	Co I	6189.00	-3.375	1.71	4.888
JS 552	Co I	6429.91	-2.596	2.137	4.675
JS 552	Co I	6455.01	-0.924	3.632	4.931
JS 552	Co I	6632.40	-2.568	2.28	5.162
JS 552	Co I	6770.99	-2.997	1.883	4.866
JS 552	Co I	6814.91	-1.957	1.956	4.970
JS 482	Co I	5331.41	-2.461	1.785	4.687
JS 482	Co I	5483.31	-2.04	1.71	4.705
JS 482	Co I	5530.80	-3.214	1.71	5.211
JS 482	Co I	5590.73	-2.424	2.042	4.915
JS 482	Co I	5647.20	-2.127	2.28	4.940
JS 482	Co I	5915.60	-3.41	2.137	4.879
JS 482	Co I	6005.00	-3.888	1.71	5.044
JS 482	Co I	6116.99	-2.695	1.785	5.223
JS 482	Co I	6189.00	-3.375	1.71	4.950
JS 482	Co I	6455.01	-0.924	3.632	4.900
JS 482	Co I	6632.40	-2.568	2.28	5.362
JS 482	Co I	6770.99	-2.997	1.883	4.940
JS 482	Co I	6814.91	-1.957	1.956	4.854
KW208	Cu I	5105.50	-2.398	1.389	4.100
KW208	Cu I	5153.22	-0.023	3.786	4.466
KW208	Cu I	5220.07	-0.975	3.817	4.147
KW208	Cu I	5700.20	-2.978	1.642	3.794
KW208	Cu I	5782.10	-2.595	1.642	4.227
KW208	Cu I	7933.12	-0.42	3.786	4.360
KW208	Cu I	8092.63	-0.131	3.817	4.410
KW30	Cu I	5105.50	-2.398	1.389	3.846
KW30	Cu I	5153.22	-0.023	3.786	4.755
KW30	Cu I	5700.20	-2.978	1.642	3.816
KW30	Cu I	5782.10	-2.595	1.642	4.223
KW30	Cu I	7933.12	-0.42	3.786	4.507
KW30	Cu I	8092.63	-0.131	3.817	4.374
KW23	Cu I	5105.50	-2.398	1.389	4.112
KW23	Cu I	5153.22	-0.023	3.786	4.355
KW23	Cu I	5700.20	-2.978	1.642	3.965
KW23	Cu I	5782.10	-2.595	1.642	4.268
KW23	Cu I	7933.12	-0.42	3.786	4.371
KW23	Cu I	8092.63	-0.131	3.817	4.400
JS 552	Cu I	5700.20	-2.978	1.642	4.106
JS 552	Cu I	5782.10	-2.595	1.642	4.287
JS 552	Cu I	8092.63	-0.131	3.817	3.941
JS 482	Cu I	5218.20	-0.095	3.817	3.933
JS 482	Cu I	5700.20	-2.978	1.642	4.211
JS 482	Cu I	5782.10	-2.595	1.642	4.028
JS 482	Cu I	7933.12	-0.42	3.786	4.180
JS 482	Cu I	8092.63	-0.131	3.817	4.229
KW208	Nd II	4947.00	-1.13	0.559	1.244
KW208	Nd II	4959.10	-1.662	0.064	1.235
KW208	Nd II	4989.90	-1.26	0.631	1.298
KW208	Nd II	5249.59	0.2	0.976	1.962
KW208	Nd II	5293.17	0.1	0.823	1.493
KW208	Nd II	5357.00	-0.28	1.264	1.551
KW208	Nd II	5361.50	-0.37	0.68	1.757
KW30	Nd II	4706.54	-0.71	0.0	1.454
KW30	Nd II	4959.10	-1.662	0.064	1.662
KW30	Nd II	4989.90	-1.26	0.631	1.575
KW30	Nd II	5249.59	0.2	0.976	2.014
KW30	Nd II	5293.17	0.1	0.823	1.725
KW30	Nd II	5361.50	-0.37	0.68	1.731
KW30	Nd II	5548.39	-1.974	0.55	1.937
KW23	Nd II	4706.54	-0.71	0.0	1.766
KW23	Nd II	4959.10	-1.662	0.064	1.726
KW23	Nd II	4989.90	-1.26	0.631	1.785
KW23	Nd II	5249.59	0.2	0.976	1.899
KW23	Nd II	5361.50	-0.37	0.68	2.063
KW23	Nd II	5416.41	-1.634	0.859	1.205
JS 482	Nd II	5249.59	0.2	0.976	1.992
JS 482	Nd II	5293.17	0.1	0.823	1.951
JS 482	Nd II	5311.48	-0.42	0.986	1.996
JS 482	Nd II	5361.50	-0.37	0.68	1.930
KW208	Y II	4854.86	-0.27	0.992	1.791
KW208	Y II	4883.68	0.19	1.084	2.643
KW208	Y II	4900.11	0.03	1.033	2.053
KW208	Y II	5087.41	-0.16	1.084	2.234
KW208	Y II	5200.40	-0.47	0.992	2.175
KW208	Y II	5289.81	-1.68	1.033	2.055
KW208	Y II	5544.61	-0.83	1.738	2.298
KW208	Y II	6613.73	-0.83	1.748	2.290
KW30	Y II	4883.68	0.19	1.084	2.668
KW30	Y II	5087.41	-0.16	1.084	2.134
KW30	Y II	5200.40	-0.47	0.992	2.007
KW30	Y II	5289.81	-1.68	1.033	2.387
KW30	Y II	5544.61	-0.83	1.738	2.326
KW30	Y I	6435.00	-0.521	0.066	2.269
KW23	Y II	4883.68	0.19	1.084	2.651
KW23	Y II	5087.41	-0.16	1.084	2.251
KW23	Y II	5200.40	-0.47	0.992	2.101
KW23	Y II	5289.81	-1.68	1.033	1.973
KW23	Y II	5544.61	-0.83	1.738	2.183
KW23	Y II	5728.88	-1.15	1.839	2.287
JS 552	Y II	4900.11	0.03	1.033	1.721
JS 552	Y I	6222.57	-1.452	0.0	2.085
JS 552	Y I	6435.00	-0.521	0.066	2.074
JS 552	Y I	6557.37	-2.093	0.0	2.345
JS 482	Y II	5200.40	-0.47	0.992	2.075
JS 482	Y II	5544.61	-0.83	1.738	2.402
JS 482	Y I	6023.40	-1.768	0.0	2.457
JS 482	Y I	6222.57	-1.452	0.0	2.290
JS 482	Y I	6435.00	-0.521	0.066	2.098
JS 482	Y I	6793.57	-1.543	3.594	2.741
KW208	C I	5059.83	-2.494	8.64	8.116
KW208	C I	5380.32	-1.615	7.685	8.438
KW208	C I	7100.11	-1.47	8.643	8.507
KW208	C I	7111.46	-1.085	8.64	8.462
KW208	C I	7113.17	-0.773	8.647	8.470
KW208	C I	7115.17	-0.934	8.643	8.398
KW208	C I	7116.98	-0.907	8.647	8.647
KW208	C I	7119.65	-1.148	8.643	8.568
KW30	C I	5059.83	-2.494	8.64	8.340
KW30	C I	5380.32	-1.615	7.685	8.314
KW30	C I	7111.46	-1.085	8.64	8.498
KW30	C I	7113.17	-0.773	8.647	8.465
KW30	C I	7115.17	-0.934	8.643	8.482
KW30	C I	7116.98	-0.907	8.647	8.680
KW23	C I	5141.27	-3.063	8.643	8.661
KW23	C I	5380.32	-1.615	7.685	8.370
KW23	C I	7100.11	-1.47	8.643	8.608
KW23	C I	7111.46	-1.085	8.64	8.386
KW23	C I	7113.17	-0.773	8.647	8.435
KW23	C I	7115.17	-0.934	8.643	8.388
KW23	C I	7116.98	-0.907	8.647	8.689
JS 552	C I	5141.27	-3.063	8.643	8.645
JS 552	C I	5380.32	-1.615	7.685	8.540
JS 552	C I	7115.17	-0.934	8.643	8.256
JS 552	C I	7116.98	-0.907	8.647	8.208
JS 482	C I	7100.11	-1.47	8.643	8.616
JS 482	C I	7115.17	-0.934	8.643	8.480
KW208	Fe I	4992.78	-2.35	4.26	7.627
KW208	Fe II	4993.35	-3.684	2.807	7.547
KW208	Fe I	5058.49	-2.83	3.642	7.441
KW208	Fe I	5197.57	-2.078	4.956	7.608
KW208	Fe II	5234.62	-2.18	3.221	7.806
KW208	Fe I	5243.77	-1.05	4.256	7.570
KW208	Fe II	5247.13	-2.014	10.909	7.586
KW208	Fe II	5256.93	-4.182	2.891	7.747
KW208	Fe II	5264.80	-3.13	3.23	7.572
KW208	Fe I	5294.54	-2.76	3.64	7.506
KW208	Fe I	5295.31	-1.59	4.415	7.606
KW208	Fe II	5316.60	-1.87	3.153	7.716
KW208	Fe II	5337.72	-3.72	3.23	7.892
KW208	Fe I	5373.70	-0.71	4.473	7.451
KW208	Fe II	5379.61	-4.977	10.596	7.613
KW208	Fe I	5389.48	-8.475	5.33	7.579
KW208	Fe I	5398.27	-0.63	4.446	7.452
KW208	Fe I	5412.78	-1.716	4.435	7.977
KW208	Fe II	5414.07	-3.58	3.221	7.758
KW208	Fe I	5417.03	-1.58	4.415	7.588
KW208	Fe I	5436.29	-1.44	4.387	7.631
KW208	Fe II	5441.32	-6.066	11.741	7.607
KW208	Fe I	5466.39	-0.63	4.371	7.788
KW208	Fe I	5473.90	-0.72	4.154	7.596
KW208	Fe I	5487.14	-1.43	4.415	7.666
KW208	Fe I	5491.83	-2.188	4.186	7.462
KW208	Fe I	5494.46	-1.99	4.076	7.807
KW208	Fe I	5501.46	-3.046	0.958	7.833
KW208	Fe I	5522.44	-1.45	4.209	7.583
KW208	Fe I	5534.78	-3.782	4.186	7.624
KW208	Fe I	5539.28	-2.56	3.642	7.576
KW208	Fe I	5543.93	-1.04	4.218	7.607
KW208	Fe II	5550.03	-6.71	8.266	7.287
KW208	Fe I	5560.21	-1.09	4.435	7.524
KW208	Fe I	5577.02	-1.543	5.033	7.322
KW208	Fe I	5618.63	-1.255	4.209	7.604
KW208	Fe I	5633.94	-0.23	4.991	7.733
KW208	Fe II	5638.32	-6.266	12.968	7.510
KW208	Fe I	5651.52	-4.761	4.446	7.678
KW208	Fe I	5652.31	-1.85	4.26	7.704
KW208	Fe II	5661.31	-3.511	10.758	7.490
KW208	Fe I	5678.99	-9.163	5.388	7.767
KW208	Fe I	5705.46	-1.355	4.301	7.518
KW208	Fe I	5731.76	-1.2	4.256	7.681
KW208	Fe I	5732.29	-1.46	4.991	7.634
KW208	Fe I	5741.84	-1.672	4.256	7.688
KW208	Fe I	5775.08	-1.126	4.22	7.711
KW208	Fe II	5778.47	-3.814	10.858	7.512
KW208	Fe I	5849.68	-2.89	3.695	7.495
KW208	Fe I	5855.07	-1.478	4.608	7.631
KW208	Fe I	5858.77	-2.16	4.22	7.527
KW208	Fe I	5861.10	-2.304	4.283	7.584
KW208	Fe I	5905.67	-0.69	4.652	7.544
KW208	Fe I	5930.18	-0.23	4.652	7.439
KW208	Fe II	5991.37	-3.647	3.153	7.675
KW208	Fe I	6027.09	-3.223	4.991	7.469
KW208	Fe I	6056.00	-0.32	4.733	7.552
KW208	Fe II	6084.10	-3.881	3.199	7.676
KW208	Fe I	6093.64	-1.4	4.608	7.604
KW208	Fe I	6113.30	-3.182	4.584	7.584
KW208	Fe II	6149.27	-3.283	13.155	7.937
KW208	Fe I	6151.61	-3.295	2.176	7.545
KW208	Fe I	6165.36	-1.473	4.143	7.651
KW208	Fe I	6173.33	-2.88	2.223	7.577
KW208	Fe I	6187.98	-1.62	3.943	7.564
KW208	Fe I	6200.31	-2.433	2.609	7.715
KW208	Fe I	6219.31	-5.082	5.458	7.682
KW208	Fe I	6226.73	-2.12	3.884	7.695
KW208	Fe II	6239.94	-3.573	3.889	7.708
KW208	Fe I	6246.31	-0.771	3.603	7.636
KW208	Fe II	6247.57	-4.827	5.956	7.743
KW208	Fe II	6252.62	-3.044	11.093	7.500
KW208	Fe I	6270.22	-2.47	2.858	7.472
KW208	Fe I	6297.79	-2.737	2.223	8.074
KW208	Fe I	6301.50	-0.72	3.654	7.704
KW208	Fe I	6322.68	-2.43	2.588	7.779
KW208	Fe I	6335.33	-2.177	2.198	7.716
KW208	Fe I	6336.82	-0.852	3.686	7.619
KW208	Fe I	6411.64	-0.596	3.654	7.527
KW208	Fe II	6416.91	-2.877	3.892	7.446
KW208	Fe II	6430.78	-2.768	12.316	7.513
KW208	Fe II	6432.67	-1.236	10.93	7.761
KW208	Fe I	6436.40	-2.58	4.186	7.791
KW208	Fe II	6456.37	-2.185	3.903	7.885
KW208	Fe I	6481.87	-2.981	2.279	7.842
KW208	Fe I	6498.87	-9.659	5.616	7.281
KW208	Fe I	6653.85	-2.215	4.154	7.553
KW208	Fe I	6710.31	-4.764	1.485	7.488
KW208	Fe I	6713.74	-1.5	4.796	7.607
KW208	Fe I	6725.43	-2.026	5.607	7.325
KW208	Fe I	6726.66	-1.133	4.607	7.622
KW208	Fe I	6739.52	-4.794	1.557	7.280
KW208	Fe I	6750.15	-2.618	2.424	7.713
KW208	Fe I	6810.31	-8.477	3.573	7.566
KW208	Fe II	7449.32	-3.09	3.889	7.387
KW208	Fe II	7711.72	-2.5	3.903	7.540
KW208	Fe I	8481.98	-1.988	4.186	7.741
KW208	Fe I	8514.07	-2.227	2.198	7.962
KW208	Fe I	8527.85	-1.625	5.02	7.563
KW208	Fe I	8582.25	-2.133	2.99	7.469
KW208	Fe I	8598.80	-2.567	5.943	7.574
KW208	Fe I	8611.80	-1.915	2.845	8.010
KW208	Fe I	8613.93	-1.247	4.988	7.706
KW208	Fe I	8621.60	-2.32	2.949	7.558
KW208	Fe I	8632.41	-2.32	4.103	7.743
KW208	Fe I	8699.45	-0.37	4.956	7.381
KW208	Fe I	8757.18	-2.035	2.845	7.864
KW208	Fe I	8763.96	-0.146	4.652	7.658
KW208	Fe I	8804.62	-3.231	2.279	7.529
KW30	Fe I	4808.14	-2.69	3.252	7.691
KW30	Fe I	5058.49	-2.83	3.642	7.648
KW30	Fe I	5197.57	-2.078	4.956	7.451
KW30	Fe II	5234.62	-2.18	3.221	7.569
KW30	Fe I	5243.77	-1.05	4.256	7.511
KW30	Fe II	5247.13	-2.014	10.909	7.475
KW30	Fe I	5253.02	-3.84	2.279	7.464
KW30	Fe II	5256.93	-4.182	2.891	7.763
KW30	Fe II	5264.80	-3.13	3.23	7.528
KW30	Fe I	5294.54	-2.76	3.64	7.564
KW30	Fe I	5295.31	-1.59	4.415	7.514
KW30	Fe II	5316.60	-1.87	3.153	7.565
KW30	Fe II	5337.72	-3.72	3.23	7.754
KW30	Fe I	5373.70	-0.71	4.473	7.344
KW30	Fe II	5379.61	-4.977	10.596	7.580
KW30	Fe I	5389.48	-8.475	5.33	7.505
KW30	Fe I	5398.27	-0.63	4.446	7.403
KW30	Fe I	5412.78	-1.716	4.435	7.566
KW30	Fe II	5414.07	-3.58	3.221	7.492
KW30	Fe I	5417.03	-1.58	4.415	7.649
KW30	Fe II	5425.24	-3.22	3.199	7.272
KW30	Fe II	5441.32	-6.066	11.741	7.654
KW30	Fe I	5466.39	-0.63	4.371	7.634
KW30	Fe I	5473.16	-2.04	4.191	7.524
KW30	Fe I	5473.90	-0.72	4.154	7.534
KW30	Fe I	5487.14	-1.43	4.415	7.617
KW30	Fe I	5491.83	-2.188	4.186	7.590
KW30	Fe I	5494.46	-1.99	4.076	7.689
KW30	Fe I	5501.46	-3.046	0.958	7.684
KW30	Fe I	5522.44	-1.45	4.209	7.569
KW30	Fe I	5534.78	-3.782	4.186	7.463
KW30	Fe I	5539.28	-2.56	3.642	7.665
KW30	Fe I	5543.93	-1.04	4.218	7.605
KW30	Fe I	5560.21	-1.09	4.435	7.507
KW30	Fe I	5577.02	-1.543	5.033	7.486
KW30	Fe I	5618.63	-1.255	4.209	7.553
KW30	Fe I	5633.94	-0.23	4.991	7.750
KW30	Fe II	5638.32	-6.266	12.968	7.413
KW30	Fe I	5651.52	-4.761	4.446	7.769
KW30	Fe I	5652.31	-1.85	4.26	7.688
KW30	Fe II	5661.31	-3.511	10.758	7.495
KW30	Fe I	5678.99	-9.163	5.388	7.706
KW30	Fe I	5705.46	-1.355	4.301	7.554
KW30	Fe I	5731.76	-1.2	4.256	7.523
KW30	Fe I	5732.29	-1.46	4.991	7.693
KW30	Fe I	5741.84	-1.672	4.256	7.611
KW30	Fe I	5775.08	-1.126	4.22	7.645
KW30	Fe II	5778.47	-3.814	10.858	7.535
KW30	Fe I	5849.68	-2.89	3.695	7.628
KW30	Fe I	5855.07	-1.478	4.608	7.573
KW30	Fe I	5858.77	-2.16	4.22	7.561
KW30	Fe I	5861.10	-2.304	4.283	7.627
KW30	Fe I	5905.67	-0.69	4.652	7.466
KW30	Fe I	5930.18	-0.23	4.652	7.685
KW30	Fe I	5934.65	-1.07	3.929	7.579
KW30	Fe II	5991.37	-3.647	3.153	7.597
KW30	Fe I	6027.09	-3.223	4.991	7.357
KW30	Fe I	6056.00	-0.32	4.733	7.485
KW30	Fe II	6084.10	-3.881	3.199	7.539
KW30	Fe I	6093.64	-1.4	4.608	7.606
KW30	Fe I	6113.30	-3.182	4.584	7.579
KW30	Fe II	6149.27	-3.283	13.155	7.569
KW30	Fe I	6151.61	-3.295	2.176	7.513
KW30	Fe I	6165.36	-1.473	4.143	7.554
KW30	Fe I	6173.33	-2.88	2.223	7.581
KW30	Fe I	6187.98	-1.62	3.943	7.514
KW30	Fe I	6200.31	-2.433	2.609	7.632
KW30	Fe I	6219.31	-5.082	5.458	7.570
KW30	Fe I	6226.73	-2.12	3.884	7.618
KW30	Fe II	6239.94	-3.573	3.889	7.767
KW30	Fe I	6246.31	-0.771	3.603	7.540
KW30	Fe II	6247.57	-4.827	5.956	7.583
KW30	Fe II	6252.62	-3.044	11.093	7.518
KW30	Fe I	6270.22	-2.47	2.858	7.486
KW30	Fe I	6297.79	-2.737	2.223	8.031
KW30	Fe I	6301.50	-0.72	3.654	7.661
KW30	Fe I	6322.68	-2.43	2.588	7.674
KW30	Fe I	6335.33	-2.177	2.198	7.498
KW30	Fe I	6336.82	-0.852	3.686	7.580
KW30	Fe I	6393.60	-1.452	2.433	7.424
KW30	Fe I	6411.64	-0.596	3.654	7.554
KW30	Fe II	6416.91	-2.877	3.892	7.336
KW30	Fe II	6430.78	-2.768	12.316	7.507
KW30	Fe II	6432.67	-1.236	10.93	7.693
KW30	Fe I	6436.40	-2.58	4.186	7.892
KW30	Fe II	6456.37	-2.185	3.903	7.695
KW30	Fe I	6481.87	-2.981	2.279	7.851
KW30	Fe I	6498.87	-9.659	5.616	7.372
KW30	Fe I	6518.36	-2.438	2.832	7.285
KW30	Fe I	6653.85	-2.215	4.154	7.409
KW30	Fe II	6699.10	-5.013	9.576	7.628
KW30	Fe I	6710.31	-4.764	1.485	7.609
KW30	Fe I	6713.74	-1.5	4.796	7.721
KW30	Fe I	6725.43	-2.026	5.607	7.432
KW30	Fe I	6726.66	-1.133	4.607	7.612
KW30	Fe I	6739.52	-4.794	1.557	7.420
KW30	Fe I	6750.15	-2.618	2.424	7.504
KW30	Fe I	6810.31	-8.477	3.573	7.544
KW30	Fe II	7449.32	-3.09	3.889	7.364
KW30	Fe II	7711.72	-2.5	3.903	7.446
KW30	Fe I	8481.98	-1.988	4.186	7.664
KW30	Fe I	8514.07	-2.227	2.198	7.863
KW30	Fe I	8582.25	-2.133	2.99	7.554
KW30	Fe I	8598.80	-2.567	5.943	7.456
KW30	Fe I	8611.80	-1.915	2.845	7.900
KW30	Fe I	8613.93	-1.247	4.988	7.873
KW30	Fe I	8621.60	-2.32	2.949	7.665
KW30	Fe I	8632.41	-2.32	4.103	7.718
KW30	Fe I	8699.45	-0.37	4.956	7.508
KW30	Fe I	8757.18	-2.035	2.845	7.703
KW30	Fe I	8763.96	-0.146	4.652	7.266
KW30	Fe I	8804.62	-3.231	2.279	7.604
KW23	Fe I	4808.14	-2.69	3.252	7.679
KW23	Fe I	4992.78	-2.35	4.26	7.062
KW23	Fe I	5058.49	-2.83	3.642	7.625
KW23	Fe I	5197.57	-2.078	4.956	7.553
KW23	Fe II	5234.62	-2.18	3.221	7.657
KW23	Fe I	5243.77	-1.05	4.256	7.657
KW23	Fe II	5247.13	-2.014	10.909	7.560
KW23	Fe I	5253.02	-3.84	2.279	7.518
KW23	Fe II	5256.93	-4.182	2.891	7.677
KW23	Fe II	5264.80	-3.13	3.23	7.538
KW23	Fe I	5294.54	-2.76	3.64	7.732
KW23	Fe I	5295.31	-1.59	4.415	7.720
KW23	Fe II	5316.60	-1.87	3.153	7.740
KW23	Fe II	5337.72	-3.72	3.23	7.798
KW23	Fe I	5373.70	-0.71	4.473	7.193
KW23	Fe II	5379.61	-4.977	10.596	7.450
KW23	Fe I	5389.48	-8.475	5.33	7.595
KW23	Fe I	5398.27	-0.63	4.446	7.557
KW23	Fe I	5412.78	-1.716	4.435	7.861
KW23	Fe II	5414.07	-3.58	3.221	7.627
KW23	Fe I	5417.03	-1.58	4.415	7.708
KW23	Fe II	5425.24	-3.22	3.199	7.537
KW23	Fe II	5441.32	-6.066	11.741	7.562
KW23	Fe I	5466.39	-0.63	4.371	7.674
KW23	Fe I	5473.16	-2.04	4.191	7.539
KW23	Fe I	5473.90	-0.72	4.154	7.585
KW23	Fe I	5487.14	-1.43	4.415	7.663
KW23	Fe I	5491.83	-2.188	4.186	7.562
KW23	Fe I	5494.46	-1.99	4.076	7.842
KW23	Fe I	5501.46	-3.046	0.958	7.843
KW23	Fe I	5534.78	-3.782	4.186	7.530
KW23	Fe I	5539.28	-2.56	3.642	7.550
KW23	Fe I	5543.93	-1.04	4.218	7.524
KW23	Fe II	5550.03	-6.71	8.266	7.530
KW23	Fe I	5560.21	-1.09	4.435	7.642
KW23	Fe I	5577.02	-1.543	5.033	7.634
KW23	Fe I	5618.63	-1.255	4.209	7.666
KW23	Fe I	5633.94	-0.23	4.991	7.682
KW23	Fe II	5638.32	-6.266	12.968	7.528
KW23	Fe I	5651.52	-4.761	4.446	7.935
KW23	Fe I	5652.31	-1.85	4.26	7.849
KW23	Fe II	5661.31	-3.511	10.758	7.604
KW23	Fe I	5678.99	-9.163	5.388	7.813
KW23	Fe I	5705.46	-1.355	4.301	7.588
KW23	Fe I	5731.76	-1.2	4.256	7.783
KW23	Fe I	5732.29	-1.46	4.991	7.790
KW23	Fe I	5741.84	-1.672	4.256	7.750
KW23	Fe I	5775.08	-1.126	4.22	7.777
KW23	Fe II	5778.47	-3.814	10.858	7.587
KW23	Fe I	5849.68	-2.89	3.695	7.578
KW23	Fe I	5855.07	-1.478	4.608	7.637
KW23	Fe I	5858.77	-2.16	4.22	7.631
KW23	Fe I	5861.10	-2.304	4.283	7.688
KW23	Fe I	5905.67	-0.69	4.652	7.434
KW23	Fe I	5930.18	-0.23	4.652	7.847
KW23	Fe I	5934.65	-1.07	3.929	7.660
KW23	Fe II	5991.37	-3.647	3.153	7.729
KW23	Fe I	6027.09	-3.223	4.991	7.452
KW23	Fe I	6056.00	-0.32	4.733	7.630
KW23	Fe II	6084.10	-3.881	3.199	7.667
KW23	Fe I	6093.64	-1.4	4.608	7.527
KW23	Fe I	6113.30	-3.182	4.584	7.612
KW23	Fe I	6151.61	-3.295	2.176	7.648
KW23	Fe I	6165.36	-1.473	4.143	7.709
KW23	Fe I	6173.33	-2.88	2.223	7.676
KW23	Fe I	6187.98	-1.62	3.943	7.624
KW23	Fe I	6200.31	-2.433	2.609	7.556
KW23	Fe I	6219.31	-5.082	5.458	7.677
KW23	Fe I	6226.73	-2.12	3.884	7.757
KW23	Fe II	6239.94	-3.573	3.889	7.786
KW23	Fe I	6246.31	-0.771	3.603	7.703
KW23	Fe II	6247.57	-4.827	5.956	7.625
KW23	Fe II	6252.62	-3.044	11.093	7.645
KW23	Fe I	6270.22	-2.47	2.858	7.513
KW23	Fe I	6297.79	-2.737	2.223	7.914
KW23	Fe I	6301.50	-0.72	3.654	7.710
KW23	Fe I	6322.68	-2.43	2.588	7.841
KW23	Fe I	6335.33	-2.177	2.198	7.621
KW23	Fe I	6336.82	-0.852	3.686	7.706
KW23	Fe I	6393.60	-1.452	2.433	7.517
KW23	Fe I	6411.64	-0.596	3.654	7.647
KW23	Fe II	6416.91	-2.877	3.892	7.472
KW23	Fe II	6430.78	-2.768	12.316	7.593
KW23	Fe II	6432.67	-1.236	10.93	7.652
KW23	Fe I	6436.40	-2.58	4.186	7.796
KW23	Fe II	6456.37	-2.185	3.903	7.712
KW23	Fe I	6481.87	-2.981	2.279	7.928
KW23	Fe I	6498.87	-9.659	5.616	7.385
KW23	Fe I	6518.36	-2.438	2.832	7.439
KW23	Fe I	6653.85	-2.215	4.154	7.617
KW23	Fe II	6699.10	-5.013	9.576	7.542
KW23	Fe I	6710.31	-4.764	1.485	7.630
KW23	Fe I	6713.74	-1.5	4.796	7.765
KW23	Fe I	6725.43	-2.026	5.607	7.488
KW23	Fe I	6726.66	-1.133	4.607	7.796
KW23	Fe I	6739.52	-4.794	1.557	7.488
KW23	Fe I	6750.15	-2.618	2.424	7.573
KW23	Fe I	6810.31	-8.477	3.573	7.732
KW23	Fe II	7449.32	-3.09	3.889	7.496
KW23	Fe II	7711.72	-2.5	3.903	7.491
KW23	Fe I	8481.98	-1.988	4.186	8.055
KW23	Fe I	8514.07	-2.227	2.198	7.938
KW23	Fe I	8527.85	-1.625	5.02	7.863
KW23	Fe I	8582.25	-2.133	2.99	7.432
KW23	Fe I	8598.80	-2.567	5.943	7.623
KW23	Fe I	8611.80	-1.915	2.845	7.709
KW23	Fe I	8613.93	-1.247	4.988	7.855
KW23	Fe I	8621.60	-2.32	2.949	7.734
KW23	Fe I	8632.41	-2.32	4.103	7.706
KW23	Fe I	8698.70	-3.452	2.99	7.837
KW23	Fe I	8699.45	-0.37	4.956	7.583
KW23	Fe I	8757.18	-2.035	2.845	7.662
KW23	Fe I	8763.96	-0.146	4.652	7.662
KW23	Fe I	8804.62	-3.231	2.279	7.745
JS 552	Fe II	5234.62	-2.18	3.221	7.424
JS 552	Fe I	5243.77	-1.05	4.256	7.569
JS 552	Fe II	5247.13	-2.014	10.909	7.215
JS 552	Fe I	5253.02	-3.84	2.279	7.760
JS 552	Fe II	5256.93	-4.182	2.891	7.922
JS 552	Fe I	5294.54	-2.76	3.64	7.305
JS 552	Fe I	5295.31	-1.59	4.415	7.219
JS 552	Fe II	5316.60	-1.87	3.153	7.634
JS 552	Fe I	5373.70	-0.71	4.473	7.400
JS 552	Fe II	5379.61	-4.977	10.596	7.307
JS 552	Fe I	5389.48	-8.475	5.33	7.389
JS 552	Fe I	5398.27	-0.63	4.446	7.417
JS 552	Fe I	5412.78	-1.716	4.435	7.658
JS 552	Fe I	5417.03	-1.58	4.415	7.807
JS 552	Fe II	5425.24	-3.22	3.199	7.705
JS 552	Fe I	5436.29	-1.44	4.387	7.654
JS 552	Fe II	5441.32	-6.066	11.741	7.712
JS 552	Fe I	5466.39	-0.63	4.371	7.575
JS 552	Fe I	5473.16	-2.04	4.191	7.498
JS 552	Fe I	5473.90	-0.72	4.154	7.274
JS 552	Fe I	5487.14	-1.43	4.415	7.413
JS 552	Fe I	5491.83	-2.188	4.186	7.030
JS 552	Fe I	5522.44	-1.45	4.209	7.708
JS 552	Fe I	5539.28	-2.56	3.642	7.871
JS 552	Fe I	5543.93	-1.04	4.218	7.626
JS 552	Fe I	5560.21	-1.09	4.435	7.344
JS 552	Fe I	5618.63	-1.255	4.209	7.608
JS 552	Fe I	5633.94	-0.23	4.991	7.575
JS 552	Fe II	5638.32	-6.266	12.968	7.360
JS 552	Fe I	5651.52	-4.761	4.446	7.574
JS 552	Fe I	5652.31	-1.85	4.26	7.612
JS 552	Fe II	5661.31	-3.511	10.758	7.597
JS 552	Fe I	5678.99	-9.163	5.388	7.702
JS 552	Fe I	5705.46	-1.355	4.301	7.413
JS 552	Fe I	5731.76	-1.2	4.256	7.833
JS 552	Fe I	5741.84	-1.672	4.256	7.741
JS 552	Fe I	5775.08	-1.126	4.22	7.755
JS 552	Fe II	5778.47	-3.814	10.858	7.787
JS 552	Fe I	5849.68	-2.89	3.695	7.587
JS 552	Fe I	5855.07	-1.478	4.608	7.463
JS 552	Fe I	5858.77	-2.16	4.22	7.359
JS 552	Fe I	5861.10	-2.304	4.283	7.681
JS 552	Fe I	5905.67	-0.69	4.652	7.976
JS 552	Fe I	5930.18	-0.23	4.652	7.680
JS 552	Fe I	5934.65	-1.07	3.929	7.494
JS 552	Fe II	5991.37	-3.647	3.153	7.365
JS 552	Fe I	6027.09	-3.223	4.991	7.258
JS 552	Fe I	6056.00	-0.32	4.733	7.400
JS 552	Fe I	6093.64	-1.4	4.608	7.376
JS 552	Fe II	6149.27	-3.283	13.155	7.062
JS 552	Fe I	6151.61	-3.295	2.176	7.511
JS 552	Fe I	6165.36	-1.473	4.143	7.585
JS 552	Fe I	6173.33	-2.88	2.223	7.616
JS 552	Fe I	6187.98	-1.62	3.943	7.618
JS 552	Fe I	6200.31	-2.433	2.609	7.872
JS 552	Fe I	6219.31	-5.082	5.458	7.699
JS 552	Fe I	6226.73	-2.12	3.884	7.653
JS 552	Fe I	6246.31	-0.771	3.603	7.681
JS 552	Fe I	6270.22	-2.47	2.858	7.215
JS 552	Fe I	6297.79	-2.737	2.223	7.922
JS 552	Fe I	6301.50	-0.72	3.654	7.798
JS 552	Fe I	6322.68	-2.43	2.588	7.598
JS 552	Fe I	6335.33	-2.177	2.198	7.556
JS 552	Fe I	6336.82	-0.852	3.686	7.802
JS 552	Fe I	6411.64	-0.596	3.654	7.617
JS 552	Fe II	6416.91	-2.877	3.892	7.194
JS 552	Fe II	6430.78	-2.768	12.316	7.586
JS 552	Fe II	6432.67	-1.236	10.93	7.788
JS 552	Fe I	6436.40	-2.58	4.186	7.861
JS 552	Fe II	6456.37	-2.185	3.903	7.849
JS 552	Fe I	6481.87	-2.981	2.279	7.520
JS 552	Fe I	6498.87	-9.659	5.616	7.511
JS 552	Fe I	6518.36	-2.438	2.832	7.276
JS 552	Fe I	6653.85	-2.215	4.154	7.414
JS 552	Fe II	6699.10	-5.013	9.576	7.485
JS 552	Fe I	6710.31	-4.764	1.485	7.296
JS 552	Fe I	6713.74	-1.5	4.796	7.707
JS 552	Fe I	6725.43	-2.026	5.607	7.405
JS 552	Fe I	6726.66	-1.133	4.607	7.834
JS 552	Fe I	6739.52	-4.794	1.557	7.224
JS 552	Fe I	6750.15	-2.618	2.424	7.457
JS 552	Fe I	6810.31	-8.477	3.573	7.638
JS 552	Fe I	8481.98	-1.988	4.186	7.653
JS 552	Fe I	8514.07	-2.227	2.198	7.912
JS 552	Fe I	8582.25	-2.133	2.99	7.374
JS 552	Fe I	8598.80	-2.567	5.943	7.335
JS 552	Fe I	8611.80	-1.915	2.845	7.781
JS 552	Fe I	8613.93	-1.247	4.988	7.771
JS 552	Fe I	8621.60	-2.32	2.949	7.069
JS 552	Fe I	8698.70	-3.452	2.99	7.098
JS 552	Fe I	8699.45	-0.37	4.956	7.282
JS 552	Fe I	8757.18	-2.035	2.845	7.773
JS 552	Fe I	8763.96	-0.146	4.652	7.605
JS 552	Fe I	8804.62	-3.231	2.279	7.489
JS 482	Fe I	4808.14	-2.69	3.252	7.924
JS 482	Fe II	5234.62	-2.18	3.221	7.441
JS 482	Fe I	5243.77	-1.05	4.256	7.313
JS 482	Fe II	5247.13	-2.014	10.909	7.484
JS 482	Fe I	5253.02	-3.84	2.279	7.559
JS 482	Fe I	5294.54	-2.76	3.64	7.268
JS 482	Fe II	5316.60	-1.87	3.153	7.608
JS 482	Fe II	5337.72	-3.72	3.23	7.437
JS 482	Fe I	5373.70	-0.71	4.473	7.325
JS 482	Fe II	5379.61	-4.977	10.596	7.051
JS 482	Fe I	5389.48	-8.475	5.33	7.430
JS 482	Fe I	5398.27	-0.63	4.446	7.422
JS 482	Fe I	5412.78	-1.716	4.435	7.658
JS 482	Fe I	5417.03	-1.58	4.415	7.483
JS 482	Fe II	5441.32	-6.066	11.741	7.703
JS 482	Fe I	5466.39	-0.63	4.371	7.475
JS 482	Fe I	5473.16	-2.04	4.191	7.300
JS 482	Fe I	5473.90	-0.72	4.154	7.255
JS 482	Fe I	5487.14	-1.43	4.415	7.154
JS 482	Fe I	5491.83	-2.188	4.186	7.210
JS 482	Fe I	5494.46	-1.99	4.076	7.141
JS 482	Fe I	5522.44	-1.45	4.209	7.702
JS 482	Fe I	5539.28	-2.56	3.642	7.612
JS 482	Fe I	5543.93	-1.04	4.218	7.593
JS 482	Fe II	5550.03	-6.71	8.266	7.459
JS 482	Fe I	5560.21	-1.09	4.435	7.358
JS 482	Fe I	5618.63	-1.255	4.209	7.364
JS 482	Fe I	5633.94	-0.23	4.991	7.595
JS 482	Fe II	5638.32	-6.266	12.968	7.252
JS 482	Fe I	5651.52	-4.761	4.446	7.904
JS 482	Fe I	5652.31	-1.85	4.26	7.693
JS 482	Fe II	5661.31	-3.511	10.758	7.627
JS 482	Fe I	5678.99	-9.163	5.388	7.711
JS 482	Fe I	5705.46	-1.355	4.301	7.516
JS 482	Fe I	5731.76	-1.2	4.256	7.878
JS 482	Fe I	5732.29	-1.46	4.991	7.772
JS 482	Fe I	5741.84	-1.672	4.256	7.740
JS 482	Fe I	5775.08	-1.126	4.22	7.841
JS 482	Fe II	5778.47	-3.814	10.858	7.630
JS 482	Fe I	5849.68	-2.89	3.695	7.305
JS 482	Fe I	5855.07	-1.478	4.608	7.47
JS 482	Fe I	5858.77	-2.16	4.22	7.336
JS 482	Fe I	5861.10	-2.304	4.283	7.598
JS 482	Fe I	5905.67	-0.69	4.652	7.800
JS 482	Fe I	5930.18	-0.23	4.652	7.717
JS 482	Fe I	5934.65	-1.07	3.929	7.603
JS 482	Fe I	6027.09	-3.223	4.991	7.211
JS 482	Fe I	6056.00	-0.32	4.733	7.514
JS 482	Fe I	6093.64	-1.4	4.608	7.460
JS 482	Fe I	6151.61	-3.295	2.176	7.592
JS 482	Fe I	6165.36	-1.473	4.143	7.448
JS 482	Fe I	6173.33	-2.88	2.223	7.452
JS 482	Fe I	6187.98	-1.62	3.943	7.555
JS 482	Fe I	6200.31	-2.433	2.609	7.644
JS 482	Fe I	6219.31	-5.082	5.458	7.498
JS 482	Fe I	6226.73	-2.12	3.884	7.767
JS 482	Fe II	6247.57	-4.827	5.956	7.506
JS 482	Fe I	6270.22	-2.47	2.858	7.280
JS 482	Fe I	6297.79	-2.737	2.223	7.687
JS 482	Fe I	6301.50	-0.72	3.654	7.576
JS 482	Fe I	6322.68	-2.43	2.588	7.657
JS 482	Fe I	6335.33	-2.177	2.198	7.453
JS 482	Fe I	6336.82	-0.852	3.686	7.645
JS 482	Fe I	6411.64	-0.596	3.654	7.574
JS 482	Fe II	6416.91	-2.877	3.892	7.453
JS 482	Fe I	6436.40	-2.58	4.186	7.716
JS 482	Fe I	6481.87	-2.981	2.279	7.677
JS 482	Fe I	6518.36	-2.438	2.832	7.381
JS 482	Fe I	6653.85	-2.215	4.154	7.355
JS 482	Fe I	6710.31	-4.764	1.485	7.450
JS 482	Fe I	6713.74	-1.5	4.796	7.804
JS 482	Fe I	6725.43	-2.026	5.607	7.386
JS 482	Fe I	6726.66	-1.133	4.607	7.774
JS 482	Fe I	6739.52	-4.794	1.557	7.445
JS 482	Fe I	6750.15	-2.618	2.424	7.578
JS 482	Fe I	6810.31	-8.477	3.573	7.751
JS 482	Fe I	8514.07	-2.227	2.198	7.643
JS 482	Fe I	8527.85	-1.625	5.02	7.615
JS 482	Fe I	8582.25	-2.133	2.99	7.333
JS 482	Fe I	8598.80	-2.567	5.943	7.434
JS 482	Fe I	8611.80	-1.915	2.845	7.599
JS 482	Fe I	8613.93	-1.247	4.988	8.132
JS 482	Fe I	8621.60	-2.32	2.949	7.318
JS 482	Fe I	8632.41	-2.32	4.103	7.247
JS 482	Fe I	8698.70	-3.452	2.99	7.994
JS 482	Fe I	8699.45	-0.37	4.956	7.475
JS 482	Fe I	8757.18	-2.035	2.845	7.892
JS 482	Fe I	8763.96	-0.146	4.652	7.586
JS 482	Fe I	8804.62	-3.231	2.279	7.542
KW208	Ca I	5260.38	-1.719	2.521	6.508
KW208	Ca I	5261.70	-0.579	2.521	6.592
KW208	Ca I	5349.46	-0.31	2.709	6.798
KW208	Ca I	5512.98	-0.464	2.933	6.672
KW208	Ca I	5581.96	-0.555	2.523	6.503
KW208	Ca I	5588.74	0.358	2.526	6.457
KW208	Ca I	5590.11	-0.571	2.521	6.697
KW208	Ca I	5857.45	0.24	2.933	6.619
KW208	Ca I	5867.56	-1.57	2.933	6.390
KW208	Ca I	6102.72	-0.85	1.879	6.551
KW208	Ca I	6122.21	-0.38	1.886	6.512
KW208	Ca I	6156.02	-2.521	2.521	6.652
KW208	Ca I	6162.17	-0.17	1.899	6.530
KW208	Ca I	6166.43	-1.142	2.521	6.470
KW208	Ca I	6169.04	-0.797	2.523	6.499
KW208	Ca I	6169.56	-0.478	2.526	6.493
KW208	Ca I	6439.07	0.39	2.526	6.499
KW208	Ca I	6455.59	-1.29	2.523	6.460
KW208	Ca II	6456.87	0.412	8.438	6.558
KW208	Ca I	6471.66	-0.686	2.526	6.801
KW208	Ca I	6493.78	-0.109	2.521	6.503
KW208	Ca I	6499.65	-0.818	2.523	6.633
KW30	Ca I	5260.38	-1.719	2.521	6.517
KW30	Ca I	5261.70	-0.579	2.521	6.546
KW30	Ca I	5349.46	-0.31	2.709	6.291
KW30	Ca I	5512.98	-0.464	2.933	6.533
KW30	Ca I	5581.96	-0.555	2.523	6.364
KW30	Ca I	5588.74	0.358	2.526	6.384
KW30	Ca I	5590.11	-0.571	2.521	6.603
KW30	Ca I	5857.45	0.24	2.933	6.578
KW30	Ca I	5867.56	-1.57	2.933	6.475
KW30	Ca I	6102.72	-0.85	1.879	6.504
KW30	Ca I	6166.43	-1.142	2.521	6.479
KW30	Ca I	6169.04	-0.797	2.523	6.432
KW30	Ca I	6169.56	-0.478	2.526	6.436
KW30	Ca I	6439.07	0.39	2.526	6.454
KW30	Ca I	6455.59	-1.29	2.523	6.385
KW30	Ca II	6456.87	0.412	8.438	6.524
KW30	Ca I	6471.66	-0.686	2.526	6.612
KW30	Ca I	6493.78	-0.109	2.521	6.467
KW30	Ca I	6499.65	-0.818	2.523	6.477
KW30	Ca II	8912.06	0.636	7.047	6.833
KW23	Ca I	5260.38	-1.719	2.521	6.552
KW23	Ca I	5261.70	-0.579	2.521	6.645
KW23	Ca I	5349.46	-0.31	2.709	6.399
KW23	Ca I	5512.98	-0.464	2.933	6.701
KW23	Ca I	5581.96	-0.555	2.523	5.896
KW23	Ca I	5590.11	-0.571	2.521	6.788
KW23	Ca I	5857.45	0.24	2.933	6.602
KW23	Ca I	5867.56	-1.57	2.933	6.559
KW23	Ca I	6102.72	-0.85	1.879	6.610
KW23	Ca I	6156.02	-2.521	2.521	6.541
KW23	Ca I	6166.43	-1.142	2.521	6.560
KW23	Ca I	6169.04	-0.797	2.523	6.558
KW23	Ca I	6169.56	-0.478	2.526	6.628
KW23	Ca I	6455.59	-1.29	2.523	6.474
KW23	Ca II	6456.87	0.412	8.438	6.627
KW23	Ca I	6471.66	-0.686	2.526	6.853
KW23	Ca I	6493.78	-0.109	2.521	6.451
KW23	Ca I	6499.65	-0.818	2.523	6.552
KW23	Ca II	8912.06	0.636	7.047	6.765
JS 552	Ca I	5260.38	-1.719	2.521	6.597
JS 552	Ca I	5867.56	-1.57	2.933	6.679
JS 552	Ca I	6156.02	-2.521	2.521	6.595
JS 552	Ca I	6166.43	-1.142	2.521	6.515
JS 552	Ca I	6455.59	-1.29	2.523	6.618
JS 552	Ca I	6499.65	-0.818	2.523	6.698
JS 552	Ca II	8912.06	0.636	7.047	6.856
JS 552	Ca II	8927.35	0.811	7.05	6.095
JS 482	Ca I	5260.38	-1.719	2.521	6.508
JS 482	Ca I	5867.56	-1.57	2.933	6.668
JS 482	Ca I	6156.02	-2.521	2.521	6.509
JS 482	Ca I	6166.43	-1.142	2.521	6.424
JS 482	Ca I	6455.59	-1.29	2.523	6.564
JS 482	Ca II	8927.35	0.811	7.05	6.485
KW208	Mg I	4571.09	-5.623	0.0	7.310
KW208	Mg I	4730.02	-2.347	4.346	7.675
KW208	Mg I	5528.40	-0.498	4.346	7.443
KW208	Mg I	5711.08	-1.724	4.346	7.546
KW208	Mg I	6318.71	-2.103	5.108	7.672
KW208	Mg I	6319.23	-2.324	5.108	7.758
KW208	Mg I	6319.49	-2.803	5.108	7.758
KW208	Mg I	8717.82	-0.866	5.933	7.615
KW208	Mg I	8736.01	-0.356	5.946	7.832
KW208	Mg I	8923.56	-1.678	5.394	7.746
KW30	Mg I	4571.09	-5.623	0.0	7.104
KW30	Mg I	4730.02	-2.347	4.346	7.735
KW30	Mg I	5711.08	-1.724	4.346	7.553
KW30	Mg I	6318.71	-2.103	5.108	7.725
KW30	Mg I	6319.23	-2.324	5.108	7.738
KW30	Mg I	6319.49	-2.803	5.108	7.736
KW30	Mg I	8712.68	-1.213	5.932	7.639
KW30	Mg I	8717.82	-0.866	5.933	7.489
KW30	Mg I	8736.01	-0.356	5.946	7.778
KW30	Mg I	8923.56	-1.678	5.394	7.725
KW23	Mg I	4571.09	-5.623	0.0	7.340
KW23	Mg I	4730.02	-2.347	4.346	7.887
KW23	Mg I	5711.08	-1.724	4.346	7.672
KW23	Mg I	6318.71	-2.103	5.108	7.667
KW23	Mg I	6319.23	-2.324	5.108	7.789
KW23	Mg I	6319.49	-2.803	5.108	7.790
KW23	Mg I	8712.68	-1.213	5.932	7.547
KW23	Mg I	8717.82	-0.866	5.933	7.607
KW23	Mg I	8736.01	-0.356	5.946	7.821
KW23	Mg I	8923.56	-1.678	5.394	7.675
JS 552	Mg I	5711.08	-1.724	4.346	7.531
JS 552	Mg I	6318.71	-2.103	5.108	7.705
JS 552	Mg I	6319.23	-2.324	5.108	7.739
JS 552	Mg I	6319.49	-2.803	5.108	7.748
JS 552	Mg I	8717.82	-0.866	5.933	7.343
JS 552	Mg I	8736.01	-0.356	5.946	7.555
JS 552	Mg I	8923.56	-1.678	5.394	7.563
JS 482	Mg I	4730.02	-2.347	4.346	7.271
JS 482	Mg I	5711.08	-1.724	4.346	7.451
JS 482	Mg I	6318.71	-2.103	5.108	7.730
JS 482	Mg I	6319.23	-2.324	5.108	7.811
JS 482	Mg I	6319.49	-2.803	5.108	7.797
JS 482	Mg I	8712.68	-1.213	5.932	7.581
JS 482	Mg I	8717.82	-0.866	5.933	7.447
JS 482	Mg I	8736.01	-0.356	5.946	7.584
JS 482	Mg I	8923.56	-1.678	5.394	7.797
KW208	Si I	5665.55	-1.94	4.92	7.555
KW208	Si I	5690.42	-1.773	4.93	7.535
KW208	Si I	5701.10	-1.953	4.93	7.257
KW208	Si I	5708.39	-1.37	4.954	7.671
KW208	Si I	5772.14	-1.653	5.082	7.740
KW208	Si I	5793.07	-1.963	4.93	7.738
KW208	Si I	5948.54	-1.13	5.082	7.923
KW208	Si II	6347.10	0.169	8.121	7.846
KW208	Si II	6371.37	-0.044	8.121	7.735
KW208	Si I	6741.62	-1.653	5.984	7.782
KW208	Si I	8892.72	-0.781	5.984	7.690
KW208	Si I	8899.23	-0.546	6.223	7.551
KW208	Si I	8949.09	-1.055	5.964	7.915
KW30	Si I	5645.61	-2.043	4.93	7.502
KW30	Si I	5665.55	-1.94	4.92	7.400
KW30	Si I	5684.48	-1.553	4.954	7.610
KW30	Si I	5690.42	-1.773	4.93	7.376
KW30	Si I	5701.10	-1.953	4.93	7.507
KW30	Si I	5708.39	-1.37	4.954	7.475
KW30	Si I	5772.14	-1.653	5.082	7.756
KW30	Si I	5793.07	-1.963	4.93	7.686
KW30	Si I	5948.54	-1.13	5.082	7.841
KW30	Si II	6347.10	0.169	8.121	7.818
KW30	Si II	6371.37	-0.044	8.121	7.531
KW30	Si I	6741.62	-1.653	5.984	7.714
KW30	Si I	8892.72	-0.781	5.984	7.862
KW30	Si I	8899.23	-0.546	6.223	7.572
KW30	Si I	8949.09	-1.055	5.964	7.910
KW23	Si I	5645.61	-2.043	4.93	7.488
KW23	Si I	5665.55	-1.94	4.92	7.471
KW23	Si I	5684.48	-1.553	4.954	7.515
KW23	Si I	5690.42	-1.773	4.93	7.528
KW23	Si I	5701.10	-1.953	4.93	7.620
KW23	Si I	5708.39	-1.37	4.954	7.711
KW23	Si I	5772.14	-1.653	5.082	7.765
KW23	Si I	5793.07	-1.963	4.93	7.696
KW23	Si I	5948.54	-1.13	5.082	7.945
KW23	Si II	6347.10	0.169	8.121	7.724
KW23	Si II	6371.37	-0.044	8.121	7.628
KW23	Si I	6741.62	-1.653	5.984	7.774
KW23	Si I	8892.72	-0.781	5.984	7.826
KW23	Si I	8899.23	-0.546	6.223	7.563
KW23	Si I	8949.09	-1.055	5.964	7.940
JS 552	Si I	5684.48	-1.553	4.954	7.126
JS 552	Si I	5690.42	-1.773	4.93	7.251
JS 552	Si I	5701.10	-1.953	4.93	7.769
JS 552	Si I	5772.14	-1.653	5.082	7.580
JS 552	Si I	5793.07	-1.963	4.93	7.487
JS 552	Si I	5948.54	-1.13	5.082	7.708
JS 552	Si II	6347.10	0.169	8.121	7.788
JS 552	Si I	6741.62	-1.653	5.984	7.617
JS 552	Si I	8892.72	-0.781	5.984	8.040
JS 552	Si I	8949.09	-1.055	5.964	7.407
JS 482	Si I	5645.61	-2.043	4.93	7.203
JS 482	Si I	5665.55	-1.94	4.92	7.811
JS 482	Si I	5690.42	-1.773	4.93	7.504
JS 482	Si I	5701.10	-1.953	4.93	7.872
JS 482	Si I	5793.07	-1.963	4.93	7.828
JS 482	Si I	5948.54	-1.13	5.082	7.469
JS 482	Si I	8892.72	-0.781	5.984	8.019
JS 482	Si I	8949.09	-1.055	5.964	7.630
KW208	Ti I	4534.77	0.35	0.836	5.065
KW208	Ti I	4548.76	-0.28	0.826	4.581
KW208	Ti II	4798.53	-2.66	1.08	4.906
KW208	Ti II	4865.61	-2.7	1.116	4.657
KW208	Ti II	4874.00	-0.86	3.095	5.043
KW208	Ti II	4911.19	-0.64	3.124	5.130
KW208	Ti I	4913.61	0.22	1.873	4.706
KW208	Ti I	4981.73	0.57	0.848	5.078
KW208	Ti I	4999.50	0.32	0.826	5.043
KW208	Ti II	5005.16	-2.73	1.566	4.918
KW208	Ti I	5016.16	-0.48	0.848	4.846
KW208	Ti I	5024.84	-0.53	0.818	4.988
KW208	Ti I	5039.94	-2.427	2.333	4.854
KW208	Ti I	5043.58	-1.59	0.836	5.129
KW208	Ti I	5113.44	-0.7	1.443	4.849
KW208	Ti II	5129.15	-1.34	1.892	5.173
KW208	Ti I	5147.47	-1.94	0.0	5.036
KW208	Ti II	5185.90	-1.41	1.893	4.535
KW208	Ti I	5210.38	-0.82	0.048	4.932
KW208	Ti II	5211.53	-1.41	2.59	5.145
KW208	Ti I	5219.70	-2.22	0.021	4.984
KW208	Ti I	5224.30	0.13	2.134	4.990
KW208	Ti I	5295.77	-1.59	1.067	4.774
KW208	Ti II	5336.78	-1.6	1.582	5.290
KW208	Ti II	5381.02	-1.97	1.566	5.289
KW208	Ti II	5418.76	-2.13	1.582	5.118
KW208	Ti I	5460.49	-2.748	0.048	5.396
KW208	Ti I	5490.12	-1.001	3.334	4.911
KW208	Ti I	5490.69	-5.508	2.154	4.793
KW208	Ti I	5490.84	-3.35	0.048	4.791
KW208	Ti I	5689.46	-0.36	2.297	4.941
KW208	Ti I	5716.45	-0.72	2.297	4.896
KW208	Ti I	5866.36	-1.055	3.305	4.740
KW208	Ti I	5918.53	-1.64	1.067	5.472
KW208	Ti I	5922.11	-1.38	1.046	5.072
KW208	Ti I	5937.80	-1.94	1.067	5.084
KW208	Ti I	5965.82	-0.353	1.879	4.676
KW208	Ti I	5978.54	-0.44	1.873	4.985
KW208	Ti I	6064.62	-1.888	1.046	5.088
KW208	Ti I	6091.17	-0.32	2.267	5.037
KW208	Ti I	6126.21	-1.368	1.067	5.046
KW208	Ti I	6258.10	-0.39	1.443	4.964
KW208	Ti I	6261.09	-0.53	1.43	5.074
KW208	Ti I	6312.23	-1.55	1.46	5.052
KW208	Ti I	8682.98	-1.79	1.053	5.012
KW30	Ti I	4534.77	0.35	0.836	4.863
KW30	Ti II	4865.61	-2.7	1.116	4.800
KW30	Ti II	4874.00	-0.86	3.095	4.901
KW30	Ti II	4911.19	-0.64	3.124	5.197
KW30	Ti I	4915.22	-0.91	1.887	5.195
KW30	Ti I	4926.14	-2.09	0.818	4.769
KW30	Ti I	4964.72	-0.82	1.969	4.470
KW30	Ti I	4981.73	0.57	0.848	5.011
KW30	Ti I	4999.50	0.32	0.826	4.838
KW30	Ti II	5005.16	-2.73	1.566	4.953
KW30	Ti I	5009.64	-2.2	0.021	4.950
KW30	Ti I	5016.16	-0.48	0.848	4.999
KW30	Ti I	5024.84	-0.53	0.818	5.107
KW30	Ti I	5039.94	-2.427	2.333	4.898
KW30	Ti I	5043.58	-1.59	0.836	5.140
KW30	Ti II	5129.15	-1.34	1.892	5.028
KW30	Ti I	5145.46	-0.54	1.46	4.609
KW30	Ti I	5147.47	-1.94	0.0	4.865
KW30	Ti II	5211.53	-1.41	2.59	4.873
KW30	Ti I	5219.70	-2.22	0.021	4.995
KW30	Ti I	5224.30	0.13	2.134	4.752
KW30	Ti I	5295.77	-1.59	1.067	4.853
KW30	Ti II	5336.78	-1.6	1.582	5.040
KW30	Ti II	5381.02	-1.97	1.566	5.201
KW30	Ti I	5384.63	-2.77	0.826	5.235
KW30	Ti II	5418.76	-2.13	1.582	5.109
KW30	Ti I	5426.25	-2.95	0.021	4.900
KW30	Ti I	5460.49	-2.748	0.048	5.407
KW30	Ti I	5490.12	-1.001	3.334	4.850
KW30	Ti I	5490.69	-5.508	2.154	4.798
KW30	Ti I	5490.84	-3.35	0.048	4.796
KW30	Ti I	5689.46	-0.36	2.297	5.030
KW30	Ti I	5716.45	-0.72	2.297	5.002
KW30	Ti I	5866.36	-1.055	3.305	4.821
KW30	Ti I	5903.31	-2.089	1.067	4.982
KW30	Ti I	5918.53	-1.64	1.067	5.417
KW30	Ti I	5922.11	-1.38	1.046	4.914
KW30	Ti I	5937.80	-1.94	1.067	5.091
KW30	Ti I	5953.16	-0.273	1.887	5.051
KW30	Ti I	5965.82	-0.353	1.879	4.698
KW30	Ti I	5978.54	-0.44	1.873	5.005
KW30	Ti I	6064.62	-1.888	1.046	5.147
KW30	Ti I	6091.17	-0.32	2.267	4.961
KW30	Ti I	6126.21	-1.368	1.067	4.986
KW30	Ti I	6258.10	-0.39	1.443	5.050
KW30	Ti I	6261.09	-0.53	1.43	5.066
KW30	Ti I	6312.23	-1.55	1.46	5.164
KW30	Ti I	6336.09	-1.69	1.443	5.181
KW30	Ti I	6554.22	-1.15	1.443	4.721
KW30	Ti I	6556.06	-1.06	1.46	4.765
KW30	Ti I	6599.10	-2.029	0.9	5.155
KW30	Ti I	8682.98	-1.79	1.053	5.071
KW23	Ti I	4534.77	0.35	0.836	4.992
KW23	Ti I	4548.76	-0.28	0.826	4.757
KW23	Ti II	4798.53	-2.66	1.08	5.036
KW23	Ti II	4865.61	-2.7	1.116	4.879
KW23	Ti II	4874.00	-0.86	3.095	4.988
KW23	Ti II	4911.19	-0.64	3.124	5.202
KW23	Ti I	4913.61	0.22	1.873	4.948
KW23	Ti I	4915.22	-0.91	1.887	5.049
KW23	Ti I	4926.14	-2.09	0.818	4.858
KW23	Ti I	4964.72	-0.82	1.969	4.979
KW23	Ti I	4981.73	0.57	0.848	5.137
KW23	Ti I	4999.50	0.32	0.826	5.082
KW23	Ti II	5005.16	-2.73	1.566	4.992
KW23	Ti I	5009.64	-2.2	0.021	4.939
KW23	Ti I	5016.16	-0.48	0.848	5.223
KW23	Ti I	5024.84	-0.53	0.818	5.117
KW23	Ti I	5039.94	-2.427	2.333	4.893
KW23	Ti I	5043.58	-1.59	0.836	5.130
KW23	Ti I	5113.44	-0.7	1.443	4.956
KW23	Ti II	5129.15	-1.34	1.892	4.937
KW23	Ti I	5145.46	-0.54	1.46	4.748
KW23	Ti I	5147.47	-1.94	0.0	4.913
KW23	Ti I	5210.38	-0.82	0.048	5.056
KW23	Ti II	5211.53	-1.41	2.59	5.074
KW23	Ti I	5219.70	-2.22	0.021	5.141
KW23	Ti I	5224.30	0.13	2.134	4.981
KW23	Ti I	5295.77	-1.59	1.067	5.021
KW23	Ti II	5336.78	-1.6	1.582	5.169
KW23	Ti II	5381.02	-1.97	1.566	5.194
KW23	Ti II	5418.76	-2.13	1.582	5.152
KW23	Ti I	5426.25	-2.95	0.021	5.004
KW23	Ti I	5460.49	-2.748	0.048	5.495
KW23	Ti I	5490.12	-1.001	3.334	5.040
KW23	Ti I	5490.69	-5.508	2.154	4.894
KW23	Ti I	5490.84	-3.35	0.048	4.894
KW23	Ti I	5689.46	-0.36	2.297	5.141
KW23	Ti I	5716.45	-0.72	2.297	5.243
KW23	Ti I	5866.36	-1.055	3.305	4.990
KW23	Ti I	5903.31	-2.089	1.067	5.116
KW23	Ti I	5918.53	-1.64	1.067	5.492
KW23	Ti I	5922.11	-1.38	1.046	5.178
KW23	Ti I	5937.80	-1.94	1.067	5.173
KW23	Ti I	5953.16	-0.273	1.887	5.190
KW23	Ti I	5965.82	-0.353	1.879	4.982
KW23	Ti I	5978.54	-0.44	1.873	5.137
KW23	Ti I	6064.62	-1.888	1.046	5.294
KW23	Ti I	6091.17	-0.32	2.267	5.099
KW23	Ti I	6126.21	-1.368	1.067	5.137
KW23	Ti I	6258.10	-0.39	1.443	5.082
KW23	Ti I	6261.09	-0.53	1.43	5.234
KW23	Ti I	6312.23	-1.55	1.46	5.136
KW23	Ti I	6554.22	-1.15	1.443	4.869
KW23	Ti I	6599.10	-2.029	0.9	5.157
KW23	Ti I	8682.98	-1.79	1.053	5.147
KW23	Ti I	8692.32	-2.13	1.046	5.429
KW23	Ti I	8734.71	-2.24	1.053	5.320
JS 552	Ti II	4865.61	-2.7	1.116	4.997
JS 552	Ti II	4911.19	-0.64	3.124	4.831
JS 552	Ti I	4913.61	0.22	1.873	5.023
JS 552	Ti I	4915.22	-0.91	1.887	5.268
JS 552	Ti I	4926.14	-2.09	0.818	5.055
JS 552	Ti I	4964.72	-0.82	1.969	4.646
JS 552	Ti I	4997.09	-2.07	0.0	4.736
JS 552	Ti II	5211.53	-1.41	2.59	4.755
JS 552	Ti I	5219.70	-2.22	0.021	5.226
JS 552	Ti I	5224.30	0.13	2.134	5.006
JS 552	Ti I	5295.77	-1.59	1.067	4.894
JS 552	Ti II	5336.78	-1.6	1.582	4.753
JS 552	Ti I	5338.30	-2.73	0.826	5.425
JS 552	Ti I	5366.63	-2.46	0.818	5.282
JS 552	Ti II	5381.02	-1.97	1.566	4.520
JS 552	Ti I	5384.63	-2.77	0.826	5.031
JS 552	Ti II	5418.76	-2.13	1.582	4.796
JS 552	Ti I	5426.25	-2.95	0.021	5.208
JS 552	Ti I	5460.49	-2.748	0.048	5.030
JS 552	Ti I	5490.12	-1.001	3.334	5.125
JS 552	Ti I	5490.69	-5.508	2.154	5.018
JS 552	Ti I	5490.84	-3.35	0.048	5.018
JS 552	Ti I	5662.15	0.01	2.318	5.185
JS 552	Ti I	5689.46	-0.36	2.297	5.017
JS 552	Ti I	5702.66	-0.59	2.292	5.074
JS 552	Ti I	5716.45	-0.72	2.297	5.174
JS 552	Ti I	5866.36	-1.055	3.305	4.870
JS 552	Ti I	5903.31	-2.089	1.067	5.227
JS 552	Ti I	5918.53	-1.64	1.067	5.181
JS 552	Ti I	5922.11	-1.38	1.046	4.807
JS 552	Ti I	5937.80	-1.94	1.067	5.171
JS 552	Ti I	5953.16	-0.273	1.887	5.001
JS 552	Ti I	5965.82	-0.353	1.879	5.170
JS 552	Ti I	5978.54	-0.44	1.873	5.053
JS 552	Ti I	6064.62	-1.888	1.046	5.259
JS 552	Ti I	6091.17	-0.32	2.267	5.000
JS 552	Ti I	6092.79	-1.38	1.887	4.892
JS 552	Ti I	6126.21	-1.368	1.067	5.044
JS 552	Ti I	6258.10	-0.39	1.443	4.821
JS 552	Ti I	6261.09	-0.53	1.43	5.249
JS 552	Ti I	6312.23	-1.55	1.46	5.083
JS 552	Ti I	6336.09	-1.69	1.443	5.395
JS 552	Ti I	6554.22	-1.15	1.443	5.169
JS 552	Ti I	6556.06	-1.06	1.46	5.116
JS 552	Ti I	6599.10	-2.029	0.9	5.299
JS 552	Ti I	8682.98	-1.79	1.053	5.139
JS 552	Ti I	8692.32	-2.13	1.046	5.306
JS 552	Ti I	8719.57	-2.3	1.739	4.906
JS 552	Ti I	8734.71	-2.24	1.053	5.219
JS 482	Ti II	4865.61	-2.7	1.116	4.928
JS 482	Ti II	4911.19	-0.64	3.124	4.837
JS 482	Ti I	4913.61	0.22	1.873	5.115
JS 482	Ti I	4926.14	-2.09	0.818	5.159
JS 482	Ti I	4997.09	-2.07	0.0	4.697
JS 482	Ti I	5113.44	-0.7	1.443	4.648
JS 482	Ti I	5219.70	-2.22	0.021	5.279
JS 482	Ti I	5224.30	0.13	2.134	4.951
JS 482	Ti I	5295.77	-1.59	1.067	4.691
JS 482	Ti II	5336.78	-1.6	1.582	4.998
JS 482	Ti I	5338.30	-2.73	0.826	5.347
JS 482	Ti II	5381.02	-1.97	1.566	4.646
JS 482	Ti I	5384.63	-2.77	0.826	4.989
JS 482	Ti II	5418.76	-2.13	1.582	4.937
JS 482	Ti I	5460.49	-2.748	0.048	5.316
JS 482	Ti I	5490.12	-1.001	3.334	5.006
JS 482	Ti I	5490.69	-5.508	2.154	5.009
JS 482	Ti I	5490.84	-3.35	0.048	5.009
JS 482	Ti I	5662.15	0.01	2.318	5.141
JS 482	Ti I	5689.46	-0.36	2.297	5.032
JS 482	Ti I	5716.45	-0.72	2.297	5.319
JS 482	Ti I	5903.31	-2.089	1.067	5.338
JS 482	Ti I	5918.53	-1.64	1.067	5.551
JS 482	Ti I	5922.11	-1.38	1.046	5.080
JS 482	Ti I	5937.80	-1.94	1.067	5.267
JS 482	Ti I	5953.16	-0.273	1.887	4.539
JS 482	Ti I	5965.82	-0.353	1.879	4.979
JS 482	Ti I	5978.54	-0.44	1.873	5.004
JS 482	Ti I	6064.62	-1.888	1.046	5.165
JS 482	Ti I	6091.17	-0.32	2.267	4.934
JS 482	Ti I	6092.79	-1.38	1.887	4.967
JS 482	Ti I	6126.21	-1.368	1.067	5.304
JS 482	Ti I	6258.10	-0.39	1.443	5.027
JS 482	Ti I	6312.23	-1.55	1.46	5.119
JS 482	Ti I	6336.09	-1.69	1.443	5.392
JS 482	Ti I	6395.47	-2.54	1.503	5.301
JS 482	Ti I	6554.22	-1.15	1.443	5.021
JS 482	Ti I	6556.06	-1.06	1.46	5.078
JS 482	Ti I	6599.10	-2.029	0.9	5.255
JS 482	Ti I	8682.98	-1.79	1.053	5.594
JS 482	Ti I	8692.32	-2.13	1.046	4.995
JS 482	Ti I	8719.57	-2.3	1.739	4.892
JS 482	Ti I	8734.71	-2.24	1.053	5.242
KW208	O I	7771.94	0.369	9.146	9.065
KW208	O I	7774.16	0.223	9.146	8.985
KW208	O I	7775.38	0.002	9.146	9.087
KW30	O I	7771.94	0.369	9.146	8.828
KW30	O I	7774.16	0.223	9.146	8.852
KW30	O I	7775.38	0.002	9.146	8.840
KW23	O I	6300.30	-9.715	0.0	8.820
KW23	O I	7771.94	0.369	9.146	8.823
KW23	O I	7774.16	0.223	9.146	8.842
KW23	O I	7775.38	0.002	9.146	9.061
JS 552	O I	7774.16	0.223	9.146	8.437
JS 482	O I	7774.16	0.223	9.146	8.455
KW208	Al I	6698.67	-1.87	3.143	6.511
KW30	Al I	6698.67	-1.87	3.143	6.515
KW23	Al I	6698.67	-1.87	3.143	6.666
JS 552	Al I	6698.67	-1.87	3.143	6.650
JS 482	Al I	6698.67	-1.87	3.143	6.563
KW208	Ba II	5853.67	-1.965	0.604	2.601
KW30	Ba II	5853.67	-1.965	0.604	2.373
KW23	Ba II	5853.67	-1.965	0.604	2.513
JS 552	Ba II	5853.67	-1.965	0.604	2.271
JS 482	Ba II	5853.67	-1.965	0.604	2.216
KW208	Na I	6154.22	-1.547	2.102	5.871
KW208	Na I	6160.74	-1.246	2.104	6.322
KW30	Na I	6154.22	-1.547	2.102	6.351
KW30	Na I	6160.74	-1.246	2.104	6.397
KW23	Na I	6154.22	-1.547	2.102	6.568
KW23	Na I	6160.74	-1.246	2.104	6.467
JS 552	Na I	6154.22	-1.547	2.102	6.353
JS 482	Na I	6154.22	-1.547	2.102	6.154
JS 482	Na I	6160.74	-1.246	2.104	6.514
KW208	Ni I	4873.43	-0.38	3.699	6.201
KW208	Ni I	4976.13	-1.26	3.606	6.248
KW208	Ni I	4976.32	-3.0	1.676	6.248
KW208	Ni I	4976.69	-1.38	4.236	6.236
KW208	Ni I	5003.74	-3.07	1.676	6.401
KW208	Ni I	5035.35	0.29	3.635	6.247
KW208	Ni I	5157.97	-1.51	3.606	5.926
KW208	Ni II	5424.57	-2.038	6.473	6.303
KW208	Ni I	5435.85	-2.58	1.986	6.374
KW208	Ni I	5476.90	-0.78	1.826	6.332
KW208	Ni I	5587.85	-2.39	1.935	6.263
KW208	Ni I	5846.99	-3.46	1.676	6.145
KW208	Ni I	6108.11	-2.6	1.676	6.337
KW208	Ni I	6176.80	-0.26	4.088	6.388
KW208	Ni I	6204.60	-1.08	4.088	6.213
KW208	Ni I	6223.98	-0.91	4.105	6.179
KW208	Ni I	6230.08	-1.26	4.105	6.413
KW208	Ni I	6327.59	-3.17	1.676	6.388
KW208	Ni I	6378.24	-0.82	4.154	6.221
KW208	Ni II	6482.80	-0.015	14.744	6.271
KW208	Ni I	6643.63	-2.22	1.676	6.572
KW208	Ni I	6767.77	-2.14	1.826	6.485
KW30	Ni I	4873.43	-0.38	3.699	6.109
KW30	Ni I	4976.32	-3.0	1.676	6.282
KW30	Ni II	5424.57	-2.038	6.473	6.195
KW30	Ni I	5435.85	-2.58	1.986	6.403
KW30	Ni I	5587.85	-2.39	1.935	6.139
KW30	Ni I	5846.99	-3.46	1.676	6.135
KW30	Ni I	6108.11	-2.6	1.676	6.360
KW30	Ni I	6176.80	-0.26	4.088	6.280
KW30	Ni I	6204.60	-1.08	4.088	6.320
KW30	Ni I	6223.98	-0.91	4.105	6.093
KW30	Ni I	6230.08	-1.26	4.105	6.476
KW30	Ni I	6327.59	-3.17	1.676	6.455
KW30	Ni I	6378.24	-0.82	4.154	6.379
KW30	Ni II	6482.80	-0.015	14.744	6.382
KW30	Ni I	6643.63	-2.22	1.676	6.551
KW30	Ni I	6767.77	-2.14	1.826	6.382
KW23	Ni I	4811.98	-1.45	3.658	6.331
KW23	Ni I	4873.43	-0.38	3.699	6.200
KW23	Ni I	4976.32	-3.0	1.676	6.308
KW23	Ni I	4976.69	-1.38	4.236	6.207
KW23	Ni I	5035.35	0.29	3.635	6.196
KW23	Ni I	5157.97	-1.51	3.606	6.207
KW23	Ni II	5424.57	-2.038	6.473	6.343
KW23	Ni I	5435.85	-2.58	1.986	6.258
KW23	Ni I	5587.85	-2.39	1.935	6.209
KW23	Ni I	5846.99	-3.46	1.676	6.255
KW23	Ni I	6108.11	-2.6	1.676	6.304
KW23	Ni I	6176.80	-0.26	4.088	6.525
KW23	Ni I	6204.60	-1.08	4.088	6.416
KW23	Ni I	6223.98	-0.91	4.105	6.237
KW23	Ni I	6230.08	-1.26	4.105	6.601
KW23	Ni I	6327.59	-3.17	1.676	6.515
KW23	Ni I	6378.24	-0.82	4.154	6.440
KW23	Ni II	6482.80	-0.015	14.744	6.451
KW23	Ni I	6643.63	-2.22	1.676	6.642
KW23	Ni I	6767.77	-2.14	1.826	6.578
JS 552	Ni I	4873.43	-0.38	3.699	6.365
JS 552	Ni I	4976.32	-3.0	1.676	6.199
JS 552	Ni I	4976.69	-1.38	4.236	6.326
JS 552	Ni I	5035.35	0.29	3.635	6.033
JS 552	Ni II	5424.57	-2.038	6.473	6.292
JS 552	Ni I	5435.85	-2.58	1.986	6.406
JS 552	Ni I	5587.85	-2.39	1.935	6.072
JS 552	Ni I	5846.99	-3.46	1.676	6.133
JS 552	Ni I	6108.11	-2.6	1.676	6.408
JS 552	Ni I	6176.80	-0.26	4.088	6.25
JS 552	Ni I	6204.60	-1.08	4.088	6.277
JS 552	Ni I	6327.59	-3.17	1.676	6.359
JS 552	Ni I	6378.24	-0.82	4.154	6.522
JS 552	Ni I	6414.58	-1.16	4.154	6.06
JS 552	Ni II	6482.80	-0.015	14.744	6.15
JS 552	Ni I	6643.63	-2.22	1.676	6.382
JS 552	Ni I	6767.77	-2.14	1.826	6.296
JS 482	Ni I	4873.43	-0.38	3.699	6.102
JS 482	Ni I	4976.32	-3.0	1.676	6.632
JS 482	Ni I	5003.74	-3.07	1.676	6.085
JS 482	Ni I	5035.35	0.29	3.635	5.913
JS 482	Ni II	5424.57	-2.038	6.473	6.295
JS 482	Ni I	5435.85	-2.58	1.986	6.468
JS 482	Ni I	5587.85	-2.39	1.935	5.796
JS 482	Ni I	5846.99	-3.46	1.676	6.227
JS 482	Ni I	6108.11	-2.6	1.676	6.531
JS 482	Ni I	6176.80	-0.26	4.088	6.33
JS 482	Ni I	6204.60	-1.08	4.088	6.458
JS 482	Ni I	6223.98	-0.91	4.105	6.208
JS 482	Ni I	6327.59	-3.17	1.676	6.691
JS 482	Ni I	6378.24	-0.82	4.154	6.44
JS 482	Ni I	6414.58	-1.16	4.154	6.164
JS 482	Ni II	6482.80	-0.015	14.744	6.512
JS 482	Ni I	6643.63	-2.22	1.676	6.52
JS 482	Ni I	6767.77	-2.14	1.826	6.422
JS 482	Eu II	6645.10	-0.625	1.380	0.986
KW208	La II	4804.00	-2.092	0.235	1.206
KW208	La II	4921.77	-0.45	0.244	1.093
KW208	La II	4970.39	-1.16	0.321	1.722
KW30	La II	4804.00	-2.092	0.235	1.705
KW30	La II	4921.77	-0.45	0.244	1.272
KW30	La II	4970.39	-1.16	0.321	1.638
KW30	La II	4986.82	-1.3	0.173	1.092
KW30	La II	6390.50	-2.079	0.321	1.481
KW23	La II	4740.28	-1.05	0.126	1.352
KW23	La II	4804.00	-2.092	0.235	1.335
KW23	La II	4921.77	-0.45	0.244	1.204
KW23	La II	4986.82	-1.3	0.173	1.341
KW23	La II	5936.19	-3.057	0.173	1.335
KW23	La II	6390.50	-2.079	0.321	1.370
JS 552	La II	4740.28	-1.05	0.126	0.926
JS 552	La II	4804.00	-2.092	0.235	1.544
JS 552	La II	6262.29	-1.22	0.403	1.542
JS 552	La II	6390.50	-2.079	0.321	1.621
JS 482	La II	4662.50	-1.24	0.0	1.354
JS 482	La II	5303.51	-1.731	0.321	1.565
JS 482	La II	6262.29	-1.22	0.403	1.113
KW208	Zr II	4496.96	-0.89	0.713	2.735
KW208	Zr II	5112.27	-0.85	1.665	2.676
KW208	Zr I	6134.55	-1.28	0.0	2.484
KW30	Zr II	4496.96	-0.89	0.713	2.197
KW30	Zr I	4784.92	-0.49	0.687	2.183
KW30	Zr I	6134.55	-1.28	0.0	2.645
KW23	Zr II	5112.27	-0.85	1.665	2.393
KW23	Zr I	6134.55	-1.28	0.0	2.788
JS 552	Zr I	5385.14	-0.71	0.519	2.476
JS 552	Zr I	6127.44	-1.06	0.154	2.803
JS 552	Zr I	6127.44	-1.06	0.154	2.796
JS 552	Zr I	6134.55	-1.28	0.0	2.831
JS 552	Zr I	6140.46	-1.41	0.519	2.641
JS 552	Zr I	6143.20	-1.1	0.071	2.631
JS 482	Zr I	4828.04	-0.64	0.623	2.512
JS 482	Zr I	5385.14	-0.71	0.519	3.084
JS 482	Zr I	6127.44	-1.06	0.154	3.063
JS 482	Zr I	6127.44	-1.06	0.154	3.069
JS 482	Zr I	6134.55	-1.28	0.0	2.853
JS 482	Zr I	6140.46	-1.41	0.519	2.666
JS 482	Zr I	6143.20	-1.1	0.071	2.943
KW208	Sr I	7070.07	-0.03	1.847	3.173
KW30	Sr I	4607.33	0.283	0.0	2.520
KW30	Sr I	4811.87	0.19	1.847	2.879
KW30	Sr I	7070.07	-0.03	1.847	3.283
KW23	Sr I	4607.33	0.283	0.0	2.732
KW23	Sr I	4811.87	0.19	1.847	2.934
KW23	Sr I	7070.07	-0.03	1.847	3.212
JS 552	Sr I	7070.07	-0.03	1.847	3.211
JS 482	Sr I	6550.24	0.46	2.69	2.899
JS 482	Sr I	6878.31	-0.24	1.798	2.666
JS 482	Sr I	7070.07	-0.03	1.847	3.204
KW208	Li I	6707.76	-0.002	0.0	2.756
KW23	Li I	6707.76	-0.002	0.0	1.928
KW208	Zn I	4680.13	-0.815	4.006	4.283
KW208	Zn I	4722.15	-0.338	4.03	4.494
KW208	Zn I	4810.52	-0.16	4.078	4.241
KW30	Zn I	4722.15	-0.338	4.03	4.541
KW23	Zn I	4722.15	-0.338	4.03	4.398
JS 552	Zn I	6362.33	0.14	5.796	4.941
JS 482	Zn I	4722.15	-0.338	4.03	3.808
KW208	Sc II	5031.02	-0.4	1.357	3.27
KW208	Sc I	5520.50	-0.309	1.865	3.253
KW208	Sc II	5526.79	0.024	1.768	3.333
KW208	Sc II	5641.00	-1.131	1.500	3.325
KW208	Sc II	5657.89	-0.603	1.507	3.573
KW208	Sc II	5667.14	-1.309	1.500	3.501
KW208	Sc I	6210.60	-2.738	0.000	3.044
KW208	Sc II	6604.60	-1.309	1.357	3.388
KW30	Sc II	5031.02	-0.4	1.357	3.419
KW30	Sc I	5520.50	-0.309	1.865	3.453
KW30	Sc II	5526.79	0.024	1.768	3.175
KW30	Sc II	5641.00	-1.131	1.500	3.431
KW30	Sc II	5657.89	-0.603	1.507	3.295
KW30	Sc II	5667.14	-1.309	1.500	3.459
KW30	Sc I	6210.60	-2.738	0.000	3.27
KW30	Sc II	6604.60	-1.309	1.357	3.232
KW23	Sc II	5031.02	-0.4	1.357	3.382
KW23	Sc I	5356.09	-0.084	1.865	3.257
KW23	Sc I	5520.50	-0.309	1.865	3.537
KW23	Sc II	5526.79	0.024	1.768	3.308
KW23	Sc II	5641.00	-1.131	1.500	3.485
KW23	Sc II	5657.89	-0.603	1.507	3.475
KW23	Sc II	5667.14	-1.309	1.500	3.5
KW23	Sc I	6210.60	-2.738	0.000	3.198
KW23	Sc II	6604.60	-1.309	1.357	3.261
JS 552	Sc II	5031.02	-0.4	1.357	2.745
JS 552	Sc I	5356.09	-0.084	1.865	2.923
JS 552	Sc I	5484.61	-0.242	1.851	3.339
JS 552	Sc I	5520.50	-0.309	1.865	3.203
JS 552	Sc II	5526.79	0.024	1.768	3.080
JS 552	Sc II	5641.00	-1.131	1.5	3.214
JS 552	Sc II	5657.89	-0.603	1.507	3.048
JS 552	Sc I	5686.82	-0.305	1.44	3.063
JS 552	Sc I	6210.60	-2.738	0.0	3.435
JS 552	Sc II	6604.60	-1.309	1.357	3.144
JS 482	Sc I	5356.09	-0.084	1.865	2.767
JS 482	Sc I	5484.61	-0.242	1.851	3.137
JS 482	Sc I	5520.50	-0.309	1.865	3.233
JS 482	Sc II	5526.79	0.024	1.768	2.910
JS 482	Sc II	5641.00	-1.131	1.5	3.437
JS 482	Sc II	5657.89	-0.603	1.507	3.545
JS 482	Sc II	5667.14	-1.309	1.5	3.43
JS 482	Sc I	6210.60	-2.738	0.0	3.400
JS 482	Sc II	6604.60	-1.309	1.357	3.462
KW208	V I	4875.50	-1.193	0.04	3.873
KW208	V I	5604.90	-1.644	1.043	3.805
KW208	V II	5627.60	-5.215	9.375	4.072
KW208	V I	5670.87	-1.272	1.081	3.845
KW208	V I	5737.10	-1.726	1.064	4.304
KW208	V I	6039.70	-1.217	1.064	3.917
KW208	V I	6081.44	-0.582	1.051	3.845
KW208	V I	6090.20	-0.754	1.081	3.946
KW208	V I	6111.60	-1.116	1.043	3.965
KW208	V I	6199.20	-2.988	0.287	3.870
KW208	V I	6216.40	-2.811	0.275	4.286
KW208	V I	6230.76	-1.977	0.267	4.290
KW208	V I	6251.80	-2.58	0.287	3.874
KW208	V I	6274.61	-2.932	0.267	3.682
KW208	V I	6292.80	-2.362	0.287	3.953
KW30	V I	4875.50	-1.193	0.04	3.951
KW30	V I	5604.90	-1.644	1.043	3.619
KW30	V II	5627.60	-5.215	9.375	4.022
KW30	V I	5668.38	-1.882	1.081	3.954
KW30	V I	5670.87	-1.272	1.081	4.065
KW30	V I	5703.59	-0.99	1.051	3.980
KW30	V I	5727.01	-0.644	1.081	3.878
KW30	V I	5727.61	-1.338	1.051	4.121
KW30	V I	5737.10	-1.726	1.064	4.260
KW30	V I	6039.70	-1.217	1.064	4.064
KW30	V I	6081.44	-0.582	1.051	4.032
KW30	V I	6090.20	-0.754	1.081	3.898
KW30	V I	6111.60	-1.116	1.043	3.949
KW30	V I	6119.50	-0.887	1.064	3.958
KW30	V I	6135.36	-0.751	1.051	3.919
KW30	V I	6199.20	-2.988	0.287	3.957
KW30	V I	6216.40	-2.811	0.275	4.206
KW30	V I	6243.10	-2.785	0.301	4.024
KW30	V I	6251.80	-2.58	0.287	4.009
KW30	V I	6274.61	-2.932	0.267	3.996
KW30	V I	6285.10	-3.568	0.275	4.039
KW30	V I	6285.18	-3.015	0.275	4.038
KW30	V I	6292.80	-2.362	0.287	3.952
KW30	V I	6531.39	-1.345	1.218	3.859
KW30	V I	8932.99	-2.959	1.195	4.173
KW23	V I	4875.50	-1.193	0.04	3.934
KW23	V I	5604.90	-1.644	1.043	4.252
KW23	V II	5627.60	-5.215	9.375	4.161
KW23	V I	5657.42	-1.587	1.064	4.255
KW23	V I	5668.38	-1.882	1.081	4.026
KW23	V I	5703.59	-0.99	1.051	4.109
KW23	V I	5727.01	-0.644	1.081	4.108
KW23	V I	5727.61	-1.338	1.051	4.082
KW23	V I	5737.10	-1.726	1.064	4.330
KW23	V I	6039.70	-1.217	1.064	4.109
KW23	V I	6081.44	-0.582	1.051	4.078
KW23	V I	6090.20	-0.754	1.081	4.031
KW23	V I	6111.60	-1.116	1.043	4.144
KW23	V I	6199.20	-2.988	0.287	4.016
KW23	V I	6216.40	-2.811	0.275	4.405
KW23	V I	6230.76	-1.977	0.267	4.475
KW23	V I	6243.10	-2.785	0.301	4.190
KW23	V I	6251.80	-2.58	0.287	4.096
KW23	V I	6256.89	-3.037	0.275	3.917
KW23	V I	6274.61	-2.932	0.267	4.179
KW23	V I	6285.10	-3.568	0.275	4.114
KW23	V I	6285.18	-3.015	0.275	4.116
KW23	V I	6292.80	-2.362	0.287	4.092
KW23	V I	6531.39	-1.345	1.218	4.23
KW23	V I	8932.99	-2.959	1.195	4.565
JS 552	V I	5604.90	-1.644	1.043	4.120
JS 552	V II	5627.60	-5.215	9.375	4.121
JS 552	V I	5632.50	-4.185	0.069	3.997
JS 552	V I	5646.10	-1.196	1.051	4.103
JS 552	V I	5657.42	-1.587	1.064	4.348
JS 552	V I	5668.38	-1.882	1.081	4.194
JS 552	V I	5670.87	-1.272	1.081	4.283
JS 552	V I	5703.59	-0.99	1.051	4.211
JS 552	V I	5727.01	-0.644	1.081	4.149
JS 552	V I	5727.61	-1.338	1.051	4.184
JS 552	V I	5737.10	-1.726	1.064	4.307
JS 552	V I	6002.30	-2.347	1.218	3.812
JS 552	V I	6039.70	-1.217	1.064	4.185
JS 552	V I	6081.44	-0.582	1.051	4.206
JS 552	V I	6090.20	-0.754	1.081	3.941
JS 552	V I	6111.60	-1.116	1.043	4.231
JS 552	V I	6119.50	-0.887	1.064	3.882
JS 552	V I	6135.36	-0.751	1.051	4.329
JS 552	V I	6199.20	-2.988	0.287	4.024
JS 552	V I	6216.40	-2.811	0.275	4.465
JS 552	V I	6243.10	-2.785	0.301	4.203
JS 552	V I	6251.80	-2.58	0.287	4.078
JS 552	V I	6256.89	-3.037	0.275	4.118
JS 552	V I	6274.61	-2.932	0.267	4.212
JS 552	V I	6285.10	-3.568	0.275	4.609
JS 552	V I	6285.18	-3.015	0.275	4.609
JS 552	V I	6292.80	-2.362	0.287	4.531
JS 552	V I	6531.39	-1.345	1.218	4.317
JS 552	V I	6565.87	-2.07	1.183	4.016
JS 552	V I	8932.99	-2.959	1.195	4.008
JS 482	V I	5604.90	-1.644	1.043	3.959
JS 482	V II	5627.60	-5.215	9.375	4.084
JS 482	V I	5632.50	-4.185	0.069	4.078
JS 482	V I	5646.10	-1.196	1.051	4.233
JS 482	V I	5657.42	-1.587	1.064	4.446
JS 482	V I	5668.38	-1.882	1.081	3.988
JS 482	V I	5670.87	-1.272	1.081	4.230
JS 482	V I	5703.59	-0.99	1.051	4.283
JS 482	V I	5727.01	-0.644	1.081	3.966
JS 482	V I	5727.61	-1.338	1.051	4.247
JS 482	V I	5737.10	-1.726	1.064	4.312
JS 482	V I	6002.30	-2.347	1.218	4.218
JS 482	V I	6039.70	-1.217	1.064	4.127
JS 482	V I	6081.44	-0.582	1.051	4.261
JS 482	V I	6090.20	-0.754	1.081	3.935
JS 482	V I	6111.60	-1.116	1.043	4.277
JS 482	V I	6119.50	-0.887	1.064	4.078
JS 482	V I	6135.36	-0.751	1.051	4.285
JS 482	V I	6199.20	-2.988	0.287	4.233
JS 482	V I	6251.80	-2.58	0.287	3.915
JS 482	V I	6256.89	-3.037	0.275	4.083
JS 482	V I	6274.61	-2.932	0.267	4.324
JS 482	V I	6285.10	-3.568	0.275	4.236
JS 482	V I	6285.18	-3.015	0.275	4.236
JS 482	V I	6292.80	-2.362	0.287	4.437
JS 482	V I	6531.39	-1.345	1.218	4.335
JS 482	V I	8932.99	-2.959	1.195	3.930
KW208	Mn I	4783.40	-1.375	2.298	5.668
KW208	Mn I	4823.50	-0.364	2.319	5.531
KW208	Mn I	5117.90	-2.831	3.134	5.609
KW208	Mn I	5407.39	-2.708	2.143	5.436
KW208	Mn I	5420.39	-2.947	2.143	5.400
KW208	Mn I	5432.50	-4.31	0.0	5.362
KW208	Mn I	5516.80	-2.878	2.178	5.528
KW208	Mn I	6013.49	-1.081	3.072	5.555
KW208	Mn I	6021.80	-1.404	3.075	5.465
KW30	Mn I	5117.90	-2.831	3.134	5.762
KW30	Mn I	5407.39	-2.708	2.143	5.421
KW30	Mn I	5420.39	-2.947	2.143	5.486
KW30	Mn I	5432.50	-4.31	0.0	5.433
KW30	Mn I	5516.80	-2.878	2.178	5.483
KW30	Mn I	6013.49	-1.081	3.072	5.583
KW30	Mn I	6021.80	-1.404	3.075	5.436
KW23	Mn I	5117.90	-2.831	3.134	5.438
KW23	Mn I	5394.70	-4.339	0.0	5.363
KW23	Mn I	5407.39	-2.708	2.143	5.556
KW23	Mn I	5420.39	-2.947	2.143	5.549
KW23	Mn I	5432.50	-4.31	0.0	5.509
KW23	Mn I	5516.80	-2.878	2.178	5.487
KW23	Mn I	6013.49	-1.081	3.072	5.546
KW23	Mn I	6021.80	-1.404	3.075	5.614
JS 552	Mn I	5117.90	-2.831	3.134	5.192
JS 552	Mn I	5407.39	-2.708	2.143	5.221
JS 552	Mn I	5516.80	-2.878	2.178	5.555
JS 552	Mn I	6013.49	-1.081	3.072	5.479
JS 552	Mn I	6021.80	-1.404	3.075	5.774
JS 482	Mn I	5117.90	-2.831	3.134	5.000
JS 482	Mn I	5516.80	-2.878	2.178	5.523
JS 482	Mn I	6013.49	-1.081	3.072	5.602
KW208	Cr II	4588.19	-0.627	4.071	6.032
KW208	Cr I	4646.16	-0.74	1.03	5.879
KW208	Cr II	4789.32	-4.464	8.634	5.414
KW208	Cr II	4848.23	-1.18	3.864	5.568
KW208	Cr I	4936.33	-0.25	3.113	5.806
KW208	Cr I	4964.92	-2.526	0.941	5.472
KW208	Cr I	5200.17	-0.58	3.385	5.185
KW208	Cr II	5239.01	-6.462	6.641	5.633
KW208	Cr I	5247.56	-1.59	0.961	5.619
KW208	Cr I	5287.17	-0.87	3.438	5.592
KW208	Cr I	5296.69	-1.36	0.983	5.782
KW208	Cr I	5300.74	-2.0	0.983	5.469
KW208	Cr I	5304.18	-0.67	3.464	5.908
KW208	Cr I	5312.85	-0.55	3.449	5.747
KW208	Cr I	5318.77	-0.67	3.438	5.74
KW208	Cr I	5345.79	-0.95	1.004	5.533
KW208	Cr I	5348.31	-1.21	1.004	5.877
KW208	Cr II	5409.79	-6.443	12.176	5.996
KW208	Cr I	5844.59	-1.77	3.013	5.75
KW30	Cr II	4588.19	-0.627	4.071	5.524
KW30	Cr I	4646.16	-0.74	1.03	5.74
KW30	Cr II	4848.23	-1.18	3.864	5.409
KW30	Cr I	4936.33	-0.25	3.113	5.708
KW30	Cr I	4953.71	-1.48	3.122	5.746
KW30	Cr I	4964.92	-2.526	0.941	5.673
KW30	Cr II	5239.01	-6.462	6.641	5.793
KW30	Cr I	5241.45	-1.92	2.71	5.594
KW30	Cr I	5247.56	-1.59	0.961	5.674
KW30	Cr I	5272.00	-0.42	3.449	5.372
KW30	Cr I	5287.17	-0.87	3.438	5.646
KW30	Cr I	5296.69	-1.36	0.983	5.733
KW30	Cr I	5300.74	-2.0	0.983	5.462
KW30	Cr I	5304.18	-0.67	3.464	5.723
KW30	Cr I	5312.85	-0.55	3.449	5.526
KW30	Cr I	5318.77	-0.67	3.438	5.582
KW30	Cr I	5345.79	-0.95	1.004	5.614
KW30	Cr I	5348.31	-1.21	1.004	5.784
KW30	Cr II	5409.79	-6.443	12.176	5.875
KW30	Cr I	5719.81	-1.58	3.013	5.706
KW30	Cr II	5788.41	-9.975	8.718	5.721
KW23	Cr II	4588.19	-0.627	4.071	5.603
KW23	Cr I	4646.16	-0.74	1.03	5.982
KW23	Cr II	4848.23	-1.18	3.864	5.581
KW23	Cr I	4936.33	-0.25	3.113	5.834
KW23	Cr I	4953.71	-1.48	3.122	5.822
KW23	Cr I	4964.92	-2.526	0.941	5.657
KW23	Cr II	5239.01	-6.462	6.641	5.757
KW23	Cr I	5241.45	-1.92	2.71	5.579
KW23	Cr I	5247.56	-1.59	0.961	5.847

Equations

$$d_j^{(O)}={\Sigma }_{k=1}^{12}({\rho }_k-p_{jk}{)}^2,$$

$${\sigma }_{tot}=\sqrt{{\sigma }_{[X/H],T_{\mathrm{eff}}}^2+{\sigma }_{[X/H],\log g}^2+{\sigma }_{[X/H],{\xi }_t}^2+{\sigma }_{\mathrm{mean}}^2}$$

Full text

open clusters and associations: individual (M44), techniques: spectroscopic, stars: abundances

††journal: ApJ††software: IRAF (Tody, 1986), PHOENIX (Husser et al., 2013; Baron & Hauschildt, 2007; Hauschildt & Baron, 2006; Hauschildt, 1993), SYNSPEC48 code (Hubeny & Lanz, 1992), ATLAS9 code (Kurucz, 1992), BACCHUS (Masseron et al., 2016), MARCS (Gustafsson et al., 2008), TURBOSPECTRUM (Alvarez & Plez, 1998; Plez, 2012)

1 Introduction

The recent advent of large-scale stellar spectroscopic surveys dedicated to the systematic determinations of abundances of many elements was in part inspired by the concept of chemical tagging, a process by which distinct stellar populations in the Galaxy might be identified based on elemental abundances (Freeman & Bland-Hawthorn, 2002; De Silva et al., 2006; Bland-Hawthorn et al., 2010). This idea originates in the notion that stars born together should share a chemical fingerprint that is sufficiently unique to distinguish these stars, even if no longer obviously associated, from the Galactic background.

There are a number of reasons to think that chemical tagging should work. Studies of solar-type wide binary systems and of open clusters, which are thought to be co-eval and co-chemical populations, have shown that their component stars have very similar abundances (e.g., Andrews, Chanamé, & Agüeros, 2018; Bovy, 2016), with differences in individual elements likely due to measurement uncertainties. Moreover, tests designed to identify stellar populations based on their chemical similarities have shown that they can recover stars that are associated in phase space or that appear to have a common origin (e.g., Hogg et al., 2016; Schiavon et al., 2017).

Equally, however, there are reasons to be skeptical that chemical tagging can work. Open clusters, for example, may have chemical-abundance patterns that are difficult to distinguish from each others’ (Blanco-Cuaresma et al., 2015), or indeed that are insufficiently distinct from those of unassociated field stars (so-called doppelgängers; Ness et al., 2018). Dynamical processes such as planet formation may also alter the photospheric compositions of stars during their main-sequence lifetimes, potentially resulting in chemical inhomogeneities within what was once a chemically homogeneous group (e.g., Spina et al., 2018). Such signatures are generally detectable only with very high precision, typically $\leq$0.02 dex (e.g., Liu et al., 2016; Teske et al., 2016), however, and may not be important for large-scale surveys.

Another potential concern for chemical tagging as applied to main-sequence stars is the derived abundance anomalies for some elements in open cluster late-G and K dwarfs. The abundances of iron derived from singly-ionized lines and oxygen derived from the near-infrared triplet, in particular, demonstrate a striking increase with decreasing temperature for stars with $T_{\mathrm{eff}}\lesssim 5300\,\mathrm{K}$ in the Hyades, Pleiades, and M34 (e.g., Schuler et al., 2003, 2004; Yong et al., 2004) and in the field (e.g., Ramírez et al., 2007). The source of the discrepant abundances has yet to be fully identified, but line-blending in the spectra of cooler stars has been suggested to account for some but not all of their observed overabundances (Aleo et al., 2017). Studies have also investigated the influence of metallicity and chromospheric activity on the abundances, with no statistically significant correlations being found (e.g., Schuler et al., 2006; Aleo et al., 2017). Schuler et al. (2006) reported a possible age-related diminution of the cool-star abundances. These authors also demonstrated that photospheric temperature inhomogeneities (i.e., starspots) in cool stars are a plausible source of the overabundances. Such uncertainty in the abundances derived for late-G and K dwarfs may be an indication of deficiencies in current cool-star model atmospheres.

To further explore these ideas and challenges, we obtained $R\approx$ 31,000 spectra (described in Section 2) of five main-sequence members of the Praesepe open cluster. In this paper, we describe our application of some of the techniques generally applied to higher-mass/evolved stars to derive fundamental properties of, and abundances for, these three G and two K dwarfs (Sections 3 and 4). We then use our results to derive a cluster metallicity and to examine the homogeneity of abundances for a range of elements in $\leq$1 M*⊙* stars in Praesepe (Section 5). We conclude that chemical tagging remains plausible, but challenging, for main-sequence stars given our data and the techniques currently available.

2 Observations and data reduction

Praesepe, the Beehive Cluster (M44; NGC2632), is a nearby ($\approx$180 pc; van Leeuwen, 2009), rich ($\approx$1200 stars; Kraus & Hillenbrand, 2007), and intermediate-age ($\approx$600 Myr; Delorme et al., 2011) open cluster. Praesepe’s proximity makes it an ideal target for observers interested in the properties of a single-aged stellar population, including multiplicity (e.g., Hillenbrand et al., 2018) and angular-momentum evolution (e.g., Douglas et al., 2017), and in circumstellar processes such as planet formation (e.g., Mann et al., 2017; Rizzuto et al., 2018).

Our spectroscopic observations of five high-confidence Praesepe members222All five have membership probabilities $>$99% in the Kraus & Hillenbrand (2007) cluster catalog. were obtained with the ARC Echelle Spectrograph (ARCES), an $R\approx$ 31,000 cross-dispersed spectrograph, mounted on the ARC 3.5-m telescope at the Apache Point Observatory, NM (see Table 1).

We began by observing two K dwarfs, JS 482 (EPIC 211928486) and JS 552 (EPIC 211966629), on the nights of 2017 November 28 and December 29, respectively. Exposures of 7200 and 8400 s achieved signal-to-noise ratios (SNRs) of $\approx$50-60. The three G dwarfs, KW23, KW30, and KW208, were observed on the night of 2018 March 30. Each of these exposures was 1800 s and the corresponding SNRs $\approx$ 80-100.

We reduced our spectra using standard IRAF333IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.(Tody, 1986) procedures that subtract biases, remove cosmic rays, normalize by the flat field, and do the wavelength calibration with exposures of a Th-Ar lamp.444An ARCES data reduction manual is available here: http://astronomy.nmsu.edu:8000/apo-wiki/attachment/wiki/ARCES/Thorburn_ARCES_manual.pdf To measure the blaze function, we fit the spectrum of an early type star with a high-order polynomial and divided the spectrum of each target by the polynomial fit to normalize each spectral order. To shift the normalized spectra into the rest-frame by removing the stellar radial velocities, we maximized the cross-correlation of the ARCES spectra with PHOENIX (Husser et al., 2013; Baron & Hauschildt, 2007; Hauschildt & Baron, 2006; Hauschildt, 1993) model spectra. All these reduction steps are implemented in the automated software of Morris & Dorn-Wallenstein (2018).

3 Determining the Fundamental Stellar parameters

Abundance analyses are very sensitive to the inputed fundamental stellar parameters, especially the effective temperature ($T_{\mathrm{eff}}$), the surface gravity ($\log g$), and the microturbulent velocity ($\xi_{t}$). These should therefore be derived as accurately as possible. For that reason, we employed three different techniques to obtain the fundamental parameters of our target stars: a Principal Component Analysis (PCA), iron-excitation-ionization balance, and photometry. These approaches and their results are described below.

3.1 Using Principal Component Analysis

We started by applying the PCA technique of Gebran et al. (2016) to our five stars. PCA is a technique that has been rarely used in stellar spectroscopy, but Gebran et al. (2016) showed that it could be used to derive accurate parameters for A stars using synthetic learning databases. Paletou et al. (2015) used PCA to successfully derive the fundamental parameters of a sample of FGK stars using a learning database composed of observed spectra with well-known and reliable parameters.

We derived the parameters of our observed G and K dwarfs using purely synthetic data. First, a learning database of synthetic spectra was calculated using the SYNSPEC48 code (Hubeny & Lanz, 1992) in the 5000$-$6000 Å wavelength range. This region, which is free of molecular bands, was chosen because of the presence of the prominent Mg i triplet and the Na i doublet, which are both sensitive to $T_{\mathrm{eff}}$ and $\log g$. In addition, the presence of a large number of weak metallic lines in this region provide a good indication of $v\sin i$ and of the metallicity ([M/H]).555[M/H] is an indicator of the overall elemental abundance and not just that of iron ([Fe/H]).

The ranges for the various stellar parameters of the spectra in the learning database are displayed in Table 2. We fixed the microturbulent velocity $\xi_{t}=1.0$ $\mbox{km}\,\mbox{s}^{-1}$, as that is the average value for GK dwarfs (Smiljanic et al., 2014) and the selected wavelength region is weakly affected by the variation of $\xi_{t}$.

We adopted the Kurucz gfhyperall.dat666http://kurucz.harvard.edu line lists, which we modified with more recent and accurate atomic data retrieved from the VALD777http://www.astro.uu.se/~vald/php/vald.php and the NIST888http://physics.nist.gov databases (for more details, see Gebran et al. 2016). The structure of the atmosphere of these synthetic models were calculated using ATLAS9 code (Kurucz, 1992). We used the new opacity distribution function of Castelli & Kurucz (2003), calculated for $\xi_{t}=1.0$ $\mbox{km}\,\mbox{s}^{-1}$. These models assume local thermodynamic equilibrium, hydrostatic equilibrium, radiative equilibrium, and a 1D plane-parallel atmosphere. Convection was treated using a mixing length parameter of 1.25 (Smalley, 2004).

Figure 1 displays the observed spectra (in black) of our G and K dwarfs as well as the best-fit synthetic spectra (in red). The best fit is calculated using the stellar parameters derived from the first neighbor that minimizes the function:

[TABLE]

where $\rho_{k}$ and $p_{jk}$ are the coefficients of the projection of the flux of the observation and the $j^{th}$ synthetic spectrum, respectively, on the $k^{th}$ eigenvector of the synthetic spectra covariance matrix. Based on an error reconstruction verification, as done in Gebran et al. (2016), the maximum number of eigenvector was fixed to be 12. The derived $T_{\mathrm{eff}}$, $\log g$, [M/H] and $v\sin i$ for our five Praesepe targets are given in Table 3. The associated errors are upper limits on the derived parameters of the $\approx$250 FGK stars to which Paletou et al. (2015) applied the same PCA.

3.2 Using Iron-Excitation-Ionization Balance

We also employed the Brussels Automatic Code for Characterizing High accUracy Spectra BACCHUS (Masseron et al., 2016) to derive the fundamental parameters of our target stars. BACCHUS uses the MARCS (Gustafsson et al., 2008) model atmosphere grid, and the radiative transfer code TURBOSPECTRUM (Alvarez & Plez, 1998; Plez, 2012). Atomic lines are taken from the most recent (fifth) version of the Gaia-ESO linelist (Heiter et al., in preparation). Molecular species are also included for CH (Masseron et al., 2014), and CN, NH, OH, MgH and C2; the lines of SiH molecules are adopted from the Kurucz linelists and those for TiO, ZrO, FeH, CaH from B. Plez (private communication).

The stellar parameters are derived using the standard iron-ionization-excitation balance. More specifically, $T_{\mathrm{eff}}$ is derived ensuring that there is no correlation between iron abundance and the excitation potential of the lines. The logarithm of the surface gravity is determined through ionization balance, which amounts to ensuring that there is no significant correlation between Fe i and Fe ii abundances. Finally, $\xi_{t}$ is determined by requiring that there is no trend between reduced equivalent width (REW = EW/$\lambda$) and the iron abundances in each line. For more details about BACCHUS and its procedure for stellar parameter derivation, we refer the reader to section 2.2 of Hawkins et al. (2015).

We used up to 120 iron lines: up to 90 Fe i lines and up to 30 Fe ii lines. To validate the line selection, we derived the parameters of a twilight solar spectrum also taken with ARCES at APO. The solar parameters were found to be 5740 K, 4.40 dex, 0.0 dex and 0.8 km/s for $T_{\mathrm{eff}}$, $\log g$, [Fe/H], and $\xi_{t}$, respectively.

An illustration of this iron-ionization-excitation balance procedure for one star, KW208, is shown in Figure 2. In the top panel, we display the logarithm of the abundance of the Fe i (black circles) and Fe ii lines (open red circles) as a function of the excitation potential. For KW208, the derived slope in this case is $-$0.004$\pm$0.008. The bottom panel of the same figure displays the logarithm of the abundance as a function of the REW for Fe i and Fe ii lines. In this case the slope is 0.161$\pm$1.732.

3.3 Using Photometry

In its second data release, Gaia (Gaia Collaboration et al., 2016, 2018) provided data for more than 1.3$\times$109 objects, including temperatures based on $G$, $BP$, and $RP$ photometry (Evans et al., 2018). We retrieved the photometric temperatures of our five stars from the Gaia archive, and they are listed in column 10 of Table 3.

We also checked the photometric calibration of Cummings et al. (2017) for the three G stars. Cummings et al. (2017) applied a 10-color combination of the UBVRI filters to derive $T_{\mathrm{eff}}$ of G stars. Their derived temperatures are 5628 K, 5687 K, and 5979 K for KW23, KW30, and KW208, respectively.

Reassuringly, the parameters we derive from these different techniques agree within the error bars. For internal consistency, we adopted the iron-excitation-ionization balance parameters for our stars, as they are based on the same technique that we used for the abundance determinations described below.

4 Abundance determination

4.1 Approach and Results

Using the “abund” module in BACCHUS, we derived the elemental abundances of up to 24 elements across the light (Li, C, O), $\alpha$ (Mg, Si, Ca, Ti), odd-Z (Na, Al, Sc, V, Ni, Cu, Zn), Fe-peak (Cr, Mn, Fe, Co), and neutron capture (Sr, Y, Zr, Ba, La, Nd) species. Briefly, this module computes the abundances by first fixing the model atmosphere to the one that has a $T_{\mathrm{eff}}$, $\log g$, [Fe/H], and $\xi_{t}$ matching those derived through iron-excitation-ionization balance. It then synthesizes spectra, using TURBOSPECTRUM and accompanying atomic and molecular line lists, with different [X/Fe] abundance ratios for each element independently by up to $\pm$1 dex.

The abundances for an individual line of a given element are then determined through several methods, including a $\chi^{2}$ minimization between the observed spectrum and the synthesized spectra and using the EW of the absorption features. All abundances are derived using atomic lines except for carbon, which is a combination of atomic and molecular999Carbone molecules include CH, C2, and CN. features.

To achieve the best possible internal precision, we did a line-by-line differential analysis with respect to the Sun (e.g., Meléndez et al., 2009; Ramírez et al., 2009; Hawkins et al., 2016). In this procedure, the abundance for each element and each absorption feature was determined from BACCHUS and then compared directly to the same element and feature in our ARCES twilight solar spectrum. This helps to reduce the systematics in the abundance determinations due to incorrect $\log(gf)$ values in the line list, for example.

The results of this line-by-line differential abundance analysis for the G and K dwarfs are shown in top and bottom panels of Figure 3, respectively. For each element, the median of the abundance of all lines is displayed. For comparison, also shown in the top panel of Figure 3 are the abundances for 15 of these elements determined by Boesgaard et al. (2013) for these three G stars using slightly higher resolution and significantly higher SNR spectra obtained with HIRES on the Keck telescope on Mauna Kea, HI.

We also tabulated the elemental abundances for each star by taking the median of the abundance for each element over all of the lines where it could be determined. These abundances are reported in Table 4, as well as the mean abundances for the three G and two K stars and the differences between these mean abundances.

4.2 Evaluating the Abundance Uncertainties

To evaluate the uncertainties in our abundances, we first studied the impact of errors in the stellar parameters. For each star and element, we recomputed the abundance while varying $T_{\mathrm{eff}}$ by $\pm$100 K, $\log g$ by $\pm$0.30 dex, and $\xi_{t}$ by $\pm$0.05 $\mbox{km}\,\mbox{s}^{-1}$. These values were chosen because they represent the typical uncertainty in the stellar parameters for our sample.

In Table 7, we indicate the sensitivity of our abundance determinations to the uncertainty in each of the stellar atmospheric parameters. We tabulate the difference in the [X/H] abundance ratio that is caused by a change in the stellar parameters.

The reported uncertainty for each chemical species is:

[TABLE]

where $\sigma_{\mathrm{mean}}$ is calculated using the classical standard deviation derived from the different abundances of the different lines for each element. $\sigma_{T_{\mathrm{eff}}}$, $\sigma_{\log g}$ and $\sigma_{\xi_{t}}$ are derived for each element and each star using the sensitivity values of Table 7 scaled to the BACCHUS errors of each fundamental parameter listed in Table 3. In addition, we report the abundances derived for each absorption feature of every element, along with the $\log(gf)$ of the absorption feature, for each star, in Table 8.

5 Discussion and Conclusion

We have used $R\approx$ 31,000, moderate SNR spectra of five main-sequence G and K stars in Praesepe to test the efficacy of using automated routines to derive the abundances of cooler main-sequence stars and to examine chemical homogeneity in this benchmark open cluster.

We used two automated, independent approaches to determine the stellar parameters for our five targets: a PCA, which is a statistical spectral fitting method, and the BACCHUS spectral analysis code, which uses iron-excitation-ionization balance. These two approaches produced consistent values for $T_{\mathrm{eff}}$ and $\log g$, which are crucial for robust chemical analysis, despite the relatively low SNR for the K star spectra in particular. For internal consistency, we adopted the BACCHUS-derived parameters for our abundance determinations, also made using BACCHUS.

In Table 5, we summarize the findings of a number of spectroscopic studies that derived a metallicity for Praesepe. The Boesgaard et al. (2013) study, which included the three G dwarfs we observed, found that [Fe/H] = 0.12$\pm$0.04 for the cluster. This was based on a sample of 11 solar-type cluster members for which these authors obtained $R\approx$ 45,000, SNR $\approx$ 150 spectra.

Our average derived iron abundance for our three G dwarf targets is 0.17$\pm$0.07 dex. For the two K dwarfs we observed, the average [Fe/H] = 0.12$\pm$0.01. Rather remarkably, averaging the iron abundances we derive for each of our targets gives us [Fe/H] = 0.15$\pm$0.08 for the cluster, consistent with what has been reported in the literature. This is despite our targets having $T_{\mathrm{eff}}$ that differ by up to $\approx$1400 K, a wider temperature range than is typical for the stars used in these studies, and despite our spectra having modest SNR compared to those generally obtained by other groups.

To investigate the efficacy of using automated routines to derive the abundances of cooler main-sequence stars, we compared the abundances we derived for the two K stars to those of the G stars. Our abundances agree within $\leq$0.1 dex or less for 13 of the 18 elements that we report for all five stars, providing more evidence that G and K stars in a given open cluster are chemically homogeneous given typical measurement uncertainties. The median difference between the mean G and K stars abundances is 0.08$\pm$0.05 dex, despite serious challenges with the noisier data for the fainter K stars. The quality of the data (and therefore of the BACCHUS measurements) prevents us from reporting abundances for oxygen, zinc, and strontium.

As a further test of the robustness of our abundance determination, we compared them to those reported by Boesgaard et al. (2013) for the 15 elements these authors report, considering first only our G dwarf targets and then the mean abundances for our five stars. As illustrated by the top panel in Figure 3, the agreement between our values for the G stars and those of Boesgaard et al. (2013) is generally excellent, with differences of order $\pm$0.05 dex.

In Table 6, we list the overall mean abundances for our sample and those of Boesgaard et al. (2013). While the uncertainties on our mean values are comparatively large, the overall agreement between these values is very good: the average difference is only about $\pm$0.06 dex. In general, the error bars on many of our K star abundances are larger than one would like (reflecting the poor SNR in our data for JS 482 in particular), highlighting the challenges involved in pushing precision abundance determination, whether automated or not, into the cool dwarf regime.

Still, the overall agreement in the abundances across our sample is encouraging for chemical tagging experiments based on large-scale spectroscopic surveys, which tend to use 4-m class telescopes (e.g., the Galactic Archaeology with HERMES (GALAH) project; Martell et al., 2017). It suggests that it may be possible to use automated abundance determination techniques to identify chemically related main-sequence stars across larger temperature ranges than are usually considered in these experiments. Larger samples of higher SNR spectra for cooler stars in benchmark clusters are needed before firmer conclusions can be drawn.

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We thank Thomas Masseron for his help. M.A.A. acknowledges support provided by the NSF through grant AST-1255419. M.G. acknowledges the support of the Fulbright Visiting Scholar Program and the Institute of International Education. M.G. thanks the Department of Astronomy at Columbia University for its hospitality. KH is partially supported by a Research Corporation for Science Advancement TDA grant. This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This work made use of the following software packages: astropy (Astropy Collaboration et al., 2018), astroplan (Morris et al., 2018) and aesop (Morris & Dorn-Wallenstein, 2018).