Table 1: Summary of the model atom used in our calculations. $N_{\hbox {\sc f}}$ is the number of full levels, $N_{\hbox {\sc s}}$ the number of super levels and $N_{\hbox {\sc t}}$ the corresponding number of transitions.
I II III IV

Ion
$N_{\hbox {\sc f}}$ $N_{\hbox {\sc s}}$ $N_{\hbox {\sc t}}$ $N_{\hbox {\sc f}}$ $N_{\hbox {\sc s}}$ $N_{\hbox {\sc t}}$ $N_{\hbox {\sc f}}$ $N_{\hbox {\sc s}}$ $N_{\hbox {\sc t}}$ $N_{\hbox {\sc f}}$ $N_{\hbox {\sc s}}$ $N_{\hbox {\sc t}}$

H 30 20

He 51 40 255 5 5 10

C 59 32 334 20 12 49 14 9 46

N 104 44 760 41 23 144 8 8 11

O 75 23 535 111 30 1093 46 26 184

Ne 242 42 5397

Na 71 22 788 35 21 181

Mg 65 22 1229

Al 44 26 156 45 17 337

Si 59 31 318 51 27 235

S 324 56 7830 98 48 832

Ca 77 21 1464

Ti 152 37 3068 206 33 4584

Cr 196 28 3580 145 30 2359

Mn 97 25 210 175 30 3173

Fe 827 265 43077 477 61 6411 282 50 7872

Co 144 34 2047 283 41 6910

Ni 93 19 817 67 15 379

**Table 1:** Summary of the model atom used in our calculations. $N_{\hbox {\sc f}}$ is the number of full levels, $N_{\hbox {\sc s}}$ the number of super levels and $N_{\hbox {\sc t}}$ the corresponding number of transitions.
	I	II	III	IV
Ion	$N_{\hbox {\sc f}}$	$N_{\hbox {\sc s}}$	$N_{\hbox {\sc t}}$	$N_{\hbox {\sc f}}$	$N_{\hbox {\sc s}}$	$N_{\hbox {\sc t}}$	$N_{\hbox {\sc f}}$	$N_{\hbox {\sc s}}$	$N_{\hbox {\sc t}}$	$N_{\hbox {\sc f}}$	$N_{\hbox {\sc s}}$	$N_{\hbox {\sc t}}$
H	30	20
He	51	40	255	5	5	10
C				59	32	334	20	12	49	14	9	46
N	104	44	760	41	23	144	8	8	11
O	75	23	535	111	30	1093	46	26	184
Ne				242	42	5397
Na	71	22	788	35	21	181
Mg				65	22	1229
Al				44	26	156	45	17	337
Si				59	31	318	51	27	235
S				324	56	7830	98	48	832
Ca				77	21	1464
Ti				152	37	3068	206	33	4584
Cr				196	28	3580	145	30	2359
Mn				97	25	210	175	30	3173
Fe				827	265	43077	477	61	6411	282	50	7872
Co				144	34	2047	283	41	6910
Ni				93	19	817	67	15	379

Source LaTeX | All tables | In the text

	1 Introduction
	2 Presentation of the code
	3 Spectroscopic modeling
	4 Discussion on model results and properties
	5 Line formation in expanding outflows of hot stars and type II SN
	6 Conclusion
	References