III. MATERIAL USED IN CHAPTER VIII

THE line intensities quoted in [Chapter VIII] were derived from the spectra of the stars enumerated below in [Table XXXII]. Successive columns contain the Draper class, the name of the star, the Boss number, the visual apparent magnitude, and the reduced proper motion H. The stars within each class are arranged in order of right ascension.

[TABLE XXXII]

	Boss	m	H		Boss	m	H
Cen	3054	3.3	1.7	Vel	2723	4.1	5.1
Phe	148	4.5	-0.5	Sgr	4832	2.7	0.0
For	474	4.7	0.1	Gru	5880	3.7	4.1
Eri	6ll	4.5	4.3	Eri	696	4.2	5.1
Dor	1081	3.5	2.1	Pic	1446	3.9	3.7
Vel	2356	2.0	1.9	Mus	3092	3.8	3.9
Car	2493	1.8	3.2	Pav	5315	3.6	2.1
Cen	3302	2.4	3.9	PsA	5916	1.3	4.1
TrA	3879	3.1	2.2	Hyi	458	3.0	5.0
Sgr	4645	2.0	2.7	Car	1622	0.9	-4.6
Car	2503	2.2	-0.7	Crv	3172	3.2	2.3
Boo	3722	3.0	4.3	Hyi	3622	5.5	4.6
Cir	3739	3.4	5.0	Cen	3623	2.3	6.7
TrA	4030	3.0	6.2	Lup	3864	3.5	4.0
Sco	4457	2.0	-2.6	Lib	3962	5.3	-1.2
Sco	4361	3.4	5.7	Apo	4168	3.9	4.6
Sgr	4874	3.0	1.0	Sco	4272	2.4	6.5
Vol	1917	4.0	0.6	Sgr	4568	3.1	4.6
CMi	2008	0.5	6.1	Sgr	4628	2.8	1.3
Pup	2153	2.9	2.9	Sgr	4665	2.9	4.4
Vel	2324	4.1	0.0	Sgr	4809	3.6	1.4
Oph	4421	4.4	5.4	Sgr	4857	3.4	5.5
Sco	4492	3.1	-3.9	Ind	5281	3.2	2.5
Pav	4778	var.	0.0	Aqr	5963	3.8	0.5
Tuc	55	4.3	10.9	Gru	5965	4.1	4.9
For	723	4.0	8.3	Cru	3218	3.6	5.1
Lep	1420	3.8	9.7,7.1	Mus	3377	3.6	5.7
CMa	1839	2.0	-4.5	TrA	4250	1.9	-0.6
Hyi	74	2.9	9.7	Ara	4406	2.8	0.6
Aur	1246	0.2	3.4	Tuc	5747	2.9	2.6
Lep	1323	3.0	2.9	Tau	1077	1.1	2.6
Pup	2065	3.5	-2.3	Pup	1896	2.7	-2.8
Leo	2618	3.1	1.5	Pup	1972	3.3	4.7
Car	2628	var.	1.1	Car	2739	3.4	1.7
Cap	5507	3.9	(1.1)	Apo	3746	3.8	1.4
Ret	994	3.4	2.6	Ara	4265	3.7	2.5
Vel	2875	2.8	2.3	Sco	4292	3.8	5.9
Hya	3042	3.7	5.3	Ara	4304	3.1	1.5
Crv	3280	2.8	1.7	And	259	2.4	-0.8
Hya	3449	3.3	2.9	Hyi	899	3.2	-1.3
CrA	4871	4.2	2.0	Ori	1468	0.9	-0.0
Pav	5138	3.6	9.7	Sco	4193	1.2	-2.5
Phe	78	2.4	5.6	Eri	759	4.0	3.2
Cas	135	2.5	1.4	Cru	3263	1.6	3.8
Phe	245	3.4	1.6	Lib	3837	3.4	3.3
Phe	336	4.0	5.4	Her	4373	3.5	0.9
Ret	875	3.8	6.2	Sgr	4617	3.2	4.9
Lep	1456	39	8.1	Gru	5854	2.2	2.8
Col	1459	3.2	6.2

IV. INTENSITY CHANGES OF LINES WITH UNKNOWN SERIES RELATIONS

THE following tabulation shows the intensity changes of lines of unknown series relations that occur in the hotter stars. The arrangement follows that of [Table XIX]. Notes on the maxima and blends are appended.

[TABLE XXXIII]

Atom	Line	Pup													Note
C++	4649	0.0	2.0	9.0	6.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	..	1
N+	3996.9	0.0	0.0	0.0	0.0	5.0	6.0	7.0	..	9.0	..	..	5.0	0.0	1
N++	4515.0	..	9.0	4.0	4.0	1.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	2
	4097.5	..	15.0	8.0	5.0	..	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	3
O+	4943.4	0.0	0.0	0.0	0.0	4.0	4.0	3.0	0.0	0.0	0.0	0.0	0.0	0.0	1
	4941.2
	4705.3	0.0	0.0	0.0	2.0	4.0	4.0	3.0	0.0	0.0	0.0	0.0	0.0	0.0	2
	4699.2
	4676.2	0.0	0.0	0.0	2.0	5.0	..	7.0	0.0	0.0	0.0	0.0	0.0	0.0	3
	4661.6	0.0	0.0	0.0	2.0	5.0	..	7.0	0.0	0.0	0.0	0.0	0.0	0.0	4
	4649.1	0.0	0.0	0.0	6.0	9.0	12.0	9.0	..	4.0	0.0	0.0	0.0	0.0	5
	4641.8	0.0	0.0	0.0	0.0	3.0	10.0	7.0	..	0.0	0.0	0.0	0.0	0.0	6
	4596.2	0.0	0.0	0.0	1.0	5.0	..	6.0	..	3.0	0.0	0.0	0.0	0.0	7
	4591.0	0.0	0.0	0.0	1.0	5.0	..	6.0	..	3.0	0.0	0.0	0.0	0.0	8
	4417.0	0.0	0.0	0.0	5.0	6.0	11.0	3.0	..	2.0	0.0	0.0	0.0	0.0	9
	4415.9	0.0	0.0	0.0				3.0	..	2.0	0.0	0.0	0.0	0.0	10
	4366.9	0.0	4.0	4.0	4.0	..	6.0	6.0	..	1.0	0.0	0.0	0.0	0.0	11
	4075.9	0.0	3.0	0.0	2.0	6.0	8.0	6.0	0.0	0.0	0.0	0.0	0.0	0.0	12
	4072.2	0.0	0.0	0.0	2.0	7.0	9.0	6.0	0.0	0.0	0.0	0.0	0.0	0.0	13
	4069.9	0.0	0.0	0.0	4.0	6.0	8.0	6.0	0.0	0.0	0.0	0.0	0.0	0.0	14
S+	4815	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	x	0.0	0.0	0.0	1
	4174.5	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	3.0	0.0	0.0	0.0	2
	4162.9	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	3.0	0.0	0.0	0.0	3
S++	4295	0.0	0.0	0.0	0.0	0.0	1.0	0.0	0.0	0.0	0.0	0.0	0.0	0.0	4
	4285.0	0.0	0.0	0.0	0.0	0.0	6.0	4.0	0.0	0.0	0.0	0.0	0.0	0.0	5
	4253.8	0.0	0.0	0.0	0.0	6.2	6.8	6.0	0.0	0.0	0.0	0.0	0.0	0.0	6

NOTES TO TABLE XXXIII

Atom	Note	Maximum	Remarks
C++	[1]		Line blended, in stars cooler than , with V+ 4649.1. Attributed by Fowler and Milne, and by Hartree, to C+++
N+	[1]		Unblended
N++	[2]
	[3]		Blended with the Si+++ line at 4096, which is probably effective throughout the whole range
O+	[1]
	[2]
	[3]	?
	[4]	?
	[5]		Blended with C++ line at 4649, which preponderates in stars hotter than , and probably contributes largely in that class
	[6]
	[7]
	[8]
	[9]
	[10]
	[11]	?	Certainly another line is here involved, but it has not been identified
	[12]
	[13]
	[14]
S+	[1] [2] [3]		Lines recorded by Lockyer; not measured by the writer
S++	[4]		Line recorded by Lockyer. Intensity from H.A., 28; not measured by the writer
	[5]
	[6]		Recorded by H. H. Plaskett in 10 Lacertae

V. MATERIAL BEARING ON THE CLASSIFICATION OF

STARS, QUOTED IN CHAPTER XII

IN illustration of the problem of Class

, observations of sixty-two stars are collected in the following table. Successive columns contain the H.D. number, the name of the star, the apparent magnitude, the reduced proper motion

, and the spectral class. Then follow columns which indicate the presence (

) or absence of metallic lines, the quality of the lines (sharp lines being represented by the letter

and hazy lines by the letter

), the presence of wings to the hydrogen lines, and the strength of the Sr+ line at 4077 and the Si+ lines at 4128, 4131.

The stars in each class are arranged in order of increasing strength of metallic lines, and it will be seen that this feature is correlated with the strength of the silicon and strontium lines, but not with the line quality or the hydrogen wings, nor with the reduced proper motion.

[TABLE XXXIV]

H. D.	Star		m	H	Class	Metalic Lines	Line Quality	H wings	Sr+	Si+
120198	84	UMa	5.53	6.4		x			9	10
108662	17	Com	5.38	2.7		x			7	8
170397	Br	2314	5.99	2.7		x	h		6	9
133029	+47°	2192	6.16	-		x	h		5	11
140160		Ser	5.26	3.5		x			10	5
94334		Uma	4.34	3.6		x	s		2	3
58142	21	Lyn	4.45	2.9			h		-	4
192913	+27°	3668	6.69	-			h		?	7
225132	2	Cet	4.62	1.2			h		-	4
41841	89	Lep	5.50	2.2					-	-
222661		Aqr	4.62	4.8			h		-	-
87887	15	Sex	4.6	1.9					-	5
213323	38	Peg	5.51	3.3					-	-
25642		Per	4.33	2.2					-	4
114330		Vir	4.44	3.2			s		-	3
109485	23	Com	4.78	4.1			s		-	3
103632		Cra	5.16	3.8				x	-	-
110411		Vir	4.95	5.6				x	-	-
133962	k	Boo	5.59	4.6				x	-	-
188260	13	Vul	4.50	2.5			h	x	-	4
124224		12	4.90	3.8					-	11
183056	4	Cyg	5.2	-0.4					-	9
183986	+35°	3658	6.04	-				x	-	5

196502	73	Dra	5.18	1.2		x	s		12	10
148367		Oph	4.68	4.3		x	s	x	9	8
118022	78	Vir	4.93	3.5		x			10	9
182564		Dra	4.63	2.9		x			7	7
125337		Vir	4.60	-1.9		x	h		7	6
214734	30	Cep	5.21	1.6		x			3?	5
7804	89	Psc	5.28	4.2		x		x	5	7
220825		Psc	4.94	-		x			6	7
72968	3	Hya	5.61	2.8		x			6	7
56405	Paris	8971	5.39	4.7		x	s	s	3?	6
20677	32	Per	4.98	3.8		x		x	-	5
48250	12	Lyn	4.89	1.8		x		x	-	5
107612	-	Com	6.56	-				x	9	-
18519,20		Ari	4.6	1.1	,		s		3	3
107966	13	Com	5.10	2.7					-	-
108382	16	Com	5.04	0.6					-	-

108945	21	Com	5.39	1.9		x			11	9
108642	+26°	2138	6.48	-		x			8	6
89904	27	Lmi	6.1	3.0		x	h	x	6	9
108651	+26°	2353	6.69	-		x	h		7	6
170296		Scu	4.73	-0.5		x	h	x	-	7
115331	196	Cen	6.0	3.4			h		9	-
108486	+26°	2352	6.57	-					7	-
104321		Vir	4.57	2.2					5	-

222345		Aqr	5.16	4.6		x			-	9
14690	70	Cet	5.62	4.3		x			7	?
189849	15	Vul	4.74	3.3		x	s	x	9	6
28546	81	Tau	5.49	5.7		x			9	9
40536	2	Mon	5.10	4.0		x	h?		7	7
15089		Cas	4.59	0.5		x			12	9
91312	Gr	1658	4.85	5.6		x	s	x	5	6
159560		Dra	4.95	6.0					8	-

90277	30	Lmi	4.85	5.0		x			9	9
57749		86	5.83	2.3		x			9	6
92787		135	5.28	7.6		x	s		9	6
112429	8	Dra	5.27	3.0		x			7	7
28485	80	Tau	5.70	5.8			h		6	5
28677	85	Tau	6.04	-		-			7	-