Chlorinelike spectra of copper to molybdenum

Victor Kaufman; Jack Sugar; William L. Rowan

doi:10.1364/JOSAB.6.001444

Journal of the Optical Society of America B
Vol. 6,
Issue 8,
pp. 1444-1446
(1989)
•https://doi.org/10.1364/JOSAB.6.001444

Chlorinelike spectra of copper to molybdenum

Victor Kaufman, Jack Sugar, and William L. Rowan

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Victor Kaufman, Jack Sugar, and William L. Rowan, "Chlorinelike spectra of copper to molybdenum," J. Opt. Soc. Am. B 6, 1444-1446 (1989)

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Abstract

Spectra of Cu to Mo (except for Rb and Sr) were generated in tokamak and laser-produced plasmas and observed photographically. Six lines have been identified in each of the spectra as Cl-like 3s²3p⁵–3s²3p⁴3d transitions. Wavelengths in the range of 75–150 Å, measured with an uncertainty of ±0.005 Å, are given. Line classifications were made by comparing the observed wavelengths and relative intensities with those calculated using the relativistic average-of-configuration Hartree–Fock code of Cowan. Predicted values for the corresponding wavelengths of Cl-like Rb and Sr were obtained from these comparisons, with an uncertainty of ±0.010 Å.

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	${{}^{2}P}_{3 / 2}^{\circ} - ({}^{3}P) {{}^{2}D}_{3 / 2}$		${{}^{2}P}_{3 / 2}^{\circ} - ({}^{3}P) {{}^{2}D}_{5 / 2}$		${{}^{2}P}_{1 / 2}^{\circ} - ({}^{3}P) {{}^{2}D}_{3 / 2}$		${{}^{2}P}_{3 / 2}^{\circ} - ({}^{3}P) {{}^{2}P}_{3 / 2}$		${{}^{2}P}_{1 / 2}^{\circ} - ({}^{3}P) {{}^{2}P}_{1 / 2}$		${{}^{2}P}_{3 / 2}^{\circ} - ({}^{1}D) {{}^{2}S}_{1 / 2}$
Transition Ion	Wavelength	Intensity	Wavelength	Intensity	Wavelength	Intensity	Wavelength	Intensity	Wavelength	Intensity	Wavelength	Intensity
Cu xiii	138.065	20	142.963	200	143.756	200bl	144.720	20	148.318	20	150.638	10
Zn xiv	129.593	5	134.793	300	135.587	200	136.303	200	140.113	100	141.781	20
Ga xv	(121.926)		127.439	3	128.292	3	128.727	8	132.680	10	133.786	10
Ge xvi	114.979	5	120.802	50	121.670	100	121.877	50	125.963	100	126.545	20
As xvii	108.597	5	114.726	10	115.622	20bl	115.622	20bl	119.801	2	119.933	10bl
Se xviii	(102.688)^b		109.144	400	110.087	20	109.873	50	114.126	20	113.824	50
Br xix	(97.243)^c		103.979	100	104.976	20	104.577	30	108.890	10	108.213	20
Kr xx	(92.187)^d		99.156	200	100.254	60	99.660	200	104.028	10	103.021	20
Rb xxi	(87.458)		(94.539)		(95.851)		(95.066)		(99.513)		(98.174)
Sr xxii	(83.015)		(91.245)		(91.720)		(90.761)		(95.267)		(93.650)
Y xxiii	78.841	1	87.169	50	87.823	10	86.687	20	91.250	20	89.396	10
Zr xxiv	74.898	5	83.433	50	84.183	5	82.840	10	87.437	5	85.401	10
Nb xxv	71.140	1	79.923	60	80.696	3	79.179	20	83.603	8	81.615	10
Mo xxvi	(67.593)		76.624	200	77.369^e	5	75.698	20	79.726	3	78.056	20

	3s²3p⁵		3s²3p⁴3d

	${{}^{2}P}_{3 / 2}^{\circ}$	$2 P_{1 / 2}^{\circ}$ ^b	(¹D)²S_1/2	(³P)²P_3/2	(³P)²D_5/2	(³P)²P_1/2	(³P)²D_3/2
CU¹²⁺	0	28 560	663 840	690 990	699 480	702 790	724 240
Zn¹³⁺	0	34 210	705 310	733 660	741880	747 920	771 700
Ga¹⁴⁺	0	40 699	747 460	776 840	784 690	794 390	820 170
Ge¹⁵⁺	0	47 944	790 230	820 500	827 800	841 830	869 800
As¹⁶⁺	0	56 268	833 800	864 890	871 640	890 990	920 840
Se¹⁷⁺	0	65 454	878 550	910 140	916 220	941 680	973 830
Br¹⁸⁺	0	(75 758)	924 100	956 230	961 730	994 120	1 028 350
Kr¹⁹⁺	0	(87 287)^c	970 680	1 003 410	1 008 510	1 048 570	1 084 750
Rb²⁰⁺	0	(100 110)	(1 018 600)	(1 051 900)	(1 057 760)	(1 105 000)	(1 143 400)
Sr²¹⁺	0	(114 320)	(1 067 800)	(1 101 800)	(1 095 940)	(1 164 000)	(1 204 600)
Y²²⁺	0	130 022	1 118 620	1 153 580	1 147 200	1 225 910	1 268 680
Zr²³⁺	0	147 254	1 170 950	1 207 150	1 198 570	1 290 940	1 335 140
Nb²⁴⁺	0	(166 230)	1 225 260	1 262 960	1 125 200	1 362 360	1 405 520
Mo²⁵⁺	0	186 950	1 281 130	1 321 040^d	1 305 070	1 441 250	1 479 460

	${{}^{2}P}_{3 / 2}^{\circ} - ({}^{3}P) {{}^{2}D}_{3 / 2}$		${{}^{2}P}_{3 / 2}^{\circ} - ({}^{3}P) {{}^{2}D}_{5 / 2}$		${{}^{2}P}_{1 / 2}^{\circ} - ({}^{3}P) {{}^{2}D}_{3 / 2}$		${{}^{2}P}_{3 / 2}^{\circ} - ({}^{3}P) {{}^{2}P}_{3 / 2}$		${{}^{2}P}_{1 / 2}^{\circ} - ({}^{3}P) {{}^{2}P}_{1 / 2}$		${{}^{2}P}_{3 / 2}^{\circ} - ({}^{1}D) {{}^{2}S}_{1 / 2}$
Transition Ion	Wavelength	Intensity	Wavelength	Intensity	Wavelength	Intensity	Wavelength	Intensity	Wavelength	Intensity	Wavelength	Intensity
Cu xiii	138.065	20	142.963	200	143.756	200bl	144.720	20	148.318	20	150.638	10
Zn xiv	129.593	5	134.793	300	135.587	200	136.303	200	140.113	100	141.781	20
Ga xv	(121.926)		127.439	3	128.292	3	128.727	8	132.680	10	133.786	10
Ge xvi	114.979	5	120.802	50	121.670	100	121.877	50	125.963	100	126.545	20
As xvii	108.597	5	114.726	10	115.622	20bl	115.622	20bl	119.801	2	119.933	10bl
Se xviii	(102.688)^b		109.144	400	110.087	20	109.873	50	114.126	20	113.824	50
Br xix	(97.243)^c		103.979	100	104.976	20	104.577	30	108.890	10	108.213	20
Kr xx	(92.187)^d		99.156	200	100.254	60	99.660	200	104.028	10	103.021	20
Rb xxi	(87.458)		(94.539)		(95.851)		(95.066)		(99.513)		(98.174)
Sr xxii	(83.015)		(91.245)		(91.720)		(90.761)		(95.267)		(93.650)
Y xxiii	78.841	1	87.169	50	87.823	10	86.687	20	91.250	20	89.396	10
Zr xxiv	74.898	5	83.433	50	84.183	5	82.840	10	87.437	5	85.401	10
Nb xxv	71.140	1	79.923	60	80.696	3	79.179	20	83.603	8	81.615	10
Mo xxvi	(67.593)		76.624	200	77.369^e	5	75.698	20	79.726	3	78.056	20

	3s²3p⁵		3s²3p⁴3d

	${{}^{2}P}_{3 / 2}^{\circ}$	$2 P_{1 / 2}^{\circ}$ ^b	(¹D)²S_1/2	(³P)²P_3/2	(³P)²D_5/2	(³P)²P_1/2	(³P)²D_3/2
CU¹²⁺	0	28 560	663 840	690 990	699 480	702 790	724 240
Zn¹³⁺	0	34 210	705 310	733 660	741880	747 920	771 700
Ga¹⁴⁺	0	40 699	747 460	776 840	784 690	794 390	820 170
Ge¹⁵⁺	0	47 944	790 230	820 500	827 800	841 830	869 800
As¹⁶⁺	0	56 268	833 800	864 890	871 640	890 990	920 840
Se¹⁷⁺	0	65 454	878 550	910 140	916 220	941 680	973 830
Br¹⁸⁺	0	(75 758)	924 100	956 230	961 730	994 120	1 028 350
Kr¹⁹⁺	0	(87 287)^c	970 680	1 003 410	1 008 510	1 048 570	1 084 750
Rb²⁰⁺	0	(100 110)	(1 018 600)	(1 051 900)	(1 057 760)	(1 105 000)	(1 143 400)
Sr²¹⁺	0	(114 320)	(1 067 800)	(1 101 800)	(1 095 940)	(1 164 000)	(1 204 600)
Y²²⁺	0	130 022	1 118 620	1 153 580	1 147 200	1 225 910	1 268 680
Zr²³⁺	0	147 254	1 170 950	1 207 150	1 198 570	1 290 940	1 335 140
Nb²⁴⁺	0	(166 230)	1 225 260	1 262 960	1 125 200	1 362 360	1 405 520
Mo²⁵⁺	0	186 950	1 281 130	1 321 040^d	1 305 070	1 441 250	1 479 460

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Journal of the Optical Society of America B