Stellar laboratories - IX. New Se v, Sr iv–vii, Te vi, and I vi oscillator strengths and the Se, Sr, Te, and I abundances in the hot white dwarfs G191−B2B and RE 0503−289

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Volume 606 (October 2017)

A&A, 606 (2017) A105

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Table 2

Identified Se v, Sr v, Te vi, and I vi lines in the UV spectrum of RE 0503−289.

Ion	Wavelength/Å	Comment

Sr v	915.994	uncertain
Sr v	917.802
I vi	919.210	blend, uncertain
I vi	919.555	blend, uncertain
Sr v	922.397
Sr v	935.509	blend, weak Ga vi
Sr v	942.943
Sr v	946.530
Te vi	951.021^a
Sr v	951.044	blend, strong Te vi
Sr v	951.159
Sr v	962.378	blend, weak O iii
Sr v	985.408	uncertain
Sr v	1013.714
Sr v	1038.990
Sr v	1041.940
I vi	1053.389	weak
I vi	1057.530	blend, strong Zn v
Te vi	1071.414^a
Se v	1094.691^a
I vi	1120.301^a
Se v	1150.986^a	shifted^b to 1151.016 Å
I vi	1153.262
Sr v	1154.871
Sr v	1159.599	uncertain
Sr v	1163.040
Se v	1227.446	shifted^c to 1227.540 Å
Te vi	1313.874
Sr v	1372.590
Sr v	1372.843
Sr v	1379.615	blend, weak Al iii
Sr v	1380.053	uncertain
Sr v	1380.477
Sr v	1387.288	uncertain
Sr v	1390.084
Sr v	1395.216	uncertain
Sr v	1396.308	blend, Sr vλ 1396.365 Å
Sr v	1396.365	blend, Sr vλ 1396.308 Å
Sr v	1404.048
Sr v	1412.958
Sr v	1413.882
Sr v	1437.898
Se v	1451.779	shifted^d to 1451.653 Å
Se v	1454.292

Notes. The wavelengths correspond to those in Table A.17.

^(a)

Identified by Werner et al. (2012b),

^(b)

shifted to match observation. Rao & Badami (1931) measured 1151.96 Å,

^(c)

shifted to match observation. Rao & Badami (1931) measured 1227.58 Å,

^(d)

shifted to match observation.

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