Stellar laboratories - VII. New Kr iv – vii oscillator strengths and an improved spectral analysis of the hot, hydrogen-deficient DO-type white dwarf RE 0503−289

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Table 3

Comparison of log gf values of Kr lines used in the abundance analysis (Figs. 5, 8).

	log gf
Wavelength/Å
	Literature	Our work

Kr v
1384.611	−0 .590^a	−1 .128
1387.961	−0 .650^a	−0 .749
1392.594	−0 .670^a	−0 .420
1393.603	−0 .170^a	−0 .224
1515.611	0 .400^a	−0 .540
1566.073	0 .300^a	0 .365
1583.456	−0 .555^a	−0 .603
1589.269	0 .680^a	0 .709
1591.875	0 .490^a	0 .415
1764.478	−0 .160^a	−0 .169
Kr vi
919.938	−1 .950^b	−2 .22
927.334	−2 .420^b	−2 .50
931.368	−2 .005^b	−2 .05
944.046	−0 .959^b	−1 .11
956.617	−0 .974^b	−0 .97
965.093	−0 .019^b	−0 .02
970.092	−2 .731^b	−2 .76
980.411	−0 .278^b	−0 .28
1002.748	−2 .748^b	−2 .88
1011.133	−1 .826^b	−1 .84
1015.765	−1 .580^b	−1 .83
1045.238	−0 .823^b	−0 .98
1052.964	−1 .561^b	−1 .72
1061.064	−0 .409^b	−0 .58
Kr vii
918.444	−0 .134^c	−0 .38

Reference.

^(a)

Raineri et al. (2012);

^(b)

Pagan et al. (1996);

^(c)

Victor & Taylor (1983).

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