Complete spectral energy distribution of the hot, helium-rich white dwarf RX J0503.9–2854

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Table 1

History of T_eff and log g determinations (cf., Müller-Ringat 2013).

T_eff/kK	log g	Model atmosphere	Method	Comment	Reference

60 − 90			EUV, PM	very low N_{H i}	Barstow et al. (1993)
60 − 80			EUV, OPT	very low N_{H i}	Barstow et al. (1993)
60 − 80	7.5−8.0	He, HHeC	NLTE, OPT, UV, EUV	EUV problem^a	Barstow et al. (1994)
60 − 70			EUV, PM	very low N_{H i}	Vennes et al. (1994)
70^b	7.0	HeCNOSiFeNi	LTE, EUV, UV		Polomski et al. (1995)
65^c	7.5^d	HHeC	NLTE, OPT	no H detectable, upper limit 5% (mass fraction)	Werner (1996)
70	7.5	HHeCNOSi	NLTE, OPT, UV	M = 0.49 M_⊙	Dreizler & Werner (1996)
66.6 − 70.4	7.13−7.27	HHe	LTE, UV	M = 0.40 M_⊙	Vennes et al. (1998)
70^e	7.5^e		NLTE, diffusion	no good fit achieved	Dreizler (1999)
69 − 75	7.26−7.63	HHeC	NLTE, OPT, UV, EUV	EUV problem^a	Barstow et al. (2000)
		HHeCNOSiFeNi
65 − 70	7.5^e	HeCNi, HeONi	NLTE, EUV	EUV problem^a	Werner et al. (2001)
70^e	7.5^e	HHeCNOSiFeNi+	NLTE, UV	EUV problem^a	Barstow et al. (2007)
		PS	LTE
68 − 72	7.4−7.6	HeCNOAlSiPS+	NLTE, OPT, UV		Rauch et al. (2016a)
		CaScTiVCrMnFeCrNi+
		ZnGaGeAsKrZrMoSnXeBa

Notes. PM denotes photometry.

^(a)

Section 7,

^(b)

adopted upper limit of Vennes et al. (1994),

^(c)

adopted value close to lower limit of Barstow et al. (1994),

^(d)

adopted from Barstow et al. (1994),

^(e)

adopted from Dreizler & Werner (1996).

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